FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Sanderson, AJR O'Sullivan, E Ponman, TJ Gonzalez, AH Sivanandam, S Zabludoff, AI Zaritsky, D AF Sanderson, Alastair J. R. O'Sullivan, Ewan Ponman, Trevor J. Gonzalez, Anthony H. Sivanandam, Suresh Zabludoff, Ann I. Zaritsky, Dennis TI The baryon budget on the galaxy group/cluster boundary SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: stellar content; cosmology: observations; X-rays: galaxies: clusters ID X-RAY LUMINOSITY; XMM-NEWTON; CHANDRA SAMPLE; OUTER REGIONS; COSMOLOGICAL SIMULATIONS; TEMPERATURE RELATION; INTRACLUSTER MEDIUM; GAS PROPERTIES; CLUSTER GAS; MASS AB We present a study of the hot gas and stellar content of five optically selected poor galaxy clusters, including a full accounting of the contribution from intracluster light (ICL) and a combined hot gas and hydrostatic X-ray mass analysis with XMM-Newton observations. We find weighted mean stellar (including ICL), gas and total baryon mass fractions within r(500) of 0.026 +/- 0.003, 0.070 +/- 0.005 and 0.096 +/- 0.006, respectively, at a corresponding weighted mean M-500 of (1.08(-0.18)(+0.21)) x 10(14) M-circle dot. Even when accounting for the intracluster stars, four out of five clusters show evidence for a substantial baryon deficit within r(500), with baryon fractions (f(b)) between 50 +/- 6 and 59 +/- 8 per cent of the universal mean level (i.e. Omega(b)/Omega(m)), the remaining cluster having f(b) = 75 +/- 11 per cent. For the three clusters where we can trace the hot halo to r(500) we find no evidence for a steepening of the gas density profile in the outskirts with respect to a power law, as seen in more massive clusters. We find that in all cases, the X-ray mass measurements are larger than those originally published on the basis of the galaxy velocity dispersion (sigma) and an assumed sigma-M-500 relation, by a factor of 1.7-5.7. Despite these increased masses, the stellar fractions (in the range 0.016-0.034, within r(500)) remain consistent with the trend with mass published by Gonzalez et al., from which our sample is drawn. C1 [Sanderson, Alastair J. R.; O'Sullivan, Ewan; Ponman, Trevor J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [Sivanandam, Suresh; Zabludoff, Ann I.; Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sivanandam, Suresh] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Sanderson, AJR (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM ajrs@star.sr.bham.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900 FU Science and Technology Facilities Council (STFC); EU Marie Curie fellowship FX AJRS acknowledges support from the Science and Technology Facilities Council (STFC) and EOS acknowledges support from an EU Marie Curie fellowship. This work made use of the NASA/IPAC Extragalactic Database (NED) and data from the Two Micron All Sky Survey (2MASS). AJRS thanks Ian McCarthy for useful discussions and acknowledges the excellent GGPLOT2 package in R (Wickham 2009) which was used to create the plots in this paper. NR 67 TC 12 Z9 12 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2013 VL 429 IS 4 BP 3288 EP 3304 DI 10.1093/mnras/sts586 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600042 ER PT J AU Bird, S Vogelsberger, M Sijacki, D Zaldarriaga, M Springel, V Hernquist, L AF Bird, Simeon Vogelsberger, Mark Sijacki, Debora Zaldarriaga, Matias Springel, Volker Hernquist, Lars TI Moving-mesh cosmology: properties of neutral hydrogen in absorption SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; intergalactic medium; cosmology: theory ID DAMPED LY-ALPHA; SMOOTHED PARTICLE HYDRODYNAMICS; COLD DARK-MATTER; LYMAN LIMIT SYSTEMS; COLUMN DENSITY DISTRIBUTION; GALAXY FORMATION MODELS; FLUX POWER SPECTRUM; DIGITAL SKY SURVEY; INTERGALACTIC MEDIUM; STAR-FORMATION AB We examine the distribution of neutral hydrogen in cosmological simulations carried out with the new moving-mesh code AREPO and compare it with the corresponding GADGET simulations based on the smoothed particle hydrodynamics (SPH) technique. The two codes use identical gravity solvers and baryonic physics implementations, but very different methods for solving the Euler equations, allowing us to assess how numerical effects associated with the hydro solver impact the results of simulations. Here we focus on an analysis of the neutral gas, as detected in quasar absorption lines. We find that the high column density regime probed by damped Ly alpha (DLA) and Lyman limit systems (LLS) exhibits significant differences between the codes. GADGET produces spurious artefacts in large haloes in the form of gaseous clumps, boosting the LLS cross-section. Furthermore, it forms haloes with denser central baryonic cores than AREPO, which leads to a substantially greater DLA cross-section from smaller haloes. AREPO thus produces a significantly lower cumulative abundance of DLAs, which is intriguingly in much closer agreement with observations. The column density function, however, is not altered enough to significantly reduce the discrepancy with the observed value. For the low column density gas probed by the Ly alpha forest, the codes differ only at the level of a few per cent, suggesting that this regime is quite well described by both methods, a fact that is reassuring for the many Ly alpha studies carried out with SPH thus far. While the residual differences are smaller than the errors on current Ly alpha forest data, we note that this will likely change for future precision experiments. C1 [Bird, Simeon; Zaldarriaga, Matias] Inst Adv Study, Princeton, NJ 08540 USA. [Vogelsberger, Mark; Sijacki, Debora; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. RP Bird, S (reprint author), Inst Adv Study, 1 Einstein Dr, Princeton, NJ 08540 USA. EM spb@ias.edu OI Bird, Simeon/0000-0001-5803-5490 FU National Science Foundation [AST-0907969, PHY-0855425, PHY-1213563]; Institute for Advanced Study; NASA Hubble Fellowship [HST-HF-51282.01-A]; David and Lucile Packard Foundation; Klaus Tschira Foundation; Deutsche Forschungsgemeinschaft [SFB 881]; NASA ATP [NNX12AC67G] FX SB would like to thank Yajima Hidenobu for sending us his collation of observational data on the column density function. SB is supported by the National Science Foundation grant number AST-0907969 and the Institute for Advanced Study. DS acknowledges NASA Hubble Fellowship through grant HST-HF-51282.01-A. MZ is supported by the National Science Foundation under PHY-0855425, AST-0907969 and PHY-1213563 and by the David and Lucile Packard Foundation. VS acknowledges financial support from the Klaus Tschira Foundation and the Deutsche Forschungsgemeinschaft through SFB 881, 'The Milky Way System'. LH is supported by NASA ATP Award NNX12AC67G. NR 89 TC 30 Z9 30 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2013 VL 429 IS 4 BP 3341 EP 3352 DI 10.1093/mnras/sts590 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600046 ER PT J AU Nelson, D Vogelsberger, M Genel, S Sijacki, D Keres, D Springel, V Hernquist, L AF Nelson, Dylan Vogelsberger, Mark Genel, Shy Sijacki, Debora Keres, Dusan Springel, Volker Hernquist, Lars TI Moving mesh cosmology: tracing cosmological gas accretion SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; galaxies: haloes; cosmology: theory ID SMOOTHED PARTICLE HYDRODYNAMICS; GALAXY FORMATION; STAR-FORMATION; HIGH-REDSHIFT; DARK-MATTER; COLD FLOWS; COSMIC GAS; SIMULATIONS; HALOES; MODE AB We investigate the nature of gas accretion on to haloes and galaxies at z=2 using cosmological hydrodynamic simulations run with the moving mesh code AREPO. Implementing a Monte Carlo tracer particle scheme to determine the origin and thermodynamic history of accreting gas, we make quantitative comparisons to an otherwise identical simulation run with the smoothed particle hydrodynamics (SPH) code GADGET-3. Contrasting these two numerical approaches, we find significant physical differences in the thermodynamic history of accreted gas in massive haloes above similar or equal to 10(10.5) M-circle dot. In agreement with previous work, GADGET simulations show a cold fraction near unity for galaxies forming in massive haloes, implying that only a small percentage of accreted gas heats to an appreciable fraction of the virial temperature during accretion. The same galaxies in AREPO show a much lower cold fraction, for instance, <20 per cent in haloes with M-halo similar or equal to 10(11) M-circle dot. This results from a hot gas accretion rate which, at this same halo mass, is an order of magnitude larger than with GADGET, together with a cold accretion rate which is lower by a factor of 2. These discrepancies increase for more massive systems, and we explain both trends in terms of numerical inaccuracies with the standard formulation of SPH. We note, however, that changes in the treatment of interstellar medium physics feedback, in particular - could modify the observed differences between codes as well as the relative importance of different accretion modes. We explore these differences by evaluating several ways of measuring a cold mode of accretion. As in previous work, the maximum past temperature of gas is compared to either a constant threshold value or some fraction of the virial temperature of each parent halo. We find that the relatively sharp transition from cold- to hot-mode-dominated accretion at halo masses of similar or equal to 10(11) M-circle dot is a consequence of the constant temperature criterion, which can only separate virialized gas above some minimum halo mass. Examining the spatial distribution of accreting gas, we find that the filamentary geometry of accreting gas near the virial radius is a common feature in massive haloes above similar or equal to 10(11.5) M-circle dot. Gas filaments in GADGET, however, tend to remain collimated and flow coherently to small radii, or artificially fragment and form a large number of purely numerical 'blobs'. These same filamentary gas streams in AREPO show increased heating and disruption at 0.25-0.5r(vir) and contribute to the hot gas accretion rate in a manner distinct from classical cooling flows. C1 [Nelson, Dylan; Vogelsberger, Mark; Genel, Shy; Sijacki, Debora; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Keres, Dusan] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. RP Nelson, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dnelson@cfa.harvard.edu OI Genel, Shy/0000-0002-3185-1540 FU NASA Hubble Fellowship [HST-HF-51282.01-A] FX DN would like to thank Claude-Andre Faucher-Giguere, Patrik Jonsson, Diego Munoz and Paul Torrey for many insightful discussions, comments and suggestions. The computations presented in this paper were performed on the Odyssey cluster at Harvard University. DS acknowledges a NASA Hubble Fellowship through grant HST-HF-51282.01-A. NR 57 TC 127 Z9 127 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2013 VL 429 IS 4 BP 3353 EP 3370 DI 10.1093/mnras/sts595 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600047 ER PT J AU Bloemen, S Steeghs, D De Smedt, K Vos, J Gansicke, BT Marsh, TR Rodriguez-Gil, P AF Bloemen, S. Steeghs, D. De Smedt, K. Vos, J. Gaensicke, B. T. Marsh, T. R. Rodriguez-Gil, P. TI Remarkable spectral variability on the spin period of the accreting white dwarf in V455 And SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: V455 And; novae, cataclysmic variables; white dwarfs ID RESOLVED OPTICAL SPECTROSCOPY; VARIABLE AE AQUARII; X-RAY OBSERVATIONS; INTERMEDIATE POLARS; CATACLYSMIC VARIABLES; MAGNETIC PROPELLER; DQ HERCULIS; SPACED DATA; WZ SGE; OSCILLATIONS AB We present spin-resolved spectroscopy of the accreting white dwarf binary V455 And. With a suggested spin period of only 67 s, it has one of the fastest spinning white dwarfs known. To study the spectral variability on the spin period of the white dwarf, we observed V455 And with 2 s integration times, which is significantly shorter than the spin rate of the white dwarf. To achieve this cadence, we used the blue arm of the ISIS spectrograph at the 4.2-m William Herschel Telescope, equipped with an electron multiplying CCD (EMCCD). Strong coherent signals were detected in our time series, which led to a robust determination of the spin period of the white dwarf (P-spin = 67.619 +/- 0.002 s). Folding the spectra on the white dwarf spin period uncovered very complex emission line variations in H gamma, HeI lambda 4472 and HeII lambda 4686. We attribute the observed spin phase dependence of the emission line shape to the presence of magnetically controlled accretion on to the white dwarf via accretion curtains, consistent with an intermediate polar type system. We are, however, not aware of any specific model that can quantitatively explain the complex velocity variations we detect in our observations. The orbital variations in the spectral lines indicate that the accretion disc of V455 And is rather structureless, contrary to the disc of the prototype of the intermediate polars, DQ Her. This work demonstrates the potential of EMCCDs to observe faint targets at high cadence, as readout noise would make such a study impossible with conventional CCDs. C1 [Bloemen, S.; De Smedt, K.; Vos, J.] Univ Louvain, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Steeghs, D.; Gaensicke, B. T.; Marsh, T. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rodriguez-Gil, P.] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain. RP Bloemen, S (reprint author), Univ Louvain, Inst Sterrenkunde, Celestijnenlaan 200 D, B-3001 Louvain, Belgium. EM steven.bloemen@ster.kuleuven.be RI Steeghs, Danny/C-5468-2009; Gaensicke, Boris/A-9421-2012; Rodriguez-Gil, Pablo/H-7709-2015 OI Steeghs, Danny/0000-0003-0771-4746; Gaensicke, Boris/0000-0002-2761-3005; Rodriguez-Gil, Pablo/0000-0002-4717-5102 FU European Research Council under the European Community [227224]; UK's Science and Technology Facilities Council (STFC) [ST/F002599/1, PP/D005914/1] FX The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no227224 (PROSPERITY). During this research DS and TRM were supported under grants from the UK's Science and Technology Facilities Council (STFC, ST/F002599/1 and PP/D005914/1 Advanced Fellowship). NR 32 TC 9 Z9 9 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2013 VL 429 IS 4 BP 3433 EP 3438 DI 10.1093/mnras/sts622 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600054 ER PT J AU Sadowski, A Narayan, R Tchekhovskoy, A Zhu, YC AF Sadowski, Aleksander Narayan, Ramesh Tchekhovskoy, Alexander Zhu, Yucong TI Semi-implicit scheme for treating radiation under M1 closure in general relativistic conservative fluid dynamics codes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; radiation transfer ID BLACK-HOLE ACCRETION; ADVECTION-DOMINATED ACCRETION; X-RAY BINARIES; MAGNETOHYDRODYNAMIC SIMULATIONS; 3-DIMENSIONAL SIMULATIONS; COMPARABLE RADIATION; SPHERICAL ACCRETION; LIMITED DIFFUSION; OPTICALLY THICK; SAGITTARIUS-A AB A numerical scheme is described for including radiation in multidimensional general relativistic conservative fluid dynamics codes. In this method, a covariant form of the M1 closure scheme is used to close the radiation moments, and the radiative source terms are treated semi-implicitly in order to handle both optically thin and optically thick regimes. The scheme has been implemented in a conservative general relativistic radiation hydrodynamics code KORAL. The robustness of the code is demonstrated on a number of test problems, including radiative relativistic shock tubes, static radiation pressure supported atmosphere, shadows, beams of light in curved space-time and radiative Bondi accretion. The advantages of M1 closure relative to other approaches such as the Eddington closure and flux-limited diffusion are discussed, and its limitations are also highlighted. C1 [Sadowski, Aleksander; Narayan, Ramesh; Zhu, Yucong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02134 USA. [Tchekhovskoy, Alexander] Princeton Univ, Princeton, NJ 08544 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02134 USA. EM asadowski@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G]; Princeton Center for Theoretical Science Fellowship; NSF [TG-AST080026N, TG-AST100040] FX The authors thank Frederic Vincent for calculating the photon trajectories shown in Fig. 13, James M. Stone for insightful discussions and the referee for helpful comments. RN and AS were supported in part by NASA grant NNX11AE16G. AT was supported by the Princeton Center for Theoretical Science Fellowship. We acknowledge NSF support via XSEDE resources, NICS Kraken and Nautilus under grant numbers TG-AST080026N (RN and AS) and TG-AST100040 (AT), and NASA support via High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center (AS and RN) that provided access to the Pleiades supercomputer. NR 80 TC 35 Z9 36 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR PY 2013 VL 429 IS 4 BP 3533 EP 3550 DI 10.1093/mnras/sts632 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135FD UT WOS:000318272600063 ER PT J AU Acharya, BS Actis, M Aghajani, T Agnetta, G Aguilar, J Aharonian, F Ajello, M Akhperjanian, A Alcubierre, M Aleksic, J Alfaro, R Aliu, E Allafort, AJ Allan, D Allekotte, I Amato, E Anderson, J Anguner, EO Antonelli, LA Antoranz, P Aravantinos, A Arlen, T Armstrong, T Arnaldi, H Arrabito, L Asano, K Ashton, T Asorey, HG Awane, Y Baba, H Babic, A Baby, N Bahr, J Bais, A Baixeras, C Bajtlik, S Balbo, M Balis, D Balkowski, C Bamba, A Bandiera, R Barber, A Barbier, C Barcelo, M Barnacka, A Barnstedt, J de Almeida, UB Barrio, JA Basili, A Basso, S Bastieri, D Bauer, C Baushev, A Becerra, J Becherini, Y Bechtol, KC Tjus, JB Beckmann, V Bednarek, W Behera, B Belluso, M Benbow, W Berdugo, J Berger, K Bernard, F Bernardino, T Bernlohr, K Bhat, N Bhattacharyya, S Bigongiari, C Biland, A Billotta, S Bird, T Birsin, E Bissaldi, E Biteau, J Bitossi, M Blake, S Bigas, OB Blasi, P Bobkov, A Boccone, V Boettcher, M Bogacz, L Bogart, J Bogdan, M Boisson, C Gargallo, JB Bolmont, J Bonanno, G Bonardi, A Bonev, T Bonifacio, P Bonnoli, G Bordas, P Borgland, A Borkowski, J Bose, R Botner, O Bottani, A Bouchet, L Bourgeat, M Boutonnet, C Bouvier, A Brau-Nogue, S Braun, I Bretz, T Briggs, M Bringmann, T Brook, P Brun, P Brunetti, L Buanes, T Buckley, J Buehler, R Bugaev, V Bulgarelli, A Bulik, T Busetto, G Buson, S Byrum, K Cailles, M Cameron, R Camprecios, J Canestrari, R Cantu, S Capalbi, M Caraveo, P Carmona, E Carosi, A Carr, J Carton, PH Casanova, S Casiraghi, M Catalano, O Cavazzani, S Cazaux, S Cerruti, M Chabanne, E Chadwick, P Champion, C Chen, A Chiang, J Chiappetti, L Chikawa, M Chitnis, VR Chollet, F Chudoba, J Cieslar, M Cillis, A Cohen-Tanugi, J Colafrancesco, S Colin, P Calome, J Colonges, S Compin, M Conconi, P Conforti, V Connaughton, V Conrad, J Contreras, JL Coppi, P Corona, P Corti, D Cortina, J Cossio, L Costantini, H Cotter, G Courty, B Couturier, S Covino, S Crimi, G Criswell, SJ Croston, J Cusumano, G Dafonseca, M Dale, O Daniel, M Darling, J Davids, I Dazzi, F De Angelis, A De Caprio, V De Frondat, F Dal Pino, EMD de la Calle, I De La Vega, GA Lopez, RD De Lotto, B De Luca, A Neto, JRTD de Naurois, M de Oliveira, Y Wilhelmi, ED de Souza, V Decerprit, G Decock, G Deil, C Delagnes, E Deleglise, G Delgado, C Della Volpe, D Demange, P Depaola, G Dettlaff, A Di Paola, A Di Pierro, F Diaz, C Dick, J Dickherber, R Dickinson, H Diez-Blanco, V Digel, S Dimitrov, D Disset, G Djannati-Atai, A Doert, M Dohmke, M Domainko, W Prester, DD Donat, A Dorner, D Doro, M Dournaux, JL Drake, G Dravins, D Drury, L Dubois, F Dubois, R Dubus, G Dufour, C Dumas, D Dumm, J Durand, D Dyks, J Dyrda, M Ebr, J Edy, E Egberts, K Eger, P Einecke, S Eleftheriadis, C Elles, S Emmanoulopoulos, D Engelhaupt, D Enomoto, R Ernenwein, JP Errando, M Etchegoyen, A Evans, P Falcone, A Fantinel, D Farakos, K Farnier, C Fasola, G Favill, B Fede, E Federici, S Fegan, S Feinstein, F Ferenc, D Ferrando, P Fesquet, M Fiasson, A Fillin-Martino, E Fink, D Finley, C Finley, JP Fiorini, M Curcoll, RF Flores, H Florin, D Focke, W Fohr, C Fokitis, E Font, L Fontaine, G Fornasa, M Forster, A Fortson, L Fouque, N Franckowiak, A Fransson, C Fraser, G Frei, R Albuquerque, IFM Fresnillo, L Fruck, C Fujita, Y Fukazawa, Y Fukui, Y Funk, S Gabele, W Gabici, S Gabriele, R Gadola, A Galante, N Gall, D Gallant, Y Gamez-Garcia, J Garcia, B Lopez, RG Gardiol, D Garrido, D Garrido, L Gascon, D Gaug, M Gaweda, J Gebremedhin, L Geffroy, N Gerard, L Ghedina, A Ghigo, M Giannakaki, E Gianotti, F Giarrusso, S Giavitto, G Giebels, B Gika, V Giommi, P Girard, N Giro, E Giuliani, A Glanzman, T Glicenstein, JF Godinovic, N Golev, V Berisso, MG Gomez-Ortega, J Gonzalez, MM Gonzalez, A Gonzalez, F Munoz, AG Gothe, KS Gougerot, M Graciani, R Grandi, P Granena, F Granot, J Grasseau, G Gredig, R Green, A Greenshaw, T Gregoire, T Grimm, O Grube, J Grudzinska, M Gruev, V Grunewald, S Grygorczuk, J Guarino, V Gunji, S Gyuk, G Hadasch, D Hagiwara, R Hahn, J Hakansson, N Hallgren, A Heras, NH Hara, S Hardcastle, MJ Harris, J Hassan, T Hatanaka, K Haubold, T Haupt, A Hayakawa, T Hayashida, M Heller, R Henault, F Henri, G Hermann, G Hermel, R Herrero, A Hidaka, N Hinton, J Hoffmann, D Hofmann, W Hofverberg, P Holder, J Horns, D Horville, D Houles, J Hrabovsky, M Hrupec, D Huan, H Huber, B Huet, JM Hughes, G Humensky, TB Huovelin, J Ibarra, A Illa, JM Impiombato, D Incorvaia, S Inoue, S Inoue, Y Ioka, K Ismailova, E Jablonski, C Jacholkowska, A Jamrozy, M Janiak, M Jean, P Jeanney, C Jimenez, JJ Jogler, T Johnson, T Journet, L Juffroy, C Jung, I Kaaret, P Kabuki, S Kagaya, M Kakuwa, J Kalkuhl, C Kankanyan, R Karastergiou, A Karcher, K Karczewski, M Karkar, S Kasperek, A Kastana, D Katagiri, H Kataoka, J Katarzynski, K Katz, U Kawanaka, N Kellner-Leidel, B Kelly, H Kendziorra, E Khelifi, B Kieda, DB Kifune, T Kihm, T Kishimoto, T Kitamoto, K Kluzniak, W Knapic, C Knapp, J Knodlseder, J Kock, F Kocot, J Kodani, K Kohne, JH Kohri, K Kokkotas, K Kolitzus, D Komin, N Kominis, I Konno, Y Koppel, H Korohoda, P Kosack, K Koss, G Kossakowski, R Kostka, P Koul, R Kowal, G Koyama, S Koziol, J Krahenbuhl, T Krause, J Krawzcynski, H Krennrich, F Krepps, A Kretzschmann, A Krobot, R Krueger, P Kubo, H Kudryavtsev, VA Kushida, J Kuznetsov, A La Barbera, A La Palombara, N La Parola, V La Rosa, G Lacombe, K Lamanna, G Lande, J Languignon, D Lapington, J Laporte, P Lavalley, C Le Flour, T Le Padellec, A Lee, SH Lee, WH de Oliveira, MAL Lelas, D Lenain, JP Leopold, DJ Lerch, T Lessio, L Lieunard, B Lindfors, E Liolios, A Lipniacka, A Lockart, H Lohse, T Lombardi, S Lopatin, A Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorca, A Lorenz, E Lubinski, P Lucarelli, F Ludecke, H Ludwin, J Luque-Escamilla, PL Lustermann, W Luz, O Lyard, E Maccarone, MC Maccarone, TJ Madejski, GM Madhavan, A Mahabir, M Maier, G Majumdar, P Malaguti, G Maltezos, S Manalaysay, A Mancilla, A Mandat, D Maneva, G Mangano, A Manigot, P Mannheim, K Manthos, I Maragos, N Marcowith, A Mariotti, M Marisaldi, M Markoff, S Marszalek, A Martens, C Marti, J Martin, JM Martin, P Martinez, G Martinez, F Martinez, M Masserot, A Mastichiadis, A Mathieu, A Matsumoto, H Mattana, F Mattiazzo, S Maurin, G Maxfield, S Maya, J Mazin, D Mc Comb, L McCubbin, N McHardy, I McKay, R Medina, C Melioli, C Melkumyan, D Mereghetti, S Mertsch, P Meucci, M Michalowski, J Micolon, P Mihailidis, A Mineo, T Minuti, M Mirabal, N Mirabel, F Miranda, JM Mirzoyan, R Mizuno, T Moal, B Moderski, R Mognet, I Molinari, E Molinaro, M Montaruli, T Monteiro, I Moore, P Olaizola, AM Mordalska, M Morello, C Mori, K Mottez, F Moudden, Y Moulin, E Mrusek, I Mukherjee, R Munar-Adrover, P Muraishi, H Murase, K Murphy, A Nagataki, S Naito, T Nakajima, D Nakamori, T Nakayama, K Naumann, C Naumann, D Naumann-Godo, M Nayman, P Nedbal, D Neise, D Nellen, L Neustroev, V Neyroud, N Nicastro, L 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Yebras, J. M. Yelos, D. Yoshida, A. Yoshida, T. Yoshikoshi, T. Zabalza, V. Zacharias, M. Zajczyk, A. Zanin, R. Zdziarski, A. Zech, A. Zhao, A. Zhou, X. Zietara, K. Ziolkowski, J. Ziolkowski, P. Zitelli, V. Zurbach, C. Zychowski, P. CA CTA Consortium TI Introducing the CTA concept SO ASTROPARTICLE PHYSICS LA English DT Article DE TeV gamma-ray astronomy; Air showers; Cherenkov Telescopes ID SUPERNOVA REMNANT W44; TELESCOPE; ASTRONOMY; EMISSION; MISSION; HESS AB The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project. (C) 2013 Elsevier B.V. All rights reserved. C1 [De La Vega, G. A.; Etchegoyen, A.; Garcia, B.; Mancilla, A.; Maya, J.; Sanchez, F.; Videla, M.; Yelos, D.] Inst Tecnol Detecc & Astroparticulas CNEA CONICET, Buenos Aires, DF, Argentina. [Allekotte, I.; Arnaldi, H.; Asorey, H. G.; Gomez Berisso, M.] Ctr Atom Bariloche CNEA CONICET IB UNCUYO, San Carlos De Bariloche, Rio Negro, Argentina. [Cillis, A.; Depaola, G.; Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio CONICET UBA, Buenos Aires, DF, Argentina. [Bouchet, L.; Medina, C.; Romero, G. 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[Kocot, J.; Ozieblo, A.; Sterzel, M.; Szepieniec, T.] Acad Comp Ctr CYFRONET AGH, Krakow, Poland. [Kasperek, Aci.; Korohoda, P.; Rajda, P. J.; Romaszkan, W.; Rupinski, M.; Winiarski, K.] AGH Univ Sci & Technol, Fac Elect Engn Automat Comp Sci & Elect, Krakow, Poland. [Bogacz, L.; Jamrozy, M.; Koziol, J.; Marszalek, A.; Ostrowski, M.; Stawarz, L.; Szostek, A.; Wierzcholska, A.; Zietara, K.] Jagiellonian Univ, Fac Phys Astron & Appl Comp Sci, PL-31007 Krakow, Poland. [Bajtlik, S.; Barnacka, A.; Borkowski, J.; Dyks, J.; Janiak, M.; Kluzniak, W.; Lubinski, P.; Moderski, R.; Rudak, B.; Sikora, M.; Zajczyk, A.; Zdziarski, A.; Ziolkowski, J.] Polish Acad Sci, Copernicus Astron Ctr, PL-00901 Warsaw, Poland. [Grygorczuk, J.; Karczewski, M.; Mordalska, M.; Nicolau-Kuklinski, J.; Platos, L.; Rataj, M.; Seweryn, K.; Sidz, M.; Tokarz, M.; Wawer, P.; Wawrzaszek, R.; Wisniewski, L.] Polish Acad Sci, Space Res Ctr, PL-00901 Warsaw, Poland. [Dyrda, M.; Ludwin, J.; Michalowski, J.; Niemiec, J.; Pyziol, R.; Sowinski, M.; Stodulski, M.; Ziolkowski, P.; Zychowski, P.] Polish Acad Sci, Inst Nucl Phys, PL-00901 Warsaw, Poland. [Katarzynski, K.] Nicolaus Copernicus Univ, Torun Ctr Astron, Torun, Poland. [Bednarek, W.; Niedzwiecki, A.; Sitarek, J.; Sobczynska, D.; Szanecki, M.] Univ Lodz, Fac Phys & Appl Comp Sci, PL-90131 Lodz, Poland. [Bulik, T.; Cieslar, M.; Grudzinska, M.; Pojmanski, G.; Suchenek, M.] Univ Warsaw, Fac Phys, PL-00325 Warsaw, Poland. [Veberic, D.] Univ Nova Gorica, Lab Astroparticle Phys, Nova Gorica, Slovenia. [Boettcher, M.; Casanova, S.; Krueger, P.; Vanderwalt, J.] North West Univ, Ctr Space Res, Potchefstroom, South Africa. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, Johannesburg, South Africa. [Berdugo, J.; Carmona, E.; Delgado, C.; Diaz, C.; Hamer Heras, N.; Martinez, G.] CIEMAT, E-28040 Madrid, Spain. [Aleksic, J.; Barcelo, M.; Blanch Bigas, O.; Boix Gargallo, J.; Cortina, J.; Firpo Curcoll, R.; Gaweda, J.; Giavitto, G.; Gonzalez, A.; Gonzalez Munoz, A.; Granena, F.; Illa, J. M.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo Olaizola, A.; Rico, J.; Sitarek, J.; Stamatescu, V.; Troyano, I.] Inst Fis Altes Energies, Barcelona, Spain. [Camprecios, J.; Calome, J.; de Ona Wilhelmi, E.; Hadasch, D.; Martinez, F.; Pedaletti, G.; Torres, D. F.] CSIC, Inst Ciencies Espai IEEC, Barcelona, Spain. [Torres, D. F.] ICREA, Barcelona, Spain. [Becerra, J.; Berger, K.; Garcia Lopez, R.; Herrero, A.; Puerto-Gimenez, I.] Inst Astrofis Canarias, La Palma, Spain. [Barrio, J. A.; Contreras, J. L.; de la Calle, I.; Dubois, F.; Hassan, T.; Ibarra, A.; Lopez, M.; Lorca, A.; Mirabal, N.; Padilla, L.; Ponz, J. D.; Racero, E.; Satalecka, K.; Scapin, V.; Tejedor, L. A.] Univ Complutense Madrid, Grp Altos Energias, E-28040 Madrid, Spain. [Antoranz, P.; Bernardino, T.; Fresnillo, L.; Jimenez, J. J.; Miranda, J. M.; Perez, M. D. C.; Vegas, I.; Yebras, J. M.] Univ Complutense Madrid, Grp Elect, E-28040 Madrid, Spain. [Gamez-Garcia, J.; Gomez-Ortega, J.; Luque-Escamilla, P. L.; Marti, J.] Univ Jaen, Escuela Politecn Super Jaen, Jaen, Spain. [Baixeras, C.; Doro, M.; Font, L.; Garrido, D.; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, E-08193 Barcelona, Spain. [Baixeras, C.; Doro, M.; Font, L.; Garrido, D.; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, E-08193 Barcelona, Spain. [Garrido, L.; Gascon, D.; Graciani, R.; Munar-Adrover, P.; Paredes, J. M.; Ribo, M.; Sanuy, A.; Sieiro, J.; Zabalza, V.; Zanin, R.] Univ Barcelona IEEC UB, ICC, Dept Astron & Meteorol, Barcelona, Spain. [Aghajani, T.; Dravins, D.] Lund Observ, S-22100 Lund, Sweden. [Ryde, F.] Royal Inst Technol KTH, Dept Phys, Oskar Klein Ctr, Stockholm, Sweden. [Conrad, J.; Dickinson, H.; Farnier, C.; Finley, C.; Fransson, C.; Ripken, J.] Stockholm Univ, S-10691 Stockholm, Sweden. [Botner, O.; Hallgren, A.] Uppsala Univ, Dept Phys & Astron, Uppsala, Sweden. [Bernard, F.; Bretz, T.; Frei, R.; Ribordy, M.] Ecole Polytech Fed Lausanne, High Energy Phys Lab, CH-1015 Lausanne, Switzerland. [Biland, A.; Braun, I.; Grimm, O.; Kraehenbuehl, T.; Lustermann, W.; Roeser, U.; Vogler, P.; von Gunten, H. -P.] Swiss Fed Inst Technol, Inst Particle Phys, Zurich, Switzerland. [Aguilar, J.; Basili, A.; Boccone, V.; Della Volpe, D.; Montaruli, T.] Univ Geneva, Dept Phys Nucl & Corpusculaire, CH-1211 Geneva 4, Switzerland. [Balbo, M.; Bretz, T.; Dorner, D.; Farnier, C.; Lyard, E.; Rohlfs, R.; Walter, R.] Univ Geneva, Observ Geneva, ISDC Data Ctr Astrophys, CH-1211 Geneva 4, Switzerland. [Florin, D.; Gadola, A.; Gredig, R.; Huber, B.; Manalaysay, A.; Steiner, S.; Straumann, U.; Vollhardt, A.] Univ Zurich, Inst Phys, CH-8006 Zurich, Switzerland. [Allan, D.; Armstrong, T.; Chadwick, P.; Daniel, M.; Harris, J.; Mc Comb, L.; Nolan, S.; Rulten, C.; Schmoll, J.; Shum, E.; Talbot, C.] Univ Durham, Dept Phys, Durham DH1 3HP, England. [Allan, D.; Armstrong, T.; Chadwick, P.; Daniel, M.; Harris, J.; Mc Comb, L.; Nolan, S.; Rulten, C.; Schmoll, J.; Shum, E.; Talbot, C.] Univ Durham, Ctr Adv Instrumentat, Durham DH1 3HP, England. [McCubbin, N.; Preece, R.] STFC Rutherford Appleton Lab, Chilton, England. [Murphy, A.] Univ Edinburgh, Sch Phys & Astron, Edinburgh EH8 9YL, Midlothian, Scotland. [Granot, J.; Hardcastle, M. J.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Ashton, T.; Blake, S.; Evans, P.; Favill, B.; Fraser, G.; Hinton, J.; Lapington, J.; Mahabir, M.; O'Brien, P.; Ohm, S.; Osborne, J.; Rosen, S.; Ross, D.; Starling, R.; Sykes, J.; Warwick, R.; White, R.; Wilkinson, M.; Willingale, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Darling, J.; Greenshaw, T.; Maxfield, S.; Sutcliffe, P.] Univ Liverpool, Oliver Lodge Lab, Liverpool L69 3BX, Merseyside, England. [Fornasa, M.; Green, A.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Brook, P.; Cotter, G.; Karastergiou, A.; Mertsch, P.; Potter, W.; Reville, B.; Sarkar, S.; Schure, K.; Silk, J.] Univ Oxford, Dept Phys, Oxford, England. [Kudryavtsev, V. A.] Univ Sheffield, Dept Phys & Astron, Sheffield, S Yorkshire, England. [Bird, T.; Croston, J.; Emmanoulopoulos, D.; Maccarone, T. J.; McHardy, I.] Univ Southampton, Sch Phys & Astron, Southampton SO9 5NH, Hants, England. [Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL USA. [Anderson, J.; Byrum, K.; Drake, G.; Guarino, V.; Krepps, A.; Wagner, R. G.; Zhao, A.] Argonne Natl Lab, Argonne, IL 60439 USA. [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Otte, N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Otte, N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Benbow, W.; Cerruti, M.; Criswell, S. J.; Galante, N.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Krennrich, F.; Madhavan, A.; McKay, R.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Smith, N.; Xiong, Q.] Pittsburg State Univ, Dept Phys, Pittsburg, KS USA. [Finley, J. P.; Sembroski, G. H.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Bouvier, A.; Gebremedhin, L.; Kuznetsov, A.; Parks, G.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Gebremedhin, L.; Kuznetsov, A.; Parks, G.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Ajello, M.; Allafort, A. J.; Bechtol, K. C.; Bogart, J.; Borgland, A.; Cameron, R.; Chiang, J.; Digel, S.; Dubois, R.; Focke, W.; Franckowiak, A.; Funk, S.; Glanzman, T.; Jogler, T.; Johnson, T.; Kelly, H.; Lande, J.; Madejski, G. M.; Sanchez-Conde, M.; Sapozhnikov, L.; Smith, D.; Tibaldo, L.; Usher, T.; Vandenbrouke, J.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A. J.; Bechtol, K. C.; Bogart, J.; Borgland, A.; Cameron, R.; Chiang, J.; Digel, S.; Dubois, R.; Focke, W.; Franckowiak, A.; Funk, S.; Glanzman, T.; Jogler, T.; Johnson, T.; Kelly, H.; Lande, J.; Madejski, G. M.; Sanchez-Conde, M.; Sapozhnikov, L.; Smith, D.; Tibaldo, L.; Usher, T.; Vandenbrouke, J.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Briggs, M.; Connaughton, V.; Engelhaupt, D.; Pelassa, V.; Reardon, P.] Univ Alabama Huntsville, Ctr Space Phys & Aeron Res, Huntsville, AL USA. [Arlen, T.; Bobkov, A.; Lockart, H.; Mognet, I.; Ong, R. A.; Rousselle, J.; Shi, J.; Vassiliev, V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Ferenc, D.] Univ Calif Davis, Davis, CA 95616 USA. [Bogdan, M.; Huan, H.; Northrop, R.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Dumm, J.; Fortson, L.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Barber, A.; Kieda, D. B.; Smith, A.; Smith, J.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT USA. [Bose, R.; Buckley, J.; Bugaev, V.; Dickherber, R.; Gruev, V.; Krawzcynski, H.; Leopold, D. J.; Moore, P.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Coppi, P.] Yale Univ, Dept Phys & Astron, New Haven, CT USA. RP Martinez, M (reprint author), Inst Fis Altes Energies, Barcelona, Spain. EM martinez@ifae.es RI Daniel, Michael/A-2903-2010; Komin, Nukri/J-6781-2015; Sao Carlos Institute of Physics, IFSC/USP/M-2664-2016; Torres, Diego/O-9422-2016; Dimitrov, Dinko/J-7682-2013; Drury, Luke/B-1916-2017; Barrio, Juan/L-3227-2014; Murase, Kohta/B-2710-2016; Moulin, Emmanuel/B-5959-2017; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Graciani Diaz, Ricardo/I-5152-2016; Nosek, Dalibor/F-1129-2017; Gascon, David/L-8464-2014; delagnes, eric/G-8782-2011; Poutanen, Juri/H-6651-2016; Sarkar, Subir/G-5978-2011; Lapington, Jon/A-7669-2012; Takahashi, Keitaro/L-5930-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya, Marcos/L-2304-2014; de Gouveia Dal Pino, Elisabete/H-9560-2013; Moura Santos, Edivaldo/K-5313-2016; Bissaldi, Elisabetta/K-7911-2016; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Neustroev, Vitaly/B-6351-2008; Casanova, Sabrina/J-8935-2013; Aguilar Sanchez, Juan Antonio/H-4467-2015; Antoranz, Pedro/H-5095-2015; Miranda, Jose Miguel/F-2913-2013; Delgado, Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Conforti, Vito/N-5681-2015; Blasi, Pasquale/O-9345-2015; Amato, Elena/P-2938-2015; de Mello Neto, Joao/C-5822-2013; Stamatescu, Victor/C-9945-2016; Bais, Alkiviadis/D-2230-2009; Babic, Ana/B-9599-2014; Todero Peixoto, Carlos Jose/G-3873-2012; Fontaine, Gerard/D-6420-2014; de souza, Vitor/D-1381-2012; Prouza, Michael/F-8514-2014; Mandat, Dusan/G-5580-2014; Ebr, Jan/H-8319-2012; van Eldik, Christopher/C-3901-2013; Tjus, Julia/G-8145-2012; Rando, Riccardo/M-7179-2013; Katz, Uli/E-1925-2013; Tejedor, Luis/N-5494-2014; Berdugo, Javier/A-2858-2015; Kokkotas, Kostas/B-7878-2010; Kominis, Iannis/C-5515-2011; Ribo, Marc/B-3579-2015; Funk, Stefan/B-7629-2015; Terada, Yukikatsu/A-5879-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015; Trifoglio, Massimo/F-5302-2015; Nicastro, Luciano/F-5866-2015; Tammi, Joni/G-2959-2012; Schovanek, Petr/G-7117-2014; Travnicek, Petr/G-8814-2014; Braun, Isabel/C-9373-2012; Ridky, Jan/H-6184-2014; Chudoba, Jiri/G-7737-2014; Reimer, Olaf/A-3117-2013; Pech, Miroslav/G-5760-2014; Rico, Javier/K-8004-2014; Martinez Botella, Gustavo/K-8834-2014; Fernandez, Ester/K-9734-2014; GAug, Markus/L-2340-2014; Font, Lluis/L-4197-2014; OI Bastieri, Denis/0000-0002-6954-8862; Martinez Rodriguez, Manel/0000-0002-9763-9155; Tiengo, Andrea/0000-0002-6038-1090; Ribo, Marc/0000-0002-9931-4557; MEREGHETTI, SANDRO/0000-0003-3259-7801; Uslenghi, Michela/0000-0002-7585-8605; Punch, Michael/0000-0002-4710-2165; Tavani, Marco/0000-0003-2893-1459; Garrido Beltran, Lluis/0000-0001-8883-6539; Gianotti, Fulvio/0000-0003-4666-119X; Di Pierro, Federico/0000-0003-4861-432X; Gardiol, Daniele/0000-0001-8213-3525; Rando, Riccardo/0000-0001-6992-818X; Vallania, Piero/0000-0001-9089-7875; Balis, Dimitris/0000-0003-1161-7746; Persic, Massimo/0000-0003-1853-4900; Marisaldi, Martino/0000-0002-4000-3789; Luque-Escamilla, Pedro Luis/0000-0002-3306-9456; Huovelin, Juhani/0000-0002-6276-5776; Della Volpe, Domenico/0000-0001-8530-7447; Daniel, Michael/0000-0002-8053-7910; Cusumano, Giancarlo/0000-0002-8151-1990; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Knapp, Johannes/0000-0003-1519-1383; Preece, Robert/0000-0003-1626-7335; Caraveo, Patrizia/0000-0003-2478-8018; Sottile, Giuseppe/0000-0003-3101-3966; Komin, Nukri/0000-0003-3280-0582; Bigongiari, Ciro/0000-0003-3293-8522; De Lotto, Barbara/0000-0003-3624-4480; Fornasa, Mattia/0000-0002-2692-117X; De Angelis, Alessandro/0000-0002-3288-2517; La Rosa, Giovanni/0000-0002-3931-2269; Asorey, Hernan/0000-0002-4559-8785; Bonanno, Giovanni/0000-0002-4792-3983; LA BARBERA, ANTONINO/0000-0002-5880-8913; Bandiera, Rino/0000-0002-7099-2151; La Parola, Valentina/0000-0002-8087-6488; Sidoli, Lara/0000-0001-9705-2883; GIARRUSSO, SALVATORE/0000-0002-0738-2940; Chadwick, Paula/0000-0002-1468-2685; Molinari, Emilio/0000-0002-1742-7735; giommi, paolo/0000-0002-2265-5003; Di Paola, Andrea/0000-0002-2189-8644; Catalano, Osvaldo/0000-0002-9554-4128; Segreto, Alberto/0000-0001-7341-6603; Chiappetti, Lucio/0000-0001-7857-7908; Fiorini, Mauro/0000-0001-8297-1983; Maccarone, Maria Concetta/0000-0001-8722-0361; Kothandan, Divay/0000-0001-9048-7518; Smareglia, Riccardo/0000-0001-9363-3007; Stringhetti, Luca/0000-0002-3961-9068; Malaguti, Giuseppe/0000-0001-9872-3378; Vercellone, Stefano/0000-0003-1163-1396; Mertsch, Philipp/0000-0002-2197-3421; Arnaldi, Luis Horacio/0000-0002-2370-4014; Paizis, Adamantia/0000-0001-5067-0377; Molinaro, Marco/0000-0001-5028-6041; Bulgarelli, Andrea/0000-0001-6347-0649; Billotta, Sergio/0000-0001-6557-8768; Knapic, Cristina/0000-0002-4752-6777; Spiga, Daniele/0000-0003-1163-7843; Fantinel, Daniela/0000-0001-8152-9480; Mineo, Teresa/0000-0002-4931-8445; Vuerli, Claudio/0000-0002-9640-8785; Pareschi, Giovanni/0000-0003-3967-403X; Torres, Diego/0000-0002-1522-9065; Drury, Luke/0000-0002-9257-2270; Barrio, Juan/0000-0002-0965-0259; Murase, Kohta/0000-0002-5358-5642; Moulin, Emmanuel/0000-0003-4007-0145; Cortina, Juan/0000-0003-4576-0452; Graciani Diaz, Ricardo/0000-0001-7166-5198; Nosek, Dalibor/0000-0001-6219-200X; Yebras, Jose Manuel/0000-0002-6861-8363; Gascon, David/0000-0001-9607-6154; Poutanen, Juri/0000-0002-0983-0049; Sarkar, Subir/0000-0002-3542-858X; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908; de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752; Moura Santos, Edivaldo/0000-0002-2818-8813; Bissaldi, Elisabetta/0000-0001-9935-8106; Temnikov, Petar/0000-0002-9559-3384; Casanova, Sabrina/0000-0002-6144-9122; Aguilar Sanchez, Juan Antonio/0000-0003-2252-9514; Antoranz, Pedro/0000-0002-3015-3601; Miranda, Jose Miguel/0000-0002-1472-9690; Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755; Conforti, Vito/0000-0002-0007-3520; Blasi, Pasquale/0000-0003-2480-599X; Amato, Elena/0000-0002-9881-8112; de Mello Neto, Joao/0000-0002-3234-6634; Stamatescu, Victor/0000-0001-9030-7513; Bais, Alkiviadis/0000-0003-3899-2001; Babic, Ana/0000-0001-9549-9710; Todero Peixoto, Carlos Jose/0000-0003-3669-8212; Prouza, Michael/0000-0002-3238-9597; Ebr, Jan/0000-0001-8807-6162; van Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418; Murphy, Alexander/0000-0001-8337-4427; Doro, Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507; Bordas, Pol/0000-0002-0266-8536; Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324; de Ona Wilhelmi, Emma/0000-0002-5401-0744; Lucarelli, Fabrizio/0000-0002-6311-764X; Tejedor, Luis/0000-0003-1525-9085; Berdugo, Javier/0000-0002-7911-8532; Kokkotas, Kostas/0000-0001-6048-2919; Funk, Stefan/0000-0002-2012-0080; Terada, Yukikatsu/0000-0002-2359-1857; Trifoglio, Massimo/0000-0002-2505-3630; Nicastro, Luciano/0000-0001-8534-6788; Tammi, Joni/0000-0002-9164-2695; Braun, Isabel/0000-0002-9389-0502; Ridky, Jan/0000-0001-6697-1393; Reimer, Olaf/0000-0001-6953-1385; Rico, Javier/0000-0003-4137-1134; Martinez Botella, Gustavo/0000-0002-1061-8520; GAug, Markus/0000-0001-8442-7877; Font, Lluis/0000-0003-2109-5961; Tagliaferri, Gianpiero/0000-0003-0121-0723; Garcia, Beatriz/0000-0003-0919-2734; Testa, Vincenzo/0000-0003-1033-1340; Hardcastle, Martin/0000-0003-4223-1117; Canestrari, Rodolfo/0000-0003-4591-7763; Lenain, Jean-Philippe/0000-0001-7284-9220; Bonnoli, Giacomo/0000-0003-2464-9077; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Golev, Valeri/0000-0002-4482-4090; La Palombara, Nicola/0000-0001-7015-6359; Inoue, Yoshiyuki/0000-0002-7272-1136; Gamez Garcia, Javier/0000-0001-9812-0139; Grandi, Paola/0000-0003-1848-6013; Ghigo, Mauro/0000-0003-2284-9251; Otte, Adam Nepomuk/0000-0002-5955-6383; silk, joe/0000-0002-1566-8148; De Luca, Andrea/0000-0001-6739-687X NR 25 TC 192 Z9 195 U1 17 U2 194 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD MAR PY 2013 VL 43 SI SI BP 3 EP 18 DI 10.1016/j.astropartphys.2013.01.007 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 133GL UT WOS:000318126800002 ER PT J AU Sol, H Zech, A Boisson, C de Almeida, UB Biteau, J Contreras, JL Giebels, B Hassan, T Inoue, Y Katarzynski, K Krawczynski, H Mirabal, N Poutanen, J Rieger, F Totani, T Benbow, W Cerruti, M Errando, M Fallon, L Dal Pino, ED Hinton, JA Inoue, S Lenain, JP Neronov, A Takahashi, K Takami, H White, R AF Sol, H. Zech, A. Boisson, C. de Almeida, U. Barres Biteau, J. Contreras, J. -L. Giebels, B. Hassan, T. Inoue, Y. Katarzynski, K. Krawczynski, H. Mirabal, N. Poutanen, J. Rieger, F. Totani, T. Benbow, W. Cerruti, M. Errando, M. Fallon, L. de Gouveia Dal Pino, E. Hinton, J. A. Inoue, S. Lenain, J. -P. Neronov, A. Takahashi, K. Takami, H. White, R. CA CTA Consortium TI Active Galactic Nuclei under the scrutiny of CTA SO ASTROPARTICLE PHYSICS LA English DT Article DE High energy astrophysics; Gamma-rays; Cherenkov astronomy; Active Galactic Nuclei ID GAMMA-RAY EMISSION; EXTRAGALACTIC MAGNETIC-FIELDS; ENERGY COSMIC-RAYS; SPACE-TELESCOPE OBSERVATIONS; SUPERMASSIVE BLACK-HOLE; REMNANT RX J1713.7-3946; KILOPARSEC-SCALE JETS; BL LACERTAE OBJECTS; LINE SEYFERT 1; PARTICLE-ACCELERATION AB Active Galactic Nuclei (hereafter AGN) produce powerful outflows which offer excellent conditions for efficient particle acceleration in internal and external shocks, turbulence, and magnetic reconnection events. The jets as well as particle accelerating regions close to the supermassive black holes (hereafter SMBH) at the intersection of plasma inflows and outflows, can produce readily detectable very high energy gamma-ray emission. As of now, more than 45 AGN including 41 blazars and 4 radiogalaxies have been detected by the present ground-based gamma-ray telescopes, which represents more than one third of the cosmic sources detected so far in the VHE gamma-ray regime. The future Cherenkov Telescope Array (CTA) should boost the sample of AGN detected in the VHE range by about one order of magnitude, shedding new light on AGN population studies, and AGN classification and unification schemes. CTA will be a unique tool to scrutinize the extreme high-energy tail of accelerated particles in SMBH environments, to revisit the central engines and their associated relativistic jets, and to study the particle acceleration and emission mechanisms, particularly exploring the missing link between accretion physics, SMBH magnetospheres and jet formation. Monitoring of distant AGN will be an extremely rewarding observing program which will inform us about the inner workings and evolution of AGN. Furthermore these AGN are bright beacons of gamma-rays which will allow us to constrain the extragalactic infrared and optical backgrounds as well as the intergalactic magnetic field, and will enable tests of quantum gravity and other "exotic" phenomena. (C) 201 Published by Elsevier B.V. C1 [Sol, H.; Zech, A.; Boisson, C.; Cerruti, M.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France. [de Almeida, U. Barres] Max Planck Inst Phys & Astrophys, D-80801 Munich, Germany. [Biteau, J.; Giebels, B.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Contreras, J. -L.; Hassan, T.; Mirabal, N.] Univ Complutense Madrid, Dpto Fis Atom Mol & Nucl, E-28040 Madrid, Spain. [Inoue, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Inoue, Y.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Katarzynski, K.] Nicolaus Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Krawczynski, H.] McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Poutanen, J.] Univ Oulu, Astron Div, Dept Phys, FI-90014 Oulu, Finland. [Rieger, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Rieger, F.] European Associated Lab Gamma Ray Astron, Paris, France. [Rieger, F.] European Associated Lab Gamma Ray Astron, Heidelberg, Germany. [Totani, T.] Kyoto Univ, Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Benbow, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Errando, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Fallon, L.] Dublin Inst Adv Studies, Dublin 2, Ireland. [de Gouveia Dal Pino, E.] Univ Sao Paulo, Inst Astron Geofis Ciencias & Atmosfer, BR-05508090 Sao Paulo, Brazil. [Hinton, J. A.; White, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Inoue, S.; Takahashi, K.] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan. [Lenain, J. -P.] Heidelberg Univ, Landessternwarte, Konigstuhl, D-69117 Heidelberg, Germany. [Neronov, A.] Observ Geneva, ISDC Data Ctr Astrophys, CH-1290 Versoix, Switzerland. [Takami, H.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. RP Sol, H (reprint author), Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France. EM helene.sol@obspm.fr RI 7, INCT/H-6207-2013; Astrofisica, Inct/H-9455-2013; Katarzynski, Krzysztof/G-4528-2014; Poutanen, Juri/H-6651-2016; Takahashi, Keitaro/L-5930-2015; Contreras Gonzalez, Jose Luis/K-7255-2014; de Gouveia Dal Pino, Elisabete/H-9560-2013; OI Poutanen, Juri/0000-0002-0983-0049; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752; Inoue, Yoshiyuki/0000-0002-7272-1136; Errando, Manel/0000-0002-1853-863X; Lenain, Jean-Philippe/0000-0001-7284-9220 FU CNRS; Paris Observatory through the LEA ELGA; Spanish MICINN [FPA2010-22056-C06-06] FX The authors thank the CTA collaboration and many scientists for discussion and comments on the paper, with special thanks to C. Dermer, T. Kneiske, E. Lindfors and the CTA internal referees M. Persic and G. Romero. The authors acknowledge the support of the CNRS and of the visitor programme of the Paris Observatory through the LEA ELGA. They thank M. Daniel, D. Emmanoulopoulos, and B. Thiam for their help. N.M. gratefully acknowledges support from the Spanish MICINN through a Ramon y Cajal fellowship under project code FPA2010-22056-C06-06. NR 235 TC 29 Z9 29 U1 0 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0927-6505 EI 1873-2852 J9 ASTROPART PHYS JI Astropart Phys. PD MAR PY 2013 VL 43 SI SI BP 215 EP 240 DI 10.1016/j.astropartphys.2012.12.005 PG 26 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 133GL UT WOS:000318126800017 ER PT J AU Walter, MJ Cottrell, E AF Walter, Michael J. Cottrell, Elizabeth TI Assessing uncertainty in geochemical models for core formation in Earth SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE siderophile elements; regression models; core formation; model uncertainty ID SILICATE PARTITION-COEFFICIENTS; DEEP MAGMA-OCEAN; SIDEROPHILE ELEMENTS; HIGH-PRESSURE; OXIDATION-STATE; OXYGEN FUGACITY; TEMPERATURE; ACCRETION; CONSTRAINTS; MANTLE AB Unraveling the conditions at which Earth's metallic iron core formed yields important information about Earth's early accretion and differentiation history. Multi-variable statistical modeling of siderophile element partitioning between core-forming metallic liquids and silicate melts form the basis for physical models of core formation. While it seems clear that core segregation in a deep peridotitic magma ocean is generally consistent with many mantle siderophile element abundances, there is considerable disparity among extant physical models in terms of the key parameters of pressure, temperature and oxygen fugacity at which the core formed. Moreover, there is ongoing debate over whether simple single-stage equilibrium or more complex multi-stage accretion models are required by the partitioning data. Here we consider how variations in the statistical regression of partitioning data affect the outcomes of physical models for core formation. Taking extant experimental data sets for four well-studied siderophile elements (Ni, Co, W and V) as examples, we find that the regression model exerts a fundamental control on physical model outcomes. Further, the experimental data are currently too imprecise to discriminate among various single-stage and continuous core formation scenarios. Progress in the development of physical models requires better isolation of the independent variables that affect partition coefficients and verification of activity models at high pressure and temperature in order to reduce the global uncertainty in multi-variable statistical models. (C) 2013 Elsevier B.V. All rights reserved. C1 [Walter, Michael J.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. [Cottrell, Elizabeth] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Walter, MJ (reprint author), Univ Bristol, Dept Earth Sci, Queens Rd, Bristol BS8 1RJ, Avon, England. EM mj.walter@bristol.ac.uk FU NSF [EAR-0738654]; NERC [NE/f019084/1] FX We thank Prof. Bernie Wood for supplying computer code for activity corrections. Nancy Chabot and an anonymous reviewer are thanked for their constructive comments. This work was supported by NSF grant EAR-0738654 to EC, and NERC grant NE/f019084/1to MJW. NR 59 TC 12 Z9 12 U1 1 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAR 1 PY 2013 VL 365 BP 165 EP 176 DI 10.1016/j.epsl.2013.01.014 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 133HR UT WOS:000318130000016 ER PT J AU Deutsch, JI AF Deutsch, James I. TI A Little Solitaire: John Frankenheimer and American film SO HISTORICAL JOURNAL OF FILM RADIO AND TELEVISION LA English DT Book Review C1 [Deutsch, James I.] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0143-9685 J9 HIST J FILM RADIO TV JI Hist. J. Film Radio Telev. PD MAR 1 PY 2013 VL 33 IS 1 BP 132 EP 134 DI 10.1080/01439685.2013.765097 PG 3 WC Film, Radio, Television SC Film, Radio & Television GA 122TY UT WOS:000317342200009 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI Enigmatic teeth of small theropod dinosaurs from the Upper Cretaceous (Cenomanian-Turonian) of Uzbekistan SO CANADIAN JOURNAL OF EARTH SCIENCES LA English DT Article ID DIVERSITY; ALBERTA; BIRDS AB Upper Cretaceous (Cenomanian-Turonian) formations in the Kyzylkum Desert of Uzbekistan, especially the Bissekty Formation at Dzharakuduk, have yielded a great diversity of continental vertebrates, including dinosaurs. Underwater screening of the sandy matrix has recovered many dinosaurian teeth. Here we describe and illustrate two types of enigmatic theropod teeth that are referable to Paronychodon and Richardoestesia, respectively. Both of these tooth taxa are well known from the Late Cretaceous of North America and possibly represent stages in the development of the teeth of various paravian theropods. Confirmation of this hypothesis awaits discovery of more complete jaws. C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Averianov, Alexander] Russian Acad Sci, Museum Zool, St Petersburg 199034, Russia. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Civilian Research & Development Foundation [RU-G1-2571-ST-04, RUB1-2860-ST-07]; Russian Fund of Basic Research [07-04-91110-AFGIRa, 04-04-49113, 04-04-49637, 07-04-00393, 10-04-01350]; President's of Russia grant [MD 255.2003.04]; Saint Petersburg State University FX We take great pleasure in offering this paper to Richard C. Fox on the occasion of his 80th birthday. The honoree has made many important contributions to vertebrate paleontology. He also first introduced Sues to the study of Cretaceous microvertebrate assemblages. The cooperation of the Zoological Institute of the National Academy of Sciences of Uzbekistan, especially D.A. Azimov and Y.A. Chikin, facilitated the fieldwork of the Uzbek-Russian-British-American-Canadian (URBAC) expeditions to the Kyzylkum Desert. We owe a great debt of gratitude to our fellow expedition members A.V. Abramov, J.D. Archibald, G.O. Cherepanov, I.G. Danilov, S. Dominguez, C. King, N. Morris, C.M. Redman, A.S. Resvyi, C. Skrabec, P.P. Skutschas, E.V. Syromyatnikova, and D.J. Ward for their efforts in the field, scientific expertise, and camaraderie. We thank J.D. Gardner and C.S. Scott for organizing this Festschrift and for inviting us to contribute to it. P.J. Currie, J.D. Gardner, and D.W. Larson provided constructive reviews of the manuscript. For financial support we are indebted to the National Science Foundation (EAR-9804771 and EAR-0207004 to J.D. Archibald and H.-D. Sues), the National Geographic Society (5901-97 and 6281-98 to J.D. Archibald and H.-D. Sues), the Civilian Research & Development Foundation (RU-G1-2571-ST-04 and RUB1-2860-ST-07), and the Russian Fund of Basic Research (07-04-91110-AFGIRa). Averianov also acknowledges research support from the President's of Russia grant MD 255.2003.04, the Russian Fund of Basic Research grants 04-04-49113, 04-04-49637, 07-04-00393, and 10-04-01350, and from a Paleontological Museum grant of Saint Petersburg State University. NR 58 TC 9 Z9 9 U1 0 U2 8 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4077 J9 CAN J EARTH SCI JI Can. J. Earth Sci. PD MAR PY 2013 VL 50 IS 3 SI SI BP 306 EP 314 DI 10.1139/e2012-033 PG 9 WC Geosciences, Multidisciplinary SC Geology GA 129JG UT WOS:000317834700009 ER PT J AU Pukazhenthi, B Quse, V Hoyer, M Gastelaars, HV Sanjur, O Brown, JL AF Pukazhenthi, Budhan Quse, Viviana Hoyer, Mark Gastelaars, Heleen van Engeldorp Sanjur, Oris Brown, Janine L. TI A review of the reproductive biology and breeding management of tapirs SO INTEGRATIVE ZOOLOGY LA English DT Review DE estrous cycle; hormones; reproduction; spermatozoa; tapir ID RHINOCEROS DICERORHINUS-SUMATRENSIS; CERATOTHERIUM-SIMUM-SIMUM; FECAL STEROID ANALYSIS; BAIRDS TAPIR; PREGNANCY DIAGNOSIS; DICEROS-BICORNIS; WHITE RHINOCEROS; ESTROUS-CYCLE; COSTA-RICA; CHORIONIC-GONADOTROPIN AB Tapirs (Tapirus sp.) have been studied extensively in the wild, yet little is known about their fundamental reproductive biology, information that is critical to establishing self-sustaining populations in captivity as a hedge against extinction. This paper reviews information on the reproductive biology of the 4 species of tapirs: Baird's (Tapirus bairdii), lowland (T terrestris), mountain (T pinchaque) and Malayan (T indicus). Both sexes reach puberty between 14 and 48 months of age. Behaviorally, tapirs display few overt signs of estrus, and external signs of pregnancy are not evident until approximately 2 months before parturition. Immunoassay techniques to measure reproductive hormones in blood and urine have been validated for tapirs, which allow monitoring of ovarian cycle activity and pregnancy. Data indicate that females are polyestrous, with an estrous cycle length of approximately 30 days. The exception is the Malayan tapir, which exhibits 2 types of cycles: short (approximately 1 month) and long (approximately 2 months). Gestation length is approximately 13 months and females can conceive at the first post-partum cycle within 1 month after birth. Good quality ejaculates have been obtained via electroejaculation in the Baird's and Malayan tapir and the sperm from Baird's tapir cryopreserved using standard cryodiluents, although more work is needed to optimize these protocols. Given that all 4 species of tapir most likely will continue to be maintained in captivity, effective genetic management is vital for long-term survival. Optimization of assisted reproductive technologies, including sperm cryopreservation and artificial insemination, could benefit the genetic management of tapirs. C1 [Pukazhenthi, Budhan; Brown, Janine L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Hoyer, Mark; Gastelaars, Heleen van Engeldorp] Artis Royal Zoo, Vet Dept, Amsterdam, Netherlands. [Gastelaars, Heleen van Engeldorp] Leiden Univ, Med Ctr, Dept Mol Cell Biol, Lab Neurophysiol, Leiden, Netherlands. [Sanjur, Oris] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Pukazhenthi, B (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu NR 71 TC 4 Z9 4 U1 5 U2 76 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1749-4877 J9 INTEGR ZOOL JI Integr. Zool. PD MAR PY 2013 VL 8 IS 1 BP 18 EP 34 DI 10.1111/j.1749-4877.2012.12008.x PG 17 WC Zoology SC Zoology GA 129RW UT WOS:000317860600003 PM 23586557 ER PT J AU Capece, PI Aliaga-Rossel, E Jansen, PA AF Capece, Paula I. Aliaga-Rossel, Enzo Jansen, Patrick A. TI Viability of small seeds found in feces of the Central American tapir on Barro Colorado Island, Panama SO INTEGRATIVE ZOOLOGY LA English DT Article DE Central America; megafauna; seed dispersal; seed size; tapir ID BAIRDS TAPIR; FRENCH-GUIANA; RAIN-FOREST; HABITAT USE; COSTA-RICA; DISPERSAL; DIET; ECOLOGY; BRAZIL; CONSERVATION AB Tapirs are known as effective dispersers of large-seeded tree species, but their role in dispersing small-seeded plant species has yet to be established. Tapir feces have been reported to contain large numbers of small seeds, but whether these are viable has rarely been evaluated. We determined the abundance and viability of small seeds in feces of Central American tapir (Tapirus bairdii) on Barro Colorado Island, Panama. A total of 72 fecal samples were collected opportunistically from 4 tapir latrine sites. Seeds were manually extracted from feces and classified by size. Seed viability was estimated by opening each seed and examining for the presence of at least 1 intact firm white endosperm. In total, we obtained 8166 seeds of at least 16 plant species. Small-seeded species dominated, with 96% of all seeds found measuring <5 mm. The canopy tree Laetia procera was the most abundant species in the samples. Of all small seeds found, 69% contained an intact endosperm and appeared viable. This suggests that small seeds, like large seeds, often pass through the digestive tract of T. bairdii intact. Thus, tapirs potentially serve as effective dispersers of a wide range of small-seeded plant species. C1 [Capece, Paula I.; Aliaga-Rossel, Enzo] Univ Hawaii Manoa, Ecol Evolut & Conservat Biol Program, Honolulu, HI 96822 USA. [Aliaga-Rossel, Enzo] Higher Univ San Andres, Inst Ecol, La Paz, Bolivia. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Panama City, Panama. [Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, NL-6700 AP Wageningen, Netherlands. RP Capece, PI (reprint author), Natl Pk Serv, 1978 Isl Ford Pkwy, Sandy Springs, GA 30350 USA. EM paula_capece@nps.gov RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU Netherlands Foundation for Scientific Research FX We thank the Smithsonian Tropical Research Institute for hosting this study; Jim Dalling for use of his laboratory; Osvaldo Calderon and Andres Hernandez for seed identification; Eloisa Lasso De Paulis for assistance in the field; Ricardo Moreno for assistance in the field and help with herbarium seed comparison; Jose M. V. Fragoso and Andrew Taylor for advice; Joe Wright for seed mass data; Roland Kays for current BCI tapir population information; and Jose M. V. Fragoso, Aaron Shiels, Laura Capece, Michael Szperka for comments on previous versions of the manuscript. Patrick A. Jansen acknowledges financial support from the Netherlands Foundation for Scientific Research. NR 47 TC 11 Z9 11 U1 3 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1749-4877 J9 INTEGR ZOOL JI Integr. Zool. PD MAR PY 2013 VL 8 IS 1 BP 57 EP 62 DI 10.1111/j.1749-4877.2012.00313.x PG 6 WC Zoology SC Zoology GA 129RW UT WOS:000317860600006 PM 23586560 ER PT J AU Jones, MM Ferrier, S Condit, R Manion, G Aguilar, S Perez, R AF Jones, Mirkka M. Ferrier, Simon Condit, Richard Manion, Glenn Aguilar, Salomon Perez, Rolando TI Strong congruence in tree and fern community turnover in response to soils and climate in central Panama SO JOURNAL OF ECOLOGY LA English DT Article DE biotic interactions; determinants of plant community diversity and structure; edaphic variation; environmental control; matrix regression; precipitation; Pteridophyta; seed and spore dispersal; tropical forests; turnover rates ID AMAZONIAN RAIN-FORESTS; BETA-DIVERSITY; FLORISTIC PATTERNS; COLOMBIAN AMAZONIA; NEOTROPICAL FOREST; VASCULAR PLANTS; BIODIVERSITY; MELASTOMATACEAE; PTERIDOPHYTES; DISTRIBUTIONS AB 1. Plant species turnover in central Panamanian forests has been principally attributed to the effects of dispersal limitation and a strong Caribbean to Pacific gradient in rainfall seasonality. Despite marked geological heterogeneity, the role of soil variation has not been rigorously examined. 2. We modelled the compositional turnover of trees and ferns in the Panama Canal watershed as a function of soil chemistry, climate and geographical separation, using generalized dissimilarity models (GDMs). 3. Predictability in both plant groups was strong, with 74% of turnover explained in trees and 49% in ferns. Major trends in the two plant groups were strikingly similar. The independent effects of soils, and of climate for trees, were sizeable, but those of geographical distance were minor. In both plant groups, distance and climatic effects on species turnover covaried strongly. 4. Including floristic dissimilarity of the other taxon as a predictor increased explained deviance to 81% in trees and 59% in ferns. Controlling for differences in plant density among plots reduced deviance explained by climate and distance, while soil effects remained strong. Limiting the analyses to soils of volcanic origin increased deviance explained by climate, soils and distance, but their effects covaried strongly. Independent soil effects on tree turnover were reduced, but their effects on fern turnover remained pronounced. 5. Dry season length was the most important climatic predictor for both taxa, and P and pH were the most important soil predictors. Particularly, rapid species turnover was associated with the driest end of the seasonality gradient, linked to declining individual densities and species richness, and with the low end of the phosphorus gradient. 6. Synthesis. While changes in rainfall and seasonality undoubtedly limit plant distributions in this region, soil effects are at least as important, and interactions between the two are sizeable. This is likely to hold elsewhere in the Caribbean region, where mosaics of marine and volcanic soils combined with pronounced rainfall gradients are common. Strong congruence between our focal taxa suggests that our results can be extrapolated to other plant groups, particularly as trees and ferns are distantly related and represent different life-forms. C1 [Jones, Mirkka M.] Aarhus Univ, Dept Biosci, Ecoinformat & Biodivers Grp, DK-8000 Aarhus C, Denmark. [Ferrier, Simon] CSIRO Ecosyst Sci, Black Mt Labs, Canberra, ACT 2601, Australia. [Condit, Richard; Aguilar, Salomon; Perez, Rolando] Smithsonian Trop Res Inst, Panama City, Panama. [Manion, Glenn] Dept Premier & Cabinet, Off Environm & Heritage, Sci Serv Div, Landscape Modelling & Decis Support Unit, Armidale, NSW 2350, Australia. RP Jones, MM (reprint author), Aarhus Univ, Dept Biosci, Ecoinformat & Biodivers Grp, DK-8000 Aarhus C, Denmark. EM mjones@biology.au.dk RI Ferrier, Simon/C-1490-2009 OI Ferrier, Simon/0000-0001-7884-2388 FU NSF [DEB021104, 021115, 0212284, 0212818]; OISE [0314581]; U.S. National Science Foundation [0948585]; Smithsonian Tropical Research Institute's Center for Tropical Forest Science and Global Earth Observatory; Smithsonian Scholarly Studies program, the U.S. Agency for International Development; Academy of Finland; Jenny and Antti Wihuri foundation; Oskar Oflunds Stiftelse FX Many thanks to staff at STRI in Panama for logistic support, to B. Turner and others at the STRI soil laboratory for running the soil analyses and to N. Guerrero, N. Mandl, D. Mitre, C. Orduna, A. Ortega and M. Quinones for able field and laboratory assistance. B. Engelbrecht and J. Wright kindly provided tree data for plots at Albrook, Sherman and Gigante and H. Tuomisto provided fern data for the BCI 50-ha plot, and also programmed the individual-based rarefaction. J. Dalling provided feedback on using the BCI 50-hectare plot soil data, which was collected under the STRI Soils Initiative and CTFS, funded by NSF grants DEB021104,021115, 0212284,0212818 and OISE grant 0314581, with the assistance of P. Segre and J. Di Trani. Tree plot censuses were funded by numerous U.S. National Science Foundation grants, most recently grant 0948585; the Smithsonian Tropical Research Institute's Center for Tropical Forest Science and Global Earth Observatory; the Smithsonian Scholarly Studies program, the U.S. Agency for International Development, and several private foundations. M. Jones was funded for this work by the Academy of Finland, the Jenny and Antti Wihuri foundation and Oskar Oflunds Stiftelse. Research permits were granted by the Autoridad Nacional del Ambiente (ANAM), Panama. K. Mokany, B. Sandel, J.-C. Svenning, G. Zuquim and an anonymous referee are acknowledged for their thoughtful comments on the manuscript. NR 45 TC 21 Z9 23 U1 3 U2 54 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD MAR PY 2013 VL 101 IS 2 BP 506 EP 516 DI 10.1111/1365-2745.12053 PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 130MX UT WOS:000317923300024 ER PT J AU Bornholdt, R Helgen, K Koepfli, KP Oliveira, L Lucherini, M Eizirik, E AF Bornholdt, Renata Helgen, Kristofer Koepfli, Klaus-Peter Oliveira, Larissa Lucherini, Mauro Eizirik, Eduardo TI Taxonomic revision of the genus Galictis (Carnivora: Mustelidae): species delimitation, morphological diagnosis, and refined mapping of geographical distribution SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE America; greater grison; lesser grison; morphometrics; Neotropical region; phylogeny; skin variation; skull variation; taxonomy ID CHARACTER DISPLACEMENT; BIOGEOGRAPHIC HISTORY; SEXUAL-DIMORPHISM; AMERICAN MINK; SYSTEMATICS; DIVERSITY; EVOLUTIONARY; PROCYONIDAE; RADIATION; MAMMALS AB Although critical for enabling in-depth evolutionary, ecological, or conservation-orientated studies, taxonomic knowledge is still scarce for many groups of organisms, including mammals of the order Carnivora. For some of these taxa, even basic aspects such as species limits and geographical distribution are still uncertain. This is the case for the Neotropical mustelid genus Galictis, considered one of the least studied carnivoran genera in the Americas. To address this issue, we performed a comprehensive assessment of morphological and molecular characters to test the number of species within Galictis, and to characterize their distinctiveness and evolutionary history. In addition, we reviewed and consolidated the available information on the taxonomy of this genus, so as to provide a historical framework upon which we could interpret our data. Our analyses demonstrated that two Galictis species can be clearly delimited and diagnosed using metric and nonmetric morphological characters as well as DNA sequences from mitochondrial and nuclear gene segments. On the basis of this clarified species-level delimitation, we reassessed the geographical range of each Galictis taxon, identifying possible areas of sympatry between them. These results provide a solid taxonomic framework for Galictis, enabling the development of additional studies focusing on this poorly known taxon. (c) 2013 The Linnean Society of London, Zoological Journal of the Linnean Society, 2013, 167, 449-472. doi: 10.1111/j.1096-3642.2012.00859.x C1 [Bornholdt, Renata; Eizirik, Eduardo] Fac Biociencias PUCRS, BR-90619900 Porto Alegre, RS, Brazil. [Helgen, Kristofer] Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20560 USA. [Koepfli, Klaus-Peter] NIH, Lab Genom Divers, Frederick, MD 21702 USA. [Lucherini, Mauro] Univ Nacl Sur, Dept Biol Bioquim & Farm, Grp Ecol Comportamental Mamiferos, RA-8000 Bahia Blanca, Buenos Aires, Argentina. [Eizirik, Eduardo] Inst Procarnivoros, BR-12945010 Atibaia, SP, Brazil. RP Eizirik, E (reprint author), Fac Biociencias PUCRS, Av Ipiranga,6681 Predio 12, BR-90619900 Porto Alegre, RS, Brazil. EM eduardo.eizirik@pucrs.br RI Eizirik, Eduardo/K-8034-2012 OI Eizirik, Eduardo/0000-0002-9658-0999 FU Pontificia Universidade Catolica do Rio Grande do Sul (PUCRS, Brazil); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil); Fundacao de Amparo a Pesquisa do Estado do Rio Grande do Sul (FAPERGS, Brazil); Smithsonian Institution (USA) FX The authors wish to thank the people in charge of the mammalian collections analysed in this study, who made this research project possible: Carla S. Fontana (MCT-PUCRS), Marcia A. Jardim (FZB/RS), Felipe Peters (ULBRA), Mauricio Graipel (LAMAq-UFSC), Mario de Vivo (MZUSP), Joao A. Oliveira (MNHN), Diego A. de Moraes (UFPE), Joao Alberto de Queiroz (MPEG), Enrique Gonzalez (MNHNA), David Flores (MACN), Hugo Lopez (MLP), Linda Gordon (USNM), Eileen Westwig (AMNH), Ned Gilmore (ANSP), Catherine Weisel (MCZ), Bill Stanley and Tracy Damitz (FMNH), Kristof Zyskowski (YPM), Robert Timm (NHMKU), Chris Conroy (MVZ), Mark Hafner (LSUMNS), Louise Tomsett and Paula Jenkins (BMNH), and Clara Stefen (SMT). We also gratefully acknowledge Cladinara Sarturi and Priscilla Mena Zamberlan (PUCRS, Brazil), as well as Jessica Tomlin and Hannah Zinnert (both supported through the Werner H. Kirsten Student Intern Program at the NCI, Frederick, Maryland, USA) for excellent laboratory assistance. We also thank all members from the Grupo de Ecologia Comportamental de Mamiferos (GECM) who participated in sample collection in Argentina, especially Estela Luengos Vidal, Diego Castillo, Claudia Manfredi, and Emma B. Casanave. Finally, we are especially grateful to Cristine S. Trinca, Andrea T. Thomaz, Joao Feliz, Henrique V. Figueiro, Lucas G. da Silva, and Tiago F. da Silva for support at various stages of this research. This project was supported by the Pontificia Universidade Catolica do Rio Grande do Sul (PUCRS, Brazil), Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil), Fundacao de Amparo a Pesquisa do Estado do Rio Grande do Sul (FAPERGS, Brazil), and the Smithsonian Institution (USA). NR 101 TC 7 Z9 12 U1 2 U2 39 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAR PY 2013 VL 167 IS 3 BP 449 EP 472 DI 10.1111/j.1096-3642.2012.00859.x PG 24 WC Zoology SC Zoology GA 114NX UT WOS:000316749600005 ER PT J AU Young, HS McCauley, DJ Dunbar, RB Hutson, MS Ter-Kuile, M Dirzo, R AF Young, Hillary S. McCauley, Douglas J. Dunbar, Robert B. Hutson, Michael S. Ter-Kuile, Miller Dirzo, Rodolfo TI The roles of productivity and ecosystem size in determining food chain length in tropical terrestrial ecosystems SO ECOLOGY LA English DT Article DE ecosystem size; food chain length; food web structure; islands; Palmyra Atoll; productivity ID WEB STRUCTURE; BODY-SIZE; SPECIES RICHNESS; REAL DIFFERENCES; DISTURBANCE; STREAMS; PREDATORS; COMMUNITIES; STRENGTH; ECOLOGY AB Many different drivers, including productivity, ecosystem size, and disturbance, have been considered to explain natural variation in the length of food chains. Much remains unknown about the role of these various drivers in determining food chain length, and particularly about the mechanisms by which they may operate in terrestrial ecosystems, which have quite different ecological constraints than aquatic environments, where most food chain length studies have been thus far conducted. In this study, we tested the relative importance of ecosystem size and productivity in influencing food chain length in a terrestrial setting. We determined that (1) there is no effect of ecosystem size or productive space on food chain length; (2) rather, food chain length increases strongly and linearly with productivity; and (3) the observed changes in food chain length are likely achieved through a combination of changes in predator size, predator behavior, and consumer diversity along gradients in productivity. These results lend new insight into the mechanisms by which productivity can drive changes in food chain length, point to potential for systematic differences in the drivers of food web structure between terrestrial and aquatic systems, and challenge us to consider how ecological context may control the drivers that shape food chain length. C1 [Young, Hillary S.; Hutson, Michael S.; Ter-Kuile, Miller; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.] Smithsonian Inst, Div Vertebrate Zool, Washington, DC 20013 USA. [Young, Hillary S.] Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA. [McCauley, Douglas J.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [McCauley, Douglas J.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 93950 USA. [Dunbar, Robert B.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA. RP Young, HS (reprint author), Harvard Univ, Ctr Environm, 24 Oxford St, Cambridge, MA 02138 USA. EM hyoung@fas.harvard.edu FU National Science Foundation [0639185]; Woods Institute for the Environment; National Geographic Society; Bishop Museum; U.S. Fish and Wildlife Service FX We thank the National Science Foundation (#0639185), the Woods Institute for the Environment, the National Geographic Society, the Bishop Museum, and the U.S. Fish and Wildlife Service for support on this project. We are grateful to P. Vitousek, N. Cormier, D. Croll, R. Fisher, S. Hathaway, C. France, C. Chu, and A. A. Briggs for data, advice, and field assistance. We also thank D. Post, and three anonymous reviewers for their careful reviews of earlier versions of the manuscript, which greatly improved this paper. Vector images are courtesy of Integration and Application Network, University of Maryland Center for Environmental Science (ian.umces.edu/imagelibrary). This is publication number PARC-0092 of the Palmyra Atoll Research Consortium. NR 53 TC 5 Z9 5 U1 1 U2 67 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 2013 VL 94 IS 3 BP 692 EP 701 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 118RU UT WOS:000317044300016 PM 23687895 ER PT J AU Simcoe, RA Burgasser, AJ Schechter, PL Fishner, J Bernstein, RA Bigelow, BC Pipher, JL Forrest, W McMurtry, C Smith, MJ Bochanski, JJ AF Simcoe, Robert A. Burgasser, Adam J. Schechter, Paul L. Fishner, Jason Bernstein, Rebecca A. Bigelow, Bruce C. Pipher, Judith L. Forrest, William McMurtry, Craig Smith, Matthew J. Bochanski, John J. TI FIRE: A Facility Class Near-Infrared Echelle Spectrometer for the Magellan Telescopes SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID OH AIRGLOW; SPECTROGRAPH; SPECTROSCOPY; ABSORPTION; EMISSION; SPECTRA; IMAGER; MMT AB We describe the design, construction, and commissioning of FIRE, a 0.82-2.51 mu m echelle spectrograph for the 6.5 m Magellan Baade telescope. FIRE may be operated in two modes. Its primary mode is a prism cross-dispersed echelle, which delivers R = 6000 spectra for an 0.6. slit, with continuous wavelength coverage over the full instrument bandpass in a single setup. Alternatively, the echelle grating may be replaced with a flat mirror to obtain high-throughput R = 400 longslit spectra through the prisms alone-again with full Y/J/H/K coverage. This contribution outlines the details of the optical design and execution, mechanical and thermal design, detector systems, and data analysis software. We also present performance metrics from commissioning observations. These have established that the instrument is achieving its design goals, particularly with regard to throughput, as is required for observations of faint, high-redshift QSOs and the lowest mass brown dwarfs. C1 [Simcoe, Robert A.; Burgasser, Adam J.; Schechter, Paul L.; Fishner, Jason; Smith, Matthew J.; Bochanski, John J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bernstein, Rebecca A.] UC Santa Cruz Dept Astron Lick Observ, Santa Cruz, CA 95064 USA. [Bigelow, Bruce C.] Santa Cruz Instruments, Santa Cruz, CA USA. [Pipher, Judith L.; Forrest, William; McMurtry, Craig] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Smith, Matthew J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Simcoe, RA (reprint author), MIT, Kavli Inst Astrophys & Space Res, 70 Vassar Street, Cambridge, MA 02139 USA. EM simcoe@space.mit.edu FU NSF MRI program [AST-0649190]; Curtis Marble Instrumentation Development Fund; MIT-Kavli Instrument Development Fund; MIT Department of Physics FX It is a great pleasure to thank the outstanding staff of the Magellan Observatory, in Pasadena, El Pino, and Las Campanas, for their tremendous support. In particular, we thank Frank Perez, Glenn Eyechaner, all of whom endured many hours of teleconferencing and travel. We also thank the members of external review panels who made valuable contributions to FIRE's development. We benefited from useful discussions on visits to the IR labs at the University of Virginia and UCLA. Finally, the FourStar team, especially Eric Persson and Christoph Birk, were extremely generous with their time and resources in helping us develop our instrument and software designs. FIRE's construction was supported by the NSF MRI program, under award number AST-0649190. We gratefully acknowledge additional support from the Curtis Marble Instrumentation Development Fund, MIT-Kavli Instrument Development Fund, and the MIT Department of Physics. NR 37 TC 51 Z9 51 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 2013 VL 125 IS 925 BP 270 EP 286 DI 10.1086/670241 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 119OG UT WOS:000317106500006 ER PT J AU Wagner, S Zotz, G Allen, NS Bader, MY AF Wagner, Sebastian Zotz, Gerhard Salazar Allen, Noris Bader, Maaike Y. TI Altitudinal changes in temperature responses of net photosynthesis and dark respiration in tropical bryophytes SO ANNALS OF BOTANY LA English DT Article DE Altitudinal gradient; bryophytes; carbon balance; dark respiration; gas-exchange measurements; hepatics; liverworts; mosses; net photosynthesis; photosynthesis-response curves; temperature; tropical rain forest ID MONTANE RAIN-FOREST; LICHEN CARBON GAIN; CO2 EXCHANGE; WATER RELATIONS; EPIPHYTIC BRYOPHYTES; PANAMA; PATTERNS; CANOPY; ACCLIMATION; ECOLOGY AB Background and Aims There is a conspicuous increase of poikilohydric organisms (mosses, liverworts and macrolichens) with altitude in the tropics. This study addresses the hypothesis that the lack of bryophytes in the lowlands is due to high-temperature effects on the carbon balance. In particular, it is tested experimentally whether temperature responses of CO2-exchange rates would lead to higher respiratory carbon losses at night, relative to potential daily gains, in lowland compared with lower montane forests. Methods Gas-exchange measurements were used to determine water-, light-, CO2- and temperature-response curves of net photosynthesis and dark respiration of 18 tropical bryophyte species from three altitudes (sea level, 500 m and 1200 m) in Panama. Key Results Optimum temperatures of net photosynthesis were closely related to mean temperatures in the habitats in which the species grew at the different altitudes. The ratio of dark respiration to net photosynthesis at mean ambient night and day temperatures did not, as expected, decrease with altitude. Water-, light- and CO2-responses varied between species but not systematically with altitude. Conclusions Drivers other than temperature-dependent metabolic rates must be more important in explaining the altitudinal gradient in bryophyte abundance. This does not discard near-zero carbon balances as a major problem for lowland species, but the main effect of temperature probably lies in increasing evaporation rates, thus restricting the time available for photosynthetic carbon gain, rather than in increasing nightly respiration rates. Since optimum temperatures for photosynthesis were so fine tuned to habitat temperatures we analysed published temperature responses of bryophyte species worldwide and found the same pattern on the large scale as we found along the tropical mountain slope we studied. C1 [Wagner, Sebastian; Zotz, Gerhard; Bader, Maaike Y.] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, D-26111 Oldenburg, Germany. [Zotz, Gerhard; Salazar Allen, Noris] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wagner, S (reprint author), Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, D-26111 Oldenburg, Germany. EM sebastian.wagner@uni-oldenburg.de RI Bader, Maaike/M-7998-2013 OI Bader, Maaike/0000-0003-4300-7598 FU German Research Foundation-DFG [BA 3843/3-1] FX We thank Lina Ludemann for measuring CO2-response curves, Steve Gonzalez and Carlos Espinosa for field work. Permission to work in Panama was granted by local authorities (ANAM; SC/P-7-11, SEX/P-62-11, SEX/P-7-10). This work was supported by the German Research Foundation-DFG (grant number BA 3843/3-1). NR 41 TC 7 Z9 9 U1 6 U2 71 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD MAR PY 2013 VL 111 IS 3 BP 455 EP 465 DI 10.1093/aob/mcs267 PG 11 WC Plant Sciences SC Plant Sciences GA 113TP UT WOS:000316691800013 PM 23258418 ER PT J AU Rugheimer, S Kaltenegger, L Zsom, A Segura, A Sasselov, D AF Rugheimer, Sarah Kaltenegger, Lisa Zsom, Andras Segura, Antigona Sasselov, Dimitar TI Spectral Fingerprints of Earth-like Planets Around FGK Stars SO ASTROBIOLOGY LA English DT Article DE Habitability; Planetary atmospheres; Extrasolar terrestrial planets; Spectroscopic biosignatures ID WEBB-SPACE-TELESCOPE; HIGH-LEVEL CLOUDS; EXTRASOLAR PLANETS; TERRESTRIAL ATMOSPHERES; FE/H DETERMINATIONS; F-STAR; SEARCH; OZONE; BIOSIGNATURES; GREENHOUSE AB We present model atmospheres for an Earth-like planet orbiting the entire grid of main sequence FGK stars with effective temperatures ranging from T-eff = 4250 K to T-eff = 7000 K in 250 K intervals. We have modeled the remotely detectable spectra of Earth-like planets for clear and cloudy atmospheres at the 1 AU equivalent distance from the VIS to IR (0.4 to 20 mu m) to compare detectability of features in different wavelength ranges in accordance with the James Webb Space Telescope and future design concepts to characterize exo-Earths. We have also explored the effect of the stellar UV levels as well as spectral energy distribution on a terrestrial atmosphere, concentrating on detectable atmospheric features that indicate habitability on Earth, namely, H2O, O-3, CH4, N2O, and CH3Cl. The increase in UV dominates changes of O-3, OH, CH4, N2O, and CH3Cl, whereas the increase in stellar temperature dominates changes in H2O. The overall effect as stellar effective temperatures and corresponding UV increase is a lower surface temperature of the planet due to a bigger part of the stellar flux being reflected at short wavelengths, as well as increased photolysis. Earth-like atmosphere models show more O-3 and OH but less stratospheric CH4, N2O, CH3Cl, and tropospheric H2O (but more stratospheric H2O) with increasing effective temperature of main sequence stars. The corresponding detectable spectral features, on the other hand, show different detectability depending on the wavelength observed. We concentrate on directly imaged planets here as a framework to interpret future light curves, direct imaging, and secondary eclipse measurements of atmospheres of terrestrial planets in the habitable zone at varying orbital positions. C1 [Rugheimer, Sarah; Kaltenegger, Lisa; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaltenegger, Lisa; Zsom, Andras] MPIA, Heidelberg, Germany. [Zsom, Andras] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [Segura, Antigona] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. RP Rugheimer, S (reprint author), Ctr Astrophys, 60 Garden St MS 10, Cambridge, MA 02138 USA. EM srugheimer@cfa.harvard.edu OI Rugheimer, Sarah/0000-0003-1620-7658 FU DFG [ENP Ka 3142/1-1]; NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]; NAI FX The authors would like to acknowledge Tyler Robinson and an anonymous referee for constructive comments and discussions. L.K. acknowledges support from DFG funding ENP Ka 3142/1-1 and NAI. This research has made use of the NASA/IPAC/NExScI Star and Exoplanet Database, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. NR 59 TC 22 Z9 22 U1 1 U2 17 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD MAR PY 2013 VL 13 IS 3 BP 251 EP 269 DI 10.1089/ast.2012.0888 PG 19 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 116CV UT WOS:000316861100003 PM 23537136 ER PT J AU Asgekar, A Oonk, JBR Yatawatta, S van Weeren, RJ McKean, JP White, G Jackson, N Anderson, J Avruch, IM Batejat, F Beck, R Bell, ME Bell, MR van Bemmel, I Bentum, MJ Bernardi, G Best, P Birzan, L Bonafede, A Braun, R Breitling, F van de Brink, RH Broderick, J Brouw, WN Bruggen, M Butcher, HR van Cappellen, W Ciardi, B Conway, JE de Gasperin, F de Geus, E de Jong, A de Vos, M Duscha, S Eisloffel, J Falcke, H Fallows, RA Ferrari, C Frieswijk, W Garrett, MA Griessmeier, JM Grit, T Gunst, AW Hassall, TE Heald, G Hessels, JWT Hoeft, M Iacobelli, M Intema, H Juette, E Karastergiou, A Kohler, J Kondratiev, VI Kuniyoshi, M Kuper, G Law, C van Leeuwen, J Maat, P Macario, G Mann, G Markoff, S McKay-Bukowski, D Mevius, M Miller-Jones, JCA Mol, JD Morganti, R Mulcahy, DD Munk, H Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pizzo, R Polatidis, AG Reich, W Rottgering, H Scheers, B Schoenmakers, A Sluman, J Smirnov, O Sobey, C Steinmetz, M Tagger, M Tang, Y Tasse, C Vermeulen, R Vocks, C Wijers, RAMJ Wise, MW Wucknitz, O Zarka, P AF Asgekar, A. Oonk, J. B. R. Yatawatta, S. van Weeren, R. J. McKean, J. P. White, G. Jackson, N. Anderson, J. Avruch, I. M. Batejat, F. Beck, R. Bell, M. E. Bell, M. R. van Bemmel, I. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bonafede, A. Braun, R. Breitling, F. van de Brink, R. H. Broderick, J. Brouw, W. N. Brueggen, M. Butcher, H. R. van Cappellen, W. Ciardi, B. Conway, J. E. de Gasperin, F. de Geus, E. de Jong, A. de Vos, M. Duscha, S. Eisloeffel, J. Falcke, H. Fallows, R. A. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. -M. Grit, T. Gunst, A. W. Hassall, T. E. Heald, G. Hessels, J. W. T. Hoeft, M. Iacobelli, M. Intema, H. Juette, E. Karastergiou, A. Kohler, J. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. Law, C. van Leeuwen, J. Maat, P. Macario, G. Mann, G. Markoff, S. McKay-Bukowski, D. Mevius, M. Miller-Jones, J. C. A. Mol, J. D. Morganti, R. Mulcahy, D. D. Munk, H. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. Scheers, B. Schoenmakers, A. Sluman, J. Smirnov, O. Sobey, C. Steinmetz, M. Tagger, M. Tang, Y. Tasse, C. Vermeulen, R. Vocks, C. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. Zarka, P. TI LOFAR detections of low-frequency radio recombination lines towards Cassiopeia A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; radio lines: ISM; ISM: individual objects: Cassiopeia A ID CARBON; MHZ; REGIONS AB Cassiopeia A was observed using the low-band antennas of the LOw Frequency ARray (LOFAR) with high spectral resolution. This allowed a search for radio recombination lines (RRLs) along the line-of-sight to this source. Five carbon alpha RRLs were detected in absorption between 40 and 50 MHz with a signal-to-noise ratio of >5 from two independent LOFAR data sets. The derived line velocities (v(LSR) similar to -50 km s(-1)) and integrated optical depths (similar to 13 s(-1)) of the RRLs in our spectra, extracted over the whole supernova remnant, are consistent within each LOFAR data set and with those previously reported. For the first time, we are able to extract spectra against the brightest hotspot of the remnant at frequencies below 330 MHz. These spectra show significantly higher (15-80 percent) integrated optical depths, indicating that there is small-scale angular structure of the order of similar to 1 pc in the absorbing gas distribution over the face of the remnant. We also place an upper limit of 3 x 10(-4) on the peak optical depths of hydrogen and helium RRLs. These results demonstrate that LOFAR has the desired spectral stability and sensitivity to study faint recombination lines in the decameter band. C1 [Asgekar, A.; Oonk, J. B. R.; Yatawatta, S.; van Weeren, R. J.; McKean, J. P.; Avruch, I. M.; van Bemmel, I.; Bentum, M. J.; van de Brink, R. H.; Brouw, W. N.; Butcher, H. R.; van Cappellen, W.; de Geus, E.; de Jong, A.; de Vos, M.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Grit, T.; Gunst, A. W.; Heald, G.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; Mevius, M.; Mol, J. D.; Morganti, R.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Schoenmakers, A.; Sluman, J.; Smirnov, O.; Tang, Y.; Vermeulen, R.; Wise, M. W.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Yatawatta, S.; Avruch, I. M.; Bernardi, G.; Brouw, W. N.; Mevius, M.; Morganti, R.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [van Weeren, R. J.; Birzan, L.; Garrett, M. A.; Iacobelli, M.; Intema, H.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [White, G.; McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [Falcke, H.; Orru, E.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Batejat, F.; Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [Hessels, J. W. T.; Law, C.; van Leeuwen, J.; Markoff, S.; Miller-Jones, J. C. A.; Scheers, B.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Smirnov, O.] Rhodes Univ, Ctr Radio Astron Tech & Technol RATT, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-3584 CA Utrecht, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Bell, M. E.; Broderick, J.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Scheers, B.] Ctr Wiskunde & Informat, NL-1090 GB Amsterdam, Netherlands. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange,UMR7293, F-06300 Nice, France. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, CNRS, UMR 8109, F-92195 Meudon, France. [Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands. [Griessmeier, J. -M.; Tagger, M.] CNRS, LPC2E, UMR 7328, F-45071 Orleans 02, France. [Law, C.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA USA. [Jackson, N.; Hassall, T. E.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Intema, H.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Anderson, J.; Beck, R.; Kohler, J.; Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Sobey, C.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Bell, M. E.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Griessmeier, J. -M.] Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Braun, R.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [White, G.] Open Univ, Dept Phys & Astron, London, England. RP Asgekar, A (reprint author), Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM asgekar@astron.nl RI Yatawatta, Sarod/E-6037-2013; Miller-Jones, James/B-2411-2013; Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Intema, Huib/D-1438-2012; Kondratiev, Vladislav/N-1105-2015; Falcke, Heino/H-5262-2012; OI Yatawatta, Sarod/0000-0001-5619-4017; Miller-Jones, James/0000-0003-3124-2814; Tagger, Michel/0000-0003-2962-3220; Intema, Huib/0000-0002-5880-2730; Kondratiev, Vladislav/0000-0001-8864-7471; Falcke, Heino/0000-0002-2526-6724; Wijers, Ralph/0000-0002-3101-1808; de Gasperin, Francesco/0000-0003-4439-2627; van Weeren, Reinout/0000-0002-0587-1660 FU IUCAA, Pune; NASA [PF2-130104, NAS8-03060]; Chandra X-ray Center; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX LOFAR, designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. A. A. would like to thank M. I. R. Alves for discussions and comments on an early version of this manuscript. A. A. acknowledges support from IUCAA, Pune, during the preparation of this manuscript. R.J.v.W. acknowledges support from NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. C. F. acknowledges financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. NR 20 TC 8 Z9 8 U1 0 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR L11 DI 10.1051/0004-6361/201221001 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600156 ER PT J AU Berta, S Lutz, D Santini, P Wuyts, S Rosario, D Brisbin, D Cooray, A Franceschini, A Gruppioni, C Hatziminaoglou, E Hwang, HS Le Floc'h, E Magnelli, B Nordon, R Oliver, S Page, MJ Popesso, P Pozzetti, L Pozzi, F Riguccini, L Rodighiero, G Roseboom, I Scott, D Symeonidis, M Valtchanov, I Viero, M Wang, L AF Berta, S. Lutz, D. Santini, P. Wuyts, S. Rosario, D. Brisbin, D. Cooray, A. Franceschini, A. Gruppioni, C. Hatziminaoglou, E. Hwang, H. S. Le Floc'h, E. Magnelli, B. Nordon, R. Oliver, S. Page, M. J. Popesso, P. Pozzetti, L. Pozzi, F. Riguccini, L. Rodighiero, G. Roseboom, I. Scott, D. Symeonidis, M. Valtchanov, I. Viero, M. Wang, L. TI Panchromatic spectral energy distributions of Herschel sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: galaxies; galaxies: statistics; galaxies: star formation; galaxies: active; galaxies: evolution ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; STAR-FORMATION RATES; FAR-INFRARED PROPERTIES; HIGH-REDSHIFT GALAXIES; MU-M OBSERVATIONS; SIMILAR-TO 2.5; PHOTOMETRIC REDSHIFTS; GOODS-HERSCHEL; COSMOS FIELD AB Combining far-infrared Herschel photometry from the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time programs with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields, it is possible to sample the 8-500 mu m spectral energy distributions (SEDs) of galaxies with at least 7-10 bands. Extending to the UV, optical, and near-infrared, the number of bands increases up to 43. We reproduce the distribution of galaxies in a carefully selected restframe ten colors space, based on this rich data-set, using a superposition of multivariate Gaussian modes. We use this model to classify galaxies and build median SEDs of each class, which are then fitted with a modified version of the MAGPHYS code that combines stellar light, emission from dust heated by stars and a possible warm dust contribution heated by an active galactic nucleus (AGN). The color distribution of galaxies in each of the considered fields can be well described with the combination of 6-9 classes, spanning a large range of far- to near-infrared luminosity ratios, as well as different strength of the AGN contribution to bolometric luminosities. The defined Gaussian grouping is used to identify rare or odd sources. The zoology of outliers includes Herschel-detected ellipticals, very blue z similar to 1 Ly-break galaxies, quiescent spirals, and torus-dominated AGN with star formation. Out of these groups and outliers, a new template library is assembled, consisting of 32 SEDs describing the intrinsic scatter in the restframe UV-to-submm colors of infrared galaxies. This library is tested against L(IR) estimates with and without Herschel data included, and compared to eight other popular methods often adopted in the literature. When implementing Herschel photometry, these approaches produce L(IR) values consistent with each other within a median absolute deviation of 10-20%, the scatter being dominated more by fine tuning of the codes, rather than by the choice of SED templates. Finally, the library is used to classify 24 mu m detected sources in PEP GOODS fields on the basis of AGN content, L(60)/L(100) color and L(160)/L(1.6) luminosity ratio. AGN appear to be distributed in the stellar mass (M-*) vs. star formation rate (SFR) space along with all other galaxies, regardless of the amount of infrared luminosity they are powering, with the tendency to lie on the high SFR side of the "main sequence". The incidence of warmer star-forming sources grows for objects with higher specific star formation rates (sSFR), and they tend to populate the "off-sequence" region of the M-* - SFR - z space. C1 [Berta, S.; Lutz, D.; Wuyts, S.; Rosario, D.; Magnelli, B.; Popesso, P.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Brisbin, D.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Franceschini, A.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Gruppioni, C.; Pozzetti, L.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Hatziminaoglou, E.] ESO, D-85748 Garching, Germany. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Le Floc'h, E.] Univ Paris Diderot, IRFU Serv Astrophys, Lab AIM, CEA DSM,CNRS,CEA Saclay, F-91191 Gif Sur Yvette, France. [Nordon, R.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Oliver, S.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Page, M. J.; Symeonidis, M.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Riguccini, L.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94305 USA. [Roseboom, I.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Valtchanov, I.] ESA, ESAC, Herschel Sci Ctr, Madrid 28691, Spain. [Viero, M.] CALTECH, Pasadena, CA 91125 USA. RP Berta, S (reprint author), Max Planck Inst Extraterr Phys MPE, Postfach 1312, D-85741 Garching, Germany. EM berta@mpe.mpg.de OI Gruppioni, Carlotta/0000-0002-5836-4056; Pozzetti, Lucia/0000-0001-7085-0412; Santini, Paola/0000-0002-9334-8705; Rodighiero, Giulia/0000-0002-9415-2296; Scott, Douglas/0000-0002-6878-9840 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (PR China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA) FX The authors wish to thank Dr. Jacopo Fritz for providing his library of AGN torus emission models, and the anonymous referee for her/his useful comments. This work made use of the code FASTEM, distributed by the Auton Lab, and developed by Andrew Moore, Paul Hsiung, Peter Sand, point of contact Saswati Ray. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM(France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including University of Lethbridge (Canada), NAOC (PR China), CEA, LAM (France), IFSI, University of Padua (Italy), IAC (Spain), Stockholm Observatory (Sweden), Imperial College London, RAL, UCL-MSSL, UKATC, University of Sussex (UK), Caltech, JPL, NHSC, University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (PR China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK) and NASA (USA). NR 116 TC 40 Z9 40 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A100 DI 10.1051/0004-6361/201220859 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600100 ER PT J AU Bourrier, V des Etangs, AL Dupuy, H Ehrenreich, D Vidal-Madjar, A Hebrard, G Ballester, GE Desert, JM Ferlet, R Sing, DK Wheatley, PJ AF Bourrier, V. des Etangs, A. Lecavelier Dupuy, H. Ehrenreich, D. Vidal-Madjar, A. Hebrard, G. Ballester, G. E. Desert, J. -M. Ferlet, R. Sing, D. K. Wheatley, P. J. TI Atmospheric escape from HD 189733b observed in H I Lyman-alpha: detailed analysis of HST/STIS September 2011 observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: atmospheres; stars: individual: HD189733 ID HUBBLE-SPACE-TELESCOPE; TRANSITING EXTRASOLAR PLANET; ENERGETIC NEUTRAL ATOMS; SMALL ORBITAL DISTANCES; TIME-SERIES PHOTOMETRY; HOT-JUPITERS; TRANSMISSION SPECTROSCOPY; EXOPLANET HD-209458B; GIANT PLANETS; MU-M AB Observations of transits of the hot giant exoplanet HD189733b in the unresolved H I Lyman-alpha line show signs of hydrogen escaping the upper atmosphere of the planet. New resolved Lyman-alpha observations obtained with the STIS spectrograph onboard the Hubble Space Telescope in April 2010 and September 2011 confirmed that the planet is evaporating, and furthermore discovered significant temporal variations in the physical conditions of its evaporating atmosphere. Here we present a detailed analysis of the September 2011 observations of HD189733b, when an atmospheric signature was detected. We present specific methods to find and characterize this absorption signature of escaping hydrogen in the Lyman-alpha line, and to calculate its false-positive probability, found to be 3.6%. Taking advantage of the spectral resolution and high sensitivity of the STIS spectrograph, we also present new results on temporal and spectro-temporal variability of this absorption feature. We also report the observation of HD189733b in other lines (Si III at 1206.5 angstrom, N V at 1240 angstrom). Variations in these lines could be explained either by early occultation by a bow-shock rich in highly ionized species, or by stellar variations. C1 [Bourrier, V.; des Etangs, A. Lecavelier; Dupuy, H.; Vidal-Madjar, A.; Hebrard, G.; Ferlet, R.] Inst Astrophys, CNRS, UMR 7095, F-75014 Paris, France. [Bourrier, V.; des Etangs, A. Lecavelier; Dupuy, H.; Vidal-Madjar, A.; Hebrard, G.; Ferlet, R.] Univ Paris 06, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Ehrenreich, D.] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sing, D. K.] Univ Exeter, Astrophys Grp, Sch Phys, Exeter EX4 4QL, Devon, England. [Wheatley, P. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Bourrier, V (reprint author), Inst Astrophys, CNRS, UMR 7095, 98Bis Blvd Arago, F-75014 Paris, France. EM bourrier@iap.fr FU NASA [NAS 5-26555]; European Commission [PIEF-GA-2011-298916]; STScI [HST-GO-11673.01-A]; Centre National d'Etudes Spatiales (CNES); Fondation Simone et Cino Del Duca; [11673] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. We thank the referee for its clarifying comments. D. E. acknowledges the funding from the European Commission's Seventh Framework Programme as a Marie Curie Intra-European Fellow (PIEF-GA-2011-298916). G. E. B. acknowledges financial support by this program through STScI grant HST-GO-11673.01-A to the University of Arizona. These observations are associated with program #11673. The authors acknowledge financial support from the Centre National d'Etudes Spatiales (CNES). This work has also been supported by an award from the Fondation Simone et Cino Del Duca. NR 91 TC 30 Z9 30 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A63 DI 10.1051/0004-6361/201220533 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600063 ER PT J AU Forbrich, J Wolk, SJ AF Forbrich, J. Wolk, S. J. TI On the radio-X-ray connection in young stellar objects in the Orion nebula cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio continuum: stars; stars: pre-main sequence; X-rays: stars; stars: protostars ID ULTRADEEP PROJECT; T-TAURI; ARRAY OBSERVATIONS; VLBI OBSERVATIONS; STARS; EMISSION; CHANDRA; MULTIWAVELENGTH; PROTOSTARS; ASTRONOMY AB Context. Both X-ray and radio observations offer insight into the high-energy processes of young stellar objects (YSOs). The observed thermal X-ray emission can be accompanied by both thermal and nonthermal radio emission. Due to variability, simultaneous X-ray and radio observations are a priori required, but only a comparably small number of YSOs have been studied in this way. Results have been inconclusive due to the even smaller number of YSOs that were simultaneously detected in X-ray and radio observations. Aims. We use archival X-ray and radio observations of the Orion nebula cluster (ONC) to significantly enlarge the sample size of known YSOs with both X-ray and radio detections. Methods. We study the ONC using multi-epoch non-simultaneous archival Chandra X-ray and NRAO Very Large Array (VLA) single-band radio data. The multiple epochs allow us to reduce the impact of variability by obtaining approximated quiescent fluxes. Results. We find that only a small fraction of the X-ray sources (7%) have radio counterparts, even if 60% of the radio sources have X-ray counterparts. YSOs with detections in both bands thus constitute a small minority of the cluster. The radio flux density is typically too low to distinguish thermal and nonthermal radio sources. Only a small fraction of the YSOs with detections in both bands are compatible with the empirical "Gudel-Benz" (GB) relation. Most of the sources not compatible with the GB relation are proplyds, and thus likely thermal sources, but only a fraction of the proplyds is detected in both bands, such that the role of these sources is inconclusive. Conclusions. While the radio sources appear to be globally unrelated to the X-ray sources, the X-ray dataset clearly is much more sensitive than the radio data. We find tentative evidence that known non-thermal radio sources and saturated X-ray sources are indeed close to the empirical relation, even if skewed to higher radio luminosities, as they are expected to be. Most of the sources that are clearly incompatible with the empirical relation are proplyds that could instead plausibly be thermal radio sources. The newly expanded Karl G. Jansky Very Large Array with its significantly enhanced continuum sensitivity is beginning to provide an ideal tool for addressing this issue. Combined X-ray and radio studies of YSOs using older VLA data are clearly limited by the typically low signal-to-noise of the radio detections, providing insufficient information to disentangle thermal and nonthermal sources. C1 [Forbrich, J.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Forbrich, J.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forbrich, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM jan.forbrich@univie.ac.at; swolk@cfa.harvard.edu OI Wolk, Scott/0000-0002-0826-9261 FU Austrian Science Fund (FWF) FX We would like to thank the referee, Manuel Gudel, for constructive comments that helped to significantly improve this paper. This publication is supported by the Austrian Science Fund (FWF). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 30 TC 8 Z9 8 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A56 DI 10.1051/0004-6361/201220579 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600056 ER PT J AU Kaminski, T Gottlieb, CA Menten, KM Patel, NA Young, KH Brunken, S Muller, HSP McCarthy, MC Winters, JM Decin, L AF Kaminski, T. Gottlieb, C. A. Menten, K. M. Patel, N. A. Young, K. H. Bruenken, S. Mueller, H. S. P. McCarthy, M. C. Winters, J. M. Decin, L. TI Pure rotational spectra of TiO and TiO2 in VY Canis Majoris SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: winds, outflows; circumstellar matter; stars: individual: VY Canis Majoris; line: identification ID INTER-STELLAR TITANIUM; MASS-LOSS; MOLECULAR-SPECTROSCOPY; CIRCUMSTELLAR GAS; COLOGNE DATABASE; MIRA VARIABLES; DUST SHELLS; SUPERGIANT; EMISSION; MILLIMETER AB We report the first detection of pure rotational transitions of TiO and TiO2 at (sub-)millimeter wavelengths towards the red supergiant VY CMa. A rotational temperature, T-rot, of about 250K was derived for TiO2. Although T-rot was not well constrained for TiO, it is likely somewhat higher than that of TiO2. The detection of the Ti oxides confirms that they are formed in the circumstellar envelopes of cool oxygen-rich stars and may be the "seeds" of inorganic-dust formation, but alternative explanations for our observation of TiO and TiO2 in the cooler regions of the envelope cannot be ruled out at this time. The observations suggest that a significant fraction of the oxides is not converted to dust, but instead remains in the gas phase throughout the outflow. C1 [Kaminski, T.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gottlieb, C. A.; Patel, N. A.; Young, K. H.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruenken, S.; Mueller, H. S. P.] Inst Phys 1, D-50937 Cologne, Germany. [Winters, J. M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. RP Kaminski, T (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kaminski@mpifr.de RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; McCarthy, Michael/0000-0001-9142-0008; Mueller, Holger/0000-0002-0183-8927 FU Bundesministerium fur Bildung und Forschung (BMBF) [FKZ 50OF0901]; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX H.S.P.M. thanks the Bundesministerium fur Bildung und Forschung (BMBF) for support via project FKZ 50OF0901 (ICC HIFI Herschel). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). We acknowledge these institutions. NR 55 TC 22 Z9 22 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A113 DI 10.1051/0004-6361/201220290 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600113 ER PT J AU Kreplin, A Weigelt, G Kraus, S Grinin, V Hofmann, KH Kishimoto, M Schertl, D Tambovtseva, L Clausse, JM Massi, F Perraut, K Stee, P AF Kreplin, A. Weigelt, G. Kraus, S. Grinin, V. Hofmann, K-H. Kishimoto, M. Schertl, D. Tambovtseva, L. Clausse, J-M. Massi, F. Perraut, K. Stee, Ph. TI Revealing the inclined circumstellar disk in the UX Orionis system KK Ophiuchi SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: interferometric; stars: pre-main sequence; stars: individual: KK Ophiuchi; circumstellar matter ID HERBIG-AE/BE STARS; BETA-PICTORIS PHENOMENON; YOUNG STELLAR OBJECTS; SELF-SHADOWED DISKS; MAIN-SEQUENCE STARS; OPTICAL-PROPERTIES; VEGA-TYPE; T-TAURI; MODEL; POLARIMETRY AB Aims. We study the inner sub-AU region of the circumstellar environment of the UX Ori-type star KK Oph with near-infrared VLTI/AMBER interferometry. We are particularly interested in the inclination of the star-disk system, and we use this information to test the current standard picture for UX Ori stars. Methods. We recorded spectrally dispersed (R similar to 35) interferograms in the near-infrared H and K bands with the VLTI/AMBER instrument. The derived visibilities, closure phases, and the spectral energy distribution of KK Oph were compared with two-dimensional geometric and radiative transfer models (RADMC). Results. We obtained visibilities at four different position angles. Using two-dimensional geometric models, we derive an axis ratio similar to 3.0 corresponding to an inclination of similar to 70 degrees. A fitted inclined ring model leads to a ring radius of 2.8 +/- 0.2 mas, corresponding to 0.44 +/- 0.03 AU at a distance of 160 pc, which is larger than the dust sublimation radius of similar to 0.1 AU predicted for a dust sublimation temperature of 1500 K. Our derived two-dimensional RADMC model consists of a circumstellar disk with an inclination angle of similar to 70 degrees and an additional dust envelope. Conclusions. The finding of an similar to 70 degrees inclined disk around KK Oph is consistent with the prediction that UX Ori objects are seen under large inclination angles, and orbiting clouds in the line of sight cause the observed variability. Furthermore, our results suggest that the orbit of the companion KK Oph B and the disk plane are coplanar. C1 [Kreplin, A.; Weigelt, G.; Hofmann, K-H.; Kishimoto, M.; Schertl, D.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kraus, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grinin, V.; Tambovtseva, L.] RAS, Pulkovo Observ, St Petersburg 196140, Russia. [Grinin, V.] St Petersburg State Univ, VV Sobolev Astron Inst, St Petersburg, Russia. [Massi, F.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Perraut, K.] Univ Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Clausse, J-M.; Stee, Ph.] UMR 7293 UNS CNRS OCA, Lab Lagrange, F-06304 Nice 4, France. RP Kreplin, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM akreplin@mpifr-bonn.mpg.de RI Grinin, Vladimir/M-9509-2013; OI Grinin, Vladimir/0000-0001-8923-9541; Massi, Fabrizio/0000-0001-6407-8032 FU ESO telescopes at Paranal Observatory [083.D-0224(C), 088.C-0575(A)]; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne; Presidium of RAS [P 21, NSh. - 1625.2012.2]; Max-Planck-Society FX Based on observations made with ESO telescopes at Paranal Observatory under program ID: 083.D-0224(C) and 088.C-0575(A).; A. Kreplin was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. V. G. and L. T. were supported in part by the grant of the Presidium of RAS P 21 and grant NSh. - 1625.2012.2. They also thank the Max-Planck-Society for the support during their stay in Bonn. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 41 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A21 DI 10.1051/0004-6361/201220806 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600021 ER PT J AU Mancini, L Southworth, J Ciceri, S Fortney, JJ Morley, CV Dittmann, JA Tregloan-Reed, J Bruni, I Barbieri, M Evans, DF D'Ago, G Nikolov, N Henning, T AF Mancini, L. Southworth, J. Ciceri, S. Fortney, J. J. Morley, C. V. Dittmann, J. A. Tregloan-Reed, J. Bruni, I. Barbieri, M. Evans, D. F. D'Ago, G. Nikolov, N. Henning, Th. TI A lower radius and mass for the transiting extrasolar planet HAT-P-8b SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: fundamental parameters; stars: fundamental parameters; stars: individual: HAT-P-8 ID PHYSICAL-PROPERTIES; EXOPLANETARY SYSTEMS; TRANSMISSION SPECTRA; ECLIPSING BINARIES; SPACE-TELESCOPE; GIANT PLANETS; LIGHT CURVES; HD 209458B; HOT; PHOTOMETRY AB Context. The extrasolar planet HAT-P-8 b was thought to be one of the more inflated transiting hot Jupiters. Aims. By using new and existing photometric data, we computed precise estimates of the physical properties of the system. Methods. We present photometric observations comprising eleven light curves covering six transit events, obtained using five medium-class telescopes and telescope-defocussing technique. One transit was simultaneously obtained through four optical filters, and two transits were followed contemporaneously from two observatories. We modelled these and seven published datasets using the JKTEBOP code. The physical parameters of the system were obtained from these results and from published spectroscopic measurements. In addition, we investigated the theoretically-predicted variation of the apparent planetary radius as a function of wavelength, covering the range 330-960 nm. Results. We find that HAT-P-8 b has a significantly lower radius (1.321 +/- 0.037 R-Jup) and mass (1.275 +/- 0.053 M-Jup) compared to previous estimates (1.50(-0.06)(+0.08) R-Jup and 1.52(-0.16)(+0.18) M-Jup respectively). We also detect a radius variation in the optical bands that, when compared with synthetic spectra of the planet, may indicate the presence of a strong optical absorber, perhaps TiO and VO gases, near the terminator of HAT-P-8 b. Conclusions. These new results imply that HAT-P-8 b is not significantly inflated, and that its position in the planetary mass-radius diagram is congruent with those of many other transiting extrasolar planets. C1 [Mancini, L.; Ciceri, S.; Nikolov, N.; Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mancini, L.; D'Ago, G.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy. [Southworth, J.; Tregloan-Reed, J.; Evans, D. F.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Fortney, J. J.; Morley, C. V.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Dittmann, J. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruni, I.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Barbieri, M.] INAF Osservatorio Astron Bologna, I-35122 Padua, Italy. RP Mancini, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM mancini@mpia.de RI D'Ago, Giuseppe/N-8318-2016; OI D'Ago, Giuseppe/0000-0001-9697-7331; Fortney, Jonathan/0000-0002-9843-4354; Barbieri, Mauro/0000-0001-8362-3462; Bruni, Ivan/0000-0002-1560-4590 FU STFC FX Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, Spain, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC); observations obtained with the 1.52m Cassini telescope at OAB Loiano Observatory, Italy; data collected at the Isaac Newton Telescope, operated on the island of La Palma, by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos. The reduced light curves presented in this work will be made available at the CDS (http://cdsweb.u-strasbg.fr/). We thank K. Todorov and R. F. Diaz for supplying photometric data. JS acknowledges financial support from STFC in the form of an Advanced Fellowship. We thank U. Thiele and R. Gualandi for their technical assistance at the CA 2.2m telescope and Cassini telescope, respectively. We thank the anonymous referee for their useful criticisms and suggestions that helped us to improve the quality of the present paper. The following internet-based resources were used in research for this paper: the ESO Digitized Sky Survey; the NASA Astrophysics Data System; the SIMBAD data base operated at CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University. LM thanks the HESS site in Namibia for the kind hospitality. NR 58 TC 30 Z9 30 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A11 DI 10.1051/0004-6361/201220291 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600011 ER PT J AU Omont, A Yang, C Cox, P Neri, R Beelen, A Bussmann, RS Gavazzi, R van der Werf, P Riechers, D Downes, D Krips, M Dye, S Ivison, R Vieira, JD Weiss, A Aguirre, JE Baes, M Baker, AJ Bertoldi, F Cooray, A Dannerbauer, H De Zotti, G Eales, SA Fu, H Gao, Y Guelin, M Harris, AI Jarvis, M Lehnert, M Leeuw, L Lupu, R Menten, K Michalowski, MJ Negrello, M Serjeant, S Temi, P Auld, R Dariush, A Dunne, L Fritz, J Hopwood, R Hoyos, C Ibar, E Maddox, S Smith, MWL Valiante, E Bock, J Bradford, CM Glenn, J Scott, KS AF Omont, A. Yang, C. Cox, P. Neri, R. Beelen, A. Bussmann, R. S. Gavazzi, R. van der Werf, P. Riechers, D. Downes, D. Krips, M. Dye, S. Ivison, R. Vieira, J. D. Weiss, A. Aguirre, J. E. Baes, M. Baker, A. J. Bertoldi, F. Cooray, A. Dannerbauer, H. De Zotti, G. Eales, S. A. Fu, H. Gao, Y. Guelin, M. Harris, A. I. Jarvis, M. Lehnert, M. Leeuw, L. Lupu, R. Menten, K. Michalowski, M. J. Negrello, M. Serjeant, S. Temi, P. Auld, R. Dariush, A. Dunne, L. Fritz, J. Hopwood, R. Hoyos, C. Ibar, E. Maddox, S. Smith, M. W. L. Valiante, E. Bock, J. Bradford, C. M. Glenn, J. Scott, K. S. TI H2O emission in high-z ultra-luminous infrared galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimeter: galaxies; radio lines: galaxies ID QUASAR APM 08279+5255; WATER-VAPOR EMISSION; DENSE MOLECULAR GAS; STAR-FORMATION RATE; HERSCHEL-ATLAS; SUBMILLIMETER GALAXY; HIGH-REDSHIFT; CLOVERLEAF QUASAR; IRAS 10214+4724; MARKARIAN 231 AB Using the IRAM Plateau de Bure interferometer (PdBI), we report the detection of water vapor in six new lensed ultra-luminous starburst galaxies at high redshift, discovered in the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS). The sources are detected either in the 2(02)-1(11) or 2(11)-2(02) H2O emission lines with integrated line fluxes ranging from 1.8 to 14 Jy km s(-1). The corresponding apparent luminosities are mu L-H2O similar to 3-12 x 10(8) L-circle dot, where mu is the lensing magnification factor (3 < mu < 12). These results confirm that H2O lines are among the strongest molecular lines in high-z ultra-luminous starburst galaxies, with intensities almost comparable to those of the high-J CO lines, and similar profiles and line widths (similar to 200-900 km s(-1)). With the current sensitivity of the PdBI, the water lines can therefore easily be detected in high-z lensed galaxies (with F(500 mu m) > 100 mJy) discovered in the Herschel surveys. Correcting the luminosities for amplification, using existing lensing models, L-H2O is found to have a strong dependence on the infrared luminosity, varying as similar to L-IR(1.2). This relation, which needs to be confirmed with better statistics, may indicate a role of radiative (infrared) excitation of the H2O lines, and implies that high-z galaxies with L-IR greater than or similar to 10(13) L-circle dot tend to be very strong emitters in water vapor, that have no equivalent in the local universe. C1 [Omont, A.; Yang, C.; Gavazzi, R.] Univ Paris 06, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Omont, A.; Yang, C.; Gavazzi, R.] CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Yang, C.; Gao, Y.] Purple Mt Observ, Nanjing, Jiangsu, Peoples R China. [Yang, C.] Beijing Normal Univ, Dept Astron, Beijing, Peoples R China. [Cox, P.; Neri, R.; Downes, D.; Krips, M.; Guelin, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Beelen, A.] Univ Paris 11, F-91405 Orsay, France. [Beelen, A.] CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Riechers, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Dye, S.] Ctr Astron & Particle Theory, Nottingham NG7 2RD, England. [Ivison, R.; Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Aguirre, J. E.; Lupu, R.; Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Baes, M.; Michalowski, M. J.; Fritz, J.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Dannerbauer, H.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Eales, S. A.; Auld, R.; Dariush, A.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fu, H.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [De Zotti, G.; Negrello, M.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [De Zotti, G.; Negrello, M.] SISSA, I-34136 Trieste, Italy. [Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Jarvis, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran. [Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Dunne, L.; Hoyos, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bock, J.; Bradford, C. M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Bradford, C. M.] Jet Prop Lab, Pasadena, CA 91109 USA. [Glenn, J.] Univ Colorado, CASA, Boulder, CO 80303 USA. [Lehnert, M.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ibar, E.] Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Leeuw, L.] Univ S Africa, Coll Grad Studies, ZA-003 Unisa, South Africa. RP Omont, A (reprint author), Univ Paris 06, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. EM omont@iap.fr RI YANG, Chentao/H-1966-2015; Ivison, R./G-4450-2011; Baes, Maarten/I-6985-2013; Lupu, Roxana/P-9060-2014 OI YANG, Chentao/0000-0002-8117-9991; Ivison, R./0000-0001-5118-1313; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; De Hoyos Fernandez De Cordova, Carlos/0000-0003-3120-6856; Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757; Lupu, Roxana/0000-0003-3444-5908 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); NASA through JPL; ASI-INAF [I/009/10/0]; CSA (Canada); NAOC (China); CEA; CNES; CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC; UKSA (UK); NASA (USA); FWO-Pegasus Marie Curie Fellowship FX Based on observations carried out with the IRAM Plateau de Bure interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The authors are grateful to the IRAM staff for their support. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. Italian participants in H-ATLAS acknowledge a financial contribution from the agreement ASI-INAF I/009/10/0. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including: Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). M.J. Michalowski acknowledges the support of a FWO-Pegasus Marie Curie Fellowship. NR 52 TC 20 Z9 20 U1 0 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A115 DI 10.1051/0004-6361/201220811 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600115 ER PT J AU Webb, NA Servillat, M AF Webb, N. A. Servillat, M. TI CV1 in the globular cluster M 22: confirming its nature through X-ray observations and optical spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE globular clusters: individual: M 22; binaries: close; stars: dwarf novae; X-rays: binaries ID HUBBLE-SPACE-TELESCOPE; ERUPTING DWARF NOVAE; CATACLYSMIC VARIABLES; XMM-NEWTON; ABSOLUTE MAGNITUDES; CLOSE BINARIES; STAR-CLUSTERS; M22; CORE; POPULATION AB Context. Observations of cataclysmic variables in globular clusters appear to show a dearth of outbursts compared to those observed in field. A number of explanations have been proposed, including low mass-transfer rates and/or moderate magnetic fields implying higher mass white dwarfs than the average observed in the field. Alternatively this apparent dearth may be simply a selection bias. Aims. We examine multi-wavelength data of a new cataclysmic variable, CV1, in the globular cluster M 22 to try to constrain its period and magnetic nature, with an aim at understanding whether globular cluster cataclysmic variables are intrinsically different from those observed in the field. Methods. We use the sub-arcsecond resolution of the Chandra ACIS-S to identify the X-ray counterpart to CV1 and analyse the X-ray spectrum to determine the spectral model that best describes this source. We also examine the low resolution optical spectrum for emission lines typical of cataclysmic variables. Cross correlating the H(alpha)line in each individual spectrum also allows us to search for orbital motion. Results. The X-ray spectrum reveals a source best-fitted with a high-temperature bremsstrahlung model and an X-ray unabsorbed luminosity of 1.8 x 10(32) erg s(-1) (0.3-8.0 keV), which are typical of cataclysmic variables. Optical spectra reveal Balmer emission lines, which are indicative of an accretion disc. Potential radial velocity in the H-alpha emission line is detected and a period for CV1 is proposed. Conclusions. These observations support the CV identification. The radial velocity measurements suggest that CV1 may have an orbital period of similar to 7 h, but further higher resolution optical spectroscopy of CV1 is needed to unequivocally establish the nature of this CV and its orbital period. C1 [Webb, N. A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Webb, N. A.] CNRS, IRAP, F-31028 Toulouse 4, France. [Servillat, M.] Univ Paris 07, CEA Saclay, CNRS, Lab AIM,CEA,DSM,IRFU,SAp, F-91191 Gif Sur Yvette, France. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Webb, NA (reprint author), Univ Toulouse, UPS OMP, IRAP, Toulouse, France. EM Natalie.Webb@irap.omp.eu FU NASA/Chandra grants [AR9-0013X, GO0-11063X]; NSF [AST-0909073]; ESA Member States; NASA; [073.D-0392(A)] FX The authors are extremely grateful to the anonymous referee who raised a number of very valuable points and thus helped to improve the manuscript enormously. M. S. acknowledges supports from NASA/Chandra grants AR9-0013X and GO0-11063X and NSF grant AST-0909073. This research has made use of data obtained from the Chandra Data Archive, and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. It was also based on observations made with ESO Telescopes at the Paranal Observatory under programme ID 073.D-0392(A) and (B), and XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 50 TC 2 Z9 2 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAR PY 2013 VL 551 AR A60 DI 10.1051/0004-6361/201117229 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 110QR UT WOS:000316460600060 ER PT J AU Frazier, M Miller, AW Ruiz, GM AF Frazier, Melanie Miller, A. Whitman Ruiz, Gregory M. TI Linking science and policy to prevent the spread of invasive species from the ballast water discharge of ships SO ECOLOGICAL APPLICATIONS LA English DT Article C1 [Frazier, Melanie] US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Washington, DC 20460 USA. [Miller, A. Whitman; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD USA. RP Frazier, M (reprint author), US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Washington, DC 20460 USA. EM frazier.melanie@epa.gov OI Ruiz, Gregory/0000-0003-2499-441X; Miller, Whitman/0000-0003-0484-182X NR 0 TC 6 Z9 6 U1 0 U2 55 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2013 VL 23 IS 2 BP 287 EP 288 PG 2 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 111ZC UT WOS:000316559800001 PM 23634580 ER PT J AU Ruiz, GM Fofonoff, PW Ashton, G Minton, MS Miller, AW AF Ruiz, Gregory M. Fofonoff, Paul W. Ashton, Gail Minton, Mark S. Miller, A. Whitman TI Geographic variation in marine invasions among large estuaries: effects of ships and time SO ECOLOGICAL APPLICATIONS LA English DT Article DE ballast water; biogeography; estuaries; invasibility; marine invasions; nonnative species; propagule supply; ships ID BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; BALLAST WATER; NORTH-AMERICA; ORGANISMS; ECOSYSTEMS; CALIFORNIA; DISCOVERY; PATTERNS; HOTSPOT AB Coastal regions exhibit strong geographic patterns of nonnative species richness. Most invasions in marine ecosystems are known from bays and estuaries, where ship-mediated transfers (on hulls or in ballasted materials) have been a dominant vector of species introductions. Conspicuous spatial differences in nonnative species richness exist among bays, but the quantitative relationship between invasion magnitude and shipping activity across sites is largely unexplored. Using data on marine invasions (for invertebrates and algae) and commercial shipping across 16 large bays in the United States, we estimated (1) geographic variation in nonnative species richness attributed to ships, controlling for effects of salinity and other vectors, (2) changes through time in geographic variation of these ship-mediated invasions, and (3) effects of commercial ship traffic and ballast water discharge magnitude on nonnative species richness. For all nonnative species together (regardless of vector, salinity, or time period), species richness differed among U. S. coasts, being significantly greater for Pacific Coast bays than Atlantic or Gulf Coast bays. This difference also existed when considering only species attributed to shipping (or ballast water), controlling for time and salinity. Variation in nonnative species richness among Pacific Coast bays was strongly affected by these same criteria. San Francisco Bay, California, had over 200 documented nonnative species, more than twice that reported for other bays, but many species were associated with other (non-shipping) vectors or the extensive low-salinity habitats (unavailable in some bays). When considering only ship-or ballast-mediated introductions in high-salinity waters, the rate of newly detected invasions in San Francisco Bay has converged increasingly through time on that for other Pacific Coast bays, appearing no different since 1982. Considering all 16 bays together, there was no relationship between either (1) number of ship arrivals (from foreign ports) and number of introductions attributed to ships since 1982 or (2) volume of foreign ballast water discharge and number of species attributed to ballast water since 1982. These shipping measures are likely poor proxies for propagule supply, although they are sometimes used as such, highlighting a fundamental gap in data needed to evaluate invasion dynamics and management strategies. C1 [Ruiz, Gregory M.; Fofonoff, Paul W.; Minton, Mark S.; Miller, A. Whitman] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ashton, Gail] Smithsonian Environm Res Ctr, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. RP Ruiz, GM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM ruizg@si.edu OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930; Miller, Whitman/0000-0003-0484-182X FU U.S. Coast Guard; Smithsonian Institution FX We thank Ashley Arnwine, Eric Bah, Tami Huber, Amanda Reynolds, and Brian Steves for assistance with collection and analysis of shipping and invasion history data. We benefited from discussion with Jim Carlton, Tuck Hines, Henry Lee, Rich Everett, and Debby Reusser. This work was supported by funding from the U.S. Coast Guard and the Smithsonian Institution. NR 50 TC 12 Z9 13 U1 0 U2 58 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2013 VL 23 IS 2 BP 311 EP 320 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 111ZC UT WOS:000316559800004 PM 23634583 ER PT J AU Reusser, DA Lee, H Frazier, M Ruiz, GM Fofonoff, PW Minton, MS Miller, AW AF Reusser, Deborah A. Lee, Henry, II Frazier, Melanie Ruiz, Gregory M. Fofonoff, Paul W. Minton, Mark S. Miller, A. Whitman TI Per capita invasion probabilities: an empirical model to predict rates of invasion via ballast water SO ECOLOGICAL APPLICATIONS LA English DT Article DE aquatic invaders; ballast water discharge; IMO standards; invasion probabilities; propagule pressure ID BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; MARINE COMMUNITIES; NORTH-AMERICA; ESTUARINE; ECOLOGY; PATTERN; SHIPS; RISK; SEA AB Ballast water discharges are a major source of species introductions into marine and estuarine ecosystems. To mitigate the introduction of new invaders into these ecosystems, many agencies are proposing standards that establish upper concentration limits for organisms in ballast discharge. Ideally, ballast discharge standards will be biologically defensible and adequately protective of the marine environment. We propose a new technique, the per capita invasion probability (PCIP), for managers to quantitatively evaluate the relative risk of different concentration-based ballast water discharge standards. PCIP represents the likelihood that a single discharged organism will become established as a new nonindigenous species. This value is calculated by dividing the total number of ballast water invaders per year by the total number of organisms discharged from ballast. Analysis was done at the coast-wide scale for the Atlantic, Gulf, and Pacific coasts, as well as the Great Lakes, to reduce uncertainty due to secondary invasions between estuaries on a single coast. The PCIP metric is then used to predict the rate of new ballast-associated invasions given various regulatory scenarios. Depending upon the assumptions used in the risk analysis, this approach predicts that approximately one new species will invade every 10-100 years with the International Maritime Organization (IMO) discharge standard of >10 organisms with body size >50 mu m per m 3 of ballast. This approach resolves many of the limitations associated with other methods of establishing ecologically sound discharge standards, and it allows policy makers to use risk-based methodologies to establish biologically defensible discharge standards. C1 [Reusser, Deborah A.] US Geol Survey, Western Fisheries Res Ctr, Newport, OR 97365 USA. [Reusser, Deborah A.] Oregon State Univ, Newport, OR 97365 USA. [Lee, Henry, II; Frazier, Melanie] US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Newport, OR 97365 USA. [Ruiz, Gregory M.; Fofonoff, Paul W.; Minton, Mark S.; Miller, A. Whitman] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reusser, DA (reprint author), US Geol Survey, Western Fisheries Res Ctr, 2111 SE Marine Sci Dr, Newport, OR 97365 USA. EM dreusser@usgs.gov OI Ruiz, Gregory/0000-0003-2499-441X; Minton, Mark/0000-0002-9439-4930; Miller, Whitman/0000-0003-0484-182X FU Department of Defense Legacy Program; National Sea Grant Program; Smithsonian Institution; U.S. EPA [AMI/GEOSS EP08D00051] FX The collection and compilation of the invasion data were supported by past funding: Department of Defense Legacy Program, National Sea Grant Program, and the Smithsonian Institution. Melanie R. Frazier's contributions were partially funded by a U.S. EPA post-doc (AMI/GEOSS EP08D00051). Sampling data were also provided by Stephan Gollasch to assist in identifying the range of organism concentrations found in sampled ballast water. This publication was subjected to review by the National Health and Environmental Effects Research Laboratory's Western Ecology Division of the EPA, and the Western Fisheries Research Center of USGS, and is approved for publication. However, approval does not signify that the contents reflect the views of the U.S. EPA. The use of trade, firm, or corporation names in this publication is for the information and convenience of the reader; such use does not constitute official endorsement or approval by the U.S. Department of Interior, the U.S. Geological Survey, or the U.S. Environmental Protection Agency of any product or service to the exclusion of others that may be suitable. NR 42 TC 7 Z9 7 U1 0 U2 39 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2013 VL 23 IS 2 BP 321 EP 330 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 111ZC UT WOS:000316559800005 PM 23634584 ER PT J AU Frazier, M Miller, AW Lee, H Reusser, DA AF Frazier, Melanie Miller, A. Whitman Lee, Henry, II Reusser, Deborah A. TI Counting at low concentrations: the statistical challenges of verifying ballast water discharge standards SO ECOLOGICAL APPLICATIONS LA English DT Article DE ballast water discharge; Clean Water Act; IMO; invasive species; NIS; performance standards; Poisson distribution ID INTRODUCTIONS AB Discharge from the ballast tanks of ships is one of the primary vectors of nonindigenous species in marine environments. To mitigate this environmental and economic threat, international, national, and state entities are establishing regulations to limit the concentration of living organisms that may be discharged from the ballast tanks of ships. The proposed discharge standards have ranged from zero detectable organisms to <10 organisms/m(3). If standard sampling methods are used, verifying whether ballast discharge complies with these stringent standards will be challenging due to the inherent stochasticity of sampling. Furthermore, at low concentrations, very large volumes of water must be sampled to find enough organisms to accurately estimate concentration. Despite these challenges, adequate sampling protocols comprise a critical aspect of establishing standards because they help define the actual risk level associated with a standard. A standard that appears very stringent may be effectively lax if it is paired with an inadequate sampling protocol. We describe some of the statistical issues associated with sampling at low concentrations to help regulators understand the uncertainties of sampling as well as to inform the development of sampling protocols that ensure discharge standards are adequately implemented. C1 [Frazier, Melanie; Lee, Henry, II] US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Newport, OR 97365 USA. [Miller, A. Whitman] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Reusser, Deborah A.] US Geol Survey, Western Fisheries Res Ctr, Newport, OR 97365 USA. RP Frazier, M (reprint author), US EPA, Western Ecol Div, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, 2111 SE Marine Sci Dr, Newport, OR 97365 USA. EM frazier.melanie@epa.gov OI Miller, Whitman/0000-0003-0484-182X FU U.S. EPA [AMI/GEOSS EP08D00051]; U.S. EPA (NHEERL) FX Funding was from U.S. EPA post-docs to M. Frazier (AMI/GEOSS EP08D00051 and NHEERL). We thank Karen Blocksom, Valerie Partridge, John Van Sickle, and three anonymous reviewers for helpful comments and discussion that helped shape this paper. We also thank Ryan Albert, Richard Everett, John Lishman, Robert J. Ozretich, Gregory Ruiz, and Jody Stecher for their valuable comments, error discovery, and general editing. This document has been reviewed in accordance with U. S. Environmental Protection Agency policy and approved for publication. Mention of trade names or commercial products does not constitute endorsement or recommendation for use. NR 36 TC 14 Z9 14 U1 1 U2 23 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD MAR PY 2013 VL 23 IS 2 BP 339 EP 351 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 111ZC UT WOS:000316559800007 PM 23634586 ER PT J AU Pimiento, C Gonzalez-Barba, G Hendy, AJW Jaramillo, C MacFadden, BJ Montes, C Suarez, SC Shippritt, M AF Pimiento, Catalina Gonzalez-Barba, Gerardo Hendy, Austin J. W. Jaramillo, Carlos MacFadden, Bruce J. Montes, Camilo Suarez, Sandra C. Shippritt, Monica TI Early Miocene chondrichthyans from the Culebra Formation, Panama: A window into marine vertebrate faunas before closure the Central American Seaway SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Batoids; Depth preferences; Neogene; Neotropics; Rays; Sharks; Systematic Paleontology ID SOUTH-AMERICA; WESTERN PANAMA; EARLY NEOGENE; ISTHMUS; STRATIGRAPHY; COLLISION; SHARKS; ARC AB The newly described chondrichthyan fauna of the early Miocene Culebra Formation of Panama provides insight into the marine vertebrates occupying shallow seas adjacent to the Central American Seaway, prior to the rise of the Isthmus of Panama. This study takes advantage of a time-limited and unique opportunity to recover fossil from renewed excavations of the Panama Canal. The chondrichthyan fauna of the Culebra Formation is composed of teeth and vertebral centra representing 12 taxa. The species found possessed a cosmopolitan tropical and warm-temperate distribution during the early Neogene and are similar to other assemblages of the tropical eastern Pacific and southern Caribbean. The taxa described suggest a neritic environment, and is in contrast with other interpretations that proposed bathyal water depths for the upper member of the Culebra Formation. The wide depth range of the most common species, Carcharocles chubutensis, and the habitat preference of Pristis sp., suggests varied marine environments, from deep, to shallow waters, close to emerged areas of the evolving isthmus. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Pimiento, Catalina; Hendy, Austin J. W.; Jaramillo, Carlos; Montes, Camilo; Suarez, Sandra C.] Smithsonian Trop Res Inst, Balboa, Panama. [Pimiento, Catalina; Hendy, Austin J. W.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Gonzalez-Barba, Gerardo] Univ Autonoma Baja California Sur, Area Ciencias Mar, Museo Hist Nat, La Paz 23080, AP, Mexico. [Montes, Camilo] Univ Los Andes, Bogota, Colombia. RP Pimiento, C (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM pimientoc@si.edu OI Suarez, Catalina/0000-0003-1562-5380; Montes, Camilo/0000-0002-3553-0787 FU U.S. NSF (National Science Foundation) PIRE (Partnerships in International Research and Education) [0966884]; Autoridad del Canal de Panama [SAA-199520-KRP]; Ricardo Perez S.A.; Mark Tupper; National Geographic Channel; Smithsonian Institution FX This project has been supported by the U.S. NSF (National Science Foundation) PIRE (Partnerships in International Research and Education) grant 0966884 (OISE, EAR, DRL), Autoridad del Canal de Panama contrato SAA-199520-KRP, Ricardo Perez S.A., Mark Tupper, National Geographic Channel, and the Smithsonian Institution. We thank the Direccion de Recursos Minerales of Panama for collecting permits; to George Kamenov of the Department of Geological Sciences and Chanika Symister from the Florida Museum of Natural History of University of Florida, for laboratory help; to Richard Hulbert, Jonathan Bloch, Gary Morgan, Dana Ehret and Aaron Wood for beneficial suggestions about this research. We thank to Jorge Ceballos, Juan Camilo Rojas, Natalia Hoyos, Sebastian Zapata, Andres Baresh and Ruth G. Reina from the Smithsonian Tropical Research Institute for logistical support. Catalina Pimiento thanks Jorge McLaughlin for support. This is University of Florida Contribution to Paleobiology number 642. NR 88 TC 15 Z9 19 U1 1 U2 21 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD MAR PY 2013 VL 42 BP 159 EP 170 DI 10.1016/j.jsames.2012.11.005 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 101GL UT WOS:000315763100014 ER PT J AU Krebs, EC AF Krebs, Edgardo C. TI The Argentine enigma. Preliminary study of Daniel Scarfo SO JOURNAL OF THE HISTORY OF THE BEHAVIORAL SCIENCES LA French DT Book Review C1 [Krebs, Edgardo C.] Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. RP Krebs, EC (reprint author), Smithsonian Inst, NMNH, Dept Anthropol, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-5061 EI 1520-6696 J9 J HIST BEHAV SCI JI J. Hist. Behav. Sci. PD SPR PY 2013 VL 49 IS 2 BP 216 EP U252 PG 3 WC History Of Social Sciences SC Social Sciences - Other Topics GA 116UO UT WOS:000316908700008 ER PT J AU Odling-Smee, J Erwin, DH Palkovacs, EP Feldman, MW Laland, KN AF Odling-Smee, John Erwin, Douglas H. Palkovacs, Eric P. Feldman, Marcus W. Laland, Kevin N. TI NICHE CONSTRUCTION THEORY: A PRACTICAL GUIDE FOR ECOLOGISTS SO QUARTERLY REVIEW OF BIOLOGY LA English DT Review DE niche construction; ecological inheritance; ecosystem engineering; ecoevolutionary feedbacks; ecosystem ecology ID ECOSYSTEM ENGINEERS; ADAPTIVE RADIATION; EVOLUTIONARY CONSEQUENCES; EXTENDED PHENOTYPES; NATURAL-POPULATIONS; RAPID EVOLUTION; DYNAMICS; DIVERSITY; ORGANISMS; SELECTION AB Niche construction theory (NCT) explicitly recognizes environmental modification by organisms ("niche construction") and their legacy over time ("ecological inheritance") to be evolutionary processes in their own right. Here we illustrate how niche construction theory provides useful conceptual tools and theoretical insights for integrating ecosystem ecology and evolutionary theory. We begin by briefly describing NCT, and illustrating how it differs from conventional evolutionary approaches. We then distinguish between two aspects of niche construction-environment alteration and subsequent evolution in response to constructed environments-equating the first of these with "ecosystem engineering." We describe some of the ecological and evolutionary impacts on ecosystems of niche construction, ecosystem engineering, and ecological inheritance, and illustrate how these processes trigger ecological and evolutionary feedbacks and leave detectable ecological signatures that are open to investigation. Finally, we provide a practical guide to how NCT could be deployed by ecologists and evolutionary biologists to explore eco-evolutionary dynamics. We suggest that, by highlighting the ecological and evolutionary ramifications of changes that organisms bring about in ecosystems, NCT helps link ecosystem ecology to evolutionary biology, potentially leading to a deeper understanding of how ecosystems change over time. C1 [Odling-Smee, John] Univ Oxford, Mansfield Coll, Oxford OX1 3TF, England. [Erwin, Douglas H.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Erwin, Douglas H.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Palkovacs, Eric P.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Feldman, Marcus W.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Laland, Kevin N.] Univ St Andrews, Sch Biol, St Andrews KY16 9TS, Fife, Scotland. RP Laland, KN (reprint author), Univ St Andrews, Sch Biol, St Andrews KY16 9TS, Fife, Scotland. EM JOHN.ODLING-SMEE@MANSFIELD.OX.AC.UK; ERWIND@SI.EDU; EPALKOVA@UCSC.EDU; MARC@CHARLES.STANFORD.EDU; KNL1@ST-ANDREWS.AC.UK FU ERC; NIH [GM28016]; NASA Astrobiology Institute FX Research supported in part by an ERC Advanced Grant to Kevin N. Laland, by NIH grant GM28016 to Marcus W. Feldman, and support from the NASA Astrobiology Institute to Douglas H. Erwin. We are grateful to Tobias Uller and Clive Jones for helpful comments on an earlier draft. NR 104 TC 41 Z9 42 U1 11 U2 152 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0033-5770 J9 Q REV BIOL JI Q. Rev. Biol. PD MAR PY 2013 VL 88 IS 1 BP 3 EP 28 PG 26 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 116FK UT WOS:000316868000001 ER PT J AU Julian, JP Davies-Colley, RJ Gallegos, CL Tran, TV AF Julian, Jason P. Davies-Colley, Robert J. Gallegos, Charles L. Tran, Trung V. TI Optical Water Quality of Inland Waters: A Landscape Perspective SO ANNALS OF THE ASSOCIATION OF AMERICAN GEOGRAPHERS LA English DT Article DE aquatic ecosystems; humanenvironment interactions; remote sensing; water resources; watershed science; ecosistemas acuaticos; percepcion remota; recursos hidricos; ciencia de las cuencas hidrograficas ID NEW-ZEALAND RIVERS; RADIOMETRIC NORMALIZATION; ORGANIC-MATTER; SHALLOW LAKES; LAND-USE; CLARITY; STREAMS; SCALE; CONSEQUENCES; WISCONSIN AB Optical water quality (OWQ) relates the composition of waters to their light transmission and thereby light availability for aquatic plants, visual range for aquatic animals, and suitability for recreational uses. This fundamental role of OWQ has led to numerous studies on the optical properties in rivers and lakes, which we overview here with a landscape perspective. International examples illustrate how the kinds and amounts of light-attenuating substances depend on landscape features on scales ranging from the river reach to the orientation of mountain ranges. OWQ is profoundly affected by increased nutrient discharges and sediment mobilization from human activities such as agriculture. Proper monitoring of OWQ is needed to fully understand and address these consequences. Remote sensing has potential for broad-scale surveys of OWQ, although currently its applications to inland waters are limited by low spatial resolution. A better understanding of OWQ will advance water management and remote sensing capabilities, as well as provide further insight into water quality impacts associated with global changes in climate, energy use, and land use. C1 [Julian, Jason P.; Tran, Trung V.] Univ Oklahoma, Dept Geog & Environm Sustainabil, Norman, OK 73019 USA. [Davies-Colley, Robert J.] Natl Inst Water & Atmospher Res, Hamilton, New Zealand. [Gallegos, Charles L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Julian, JP (reprint author), Univ Oklahoma, Dept Geog & Environm Sustainabil, Norman, OK 73019 USA. EM jjuilan@ou.edu; Rob.Davies-Colley@niwa.co.nz; gallegosc@si.edu; trungtv@ou.edu NR 45 TC 9 Z9 9 U1 3 U2 51 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0004-5608 J9 ANN ASSOC AM GEOGR JI Ann. Assoc. Am. Geogr. PD MAR 1 PY 2013 VL 103 IS 2 SI SI BP 309 EP 318 DI 10.1080/00045608.2013.754658 PG 10 WC Geography SC Geography GA 096DC UT WOS:000315383200008 ER PT J AU Bixenmann, RJ Coley, PD Kursar, TA AF Bixenmann, Ryan J. Coley, Phyllis D. Kursar, Tom A. TI Developmental Changes in Direct and Indirect Defenses in the Young Leaves of the Neotropical Tree Genus Inga (Fabaceae) SO BIOTROPICA LA English DT Article DE ant-plant mutualism; defense chemistry; extrafloral nectary; optimal defense; Panama; plant-herbivore interactions ID EXTRAFLORAL NECTAR SECRETION; TRADE-OFFS; ANTIHERBIVORE DEFENSES; LEAF DEVELOPMENT; UMBELLIFERA FABACEAE; CHEMICAL DEFENSES; INDUCED RESPONSES; ANT-PLANTS; L-TYROSINE; HERBIVORY AB Plant fitness is affected by herbivory, and in moist tropical forests, 70 percent of herbivore damage occurs on young leaves. Thus, to understand the effects of herbivory on tropical plant fitness, it is necessary to understand how tropical young leaves survive the brief, but critical, period of susceptibility. In this study, we surveyed three species of Inga during young leaf expansion. Three classes of toxic secondary metabolites (phenolics, saponins, and tyrosine), extrafloral nectar production, leaf area, and extrafloral nectary area were measured at randomly assigned young leaf sizes. In addition, all defenses were compared for potential trade-offs during leaf expansion. No trade-offs among defenses were found, and the concentration of all defenses, except tyrosine, decreased during leaf expansion. We suggest that plants continued to increase phenolic and saponin content, but at a rate that resulted in decreasing concentrations. In contrast, tyrosine content per leaf steadily increased such that a constant concentration was maintained regardless of young leaf size. Nectar production remained constant during leaf expansion, but, because young leaf area increased by tenfold, the investment in extrafloral nectar per leaf area significantly decreased. In addition, nectary area did not change during leaf expansion and therefore the relative size of the nectary significantly decreased during young leaf expansion. These results support the predictions of the optimal defense hypothesis and demonstrate that the youngest leaves have the highest investment in multiple defenses, most likely because they have the highest nitrogen content and are most susceptible to a diversity of herbivores. Resumen El fitness de las plantas se ve afectado por los herbivoros, y en los bosques tropicales humedos, el 70 por ciento del dano por herbivoros se produce en las hojas jovenes. Por lo tanto, con el fin de comprender los efectos de la herbivoria sobre el fintess de las plantas tropicales, es necesario entender como sobreviven las hojas jovenes al breve, pero critico, periodo de susceptibilidad. Se estudiaron tres especies de Inga durante la expansion de las hojas jovenes. Como medida de las defensas, se midieron tres clases de metabolitos secundarios toxicos (fenoles, saponinas y tirosina), la produccion de nectar extraflorales, area foliar y el area de nectarios extraflorales en hojas jovenes seleccionadas al azar. Ademas, todas las defensas fueron comparadas para evaluar posibles compromisos o trade-offs durante la expansion de la hoja. No se encontraron trade-offs entre las defensasevaluadas, y la concentracion de todas las defensas, con excepcion de la tirosina, disminuyocon la expansion de la hoja. Se sugiere que las plantas continuaron aumentando el contenido fenolico y el contenido de saponina, pero a una velocidad menor que dio lugar a concentraciones decrecientes. En contraste, el contenido de tirosina por hoja aumento constantemente de tal manera que su concentracion se mantuvo constante, independientemente del tamano de hojas jovenes. La produccion de nectar se mantuvo constante durante la expansion de las hojas, pero, dado que el area foliar joven aumento 10 veces, la inversion en el nectar extrafloral por area foliar disminuyo significativamente. Ademas, el area del nectario no cambio durante la expansion de la hoja y por lo tanto, el tamano relativo del nectario disminuyo significativamente durante la expansion de las hojas jovenes. Estos resultados demuestran que las hojas mas jovenes tienen una mayor inversion en defensas multiples, muy probablemente debido a que tienen el mayor contenido de nitrogeno y son los mas susceptibles a una gran diversidad de herbivoros. C1 [Bixenmann, Ryan J.; Coley, Phyllis D.; Kursar, Tom A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Bixenmann, Ryan J.; Coley, Phyllis D.; Kursar, Tom A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Bixenmann, RJ (reprint author), Univ Utah, Dept Biol, 257S 1400E, Salt Lake City, UT 84112 USA. EM ryan.bixenmann@montana.edu FU Smithsonian Tropical Research Institute; Sigma Xi; NSF [DEB-0640630, DEB-0234936, OISE-0531803] FX This project was supported by short-term awards from the Smithsonian Tropical Research Institute, a Grants-in-Aid of Research award from Sigma Xi (RJB), and funding from NSF grants DEB-0640630, DEB-0234936, and OISE-0531803 (PDC and TAK). RJB thanks John Lokvam for his help in developing the quantitative chemical analyses. In addition, RJB thanks Erik Murakami for his advice in laboratory analyses. The authors also thank M. Denise Dearing, Don Feener Jr., Colleen Farmer, Johanna Varner, and two anonymous reviewers for their comments on this manuscript. The field portion of this study complies with the current laws of the Autoridad Nacional del Ambiente de la Republica de Panama. NR 56 TC 4 Z9 4 U1 12 U2 79 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2013 VL 45 IS 2 BP 175 EP 184 DI 10.1111/j.1744-7429.2012.00914.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 099TE UT WOS:000315643900004 ER PT J AU Gowda, V Kress, WJ AF Gowda, Vinita Kress, W. John TI A Geographic Mosaic of PlantPollinator Interactions in the Eastern Caribbean Islands SO BIOTROPICA LA English DT Article DE adaptation; coevolution; Eulampis jugularis; geographic mosaic of coevolution; phenology; pollination; visitation frequency; visitation rate ID PURPLE-THROATED CARIBS; HERMIT HUMMINGBIRDS; IPOMOPSIS-AGGREGATA; EULAMPIS-JUGULARIS; NECTAR PRODUCTION; FLORAL NECTAR; PLANT; PATTERNS; COEVOLUTION; VARIABILITY AB The interplay between generalized and specialized plantanimal interactions is a core concept in understanding the evolution of mutualisms. Within the Eastern Caribbean, Heliconia bihai is a dominant forest species in the southern island of St. Vincent where H. caribaea is virtually absent. Heliconia caribaea is most common on the northern island of St. Kitts where H. bihai is restricted to the tops of the highest peaks. Both species are abundant on the central island of Dominica. We compared flowering patterns, nectar characteristics, and visitation frequency of hummingbirds in the two heliconias on the three islands to determine the extent of geographic variations in this plantpollinator mutualism. The peak flowering season of the two heliconias was observed to be in AprilMay on all three islands with little within- and between-island variations. Nectar production significantly varied between species and between islands. Visitation patterns by the principal hummingbird pollinators also varied between the islands: (1) on Dominica, only females of a single species of hummingbird pollinated the flowers of H. bihai (sexual specialization), whereas both sexes of the same hummingbird pollinated the flowers of H. caribaea (species specialization); (2) on St. Vincent, both sexes of the same hummingbird pollinated the flowers of H. bihai (species specialization); and (3) on St. Kitts, only females pollinated the flowers of H. bihai (sexual specialization), whereas several species of hummingbird visited the flowers of H. caribaea (species generalization). We propose that the Heliconiahummingbird interactions in the Eastern Caribbean represent a geographically variable coevolutionary mosaic of plantpollinator interactions. C1 [Gowda, Vinita] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Gowda, Vinita; Kress, W. John] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Gowda, V (reprint author), George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. EM gowda@gwmail.gwu.edu FU Department of Biological Sciences, The George Washington University; Cosmos Club; Sigma-Xi; Smithsonian Institution; National Science Foundation [DEB-0614218] FX This study was supported by a Weintraub Graduate Fellowship from the Department of Biological Sciences, The George Washington University to VG and also by the Cosmos Club, Sigma-Xi, and Smithsonian Institution to VG. Fieldwork for this study was supported by grants from National Science Foundation (DEB-0614218) to E. J. Temeles and W. J. Kress. NR 51 TC 3 Z9 3 U1 5 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAR PY 2013 VL 45 IS 2 BP 224 EP 235 DI 10.1111/j.1744-7429.2012.00915.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 099TE UT WOS:000315643900010 ER PT J AU Ross, C Ritson-Williams, R Olsen, K Paul, VJ AF Ross, C. Ritson-Williams, R. Olsen, K. Paul, V. J. TI Short-term and latent post-settlement effects associated with elevated temperature and oxidative stress on larvae from the coral Porites astreoides SO CORAL REEFS LA English DT Article DE Coral recruitment; Larval ecology; Oxidative stress; Settlement; Thermal stress; Latent effects ID HYDROGEN-PEROXIDE; SCLERACTINIAN CORAL; CARIBBEAN CORALS; STAGHORN CORALS; CLIMATE-CHANGE; REEF CORALS; SETTLEMENT; REGION; LIGHT; PHOTOSYNTHESIS AB Coral reefs across the Caribbean are undergoing unprecedented rates of decline in coral cover during the last three decades, and coral recruitment is one potential process that could aid the recovery of coral populations. To better understand the effects of climate change on coral larval ecology, the larvae of Porites astreoides were studied to determine the immediate and post-settlement effects of elevated temperature and associated oxidative stress. Larvae of Porites astreoides were exposed to 27 A degrees C (ambient) and +3.0 A degrees C (elevated temperature) seawater for a short duration of 24 h; then, a suite of physiological parameters were measured to determine the extent of sublethal stress. Following the +3.0 A degrees C treatment, larvae did not show a significant difference in maximum quantum yield of PSII (F (v)/F (m)) or respiratory demand when compared to controls maintained at 27 A degrees C. The addition of micromolar concentrations of hydrogen peroxide did not impact respiration or photochemical efficiency. Catalase activity in the larvae increased (> 60 %) following exposure to elevated temperature when compared to the controls. Short-term larval survival and settlement and metamorphosis were not affected by increased temperature or the H2O2 treatment. However, the settled spat that were exposed to elevated temperature underwent a 99 % reduction in survival compared to 90 % reduction for the control spat when examined 24 days following the deployment of 4-day-old settled spat on settlement tiles in the field. These results show that short-term exposure to some stressors might have small impacts on coral physiology, and no effects on larval survival, settlement and metamorphosis. However, due to post-settlement mortality, these stressors can cause a significant reduction in coral recruitment. C1 [Ross, C.; Olsen, K.] Univ N Florida, Dept Biol, Jacksonville, FL 32224 USA. [Ritson-Williams, R.; Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Ross, C (reprint author), Univ N Florida, Dept Biol, 1 UNF Dr, Jacksonville, FL 32224 USA. EM cliff.ross@unf.edu RI Ross, Cliff/B-8291-2011 FU University of North Florida's "Transformational Learning Opportunity" program; Mote Protect our Reefs Grant [2009-16]; Smithsonian Marine Science Network FX We thank Tom Bartlett, Erin Hoover, Angela Virgilio and Angela Davis for assistance with coral collection and larval husbandry. We also thank Erich Bartels for field assistance. This work was conducted under permit no. FKNMS-2010-023 issued by the Florida Keys National Marine Sanctuary. This work was supported by the University of North Florida's "Transformational Learning Opportunity" program. VP and RRW were supported by Mote Protect our Reefs Grant 2009-16 and the Smithsonian Marine Science Network. This is contribution #891 of the Smithsonian Marine Station at Ft. Pierce. NR 52 TC 12 Z9 12 U1 2 U2 57 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 2013 VL 32 IS 1 BP 71 EP 79 DI 10.1007/s00338-012-0956-2 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 104TQ UT WOS:000316018600009 ER PT J AU Becker, NI Encarnacao, JA Tschapka, M Kalko, EKV AF Becker, N. I. Encarnacao, J. A. Tschapka, M. Kalko, E. K. V. TI Energetics and life-history of bats in comparison to small mammals SO ECOLOGICAL RESEARCH LA English DT Article DE Ecophysiology; Compensation; Energy-saving mechanisms; Respirometry; Energy demand ID BASAL METABOLIC-RATE; MALE DAUBENTONS BATS; PLECOTUS-AURITUS; ENERGY BUDGETS; MYOTIS-DAUBENTONII; SEASONAL-VARIATION; BROWN BAT; WATER-BALANCE; LIVING FAST; GROWTH-RATE AB Mammals can be aligned along a slow-fast life-history continuum and a low-high metabolic rate continuum based on their traits. Small non-volant mammals occupy the fast/high end in both continua with high reproductive rates and short life spans linked with high mass-specific metabolic rates. Bats occupy the high end of the metabolic continuum, but the slow end of the life-history continuum with low reproductive rates and long life spans. Typically, both continua are linked, and similar life-history traits of species are reflected in more similar metabolic rates. We therefore hypothesized that metabolic rates are similar in species with similar life-history traits. Resting metabolic rates (RMR) were measured for three ecologically and morphologically similar sympatric bat species (Myotis nattereri, M. bechsteinii, and Plecotus auritus; Vespertilionidae) and compared to data from other similar-sized, temperate insectivorous mammals with other life-history strategies. The bat species share similar life-histories and RMRs, both of which differ from the remaining mammals and therefore supporting our hypothesis. To verify that bats are similar in RMR, two energetically contrasting periods were compared. RMRs in post-lactating females did not differ between bat species. It was, however, positively correlated with parasite load in both Myotis species. However, RMRs differed during energy-demanding pregnancy where M. nattereri had the significantly lowest RMR, suggesting metabolic compensation as an energy-saving strategy. We conclude that the energy requirements of bat species with similar life-history traits resemble each other during periods of low energetic demands and are more similar to each other than to other small temperate mammals. C1 [Becker, N. I.; Tschapka, M.; Kalko, E. K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Becker, N. I.; Encarnacao, J. A.] Univ Giessen, Mammalian Ecol Grp, Dept Anim Ecol & Syst, D-35390 Giessen, Germany. [Tschapka, M.; Kalko, E. K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Becker, NI (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM nina.becker@uni-ulm.de FU Landesgraduiertenforduierung Baden- Wurttemberg FX We thank all who contributed to this manuscript and made data acquisition possible. Special thanks go to D. Bethel for improvement of the English. The study was supported by a stipend of the Landesgraduiertenforduierung Baden- Wurttemberg to N. I. Becker. The experiments performed in this study comply with the current laws of Germany. The permissions were issued by the Regional Council of Giessen.. Experiments followed the "Guiding principles in the care and use of animals'' approved by the Council of the American Physiological Society. NR 94 TC 8 Z9 8 U1 3 U2 63 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 0912-3814 J9 ECOL RES JI Ecol. Res. PD MAR PY 2013 VL 28 IS 2 BP 249 EP 258 DI 10.1007/s11284-012-1010-0 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 104OB UT WOS:000316002800014 ER PT J AU Zimmermann, A Schinn, DS Francke, T Elsenbeer, H Zimmermann, B AF Zimmermann, Alexander Schinn, Dustin S. Francke, Till Elsenbeer, Helmut Zimmermann, Beate TI Uncovering patterns of near-surface saturated hydraulic conductivity in an overland flow-controlled landscape SO GEODERMA LA English DT Article DE Soil hydrology; Saturated hydraulic conductivity; Overland flow generation; Spatial patterns; Drainage network ID RAIN-FOREST CATCHMENT; SOIL PHYSICAL-PROPERTIES; BARRO COLORADO ISLAND; SPATIAL VARIABILITY; STORMFLOW GENERATION; RUNOFF; MANAGEMENT; PASTURE; ENGLAND; PLAIN AB Saturated hydraulic conductivity (K-s) is an important soil characteristic affecting soil water storage, runoff generation and erosion processes. In some areas where high-intensity rainfall coincides with low K-s values at shallow soil depths, frequent overland flow entails dense drainage networks. Consequently, linear structures such as flowlines alternate with inter-flowline areas. So far, investigations of the spatial variability of K-s mainly relied on isotropic covariance models which are unsuitable to reveal patterns resulting from linear structures. In the present study, we applied two sampling approaches so as to adequately characterize K-s spatial variability in a tropical forest catchment that features a high density of flowlines: A classical nested sampling survey and a purposive sampling strategy adapted to the presence of flowlines. The nested sampling approach revealed the dominance of small-scale variability, which is in line with previous findings. Our purposive sampling, however, detected a strong spatial gradient: surface K-s increased substantially as a function of distance to flowline; 10 m off flowlines, values were similar to the spatial mean of K-s. This deterministic trend can be included as a fixed effect in a linear mixed modeling framework to obtain realistic spatial fields of K-s. In a next step we used probability maps based on those fields and prevailing rainfall intensities to assess the hydrological relevance of the detected pattern. This approach suggests a particularly good agreement between the probability statements of K-s exceedance and observed overland flow occurrence during wet stages of the rainy season. (c) 2012 Elsevier B.V. All rights reserved. C1 [Zimmermann, Alexander; Schinn, Dustin S.; Francke, Till; Elsenbeer, Helmut; Zimmermann, Beate] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zimmermann, A (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. EM alexander.zimmermann.ii@uni-potsdam.de RI Zimmermann, Alexander/B-6831-2011 FU German Research Foundation [El 255/6-1]; German Academic Exchange Service fellowship [D/10/12554]; Smithsonian Tropical Research Institute FX This research was partially funded by the German Research Foundation (El 255/6-1). Dustin S. Schinn acknowledges support from a German Academic Exchange Service fellowship (D/10/12554), and Helmut Elsenbeer acknowledges support by the Smithsonian Tropical Research Institute during his sabbatical in 2008. Furthermore, we thank Anna Schurkmann, Lena Katharina Schmidt, Simon Plate, and Sophie Godow for participating in the field work, Andreas Papritz (ETH Zurich) for providing the R-code used in the nested sampling analysis, Oris Acevedo (Smithsonian Tropical Research Institute, STRI) for logistical support, and Sergio dos Santos (Environmental Sciences Program, STRI) for providing long-term rainfall data. Finally, we thank two anonymous reviewers for their constructive comments. NR 53 TC 14 Z9 15 U1 1 U2 74 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 J9 GEODERMA JI Geoderma PD MAR PY 2013 VL 195 BP 1 EP 11 DI 10.1016/j.geoderma.2012.11.002 PG 11 WC Soil Science SC Agriculture GA 108PF UT WOS:000316307200001 ER PT J AU Reddy, V Le Corre, L O'Brien, DP Nathues, A Cloutis, EA Durda, DD Bottke, WF Bhatt, MU Nesvorny, D Buczkowski, D Scully, JEC Palmer, EM Sierks, H Mann, PJ Becker, KJ Beck, AW Mittlefehldt, D Li, JY Gaskell, R Russell, CT Gaffey, MJ McSween, HY McCord, TB Combe, JP Blewett, D AF Reddy, Vishnu Le Corre, Lucille O'Brien, David P. Nathues, Andreas Cloutis, Edward A. Durda, Daniel D. Bottke, William F. Bhatt, Megha U. Nesvorny, David Buczkowski, Debra Scully, Jennifer E. C. Palmer, Elizabeth M. Sierks, Holger Mann, Paul J. Becker, Kris J. Beck, Andrew W. Mittlefehldt, David Li, Jian-Yang Gaskell, Robert Russell, Christopher T. Gaffey, Michael J. McSween, Harry Y. McCord, Thomas B. Combe, Jean-Philippe Blewett, David TI Delivery of dark material to Vesta via carbonaceous chondritic impacts (vol 221, pg 544, 2012) SO ICARUS LA English DT Correction C1 [Reddy, Vishnu; Le Corre, Lucille; Nathues, Andreas; Bhatt, Megha U.; Sierks, Holger] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Reddy, Vishnu; Gaffey, Michael J.] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA. [O'Brien, David P.; Gaskell, Robert] Planetary Sci Inst, Tucson, AZ USA. [Cloutis, Edward A.; Mann, Paul J.] Univ Winnipeg, Dept Geog, Winnipeg, MB R3B 2E9, Canada. [Durda, Daniel D.; Bottke, William F.; Nesvorny, David] SW Res Inst, Boulder, CO USA. [Buczkowski, Debra; Blewett, David] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Scully, Jennifer E. C.; Palmer, Elizabeth M.; Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Becker, Kris J.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Beck, Andrew W.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC USA. [Mittlefehldt, David] NASA, Astromat Res Off, Johnson Space Ctr, Houston, TX USA. [Li, Jian-Yang] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN USA. [McCord, Thomas B.; Combe, Jean-Philippe] Bear Fight Inst, Winthrop, WA USA. RP Reddy, V (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. EM reddy@mps.mpg.de RI Blewett, David/I-4904-2012; Beck, Andrew/J-7215-2015 OI Blewett, David/0000-0002-9241-6358; Beck, Andrew/0000-0003-4455-2299 NR 1 TC 0 Z9 0 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 2013 VL 223 IS 1 BP 632 EP 632 DI 10.1016/j.icarus.2012.10.006 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 104FP UT WOS:000315977600049 ER PT J AU Jaramillo, C Zavada, M Ortiz, J Pardo, A Ochoa, D AF Jaramillo, Carlos Zavada, Michael Ortiz, John Pardo, Andres Ochoa, Diana TI THE BIOGEOGRAPHY OF THE ARAUCARIAN DISPERSED POLLEN CYCLUSPHAERA SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Araucariaceae; biogeography; Cyclusphaera; Gondwana; paleoenvironment ID NORTHERN SOUTH-AMERICA; CERREJON FORMATION; LLANOS FOOTHILLS; PALEOCENE; ARGENTINA; COLOMBIA; DIVERSIFICATION; PALYNOLOGY; DIVERSITY; CLIMATE AB The pollen genus Cyclusphaera was first described from the Campanian of Peru. The distinctive pollen is spherical to ovoid and disc shaped, with two large openings, resembling pores, opposite each other on the pollen grain. We emend the description of Cyclusphaera scabrata from the Cenozoic of northern South America, based on new data from transmission electron and scanning electron microscopy. The worldwide spatial and temporal distributions of Cyclusphaera are examined. This taxon originated in midlatitudes in the Southern Hemisphere (Gondwana) and subsequently expanded its distribution to higher and lower latitudes, reaching a maximum latitudinal and longitudinal distribution by the middle Cretaceous. Following the Cretaceous, Cyclusphaera was extirpated from middle and high latitudes during the late Cretaceous and Paleogene while increasing its frequency in the tropics during the Cenozoic in both Africa and South America. By the Oligocene, Cyclusphaera was a common element of palynofloras in Colombia and Venezuela. During the Neogene, the distribution in tropical South America became restricted, with the youngest record occurring in the late Miocene of western Colombia. The overall biogeographic pattern of Cyclusphaera is similar to that of Podocarpaceae, one of the most persistent gymnosperm families in the tropics. The extinction of Cyclusphaera could be related to the increase in aridity and expansion of savanna habitats in the northern tropics of South America during the Neogene. C1 [Jaramillo, Carlos; Ortiz, John] Smithsonian Trop Res Inst, Panama City, Panama. [Zavada, Michael] Seton Hall Univ, S Orange, NJ 07079 USA. [Pardo, Andres; Ochoa, Diana] Univ Caldas, Manizales, Colombia. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM jaramilloc@si.edu OI Ochoa, Diana/0000-0001-6242-4202 FU Smithsonian Paleobiology Endowment Fund [NSF EAR 0957679]; Yale University Edward P. Bass Distinguished Visiting Environmental Scholars Program; National Hydrocarbon Agency from Colombia FX This project was supported by the Smithsonian Paleobiology Endowment Fund, NSF EAR 0957679, and the Yale University Edward P. Bass Distinguished Visiting Environmental Scholars Program. Thanks to the biostratigraphy team at both the Colombian Petroleum Institute and the Smithsonian Tropical Research Institute. Thanks to the National Hydrocarbon Agency from Colombia for supporting the research in western Colombia. Special thanks go to M. I. Barreto for her continuous support and ideas. NR 71 TC 3 Z9 4 U1 1 U2 11 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD MAR-APR PY 2013 VL 174 IS 3 SI SI BP 489 EP 498 DI 10.1086/668869 PG 10 WC Plant Sciences SC Plant Sciences GA 106EO UT WOS:000316125700018 ER PT J AU Stull, GW Labandeira, CC Dimichele, WA Chaney, DS AF Stull, Gregory W. Labandeira, Conrad C. Dimichele, William A. Chaney, Dan S. TI THE "SEEDS" ON PADGETTIA READI ARE INSECT GALLS: REASSIGNMENT OF THE PLANT TO ODONTOPTERIS, THE GALL TO OVOFOLIGALLITES N. GEN., AND THE EVOLUTIONARY IMPLICATIONS THEREOF SO JOURNAL OF PALEONTOLOGY LA English DT Article ID NORTH-CENTRAL TEXAS; PALEOZOIC ICE-AGE; PENNSYLVANIAN SPECIMENS; ASSOCIATIONS; USA; HOLOMETABOLA; TRANSITION; ARTHROPOD; ILLINOIS; HISTORY AB The Early Permian (Asselian) Euramerican plant Padgettia readi Mamay is reassigned to Odontopteris Brongniart, as O. readi (Mamay) Stull et al. n. comb. Distinctive elongate structures on neuropteroid pinnules of this plant, previously interpreted as fructifications, are herein reinterpreted as foliar histoid galls, structurally analogous to blister or vein galls, and probably induced by an early lineage of hemipterans or mites. These distinctive features are assigned to the new gall ichnogenus Ovofoligallites Labandeira, n. ichnogen. n. ichnosp, as O. padgetti Labandeira. The Early Permian association between an Odontopteris host and Ovofoligallites gallers probably originated during the Middle Pennsylvanian as a similar, antecedent association between Macroneuropteris scheuchzeri (Hoffmann) Cleal, Shute, and Zodrow and the maker of U-shaped surface features long known as a distinctive, unattributed damage type, but now recognizable as a likely gall. The persistence of this association between the galler and certain medullosan pteridosperms into the Permian adds to the morphological richness of the Permian galler insect fauna. The Permian ecological expansion of galling insects resulted in colonization of new host plants, primarily through a shift from the consumption of entire, mostly pteridophyte axial organs during the Pennsylvanian to the partitioning of seed plant tissues in leaves and small branches in the Permian. The Ovofoligallites galler was part of a diverse Permian galler guild involving a variety of plant taxa, organs and tissues that overwhelmingly targeted multiple lineages of seed plants. C1 [Stull, Gregory W.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Stull, Gregory W.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Labandeira, Conrad C.; Dimichele, William A.; Chaney, Dan S.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. RP Stull, GW (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM gwstull@gmail.com FU Natural History Research Experiences internship program; National Museum of Natural History; NMNH; SI Endowment Funds FX GS acknowledges support from the Natural History Research Experiences internship program, funded by the National Museum of Natural History. WD acknowledges support from the NMNH Small Grants Program and the SI Endowment Funds. F. Marsh expertly drafted the figures. This is contribution 252 of the Evolution of Terrestrial Ecosystems consortium at the National Museum of Natural History. The authors thank J. Genise and an anonymous reviewer for their suggestions to the manuscript. NR 86 TC 7 Z9 7 U1 2 U2 9 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAR PY 2013 VL 87 IS 2 BP 217 EP 231 PG 15 WC Paleontology SC Paleontology GA 106TB UT WOS:000316166500005 ER PT J AU Korth, WW Emry, RJ AF Korth, William W. Emry, Robert J. TI PIPESTONEOMYIDAE, A NEW FAMILY OF FOSSIL RODENTS (MAMMALIA) FROM THE DUCHESNEAN (LATE MIDDLE EOCENE, BARTONIAN) TO ORELLAN (EARLY OLIGOCENE, PRIABONIAN) OF NORTH AMERICA SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Additional specimens of the problematical rodent Pipestoneomys Donahoe, 1956, have allowed for recognition of a new family, Pipestoneomyidae. A new genus and species of pipestoneomyid is recognized from the late middle Eocene (Duchesnean North American Land Mammal Age; Bartonian), Argorheomys septendrionalis, which is morphologically more primitive than Pipestoneomys and demonstrates that this new family has been distinct since the Duchesnean. The Pipestoneomyidae share a number of derived characters with the Geomorpha, especially the two-part inner layer of incisor enamel of the Eoymidae. The Pipestoneomyidae differ from the Eomyidae in lacking the basic "omega" pattern of the cheek teeth of the former, so are in the Eomyoidea as a distinct family. C1 [Korth, William W.] Rochester Inst Vertebrate Paleontol, Rochester, NY 14610 USA. [Emry, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Korth, WW (reprint author), Rochester Inst Vertebrate Paleontol, 265 Carling Rd, Rochester, NY 14610 USA. EM wwkorth@frontiernet.net; emryr@si.edu NR 30 TC 0 Z9 0 U1 0 U2 3 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD MAR PY 2013 VL 87 IS 2 BP 289 EP 296 PG 8 WC Paleontology SC Paleontology GA 106TB UT WOS:000316166500011 ER PT J AU Shen, Y Santiago, LS Ma, L Lin, GJ Lian, JY Cao, HL Ye, WH AF Shen, Yong Santiago, Louis S. Ma, Lei Lin, Guo-Jun Lian, Ju-Yu Cao, Hong-Lin Ye, Wan-Hui TI Forest dynamics of a subtropical monsoon forest in Dinghushan, China: recruitment, mortality and the pace of community change SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE forest dynamics; population trends; size-class distributions; spatial patterns; subtropical forest; tree mortality ID TROPICAL FOREST; TREE MORTALITY; JANZEN-CONNELL; RAIN-FOREST; GROWTH; MODEL; DISTRIBUTIONS; ENVIRONMENTS; BIODIVERSITY; COMPETITION AB Structure and demographics in many tropical forests is changing, but the causes of these changes remain unclear. We studied 5 y (2005-2010) of species turnover, recruitment, mortality and population change data from a 20-ha subtropical forest plot in Dinghushan, China, to identify trends in forest change, and to test whether tree mortality is associated with intraspecific or interspecific competition. We found the Dinghushan forest to be more dynamic than one temperate and two tropical forests in a comparison of large, long-term forest dynamics plots. Within Dinghushan, size-class distributions were bell-shaped only for the three most dominant species and reverse J-shaped for other species. Bell-shaped population distributions can indicate a population in decline, but our data suggest that these large and long-lived species are not in decline because the pattern is driven by increasing probabilities of transition to larger size class with increasing size and fast growth in saplings. Spatially aggregated tree species distributions were common for surviving and dead individuals. Competitive associations were more frequently intraspecific than interspecific. The competition that induced tree mortality was more associated with intraspecific than interspecific interactions. Intraspecific competitive exclusion and density-dependence appear to play important roles in tree mortality in this subtropical forest. C1 [Shen, Yong; Ma, Lei; Lin, Guo-Jun; Lian, Ju-Yu; Cao, Hong-Lin; Ye, Wan-Hui] Chinese Acad Sci, Key Lab Vegetat Restorat & Management Degraded Ec, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Shen, Yong; Ma, Lei; Lin, Guo-Jun] Univ Chinese Acad Sci, Beijing 10049, Peoples R China. [Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ye, WH (reprint author), Chinese Acad Sci, Key Lab Vegetat Restorat & Management Degraded Ec, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. EM why@scbg.ac.cn RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU National Natural Science Foundation of China [31061160188-02, 31011120470-02, 31100312]; Knowledge Innovation Project of the Chinese Academy of Sciences [KZCX-YW-430-03]; Chinese Forest Biodiversity Monitoring Network FX We thank many individuals in South China Botanical Garden who contributed to the field survey of Dinghushan plot, and the Center for Tropical Forest Science and Smithsonian Tropical Research Institute for data support. The study was funded by National Natural Science Foundation of China (31061160188-02), Knowledge Innovation Project of the Chinese Academy of Sciences (KZCX-YW-430-03), the National Natural Science Foundation of China (31011120470-02), National Natural Science Foundation of China (31100312) and Chinese Forest Biodiversity Monitoring Network. NR 39 TC 10 Z9 14 U1 4 U2 51 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD MAR PY 2013 VL 29 BP 131 EP 145 DI 10.1017/S0266467413000059 PN 2 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 108FT UT WOS:000316277900005 ER PT J AU Zotz, G Winkler, U AF Zotz, Gerhard Winkler, Uwe TI Aerial roots of epiphytic orchids: the velamen radicum and its role in water and nutrient uptake SO OECOLOGIA LA English DT Article DE Cation exchange capacity; Epiphytes; Phosphorus; Potassium ID HIGHLY EFFICIENT UPTAKE; VASCULAR EPIPHYTES; BROMELIADS; POTASSIUM; DIVERSITY; FOREST AB The velamen radicum, a spongy, usually multiple epidermis of the roots, which at maturity consists of dead cells, is frequently described as an important adaptation of epiphytic orchids. Yet, quantitative evidence for the alleged functions, e.g., efficient water and nutrient uptake, nutrient retention, reduction of water loss, mechanical protection, or the avoidance of overheating, is rare or missing. We tested the notion originally put forward by Went in 1940 that the velamen allows plants to capture and immobilize the first solutions arriving in a rainfall, which are the most heavily charged with nutrients. In a series of experiments, we examined whether all necessary functional characteristics are given for this scenario to be realistic under ecological conditions. First, we show that the velamen of a large number of orchid species takes up solutions within seconds, while evaporation from the velamen takes several hours. Charged ions are retained in the velamen probably due to positive and negative charges in the cell walls, while uncharged compounds are lost to the external medium. Finally, we demonstrate that nutrient uptake follows biphasic kinetics with a highly efficient, active transport system at low external concentrations. Thus, our results lend strong support to Went's hypothesis: the velamen fulfills an important function in nutrient uptake in the epiphytic habitat. Most of the other functions outlined above still await similar experimental scrutiny. C1 [Zotz, Gerhard; Winkler, Uwe] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 39 TC 12 Z9 13 U1 7 U2 68 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAR PY 2013 VL 171 IS 3 SI SI BP 733 EP 741 DI 10.1007/s00442-012-2575-6 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 109BK UT WOS:000316339900012 PM 23292456 ER PT J AU Turner, S AF Turner, Steven TI Reconstructions: Recreating Science and Technology of the Past SO SCIENCE & EDUCATION LA English DT Book Review C1 [Turner, Steven] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Turner, S (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. EM turners@si.edu NR 1 TC 0 Z9 0 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0926-7220 J9 SCI EDUC-NETHERLANDS JI Sci. Educ. PD MAR PY 2013 VL 22 IS 3 BP 733 EP 736 DI 10.1007/s11191-012-9462-8 PG 4 WC Education & Educational Research; History & Philosophy Of Science SC Education & Educational Research; History & Philosophy of Science GA 109JN UT WOS:000316363400016 ER PT J AU Wilke, T Haase, M Hershler, R Liu, HP Misof, B Ponder, W AF Wilke, Thomas Haase, Martin Hershler, Robert Liu, Hsiu-Ping Misof, Bernhard Ponder, Winston TI Pushing short DNA fragments to the limit: Phylogenetic relationships of 'hydrobioid' gastropods (Caenogastropoda: Rissooidea) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Gastropoda; Rissooidea; Hydrobiidae; Systematics; Structural alignment; Phylogenetic signal; Long-branch attraction ID MULTIPLE SEQUENCE ALIGNMENTS; RIBOSOMAL-RNA SEQUENCES; LONG-BRANCH ATTRACTION; LSU RDNA SEQUENCES; ERHAIA GASTROPODA; CHINA GASTROPODA; MOLECULAR SYSTEMATICS; TRICULINAE GASTROPODA; TEMPERATE AUSTRALIA; EVOLUTIONARY TREES AB Although phylogenetic studies are increasingly utilizing multi-locus datasets, a review of GenBank data for the Gastropoda indicates a strong bias towards a few short gene fragments (most commonly COI, LSU rRNA, and SSU rRNA). This is particularly the case for the Rissooidea, one of the largest and most taxonomically difficult gastropod superfamilies. Here we analyze fragments of these three genes from 90 species to determine whether they can well resolve higher relationships within this superfamily, whether structurally aligned sequence datasets increase phylogenetic signal, and whether the inclusion of highly variable regions introduces noise. We also used the resulting phylogenetic data in combination with morphological/anatomical evidence to re-evaluate the taxonomic status of 'hydrobioid' family-level groups. Our results indicate that all three of the alignment strategies that were used resulted in phylogenies having similar signal levels. However, there was a slight advantage to using structural alignment for inferring family-level relationships. Moreover, the set of 'standard' gastropod genes supported recognition of many previously recognized families and provides new insight into the systematics of several problematic groups. However, some family-group taxa were unresolved and the relationships among families were also poorly supported, suggesting a need for more extensive sampling and inclusion of additional genes. (C) 2012 Elsevier Inc. All rights reserved. C1 [Wilke, Thomas] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Haase, Martin] Ernst Moritz Arndt Univ Greifswald, Zool Inst & Museum, Vogelwarte Hiddensee, D-17489 Greifswald, Germany. [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll Denver, Dept Biol, Denver, CO 80217 USA. [Misof, Bernhard] Zool Forschungsinst, D-53113 Bonn, Germany. [Misof, Bernhard] Museum A Koenig, D-53113 Bonn, Germany. [Ponder, Winston] Australian Museum, Sydney, NSW 2010, Australia. RP Wilke, T (reprint author), Univ Giessen, Dept Anim Ecol & Systemat, Heinrich Buff Ring 26-32 IFZ, D-35392 Giessen, Germany. EM tom.wilke@allzool.bio.uni-giessen.de RI Haase, Martin/G-5034-2012; Wilke, Thomas/G-1517-2012 OI Wilke, Thomas/0000-0001-8263-7758 FU German Science Foundation [WI 1902/8-1, WI 1902/8-2, HA 4752/2-1] FX The study was, in part, supported by grants of the German Science Foundation (WI 1902/8-1, 2 to TW and HA 4752/2-1 to MH). Our analyses could not have been done without the kind help of many colleagues who provided samples or assistance in determining the species studied (see Appendix A). NR 140 TC 34 Z9 40 U1 1 U2 31 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2013 VL 66 IS 3 BP 715 EP 736 DI 10.1016/j.ympev.2012.10.025 PG 22 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 098MM UT WOS:000315553400011 PM 23142112 ER PT J AU Alda, F Reina, RG Doadrio, I Bermingham, E AF Alda, Fernando Reina, Ruth G. Doadrio, Ignacio Bermingham, Eldredge TI Phylogeny and biogeography of the Poecilia sphenops species complex (Actinopterygii, Poeciliidae) in Central America SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Incomplete lineage sorting; Mesoamerica; Molecular clock; Molecular systematics; Poecilia; Secondary freshwater fishes ID FRESH-WATER FISHES; MITOCHONDRIAL-DNA SEQUENCES; CYTOCHROME-B GENE; MOLECULAR PHYLOGENY; HISTORICAL BIOGEOGRAPHY; EVOLUTIONARY HISTORY; CICHLID FISH; COMPARATIVE PHYLOGEOGRAPHY; ADAPTIVE RADIATION; BAYESIAN-INFERENCE AB We inferred the phylogenetic relationships among members of the Poecilia sphenops species complex to resolve the colonization process and radiation of this group in Central America. We analyzed 2550 base pairs (bp) of mitochondrial DNA (mtDNA), including ATP synthase 6 and 8, cytochrome oxidase subunit I and NADH dehydrogenase subunit 2 genes, and 906 bp of the nuclear S7 ribosomal protein of 86 ingroup individuals from 61 localities spanning most of its distribution from Mexico to Panama. Our mitochondrial data rendered a well-supported phylogeny for the P. sphenops complex that differed with the nuclear data set topology, which did not recover the monophyly of the P. mexicana mitochondrial lineage. Coalescent-based simulations tests indicated that, although hybridization cannot be completely ruled out, this incongruence is most likely due to incomplete lineage sorting in this group, which also showed the widest geographic distribution. A single colonization event of Central America from South America was estimated to have occurred between the early Paleocene and Oligocene (53-22 million years ago). Subsequently, two largely differentiated evolutionary lineages diverged around the Early Oligocene-Miocene (38-13 million years ago), which are considered two separate species complexes: P. sphenops and P. mexicana, which can also be distinguished by their tricuspid and unicuspid inner jaw teeth, respectively. Ultimately, within lineage diversification occurred mainly during the Miocene (22-5 million years ago). All major cladogenetic events predated the final closure of the Isthmus of Panama. The allopatric distribution of lineages together with the long basal internodes suggest that vicariance and long term isolations could be the main evolutionary forces promoting radiation in this group, although dispersal through water barriers might also have occurred. Lastly, our results suggest the need to review the current species distribution and taxonomy of the P. sphenops complex sensu lato. (C) 2012 Elsevier Inc. All rights reserved. C1 [Alda, Fernando; Reina, Ruth G.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Alda, Fernando; Doadrio, Ignacio] CSIC, Museo Nacl Ciencias Nat, Dpto Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. RP Alda, F (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM alda.fernando@gmail.com; reinar@si.edu; mcnd147@mncn.csic.es; bermingham@si.edu OI Doadrio, Ignacio/0000-0003-4863-9711 FU [CGL2010-15231.BOS] FX We are grateful to all the people who assisted in the collection of specimens: P. Garzon-Heydt, F. Morcillo, A. Perdices, M. Pomes and A. de Sostoa. We thank L. Alcaraz for assisting in the laboratory and S. Perea for so many insightful comments while preparing this manuscript. We also thank W. Matamoros for his help identifying specimens and suggestions, I. Martinez-Solano for helpful discussion and the members of the Bermingham lab for critical reading and English revision of the text, especially to: I. Ceron-Souza, S. Lipshutz, S. Picq, O. Puebla, C. Salazar and K. Saltonstall. We are indebted to O. Sanjur for her support during this project and to M. Iturralde-Vinent for discussion while preparing the manuscript. Finally, we wish to thank three anonymous reviewers that with their comments helped improve the manuscript. This study was partially financed by Project CGL2010-15231.BOS to I.D. NR 101 TC 14 Z9 14 U1 0 U2 64 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAR PY 2013 VL 66 IS 3 BP 1011 EP 1026 DI 10.1016/j.ympev.2012.12.012 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 098MM UT WOS:000315553400038 PM 23277160 ER PT J AU Gregoric, M Kiesbuy, HC Lebron, SGQ Rozman, A Agnarsson, I Kuntner, M AF Gregoric, Matjaz Kiesbuey, Heine C. Lebron, Shakira G. Quiones Rozman, Alenka Agnarsson, Ingi Kuntner, Matjaz TI Optimal foraging, not biogenetic law, predicts spider orb web allometry SO NATURWISSENSCHAFTEN LA English DT Article DE Recapitulation theory; Ontogeny; Ontogenetic change; Asymmetry; Optimal foraging; Leucauge venusta ID ONTOGENIC CHANGES; WEAVING SPIDERS; PHYLOGENY; ARANEAE; EVOLUTION; BEHAVIOR; NEPHILIDAE; ASYMMETRY; ARANEOIDEA; PATTERNS AB The biogenetic law posits that the ontogeny of an organism recapitulates the pattern of evolutionary changes. Morphological evidence has offered some support for, but also considerable evidence against, the hypothesis. However, biogenetic law in behavior remains underexplored. As physical manifestation of behavior, spider webs offer an interesting model for the study of ontogenetic behavioral changes. In orb-weaving spiders, web symmetry often gets distorted through ontogeny, and these changes have been interpreted to reflect the biogenetic law. Here, we test the biogenetic law hypothesis against the alternative, the optimal foraging hypothesis, by studying the allometry in Leucauge venusta orb webs. These webs range in inclination from vertical through tilted to horizontal; biogenetic law predicts that allometry relates to ontogenetic stage, whereas optimal foraging predicts that allometry relates to gravity. Specifically, pronounced asymmetry should only be seen in vertical webs under optimal foraging theory. We show that, through ontogeny, vertical webs in L. venusta become more asymmetrical in contrast to tilted and horizontal webs. Biogenetic law thus cannot explain L. venusta web allometry, but our results instead support optimization of foraging area in response to spider size. C1 [Gregoric, Matjaz; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kiesbuey, Heine C.; Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT USA. [Lebron, Shakira G. Quiones] Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA. [Rozman, Alenka] Univ Ljubljana, Dept Biol, Biotech Fac, Ljubljana, Slovenia. [Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Gregoric, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. EM matjaz.gregoric@gmail.com FU Slovenian Research Agency [P1-0236, J1-2063]; Slovene Human Resources Development and Scholarship Fund [11010-50/2010]; National Science Foundation [DEB-1050187-1050253] FX We thank Laura May-Collado, Arian Avalos, and Mayte Avalos for logistic help, and Simona Kralj-Fiser for help in statistical analysis. This work was supported by the Slovenian Research Agency (grants P1-0236, J1-2063 to MK), the Slovene Human Resources Development and Scholarship Fund (grant 11010-50/2010 to MG), and National Science Foundation (DEB-1050187-1050253 to IA). NR 43 TC 4 Z9 4 U1 4 U2 46 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD MAR PY 2013 VL 100 IS 3 BP 263 EP 268 DI 10.1007/s00114-013-1015-8 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 104PI UT WOS:000316006200008 PM 23354758 ER PT J AU Miller, DS Gingerich, JAM AF Miller, D. Shane Gingerich, Joseph A. M. TI Regional variation in the terminal Pleistocene and early Holocene radiocarbon record of eastern North America SO QUATERNARY RESEARCH LA English DT Article DE Younger Dryas; Eastern North America; Paleoindians; Radiocarbon dating ID EXTRATERRESTRIAL IMPACT HYPOTHESIS; TEMPORAL FREQUENCY-DISTRIBUTIONS; DATA QUANTITATIVE STRATEGIES; COLONIZATION FRONT SPEEDS; YOUNGER DRYAS; CLIMATE-CHANGE; PROBABILITY-DISTRIBUTIONS; PALEOINDIAN POPULATION; PREHISTORIC DEMOGRAPHY; EVENT DENSITIES AB In this paper we use radiocarbon dates to evaluate the signature of the Younger Dryas Chronozone (YDC) in eastern North America. Using an approach that examines radiocarbon dates by region, we argue that the northeastern United States shows a better overall representation of radiocarbon dates when compared to the Mid-Atlantic and Southeast. These data result in a peak in summed probability distributions during the YDC, which is often interpreted as evidence of population growth. Further examination of these distributions, however, illustrates that differential standard deviations, varying sample size, and the effect of taphonomic and research biases likely overwhelm any demographic signatures in our study sample. Consequently, the frequency of radiocarbon dates by itself is insufficient for understanding the relationship between climate, culture and demography in eastern North America. (c) 2013 University of Washington. Published by Elsevier Inc. All rights reserved. C1 [Miller, D. Shane] Univ Arizona, Sch Anthropol, Tucson, AZ 85721 USA. [Gingerich, Joseph A. M.] NMNH Smithsonian Inst, Dept Anthropol MRC 112, Paleoindian Program, Washington, DC 20560 USA. RP Miller, DS (reprint author), Univ Arizona, Sch Anthropol, 1009 East South Campus Dr,POB 210030, Tucson, AZ 85721 USA. EM dsmiller@email.arizona.edu; GingerichJ@si.edu NR 159 TC 12 Z9 12 U1 2 U2 20 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 EI 1096-0287 J9 QUATERNARY RES JI Quat. Res. PD MAR PY 2013 VL 79 IS 2 BP 175 EP 188 DI 10.1016/j.ygres.2012.12.003 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 101EJ UT WOS:000315757700008 ER PT J AU Fenton, LK Hayward, RK Horgan, BHN Rubin, DM Titus, TN Bishop, MA Burr, DM Chojnacki, M Dinwiddie, CL Kerber, L Le Gall, A Michaels, TI Neakrase, LDV Newman, CE Tirsch, D Yizhaq, H Zimbelman, JR AF Fenton, Lori K. Hayward, Rosalyn K. Horgan, Briony H. N. Rubin, David M. Titus, Timothy N. Bishop, Mark A. Burr, Devon M. Chojnacki, Matthew Dinwiddie, Cynthia L. Kerber, Laura Le Gall, Alice Michaels, Timothy I. Neakrase, Lynn D. V. Newman, Claire E. Tirsch, Daniela Yizhaq, Hezi Zimbelman, James R. TI Summary of the Third International Planetary Dunes Workshop: Remote Sensing and Image Analysis of Planetary Dunes, Flagstaff, Arizona, USA, June 12-15, 2012 SO AEOLIAN RESEARCH LA English DT Review DE Aeolian processes; Bedform dynamics; Bedform morphology; Sand provenance; Meeting summary ID AEOLIAN DUNES; MARS; SANDS AB The Third International Planetary Dunes Workshop took place in Flagstaff, AZ, USA during June 12-15, 2012. This meeting brought together a diverse group of researchers to discuss recent advances in terrestrial and planetary research on aeolian bedforms. The workshop included two and a half days of oral and poster presentations, as well as one formal (and one informal) full-day field trip. Similar to its predecessors, the presented work provided new insight on the morphology, dynamics, composition, and origin of aeolian bedforms on Venus, Earth, Mars, and Titan, with some intriguing speculation about potential aeolian processes on Triton (a satellite of Neptune) and Pluto. Major advancements since the previous International Planetary Dunes Workshop include the introduction of several new data analysis and numerical tools and utilization of low-cost field instruments (most notably the time-lapse camera). Most presentations represented advancement towards research priorities identified in both of the prior two workshops, although some previously recommended research approaches were not discussed. In addition, this workshop provided a forum for participants to discuss the uncertain future of the Planetary Aeolian Laboratory; subsequent actions taken as a result of the decisions made during the workshop may lead to an expansion of funding opportunities to use the facilities, as well as other improvements. The interactions during this workshop contributed to the success of the Third International Planetary Dunes Workshop, further developing our understanding of aeolian processes on the aeolian worlds of the Solar System. (c) 2012 Elsevier B.V. All rights reserved. C1 [Fenton, Lori K.; Michaels, Timothy I.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Hayward, Rosalyn K.; Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Horgan, Briony H. N.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Rubin, David M.] US Geol Survey, Santa Cruz, CA 95060 USA. [Bishop, Mark A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Bishop, Mark A.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Burr, Devon M.; Chojnacki, Matthew] Univ Tennessee, Planetary Geosci Inst, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Dinwiddie, Cynthia L.] SW Res Inst, Geosci & Engn Div, San Antonio, TX 78238 USA. [Kerber, Laura] Univ Paris 06, CNRS, Meteorol Dynam Lab, Paris, France. [Le Gall, Alice] Observ Spati LATMOS UVSQ, Lab Atmospher, Paris, France. [Neakrase, Lynn D. V.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Newman, Claire E.] Ashima Res, Pasadena, CA USA. [Tirsch, Daniela] German Aerosp Ctr DLR, Inst Planetary Res, D-12489 Berlin, Germany. [Yizhaq, Hezi] Ben Gurion Univ Negev, BIDR, Midreshet Ben Gurion, Israel. [Zimbelman, James R.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20013 USA. RP Fenton, LK (reprint author), 189 Bernardo Ave,Ste 100, Mountain View, CA 94043 USA. EM lfenton@carlsagancenter.org RI Chojnacki, Matthew/A-4245-2013; Tirsch, Daniela/I-7916-2012; OI Chojnacki, Matthew/0000-0001-8497-8994; Tirsch, Daniela/0000-0001-5905-5426 NR 71 TC 3 Z9 4 U1 2 U2 17 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 J9 AEOLIAN RES JI Aeolian Res. PD MAR PY 2013 VL 8 BP 29 EP 38 DI 10.1016/j.aeolia.2012.10.006 PG 10 WC Geography, Physical SC Physical Geography GA 095XR UT WOS:000315368800004 ER PT J AU Engene, N Gunasekera, SP Gerwick, WH Paul, VJ AF Engene, Niclas Gunasekera, Sarath P. Gerwick, William H. Paul, Valerie J. TI Phylogenetic Inferences Reveal a Large Extent of Novel Biodiversity in Chemically Rich Tropical Marine Cyanobacteria SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID CF. OSCILLATORIA-MARGARITIFERA; PALMYRA ATOLL CYANOBACTERIA; LYNGBYA-MAJUSCULA; ABSOLUTE STEREOCHEMISTRY; HARMFUL CYANOBACTERIA; CYCLIC DEPSIPEPTIDES; MAXIMUM-LIKELIHOOD; NATURAL-PRODUCTS; DRUG DISCOVERY; CLIMATE-CHANGE AB Benthic marine cyanobacteria are known for their prolific biosynthetic capacities to produce structurally diverse secondary metabolites with biomedical application and their ability to form cyanobacterial harmful algal blooms. In an effort to provide taxonomic clarity to better guide future natural product drug discovery investigations and harmful algal bloom monitoring, this study investigated the taxonomy of tropical and subtropical natural product-producing marine cyanobacteria on the basis of their evolutionary relatedness. Our phylogenetic inferences of marine cyanobacterial strains responsible for over 100 bioactive secondary metabolites revealed an uneven taxonomic distribution, with a few groups being responsible for the vast majority of these molecules. Our data also suggest a high degree of novel biodiversity among natural product-producing strains that was previously overlooked by traditional morphology-based taxonomic approaches. This unrecognized biodiversity is primarily due to a lack of proper classification systems since the taxonomy of tropical and subtropical, benthic marine cyanobacteria has only recently been analyzed by phylogenetic methods. This evolutionary study provides a framework for a more robust classification system to better understand the taxonomy of tropical and subtropical marine cyanobacteria and the distribution of natural products in marine cyanobacteria. C1 [Engene, Niclas; Gunasekera, Sarath P.; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. RP Engene, N (reprint author), Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. EM engenen@si.edu; paul@si.edu FU Smithsonian Marine Science Network postdoctoral fellowship; NIH [CA100851, NS053398] FX This work was generously supported by a Smithsonian Marine Science Network postdoctoral fellowship (to N.E.). W.H.G. thanks NIH (grants CA100851 and NS053398) for support. The fieldwork was supported by the Carmabi Research Station (Curacao), the Carrie Bow Cay Field Station (Belize), the Smithsonian Marine Station (Ft. Pierce, FL), the Mote Marine Laboratory (Summerland Key, FL), and the Council on International Educational Exchange Research Station (Bonaire). NR 52 TC 24 Z9 25 U1 0 U2 48 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD MAR PY 2013 VL 79 IS 6 BP 1882 EP 1888 DI 10.1128/AEM.03793-12 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 097DP UT WOS:000315454500015 PM 23315747 ER PT J AU Duarte, CM Pitt, KA Lucas, CH Purcell, JE Uye, S Robinson, K Brotz, L Decker, MB Sutherland, KR Malej, A Madin, L Mianzan, H Gili, JM Fuentes, V Atienza, D Pages, F Breitburg, D Malek, J Graham, WM Condon, RH AF Duarte, Carlos M. Pitt, Kylie A. Lucas, Cathy H. Purcell, Jennifer E. Uye, Shin-ichi Robinson, Kelly Brotz, Lucas Decker, Mary Beth Sutherland, Kelly R. Malej, Alenka Madin, Laurence Mianzan, Hermes Gili, Josep-Maria Fuentes, Veronica Atienza, Dacha Pages, Francesc Breitburg, Denise Malek, Jennafer Graham, William M. Condon, Robert H. TI Is global ocean sprawl a cause of jellyfish blooms? SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID SCYPHOZOAN AURELIA-LABIATA; LOW DISSOLVED-OXYGEN; LIFE-HISTORY; SETTLEMENT PREFERENCES; COMMON JELLYFISH; PLASTIC DEBRIS; AURITA; POLYPS; BAY; POPULATION AB Jellyfish (Cnidaria, Scyphozoa) blooms appear to be increasing in both intensity and frequency in many coastal areas worldwide, due to multiple hypothesized anthropogenic stressors. Here, we propose that the proliferation of artificial structures associated with (1) the exponential growth in shipping, aquaculture, and other coastal industries, and (2) coastal protection (collectively, "ocean sprawl") provides habitat for jellyfish polyps and may be an important driver of the global increase in jellyfish blooms. However, the habitat of the benthic polyps that commonly result in coastal jellyfish blooms has remained elusive, limiting our understanding of the drivers of these blooms. Support for the hypothesized role of ocean sprawl in promoting jellyfish blooms is provided by observations and experimental evidence demonstrating that jellyfish larvae settle in large numbers on artificial structures in coastal waters and develop into dense concentrations of jellyfish-producing polyps. Front Ecol Environ 2013; 11(2): 91-97, doi:10.1890/110246 (published online 7 Sep 2012) C1 [Duarte, Carlos M.; Pages, Francesc] Univ Western Australia, Oceans Inst, Crawley, WA, Australia. [Duarte, Carlos M.] Inst Mediterraneo Estudios Avanzados, Dept Global Change Res, Esporles, Spain. [Pitt, Kylie A.] Griffith Univ, Australian Rivers Inst, Gold Coast, Australia. [Pitt, Kylie A.] Griffith Univ, Griffith Sch Environm, Gold Coast, Australia. [Lucas, Cathy H.] Univ Southampton, Sch Ocean & Earth Sci, Natl Oceanog Ctr, Southampton, Hants, England. [Purcell, Jennifer E.] Western Washington Univ, Shannon Point Marine Ctr, Anacortes, WA, Australia. [Uye, Shin-ichi] Hiroshima Univ, Grad Sch Biosphere Sci, Higashihiroshima 724, Japan. [Robinson, Kelly; Condon, Robert H.] Dauphin Isl Sea Lab, Dauphin Isl, AL USA. [Brotz, Lucas] Univ British Columbia, Fisheries Ctr, Vancouver, BC V5Z 1M9, Canada. [Decker, Mary Beth] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT USA. [Sutherland, Kelly R.] CALTECH, Pasadena, CA 91125 USA. [Malej, Alenka] Natl Inst Biol, Marine Biol Stn, Piran, Slovenia. [Madin, Laurence] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Mianzan, Hermes] CONICEPT Inst Nacl Invest & Desarrollo Pesquero, Mar Del Plata, Buenos Aires, Argentina. [Gili, Josep-Maria; Fuentes, Veronica; Atienza, Dacha] Inst Ciencies Mar, Barcelona, Spain. [Breitburg, Denise; Malek, Jennafer] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Graham, William M.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS USA. RP Duarte, CM (reprint author), Univ Western Australia, Oceans Inst, Crawley, WA, Australia. EM carlos.duarte@uwa.edu.au RI Lucas, Cathy/N-1230-2013; Fuentes, Veronica/K-7589-2014; Pitt, Kylie/N-7421-2014; Atienza, Dacha/I-2162-2015; Duarte, Carlos M/A-7670-2013 OI Lucas, Cathy/0000-0002-5929-7481; Fuentes, Veronica/0000-0002-6380-0174; Pitt, Kylie/0000-0002-2292-2052; Atienza, Dacha/0000-0002-3342-5297; Duarte, Carlos M/0000-0002-1213-1361 FU National Center for Ecological Analysis and Synthesis (NCEAS); National Science Foundation [DEB-94-21535]; University of California at Santa Barbara; State of California; Evaluation of Ecosystem Impacts of Global Change in Mediterranean Ecosystems (MEDEICG) project; Spanish National Plan of I+D [CTM2009-07013]; National Oceanic and Atmospheric Administration [NA09NOS4780214] FX This research is a contribution to the Global Expansion of Jellyfish Blooms: Magnitude, Causes and Consequences Working Group, supported by the National Center for Ecological Analysis and Synthesis (NCEAS is supported by the National Science Foundation [grant #DEB-94-21535], the University of California at Santa Barbara, and the State of California) and the Evaluation of Ecosystem Impacts of Global Change in Mediterranean Ecosystems (MEDEICG) project, funded by the Spanish National Plan of I+D (CTM2009-07013). The C quinquecirrha experiments were conducted by DB and JM and supported by National Oceanic and Atmospheric Administration grant #NA09NOS4780214 to DB. We thank K Davies for artistic work. NR 42 TC 42 Z9 43 U1 11 U2 227 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD MAR PY 2013 VL 11 IS 2 BP 91 EP 97 DI 10.1890/110246 PG 7 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 100NC UT WOS:000315706900017 ER PT J AU Thomas, DB Fordyce, RE Gordon, KC AF Thomas, Daniel B. Fordyce, R. Ewan Gordon, Keith C. TI Evidence for a krill-rich diet from non-destructive analyses of penguin bone SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID RAMAN-SPECTROSCOPY; FLUORIDE CONTENT; ADELIE PENGUINS; MEGANYCTIPHANES-NORVEGICA; DIAGENETIC ALTERATION; PYGOSCELIS-ADELIAE; EUPHAUSIA-SUPERBA; BREEDING-SEASON; ANTARCTICA; PHOSPHATES AB Diet strongly influences the chemistry of vertebrate soft and hard tissues. Bird bone and eggshell mineral preserve reliable records of prey consumption, even beyond the life of the predator, and analyses of hard tissues have usefully reconstructed avian diet. Here, we assess the feasibility of a non-destructive method for distinguishing krill-poor from krill-rich diets in penguins. Krill (Euphausiaceae) are fluoride-rich, and penguins that consume krill produce fluoride-rich bones. The chemistry of bone mineral may be elucidated using Raman spectroscopy without recourse to specialised sample preparation. Published data from the diet of six penguin species were compared to a fluoride-informative spectral band (phosphate symmetric stretch, 1-PO43) in the Raman spectra of penguin humeri. Penguins that consume abundant krill (e.g. Adelie and emperor) have 1-PO43-band positions higher than 963 cm1, whereas penguins that primarily eat teleost fish or cephalopods (e.g. Fiordland crested, Humboldt, little blue and yellow-eyed) have 1-PO43-band positions lower than 963 cm1. A krill-rich diet can therefore be determined from the Raman spectra of penguin bones. Raman spectroscopy could be a useful supplement to existing diet analysis techniques. C1 [Thomas, Daniel B.; Fordyce, R. Ewan] Univ Otago, Dept Geol, Dunedin 9054, New Zealand. [Gordon, Keith C.] Univ Otago, Dept Chem, Dunedin 9054, New Zealand. [Gordon, Keith C.] Univ Otago, MacDiarmid Inst Adv Mat & Nanotechnol, Dunedin 9054, New Zealand. RP Thomas, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, MRC 116, Washington, DC 20013 USA. EM thomasd@si.edu RI Gordon, Keith/B-7149-2008; OI Fordyce, Ewan/0000-0002-2656-730X; Gordon, Keith/0000-0003-2833-6166 FU Divisional scholarship; Dept of Geology, Univ. of Otago; Dept of Chemistry, Univ. of Otago FX Cushla McGoverin, Steven Emslie, Yolanda van Heezik and Yutaka Watanuki provided helpful comments on the manuscript. DBT was funded by a Divisional scholarship supplied by the Division of Sciences, Univ. of Otago, and additional scholarship funds from the Depts of Geology and Chemistry, Univ. of Otago. NR 33 TC 1 Z9 1 U1 4 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD MAR PY 2013 VL 44 IS 2 BP 203 EP 207 DI 10.1111/j.1600-048X.2012.00095.x PG 5 WC Ornithology SC Zoology GA 099UG UT WOS:000315647300013 ER PT J AU Baeza, JA Ritson-Williams, R Fuentes, MS AF Baeza, J. A. Ritson-Williams, R. Fuentes, M. S. TI Sexual and mating system in a caridean shrimp symbiotic with the winged pearl oyster in the Coral Triangle SO JOURNAL OF ZOOLOGY LA English DT Article DE monogamy; mating system; sexual system; symbiosis; shrimp; Pontoniidae ID SNAPPING SHRIMP; SEA-ANEMONE; SOCIAL MONOGAMY; CARIBBEAN SEA; LIFE-HISTORY; PINNA-CARNEA; DECAPODA; CRUSTACEA; HERMAPHRODITISM; ALLOCATION AB For symbiotic crustaceans, theory predicts that monogamy is adaptive when species inhabit scarce, relatively small and morphologically simple hosts in tropical environments where predation risk away from hosts is high. We tested this prediction in the shrimp Paranchistus pycnodontae, which inhabits the mantle cavity of the winged pearl oyster Pteria penguin in the Coral Triangle. In various symbiotic crustaceans, males are smaller than females, and this sexual dimorphism has been used as evidence of sex change (protandry) in these organisms. Preliminary observations in Pa.pycnodontae suggested that males were smaller than females. Thus, we first investigated the sexual system of Pa.pycnodontae to determine if the species was protandric. Morphological identification and size frequency distributions indicated that the population comprised small males, small immature females and larger mature females, which was confirmed by dissections. No transitional individuals were found. Thus, Pa.pycnodontae is a gonochoric species with reverse sexual dimorphism. Pa.pycnodontae inhabit as heterosexual pairs in the mantle cavity of hosts more frequently than is expected by chance alone. Pairing was size assortative; both carapace length and propodus length of the major cheliped were positively correlated between males and females forming pairs. Males occur with females in the same host, independent of the female gravid condition or of the stage of development of the brooded eggs. Lastly, the major cheliped did not exhibit positive allometry in males. All the available information suggests that Pa.pycnodontae has adopted a socially monogamous mating system with males and females forming exclusive pairs from other adults. Symbiotic shrimps can be used as a model system to understand behavioural diversity within socially monogamous marine invertebrates. C1 [Baeza, J. A.; Ritson-Williams, R.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. A.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. [Fuentes, M. S.] Algenol Biofuels, Ft Myers, FL USA. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU Committee for Research and Exploration Grant of the National Geographic Society FX This research was partially funded by the Committee for Research and Exploration Grant of the National Geographic Society (to J.A.B.). Thanks to Dr Charles Fransen (Naturalis, the Netherlands) for aiding with shrimp identification and to Dr Robert W. Elwood and one anonymous referee whose comments improved this paper. This is SMSFP contribution number 896. NR 53 TC 11 Z9 11 U1 1 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 EI 1469-7998 J9 J ZOOL JI J. Zool. PD MAR PY 2013 VL 289 IS 3 BP 172 EP 181 DI 10.1111/j.1469-7998.2012.00974.x PG 10 WC Zoology SC Zoology GA 097TN UT WOS:000315496500002 ER PT J AU Riley, SM AF Riley, Sheila M. TI Five Days. SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 2013 VL 138 IS 4 BP 71 EP 71 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 099ZD UT WOS:000315663600064 ER PT J AU Hong, T AF Hong, Terry TI Sandalwood Death: A Novel. SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian Book Dragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian Book Dragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAR 1 PY 2013 VL 138 IS 4 BP 72 EP 72 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 099ZD UT WOS:000315663600066 ER PT J AU Corral-Santana, JM Casares, J Munoz-Darias, T Rodriguez-Gil, P Shahbaz, T Torres, MAP Zurita, C Tyndall, AA AF Corral-Santana, J. M. Casares, J. Munoz-Darias, T. Rodriguez-Gil, P. Shahbaz, T. Torres, M. A. P. Zurita, C. Tyndall, A. A. TI A Black Hole Nova Obscured by an Inner Disk Torus SO SCIENCE LA English DT Article ID X-RAY BINARIES; ACCRETION DISKS; MASS; GALAXY AB Stellar-mass black holes (BHs) are mostly found in x-ray transients, a subclass of x-ray binaries that exhibit violent outbursts. None of the 50 galactic BHs known show eclipses, which is surprising for a random distribution of inclinations. Swift J1357.2-093313 is a very faint x-ray transient detected in 2011. On the basis of spectroscopic evidence, we show that it contains a BH in a 2.8-hour orbital period. Further, high-time-resolution optical light curves display profound dips without x-ray counterparts. The observed properties are best explained by the presence of an obscuring toroidal structure moving outward in the inner disk, seen at very high inclination. This observational feature should play a key role in models of inner accretion flows and jet collimation mechanisms in stellar-mass BHs. C1 [Corral-Santana, J. M.; Casares, J.; Rodriguez-Gil, P.; Shahbaz, T.; Zurita, C.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, SC de Tenerife, Spain. [Corral-Santana, J. M.; Casares, J.; Rodriguez-Gil, P.; Shahbaz, T.; Zurita, C.] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, SC de Tenerife, Spain. [Munoz-Darias, T.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tyndall, A. A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tyndall, A. A.] European So Observ, Santiago 19001, Chile. [Tyndall, A. A.] Isaac Newton Grp Telescopes, E-38700 SC De La Palma, Spain. RP Corral-Santana, JM (reprint author), Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, SC de Tenerife, Spain. EM jcorral@iac.es RI Corral-Santana, Jesus/A-6956-2016; Rodriguez-Gil, Pablo/H-7709-2015 OI Corral-Santana, Jesus/0000-0003-1038-9104; Rodriguez-Gil, Pablo/0000-0002-4717-5102 FU Spanish Ministerio de Ciencia e Innovacion (MICINN) [AYA2010-18080]; Spanish MICINN under the Consolider-Ingenio Program [CSD2006-00070] FX This work made use of the Image Reduction and Analysis Facility (IRAF) and the MOLLY software developed by T. R. Marsh. We thank P. Charles, G. Ponti, and D. M. Russell for their useful comments; G. Perez and M. Leal for their help with fig. S3 and movie S1; and I. Negueruela and C. Gonzalez-Fernandez for obtaining the Intermediate Dispersion Spectrograph (IDS) spectra. Based on observations made with the INT and WHT, operated by the Isaac Newton Group; the LT, operated by the Liverpool John Moores University with financial support from the UK Science and Technology Facilities Council; and the MT, operated by the University of Leuven and the Observatory of Geneva. All of them are installed at the Spanish Observatorio del Roque de Los Muchachos (on the island of La Palma) of the Instituto de Astrofisica de Canarias (IAC). The photometry taken on 26 April 2011 is based on observations made with the INT under the Spanish IAC Director's Discretionary Time. T. M. D. acknowledges funding via a European Union Marie Curie Intra-European Fellowship under contract no. 2011-301355. This research was supported by the Spanish Ministerio de Ciencia e Innovacion (MICINN) under grant AYA2010-18080 and partly funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: "First science with the GTC" (www.iac.es/consolider-ingenio-gtc/). NR 31 TC 32 Z9 33 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD MAR 1 PY 2013 VL 339 IS 6123 BP 1048 EP 1051 DI 10.1126/science.1228222 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 097CQ UT WOS:000315452000033 PM 23449588 ER PT J AU Lee, KG Bailey, S Bartsch, LE Carithers, W Dawson, KS Kirkby, D Lundgren, B Margala, D Palanque-Delabrouille, N Pieri, MM Schlegel, DJ Weinberg, DH Yeche, C Aubourg, E Bautista, J Bizyaev, D Blomqvist, M Bolton, AS Borde, A Brewington, H Busca, NG Croft, RAC Delubac, T Ebelke, G Eisenstein, DJ Font-Ribera, A Ge, J Hamilton, JC Hennawi, JF Ho, S Honscheid, K Le Goff, JM Malanushenko, E Malanushenko, V Miralda-Escude, J Myers, AD Noterdaeme, P Oravetz, D Pan, K Paris, I Petitjean, P Rich, J Rollinde, E Ross, NP Rossi, G Schneider, DP Simmons, A Snedden, S Slosar, A Spergel, DN Suzuki, N Viel, M Weaver, BA AF Lee, Khee-Gan Bailey, Stephen Bartsch, Leslie E. Carithers, William Dawson, Kyle S. Kirkby, David Lundgren, Britt Margala, Daniel Palanque-Delabrouille, Nathalie Pieri, Matthew M. Schlegel, David J. Weinberg, David H. Yeche, Christophe Aubourg, Eric Bautista, Julian Bizyaev, Dmitry Blomqvist, Michael Bolton, Adam S. Borde, Arnaud Brewington, Howard Busca, Nicolas G. Croft, Rupert A. C. Delubac, Timothee Ebelke, Garrett Eisenstein, Daniel J. Font-Ribera, Andreu Ge, Jian Hamilton, Jean-Christophe Hennawi, Joseph F. Ho, Shirley Honscheid, Klaus Le Goff, Jean-Marc Malanushenko, Elena Malanushenko, Viktor Miralda-Escude, Jordi Myers, Adam D. Noterdaeme, Pasquier Oravetz, Daniel Pan, Kaike Paris, Isabelle Petitjean, Patrick Rich, James Rollinde, Emmanuel Ross, Nicholas P. Rossi, Graziano Schneider, Donald P. Simmons, Audrey Snedden, Stephanie Slosar, Aneze Spergel, David N. Suzuki, Nao Viel, Matteo Weaver, Benjamin A. TI THE BOSS Ly alpha FOREST SAMPLE FROM SDSS DATA RELEASE 9 SO ASTRONOMICAL JOURNAL LA English DT Article DE intergalactic medium; methods: data analysis; quasars: absorption lines; quasars: emission lines ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; COLD DARK-MATTER; PROBABILITY-DISTRIBUTION FUNCTION; COLUMN DENSITY DISTRIBUTION; QUASI-STELLAR OBJECTS; 9TH DATA RELEASE; POWER SPECTRUM; GRAVITATIONAL COLLAPSE; INTERGALACTIC MEDIUM AB We present the BOSS Lyman-alpha (Ly alpha) Forest Sample from SDSS Data Release 9, comprising 54,468 quasar spectra with z(qso) > 2.15 suitable for Ly alpha forest analysis. This data set probes the intergalactic medium with absorption redshifts 2.0 < z alpha < 5.7 over an area of 3275 deg(2), and encompasses an approximate comoving volume of 20 h(-3) Gpc(3). With each spectrum, we have included several products designed to aid in Ly alpha forest analysis: improved sky masks that flag pixels where data may be unreliable, corrections for known biases in the pipeline estimated noise, masks for the cores of damped Ly alpha systems and corrections for their wings, and estimates of the unabsorbed continua so that the observed flux can be converted to a fractional transmission. The continua are derived using a principal component fit to the quasar spectrum redward of rest-frame Ly alpha (lambda > 1216 angstrom), extrapolated into the forest region and normalized by a linear function to fit the expected evolution of the Ly alpha forest mean flux. The estimated continuum errors are less than or similar to 5% rms. We also discuss possible systematics arising from uncertain spectrophotometry and artifacts in the flux calibration; global corrections for the latter are provided. Our sample provides a convenient starting point for users to analyze clustering in BOSS Ly alpha forest data, and it provides a fiducial data set that can be used to compare results from different analyses of baryon acoustic oscillations in the Ly alpha forest. The full data set is available from the SDSS-III DR9 Web site. C1 [Lee, Khee-Gan; Hennawi, Joseph F.] Max Planck Inst Astron, D-69115 Heidelberg, Germany. [Bailey, Stephen; Carithers, William; Schlegel, David J.; Font-Ribera, Andreu; Ross, Nicholas P.; Suzuki, Nao] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Bartsch, Leslie E.; Croft, Rupert A. C.; Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Bartsch, Leslie E.; Croft, Rupert A. C.; Ho, Shirley] Carnegie Mellon Univ, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Dawson, Kyle S.; Bolton, Adam S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kirkby, David; Margala, Daniel; Blomqvist, Michael] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Lundgren, Britt] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Palanque-Delabrouille, Nathalie; Yeche, Christophe; Borde, Arnaud; Delubac, Timothee; Le Goff, Jean-Marc; Rich, James; Rossi, Graziano] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Pieri, Matthew M.; Rossi, Graziano] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Aubourg, Eric; Bautista, Julian; Busca, Nicolas G.; Hamilton, Jean-Christophe] Univ Paris 07, APC, CNRS IN2P3, Observ Paris,CEA, Paris, France. [Bizyaev, Dmitry; Brewington, Howard; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Eisenstein, Daniel J.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Font-Ribera, Andreu] Univ Zurich, Inst Theoret Phys, CH-8057 Zurich, Switzerland. [Ge, Jian] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona, Catalonia, Spain. [Miralda-Escude, Jordi] Univ Barcelona IEEC, Inst Ciencies Cosmos, Barcelona 08028, Catalonia, Spain. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Noterdaeme, Pasquier; Paris, Isabelle; Petitjean, Patrick; Rollinde, Emmanuel] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Noterdaeme, Pasquier; Paris, Isabelle; Petitjean, Patrick; Rollinde, Emmanuel] CNRS, F-75014 Paris, France. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Slosar, Aneze] Bldg 510 Brookhaven Natl Lab, Upton, NY 11973 USA. [Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Viel, Matteo] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Viel, Matteo] INFN Natl Inst Nucl Phys, I-34127 Trieste, Italy. [Weaver, Benjamin A.] New York Univ, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Lee, KG (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69115 Heidelberg, Germany. EM lee@mpia.de RI Le Goff, Jean-Marc/E-7629-2013; Spergel, David/A-4410-2011; Ho, Shirley/P-3682-2014; Croft, Rupert/N-8707-2014; OI Ho, Shirley/0000-0002-1068-160X; Croft, Rupert/0000-0003-0697-2583; Kirkby, David/0000-0002-8828-5463; Miralda-Escude, Jordi/0000-0002-2316-8370; Viel, Matteo/0000-0002-2642-5707 FU European Union [PIIF-GA-2011-301665]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group, University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. [PIIF-GA-2011-301665].; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 62 TC 29 Z9 29 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 2013 VL 145 IS 3 AR 69 DI 10.1088/0004-6256/145/3/69 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089XU UT WOS:000314944100017 ER PT J AU Loomis, RA Zaleski, DP Steber, AL Neill, JL Muckle, MT Harris, BJ Hollis, JM Jewell, PR Lattanzi, V Lovas, FJ Martinez, O McCarthy, MC Remijan, AJ Pate, BH Corby, JF AF Loomis, Ryan A. Zaleski, Daniel P. Steber, Amanda L. Neill, Justin L. Muckle, Matthew T. Harris, Brent J. Hollis, Jan M. Jewell, Philip R. Lattanzi, Valerio Lovas, Frank J. Martinez, Oscar, Jr. McCarthy, Michael C. Remijan, Anthony J. Pate, Brooks H. Corby, Joanna F. TI THE DETECTION OF INTERSTELLAR ETHANIMINE (CH3CHNH) FROM OBSERVATIONS TAKEN DURING THE GBT PRIMOS SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE catalogs; ISM: abundances; ISM: individual objects (SgrB2N); ISM: molecules; methods: laboratory; surveys ID TRANSFORM MICROWAVE SPECTROMETER; ICE ANALOGS; CHIRPED-PULSE; AMINO-ACIDS; HYDROGEN-CYANIDE; SAGITTARIUS B2; LINE SURVEY; GAS-PHASE; ORION-KL; SPECTRUM AB We have performed reaction product screening measurements using broadband rotational spectroscopy to identify rotational transition matches between laboratory spectra and the Green Bank Telescope PRIMOS radio astronomy survey spectra in Sagittarius B2 North (Sgr B2(N)). The broadband rotational spectrum of molecules created in an electrical discharge of CH3CN and H2S contained several frequency matches to unidentified features in the PRIMOS survey that did not have molecular assignments based on standard radio astronomy spectral catalogs. Several of these transitions are assigned to the E- and Z-isomers of ethanimine. Global fits of the rotational spectra of these isomers in the range of 8-130 GHz have been performed for both isomers using previously published mm-wave spectroscopy measurements and the microwave measurements of the current study. Possible interstellar chemistry formation routes for E- ethanimine and Z- ethanimine are discussed. The detection of ethanimine is significant because of its possible role in the formation of alanine-one of the twenty amino acids in the genetic code. C1 [Loomis, Ryan A.; Zaleski, Daniel P.; Steber, Amanda L.; Neill, Justin L.; Muckle, Matthew T.; Harris, Brent J.; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. [Lattanzi, Valerio; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, Valerio; Martinez, Oscar, Jr.; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Lovas, Frank J.] NIST, Gaithersburg, MD 20899 USA. [Corby, Joanna F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Loomis, RA (reprint author), Univ Virginia, Dept Chem, McCormick Rd, Charlottesville, VA 22904 USA. OI McCarthy, Michael/0000-0001-9142-0008; Steber, Amanda/0000-0002-8203-2174; Zaleski, Daniel/0000-0003-0153-9158 FU Centers for Chemical Innovation program of the National Science Foundation [CHE-0847919]; NSF Chemistry [CHE-1213200]; College Science Scholars program at the University of Virginia FX The authors acknowledge support from the Centers for Chemical Innovation program of the National Science Foundation (CHE-0847919), NSF Chemistry (CHE-1213200), and the College Science Scholars program at the University of Virginia. We also thank B. McGuire and R. Pulliam for helpful comments to improve the manuscript. Finally, we thank the anonymous referee for valuable comments and suggestions on the manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 43 TC 15 Z9 15 U1 2 U2 31 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2013 VL 765 IS 1 AR L9 DI 10.1088/2041-8205/765/1/L9 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 093JK UT WOS:000315187800009 ER PT J AU Qi, CH Oberg, KI Wilner, DJ Rosenfeld, KA AF Qi, Chunhua Oeberg, Karin I. Wilner, David J. Rosenfeld, Katherine A. TI FIRST DETECTION OF c-C3H2 IN A CIRCUMSTELLAR DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM; stars: formation; techniques: high angular resolution ID DIFFUSE INTERSTELLAR-MEDIUM; HERBIG-AE STARS; PROTOPLANETARY DISKS; SMALL HYDROCARBONS; ORGANIC-MOLECULES; IMAGING SURVEY; DARK CLOUDS; DENSE CORES; HD 163296; DM-TAU AB We report the first detection of c-C3H2 in a circumstellar disk. The c-C3H2 J = 6-5 line (217.882 GHz) is detected and imaged through Atacama Large Millimeter Array ( ALMA) Science Verification observations toward the disk around the Herbig Ae star HD 163296 at 0.'' 8 resolution. The emission is consistent with that arising from a Keplerian rotating disk. Two additional c-C3H2 transitions are also tentatively detected, bolstering the identification of this species, but with insufficient signal-to-noise ratio to constrain the spatial distribution. Using a previously developed model for the physical structure of this disk, we fit a radial power-law distribution model to the c-C3H2 6-5 emission and find that c-C3H2 is present in a ring structure from an inner radius of about 30 AU to an outer radius of about 165 AU. The column density is estimated to be 10(12)-10(13) cm(-2). The clear detection and intriguing ring structure suggest that c-C3H2 has the potential to become a useful probe of radiation penetration in disks. C1 [Qi, Chunhua; Wilner, David J.; Rosenfeld, Katherine A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oeberg, Karin I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, Karin I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Origins of Solar Systems [NNX11AK63] FX We would like to thank the anonymous referee for thoughtful suggestions for the Letter. We also acknowledge NASA Origins of Solar Systems grant No. NNX11AK63. NR 45 TC 16 Z9 16 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2013 VL 765 IS 1 AR L14 DI 10.1088/2041-8205/765/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 093JK UT WOS:000315187800014 ER PT J AU Zaleski, DP Seifert, NA Steber, AL Muckle, MT Loomis, RA Corby, JF Martinez, O Crabtree, KN Jewell, PR Hollis, JM Lovas, FJ Vasquez, D Nyiramahirwe, J Sciortino, N Johnson, K McCarthy, MC Remijan, AJ Pate, BH AF Zaleski, Daniel P. Seifert, Nathan A. Steber, Amanda L. Muckle, Matt T. Loomis, Ryan A. Corby, Joanna F. Martinez, Oscar, Jr. Crabtree, Kyle N. Jewell, Philip R. Hollis, Jan M. Lovas, Frank J. Vasquez, David Nyiramahirwe, Jolie Sciortino, Nicole Johnson, Kennedy McCarthy, Michael C. Remijan, Anthony J. Pate, Brooks H. TI DETECTION OF E-CYANOMETHANIMINE TOWARD SAGITTARIUS B2(N) IN THE GREEN BANK TELESCOPE PRIMOS SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE catalogs; ISM: abundances; ISM: individual objects (SgrB2N); ISM: molecules; methods: laboratory; surveys ID SPECTRAL-LINE SURVEY; Z-C-CYANOMETHANIMINE; OBSERVATIONAL DATA; ORGANIC-MOLECULES; MICROWAVE-SPECTRA; PRIMITIVE EARTH; HCN DIMER; INTERSTELLAR; DELIVERY; ADENINE AB The detection of E-cyanomethanimine (E-HNCHCN) toward Sagittarius B2(N) is made by comparing the publicly available Green Bank Telescope (GBT) PRIMOS survey spectra to laboratory rotational spectra from a reaction product screening experiment. The experiment uses broadband molecular rotational spectroscopy to monitor the reaction products produced in an electric discharge source using a gas mixture of NH3 and CH3CN. Several transition frequency coincidences between the reaction product screening spectra and previously unassigned interstellar rotational transitions in the PRIMOS survey have been assigned to E-cyanomethanimine. A total of eight molecular rotational transitions of this molecule between 9 and 50 GHz are observed with the GBT. E-cyanomethanimine, often called the HCN dimer, is an important molecule in prebiotic chemistry because it is a chemical intermediate in proposed synthetic routes of adenine, one of the two purine nucleobases found in DNA and RNA. New analyses of the rotational spectra of both E-cyanomethanimine and Z-cyanomethanimine that incorporate previous millimeter-wave measurements are also reported. C1 [Zaleski, Daniel P.; Seifert, Nathan A.; Steber, Amanda L.; Muckle, Matt T.; Loomis, Ryan A.; Vasquez, David; Nyiramahirwe, Jolie; Sciortino, Nicole; Johnson, Kennedy; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Corby, Joanna F.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Martinez, Oscar, Jr.; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martinez, Oscar, Jr.; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Jewell, Philip R.; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Hollis, Jan M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Lovas, Frank J.] NIST, Gaithersburg, MD 20899 USA. RP Zaleski, DP (reprint author), Univ Virginia, Dept Chem, McCormick Rd, Charlottesville, VA 22904 USA. EM bp2k@virginia.edu; mccarthy@cfa.harvard.edu; aremijan@nrao.edu OI Crabtree, Kyle/0000-0001-5629-5192; McCarthy, Michael/0000-0001-9142-0008; Steber, Amanda/0000-0002-8203-2174; Zaleski, Daniel/0000-0003-0153-9158 FU NSF Centers for Chemical Innovation [CHE-0847919]; NSF Chemistry [CHE-1213200]; Virginia-North Carolina Alliance, a NSF Louis Stokes Alliance for Minority Participation [HRD-1202181]; National Radio Astronomy Observatory FX This work was supported by the NSF Centers for Chemical Innovation (CHE-0847919) and NSF Chemistry (CHE-1213200). Additional support was provided by the Virginia-North Carolina Alliance, a NSF Louis Stokes Alliance for Minority Participation (HRD-1202181) and the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Finally, we thank the anonymous referee for a favorable review and valuable comments that greatly improved the quality of this manuscript. NR 36 TC 26 Z9 26 U1 1 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAR 1 PY 2013 VL 765 IS 1 AR L10 DI 10.1088/2041-8205/765/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 093JK UT WOS:000315187800010 ER PT J AU Wang, LH Newchurch, MJ Pour-Biazar, A Kuang, S Khan, M Liu, X Koshak, W Chance, K AF Wang, Lihua Newchurch, M. J. Pour-Biazar, Arastoo Kuang, Shi Khan, Maudood Liu, Xiong Koshak, William Chance, Kelly TI Estimating the influence of lightning on upper tropospheric ozone using NLDN lightning data and CMAQ model SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE LNOx; CMAQ; Ozone; Lightning; NLDN; OMI; IONS06 ID CONTINENTAL UNITED-STATES; NITROGEN-OXIDES; NOX PRODUCTION; MONITORING INSTRUMENT; PROFILE RETRIEVALS; GENERATED NOX; STERAO-A; TRANSPORT; THUNDERSTORMS; MIDLATITUDES AB Lightning is a particularly significant NOx source in the middle and upper troposphere where it affects tropospheric chemistry and ozone. Because the version-4 Community Multiscale Air Quality Modeling System (CMAQ) does not account for NOx emission from lightning, it underpredicts NOx above the mixed layer. In this study, the National Lightning Detection Network (TM) (NLDN) lightning data are applied to the CMAQ model to simulate the influence of lightning-produced NOx (LNOx) on upper tropospheric NOx and subsequent ozone concentration. Using reasonable values for salient parameters (detection efficiency similar to 95%, cloud flash to ground flash ratio similar to 3, LNOx production rate similar to 500 mol N per flash), the NLDN ground flashes are converted into total lightning NOx amount and then vertically distributed on 39 CMAQ model layers according to a vertical-distribution profile of lightning N mass. This LNOx contributes 27% of the total NOx emission during 15 July similar to 7 September 2006. This additional NOx reduces the low-bias of simulated tropospheric O-3 columns with respect to OMI tropospheric O-3 columns from 10 to 5%. Although the model prediction of ozone in upper troposphere improves by similar to 20 ppbv due to lightning-produced NOx above the southeastern and eastern U.S.A., the improved ozone prediction is still similar to 20-25 ppbv lower than ozonesonde measurements. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Wang, Lihua; Newchurch, M. J.; Pour-Biazar, Arastoo; Kuang, Shi] Univ Alabama, Huntsville, AL 35899 USA. [Khan, Maudood] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koshak, William] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Wang, LH (reprint author), Univ Alabama, Huntsville, AL 35899 USA. EM lihuawang@nsstc.uah.edu RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Minerals Management Service; Minerals Management Service on Gulf of Mexico Issues; NASA Science Mission Directorate Applied Sciences Program; Atmospheric Chemistry Program; NOAA/NESDIS FX This work is supported by the Minerals Management Service under Cooperative Agreement between the University of Alabama in Huntsville and the Minerals Management Service on Gulf of Mexico Issues, the NASA Science Mission Directorate Applied Sciences Program and Atmospheric Chemistry Program, and NOAA/NESDIS. NR 63 TC 5 Z9 5 U1 1 U2 33 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 J9 ATMOS ENVIRON JI Atmos. Environ. PD MAR PY 2013 VL 67 BP 219 EP 228 DI 10.1016/j.atmosenv.2012.11.001 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 093EA UT WOS:000315173300026 ER PT J AU Alda, F Ruiz-Lopez, MJ Garcia, FJ Gompper, ME Eggert, LS Garcia, JT AF Alda, Fernando Jose Ruiz-Lopez, Maria Jose Garcia, Francisco Gompper, Matthew E. Eggert, Lori S. Garcia, Jesus T. TI Genetic evidence for multiple introduction events of raccoons (Procyon lotor) in Spain SO BIOLOGICAL INVASIONS LA English DT Article DE Raccoon; Procyon lotor; Spain; Founder population size; Invasion; Genetic variation ID EFFECTIVE POPULATION-SIZE; MULTILOCUS GENOTYPE DATA; FREE-RANGING RACCOONS; LINKAGE DISEQUILIBRIUM; PROGRAM; TRADE; LOCI; VARIABILITY; LANDSCAPE; DIVERSITY AB The common raccoon (Procyon lotor) is endemic to Central and North America, although non-native populations have become established around the world. In Spain, growing evidence of the introduction of raccoons has been reported across the country in the last decade, especially in Central Spain where the largest population is thought to occur. We used mitochondrial and microsatellite DNA data to investigate the genetics of invasive raccoons in Central Spain and to infer: the number of introduction events, the number of founders and the genetic variability of the introduced populations compared to a native population. We found that at least two introduction events have occurred along the Jarama and Henares Rivers in Central Spain, which currently constitute two genetically differentiated subpopulations. In both localities the number of effective founders from a native population was estimated as 2-4 individuals. These newly founded populations have expanded and show evidence of incipient contact and reproduction between them. This may allow for an increase in the genetic variability and adaptive potential of the population(s), possibly increasing the difficulty of controlling this invasive species. Our results reveal the ability to longitudinally monitor the genetics of the raccoon range expansion and emphasize the urgent need to control the pet trade of potentially invasive species. C1 [Alda, Fernando; Garcia, Jesus T.] Inst Invest Recursos Cineget CSIC UCLM JCCLM, Ciudad Real 13005, Spain. [Alda, Fernando] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Jose Ruiz-Lopez, Maria; Eggert, Lori S.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Jose Garcia, Francisco] BIOTA, Madrid 28011, Spain. [Gompper, Matthew E.] Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO 65211 USA. RP Alda, F (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM alda.fernando@gmail.com FU Regional Park Parque Regional del Sureste; Comunidad Autonoma de Madrid; National Science Foundation [DEB-0347609, DEB-0841654] FX The authors would like to thank M.J. Aramburu, Y. Cortes, L. Garcia-Roman, J.L. Gonzalez, J. Herrera, M. Perez, B. Pliego, B. Prieto and the staff of the Regional Park Parque Regional del Sureste, Comunidad Autonoma de Madrid, for their help during fieldwork. Capture authorizations were provided by the Comunidad Autonoma de Madrid according to EU laws. We also thank C. I. Cullingham for providing additional information on the geographical distribution of native raccoon haplotypes. Two anonymous referees provided useful suggestions that helped to improve the manuscript. This study was partially funded by the Regional Park Parque Regional del Sureste and the Comunidad Autonoma de Madrid. Sampling and genotyping of Missouri raccoons was supported by grants from the National Science Foundation (DEB-0347609 and DEB-0841654). NR 59 TC 11 Z9 12 U1 1 U2 60 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD MAR PY 2013 VL 15 IS 3 BP 687 EP 698 DI 10.1007/s10530-012-0318-6 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 094UR UT WOS:000315290100019 ER PT J AU Pyenson, ND Goldbogen, JA Shadwick, RE AF Pyenson, Nicholas D. Goldbogen, Jeremy A. Shadwick, Robert E. TI Mandible allometry in extant and fossil Balaenopteridae (Cetacea: Mammalia): the largest vertebrate skeletal element and its role in rorqual lunge feeding SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE bone; Cetacea; Mysticeti ID FIN WHALES; MYSTICETE WHALES; BALEEN WHALE; LONG BONES; BODY-SIZE; EVOLUTION; PLIOCENE; SKULL; MECHANISMS; REGRESSION AB Rorqual whales (crown Balaenopteridae) are unique among aquatic vertebrates in their ability to lunge feed. During a single lunge, rorquals rapidly engulf a large volume of prey-laden water at high speed, which they then filter to capture suspended prey. Engulfment biomechanics are mostly governed by the coordinated opening and closing of the mandibles at large gape angles, which differentially exposes the floor of the oral cavity to oncoming flow. The mouth area in rorquals is delimited by unfused bony mandibles that form kinetic linkages to each other and with the skull. The relative scale and morphology of these skeletal elements have profound consequences for the energetic efficiency of foraging in these gigantic predators. Here, we performed a morphometric study of rorqual mandibles using a data set derived from a survey of museum specimens. Across adult specimens of extant balaenopterids, mandibles range in size from approximate to 16m in length, and at their upper limit they represent the single largest osteological element of any vertebrate, living or extinct. Our analyses determined that rorqual mandibles exhibit positive allometry, whereby the relative size of these mandibles becomes greater with increasing body size. These robust scaling relationships allowed us to predict mandible length for fragmentary remains (e.g. incomplete and/or fossil specimens), as we demonstrated for two partial mandibles from the latest Miocene of California, USA, and for mandibles from previously described fossil balaenopterids. Furthermore, we showed the allometry of mandible length to body size in extant mysticetes, which hints at fundamental developmental constraints in mysticetes despite their ecomorphological differences in feeding styles. Lastly, we outlined how our findings can be used to test hypotheses about the antiquity and evolution of lunge feeding.(c) 2012 The Linnean Society of London, Biological Journal of the Linnean Society, 2013, 108, 586-599. C1 [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. [Goldbogen, Jeremy A.] Cascadia Res Collect, Olympia, WA USA. [Shadwick, Robert E.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM pyensonn@si.edu OI Goldbogen, Jeremy/0000-0002-4170-7294 FU National Science Foundation Graduate Research Fellowship; Natural Sciences and Engineering Research Council of Canada (NSERC); Smithsonian Institution and its Remington Kellogg Fund; University Graduate Fellowship for Research from the University of British Columbia; Scripps Postdoctoral Research Fellowship; NSERC FX We thank E. M. G. Fitzgerald, A. Werth, and an anonymous reviewer for diligent, insightful, and constructive comments that improved the quality of this article. For their assistance with museum collections under their care, we thank: M. Flannery, B. Simison, J. DeMouthe, and S. Mansfield (all CAS); S. Stollman (CM); D. Casper and S. Davenport (both Long Marine Laboratory); the staff at the Whale Interpretive Centre, Telegraph Cove, British Columbia; J. Dynes and D. Janiger (both LACM); C. Conroy (MVZ); A. van Helden (Te Papa Tongarewa National Museum of New Zealand); E. M. G. Fitzgerald (Museum Victoria); K. A. Fahy (Santa Barbara Museum of Natural History); E. Rickett, W. Maddison, and A. Trites, (all UBC); P. A. Holroyd (UCMP); C. W. Potter and J. G. Mead (both USNM); and J. Bradley (Burke Museum of Natural History and Culture). For additional logistical support with data collection, we thank K. Kuker, C. Birdsall, F. Perry, R. E. Fordyce, D. J. Field, T. A. Demere, and M. deRoos. N.D.P. was supported by a National Science Foundation Graduate Research Fellowship, a postdoctoral research fellowship from the Natural Sciences and Engineering Research Council of Canada (NSERC), and by funding from the Smithsonian Institution and its Remington Kellogg Fund. J. A. G. was supported by a University Graduate Fellowship for Research from the University of British Columbia, a Scripps Postdoctoral Research Fellowship and NSERC funding to R.E.S. NR 69 TC 12 Z9 12 U1 1 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD MAR PY 2013 VL 108 IS 3 BP 586 EP 599 DI 10.1111/j.1095-8312.2012.02032.x PG 14 WC Evolutionary Biology SC Evolutionary Biology GA 092KP UT WOS:000315120300010 ER PT J AU Zotz, G AF Zotz, Gerhard TI The systematic distribution of vascular epiphytes a critical update SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE accidental epiphytes; Bromeliaceae; hemiepiphytes; intraspecific variation; life form; Orchidaceae; vines ID LINEAR SEQUENCE; PHYLOGENETIC CLASSIFICATION; APG III; REVISION; BROMELIACEAE; ORCHIDACEAE; TERRESTRIAL; DIVERSITY; INSIGHTS; MELASTOMATACEAE AB Vascular epiphyte species exclusively, or at least primarily, germinate and grow on other plants without contact with the soil and, in contrast to mistletoes, without parasitizing their hosts. The last review of the systematic distribution of this diverse group of plants dates back more than two decades. The present study pursues three major goals: (1) it critically discusses conceptual problems arising from the distinction of epiphytes from non-epiphytes; (2) it presents a compilation of epiphytic diversity derived from a vast number of sources; and (3) it arranges epiphyte diversity in an up-to-date taxonomic framework. The resulting compilation, which identifies 27614 species of vascular epiphytes (including primary hemiepiphytes) representing 913 genera in 73 families, or approximately 9% of extant vascular plant diversity, is meant to be an important tool for studies on the ecology and evolution of epiphytes, but also for comparative studies with a focus on other life forms. (c) 2013 The Linnean Society of London C1 [Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, Inst Biol & Environm Sci, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 74 TC 65 Z9 76 U1 8 U2 97 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD MAR PY 2013 VL 171 IS 3 BP 453 EP 481 DI 10.1111/boj.12010 PG 29 WC Plant Sciences SC Plant Sciences GA 097PD UT WOS:000315485100002 ER PT J AU Roque, N Funk, VA AF Roque, Nadia Funk, Vicki A. TI Morphological characters add support for some members of the basal grade of Asteraceae SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE character evolution; Compositae; morphology; phylogeny ID SUNFLOWER FAMILY; MAJOR LINEAGES; COMPOSITAE; SUBFAMILY; MUTISIEAE; CLADES; GENUS AB Recent molecular studies in Asteraceae have divided tribe Mutisieae (sensu Cabrera) into 13 tribes and eight subfamilies. Each of the major clades is well supported but the relationships among them are not always clear. Some of the new taxa are easily characterized by morphological data but others are not, chief among the latter being three subfamilies (Stifftioideae, Wunderlichioideae and Gochnatioideae) and the tribe Hyalideae. To understand evolution in the family it is critical to investigate potential morphological characters that can help to evaluate the basal lineages of the Asteraceae. The data for this study were taken from 52 species in 24 genera representing the basal groups in the family. Many characters were examined but most of the useful ones were from reproductive structures. Several apomorphies supported a few of the clades. For instance, members of subfamily Wunderlichioideae (Hyalideae and Wunderlichieae) share predominantly ten-ribbed achenes and members of Wunderlichioideae+Stifftioideae share two synapomorphies: 100150 (200) pappus elements, arranged in (three) four or five series. These apomorphies can be viewed as an indication of a sister-group relationship between the two subfamilies as the placement of Stifftieae was not well resolved by the molecular data. Members of Wunderlichieae are characterized by having a paleaceous receptacle, style branches that are strongly papillose above and below the bifurcation, and a pappus of scales. Hyalis and Ianthopappus (Hyalideae) share venation type and an apiculate anther appendage but these are also found in Gochnatieae. Other clades have fewer supporting characters. These characters are just a beginning. Cladograms with morphology characters plotted, illustrations and a key to the basal grade of Asteraceae are provided.(c) 2013 The Linnean Society of London C1 [Roque, Nadia] Univ Fed Bahia, Inst Biol, BR-40170110 Salvador, BA, Brazil. [Funk, Vicki A.] Smithsonian Inst MRC 166, US Natl Herbarium, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Roque, N (reprint author), Univ Fed Bahia, Inst Biol, Campus Univ Ondina, BR-40170110 Salvador, BA, Brazil. EM nadiaroque@gmail.com RI Roque, Nadia/I-3157-2012 FU Smithsonian Institution Cuatrecasas Travel; CNPq [PQ 307156/2010-9]; National Museum of Natural History; Smithsonian Institution FX We thank Natanael Nascimento for the lovely and informative line drawings. We are grateful to the reviewers of the manuscript for valuable comments and suggestions. Funding for travel for Nadia Roque to Washington, DC, was provided by the Smithsonian Institution Cuatrecasas Travel Awards Program. This work was supported by grants from CNPq (PQ 307156/2010-9) and the National Museum of Natural History, Smithsonian Institution. NR 38 TC 12 Z9 13 U1 2 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD MAR PY 2013 VL 171 IS 3 BP 568 EP 586 DI 10.1111/boj.12000 PG 19 WC Plant Sciences SC Plant Sciences GA 097PD UT WOS:000315485100008 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Untitled SO JOURNAL OF AMERICAN HISTORY LA English DT Letter C1 Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD MAR PY 2013 VL 99 IS 4 BP 1336 EP 1337 DI 10.1093/jahist/jas641 PG 2 WC History SC History GA 092WV UT WOS:000315154600164 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Csaszar, AG Daumont, L Gamache, RR Hodges, JT Naumenko, OV Polyansky, OL Rothman, LS Vandaele, AC Zobov, NF Al Derzi, AR Fabri, C Fazliev, AZ Furtenbacher, T Gordon, IE Lodi, L Mizus, II AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Csaszar, Attila G. Daumont, Ludovic Gamache, Robert R. Hodges, Joseph T. Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Vandaele, Ann Carine Zobov, Nikolai F. Al Derzi, Afaf R. Fabri, Csaba Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Lodi, Lorenzo Mizus, Irina I. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor, Part III: Energy levels and transition wavenumbers for (H2O)-O-16 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; MARVEL; Information system; Database; W@DIS; Infrared spectra; Microwave spectra ID MOLECULAR SPECTROSCOPIC DATABASE; HIGH-RESOLUTION SPECTRUM; THZ FREQUENCY REGION; FOURIER-TRANSFORM SPECTROSCOPY; PADE HAMILTONIAN OPERATOR; EMPIRICAL LINE PARAMETERS; RING-DOWN SPECTROSCOPY; HIGHLY EXCITED-STATES; LAMB-DIP TECHNIQUE; MU-M AB This is the third of a series of articles reporting critically evaluated rotational-vibrational line positions, transition intensities, and energy levels, with associated critically reviewed labels and uncertainties, for all the main isotopologues of water. This paper presents experimental line positions, experimental-quality energy levels, and validated labels for rotational-vibrational transitions of the most abundant isotopologue of water, (H2O)-O-16. The latest version of the MARVEL (Measured Active Rotational-Vibrational Energy Levels) line-inversion procedure is used to g determine the rovibrational energy levels of the electronic ground state of (H2O)-O-16 from experimentally measured lines, together with their self-consistent uncertainties, for the spectral region up to the first dissociation limit. The spectroscopic network of (H2O)-O-16 contains two components, an ortho (o) and a para (p) one. For o-(H2O)-O-16 and p-(H2O)-O-16, experimentally measured, assigned, and labeled transitions were analyzed from more than 100 sources. The measured lines come from one-photon spectra recorded at room temperature in absorption, from hot samples with temperatures up to 3000 K recorded in emission, and from multiresonance excitation spectra which sample levels up to dissociation. The total number of transitions considered is 184 667 of which 182 156 are validated: 68 027 between para states and 114 129 ortho ones. These transitions give rise to 18 486 validated energy levels, of which 10 446 and 8040 belong to o-(H2O)-O-16 and p-(H2O)-O-16, respectively. The energy levels, including their labeling with approximate normal-mode and rigid-rotor quantum numbers, have been checked against ones determined from accurate variational nuclear motion computations employing exact kinetic energy operators as well as against previous compilations of energy levels. The extensive list of MARVEL lines and levels obtained are deposited in the supplementary data of this paper, as well as in a distributed information system applied to water, W@DIS, where they can easily be retrieved. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.; Al Derzi, Afaf R.; Lodi, Lorenzo] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Old Dominion Univ, Norfolk, VA USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble 1, Grenoble, France. [Csaszar, Attila G.; Fabri, Csaba; Furtenbacher, Tibor] Eotvos Lorand Univ, Budapest, Hungary. [Daumont, Ludovic] Univ Reims, Reims, France. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] NIST, Gaithersburg, MD 20899 USA. [Naumenko, Olga V.; Fazliev, Alexander Z.] Russian Acad Sci, Inst Atmospher Opt, Tomsk, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belg, Brussels, Belgium. [Zobov, Nikolai F.; Mizus, Irina I.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod, Russia. RP Tennyson, J (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.UK RI Csaszar, Attila/A-5241-2009; Bernath, Peter/B-6567-2012; Tennyson, Jonathan/I-2222-2012; Lodi, Lorenzo/C-6009-2013; Fabri, Csaba/D-3858-2017; OI Rothman, Laurence/0000-0002-3837-4847; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841 FU International Union of Pure and Applied Chemistry [2004-035-1-100]; European Research Council [267219]; Scientific Research Fund of Hungary [OTKA K77825, NK83583]; National Science Foundation of the U.S.A. [ATM-0803135]; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)]; NASA Earth Observing System [NAG5-13534]; Groupement de Recherche International SAMIA (Spectroscopie d'Absorption des Molecules d'Interet Atmospherique) FX We all thank the International Union of Pure and Applied Chemistry for funding under Project 2004-035-1-100 (a database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Natural Environment Research Council, the Royal Society, the European Research Council under Advanced Investigator Project 267219, the Scientific Research Fund of Hungary (Grant OTKA K77825 and NK83583), NATO, the National Science Foundation of the U.S.A. through Grant No. ATM-0803135, the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (contracts EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaute de Belgique (Action de Recherche Concertees), NASA Earth Observing System (EOS), under Grant NAG5-13534, and the Programme National LEFE (CHAT) of CNRS (INSU). This work is partly supported by the Groupement de Recherche International SAMIA (Spectroscopie d'Absorption des Molecules d'Interet Atmospherique) between CNRS (France) and RFBR (Russia). Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contracts and grants with the National Aeronautics and Space Administration. Dr. Semen N. Mikhailenko is thanked for his help collecting experimental sources of measured transitions. NR 231 TC 73 Z9 78 U1 6 U2 88 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD MAR PY 2013 VL 117 BP 29 EP 58 DI 10.1016/j.jqsrt.2012.10.002 PG 30 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 095VF UT WOS:000315362400005 ER PT J AU Lombardo, RC Christy, JH Cipriani, R AF Lombardo, Roberto C. Christy, John H. Cipriani, Roberto TI The false limpet Siphonaria gigas, a simultaneous hermaphrodite, lives in pairs in rock fissures on the Pacific coast of Panama SO MARINE BIOLOGY LA English DT Article ID PULMONATE LIMPET; SEXUAL SELECTION; SOCIAL MONOGAMY; GASTROPODS; SIZE; COMMUNITIES; ALLOCATION; EVOLUTION; PREDATION; PATTERNS AB The pulmonate limpet Siphonaria gigas, a simultaneous hermaphrodite, lives in the mid- to upper-intertidal zone on rocky shores in the tropical Eastern Pacific. Samples along five transects taken in June-July, 2004, on Culebra Point (8A(0)54'N to 79A(0)31'W), Republic of Panama, showed that 71 % of the population occurred in fissures, a significant preference for this habitat. Of 200 adults in 27 fissures, 150 lived side by side in pairs with their shells touching or nearly so, a significant deviation from the number of pairs expected given a random arrangement. Pair frequency did not increase with limpet density suggesting pairing was not an incidental consequence of crowding. Pair living was unknown in the genus Siphonaria, and is very uncommon among simultaneous hermaphrodites. Reproductive synchrony and restrictions on movement due to predation and environmental stress may limit opportunities for encountering and mating with multiple partners favoring pair living in S. gigas. C1 [Lombardo, Roberto C.] Hokkaido Univ, Dept Marine Biol & Biodivers, Grad Sch Fisheries Sci, Hakodate, Hokkaido 0418611, Japan. [Christy, John H.] Smithsonian Trop Res Inst, Panama City, Panama. [Cipriani, Roberto] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92834 USA. RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM christyj@si.edu FU Smithsonian Tropical Research Institute FX Our gratitude goes to Malina Lopez and Pedro Zevallos for their kind hospitality, to Rebecca Rissanen for assistance in the field, and to The Culebra Nature Center staff for their cooperation and support. This work was supported by a short-term Fellowship at the Smithsonian Tropical Research Institute awarded to R. C. Lombardo. NR 33 TC 0 Z9 0 U1 2 U2 19 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD MAR PY 2013 VL 160 IS 3 BP 729 EP 735 DI 10.1007/s00227-012-2127-y PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 094PD UT WOS:000315275400021 ER PT J AU Murphy, RW Crawford, AJ Bauer, AM Che, J Donnellan, SC Fritz, U Haddad, CFB Nagy, ZT Poyarkov, NA Vences, M Wang, WZ Zhang, YP AF Murphy, Robert W. Crawford, Andrew J. Bauer, Aaron M. Che, Jing Donnellan, Stephen C. Fritz, Uwe Haddad, Celio F. B. Nagy, Zoltan T. Poyarkov, Nikolay A. Vences, Miguel Wang, Wen-Zhi Zhang, Ya-Ping TI Cold Code: the global initiative to DNA barcode amphibians and nonavian reptiles SO MOLECULAR ECOLOGY RESOURCES LA English DT News Item DE amphibia; barcoding; COI; crocodylia; identification; lepidosauria; testudines ID MITOCHONDRIAL-DNA; SPECIES-DIVERSITY; TAXONOMY; BIODIVERSITY; CONSERVATION; TESTUDINES; PRIMERS; TURTLES; NUCLEAR; FROGS AB DNA barcoding facilitates the identification of species and the estimation of biodiversity by using nucleotide sequences, usually from the mitochondrial genome. Most studies accomplish this task by using the gene encoding cytochrome oxidase subunit I (COI; Entrez COX1). Within this barcoding framework, many taxonomic initiatives exist, such as those specializing in fishes, birds, mammals, and fungi. Other efforts center on regions, such as the Arctic, or on other topics, such as health. DNA barcoding initiatives exist for all groups of vertebrates except for amphibians and nonavian reptiles. We announce the formation of Cold Code, the international initiative to DNA barcode all species of these cold-blooded' vertebrates. The project has a Steering Committee, Coordinators, and a home page. To facilitate Cold Code, the Kunming Institute of Zoology, Chinese Academy of Sciences will sequence COI for the first 10 specimens of a species at no cost to the steward of the tissues. C1 [Murphy, Robert W.; Che, Jing; Wang, Wen-Zhi; Zhang, Ya-Ping] Chinese Acad Sci, State Key Lab Genet Resources & Evolut State, Kunming 650223, Peoples R China. [Murphy, Robert W.; Che, Jing; Wang, Wen-Zhi; Zhang, Ya-Ping] Chinese Acad Sci, Yunnan Lab Mol Biol Domest Anim, Kunming Inst Zool, Kunming 650223, Peoples R China. [Murphy, Robert W.] Royal Ontario Museum, Ctr Biodivers & Conservat Biol, Toronto, ON M5S 2C6, Canada. [Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Bauer, Aaron M.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Donnellan, Stephen C.] S Australian Museum, Evolutionary Biol Unit, Adelaide, SA 5000, Australia. [Fritz, Uwe] Museum Zool, D-01109 Dresden, Germany. [Haddad, Celio F. B.] Univ Estadual Paulista, Inst Biociencias, Dept Zool, BR-13506900 Sao Paulo, Brazil. [Nagy, Zoltan T.] Royal Belgian Inst Nat Sci, Joint Expt Mol Unit, Brussels, Belgium. [Poyarkov, Nikolay A.] Moscow MV Lomonosov State Univ, Dept Vertebrate Zool, Moscow 119991, Russia. [Vences, Miguel] Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, D-38106 Braunschweig, Germany. [Zhang, Ya-Ping] Yunnan Univ, Lab Conservat & Utilizat Bioresources, Kunming 650091, Peoples R China. RP Murphy, RW (reprint author), Chinese Acad Sci, State Key Lab Genet Resources & Evolut State, Kunming 650223, Peoples R China. EM bob.murphy@utoronto.ca RI Haddad, Celio/C-4267-2012; Donnellan, Stephen/F-2442-2013; OI Donnellan, Stephen/0000-0002-5448-3226; Murphy, Robert/0000-0001-8555-2338; Vences, Miguel/0000-0003-0747-0817; Crawford, Andrew J./0000-0003-3153-6898 NR 69 TC 34 Z9 37 U1 6 U2 71 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X EI 1755-0998 J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAR PY 2013 VL 13 IS 2 BP 161 EP 167 DI 10.1111/1755-0998.12050 PG 7 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 091EQ UT WOS:000315032600001 ER PT J AU Smith, MA Fernandez-Triana, JL Eveleigh, E Gomez, J Guclu, C Hallwachs, W Hebert, PDN Hrcek, J Huber, JT Janzen, D Mason, PG Miller, S Quicke, DLJ Rodriguez, JJ Rougerie, R Shaw, MR Varkonyi, G Ward, DF Whitfield, JB Zaldivar-Riveron, A AF Smith, M. Alex Fernandez-Triana, J. L. Eveleigh, E. Gomez, J. Guclu, C. Hallwachs, W. Hebert, P. D. N. Hrcek, J. Huber, J. T. Janzen, D. Mason, P. G. Miller, S. Quicke, D. L. J. Rodriguez, J. J. Rougerie, R. Shaw, M. R. Varkonyi, G. Ward, D. F. Whitfield, J. B. Zaldivar-Riveron, A. TI DNA barcoding and the taxonomy of Microgastrinae wasps (Hymenoptera, Braconidae): impacts after 8years and nearly 20000 sequences SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE cytochrome c oxidase; data release; deoxyribonucleic acid barcode; microgastrine; parasitoid ID LEPIDOPTERA-TORTRICIDAE; SPECIES LEPIDOPTERA; NATURAL-HISTORY; AMERICA NORTH; MORPHOLOGY; HOST; CHORISTONEURA; BIODIVERSITY; PARASITOIDS; INTEGRATION AB Microgastrine wasps are among the most species-rich and numerous parasitoids of caterpillars (Lepidoptera). They are often host-specific and thus are extensively used in biological control efforts and figure prominently in trophic webs. However, their extraordinary diversity coupled with the occurrence of many cryptic species produces a significant taxonomic impediment. We present and release the results of 8years (20042011) of DNA barcoding microgastrine wasps. Currently they are the best represented group of parasitoid Hymenoptera in the Barcode of Life Data System (BOLD), a massive barcode storage and analysis data management site for the International Barcoding of Life (iBOL) program. There are records from more than 20000 specimens from 75 countries, including 50 genera (90% of the known total) and more than 1700 species (as indicated by Barcode Index Numbers and 2% MOTU). We briefly discuss the importance of this DNA data set and its collateral information for future research in: (1) discovery of cryptic species and description of new taxa; (2) estimating species numbers in biodiversity inventories; (3) clarification of generic boundaries; (4) biological control programmes; (5) molecular studies of host-parasitoid biology and ecology; (6) evaluation of shifts in species distribution and phenology; and (7) fostering collaboration at national, regional and world levels. The integration of DNA barcoding with traditional morphology-based taxonomy, host records, and other data has substantially improved the accuracy of microgastrine wasp identifications and will significantly accelerate further studies on this group of parasitoids. C1 [Smith, M. Alex; Fernandez-Triana, J. L.; Hebert, P. D. N.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Smith, M. Alex; Fernandez-Triana, J. L.; Hebert, P. D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Fernandez-Triana, J. L.; Mason, P. G.] Agr & Agri Food Canada, Res Ctr, Ottawa, ON K1A 0C6, Canada. [Eveleigh, E.] Nat Resources Canada, Atlantic Forestry Ctr, Canadian Forest Serv, Fredericton, NB E3B 5P7, Canada. [Gomez, J.] Colegio Frontera Sur, San Cristobal de las Casa 29290, Chiapas, Mexico. [Guclu, C.] Ataturk Univ, Fac Agr, Dept Plant Protect, TR-25240 Erzurum, Turkey. [Hallwachs, W.; Janzen, D.] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Hrcek, J.] Univ S Bohemia, Czech Acad Sci, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Hrcek, J.] Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Huber, J. T.] Agr & Agri Food Canada, Nat Resources Canada, Canadian Natl Collect Insects, Res Ctr, Ottawa, ON K1A 0C6, Canada. [Miller, S.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Quicke, D. L. J.] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Ascot SL5 7PY, Berks, England. [Quicke, D. L. J.] Nat Hist Museum, Dept Entomol, London SW7 5DB, England. [Rodriguez, J. J.] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Rougerie, R.] Univ Rouen, Lab ECODIV, F-76821 Mont St Aignan, France. [Shaw, M. R.] Natl Museums Scotland, Honorary Res Associate, Edinburgh EH1 1JF, Midlothian, Scotland. [Varkonyi, G.] Friendship Pk Res Ctr, Finnish Environm Inst, FI-88900 Kuhmo, Finland. [Ward, D. F.] New Zealand Arthropod Collect, Auckland, New Zealand. [Whitfield, J. B.] Univ Illinois, Dept Entomol, Urbana, IL 62801 USA. [Zaldivar-Riveron, A.] Univ Nacl Autonoma Mexico, Colecc Nacl Insectos, Inst Biol, Copilco Coyoacan 04510, DF, Mexico. RP Smith, MA (reprint author), Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. EM salex@uoguelph.ca; jftriana@uoguelph.ca RI Smith, M Alex/B-4468-2013; Hebert, Paul/C-4161-2013; Varkonyi, Gergely/I-2310-2012; Rougerie, Rodolphe/D-2930-2009; Hrcek, Jan/D-7335-2015; Gomez, Jaime/O-1717-2016 OI Smith, M Alex/0000-0002-8650-2575; Hebert, Paul/0000-0002-3081-6700; Varkonyi, Gergely/0000-0002-7977-2753; Miller, Scott/0000-0002-4138-1378; Rougerie, Rodolphe/0000-0003-0937-2815; Hrcek, Jan/0000-0003-0711-6447; Gomez, Jaime/0000-0002-9704-9761 FU NSF [DEB 07-17402, 1020510, DEB 0515699, OISE-0809175]; Natural Sciences and Engineering Research Council of Canada (NSERC); National Center for Ecological Analysis and Synthesis postdoctoral fellowship; "Defining New Zealand's Land Biota" programme (MSI); International Mobility Fund grant; CONACyT (Red del Codigo de Barras de la Vida); Natural Resources Canada, Canadian Forest Service; Government of Canada through Genome Canada; Ontario Genomics Institute [2008-0GI-ICI-03]; US National Science Foundation [DEB 0841885, 0816749, 0515678]; Czech Science Foundation [206/08/H044, 206/09/0115, P505/10/0673]; Czech Ministry of Education [LC06073, ME9082, MSM6007665801]; Grant Agency of the University of South Bohemia [GAJU 136/2010/P] FX JFT is greatly indebted to all curators that kindly sent extensive samples of Microgastrinae and allowed some of them to be barcoded: Kees van Achterberg (the Netherlands), Antonius van Harten (UAE), Mark Shaw (UK), Michael Sharkey and Robert Zuparko (US), the Sweddish Malaise Trap Project (Sweden) and many Canadian institutions. JBW was supported by NSF grants DEB 07-17402 and 1020510. DHJ supported by NSF DEB 0515699 and DHJ and WH emphatically and gratefully acknowledge the support of the parataxonomist team in finding and rearing the caterpillars and their parasites from Area de Conservacion Guanacaste, Costa Rica and the Guanacaste Dry Forest Conservation Fund and the Wedge Foundation for funding portions of the research. MAS was supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. JR was supported by a National Center for Ecological Analysis and Synthesis postdoctoral fellowship and NSF Doctoral Dissertation Enhancement Program award OISE-0809175. DFW and JFT were supported by The "Defining New Zealand's Land Biota" programme (MSI), and an International Mobility Fund grant. AZR was supported by grants given by CONACyT (Red del Codigo de Barras de la Vida; proyecto SEP-Ciencia Basica convocatoria 2008). EE gratefully acknowledges the support of Natural Resources Canada, Canadian Forest Service. Laboratory analyses on sequences generated since 2009 were funded by the Government of Canada through Genome Canada and the Ontario Genomics Institute (2008-0GI-ICI-03). For those specimens collected in Canadian National Parks by the Biodiversity Institute of Ontario's BIObus program we gratefully acknowledge the support from Parks Canada (permit NAP-2008-1636). The Papua New Guinea work, in collaboration with Vojtech Novotny, George Weiblen and Yves Basset, was supported by the US National Science Foundation (DEB 0841885, 0816749, 0515678), Czech Science Foundation (206/08/H044, 206/09/0115 and P505/10/0673), Czech Ministry of Education (LC06073, ME9082 and MSM6007665801) and Grant Agency of the University of South Bohemia (GAJU 136/2010/P). NR 49 TC 31 Z9 33 U1 3 U2 89 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAR PY 2013 VL 13 IS 2 BP 168 EP 176 DI 10.1111/1755-0998.12038 PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 091EQ UT WOS:000315032600002 ER PT J AU Cheesman, AW Winter, K AF Cheesman, Alexander W. Winter, Klaus TI Elevated night-time temperatures increase growth in seedlings of two tropical pioneer tree species SO NEW PHYTOLOGIST LA English DT Article DE carbon balance; night-time warming; Panama; photosynthesis; respiration ID PLANT RESPIRATION; CARBON-DIOXIDE; RAIN-FOREST; PHENOTYPIC PLASTICITY; POPULUS-DELTOIDES; DARK RESPIRATION; MOUNTAIN PASSES; CLIMATE MODEL; GRAIN-SORGHUM; SEED-SET AB Increased night-time temperatures, through their influence on dark respiration, have been implicated as a reason behind decreasing growth rates in tropical trees in the face of contemporary climate change. Seedlings of two neo-tropical tree species (Ficus insipida and Ochroma pyramidale) were grown in controlled-environment chambers at a constant daytime temperature (33 degrees C) and a range of increasing night-time temperatures (22, 25, 28, 31 degrees C) for between 39d and 54d. Temperature regimes were selected to represent a realistic baseline condition for lowland Panama, and a rise in night-time temperatures far in excess of those predicted for Central America in the coming decades. Experiments were complemented by an outdoor open-top chamber study in which night-time temperatures were elevated by 2.4 degrees C above ambient. Increasing night-time temperatures resulted in >2-fold increase in biomass accumulation in growth-chamber studies despite an increase in leaf-level dark respiration. Similar trends were seen in open-top chambers, in which elevated night-time temperatures resulted in stimulation of growth. These findings challenge simplistic considerations of photosynthesis-directed growth, highlighting the role of temperature-dependent night-time processes, including respiration and leaf development as drivers of plant performance in the tropics. C1 [Cheesman, Alexander W.; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cheesman, AW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM alexander.cheesman@gmail.com RI Cheesman, Alexander/H-5918-2013 OI Cheesman, Alexander/0000-0003-3931-5766 FU Smithsonian Tropical Research Institute through the Center for Tropical Forest Studies (CTFS) Smithsonian Institute Global Earth Observatory (SIGEO) FX This work was supported by the Smithsonian Tropical Research Institute through the Center for Tropical Forest Studies (CTFS) Smithsonian Institute Global Earth Observatory (SIGEO). We thank Jorge Aranda for logistical support at the Santa Cruz facility; and Timothy Davidson, Kelly Anderson, Helene C. Muller-Landau and three anonymous reviewers for constructive comments on previous drafts of this manuscript. NR 63 TC 20 Z9 21 U1 1 U2 91 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1469-8137 J9 NEW PHYTOL JI New Phytol. PD MAR PY 2013 VL 197 IS 4 BP 1185 EP 1192 DI 10.1111/nph.12098 PG 8 WC Plant Sciences SC Plant Sciences GA 086AU UT WOS:000314656200018 PM 23278464 ER PT J AU Dodonov, AV AF Dodonov, A. V. TI Continuous intracavity monitoring of the dynamical Casimir effect SO PHYSICA SCRIPTA LA English DT Article ID OPTICAL PARAMETRIC OSCILLATOR; INJECTED SQUEEZED VACUUM; JAYNES-CUMMINGS MODEL; N 2-LEVEL ATOMS; RESONANCE FLUORESCENCE; CAVITY-MODE; SINGLE-ATOM; 2ND-HARMONIC GENERATION; STATISTICAL PROPERTIES; NONSTATIONARY CAVITY AB Dynamical Casimir effect (DCE) is the name assigned to the process of generating quanta from vacuum due to an accelerated motion of macroscopic neutral bodies (mirrors) or time-modulation of cavity material properties, as well as the simulation of such processes. Here I review the theoretical results on the detection of DCE using intracavity quantum detectors, such as multi-level atoms, atomic networks and harmonic oscillators. I also stress the mathematical equivalence of this problem to the physics of optical parametric oscillators interacting with atoms or quantum wells, studied in quantum nonlinear optics. C1 [Dodonov, A. V.] Univ Brasilia, Inst Fis, BR-70910900 Brasilia, DF, Brazil. [Dodonov, A. V.] Univ Brasilia, Int Ctr Condensed Matter Phys, BR-70910900 Brasilia, DF, Brazil. [Dodonov, A. V.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Dodonov, AV (reprint author), Univ Brasilia, Inst Fis, POB 04455, BR-70910900 Brasilia, DF, Brazil. EM adodonov@fis.unb.br RI Dodonov, Alexander/N-2730-2014 FU CNPq, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico-Brazil; Decanato de Pesquisa e Pos-Graduacao (DPP-UnB, Brazil) FX The present work was supported by CNPq, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico-Brazil. Partial support by Decanato de Pesquisa e Pos-Graduacao (DPP-UnB, Brazil) is acknowledged. NR 62 TC 6 Z9 6 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-8949 J9 PHYS SCRIPTA JI Phys. Scr. PD MAR PY 2013 VL 87 IS 3 AR 038103 DI 10.1088/0031-8949/87/03/038103 PG 7 WC Physics, Multidisciplinary SC Physics GA 093LS UT WOS:000315194000025 ER PT J AU Eisert, R Oftedal, OT Barrell, GK AF Eisert, Regina Oftedal, Olav T. Barrell, Graham K. TI Milk Composition in the Weddell Seal Leptonychotes weddellii: Evidence for a Functional Role of Milk Carbohydrates in Pinnipeds SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID LINEAR-REGRESSION PROCEDURES; CHEMICAL-CHARACTERIZATION; HALICHOERUS-GRYPUS; HOODED SEAL; LACTATION STRATEGIES; CYSTOPHORA-CRISTATA; MAMMARY-GLAND; ELEPHANT SEAL; ST-LAWRENCE; FUR-SEAL AB We propose that secretion of milk sugar has important consequences for the metabolic economies of lactating phocid seals and their pups. Milk was collected from 21 Weddell seals Leptonychotes weddellii in McMurdo Sound, Antarctica, and assayed by standard methods. Milk composition changed over the course of lactation, but at mid- to late lactation (16-40 d postpartum), Weddell seal milk composition was relatively constant at 33.8% +/- 0.82% water, 54.0% +/- 0.80% fat, 10.1% +/- 0.16% crude protein, 0.84% +/- 0.03% sugar, 0.75% +/- 0.02% ash, and 23.3 +/- 0.3 kJ g(-1) whole milk (WM). At this stage, milk composition varied among individual seals in all assayed constituents except ash. The concentration of sugar in the aqueous phase of Weddell seal milk (24.9 +/- 0.6 g sugar L-1 water) was ca. 44%-77% of levels found in terrestrial carnivores, indicating that the low sugar concentration of WM is primarily due to its high fat content, not alteration of the aqueous phase. In early lactation, fasting Weddell seals were estimated to devote 39 g d(-1) glucose to milk sugar synthesis, an amount similar to the estimated demand of the maternal brain. This additional glucose demand must be covered by gluconeogenesis in fasting animals and represents a considerable additional drain on maternal resources. However, provision of sugar to offspring at rates sufficient to meet neonatal substrate requirements appears to be essential for efficient fat and protein deposition and thus may be an important component of the phocid reproductive strategy of rapid growth and early weaning. C1 [Eisert, Regina; Oftedal, Olav T.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Eisert, Regina] Univ Canterbury, Christchurch 8140, New Zealand. [Barrell, Graham K.] Lincoln Univ, Fac Agr & Life Sci, Lincoln 7647, New Zealand. RP Eisert, R (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM eisertr@si.edu FU Antarctica New Zealand; New Zealand Lotteries Science Grants Board; Science Research Grant [AP52833]; Smithsonian Visiting Scholar Grant; National Science Foundation-Office of Polar Programs [ANT-0538592] FX We thank our teams who assisted in the field in 1998 (J. Banks, D. Geddes, P. Isherwood, S. Leslie, B. Stewart, H. Stoklosinski, and particularly S. Ramdohr from the Alfred-Wegener-Institute of Bremerhaven, Germany) and in 2006 (D. Boness, D. Boritt, R. Joss, B. Krafft, M. Lara, M. Riser, J. Robinson, and H. Routti). We also thank the staff at Scott Base and McMurdo Station for their support of our research. All analytical work was completed at the Nutrition Laboratory, Smithsonian National Zoological Park, and we are grateful to laboratory manager M. Jakubasz and all the interns who helped with milk analysis (1999: D. Hellinga, K. Roback, and L. Nelson; 2008/2009: J. Behler, R. Harley, M. Collins, C. Petzinger, K. Smythe, and M. Snyder). R.E. thanks M. Maslanka and M. Power for sharing their interns, J. Seidensticker for his support, and J. Noordhof for commenting on the manuscript. This work was supported by Antarctica New Zealand (field logistics in 1998), New Zealand Lotteries Science Grants Board, Science Research Grant AP52833 to G.K.B., a Smithsonian Visiting Scholar Grant to R.E., and National Science Foundation-Office of Polar Programs grant ANT-0538592 to O.T.O., R.E., and D. Boness. NR 158 TC 7 Z9 7 U1 3 U2 46 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAR-APR PY 2013 VL 86 IS 2 BP 159 EP 175 DI 10.1086/669036 PG 17 WC Physiology; Zoology SC Physiology; Zoology GA 095KP UT WOS:000315333600001 PM 23434776 ER PT J AU Clough, GW AF Clough, G. Wayne TI From the Castle SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAR PY 2013 VL 43 IS 11 BP 8 EP 8 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 095VV UT WOS:000315364000002 ER PT J AU Ackermann, M Ajello, M Allafort, A Asano, K Atwood, WB Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Bloom, ED Bonamente, E Borgland, AW Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Burnett, TH Busetto, G Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Charles, E Chaty, S Chekhtman, A Cheung, CC Chiang, J Cillis, AN Ciprini, S Claus, R Cohen-Tanugi, J Colafrancesco, S Conrad, J Cutini, S D'Ammando, F de Palma, F Dermer, CD Silva, EDE Drell, S Drlica-Wagner, A Dubois, R Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grandi, P Grenier, IA Grove, JE Guiriec, S Hadasch, D Hayashida, M Hays, E Horan, D Hou, X Hughes, RE Jackson, MS Jogler, T Johannesson, G Johnson, RP Johnson, AS Kamae, T Kataoka, J Kerr, M Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lavalley, C Lee, SH Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mazziotta, MN McConville, W McEnery, JE Mehault, J Michelson, PF Mignani, RP Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nemmen, R Nishino, S Norris, JP Nuss, E Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Pelassa, V Perkins, JS Pesce-Rollins, M Pierbattista, M Piron, F Pivato, G Poon, H Porter, TA Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Reyes, LC Ritz, S Rochester, LS Romoli, C Roth, M Sanchez, DA Parkinson, PMS Scargle, JD Sgro, C Siskind, EJ Snyder, A Spandre, G Spinelli, P Stephens, TE Suson, DJ Tajima, H Takahashi, H Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tibolla, O Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V von Kienlin, A Waite, AP Wallace, E Weltevrede, P Winer, BL Wood, KS Wood, M Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Asano, K. Atwood, W. B. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Burnett, T. H. Busetto, G. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Charles, E. Chaty, S. Chekhtman, A. Cheung, C. C. Chiang, J. Cillis, A. N. Ciprini, S. Claus, R. Cohen-Tanugi, J. Colafrancesco, S. Conrad, J. Cutini, S. D'Ammando, F. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, S. Drlica-Wagner, A. Dubois, R. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grandi, P. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hayashida, M. Hays, E. Horan, D. Hou, X. Hughes, R. E. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, R. P. Johnson, A. S. Kamae, T. Kataoka, J. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lavalley, C. Lee, S. -H. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McConville, W. McEnery, J. E. Mehault, J. Michelson, P. F. Mignani, R. P. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nemmen, R. Nishino, S. Norris, J. P. Nuss, E. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Pelassa, V. Perkins, J. S. Pesce-Rollins, M. Pierbattista, M. Piron, F. Pivato, G. Poon, H. Porter, T. A. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Reyes, L. C. Ritz, S. Rochester, L. S. Romoli, C. Roth, M. Sanchez, D. A. Parkinson, P. M. Saz Scargle, J. D. Sgro, C. Siskind, E. J. Snyder, A. Spandre, G. Spinelli, P. Stephens, T. E. Suson, D. J. Tajima, H. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tibolla, O. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. von Kienlin, A. Waite, A. P. Wallace, E. Weltevrede, P. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. Zimmer, S. TI DETERMINATION OF THE POINT-SPREAD FUNCTION FOR THE FERMI LARGE AREA TELESCOPE FROM ON-ORBIT DATA AND LIMITS ON PAIR HALOS OF ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: halos; gamma rays: galaxies; instrumentation: detectors; intergalactic medium ID EXTRAGALACTIC MAGNETIC-FIELDS; VHE GAMMA-RAYS; TEV BLAZARS; BACKGROUND LIGHT; SPACE-TELESCOPE; SOURCE CATALOG; 1ES 0229+200; PULSAR; CONSTRAINTS; DISCOVERY AB The Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope is a pair-conversion telescope designed to detect photons with energies from approximate to 20 MeV to > 300 GeV. The pre-launch response functions of the LAT were determined through extensive Monte Carlo simulations and beam tests. The point-spread function (PSF) characterizing the angular distribution of reconstructed photons as a function of energy and geometry in the detector is determined here from two years of on-orbit data by examining the distributions of gamma rays from pulsars and active galactic nuclei (AGNs). Above 3 GeV, the PSF is found to be broader than the pre-launch PSF. We checked for dependence of the PSF on the class of gamma-ray source and observation epoch and found none. We also investigated several possible spatial models for pair-halo emission around BL Lac AGNs. We found no evidence for a component with spatial extension larger than the PSF and set upper limits on the amplitude of halo emission in stacked images of low-and high-redshift BL Lac AGNs and the TeV blazars 1ES0229 + 200 and 1ES0347-121. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Allafort, A.; Bechtol, K.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Snyder, A.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ajello, M.; Allafort, A.; Bechtol, K.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, S.; Drlica-Wagner, A.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Snyder, A.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan. [Atwood, W. B.; Johnson, R. P.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Atwood, W. B.; Johnson, R. P.; Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaty, S.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Busetto, G.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Busetto, G.; Buson, S.; Pivato, G.; Poon, H.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; D'Ammando, F.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brandt, T. J.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Brandt, T. J.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Burnett, T. H.; Roth, M.; Wallace, E.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Cheung, C. C.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA. [Cillis, A. N.] Inst Astron & Fis Espacio, Parbellon IAFE, RA-1428 Buenos Aires, DF, Argentina. [Cillis, A. N.; Ferrara, E. C.; Gehrels, N.; Hays, E.; McConville, W.; McEnery, J. E.; Moiseev, A. A.; Nemmen, R.; Perkins, J. S.; Stephens, T. E.; Thompson, D. 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S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stephens, T. E.] Wyle Labs, El Segundo, CA 90245 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Weltevrede, P.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM mar0@uw.edu; mdwood@slac.stanford.edu RI Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016; Tosti, Gino/E-9976-2013; Moskalenko, Igor/A-1301-2007; Saz Parkinson, Pablo Miguel/I-7980-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012 OI orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Mazziotta, Mario /0000-0001-9325-4672; Stephens, Thomas/0000-0003-3065-6871; Grandi, Paola/0000-0003-1848-6013; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; Moskalenko, Igor/0000-0001-6141-458X; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888 FU K. A. Wallenberg Foundation; Commonwealth Government; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. We thank our colleagues for their assistance with the radio timing observations.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. NR 41 TC 25 Z9 25 U1 0 U2 22 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 54 DI 10.1088/0004-637X/765/1/54 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900054 ER PT J AU Czekala, I Berger, E Chornock, R Pastorello, A Marion, GH Margutti, R Botticella, MT Challis, P Ergon, M Smartt, S Sollerman, J Vinko, J Wheeler, JC AF Czekala, Ian Berger, E. Chornock, R. Pastorello, A. Marion, G. H. Margutti, R. Botticella, M. T. Challis, P. Ergon, M. Smartt, S. Sollerman, J. Vinko, J. Wheeler, J. C. TI THE UNUSUALLY LUMINOUS EXTRAGALACTIC NOVA SN 2010U SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; supernovae: individual (SN 2010U); X-rays: stars ID HOBBY-EBERLY TELESCOPE; CLASSICAL NOVAE; SPATIAL-DISTRIBUTION; STELLAR POPULATION; CENTRAL REGION; LMC 1991; M31; EVOLUTION; SPECTRA; GALAXY AB We present observations of the unusual optical transient SN 2010U, including spectra taken 1.03 days to 15.3 days after maximum light that identify it as a fast and luminous Fe II type nova. Our multi-band light curve traces the fast decline (t(2) = 3.5 +/- 0.3 days) from maximum light (M-V = -10.2 +/- 0.1 mag), placing SN 2010U in the top 0.5% of the most luminous novae ever observed. We find typical ejecta velocities of approximate to 1100 km s(-1) and that SN 2010U shares many spectral and photometric characteristics with two other fast and luminous Fe II type novae, including Nova LMC 1991 and M31N-2007-11d. For the extreme luminosity of this nova, the maximum magnitude versus rate of decline relationship indicates a massive white dwarf (WD) progenitor with a low pre-outburst accretion rate. However, this prediction is in conflict with emerging theories of nova populations, which predict that luminous novae from massive WDs should preferentially exhibit an alternate spectral type (He/N) near maximum light. C1 [Czekala, Ian; Berger, E.; Chornock, R.; Marion, G. H.; Margutti, R.; Challis, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pastorello, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Marion, G. H.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Botticella, M. T.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Ergon, M.; Sollerman, J.] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Smartt, S.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Vinko, J.] Univ Szeged, Dept Opt & Quantumelect, Szeged, Hungary. RP Czekala, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. EM iczekala@cfa.harvard.edu OI Sollerman, Jesper/0000-0003-1546-6615; Czekala, Ian/0000-0002-1483-8811 FU NSF [AST 11-09881]; Hungarian OTKA [K76816]; UK Science and Technology Facilities Council; Gemini Observatory [GN-2010A-Q-30] FX I. C. thanks Greg Schwarz, Robert Williams, Maxwell Moe, Alica Soderberg, Warren Brown, James Moran, and Rosanne Di Stefano for valuable conversations about nova physics, and Wen-fai Fong for helpful comments on this manuscript. We graciously acknowledge the amateur astronomers who contributed critical discovery images: K. Itagaki, J. Brimacombe, T. Yusa, and J. Nicolas. I. C. is supported by the NSF Graduate Research Fellowship Grant. J.C.W.'s group at UT Austin is supported by NSF Grant AST 11-09881. J. V. is supported by Hungarian OTKA Grant K76816. This research was completed through the use of many facilities. It is based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de losMuchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. This research is based on observations obtained at the Gemini Observatory under program GN-2010A-Q-30 and principal investigator Edo Berger. Gemini Observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology FacilitiesCouncil (United Kingdom), theNational Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Cienciae Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). We acknowledge the use of public data from the Swift data archive. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. The NIST Atomic Spectra Database was used (Ralchenko et al. 2011). NR 71 TC 4 Z9 4 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 57 DI 10.1088/0004-637X/765/1/57 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900057 ER PT J AU Green, P AF Green, Paul TI INNOCENT BYSTANDERS: CARBON STARS FROM THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; stars: carbon; stars: statistics; surveys ID DQ WHITE-DWARFS; HIGH GALACTIC LATITUDE; SPHEROIDAL GALAXY; CH STARS; X-RAY; SOURCE CATALOG; PROPER-MOTION; BINARY NATURE; BARIUM STARS; LOCAL GROUP AB Among stars showing carbon molecular bands (C stars), the main-sequence dwarfs, likely in post-mass transfer binaries, are numerically dominant in the Galaxy. Via spectroscopic selection from the Sloan Digital Sky Survey, we retrieve 1220 high galactic latitude C stars, similar to 5 times more than previously known, including a wider variety than past techniques such as color or grism selection have netted, and additionally yielding 167 DQ white dwarfs. Of the C stars with proper motion measurements, we identify 69% clearly as dwarfs (dCs), while similar to 7% are giants. The dCs likely span absolute magnitudes M-i from similar to 6.5 to 10.5. "G-type" dC stars with weak CN and relatively blue colors are probably the most massive dCs still cool enough to show C-2 bands. We report Balmer emission in 22 dCs, none of which are G-types. We find 8 new DA/dC stars in composite spectrum binaries, quadrupling the total sample of these "smoking guns" for AGB binary mass transfer. Eleven very red C stars with strong red CN bands appear to be "N"-type AGB stars at large Galactocentric distances, one likely a new discovery in the dIrr galaxy Leo A. Two such stars within 30' of each other may trace a previously unidentified dwarf galaxy or tidal stream at similar to 40 kpc. We explore the multiwavelength properties of the sample and report the first X-ray detection of a dC star, which shows strong Balmer emission. Our own spectroscopic survey additionally provides the dC surface density from a complete sample of dwarfs limited by magnitude, color, and proper motion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Green, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University,; United States Naval Observatory; University of Washington FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 71 TC 19 Z9 19 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 12 DI 10.1088/0004-637X/765/1/12 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900012 ER PT J AU Moyerman, S Bierman, E Ade, PAR Aiken, R Barkats, D Bischoff, C Bock, JJ Chiang, HC Dowell, CD Duband, L Hivon, EF Holzapfel, WL Hristov, VV Jones, WC Kaufman, J Keating, BG Kovac, JM Kuo, CL Leitch, EM Mason, PV Matsumura, T Nguyen, HT Ponthieu, N Pryke, C Richter, S Rocha, G Sheehy, C Takahashi, YD Tolan, JE Wollack, E Yoon, KW AF Moyerman, S. Bierman, E. Ade, P. A. R. Aiken, R. Barkats, D. Bischoff, C. Bock, J. J. Chiang, H. C. Dowell, C. D. Duband, L. Hivon, E. F. Holzapfel, W. L. Hristov, V. V. Jones, W. C. Kaufman, J. Keating, B. G. Kovac, J. M. Kuo, C. L. Leitch, E. M. Mason, P. V. Matsumura, T. Nguyen, H. T. Ponthieu, N. Pryke, C. Richter, S. Rocha, G. Sheehy, C. Takahashi, Y. D. Tolan, J. E. Wollack, E. Yoon, K. W. TI SCIENTIFIC VERIFICATION OF FARADAY ROTATION MODULATORS: DETECTION OF DIFFUSE POLARIZED GALACTIC EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: structure; instrumentation: polarimeters; techniques: polarimetric ID PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND TEMPERATURE; ANGULAR SCALE INTERFEROMETER; SOUTH-POLE TELESCOPE; POWER SPECTRUM; 2003 FLIGHT; ANISOTROPY; QUAD; POLARIMETRY; MAPS AB The design and performance of a wide bandwidth linear polarization modulator based on the Faraday effect is described. Faraday Rotation Modulators (FRMs) are solid-state polarization switches that are capable of modulation up to 10 kHz. Six FRMs were utilized during the 2006 observing season in the Background Imaging of Cosmic Extragalactic Polarization (BICEP) experiment; three FRMs were used at each of BICEP's 100 and 150 GHz frequency bands. The technology was verified through high signal-to-noise detection of Galactic polarization using two of the six FRMs during four observing runs in 2006. The features exhibit strong agreement with BICEP's measurements of the Galaxy using non-FRM pixels and with the Galactic polarization models. This marks the first detection of high signal-to-noise mm-wave celestial polarization using fast, active optical modulation. The performance of the FRMs during periods when they were not modulated was also analyzed and compared to results from BICEP's 43 pixels without FRMs. C1 [Moyerman, S.; Bierman, E.; Kaufman, J.; Keating, B. G.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92037 USA. [Ade, P. A. R.] Univ Wales Coll Cardiff, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aiken, R.; Hristov, V. V.; Jones, W. C.; Mason, P. V.; Richter, S.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Bischoff, C.; Kovac, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Dowell, C. D.; Nguyen, H. T.; Rocha, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chiang, H. C.; Jones, W. C.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Duband, L.] Commissariat Energie Atom Apostrophe, SBT, F-38054 Grenoble, France. [Hivon, E. F.] Inst Astrophys, F-75014 Paris, France. [Holzapfel, W. L.; Takahashi, Y. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kuo, C. L.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Palo Alto, CA 94305 USA. [Kuo, C. L.; Tolan, J. E.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Leitch, E. M.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Matsumura, T.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki, Japan. [Ponthieu, N.] Univ Paris 11, Inst Astrophys Spaciale, F-91405 Orsay, France. [Pryke, C.; Sheehy, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Wollack, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Moyerman, S (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92037 USA. EM smoyerma@ucsd.edu RI Holzapfel, William/I-4836-2015; Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Barkats, Denis/0000-0002-8971-1954; Bischoff, Colin/0000-0001-9185-6514; Hivon, Eric/0000-0003-1880-2733 FU American Association of University Women; NSF PECASE Award [AST-0548262]; NASA Science Mission Directorate via the US Planck project; NSF [OPP-0230438]; Caltech Discovery Fund; Caltech Presidents Fund [PF-471]; JPL Research and Technology Fund FX S.M. gratefully acknowledges the American Association of University Women for a fellowship supporting this research. B. G. K. also acknowledges NSF PECASE Award No. AST-0548262. G. R. gratefully acknowledges support by the NASA Science Mission Directorate via the US Planck project.; BICEP is supported by NSF grant OPP-0230438, Caltech Discovery Fund, Caltech Presidents Fund PF-471, JPL Research and Technology Fund, and the late J. Robinson. NR 57 TC 8 Z9 8 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 64 DI 10.1088/0004-637X/765/1/64 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900064 ER PT J AU Qi, CH Oberg, KI Wilner, DJ AF Qi, Chunhua Oeberg, Karin I. Wilner, David J. TI H2CO AND N2H+ IN PROTOPLANETARY DISKS: EVIDENCE FOR A CO-ICE REGULATED CHEMISTRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM; stars: formation; techniques: high angular resolution ID SUBMILLIMETER ARRAY; DETERMINISTIC MODEL; PLANETARY FORMATION; SURFACE-DENSITY; IMAGING SURVEY; SOLAR NEBULA; TW HYDRAE; SNOW LINE; DM TAU; MOLECULES AB We present Submillimeter Array (SMA) observations of H2CO and N2H+ emission in the disks around the T Tauri star TW Hya and the Herbig Ae star HD 163296 at 2 ''-6 '' resolution and discuss the distribution of these species with respect to CO freezeout. The H2CO and N2H+ emission toward HD 163296 does not peak at the continuum emission center that marks the stellar position but is instead significantly offset. Using a previously developed model for the physical structure of this disk, we show that the H2CO observations are reproduced if H2CO is present predominantly in the cold outer disk regions. A model where H2CO is present only beyond the CO snow line (estimated at a radius of 160 AU) matches the observations well. We also show that the average H2CO excitation temperature, calculated from two transitions of H2CO observed in these two disks and a larger sample of disks around T Tauri stars in the DISCS (the Disk Imaging Survey of Chemistry with SMA) program, is consistent with the CO freezeout temperature of similar to 20 K. In addition, we show that N2H+ and H2CO line fluxes in disks are strongly correlated, indicative of co-formation of these species across the sample. Taken together, these results imply that H2CO and N2H+ are generally present in disks only at low temperatures where CO depletes onto grains, consistent with fast destruction of N2H+ by gas-phase CO, and in situ formation of H2CO through hydrogenation of CO ice. In this scenario H2CO, CH3OH, and N2H+ emission in disks should appear as rings with the inner edge at the CO midplane snow line. This prediction can be tested directly using observations from ALMA with higher resolution and better sensitivity. C1 [Qi, Chunhua; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oeberg, Karin I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, Karin I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Smithsonian Institution; Academia Sinica; NASA through Space Telescope Science Institute [NAS 5-26555]; NASA Origins of Solar Systems [NNX11AK63] FX The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We thank Edwin Bergin and Paola D'Alessio for their helpful suggestions, and a referee for constructive comments on the paper. Support for K.I.O. is provided by NASA through a Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. We also acknowledge NASA Origins of Solar Systems grant No. NNX11AK63. NR 56 TC 38 Z9 38 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 34 DI 10.1088/0004-637X/765/1/34 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900034 ER PT J AU Sargent, BA Patel, NA Meixner, M Otsuka, M Riebel, D Srinivasan, S AF Sargent, Benjamin A. Patel, N. A. Meixner, M. Otsuka, M. Riebel, D. Srinivasan, S. TI CO J=2-1 EMISSION FROM EVOLVED STARS IN THE GALACTIC BULGE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; radio lines: stars; stars: AGB and post-AGB ID GIANT BRANCH STARS; ROTATIONAL LINE-PROFILES; SPITZER-SPACE-TELESCOPE; RED SUPERGIANT STARS; MASS-LOSS HISTORY; ALL-SKY SURVEY; OH/IR STARS; AGB STARS; CENTER REGION; FORMING REGIONS AB We observe a sample of eight evolved stars in the Galactic bulge in the CO J = 2-1 line using the Submillimeter Array with angular resolution of 1 ''-4 ''. These stars have been detected previously at infrared wavelengths, and several of them have OH maser emission. We detect CO J = 2-1 emission from three of the sources in the sample: OH 359.943 + 0.260, [SLO2003] A12, and [SLO2003] A51. We do not detect the remaining five stars in the sample because of heavy contamination from the galactic CO emission. Combining CO data with observations at infrared wavelengths constraining dust mass loss from these stars, we determine the gas-to-dust ratios of the Galactic bulge stars for which CO emission is detected. For OH 359.943 + 0.260, we determine a gas mass-loss rate of 7.9 (+/- 2.2) x 10(-5)M(circle dot) yr(-1) and a gas-to-dust ratio of 310 (+/- 89). For [SLO2003] A12, we find a gas mass-loss rate of 5.4 (+/- 2.8) x 10(-5)M(circle dot) yr(-1) and a gas-to-dust ratio of 220 (+/- 110). For [SLO2003] A51, we find a gas mass-loss rate of 3.4 (+/- 3.0) x 10(-5)M(circle dot) yr(-1) and a gas-to-dust ratio of 160 (+/- 140), reflecting the low quality of our tentative detection of the CO J = 2-1 emission from A51. We find that the CO J = 2-1 detections of OH/IR stars in the Galactic bulge require lower average CO J = 2-1 backgrounds. C1 [Sargent, Benjamin A.; Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sargent, Benjamin A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Sargent, Benjamin A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Otsuka, M.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Riebel, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riebel, D.] USN Acad, Dept Phys, Annapolis, MD 21402 USA. [Srinivasan, S.] Inst Astrophys Paris, UPMC CNRS UMR7095, F-75014 Paris, France. RP Sargent, BA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM baspci@rit.edu FU Smithsonian Institution; Academia Sinica; NASA [1407]; NASA ADP grant [NNX11AB06G] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The authors acknowledge Anders Winnberg for discussions via email that have been very helpful in interpreting our SMA data. The authors thank the anonymous referee for comments that greatly improved this manuscript. This work makes use of observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. The original description of the VizieR service was published in A&AS, 143, 23 (Ochsenbein et al. 2000). This research was supported by NASA ADP grant NNX11AB06G. NR 59 TC 0 Z9 0 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 20 DI 10.1088/0004-637X/765/1/20 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900020 ER PT J AU Tobin, JJ Bergin, EA Hartmann, L Lee, JE Maret, S Myers, PC Looney, LW Chiang, HF Friesen, R AF Tobin, John J. Bergin, Edwin A. Hartmann, Lee Lee, Jeong-Eun Maret, Sebastien Myers, Phillip C. Looney, Leslie W. Chiang, Hsin-Fang Friesen, Rachel TI RESOLVED DEPLETION ZONES AND SPATIAL DIFFERENTIATION OF N2H+ AND N2D+ SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; stars: formation ID LOW-MASS PROTOSTARS; SUBMILLIMETER CONTINUUM OBSERVATIONS; RADIO-ASTRONOMICAL SPECTROSCOPY; YOUNG STELLAR OBJECTS; EVOLVED STARLESS CORE; SPITZER C2D SURVEY; DENSE CLOUD CORES; LINE EMISSION; DARK CLOUDS; EVOLUTIONARY SIGNATURES AB We present a study on the spatial distribution of N2D+ and N2H+ in 13 protostellar systems. Eight of thirteen objects observed with the IRAM 30 m telescope show relative offsets between the peak N2D+ (J = 2 -> 1) and N2H+ (J = 1 -> 0) emission. We highlight the case of L1157 using interferometric observations from the Submillimeter Array and Plateau de Bure Interferometer of the N2D+ (J = 3 -> 2) and N2H+ (J = 1 -> 0) transitions, respectively. Depletion of N2D+ in L1157 is clearly observed inside a radius of similar to 2000 AU (7 '') and the N2H+ emission is resolved into two peaks at radii of similar to 1000 AU (3 ''.5), inside the depletion region of N2D+. Chemical models predict a depletion zone in N2D+ and N2H+ due to destruction of H2D+ at T similar to 20 K and the evaporation of CO off dust grains at the same temperature. However, the abundance offsets of 1000 AU between the two species are not reproduced by chemical models, including a model that follows the infall of the protostellar envelope. The average abundance ratios of N2D+ to N2H+ have been shown to decrease as protostars evolve by Emprechtinger et al., but this is the first time depletion zones of N2D+ have been spatially resolved. We suggest that the difference in depletion zone radii for N2H+ and N2D+ is caused by either the CO evaporation temperature being above 20 K or an H-2 ortho-to-para ratio gradient in the inner envelope. C1 [Tobin, John J.; Friesen, Rachel] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Tobin, John J.; Bergin, Edwin A.; Hartmann, Lee] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Gyeonggi Do, South Korea. [Maret, Sebastien] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Myers, Phillip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Looney, Leslie W.; Chiang, Hsin-Fang] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Chiang, Hsin-Fang] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. RP Tobin, JJ (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. EM jtobin@nrao.edu RI Lee , Jeong-Eun/E-2387-2013 FU Smithsonian Institution; Academia Sinica; NASA [HST-HF-51300.01-A, NAS 5-26555]; National Research Foundation of Korea; Ministry of Education, Science and Technology [2012-0002330]; David Dunlap family; University of Toronto FX We thank the referee Paola Caselli for helpful comments that improved the final manuscript. The authors wish to acknowledge useful discussions with K. Oberg. We thank the SMA staff for carrying out the observations, IRAM 30 m staff for allowing us to use the E330 receiver with its interim local oscillator in the Fall of 2009 and assistance with the observations. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. J.T. acknowledges support provided by NASA through Hubble Fellowship grant HST-HF-51300.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. J.-E. Lee was supported by the Basic Science Research Program through the National Research Foundation of Korea, funded by the Ministry of Education, Science and Technology (No. 2012-0002330). R. F. is a Dunlap Fellow at the Dunlap Institute for Astronomy & Astrophysics, University of Toronto. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 75 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 18 DI 10.1088/0004-637X/765/1/18 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900018 ER PT J AU Torrejon, JM Schulz, NS Nowak, MA Testa, P Rodes, JJ AF Torrejon, J. M. Schulz, N. S. Nowak, M. A. Testa, P. Rodes, J. J. TI HOT THERMAL X-RAY EMISSION FROM THE Be STAR HD 119682 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (HD 119682); X-rays: binaries ID GAMMA-CASSIOPEIAE; CHANDRA; SPECTROSCOPY; DISCOVERY; BINARY AB We present an analysis of a series of four consecutive Chandra high-resolution transmission gratings observations, amounting to a total of 150 ks, of the Be X-ray source HD 119682 (=1WGA J1346.5-6255), a member of the new class of. Cas analogs. The Chandra light curve shows significant brightness variations on timescales of hours. However, the spectral distribution appears rather stable within each observation and during the whole campaign. A detailed analysis is not able to detect any coherent pulsation up to a frequency of 0.05 Hz. The Chandra High Energy Transmission Gratings spectrum seems to be devoid of any strong emission line, including Fe K alpha fluorescence. The continuum is well described with the addition of two collisionally ionized plasmas of temperatures kT approximate to 15 keV and 0.2 keV, respectively, by the apec model. Models using photoionized plasma components (mekal) or non-thermal components (powerlaw) give poorer fits, providing support for the pure thermal scenario. These two components are absorbed by a single column with N-H = (0.20(-0.03)(+0.15)) x 10(22) cm(-2) compatible with the interstellar value. We conclude that HD 119682 can be regarded as a pole-on gamma Cas analog. C1 [Torrejon, J. M.; Rodes, J. J.] Univ Alicante, Inst Univ Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain. [Schulz, N. S.; Nowak, M. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torrejon, JM (reprint author), Univ Alicante, Inst Univ Fis Aplicada Ciencias & Tecnol, E-03080 Alicante, Spain. EM jmt@ua.es RI Torrejon, Jose /K-6395-2014; Rodes Roca, Jose Joaquin/K-9259-2014 OI Torrejon, Jose /0000-0002-5967-5163; Rodes Roca, Jose Joaquin/0000-0003-4363-8138 FU Spanish Ministerio de Ciencia e Innovacion (MICINN) [AYA2010-15431, AIB2010DE-00057] FX The authors acknowledge the constructive criticism of an anonymous referee. This work has been supported by the Spanish Ministerio de Ciencia e Innovacion (MICINN) through the grants AYA2010-15431 and AIB2010DE-00057. NR 22 TC 2 Z9 2 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 2013 VL 765 IS 1 AR 13 DI 10.1088/0004-637X/765/1/13 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090CZ UT WOS:000314957900013 ER PT J AU Beltran, JD Lasso, E Madrinan, S Virgo, A Winter, K AF Beltran, J. D. Lasso, E. Madrinan, S. Virgo, A. Winter, K. TI Juvenile tank-bromeliads lacking tanks: do they engage in CAM photosynthesis? SO PHOTOSYNTHETICA LA English DT Article DE bromeliads; CO2 exchange; carbon isotope discrimination; crassulacean acid metabolism; drought stress; Guzmania; heteroblasty; photosynthesis; Werauhia ID CRASSULACEAN ACID METABOLISM; TILLANDSIA-DEPPEANA BROMELIACEAE; CARBON-ISOTOPE COMPOSITION; TROPICAL PIONEER TREE; COMPARATIVE ECOPHYSIOLOGY; WATER RELATIONS; C-3 BROMELIADS; EPIPHYTIC BROMELIADS; VRIESEA-SANGUINOLENTA; DELTA-C-13 VALUES AB In the epiphytic tillandsioids, Guzmania monostachia, Werauhia sanguinolenta, and Guzmania lingulata (Bromeliaceae), juvenile plants exhibit an atmospheric habit, whereas in adult plants the leaf bases overlap and form water-holding tanks. CO2 gas-exchange measurements of the whole, intact plants and delta C-13 values of mature leaves demonstrated that C-3 photosynthesis was the principal pathway of CO2 assimilation in juveniles and adults of all three species. Nonetheless, irrespective of plant size, all three species were able to display features of facultative CAM when exposed to drought stress. The capacity for CAM was the greatest in G. monostachia, allowing drought-stressed juvenile and adult plants to exhibit net CO2 uptake at night. CAM expression was markedly lower in W. sanguinolenta, and minimal in G. lingulata. In both species, low-level CAM merely sufficed to reduce nocturnal respiratory net loss of CO2. delta C-13 values were generally less negative in juveniles than in adult plants, probably indicating increased diffusional limitation of CO2 uptake in juveniles. C1 [Beltran, J. D.; Lasso, E.; Madrinan, S.] Univ Los Andes, Lab Bot, Bogota, Colombia. [Virgo, A.; Winter, K.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Winter, K (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM winterk@si.edu OI Lasso, Eloisa/0000-0003-4586-8674 FU Smithsonian Tropical Research Institute FX J.D.B. was recipient of a short-term fellowship from the Smithsonian Tropical Research Institute and received travel support from the Facultad de Ciencias, Universidad de los Andes. Dayana Agudo performed the delta13C analyses, Jorge Ceballos helped with microscopy, and Oris Acevedo provided logistical support on Barro Colorado Nature Monument. NR 46 TC 4 Z9 4 U1 1 U2 51 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0300-3604 J9 PHOTOSYNTHETICA JI Photosynthetica PD MAR PY 2013 VL 51 IS 1 BP 55 EP 62 DI 10.1007/s11099-012-0077-8 PG 8 WC Plant Sciences SC Plant Sciences GA 092BS UT WOS:000315094400007 ER PT J AU Banda, JM Angryk, RA Martens, PCH AF Banda, J. M. Angryk, R. A. Martens, P. C. H. TI On Dimensionality Reduction for Indexing and Retrieval of Large-Scale Solar Image Data SO SOLAR PHYSICS LA English DT Article DE Dimensionality reduction; Indexing; Retrieval; Content-based image retrieval (CBIR) ID CLASSIFICATION; OSCILLATIONS; FEATURES; SEARCH AB This work investigates the applicability of several dimensionality reduction techniques for large-scale solar data analysis. Using a solar benchmark dataset that contains images of multiple types of phenomena, we investigate linear and nonlinear dimensionality reduction methods in order to reduce our storage and processing costs and maintain a good representation of our data in a new vector space. We present a comparative analysis of several dimensionality reduction methods and different numbers of target dimensions by utilizing different classifiers in order to determine the degree of data dimensionality reduction that can be achieved with these methods, and to discover the method that is the most effective for solar images. After determining the optimal number of dimensions, we then present preliminary results on indexing and retrieval of the dimensionally reduced data. C1 [Banda, J. M.; Angryk, R. A.] Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. [Martens, P. C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Martens, P. C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Banda, JM (reprint author), Montana State Univ, Dept Comp Sci, Bozeman, MT 59717 USA. EM juan.banda@cs.montana.edu; angryk@cs.montana.edu; martens@physics.montana.edu OI Banda, Juan/0000-0001-8499-824X FU NASA [08-SDOSC08-0008, NNH08ZDA001N-SDOSC solicitation, NNX11AM13A, NNH11ZHA003C solicitation] FX This work was supported in part by two NASA Grant Awards: i) No. 08-SDOSC08-0008, funded from NNH08ZDA001N-SDOSC solicitation, and ii) No. NNX11AM13A, funded from NNH11ZHA003C solicitation. We would also like to thank our internal reviewers Michael Schuh, Richard McAllister, and Alexander Engell and the anonymous reviewers during the submission process. NR 77 TC 9 Z9 9 U1 0 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAR PY 2013 VL 283 IS 1 BP 113 EP 141 DI 10.1007/s11207-012-0027-4 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 090NB UT WOS:000314984700008 ER PT J AU Liu, CX Liu, Y Liu, X Chance, K AF Liu Chuanxi Liu Yi Liu, Xiong Chance, Kelly TI Dynamical and chemical features of a cutoff low over northeast China in July 2007: Results from satellite measurements and reanalysis SO ADVANCES IN ATMOSPHERIC SCIENCES LA English DT Article DE stratosphere-troposphere exchange; cutoff low; tropopause; ozone; satellite observation ID STRATOSPHERE-TROPOSPHERE EXCHANGE; OZONE MONITORING INSTRUMENT; OFF-LOW SYSTEMS; MASS-EXCHANGE; CLIMATOLOGY; TROPOPAUSE; HEMISPHERE; ASIA; CYCLONE; AURA AB The European Centre for Medium-Range Weather Forecasts Re-Analysis Interim (ERA-Interim) meteorology and measurements from the Microwave Limb Sounder, High Resolution Dynamics Limb Sounder, and Ozone Monitoring Instrument onboard the Earth Observing System Aura satellite were applied to analyze the dynamical and chemical features of a cutoff low (COL) event over northeast China in early July 2007. The results showed the polar stratospheric origin of an upper-level warm-core cyclone at 100-300 hPa, associated with a funnel-shaped tropopause intruding into the mid-troposphere just above the COL center. The impacts of the stratospheric intrusion on both column ozone and ozone profiles were investigated using satellite measurements. When the intensity of the COL peaked on 10 July 2007, the total column ozone (TCO) increase reached a maximum (40-70 DU). This could be dynamically attributed to both the descent of the tropopause (similar to 75%) and the downward transport of stratospheric ozone across the tropopause (similar to 25%). Analysis of the tropospheric ozone profiles provided evidence for irreversible transport/mixing of ozone-rich stratospheric air across the tropopause near the upper-level front region ahead of the COL center. This ozone intrusion underwent downstream transport by the upper tropospheric winds, leading to further increase in TCO by 12-16 DU over broad regions extending from east China toward the northern Japan Sea via South Korea. Meteorological analysis also showed the precedence of the stratospheric intrusion ahead of the development of cyclones in the middle and lower troposphere. C1 [Liu Chuanxi; Liu Yi] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, Y (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. EM liuyi@mail.iap.ac.cn RI Liu, Xiong/P-7186-2014; AAS, AAS/C-2949-2014 OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577; FU National Basic Research Program of China [2010CB428604]; National Science Foundation of China [41105025]; Dragon 3 Programme [10577]; NASA; Smithsonian Institution FX This work was funded by the National Basic Research Program of China (Grant No. 2010CB428604), National Science Foundation of China (Grant No. 41105025), and the Dragon 3 Programme (ID: 10577). Research at Harvard-Smithsonian was funded by NASA and the Smithsonian Institution. We thank the HIRDLS, MLS, and OMI science teams for providing satellite products. ERA-Interim meteorological reanalysis has been kindly provided by ECMWF. NR 49 TC 7 Z9 8 U1 0 U2 18 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 0256-1530 J9 ADV ATMOS SCI JI Adv. Atmos. Sci. PD MAR PY 2013 VL 30 IS 2 BP 525 EP 540 DI 10.1007/s00376-012-2086-8 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 087FU UT WOS:000314747500021 ER PT J AU Robertson, BA Landis, DA Sillett, TS Loomis, ER Rice, RA AF Robertson, Bruce A. Landis, Douglas A. Sillett, T. Scott Loomis, Elizabeth R. Rice, Robert A. TI Perennial Agroenergy Feedstocks as En Route Habitat for Spring Migratory Birds SO BIOENERGY RESEARCH LA English DT Article DE Biofuels; Agriculture; Grassland birds; Habitat selection; Agroecology; Switchgrass ID PASSERINE MIGRANTS; GRASSLAND BIRDS; STOPOVER; BIOMASS; CONSERVATION; COMMUNITIES; DIVERSITY; ABUNDANCE; COMPETITION; LANDSCAPES AB Increased production of bioenergy crops in North America is projected to exacerbate already heavy demands upon existing agricultural landscapes with potential to impact biodiversity negatively. Grassland specialist birds are an imperilled avifauna for which perennial-based, next-generation agroenergy feedstocks may provide suitable habitat. We take a multi-scaled spatial approach to evaluate the ability of two candidate second-generation agroenergy feedstocks (switchgrass, Panicum virgatum, and mixed grass-forb plantings) to act as spring migratory stopover habitat for birds. In total, we detected 35 bird species in mixed grass-forb plantings and switchgrass plantings, including grassland specialists and species of state and national conservation concern (e.g., Henslow's Sparrow, Ammodramus henslowii). Some evidence indicated that patches with higher arthropod food availability attracted a greater diversity of migrant bird species, but species richness, total bird abundance, and the abundance of grassland specialist species were similar in fields planted with either feedstock. Species richness per unit area (species density) was relatively higher in switchgrass fields. The percent land cover of forest in landscapes surrounding study fields was negatively associated with bird species richness and species density. Habitat patch size and within-patch vegetation structure were unimportant in predicting the diversity or abundance of spring en route bird assemblages. Our results demonstrate that both switchgrass and mixed grass-forb plantings can attract diverse assemblages of migrant birds. As such, industrialized production of these feedstocks as agroenergy crops has the potential to provide a source of en route habitat for birds, particularly where fields are located in relatively unforested landscapes. Because industrialization of cellulosic biomass production will favor as yet unknown harvest and management regimes, predicting the ultimate value of perennial-based biomass plantings for spring migrants remains difficult. C1 [Robertson, Bruce A.; Sillett, T. Scott; Rice, Robert A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Robertson, Bruce A.] Bard Coll, Div Sci Math & Comp, Annandale On Hudson, NY 12504 USA. [Robertson, Bruce A.; Landis, Douglas A.; Loomis, Elizabeth R.] Michigan State Univ, DOE Great Lakes Bioenergy Res Ctr, E Lansing, MI 48824 USA. RP Robertson, BA (reprint author), Bard Coll, Div Sci Math & Comp, 30 Campus Dr, Annandale On Hudson, NY 12504 USA. EM broberts@bard.edu FU Migratory Bird Center of the Smithsonian Conservation Biology Institute, US Fish and Wildlife Service [30181AG045]; DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science) [DE-FC02-07ER64494]; DOE OBP Office of Energy Efficiency and Renewable Energy [DE-AC05-76RL01830]; U.S. National Science Foundation LTER program FX This work was funded by the Migratory Bird Center of the Smithsonian Conservation Biology Institute, US Fish and Wildlife Service (grant # 30181AG045), the DOE Great Lakes Bioenergy Research Center (DOE BER Office of Science DE-FC02-07ER64494), DOE OBP Office of Energy Efficiency and Renewable Energy (DE-AC05-76RL01830), and the U.S. National Science Foundation LTER program. NR 56 TC 8 Z9 8 U1 3 U2 48 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1939-1234 EI 1939-1242 J9 BIOENERG RES JI BioEnergy Res. PD MAR PY 2013 VL 6 IS 1 BP 311 EP 320 DI 10.1007/s12155-012-9258-3 PG 10 WC Energy & Fuels; Environmental Sciences SC Energy & Fuels; Environmental Sciences & Ecology GA 084EA UT WOS:000314518300029 ER PT J AU Vencl, FV Srygley, RB AF Vencl, Fredric V. Srygley, Robert B. TI Enemy targeting, trade-offs, and the evolutionary assembly of a tortoise beetle defense arsenal SO EVOLUTIONARY ECOLOGY LA English DT Article DE Acromis sparsa; Community assembly; Modes of selection; Escalation; Shield; Gregariousness; Guild; Maternal care; Multiple species interactions; Trade-offs ID SHIELD DEFENSE; PLANT DEFENSE; HOST-PLANT; PREDATORS; BEHAVIOR; INSECTS; ECOLOGY; ANTS; GREGARIOUSNESS; HETEROPTERA AB In response to intense enemy selection, immature folivorous insects have evolved elaborate, multi-trait defense arsenals. How enemies foster trait diversification and arsenal assembly depends on which selective mode they impose: whether different enemies select for the same defense or exert conflicting selection on a prey species. Theory has long supposed that the selective advantage of a defense depends on its efficacy against a broad spectrum of enemies, which implies that predator selection is more diffuse than pairwise. Here, we use the multi-trait defense arsenal of the tortoise beetle, Acromis sparsa, which consists of shields, gregariousness and maternal guarding to test whether: (1) diverse enemies have selected for narrowly targeted defenses in the Acromis lineage; (2) newer traits out-performed older ones or vice versa, and; (3) if selection by different enemies results in positive (escalation) trends in defense effectiveness. Because their defenses could be modified or ablated, individuals were rendered differentially protected, and their survival was quantified in a long-term field study. Exclusion experiments evaluated defense efficacy against particular enemy guilds. Logit regression revealed that: (1)no single trait increased survival against the entire enemy suite; (2)trait efficacy was strongly correlated with a particular enemy, consistent with narrow targeting; (3)traits lacked strong cross-resistance among enemies; (4)traits performed synergistically, consistent with the idea of escalation, and; (5)traits interacted negatively to decrease survival, indicative of performance trade-offs. From collation of the phylogenetic histories of arsenal and enemy community assembly we hypothesize that older traits performed better against older enemies and that patterns of both trait and enemy accumulation are consistent with defense escalation. Trade-offs and lack of cross-resistance among defenses imply that enemy selection has been conflicting at the guild level and that negative functional interactions among defenses have fostered the evolution of a defense arsenal of increasing complexity. C1 [Vencl, Fredric V.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Vencl, Fredric V.; Srygley, Robert B.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Srygley, Robert B.] ARS, USDA, No Plains Agr Res Lab, Sidney, MT 59270 USA. RP Vencl, FV (reprint author), SUNY Stony Brook, Stony Brook, NY 11794 USA. EM fvencl@life.bio.sunysb.edu NR 59 TC 7 Z9 7 U1 0 U2 34 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0269-7653 J9 EVOL ECOL JI Evol. Ecol. PD MAR PY 2013 VL 27 IS 2 BP 237 EP 252 DI 10.1007/s10682-012-9603-1 PG 16 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 084FZ UT WOS:000314524900001 ER PT J AU Kitahara, MV Cairns, SD Stolarski, J Miller, DJ AF Kitahara, Marcelo V. Cairns, Stephen D. Stolarski, Jaroslaw Miller, David J. TI Deltocyathiidae, an early-diverging family of Robust corals (Anthozoa, Scleractinia) SO ZOOLOGICA SCRIPTA LA English DT Article ID AZOOXANTHELLATE SCLERACTINIA; CNIDARIA ANTHOZOA; MITOCHONDRIAL; PHYLOGENY; EVOLUTION; ATLANTIC; CARYOPHYLLIIDAE; SYSTEMATICS; DIVERGENCE; PSAMMOCORA AB Kitahara, M.V., Cairns, S.D., Stolarski, J. & Miller, D.J. (2012). Deltocyathiidae, an early-diverging family of Robust corals (Anthozoa, Scleractinia). Zoologica Scripta, 00, 000000. Over the last decade, molecular phylogenetics has called into question some fundamental aspects of coral systematics. Within the Scleractinia, most families composed exclusively by zooxanthellate species are polyphyletic on the basis of molecular data, and the second most speciose coral family, the Caryophylliidae (most members of which are azooxanthellate), is an unnatural grouping. As part of the process of resolving taxonomic affinities of caryophylliids', here a new Robust' scleractinian family (Deltocyathiidae fam. n.) is proposed on the basis of combined molecular (CO1 and 28S rDNA) and morphological data, accommodating the early-diverging clade of traditional caryophylliids (represented today by the genus Deltocyathus). Whereas this family captures the full morphological diversity of the genus Deltocyathus, one species, Deltocyathus magnificus, is an outlier in terms of molecular data, and groups with the Complex coral family Turbinoliidae. Ultrastructural data, however, place D.magnificus within Deltocyathiidae fam. nov. Unfortunately, limited ultrastructural data are as yet available for turbinoliids, but D.magnificus may represent the first documented case of morphological convergence at the microstructural level among scleractinian corals. Marcelo V.Kitahara, Centro de Biologia Marinha, Universidade de SAo Paulo, SAo SebastiAo, S.P. 11600-000, Brazil. E-mail:kitahara@usp.br C1 [Kitahara, Marcelo V.] Univ Sao Paulo, Ctr Biol Marinha, BR-11600000 Sao Sebastiao, SP, Brazil. [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Stolarski, Jaroslaw] Polish Acad Sci, Inst Paleobiol, PL-00818 Warsaw, Poland. [Miller, David J.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [Miller, David J.] James Cook Univ, Sch Pharm & Mol Sci, Townsville, Qld 4811, Australia. RP Kitahara, MV (reprint author), Univ Sao Paulo, Ctr Biol Marinha, BR-11600000 Sao Sebastiao, SP, Brazil. EM kitahara@usp.br; cairnss@si.edu; stolacy@twarda.pan.pl; david.miller@jcu.edu.au RI Kitahara, Marcelo/D-5560-2011; Manager, MEEL/C-4732-2015 FU Sao Paulo State Research Foundation (FAPESP); Australian Research Council (ARC) via the ARC Centre of Excellence for Coral Reef Studies (ARC CoE); Polish Ministry of Science and Higher Education; Fisheries Research and Development Corporation (FRDC); Australian Government Department of Environment, Water, Heritage and the Arts; New Zealand's Ministry of Fisheries; New Zealand's National Institute of Water and Atmospheric Sciences FX This work was supported in part by the Sao Paulo State Research Foundation (FAPESP) via postdoctoral fellowship support for MVK, the Australian Research Council (ARC) via the ARC Centre of Excellence for Coral Reef Studies (ARC CoE) to DJM and the Polish Ministry of Science and Higher Education to JS. The authors thank Philippe Bouchet (MNHN) who generously loaned the New Caledonian material from the Paris Museum to the Smithsonian Institution, and Bertrand Richer de Forges and IRD-Noumea and MNHN staff and collaborators for their great effort in collecting and preserving the New Caledonian specimens examined in the present study. We extend our gratitude to Felicity McEnnulty (CSIRO) for the loan of material collected off Australia, which was conducted by the Australian CSIRO Marine Research with funding from the Fisheries Research and Development Corporation (FRDC), the Australian Government Department of Environment, Water, Heritage and the Arts, New Zealand's Ministry of Fisheries and New Zealand's National Institute of Water and Atmospheric Sciences. We also thank Kevin Blake and Jen Whan (JCU) for advice in electron microscopy. Special thanks are due to Carden Wallace and Barbara Done (MTQ) for the use of facilities at the Museum of Tropical Queensland. NR 50 TC 3 Z9 3 U1 1 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD MAR PY 2013 VL 42 IS 2 BP 201 EP 212 DI 10.1111/j.1463-6409.2012.00575.x PG 12 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 086BK UT WOS:000314657800006 ER PT J AU Sonneborn, DA AF Sonneborn, D. A. TI Muslim Rap, Halal Soaps, and Revolutionary Theater: Artistic Developments in the Muslim World. SO ETHNOMUSICOLOGY LA English DT Book Review C1 [Sonneborn, D. A.] Smithsonian Inst, Washington, DC 20560 USA. RP Sonneborn, DA (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 USA SN 0014-1836 EI 2156-7417 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 2013 VL 57 IS 2 BP 347 EP 351 PG 5 WC Music SC Music GA AC0LU UT WOS:000332187600010 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI The Bioarchaeology of Individuals SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 [Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV NEW MEXICO, DEPT ANTHROPOL PI ALBUQUERQUE PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA SN 0091-7710 EI 2153-3806 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SPR PY 2013 VL 69 IS 1 BP 121 EP 122 PG 2 WC Anthropology SC Anthropology GA AP7MV UT WOS:000342262300008 ER PT J AU Stanton, JJ Zong, JC Eng, C Howard, L Flanagan, J Stevens, M Schmitt, D Wiedner, E Graham, D Junge, RE Weber, MA Fischer, M Mejia, A Tan, J Latimer, E Herron, A Hayward, GS Ling, PD AF Stanton, Jeffrey J. Zong, Jian-Chao Eng, Crystal Howard, Lauren Flanagan, Joe Stevens, Martina Schmitt, Dennis Wiedner, Ellen Graham, Danielle Junge, Randall E. Weber, Martha A. Fischer, Martha Mejia, Alicia Tan, Jie Latimer, Erin Herron, Alan Hayward, Gary S. Ling, Paul D. TI KINETICS OF VIRAL LOADS AND GENOTYPIC ANALYSIS OF ELEPHANT ENDOTHELIOTROPIC HERPESVIRUS-1 INFECTION IN CAPTIVE ASIAN ELEPHANTS (ELEPHAS MAXIMUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Elephant; EEHV; herpesvirus; Proboscivirus; real-time polymerase chain reaction; viral load ID AFRICAN ELEPHANTS AB Elephant endotheliotropic herpesviruses (EEHVs) can cause fatal hemorrhagic disease in juvenile Asian elephants (Elephas maximus); however, sporadic shedding of virus in trunk washes collected from healthy elephants also has been detected. Data regarding the relationship of viral loads in blood compared with trunk washes are lacking, and questions about whether elephants can undergo multiple infections with EEHVs have not been addressed previously. Real-time quantitative polymerase chain reaction was used to determine the kinetics of EEHV1 loads, and genotypic analysis was performed on EEHV1 DNA detected in various fluid samples obtained from five Asian elephants that survived detectable EEHV1 DNAemia on at least two separate occasions. In three elephants displaying clinical signs of illness, preclinical EEHV1 DNAemia was detectable, and peak whole-blood viral loads occurred 3-8 days after the onset of clinical signs. In two elephants with EEHV1 DNAemia that persisted for 7-21 days, no clinical signs of illness were observed. Detection of EEHV1 DNA in trunk washes peaked approximately 21 days after DNAemia, and viral genotypes detected during DNAemia matched those detected in subsequent trunk washes from the same elephant. In each of the five elephants, two distinct EEHV1 genotypes were identified in whole blood and trunk washes at different time points. In each case, these genotypes represented both an EEHV1A and an EEHV1B subtype. These data suggest that knowledge of viral loads could be useful for the management of elephants before or during clinical illness. Furthermore, sequential infection with both EEHV1 subtypes occurs in Asian elephants, suggesting that they do not elicit cross-protective sterilizing immunity. These data will be useful to individuals involved in the husbandry and clinical care of Asian elephants. C1 [Stanton, Jeffrey J.; Eng, Crystal; Mejia, Alicia; Tan, Jie; Herron, Alan; Ling, Paul D.] Baylor Coll Med, Dept Mol Virol & Microbiol, Houston, TX 77030 USA. [Zong, Jian-Chao; Hayward, Gary S.] Johns Hopkins Sch Med, Viral Oncol Program, Baltimore, MD 21231 USA. [Howard, Lauren; Flanagan, Joe; Stevens, Martina] Houston Zoo Inc, Houston, TX 77030 USA. [Schmitt, Dennis] Missouri State Univ, William H Darr Sch Agr, Springfield, MO 65897 USA. [Schmitt, Dennis; Wiedner, Ellen; Graham, Danielle] Ringling Bros Ctr Elephant Conservat, Polk City, FL 33868 USA. [Junge, Randall E.; Weber, Martha A.; Fischer, Martha] St Louis Zoo, St Louis, MO 63110 USA. [Latimer, Erin] Smithsonian Natl Zool Pk, Natl Elephant Herpesvirus Lab, Washington, DC 20008 USA. RP Ling, PD (reprint author), Baylor Coll Med, Dept Mol Virol & Microbiol, One Baylor Plaza, Houston, TX 77030 USA. EM pling@bcm.edu FU Houston Zoo, Inc; Elephant Managers Association; Dan Duncan Family Foundation; National Institutes of Health training grant [T-32-AI-07471]; Morris Animal Foundation; International Elephant Foundation at the National Elephant Herpesvirus Laboratory; National Institutes of Health research grant [NIAID AI24576]; International Elephant Foundation FX The authors acknowledge the hard work and dedication of the elephant care staff at the Houston Zoo, Inc.; the Saint Louis Zoo; and the Ringling Bros. Center for Elephant Conservation. We thank Daryl Hoffman for advice regarding the management of elephants infected with EEHV; Virginia Mohlere for review of the manuscript, and Sarah Heaggans for assistance in managing the sequence data information and GenBank submissions. Work at Baylor College of Medicine was supported by Houston Zoo, Inc.; Elephant Managers Association; the Dan Duncan Family Foundation; and the National Institutes of Health training grant T-32-AI-07471. A student scholarship from the Morris Animal Foundation supported the work of C. E. The International Elephant Foundation supported work at the National Elephant Herpesvirus Laboratory. Work at Johns Hopkins School of Medicine was supported by the National Institutes of Health research grant NIAID AI24576, the International Elephant Foundation, and the Morris Animal Foundation. NR 18 TC 17 Z9 17 U1 1 U2 5 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2013 VL 44 IS 1 BP 42 EP 54 PG 13 WC Veterinary Sciences SC Veterinary Sciences GA AM1PK UT WOS:000339619500007 PM 23505702 ER PT J AU Atkins, L Zong, JC Tan, J Mejia, A Heaggans, SY Nofs, SA Stanton, JJ Flanagan, JP Howard, L Latimer, E Stevens, MR Hoffman, DS Hayward, GS Ling, PD AF Atkins, Lisa Zong, Jian-Chao Tan, Jie Mejia, Alicia Heaggans, Sarah Y. Nofs, Sally A. Stanton, Jeffrey J. Flanagan, Joseph P. Howard, Lauren Latimer, Erin Stevens, Martina R. Hoffman, Daryl S. Hayward, Gary S. Ling, Paul D. TI ELEPHANT ENDOTHELIOTROPIC HERPESVIRUS 5, A NEWLY RECOGNIZED ELEPHANT HERPESVIRUS ASSOCIATED WITH CLINICAL AND SUBCLINICAL INFECTIONS IN CAPTIVE ASIAN ELEPHANTS (ELEPHAS MAXIMUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Asian elephant; Elephas maximus; elephant endotheliotropic herpesviruses; Proboscivirus; real-time PCR; viremia AB Elephant endotheliotropic herpesviruses (EEHVs) can cause acute hemorrhagic disease with high mortality rates in Asian elephants (Elephas maximus). Recently, a new EEHV type known as EEHV5 has been described, but its prevalence and clinical significance remain unknown. In this report, an outbreak of EEHV5 infection in a herd of captive Asian elephants in a zoo was characterized. In February 2011, a 42-yr-old wild-born female Asian elephant presented with bilaterally swollen temporal glands, oral mucosal hyperemia, vesicles on the tongue, and generalized lethargy. The elephant had a leukopenia and thrombocytopenia. She was treated with flunixin meglumine, famciclovir, and fluids. Clinical signs of illness resolved gradually over 2 wk, and the white blood cell count and platelets rebounded to higher-than-normal values. EEHV5 viremia was detectable starting 1 wk before presentation and peaked at the onset of clinical illness. EEHV5 shedding in trunk secretions peaked after viremia resolved and continued for more than 2 mo. EEHV5 trunk shedding from a female herd mate without any detectable viremia was detected prior to onset of clinical disease in the 42-yr-old elephant, indicating reactivation rather than primary infection in this elephant. Subsequent EEHV5 viremia and trunk shedding was documented in the other five elephants in the herd, who remained asymptomatic, except for 1 day of temporal gland swelling in an otherwise-healthy 1-yr-old calf. Unexpectedly, the two elephants most recently introduced into the herd 40 mo previously shed a distinctive EEHV5 strain from that seen in the other five elephants. This is the first report to document the kinetics of EEHV5 infection in captive Asian elephants and to provide evidence that this virus can cause illness in some animals. C1 [Atkins, Lisa; Tan, Jie; Mejia, Alicia; Nofs, Sally A.; Stanton, Jeffrey J.; Ling, Paul D.] Baylor Coll Med, Dept Mol Virol & Microbiol, Houston, TX 77030 USA. [Zong, Jian-Chao; Heaggans, Sarah Y.; Hayward, Gary S.] Johns Hopkins Sch Med, Viral Oncol Program, Baltimore, MD 21231 USA. [Flanagan, Joseph P.; Howard, Lauren; Stevens, Martina R.; Hoffman, Daryl S.] Houston Zoo Inc, Houston, TX 77030 USA. [Latimer, Erin] Smithsonian Natl Zool Pk, Elephant Herpesvirus Lab, Washington, DC 20008 USA. RP Ling, PD (reprint author), Baylor Coll Med, Dept Mol Virol & Microbiol, One Baylor Plaza, Houston, TX 77030 USA. EM pling@bcm.edu FU Dan L. Duncan Foundation; International Elephant Foundation; National Institutes of Health [R01 AI24576, T32-AI-07471]; Houston Zoo FX Support for this study was provided by the Houston Zoo and a grant from the Dan L. Duncan Foundation, as well as by grants from the International Elephant Foundation to the National Zoological Park Elephant Herpesvirus Laboratory and by National Institutes of Health grant R01 AI24576 to G. S. Hayward at Johns Hopkins. Sally Nofs was supported by National Institutes of Health training grant T32-AI-07471. NR 11 TC 15 Z9 15 U1 1 U2 14 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD MAR PY 2013 VL 44 IS 1 BP 136 EP 143 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA AM1PK UT WOS:000339619500019 PM 23505714 ER PT J AU Herranz, M Pardos, F Boyle, MJ AF Herranz, Maria Pardos, Fernando Boyle, Michael J. TI Comparative morphology of serotonergic-like immunoreactive elements in the central nervous system of kinorhynchs (kinorhyncha, cyclorhagida) SO JOURNAL OF MORPHOLOGY LA English DT Article DE Kinorhyncha; nervous system; confocal laser scanning microscopy; serotonin; Cycloneuralia ID PHYLOGENETIC-RELATIONSHIPS; ECHINODERES; ULTRASTRUCTURE; RECONSTRUCTION; HOMALORHAGIDA; MACRODASYIDA; GASTROTRICHA; ARCHITECTURE; MUSCULATURE; CHARACTERS AB Cycloneuralian taxa exhibit similar organ system architectures, providing informative characters of metazoan evolution, yet very few modern comparative descriptions of cellular and molecular homologies within and among those taxa are available. We immunolabeled and characterized elements of the serotonergic nervous system in the kinorhynchs Echinoderes spinifurca, Antygomonas paulae, and Zelinkaderes brightae using confocal laser scanning microscopy. Fluorescent markers targeting DNA were combined with observations of auto-fluorescent structures to guide interpretations of the internal and external anatomy in each species. Results show a common pattern of the central nervous system with a circumenteric brain divided into ring-shaped anterior and posterior neuronal somata and a central neuropil connected to a multi-stringed, longitudinal ventral nerve cord. Structural similarities and differences in the nervous systems of these species were observed and described, stressing the incomplete ring nature of the anterior region of the kinorhynch brain, the functional relationship between the brain and the movable introvert, and the number and arrangement of nerve strings and somata of the ventral nerve cord. The ventral cord ends in two ventrolateral cell bodies in E. spinifurca, and forms a terminal loop associated with a midterminal spine in A. paulae and Z. brightae. The possible functional and phylogenetic significance of these features and arrangements are discussed. J. Morphol., 2013. (c) 2012 Wiley Periodicals, Inc. C1 [Herranz, Maria; Pardos, Fernando] Univ Complutense Madrid, Dept Zool & Antropol Fis Zool Invertebrados, Fac Biol, E-28040 Madrid, Spain. [Boyle, Michael J.] Smithsonian Marine Stn Ft Pierce, Smithsonian Inst, Ft Pierce, FL 34949 USA. RP Herranz, M (reprint author), Univ Complutense Madrid, Dept Zool & Antropol Fis Zool Invertebrados, Fac Biol, C Jose Antonio Novais 2, E-28040 Madrid, Spain. EM mariaherranz@bio.ucm.es RI HERRANZ, MARIA/J-8042-2014; OI PARDOS MARTINEZ, FERNANDO/0000-0002-6292-9793 FU Link Foundation/Smithsonian Institution; Ministerio de Ciencia y Tecnologia, Plan Nacional de Investigacion Cientifica, Desarrollo e Investigacion Tecnologica [CGL2009-08928] FX Contract grant sponsor: Link Foundation/Smithsonian Institution Graduate Fellowship (to M.H.); Contract grant sponsor: Ministerio de Ciencia y Tecnologia, Plan Nacional de Investigacion Cientifica, Desarrollo e Investigacion Tecnologica (to F.P.); Grant number: CGL2009-08928. NR 55 TC 10 Z9 10 U1 1 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD MAR PY 2013 VL 274 IS 3 BP 258 EP 274 DI 10.1002/jmor.20089 PG 17 WC Anatomy & Morphology SC Anatomy & Morphology GA 075JN UT WOS:000313881400002 PM 23109054 ER PT J AU St-Laurent, GP Gelinas, N Potvin, C AF St-Laurent, Guillaume Peterson Gelinas, Nancy Potvin, Catherine TI REDD+ and the agriculture frontier: Understanding colonists' utilization of the land SO LAND USE POLICY LA English DT Article DE Colonist; Perception; REDD; Land use; Deforestation; Eastern Panama ID ENVIRONMENTAL SERVICES; TROPICAL FOREST; COSTA-RICA; BRAZILIAN AMAZON; COVER CHANGE; DEFORESTATION; CONSERVATION; CARBON; PANAMA; PAYMENTS AB Given the importance of the agricultural frontier as an engine of deforestation, this paper focuses on how colonists (from the Spanish word for "colonists" that is used to describe migrants to the agricultural frontier), who are important and largely overlooked stakeholders, perceive the new climate mitigation mechanism known as Reducing Emissions from Deforestation and forest Degradation in developing countries (REDD+). We aimed (1) to document colonists' land use, perceptions, needs, and aspirations and (2) to understand if and how they could be taken into account under REDD+ policies. The study, including multiple data collection techniques (e.g., focus group, interviews, and participatory activities), was conducted in eastern Panama. Three areas that were adjacent to the Province of Darien border were chosen because of their similar forested landscapes and varying accessibility to a main road. Our results suggest that land use preferences, culture, forest scarcity and dependency, inequalities (e.g., land use, amount of forest, and land area), and lack of technical capacities are key elements to be considered when developing a REDD+ strategy with colonist communities. We propose that halting deforestation without both considering local communities' perceptions and giving effective alternatives could seriously undermine livelihoods. (C) 2012 Elsevier Ltd. All rights reserved. C1 [St-Laurent, Guillaume Peterson; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Gelinas, Nancy] Univ Laval, Faculte Foresterie Geog & Geomat, Quebec City, PQ G1K 7P4, Canada. [St-Laurent, Guillaume Peterson; Potvin, Catherine] Smithsonian Trop Res Inst, Panama City, Panama. RP St-Laurent, GP (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM guillaume.petersonst-laurent@mail.mcgill.ca NR 91 TC 5 Z9 5 U1 3 U2 55 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0264-8377 J9 LAND USE POLICY JI Land Use Pol. PD MAR PY 2013 VL 31 SI SI BP 516 EP 525 DI 10.1016/j.landusepol.2012.08.017 PG 10 WC Environmental Studies SC Environmental Sciences & Ecology GA 067TM UT WOS:000313318000052 ER PT J AU Lynam, AJ Jenks, KE Tantipisanuh, N Chutipong, W Ngoprasert, D Gale, GA Steinmetz, R Sukmasuang, R Bhumpakphan, N Grassman, LI Cutter, P Kitamura, S Reed, DH Baker, MC McShea, W Songsasen, N Leimgruber, P AF Lynam, Antony J. Jenks, Kate E. Tantipisanuh, Naruemon Chutipong, Wanlop Ngoprasert, Dusit Gale, George A. Steinmetz, Robert Sukmasuang, Ronglarp Bhumpakphan, Naris Grassman, Lon I., Jr. Cutter, Passanan Kitamura, Shumpei Reed, David H. Baker, Megan C. McShea, William Songsasen, Nucharin Leimgruber, Peter TI TERRESTRIAL ACTIVITY PATTERNS OF WILD CATS FROM CAMERA-TRAPPING SO RAFFLES BULLETIN OF ZOOLOGY LA English DT Article DE small cats; activity patterns; camera-traps; Thailand ID LEOPARD PANTHERA-PARDUS; NORTH-CENTRAL THAILAND; PUMA PUMA-CONCOLOR; YAI NATIONAL-PARK; PRIONAILURUS-BENGALENSIS; RAIN-FOREST; TROPICAL FORESTS; EVERGREEN FOREST; CONSERVATION; DIVERSITY AB The behaviour of wild cats is poorly understood. Using camera-trapping, we quantifi ed temporal overlap among seven species of Asian wild cats, including tiger Panthera tigris and leopard Panthera pardus. Based on time stamp data from 780 camera-traps and 24 study sites from 14 protected areas across Thailand, we assessed terrestrial activity patterns and temporal overlap in habitat use. For quantifying overlap, we used a coeffi cient estimator (Delta) over cap (1) that allows for calculation of confi dence intervals. Our study provided insight into temporal interactions among species of wild cats, particularly between small cats and their larger cat relatives. We found temporal habitat segregation in several small cats with some species being strongly nocturnal (>= 85% records between 1800 and 0600 hours - leopard cat Prionailurus bengalensis), mostly (>50%) nocturnal (clouded leopard Neofelis nebulosa), mostly diurnal (>50% records between 0600 and 1800 hours - Asiatic golden cat Catopuma temminckii), or strongly (>= 85%) diurnal (marbled cat Pardofelis marmorata). We found high temporal overlap ((Delta) over cap >= 0.80) between leopard cat and clouded leopard (95% CI = 0.77-0.91), Asiatic golden cat and leopard (95% CI = 0.69-0.87), Asiatic golden cat and tiger (95% CI = 0.72-0.90), and clouded leopard and tiger (95% CI = 0.69-0.85). Our research demonstrates that temporal habitat or niche segregation may be an important process in maintaining the functioning of diverse predator guilds in tropical forests. We developed several avoidance or overlap hypotheses that can explain the patterns observed in our study and that should be further tested. C1 [Lynam, Antony J.] Wildlife Conservat Soc, Global Conservat Program, Bronx, NY 10540 USA. [Jenks, Kate E.] Univ New Hampshire, Dept Nat Resources & Environm, Durham, NH 03824 USA. [Jenks, Kate E.] Univ Massachusetts, Grad Program Organism & Evolutionary Biol, Amherst, MA 01003 USA. [Jenks, Kate E.] Univ Massachusetts, Grad Program Wildlife & Fisheries Conservat, Amherst, MA 01003 USA. [Jenks, Kate E.; Baker, Megan C.; McShea, William; Songsasen, Nucharin; Leimgruber, Peter] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Tantipisanuh, Naruemon; Chutipong, Wanlop; Ngoprasert, Dusit; Gale, George A.] King Mongkuts Univ Technol Thonburi, Conservat Ecol Program, Bangkok 10150, Thailand. [Steinmetz, Robert] WWF Thailand, Bangkok, Thailand. [Sukmasuang, Ronglarp; Bhumpakphan, Naris] Kasetsart Univ, Dept Forest Biol, Bangkok 10900, Thailand. [Grassman, Lon I., Jr.] Texas A&I Univ Kingsville, Caesar Kleberg Wildlife Res Inst, Feline Res Ctr, Kingsville, TX 78363 USA. [Cutter, Passanan] Univ Minnesota, Conservat Biol Program, St Paul, MN 55108 USA. [Kitamura, Shumpei] Museum Nat & Human Activ, Div Nat & Environm Management, Sanda, Hyogo 6691546, Japan. [Reed, David H.] Univ Louisville, Dept Biol, Louisville, KY 40292 USA. RP Lynam, AJ (reprint author), Wildlife Conservat Soc, Global Conservat Program, 2300 Southern Blvd, Bronx, NY 10540 USA. EM tlynam@wcs.org; kate@katejenks.info; ttpisanu@gmail.com; wanlop.chutipong2012@gmail.com; ndusit@gmail.com; ggkk1990@gmail.com; roberts@wwfgreatermekong.org; fforrls@ku.ac.th; ffornrb@ku.ac.th; longrassman@hotmail.com; namfonb@yahoo.com; kshumpei@wg8.so-net.ne.jp; bakermc@si.edu; bakermc@si.edu; songsasenn@si.edu; leimgruberp@si.edu RI Leimgruber, Peter/O-1304-2015; OI Leimgruber, Peter/0000-0002-3682-0153; Lynam, Antony/0000-0002-8395-7902 FU Clouded Leopard Project; TRF/BIOTEC Special Program for Biodiversity Research and Training Thailand, Kasetsart University; Smithsonian Conservation Biology Institute; Mahidol University Government Research Grant; National Center for Genetic Engineering and Biotechnology; Hornbill Research Foundation; JSPS Research Fellowship FX We wish to thank the Clouded Leopard Project, TRF/BIOTEC Special Program for Biodiversity Research and Training Thailand, Kasetsart University, and the Smithsonian Conservation Biology Institute for providing funding for a workshop that brought some of the authors together to discuss collaboration. S. Kitamura was funded by the Mahidol University Government Research Grant, the National Center for Genetic Engineering and Biotechnology, the Hornbill Research Foundation, and a JSPS Research Fellowship. We thank the Wildlife Conservation Society Thailand, World Wide Fund for Nature-Thailand, and the Smithsonian Conservation Biology Institute for allowing participants to use data collected under their auspices. We also thank R. Phoonjampa, S. Tanasarnpaiboon. and M. Pliwsungnoen for their assistance. Finally we thank two anonymous reviewers for their comments and suggestions which helped improve the final version of the paper. NR 53 TC 11 Z9 16 U1 9 U2 116 PU NATL UNIV SINGAPORE, SCHOOL BIOLOGICAL SCIENCES PI SINGAPORE PA DEPT ZOOLOGY, KENT RIDGE, SINGAPORE 0511, SINGAPORE SN 0217-2445 J9 RAFFLES B ZOOL JI Raffles Bull. Zool. PD FEB 28 PY 2013 VL 61 IS 1 BP 407 EP 415 PG 9 WC Zoology SC Zoology GA 103RT UT WOS:000315937300026 ER PT J AU Loreau, J Sadeghpour, HR Dalgarno, A AF Loreau, J. Sadeghpour, H. R. Dalgarno, A. TI Potential energy curves for the interaction of Ag(5s) and Ag(5p) with noble gas atoms SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; CONSISTENT BASIS-SETS; CONVERGENT BASIS-SETS; DER-WAALS MOLECULES; PHOTOIONIZATION SPECTROSCOPY; COUPLED-CLUSTER; HARTREE-FOCK; AU; AG AB We investigate the interaction of ground and excited states of a silver atom with noble gases (NG), including helium. Born-Oppenheimer potential energy curves are calculated with quantum chemistry methods and spin-orbit effects in the excited states are included by assuming a spin-orbit splitting independent of the internuclear distance. We compare our results with experimentally available spectroscopic data, as well as with previous calculations. Because of strong spin-orbit interactions, excited Ag-NG potential energy curves cannot be fitted to Morse-like potentials. We find that the labeling of the observed vibrational levels has to be shifted by one unit. (C) 2013 American Institute of Physics. [http://dx.doi.org/10.1063/1.4790586] C1 [Loreau, J.; Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Loreau, J (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. OI Loreau, Jerome/0000-0002-6142-1509 FU U.S. Department of Energy; NSF; Smithsonian Astrophysical Observatory FX This work was supported by the U.S. Department of Energy and by an NSF grant to ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 47 TC 6 Z9 6 U1 1 U2 21 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD FEB 28 PY 2013 VL 138 IS 8 AR 084301 DI 10.1063/1.4790586 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 100AT UT WOS:000315667800014 PM 23464145 ER PT J AU Risaliti, G Harrison, FA Madsen, KK Walton, DJ Boggs, SE Christensen, FE Craig, WW Grefenstette, BW Hailey, CJ Nardini, E Stern, D Zhang, WW AF Risaliti, G. Harrison, F. A. Madsen, K. K. Walton, D. J. Boggs, S. E. Christensen, F. E. Craig, W. W. Grefenstette, B. W. Hailey, C. J. Nardini, E. Stern, Daniel Zhang, W. W. TI A rapidly spinning supermassive black hole at the centre of NGC 1365 SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEI; EMISSION-LINES; 1H 0707-495; ABSORPTION; REGION; MODEL; MCG-6-30-15; REFLECTION; NGC-1365; SIZE AB Broad X-ray emission lines from neutral and partially ionized iron observed in active galaxies have been interpreted as fluorescence produced by the reflection of hard X-rays off the inner edge of an accretion disk(1-7). In this model, line broadening and distortion result from rapid rotation and relativistic effects near the black hole, the line shape being sensitive to its spin. Alternative models in which the distortions result from absorption by intervening structures provide an equally good description of the data(8,9), and there has been no general agreement on which is correct. Recent claims(10) that the black hole(11,12) (2 X 10(6) solar masses) at the centre of the galaxy NGC 1365 is rotating at close to its maximum possible speed rest on the assumption of relativistic reflection. Here we report X-ray observations of NGC 1365 that reveal the relativistic disk features through broadened Fe-line emission and an associated Compton scattering excess of 10-30 kiloelectronvolts. Using temporal and spectral analyses, we disentangle continuum changes due to time-variable absorption from reflection, which we find arises from a region within 2.5 gravitational radii of the rapidly spinning black hole. Absorption-dominated models that do not include relativistic disk reflection can be ruled out both statistically and on physical grounds. C1 [Risaliti, G.] INAF Osservatoria Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harrison, F. A.; Madsen, K. K.; Walton, D. J.; Grefenstette, B. W.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Nardini, E.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Risaliti, G (reprint author), INAF Osservatoria Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM risaliti@arcetri.astro.it; fiona@srl.caltech.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; ESA Member States FX This work was supported under NASA grant number NNG08FD60C, and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with execution and analysis of these observations. This work also made use of observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. NR 27 TC 118 Z9 118 U1 1 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD FEB 28 PY 2013 VL 494 IS 7438 BP 449 EP 451 DI 10.1038/nature11938 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 099YI UT WOS:000315661500031 PM 23446416 ER PT J AU Barclay, T Rowe, JF Lissauer, JJ Huber, D Fressin, F Howell, SB Bryson, ST Chaplin, WJ Deseret, JM Lopez, ED Marcy, GW Mullally, F Ragozzine, D Torres, G Adams, ER Agol, E Barrado, D Basu, S Bedding, TR Buchhave, LA Charbonneau, D Christiansen, JL Christensen-Dalsgaard, J Ciardi, D Cochran, WD Dupree, AK Elsworth, Y Everett, M Fischer, DA Ford, EB Fortney, JJ Geary, JC Haas, MR Handberg, R Hekker, S Henze, CE Horch, E Howard, AW Hunter, RC Isaacson, H Jenkins, JM Karoff, C Kawaler, SD Kjeldsen, H Klaus, TC Latham, DW Li, J Lillo-Box, J Lund, MN Lundkvist, M Metcalfe, TS Miglio, A Morris, RL Quintana, EV Stello, D Smith, JC Still, M Thompson, SE AF Barclay, Thomas Rowe, Jason F. Lissauer, Jack J. Huber, Daniel Fressin, Francois Howell, Steve B. Bryson, Stephen T. Chaplin, William J. Deseret, Jean-Michel Lopez, Eric D. Marcy, Geoffrey W. Mullally, Fergal Ragozzine, Darin Torres, Guillermo Adams, Elisabeth R. Agol, Eric Barrado, David Basu, Sarbani Bedding, Timothy R. Buchhave, Lars A. Charbonneau, David Christiansen, Jessie L. Christensen-Dalsgaard, Jorgen Ciardi, David Cochran, William D. Dupree, Andrea K. Elsworth, Yvonne Everett, Mark Fischer, Debra A. Ford, Eric B. Fortney, Jonathan J. Geary, John C. Haas, Michael R. Handberg, Rasmus Hekker, Saskia Henze, Christopher E. Horch, Elliott Howard, Andrew W. Hunter, Roger C. Isaacson, Howard Jenkins, Jon M. Karoff, Christoffer Kawaler, Steven D. Kjeldsen, Hans Klaus, Todd C. Latham, David W. Li, Jie Lillo-Box, Jorge Lund, Mikkel N. Lundkvist, Mia Metcalfe, Travis S. Miglio, Andrea Morris, Robert L. Quintana, Elisa V. Stello, Dennis Smith, Jeffrey C. Still, Martin Thompson, Susan E. TI A sub-Mercury-sized exoplanet SO NATURE LA English DT Article ID TRANSITING PLANET; EXTRASOLAR PLANETS; BLEND SCENARIOS; MULTIPLE SYSTEM; KEPLER-MISSION; LIGHT CURVES; ASTEROSEISMOLOGY; METALLICITIES; VALIDATION; CANDIDATES AB Since the discovery of the first exoplanets(1,2), it has been known that other planetary systems can look quite unlike our own(3). Until fairly recently, we have been able to probe only the upper range of the planet size distribution(4,5), and, since last year, to detect planets that are the size of Earth(6) or somewhat smaller(7). Hitherto, no planets have been found that are smaller than those we see in the Solar System. Here we report a planet significantly smaller than Mercury(8). This tiny planet is the innermost of three that orbit the Sun-like host star, which we have designated Kepler-37. Owing to its extremely small size, similar to that of the Moon, and highly irradiated surface, the planet, Kepler-37b, is probably rocky with no atmosphere or water, similar to Mercury. C1 [Barclay, Thomas; Rowe, Jason F.; Lissauer, Jack J.; Huber, Daniel; Howell, Steve B.; Bryson, Stephen T.; Mullally, Fergal; Christiansen, Jessie L.; Haas, Michael R.; Henze, Christopher E.; Hunter, Roger C.; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Quintana, Elisa V.; Smith, Jeffrey C.; Still, Martin; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Rowe, Jason F.; Mullally, Fergal; Christiansen, Jessie L.; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Quintana, Elisa V.; Smith, Jeffrey C.; Thompson, Susan E.] SETI Inst, Mountain View, CA 94043 USA. [Fressin, Francois; Deseret, Jean-Michel; Ragozzine, Darin; Torres, Guillermo; Adams, Elisabeth R.; Charbonneau, David; Dupree, Andrea K.; Geary, John C.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chaplin, William J.; Elsworth, Yvonne; Hekker, Saskia; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, England. [Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ragozzine, Darin; Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barrado, David] Ctr Astron Hispano Aleman, Calar Alto Observ, E-04004 Almeria, Spain. [Barrado, David; Lillo-Box, Jorge] Ctr Astrobiol, Dept Astrofis, E-28691 Villanueva De La Canada, Spain. [Basu, Sarbani; Fischer, Debra A.] Yale Univ, New Haven, CT 06520 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christoffer; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Ciardi, David] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Klaus, Todd C.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA. RP Barclay, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM thomas.barclay@nasa.gov; jason.rowe@nasa.gov RI Karoff, Christoffer/L-1007-2013; Basu, Sarbani/B-8015-2014; Lillo-Box, Jorge/I-2841-2015; Barrado Navascues, David/C-1439-2017; OI Lund, Mikkel Norup/0000-0001-9214-5642; Lundkvist, Mia Sloth/0000-0002-8661-2571; Fischer, Debra/0000-0003-2221-0861; Handberg, Rasmus/0000-0001-8725-4502; Kawaler, Steven/0000-0002-6536-6367; Karoff, Christoffer/0000-0003-2009-7965; Basu, Sarbani/0000-0002-6163-3472; Lillo-Box, Jorge/0000-0003-3742-1987; Barrado Navascues, David/0000-0002-5971-9242; Bedding, Timothy/0000-0001-5943-1460; Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Bedding, Tim/0000-0001-5222-4661; Metcalfe, Travis/0000-0003-4034-0416 FU NASA's Science Mission Directorate; NASA; JPL/Caltech; Danish National Research Foundation; ASTERISK; European Research Council; NSF FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. Some of this work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award. issued by JPL/Caltech. Kepler flux time series data presented in this paper are available from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation. The research is supported by the ASTERISK project funded by the European Research Council. E.A. acknowledges support through an NSF Career grant. D.H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center. NR 30 TC 92 Z9 92 U1 2 U2 40 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD FEB 28 PY 2013 VL 494 IS 7438 BP 452 EP 454 DI 10.1038/nature11914 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 099YI UT WOS:000315661500032 PM 23426260 ER PT J AU Kasper, JC Maruca, BA Stevens, ML Zaslavsky, A AF Kasper, Justin C. Maruca, Bennett A. Stevens, Michael L. Zaslavsky, Arnaud TI Sensitive Test for Ion-Cyclotron Resonant Heating in the Solar Wind SO PHYSICAL REVIEW LETTERS LA English DT Article ID ALFVEN-WAVE TURBULENCE; HEAVY-IONS; PREFERENTIAL ACCELERATION; CORONAL HOLE; MINOR IONS; CONSTRAINTS; PROTON; SCATTERING; LATITUDE; ULYSSES AB Plasma carrying a spectrum of counterpropagating field-aligned ion-cyclotron waves can strongly and preferentially heat ions through a stochastic Fermi mechanism. Such a process has been proposed to explain the extreme temperatures, temperature anisotropies, and speeds of ions in the solar corona and solar wind. We quantify how differential flow between ion species results in a Doppler shift in the wave spectrum that can prevent this strong heating. Two critical values of differential flow are derived for strong heating of the core and tail of a given ion distribution function. Our comparison of these predictions to observations from the Wind spacecraft reveals excellent agreement. Solar wind helium that meets the condition for strong core heating is nearly 7 times hotter than hydrogen on average. Ion-cyclotron resonance contributes to heating in the solar wind, and there is a close link between heating, differential flow, and temperature anisotropy. DOI: 10.1103/PhysRevLett.110.091102 C1 [Kasper, Justin C.; Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maruca, Bennett A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Zaslavsky, Arnaud] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. RP Kasper, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jkasper@cfa.harvard.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NASA [NNX12AB19G] FX This work was supported by NASA Grant No. NNX12AB19G. The authors gratefully acknowledge productive discussions with S. Bale, B. Chandran, S. Cranmer, S. P. Gary, P. Isenberg, and W. Matthaeus. NR 35 TC 37 Z9 37 U1 0 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 28 PY 2013 VL 110 IS 9 AR 091102 DI 10.1103/PhysRevLett.110.091102 PG 5 WC Physics, Multidisciplinary SC Physics GA 097QJ UT WOS:000315488300005 PM 23496700 ER PT J AU Mettke-Hofmann, C Winkler, H Hamel, PB Greenberg, R AF Mettke-Hofmann, Claudia Winkler, Hans Hamel, Paul B. Greenberg, Russell TI Migratory New World Blackbirds (Icterids) Are More Neophobic than Closely Related Resident Icterids SO PLOS ONE LA English DT Article ID ECOLOGICAL PLASTICITY; PUBLIC INFORMATION; NOVELTY RESPONSES; SWAMP SPARROWS; BIRDS; EXPERIENCE; ASSEMBLAGE; FOOD; SONG; EXPLORATION AB Environments undergo short-term and long-term changes due to natural or human-induced events. Animals differ in their ability to cope with such changes which can be related to their ecology. Changes in the environment often elicit avoidance reactions (neophobia) which protect animals from dangerous situations but can also inhibit exploration and familiarization with novel situations and thus, learning about new resources. Studies investigating the relationship between a species' ecology and its neophobia have so far been restricted to comparing only a few species and mainly in captivity. The current study investigated neophobia reactions to experimentally-induced changes in the natural environment of six closely-related blackbird species (Icteridae), including two species represented by two distinct populations. For analyses, neophobic reactions (difference in number of birds feeding and time spent feeding with and without novel objects) were related to several measures of ecological plasticity and the migratory strategy (resident or migratory) of the population. Phylogenetic relationships were incorporated into the analysis. The degree of neophobia was related to migratory strategy with migrants expressing much higher neophobia (fewer birds feeding and for a shorter time with objects present) than residents. Furthermore, neophobia showed a relationship to diet breadth with fewer individuals of diet generalists than specialists returning when objects were present supporting the dangerous niche hypothesis. Residents may have evolved lower neophobia as costs of missing out on opportunities may be higher for residents than migrants as the former are restricted to a smaller area. Lower neophobia allows them approaching changes in the environment (e. g. novel objects) quickly, thereby securing access to resources. Additionally, residents have a greater familiarity with similar situations in the area than migrants and the latter may, therefore, initially stay behind resident species. C1 [Mettke-Hofmann, Claudia] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 5UX, Merseyside, England. [Mettke-Hofmann, Claudia; Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Winkler, Hans] Univ Vet Med, Dept Integrat Biol & Evolut, Konrad Lorenz Inst Ethol, Vienna, Austria. [Hamel, Paul B.] US Forest Serv, Southern Hardwood Lab, Stoneville, MS USA. RP Mettke-Hofmann, C (reprint author), Liverpool John Moores Univ, Sch Nat Sci & Psychol, Liverpool L3 5UX, Merseyside, England. EM C.C.Mettke-Hofmann@ljmu.ac.uk FU Max Kade Foundation; Max Planck Institute for Ornithology, Andechs, Germany; German Ethological Society; Society for Tropical Ornithology, Germany; Point Reyes Bird Observatory, CA; USDA Forest Service, Center for Bottomland Hardwoods, MS FX The study was supported by a grant from the Max Kade Foundation. Assistants, travel and material were supported by the Max Planck Institute for Ornithology, Andechs, Germany, the German Ethological Society, and the Society for Tropical Ornithology, Germany. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We thank the Point Reyes Bird Observatory, CA, and the USDA Forest Service, Center for Bottomland Hardwoods, MS, for providing housing and support, the National Park Service Point Reyes National Seashore, CA, Yazoo NWR, Leroy Percy SP, Delta Research and Experimental Center, (all MS), and all cooperating farmers for permitting experiments on their land and Gerhard Hofmann for his assistance with the experiments. NR 53 TC 13 Z9 13 U1 4 U2 52 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 27 PY 2013 VL 8 IS 2 AR e57565 DI 10.1371/journal.pone.0057565 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 098BN UT WOS:000315519000130 PM 23460875 ER PT J AU Itoh, R Fukazawa, Y Chiang, J Hanabata, Y Hayashida, M Hayashi, K Mizuno, T Ohno, M Ohsugi, T Perkins, JS Raino, S Reyes, LC Takahashi, H Tanaka, Y Tosti, G Akitaya, H Arai, A Kino, M Ikejiri, Y Kawabata, KS Komatsu, T Sakimoto, K Sasada, M Sato, S Uemura, M Ui, T Yamanaka, M Yoshida, M AF Itoh, Ryosuke Fukazawa, Yasushi Chiang, James Hanabata, Yoshitaka Hayashida, Masaaki Hayashi, Katsuhiro Mizuno, Tsunefumi Ohno, Masanori Ohsugi, Takashi Perkins, Jeremy S. Raino, Silvia Reyes, Luis C. Takahashi, Hiromitsu Tanaka, Yasuyuki Tosti, Gino Akitaya, Hiroshi Arai, Akira Kino, Masaru Ikejiri, Yuki Kawabata, Koji S. Komatsu, Tomoyuki Sakimoto, Kiyoshi Sasada, Mahito Sato, Shuji Uemura, Makoto Ui, Takahiro Yamanaka, Masayuki Yoshida, Michitoshi TI A Study of the Long-Term Spectral Variations of 3C 66A Observed with the Fermi and Kanata Telescopes SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: BL Lacertae objects: general; gamma rays: observations ID LARGE-AREA TELESCOPE; GAMMA-RAY FLARE; MULTIWAVELENGTH OBSERVATIONS; SOURCE CATALOG; BLAZAR; POLARIZATION; OUTBURST; EMISSION AB 3C 66A is an intermediate-frequency-peaked BL Lac object detected by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope. We present a study of the long-term variations of this blazar seen over similar to 2 yr at GeV energies with Fermi and in the optical (flux and polarization) and near infrared with the Kanata telescope. In 2008, the first year of the study, we find a correlation between the gamma-ray flux and the measurements taken with the Kanata telescope. This is in contrast to the later measurements performed during 2009-2010 which show only a weak correlation along with a gradual increase of the optical flux. We calculate an external seed photon energy density assuming that the gamma-ray emission is due to external Compton scattering. The energy density of the external photons is found to be higher by a factor of two in 2008 compared to 2009-2010. We conclude that the different behaviors observed between the first year and the later years might be explained by postulating two different emission components. C1 [Itoh, Ryosuke; Fukazawa, Yasushi; Hanabata, Yoshitaka; Hayashi, Katsuhiro; Ohno, Masanori; Ohsugi, Takashi; Takahashi, Hiromitsu; Ikejiri, Yuki; Komatsu, Tomoyuki; Sakimoto, Kiyoshi; Ui, Takahiro] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Chiang, James; Hayashida, Masaaki] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Chiang, James] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Chiang, James] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Hayashida, Masaaki] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Mizuno, Tsunefumi; Tanaka, Yasuyuki; Akitaya, Hiroshi; Kawabata, Koji S.; Uemura, Makoto; Yoshida, Michitoshi] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Perkins, Jeremy S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perkins, Jeremy S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, Jeremy S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, Jeremy S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, Jeremy S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Raino, Silvia] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Raino, Silvia] Politecn Bari, I-70126 Bari, Italy. [Raino, Silvia] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Reyes, Luis C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93401 USA. [Tosti, Gino] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Tosti, Gino] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Arai, Akira] Kyoto Sangyo Univ, Dept Phys, Kita Ku, Kyoto 6038555, Japan. [Kino, Masaru; Sato, Shuji] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Sasada, Mahito] Kyoto Univ, Dept Phys, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Yamanaka, Masayuki] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan. RP Itoh, R (reprint author), Hiroshima Univ, Dept Phys Sci, 1-3-1 Kagamiyama, Hiroshima 7398526, Japan. EM itoh@hep01.hepl.hiroshima-u.ac.jp; fukazawa@hep01.hepl.hiroshima-u.ac.jp RI Tosti, Gino/E-9976-2013 FU Japan Society for the Promotion of Science (JSPS) FX This work was supported by the Japan Society for the Promotion of Science (JSPS). NR 28 TC 2 Z9 2 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD FEB 25 PY 2013 VL 65 IS 1 AR UNSP 18 DI 10.1093/pasj/65.1.18 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 123FU UT WOS:000317374600018 ER PT J AU Adamski, D AF Adamski, David TI Review of the Blastobasinae of Costa Rica (Lepidoptera: Gelechioidea: Blastobasidae) SO ZOOTAXA LA English DT Review DE Central America; Costa Rica; Lepidoptera Survey; INBio; morphology; taxonomy ID SUGARCANE PEST; COLEOPHORIDAE; GRAMINEA; BIOLOGY AB The Blastobasinae (Lepidoptera: Gelechioidea: Blastobasidae) of Costa Rica are reviewed. Five new genera, Barbaloba, Hallicis, Koleps, Pheos, and Pseudokoleps, and 101 new species are described. They include: Barbaloba jubae, B. meleagrisellae, Hallicis bisetosellus, H. calvicula, Koleps angulatus, Pheos aculeatus, Pseudokoleps akainae, Blastobasis abollae, B. achaea, B. aedes, B. babae, B. balucis, B. beo, B. caetrae, B. chanes, B. custodis, B. dapis, B. deae, B. deliciolarum, B. dicionis, B. echus, B. erae, B. fax, B. furtivus, B. iuanae, B. lex, B. litis, B. lygdi, B. manto, B. neniae, B. nivis, B. orithyia, B. paludis, B. phaedra, B. rotae, B. rotullae, B. tapetae, B. thyone, B. usurae, B. vesta, B. xiphiae, Hypatopa actes, H. acus, H. agnae, H. arxcis, H. bilobata, H. caedis, H. caepae, H. cladis, H. cotis, H. cotytto, H. crux, H. cyane, H. dicax, H. dolo, H. dux, H. edax, H. eos, H. erato, H. fio, H. gena, H. hecate, H. hera, H. hora, H. io, H. ira, H. leda, H. limae, H. lucina, H. joniella, H. juno, H. manus, H. mora, H. musa, H. nex, H. nox, H. phoebe, H. pica, H. plebis, H. rabio, H. rea, H. rego, H. rudis, H. sais, H. scobis, H. semela, H. solea, H. styga, H. texla, H. texo, H. umbra, H. verax, H. vitis, H. vox, Pigritia dido, P. faux, P. gruis, P. haha, P. sedis, P. stips, and P. ululae. Diagnoses, descriptions, and type data are provided for each species. Photographs of imagos, illustrations of wing venation for selected species, male and female genitalia, and distribution maps are furnished. Keys to all genera in Blastobasinae and keys to all species within each genus are provided to assist with identifications. In addition, scanning electron micrographs of the inner surface of the dilated first antennal flagellomere and associated sex scales for all Blastobasis are provided. Blastobasis coffeaella (Busck, 1925), B. graminea Adamski, 1999, Hypatopa tapadulcea Adamski, 1999, and Pigritia marjoriella Adamski, 1998 are redescribed. C1 Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Adamski, D (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC 168,NHB-E519, Washington, DC 20013 USA. EM adamskid@si.edu RI Yakovlev, Roman/J-7243-2013 NR 33 TC 2 Z9 2 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD FEB 25 PY 2013 VL 3618 IS 1 BP 1 EP 223 PG 223 WC Zoology SC Zoology GA 093LU UT WOS:000315194200001 PM 25136727 ER PT J AU Safavi-Naini, A Kim, E Weck, PF Rabl, P Sadeghpour, HR AF Safavi-Naini, A. Kim, E. Weck, P. F. Rabl, P. Sadeghpour, H. R. TI Influence of monolayer contamination on electric-field-noise heating in ion traps SO PHYSICAL REVIEW A LA English DT Article ID AUGMENTED-WAVE METHOD; ENERGY; GOLD AB Electric field noise is a hinderance to the assembly of large-scale quantum computers based on entangled trapped ions. Apart from ubiquitous technical noise, experimental studies of trapped ion heating have revealed additional limiting contributions to this noise, originating from atomic processes on the electrode surfaces. In a recent work [Safavi-Naini, Rabl, Weck, and Sadeghpour, Phys. Rev. A 84, 023412 (2011)] we described a microscopic model for this excess electric field noise, which points away towards a more systematic understanding of surface adsorbates as progenitors of electric field jitter noise. Here, we address the impact of surface monolayer contamination on adsorbate-induced noise processes. Using exact numerical calculations for H and N atomic monolayers on a Au(111) surface, representing opposite extremes of physisorption and chemisorption, we show that an additional monolayer can significantly affect the noise power spectrum and, respectively, enhance and suppress the heating rates. DOI: 10.1103/PhysRevA.87.023421 C1 [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Safavi-Naini, A.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kim, E.] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA. [Weck, P. F.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Rabl, P.] TU Wien, Inst Atom & Subatom Phys, A-1020 Vienna, Austria. RP Safavi-Naini, A (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Rabl, Peter/F-2810-2012; OI Rabl, Peter/0000-0002-2560-8835; , Philippe/0000-0002-7610-2893 FU US Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; Austrian Academy of Sciences; Austrian Science Fund (FWF) through START [Y 591-N16]; NSF at the Harvard-Smithsonian Center for Astrophysics FX Sandia National Laboratories is a multiprogram laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the US Department of Energy's National Nuclear Security Administration under Contract No. DE-AC04-94AL85000. P. R. acknowledges support by the Austrian Academy of Sciences and the Austrian Science Fund (FWF) through START Grant No. Y 591-N16. This work was supported by NSF through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. NR 38 TC 10 Z9 10 U1 0 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD FEB 22 PY 2013 VL 87 IS 2 AR 023421 DI 10.1103/PhysRevA.87.023421 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 094NF UT WOS:000315270200009 ER PT J AU Baldeck, CA Harms, KE Yavitt, JB John, R Turner, BL Valencia, R Navarrete, H Davies, SJ Chuyong, GB Kenfack, D Thomas, DW Madawala, S Gunatilleke, N Bunyavejchewin, S Kiratiprayoon, S Yaacob, A Supardi, MNN Dalling, JW AF Baldeck, Claire A. Harms, Kyle E. Yavitt, Joseph B. John, Robert Turner, Benjamin L. Valencia, Renato Navarrete, Hugo Davies, Stuart J. Chuyong, George B. Kenfack, David Thomas, Duncan W. Madawala, Sumedha Gunatilleke, Nimal Bunyavejchewin, Sarayudh Kiratiprayoon, Somboon Yaacob, Adzmi Supardi, Mohd N. Nur Dalling, James W. TI Soil resources and topography shape local tree community structure in tropical forests SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE beta diversity; community structure; dispersal; soil; topography; tropical forest ID BETA DIVERSITY; HABITAT ASSOCIATIONS; NEIGHBOR MATRICES; ECOLOGICAL DATA; RAIN-FORESTS; HETEROGENEITY; DISTRIBUTIONS; ORDINATION; NUTRIENTS; PATTERNS AB Both habitat filtering and dispersal limitation influence the compositional structure of forest communities, but previous studies examining the relative contributions of these processes with variation partitioning have primarily used topography to represent the influence of the environment. Here, we bring together data on both topography and soil resource variation within eight large (24-50 ha) tropical forest plots, and use variation partitioning to decompose community compositional variation into fractions explained by spatial, soil resource and topographic variables. Both soil resources and topography account for significant and approximately equal variation in tree community composition (9-34% and 5-29%, respectively), and all environmental variables together explain 13-39% of compositional variation within a plot. A large fraction of variation (19-37%) was spatially structured, yet unexplained by the environment, suggesting an important role for dispersal processes and unmeasured environmental variables. For the majority of sites, adding soil resource variables to topography nearly doubled the inferred role of habitat filtering, accounting for variation in compositional structure that would previously have been attributable to dispersal. Our results, illustrated using a new graphical depiction of community structure within these plots, demonstrate the importance of small-scale environmental variation in shaping local community structure in diverse tropical forests around the globe. C1 [Baldeck, Claire A.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Baldeck, Claire A.; Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Harms, Kyle E.; Turner, Benjamin L.; Davies, Stuart J.; Dalling, James W.] Smithsonian Trop Res Inst, Panama City, Panama. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [John, Robert] Indian Inst Sci Educ & Res, Nadia 741252, W Bengal, India. [Valencia, Renato; Navarrete, Hugo] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Apartado 17012184, Quito, Ecuador. [Davies, Stuart J.; Kenfack, David] Harvard Univ, Arnold Arboretum Asia Program, Ctr Trop Forest Sci, Cambridge, MA USA. [Chuyong, George B.] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon. [Thomas, Duncan W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Madawala, Sumedha; Gunatilleke, Nimal; Bunyavejchewin, Sarayudh] Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka. [Bunyavejchewin, Sarayudh] Dept Natl Pk Wildlife & Plant Conservat, Bangkok 10900, Thailand. [Kiratiprayoon, Somboon] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. [Yaacob, Adzmi] Univ Teknol MARA, Fac Plantat & Agrotechnol, Shah Alam 40450, Staffs, Malaysia. [Supardi, Mohd N. Nur] Forest Res Inst Malaysia, Forest Environm Div, Kepong 52109, Selangor Darul, Malaysia. RP Baldeck, CA (reprint author), Univ Illinois, Program Ecol Evolut & Conservat Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM baldeck2@life.illinois.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU US National Science Foundation [DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818, OISE 0314581]; Smithsonian Tropical Research Institute; CTFS FX Financial support for soils work was provided by the US National Science Foundation grants DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818 and OISE 0314581, the soils initiative of the Smithsonian Tropical Research Institute, and a CTFS grant to cover collection and extraction of soils from Korup. We also thank Jonathan Myers, Editor Fangliang He and two anonymous reviewers for their valuable comments on the manuscript. The tree census and topographic data are maintained by CTFS and data enquiries should be made to Stuart Davies. The soils data are maintained by J.W.D. and enquires should be made to him. NR 35 TC 42 Z9 42 U1 6 U2 117 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD FEB 22 PY 2013 VL 280 IS 1753 AR UNSP 20122532 DI 10.1098/rspb.2012.2532 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 070ML UT WOS:000313510600010 PM 23256196 ER PT J AU Vilstrup, JT Seguin-Orlando, A Stiller, M Ginolhac, A Raghavan, M Nielsen, SCA Weinstock, J Froese, D Vasiliev, SK Ovodov, ND Clary, J Helgen, KM Fleischer, RC Cooper, A Shapiro, B Orlando, L AF Vilstrup, Julia T. Seguin-Orlando, Andaine Stiller, Mathias Ginolhac, Aurelien Raghavan, Maanasa Nielsen, Sandra C. A. Weinstock, Jacobo Froese, Duane Vasiliev, Sergei K. Ovodov, Nikolai D. Clary, Joel Helgen, Kristofer M. Fleischer, Robert C. Cooper, Alan Shapiro, Beth Orlando, Ludovic TI Mitochondrial Phylogenomics of Modern and Ancient Equids SO PLOS ONE LA English DT Article ID MAXIMUM-LIKELIHOOD; PHYLOGENETIC ANALYSIS; EQUUS-CABALLUS; GENUS EQUUS; EVOLUTIONARY HISTORY; MOLECULAR ECOLOGY; EXTINCT QUAGGA; CONTROL REGION; DNA-SEQUENCES; FOSSIL HORSES AB The genus Equus is richly represented in the fossil record, yet our understanding of taxonomic relationships within this genus remains limited. To estimate the phylogenetic relationships among modern horses, zebras, asses and donkeys, we generated the first data set including complete mitochondrial sequences from all seven extant lineages within the genus Equus. Bayesian and Maximum Likelihood phylogenetic inference confirms that zebras are monophyletic within the genus, and the Plains and Grevy's zebras form a well-supported monophyletic group. Using ancient DNA techniques, we further characterize the complete mitochondrial genomes of three extinct equid lineages (the New World stilt-legged horses, NWSLH; the subgenus Sussemionus; and the Quagga, Equus quagga quagga). Comparisons with extant taxa confirm the NWSLH as being part of the caballines, and the Quagga and Plains zebras as being conspecific. However, the evolutionary relationships among the non-caballine lineages, including the now-extinct subgenus Sussemionus, remain unresolved, most likely due to extremely rapid radiation within this group. The closest living outgroups (rhinos and tapirs) were found to be too phylogenetically distant to calibrate reliable molecular clocks. Additional mitochondrial genome sequence data, including radiocarbon dated ancient equids, will be required before revisiting the exact timing of the lineage radiation leading up to modern equids, which for now were found to have possibly shared a common ancestor as far as up to 4 Million years ago (Mya). C1 [Vilstrup, Julia T.; Seguin-Orlando, Andaine; Ginolhac, Aurelien; Raghavan, Maanasa; Nielsen, Sandra C. A.; Orlando, Ludovic] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Copenhagen, Denmark. [Stiller, Mathias; Shapiro, Beth] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Weinstock, Jacobo] Univ Southampton, Fac Humanities, Southampton, Hants, England. [Froese, Duane] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2M7, Canada. [Vasiliev, Sergei K.] Russian Acad Sci, Inst Archaeol & Ethnog, Novosibirsk, Russia. [Ovodov, Nikolai D.] Russian Acad Sci, Inst Archaeol & Ethnog, Lab Archaeol & Paleogeog Cent Siberia, Novosibirsk, Russia. [Clary, Joel] Musee Confluences, Ctr Conservat & Etud Collect, Lyon, France. [Helgen, Kristofer M.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, Washington, DC 20560 USA. [Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Cooper, Alan] Univ Adelaide, Sch Earth & Environm Sci, Australian Ctr Ancient DNA, Adelaide, SA 5005, Australia. RP Orlando, L (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Copenhagen, Denmark. EM lorlando@snm.ku.dk RI Cooper, Alan/E-8171-2012; Orlando, Ludovic/A-8932-2013; OI Cooper, Alan/0000-0002-7738-7851; Orlando, Ludovic/0000-0003-3936-1850; Raghavan, Maanasa/0000-0003-1997-0739; Shapiro, Beth/0000-0002-2733-7776 FU Danish National Research foundation; Marie Curie Intra European Fellowship [FP7-IEF-299176]; Marie-Curie Career Integration Grant [FP7-CIG-293845]; Australian Research Council; US National Science Foundation ARC [0909456]; Searle Scholars Program; David and Lucille Packard Foundation FX Julia Vilstrup is supported by a PhD grant from The Danish National Research foundation; Aurelien Ginolhac is supported by a Marie Curie Intra European Fellowship (FP7-IEF-299176); this research was also funded by one Marie-Curie Career Integration Grant (FP7-CIG-293845); Alan Cooper is supported by the Australian Research Council; Mathias Stiller and Beth Shapiro are supported by the US National Science Foundation ARC 0909456, the Searle Scholars Program, and by the David and Lucille Packard Foundation. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 77 TC 28 Z9 29 U1 0 U2 78 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 20 PY 2013 VL 8 IS 2 AR e55950 DI 10.1371/journal.pone.0055950 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 093IE UT WOS:000315184200033 PM 23437078 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, Benjamin C. Kenyon, Scott J. TI MIGRATION OF SMALL MOONS IN SATURN's RINGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-disk interactions; planetary systems; planets and satellites: formation; planets and satellites: general; planets and satellites: individual: Saturn; planets and satellites: rings ID I PLANETARY MIGRATION; BODY-COAGULATION CODE; GAS GIANT PLANETS; ORBITAL MIGRATION; DENSITY WAVES; ENCKE GAP; PROTOPLANETARY DISK; SECULAR EVOLUTION; SATELLITE SYSTEM; ACCRETION DISKS AB The motions of small moons through Saturn's rings provide excellent tests of radial migration models. In theory, torque exchange between these moons and ring particles leads to radial drift. We predict that moons with Hill radii r(H) similar to 2-24 km should migrate through the A ring in 1000 yr. In this size range, moons orbiting in an empty gap or in a full ring eventually migrate at the same rate. Smaller moons or moonlets-such as the propellers-are trapped by diffusion of disk material into corotating orbits, creating inertial drag. Larger moons-such as Pan or Atlas-do not migrate because of their own inertia. Fast migration of 2-24 km moons should eliminate intermediate-size bodies from the A ring and may be responsible for the observed large-radius cutoff of r(H) similar to 1-2 km in the size distribution of the A ring's propeller moonlets. Although the presence of Daphnis (r(H) approximate to 5 km) inside the Keeler gap challenges this scenario, numerical simulations demonstrate that orbital resonances and stirring by distant, larger moons (e. g., Mimas) may be important factors. For Daphnis, stirring by distant moons seems the most promising mechanism to halt fast migration. Alternatively, Daphnis may be a recent addition to the ring that is settling into a low inclination orbit in similar to 10(3) yr prior to a phase of rapid migration. We provide predictions of observational constraints required to discriminate among possible scenarios for Daphnis. C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA's Astrophysics Theory Program; Origin of Solar Systems Program [NNX10AF35G]; Outer Planets Program [NNX11AM37G] FX We are grateful for advice and comments from M. Geller. We thank A. Youdin for suggesting important improvements to the manuscript. Numerous helpful comments from the referee, M. Tiscareno, significantly improved the text. Portions of this project were supported by NASA's Astrophysics Theory Program and the Origin of Solar Systems Program through grant NNX10AF35G and the Outer Planets Program through grant NNX11AM37G. We also acknowledge generous allotments of computer time on the NASA "discover" computer cluster operated by the National Center for Climate Simulation. NR 95 TC 7 Z9 7 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 192 DI 10.1088/0004-637X/764/2/192 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600080 ER PT J AU Drake, JJ Cohen, O Yashiro, S Gopalswamy, N AF Drake, Jeremy J. Cohen, Ofer Yashiro, Seiji Gopalswamy, Nat TI IMPLICATIONS OF MASS AND ENERGY LOSS DUE TO CORONAL MASS EJECTIONS ON MAGNETICALLY ACTIVE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: flare; stars: winds, outflows; Sun: coronal mass ejections (CMEs); X-rays: stars ID SOLAR PARTICLE EVENTS; EARTH-LIKE EXOPLANETS; IN HABITABLE ZONES; X-RAY-EMISSION; ANGULAR-MOMENTUM; TERRESTRIAL EXOPLANETS; STELLAR CORONAE; PROTON EVENTS; FLARE ENERGY; CME ACTIVITY AB Analysis of a database of solar coronal mass ejections (CMEs) and associated flares over the period 1996-2007 finds well-behaved power-law relationships between the 1-8 angstrom flare X-ray fluence and CME mass and kinetic energy. We extrapolate these relationships to lower and higher flare energies to estimate the mass and energy loss due to CMEs from stellar coronae, assuming that the observed X-ray emission of the latter is dominated by flares with a frequency as a function of energy dn/dE = kE(-alpha). For solar-like stars at saturated levels of X-ray activity, the implied losses depend fairly weakly on the assumed value of alpha and are very large: (M) over dot similar to 5 x 10(-10) M-circle dot yr(-1) and (E) over dot similar to 0.1 L-circle dot. In order to avoid such large energy requirements, either the relationships between CME mass and speed and flare energy must flatten for X-ray fluence greater than or similar to 10(31) erg, or the flare-CME association must drop significantly below 1 for more energetic events. If active coronae are dominated by flares, then the total coronal energy budget is likely to be up to an order of magnitude larger than the canonical 10(-3) L-bol X-ray saturation threshold. This raises the question of what is the maximum energy a magnetic dynamo can extract from a star? For an energy budget of 1% of L-bol, the CME mass loss rate is about 5 x 10(-11) M-circle dot yr(-1). C1 [Drake, Jeremy J.; Cohen, Ofer] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yashiro, Seiji] Interferometrics Inc, Herndon, VA 20171 USA. [Yashiro, Seiji; Gopalswamy, Nat] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu OI Gopalswamy, Nat/0000-0001-5894-9954; Cohen, Ofer/0000-0003-3721-0215 FU NASA [NAS8-03060]; Chandra Grant [TM2-13001X] FX J.J.D. was funded by NASA contract NAS8-03060 to the Chandra X-Ray Center (CXC) and thanks the CXC director, H. Tananbaum, and the CXC science team for continuing advice and support. O.C. was supported by Chandra Grant TM2-13001X. J.J.D. also thanks David Soderblom for organizing a workshop on the Faint Early Sun that provided the impetus for this study, and Vinay Kashyap for fruitful discussion. Finally, we thank the referee for a very helpful report that enabled us to improve the manuscript significantly. NR 75 TC 20 Z9 20 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 170 DI 10.1088/0004-637X/764/2/170 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600058 ER PT J AU Fohlmeister, J Kochanek, CS Falco, EE Wambsganss, J Oguri, M Dai, XY AF Fohlmeister, Janine Kochanek, Christopher S. Falco, Emilio E. Wambsganss, Joachim Oguri, Masamune Dai, Xinyu TI A TWO-YEAR TIME DELAY FOR THE LENSED QUASAR SDSS J1029+2623 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; gravitational lensing: strong; quasars: individual (SDSS J102913.94+262317.9) ID HUBBLE CONSTANT; HE 0435-1223; SEPARATION; IMAGE; VARIABILITY; CURVE AB We present 279 epochs of optical monitoring data spanning 5.4 years from 2007 January to 2012 June for the largest image separation (22.'' 6) gravitationally lensed quasar, SDSS J1029+2623. We find that image A leads the images B and C by Delta t(AB) = (744 +/- 10) days (90% confidence); the uncertainty includes both statistical uncertainties and systematic differences due to the choice of models. With only a similar to 1% fractional error, the interpretation of the delay is limited primarily by cosmic variance due to fluctuations in the mean line-of-sight density. We cannot separate the fainter image C from image B, but since image C trails image B by only 2-3 days in all models, the estimate of the time delay between images A and B is little affected by combining the fluxes of images B and C. There is weak evidence for a low level of microlensing, perhaps created by the small galaxy responsible for the flux ratio anomaly in this system. Interpreting the delay depends on better constraining the shape of the gravitational potential using the lensed host galaxy, other lensed arcs, and the structure of the X-ray emission. C1 [Fohlmeister, Janine; Wambsganss, Joachim] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oguri, Masamune] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Dai, Xinyu] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. RP Fohlmeister, J (reprint author), Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. RI Oguri, Masamune/C-6230-2011; Dai, Xinyu/B-5735-2011 OI Dai, Xinyu/0000-0001-9203-2808 FU Smithsonian Astrophysical Observatory; NSF [AST-1009756]; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)"; World Premier International Research Center Initiative (WPI Initiative); MEXT, Japan; JSPS [23740161]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank all the participating observers at the Harvard-Smithsonian Center for Astrophysics for their support of these observations. Our observations were obtained with the F. L. Whipple 1.2 m telescope, with support from the Smithsonian Astrophysical Observatory. C. S. K. is supported by NSF grant AST-1009756. This work was supported in part by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 27 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 186 DI 10.1088/0004-637X/764/2/186 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600074 ER PT J AU Fryer, CL Belczynski, K Berger, E Thone, C Ellinger, C Bulik, T AF Fryer, Chris L. Belczynski, Krzysztof Berger, Edo Thoene, Christina Ellinger, Carola Bulik, Tomasz TI THE POPULATION OF HELIUM-MERGER PROGENITORS: OBSERVATIONAL PREDICTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: neutron; supernovae: general ID GAMMA-RAY BURSTS; BLACK-HOLE; MASSIVE STARS; BINARY EVOLUTION; ACCRETION DISKS; CLOSE BINARIES; SUPERNOVAE; NUCLEOSYNTHESIS; HYDRODYNAMICS; DYNAMICS AB The helium-merger gamma-ray burst (GRB) progenitor is produced by the rapid accretion onto a compact remnant (neutron star or black hole) when it undergoes a common envelope inspiral with its companion's helium core. This merger phase produces a very distinct environment around these outbursts and recent observations suggest that, in some cases, we are detecting the signatures of the past merger in the GRB afterglow. These observations allow us, for the first time, to study the specific features of the helium-merger progenitor. In this paper, we couple population synthesis calculations to our current understanding of GRB engines and common envelope evolution to make observational predictions for the helium-merger GRB population. Many mergers do not produce GRB outbursts and we discuss the implications of these mergers with the broader population of astrophysical transients. C1 [Fryer, Chris L.] Los Alamos Natl Lab, CCS Div, Los Alamos, NM 87545 USA. [Fryer, Chris L.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Fryer, Chris L.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Belczynski, Krzysztof; Bulik, Tomasz] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, Krzysztof] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thoene, Christina] IAA CSIC, E-18008 Granada, Spain. [Ellinger, Carola] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. RP Fryer, CL (reprint author), Los Alamos Natl Lab, CCS Div, POB 1663, Los Alamos, NM 87545 USA. OI Thone, Christina/0000-0002-7978-7648 FU U.S. Dept. of Energy; MSHE [N203 404939]; [W-7405-ENG-36] FX This project was funded in part under the auspices of the U.S. Dept. of Energy, and supported by its contract W-7405-ENG-36 to Los Alamos National Laboratory. K. B. acknowledges support from MSHE grant No. N203 404939. NR 52 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 181 DI 10.1088/0004-637X/764/2/181 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600069 ER PT J AU Gladders, MD Rigby, JR Sharon, K Wuyts, E Abramson, LE Dahle, H Persson, SE Monson, AJ Kelson, DD Benford, DJ Murphy, D Bayliss, MB Finkelstein, KD Koester, BP Bans, A Baxter, EJ Helsby, JE AF Gladders, Michael D. Rigby, Jane R. Sharon, Keren Wuyts, Eva Abramson, Louis E. Dahle, Hakon Persson, S. E. Monson, Andrew J. Kelson, Daniel D. Benford, Dominic J. Murphy, David Bayliss, Matthew B. Finkelstein, Keely D. Koester, Benjamin P. Bans, Alissa Baxter, Eric J. Helsby, Jennifer E. TI SGAS 143845.1+145407: A BIG, COOL STARBURST AT REDSHIFT 0.816 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; gravitational lensing: strong ID SPECTRAL ENERGY-DISTRIBUTIONS; LENSED SUBMILLIMETER GALAXIES; STAR-FORMING GALAXIES; LYMAN BREAK GALAXIES; SOUTH-POLE TELESCOPE; GIANT ARCS SURVEY; INFRARED GALAXIES; INTERNAL KINEMATICS; STELLAR POPULATION; HERSCHEL-ATLAS AB We present the discovery and detailed multi-wavelength study of a strongly lensed luminous infrared galaxy at z = 0.816. Unlike most known lensed galaxies discovered at optical or near-infrared wavelengths, this lensed source is red, (r - K-s)(AB) = 3.9, which the data presented here demonstrate is due to ongoing dusty star formation. The overall lensing magnification (a factor of 17) facilitates observations from the blue optical through to 500 mu m, fully capturing both the stellar photospheric emission and the re-processed thermal dust emission. We also present optical and near-IR spectroscopy. These extensive data show that this lensed galaxy is in many ways typical of IR-detected sources at z similar to 1, with both a total luminosity and size in accordance with other (albeit much less detailed) measurements for samples of galaxies observed in deep fields with the Spitzer telescope. Its far-infrared spectral energy distribution is well fit by local templates that are an order of magnitude less luminous than the lensed galaxy; local templates of comparable luminosity are too hot to fit. Its size (D similar to 7 kpc) is much larger than local luminous infrared galaxies, but in line with sizes observed for such galaxies at z similar to 1. The star formation appears uniform across this spatial scale. In this source, the luminosity of which is typical of sources that dominate the cosmic infrared background, we find that star formation is spatially extended and well organized, quite unlike the compact merger-driven starbursts that are typical for sources of this luminosity at z similar to 0. C1 [Gladders, Michael D.; Wuyts, Eva; Abramson, Louis E.; Bans, Alissa; Baxter, Eric J.; Helsby, Jennifer E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.; Sharon, Keren; Wuyts, Eva; Abramson, Louis E.; Helsby, Jennifer E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Rigby, Jane R.; Benford, Dominic J.] NASA, Observat Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Persson, S. E.; Monson, Andrew J.; Kelson, Daniel D.; Murphy, David] Carnegie Observ, Pasadena, CA 91101 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Finkelstein, Keely D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Koester, Benjamin P.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. RP Gladders, MD (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM gladders@oddjob.uchicago.edu RI Rigby, Jane/D-4588-2012; Benford, Dominic/D-4760-2012 OI Rigby, Jane/0000-0002-7627-6551; Benford, Dominic/0000-0002-9884-4206 FU Research Corporation; National Aeronautics and Space Administration (NASA); NASA through JPL/Caltech; NASA Keck PI Data Award; W. M. Keck Foundation; NASA; NSF; UVES Paranal Observatory Project [266.D-5655] FX M.D.G. thanks the Research Corporation for support of this work through a Cottrell Scholars award.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA).; This work made use of observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Partial support for this work was provided by NASA through an award issued by JPL/Caltech.; This work includes observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the National Science Foundation (NSF) on behalf of the Gemini partnership: the NSF (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia, Tecnologia e Inovao (Brazil), and Ministerio de Ciencia, Tecnologa e Innovacin Productiva (Argentina).; This work was partially supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. This work includes data obtained at the W. M. Keck Observatory from telescope time allocated to NASA through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF.; We acknowledge the use of data from the UVES Paranal Observatory Project (ESO DDT Program ID 266.D-5655). This paper makes use of the ROSAT Data Archive of the Max-Planck-Institut fur extraterrestrische Physik (MPE) at Garching, Germany. NR 80 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 177 DI 10.1088/0004-637X/764/2/177 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600065 ER PT J AU Harvey, PM Fallscheer, C Ginsburg, A Terebey, S Andre, P Bourke, TL Di Francesco, J Konyves, V Matthews, BC Peterson, DE AF Harvey, Paul M. Fallscheer, Cassandra Ginsburg, Adam Terebey, Susan Andre, Philippe Bourke, Tyler L. Di Francesco, James Koenyves, Vera Matthews, Brenda C. Peterson, Dawn E. TI A FIRST LOOK AT THE AURIGA-CALIFORNIA GIANT MOLECULAR CLOUD WITH HERSCHEL AND THE CSO: CENSUS OF THE YOUNG STELLAR OBJECTS AND THE DENSE GAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: clouds; ISM: structure; stars: formation ID STAR-FORMATION; MILKY-WAY; SPITZER SURVEY; MISSION; CLUSTER; NEARBY; PERFORMANCE; POPULATION; EXTRACTION; OPHIUCHUS AB We have mapped the Auriga/California molecular cloud with the Herschel PACS and SPIRE cameras and the Bolocam 1.1 mm camera on the Caltech Submillimeter Observatory with the eventual goal of quantifying the star formation and cloud structure in this giant molecular cloud (GMC) that is comparable in size and mass to the Orion GMC, but which appears to be forming far fewer stars. We have tabulated 60 compact 70/160 mu m sources that are likely pre-main-sequence objects and correlated those with Spitzer and WISE mid-IR sources. At 1.1 mm, we find 18 cold, compact sources and discuss their properties. The most important result from this part of our study is that we find a modest number of additional compact young objects beyond those identified at shorter wavelengths with Spitzer. We also describe the dust column density and temperature structure derived from our photometric maps. The column density peaks at a few x 10(22) cm(-2) (N-H2) and is distributed in a clear filamentary structure along which nearly all of the pre-main-sequence objects are found. We compare the young stellar object surface density to the gas column density and find a strong nonlinear correlation between them. The dust temperature in the densest parts of the filaments drops to similar to 10 K from values similar to 14-15 K in the low-density parts of the cloud. We also derive the cumulative mass fraction and probability density function of material in the cloud, which we compare with similar data on other star-forming clouds. C1 [Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Fallscheer, Cassandra] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Ginsburg, Adam] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Terebey, Susan] Calif State Univ Los Angeles, Dept Phys & Astron PS315, Los Angeles, CA 90032 USA. [Andre, Philippe; Koenyves, Vera] Univ Paris Diderot, CNRS, DSM, Lab AIM,CEA,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Di Francesco, James; Matthews, Brenda C.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Koenyves, Vera] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France. [Peterson, Dawn E.] Space Sci Inst, Boulder, CO 80303 USA. RP Harvey, PM (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA. EM pmh@astro.as.utexas.edu; Cassandra.Fallscheer@nrc-cnrc.gc.ca; adam.ginsburg@colorado.edu; sterebe@calstatela.edu; pandre@cea.fr; tbourke@cfa.harvard.edu; James.DiFrancesco@nrc-cnrc.gc.ca; vera.konyves@cea.fr; Brenda.Matthews@nrc-cnrc.gc.ca; dpeterson@spacescience.org OI Ginsburg, Adam/0000-0001-6431-9633 FU NASA issued by the Jet Propulsion Laboratory, California Institute of Technology [1433108]; National Aeronautics and Space Administration; National Science Foundation [AST-0838261] FX We thank Nicholas Chapman and Giles Novak for their help with the CSO/Bolocam observations, and we also thank the anonymous referee who provided a number of comments that noticeably improved this paper. Support for this work, as part of the NASA Herschel Science Center data analysis funding program, was provided by NASA through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology to the University of Texas. Partial support for T. L. B. was provided by NASA through contract 1433108 issued by the Jet Propulsion Laboratory, California Institute of Technology, to the Smithsonian Astronomical Observatory.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has also made use of the SIMBAD database, operated at CDS, Strasbourg, France. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). NR 43 TC 20 Z9 20 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 133 DI 10.1088/0004-637X/764/2/133 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600021 ER PT J AU Juneau, S Dickinson, M Bournaud, F Alexander, DM Daddi, E Mullaney, JR Magnelli, B Kartaltepe, JS Hwang, HS Willner, SP Coil, AL Rosario, DJ Trump, JR Weiner, BJ Willmer, CNA Cooper, MC Elbaz, D Faber, SM Frayer, DT Kocevski, DD Laird, ES Monkiewicz, JA Nandra, K Newman, JA Salim, S Symeonidis, M AF Juneau, Stephanie Dickinson, Mark Bournaud, Frederic Alexander, David M. Daddi, Emanuele Mullaney, James R. Magnelli, Benjamin Kartaltepe, Jeyhan S. Hwang, Ho Seong Willner, S. P. Coil, Alison L. Rosario, David J. Trump, Jonathan R. Weiner, Benjamin J. Willmer, Christopher N. A. Cooper, Michael C. Elbaz, David Faber, S. M. Frayer, David T. Kocevski, Dale D. Laird, Elise S. Monkiewicz, Jacqueline A. Nandra, Kirpal Newman, Jeffrey A. Salim, Samir Symeonidis, Myrto TI WIDESPREAD AND HIDDEN ACTIVE GALACTIC NUCLEI IN STAR-FORMING GALAXIES AT REDSHIFT > 0.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: high-redshift; galaxies: ISM; galaxies: star formation; infrared: galaxies ID SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH STRIP; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; HARD X-RAY; DIGITAL SKY SURVEY; SIMILAR-TO 2; MASS-METALLICITY RELATION; GOODS-NORTH FIELD; HOST GALAXIES AB We characterize the incidence of active galactic nuclei (AGNs) in 0.3 < z < 1 star-forming galaxies by applying multi-wavelength AGN diagnostics (X-ray, optical, mid-infrared, radio) to a sample of galaxies selected at 70 mu m from the Far-Infrared Deep Extragalactic Legacy survey (FIDEL). Given the depth of FIDEL, we detect "normal" galaxies on the specific star formation rate (sSFR) sequence as well as starbursting systems with elevated sSFR. We find an overall high occurrence of AGN of 37% +/- 3%, more than twice as high as in previous studies of galaxies with comparable infrared luminosities and redshifts but in good agreement with the AGN fraction of nearby (0.05 < z < 0.1) galaxies of similar infrared luminosities. The more complete census of AGNs comes from using the recently developed Mass-Excitation (MEx) diagnostic diagram. This optical diagnostic is also sensitive to X-ray weak AGNs and X-ray absorbed AGNs, and reveals that absorbed active nuclei reside almost exclusively in infrared-luminous hosts. The fraction of galaxies hosting an AGN appears to be independent of sSFR and remains elevated both on the sSFR sequence and above. In contrast, the fraction of AGNs that are X-ray absorbed increases substantially with increasing sSFR, possibly due to an increased gas fraction and/or gas density in the host galaxies. C1 [Juneau, Stephanie; Bournaud, Frederic; Daddi, Emanuele; Elbaz, David] CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Juneau, Stephanie; Weiner, Benjamin J.; Willmer, Christopher N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Dickinson, Mark; Kartaltepe, Jeyhan S.; Monkiewicz, Jacqueline A.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Alexander, David M.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Magnelli, Benjamin] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Hwang, Ho Seong; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Coil, Alison L.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA. [Rosario, David J.; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Trump, Jonathan R.; Faber, S. M.; Kocevski, Dale D.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Frayer, David T.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Laird, Elise S.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Monkiewicz, Jacqueline A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Salim, Samir] Indiana Univ, Dept Astron, Bloomington, IN 47404 USA. [Symeonidis, Myrto] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Juneau, S (reprint author), CEA Saclay, DSM IRFU SAp, F-91191 Gif Sur Yvette, France. EM stephanie.juneau@cea.fr RI Bournaud, Frederic/K-1263-2013; Daddi, Emanuele/D-1649-2012; OI Daddi, Emanuele/0000-0002-3331-9590; Weiner, Benjamin/0000-0001-6065-7483; Salim, Samir/0000-0003-2342-7501 FU NASA [NAS8-03060]; W. M. Keck Foundation; NSF [AST95-09298, AST-0071048, AST-0071198, AST-0507428, AST-0507483]; NASA LTSA [NNG04GC89G]; National Science Foundation; FQRNT (Fonds Quebecois de recherche sur la nature et la technologie, Canada); Philanthropic Educational Organization (P.E.O.); EU [ERC-StG-257720]; CosmoComp ITN FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, and on observations made with the Chandra X-Ray Observatory, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. Additionally, some of the data used herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The Keck Observatory acknowledges the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community and appreciate the opportunity to conduct observations from this mountain.; Funding for the DEEP2 survey has been provided by NSF grants AST95-09298, AST-0071048, AST-0071198, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. The TKRS was funded by a grant to WMKO by the National Science Foundation's Small Grant for Exploratory Research program.; S.J. was partially funded by a FQRNT fellowship (Fonds Quebecois de recherche sur la nature et la technologie, Canada), a Philanthropic Educational Organization (P.E.O.) Scholar Award. S.J. and F. B. acknowledge support from the EU through grants ERC-StG-257720 and CosmoComp ITN. J.R.M. thanks The Leverhulme Trust. NR 129 TC 47 Z9 47 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 176 DI 10.1088/0004-637X/764/2/176 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600064 ER PT J AU Kallivayalil, N van der Marel, RP Besla, G Anderson, J Alcock, C AF Kallivayalil, Nitya van der Marel, Roeland P. Besla, Gurtina Anderson, Jay Alcock, Charles TI THIRD-EPOCH MAGELLANIC CLOUD PROPER MOTIONS. I. HUBBLE SPACE TELESCOPE/WFC3 DATA AND ORBIT IMPLICATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: kinematics and dynamics; Galaxy: structure; Magellanic Clouds ID STAR-FORMATION HISTORY; HIGH-VELOCITY CLOUDS; DARK-MATTER HALOES; N-BODY SIMULATIONS; MILKY-WAY; COSMOLOGICAL SIMULATIONS; SATELLITE GALAXIES; TIDAL ORIGIN; MASS MODELS; STREAM AB We present proper motions for the Large and Small Magellanic Clouds (LMC and SMC) based on three epochs of Hubble Space Telescope data, spanning a similar to 7 yr baseline, and centered on fields with background QSOs. The first two epochs, the subject of past analyses, were obtained with ACS/HRC, and have been reanalyzed here. The new third epoch with WFC3/UVIS increases the time baseline and provides better control of systematics. The three-epoch data yield proper-motion random errors of only 1%-2% per field. For the LMC this is sufficient to constrain the internal proper-motion dynamics, as will be discussed in a separate paper. Here we focus on the implied center-of-mass proper motions: mu(W,LMC) = -1.910 +/- 0.020 mas yr(-1), mu(N,LMC) = 0.229 +/- 0.047 mas yr(-1), and mu(W,SMC) = -0.772 +/- 0.063 mas yr(-1), mu(N,SMC) = -1.117 +/- 0.061 mas yr(-1). We combine the results with a revised understanding of the solar motion in the Milky Way to derive Galactocentric velocities: v(tot,LMC) = 321 +/- 24 km s(-1) and v(tot,SMC) = 217 +/- 26 km s(-1). Our proper-motion uncertainties are now dominated by limitations in our understanding of the internal kinematics and geometry of the Clouds, and our velocity uncertainties are dominated by distance errors. Orbit calculations for the Clouds around the Milky Way allow a range of orbital periods, depending on the uncertain masses of the Milky Way and LMC. Periods less than or similar to 4 Gyr are ruled out, which poses a challenge for traditional Magellanic Stream models. First-infall orbits are preferred (as supported by other arguments as well) if one imposes the requirement that the LMC and SMC must have been a bound pair for at least several Gyr. C1 [Kallivayalil, Nitya] Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Kallivayalil, Nitya] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [van der Marel, Roeland P.; Anderson, Jay] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Besla, Gurtina] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Alcock, Charles] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kallivayalil, N (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06511 USA. EM nitya.kallivayalil@yale.edu FU NASA from the Space Telescope Science Institute (STScI) [GO-11730, GO-11201]; NASA [NAS 5-26555]; NASA through Hubble Fellowship [HST-HF-51284.01-A] FX We thank Lars Hernquist, Mike Boylan-Kolchin, Marla Geha, Ana Bonaca, Luis Vargas, Nhung Ho, and Jeremy Bradford for useful discussions about this project as a whole. William van Altena, Dana Dinescu, and Terry Girard provided valuable insight on per-field errors versus final errors for the center-of-mass motion. Support for this work was provided by NASA through grants associated with projects GO-11730 and GO-11201 from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. G.B. acknowledges support from NASA through Hubble Fellowship grant HST-HF-51284.01-A. NR 97 TC 102 Z9 102 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 161 DI 10.1088/0004-637X/764/2/161 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600049 ER PT J AU Metzger, BD Kaplan, DL Berger, E AF Metzger, Brian D. Kaplan, David L. Berger, Edo TI COMPARING H alpha AND HI SURVEYS AS MEANS TO A COMPLETE LOCAL GALAXY CATALOG IN THE ADVANCED LIGO/VIRGO ERA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; gamma-ray burst: general; gravitational waves; radio lines: galaxies ID STAR-FORMATION RATE; DIGITAL SKY SURVEY; GAMMA-RAY BURSTS; FRACTION SCALING RELATIONS; HERSCHEL REFERENCE SURVEY; COMPACT OBJECT MERGERS; ARECIBO SDSS SURVEY; I MASS FUNCTION; LUMINOSITY FUNCTION; HOST GALAXIES AB Identifying the electromagnetic counterparts of gravitational wave (GW) sources detected by upcoming networks of advanced ground-based interferometers will be challenging, due in part to the large number of unrelated astrophysical transients within the similar to 10-100 deg(2) sky localizations. A potential way to greatly reduce the number of such false positives is to limit detailed follow-up to only those candidates near galaxies within the GW sensitivity range of similar to 200 Mpc for binary neutron star mergers. Such a strategy is currently hindered by the fact that galaxy catalogs are grossly incomplete within this volume. Here, we compare two methods for completing the local galaxy catalog: (1) a narrowband H alpha imaging survey and (2) an HI emission line radio survey. Using H alpha fluxes, stellar masses (M-star), and star formation rates (SFRs) from galaxies in the Sloan Digital Sky Survey (SDSS), combined with HI data from the GALEX Arecibo SDSS Survey and the Herschel Reference Survey, we estimate that an H alpha survey with a luminosity sensitivity of L-H alpha = 10(40) erg s(-1) at 200 Mpc could achieve a completeness of f(SFR)(H alpha) approximate to 75% with respect to total SFR, but only f(M star)(H alpha) approximate to 33% with respect to M-star (due to lack of sensitivity to early-type galaxies). These numbers are significantly lower than those achieved by an idealized spectroscopic survey due to the loss of H alpha flux resulting from resolving out nearby galaxies and the inability to correct for the underlying stellar continuum. An HI survey with sensitivity similar to the proposed WALLABY survey on ASKAP could achieve f(SFR)(HI) approximate to 80% and f(M star)(HI) approximate to 50%, somewhat higher than that of the H alpha survey. Finally, both H alpha and HI surveys should achieve >= 50% completeness with respect to the host galaxies of short-duration gamma-ray bursts, which may trace the population of binary neutron star mergers. C1 [Metzger, Brian D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08542 USA. [Kaplan, David L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. [Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metzger, BD (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08542 USA. EM bmetzger@astro.princeton.edu; kaplan@uwm.edu; eberger@cfa.harvard.edu FU NASA through Einstein Postdoctoral Fellowship [PF-00065]; Lyman Spitzer, Jr. Fellowship; Department of Astrophysical Sciences at Princeton University; National Science Foundation [PHY11-25915 (KITP), AST-1008353, AST-1107973]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank Jarle Brinchmann and Christy Tremonti for helpful conversations and guidance using the MPA-SDSS galaxy data; Barbara Cantinella and Luca Cortese for helpful conversations and guidance using the GASS and HRS HI data; and Dawn Erb, Wen-fai Fong, Alicia Soderberg, and Mansi Kasliwal for helpful discussions. We are grateful to the KITP in Santa Barbara for hosting the program "Chirps, Mergers and Explosions," where this work began. B.D.M. was supported in part by NASA through Einstein Postdoctoral Fellowship grant No. PF-00065. B.D.M. also acknowledges support from the Lyman Spitzer, Jr. Fellowship awarded by the Department of Astrophysical Sciences at Princeton University. This research was also supported in part by the National Science Foundation under grant Nos. PHY11-25915 (KITP), AST-1008353 (D.L.K.), and AST-1107973 (E.B.). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 84 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 149 DI 10.1088/0004-637X/764/2/149 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600037 ER PT J AU Myers, PC AF Myers, Philip C. TI ORIGIN OF THE DENSE CORE MASS FUNCTION IN CONTRACTING FILAMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID MOLECULAR CLOUD CORES; STAR CLUSTER FORMATION; OPHIUCHI MAIN CLOUD; PHOTODISSOCIATION REGIONS; GRAVITATIONAL COLLAPSE; INITIAL CONDITIONS; LUMINOSITY FUNCTION; GLOBULAR FILAMENTS; CYLINDRICAL CLOUDS; PRESTELLAR CORES AB Mass functions of starless dense cores (CMFs) may arise from contraction and dispersal of core-forming filaments. In an illustrative model, a filament contracts radially by self-gravity, increasing the mass of its cores. During this contraction, FUV photoevaporation and ablation by shocks and winds disperse filament gas and limit core growth. The stopping times of core growth are described by a waiting-time distribution. The initial filament column density profile and the resulting CMF each match recent Herschel observations in detail. Then low-mass cores have short growth ages and arise from the innermost filament gas, while massive cores have long growth ages and draw from more extended filament gas. The model fits the initial density profile and CMF best for mean core density 2 x 10(4) cm(-3) and filament dispersal timescale 0.5 Myr. Then the typical core mass, radius, mean column density, and contraction speed are respectively 0.8 solar masses, 0.06 pc, 6 x 10(21) cm(-2), and 0.07 km s(-1), also in accord with observed values. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmyers@cfa.harvard.edu NR 89 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 140 DI 10.1088/0004-637X/764/2/140 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600028 ER PT J AU Perets, HB Kenyon, SJ AF Perets, Hagai B. Kenyon, Scott J. TI WIND-ACCRETION DISKS IN WIDE BINARIES, SECOND-GENERATION PROTOPLANETARY DISKS, AND ACCRETION ONTO WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: symbiotic; protoplanetary disks; stars: AGB and post-AGB; stars: chemically peculiar; stars: winds, outflows; supernovae: general; white dwarfs ID SPECTRAL ENERGY-DISTRIBUTIONS; T-TAURI STARS; VISCOUS DISKS; SYMBIOTIC STARS; CH STARS; ANALYTIC MODEL; SOLAR NEBULA; RS OPHIUCHI; CI CYGNI; MIRA-B AB Mass transfer from an evolved donor star to its binary companion is a standard feature of stellar evolution in binaries. In wide binaries, the companion star captures some of the mass ejected in a wind by the primary star. The captured material forms an accretion disk. Here, we study the evolution of wind-accretion disks, using a numerical approach which allows us to follow the long-term evolution. For a broad range of initial conditions, we derive the radial density and temperature profiles of the disk. In most cases, wind accretion leads to long-lived stable disks over the lifetime of the asymptotic giant branch donor star. The disks have masses of a few times 10(-5)-10(-3) M-circle dot, with surface density and temperature profiles that follow broken power laws. The total mass in the disk scales approximately linearly with the viscosity parameter used. Roughly, 50%-80% of the mass falling into the disk accretes onto the central star; the rest flows out through the outer edge of the disk into the stellar wind of the primary. For systems with large accretion rates, the secondary accretes as much as 0.1 M-circle dot. When the secondary is a white dwarf, accretion naturally leads to nova and supernova eruptions. For all types of secondary star, the surface density and temperature profiles of massive disks resemble structures observed in protoplanetary disks, suggesting that coordinated observational programs might improve our understanding of uncertain disk physics. C1 [Perets, Hagai B.] Technion Israel Inst Technol, Haifa, Israel. [Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perets, HB (reprint author), Technion Israel Inst Technol, Haifa, Israel. EM hperets@physics.technion.ac.il RI Perets, Hagai/K-9605-2015; OI Perets, Hagai/0000-0002-5004-199X; Kenyon, Scott/0000-0003-0214-609X NR 58 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 169 DI 10.1088/0004-637X/764/2/169 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600057 ER PT J AU Sato, M Reid, MJ Menten, KM Carilli, CL AF Sato, M. Reid, M. J. Menten, K. M. Carilli, C. L. TI ON MEASURING THE COSMIC MICROWAVE BACKGROUND TEMPERATURE AT REDSHIFT 0.89 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: ISM; quasars: absorption lines; quasars: individual (PKS 1830-211) ID LENS PKS 1830-211; RADIO-SOURCE PKS1830-211; GRAVITATIONAL LENS; MOLECULAR ABSORPTION; COLOGNE DATABASE; EINSTEIN RING; PKS-1830-211; SPECTRUM; SYSTEM; SPECTROSCOPY AB We report on a measurement of the temperature of the cosmic microwave background radiation field, T-CMB, at z = 0.88582 by imaging HC3N(3 <- 2) and (5 <- 4) absorption in the foreground galaxy of the gravitationally lens magnified radio source PKS 1830-211 using the Very Long Baseline Array and the phased Very Large Array. Low-resolution imaging of the data yields a value of T-rot = 5.6(-0.9)(+2.5) K for the rotational temperature, T-rot, which is consistent with the temperature of the cosmic microwave background at the absorber's redshift of 2.73(1 + z) K. However, our high-resolution imaging reveals that the absorption peak position of the foreground gas is offset from the continuum peak position of the synchrotron radiation from PKS 1830-211SW, which indicates that the absorbing cloud is covering only part of the emission from PKS 1830-211, rather than the entire core-jet region. This changes the line-to-continuum ratios, and we find T-rot between 1.1 and 2.5 K, which is lower than the expected value. This shows that previous T-rot measurements could be biased due to unresolved structure. C1 [Sato, M.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Sato, M (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. FU JSPS FX M.S. acknowledges financial support from a JSPS Postdoctoral Fellowship for Research Abroad. The authors are grateful to Christian Henkel and Arnaud Belloche for careful reading of the manuscript and to Joris Verbiest for discussions and contributions to the manuscript. We thank the referee, Professor Francoise Combes, for insightful comments and suggestions that improved the paper. NR 35 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 132 DI 10.1088/0004-637X/764/2/132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600020 ER PT J AU Winkler, PF Williams, BJ Blair, WP Borkowski, KJ Ghavamian, P Long, KS Raymond, JC Reynolds, SP AF Winkler, P. Frank Williams, Brian J. Blair, William P. Borkowski, Kazimierz J. Ghavamian, Parviz Long, Knox S. Raymond, John C. Reynolds, Stephen P. TI THE FIRST REPORTED INFRARED EMISSION FROM THE SN 1006 REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (SNR SN1006); ISM: kinematics and dynamics; ISM: supernova remnants; shock waves ID LARGE-MAGELLANIC-CLOUD; GALACTIC SUPERNOVA-REMNANTS; BALMER-DOMINATED SHOCKS; SPITZER-SPACE-TELESCOPE; DUST DESTRUCTION; IA SUPERNOVA; NONRADIATIVE SHOCKS; OPTICAL REMNANT; PROPER MOTIONS; SN-1006 AB We report results of infrared imaging and spectroscopic observations of the SN 1006 remnant, carried out with the Spitzer Space Telescope. The 24 mu m image from Multiband Imaging Photometer for Spitzer clearly shows faint filamentary emission along the northwest rim of the remnant shell, nearly coincident with the Balmer filaments that delineate the present position of the expanding shock. The 24 mu m emission traces the Balmer filaments almost perfectly but lies a few arcsec within, indicating an origin in interstellar dust heated by the shock. Subsequent decline in the IR behind the shock is presumably due largely to grain destruction through sputtering. The emission drops far more rapidly than current models predict, however, even for a higher proportion of small grains than would be found closer to the Galactic plane. The rapid drop may result in part from a grain density that has always been lower-a relic effect from an earlier epoch when the shock was encountering a lower density-but higher grain destruction rates still seem to be required. Spectra from three positions along the NW filament from the Infrared Spectrometer instrument all show only a featureless continuum, consistent with thermal emission from warm dust. The dust-to-gas mass ratio in the pre-shock interstellar medium (ISM) is lower than that expected for the Galactic ISM-as has also been observed in the analysis of IR emission from other supernova remnants, but whose cause remains unclear. As with other Type Ia supernova (SN Ia) remnants, SN 1006 shows no evidence for dust grain formation in the SN ejecta. C1 [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA. [Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Winkler, PF (reprint author), Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. EM winkler@middlebury.edu; brian.j.williams@nasa.gov; wpb@pha.jhu.edu; kborkow@ncsu.edu; pghavamian@towson.edu; long@stsci.edu; jraymond@cfa.harvard.edu; reynolds@ncsu.edu FU NASA [RSA 1330031, NNX11AB14G]; NSF [AST-0908566] FX This research is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We are grateful to the support staff at IPAC for their guidance with some of the subtleties of Spitzer data analysis. We also acknowledge thoughtful comments from the anonymous referee, which have prompted us to, we hope, clarify much of this paper. Primary financial support for this project has been provided by NASA through RSA 1330031. P.F.W. acknowledges additional support from the NSF through grant AST-0908566, and K.J.B. acknowledges additional support from NASA through grant NNX11AB14G. NR 67 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 2013 VL 764 IS 2 AR 156 DI 10.1088/0004-637X/764/2/156 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088CY UT WOS:000314812600044 ER PT J AU Busquet, G Zhang, QZ Palau, A Liu, HB Sanchez-Monge, A Estalella, R Ho, PTP de Gregorio-Monsalvo, I Pillai, T Wyrowski, F Girart, JM Santos, FP Franco, GAP AF Busquet, Gemma Zhang, Qizhou Palau, Aina Liu, Hauyu Baobab Sanchez-Monge, Alvaro Estalella, Robert Ho, Paul T. P. de Gregorio-Monsalvo, Itziar Pillai, Thushara Wyrowski, Friedrich Girart, Josep M. Santos, Fabio P. Franco, Gabriel A. P. TI UNVEILING A NETWORK OF PARALLEL FILAMENTS IN THE INFRARED DARK CLOUD G14.225-0.506 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: clouds; ISM: individual objects (G14.225-0.506); stars: formation ID MASSIVE STAR-FORMATION; LARGE-SCALE STRUCTURE; MOLECULAR CLOUDS; CORE FORMATION; H2O MASERS; FRAGMENTATION; NH3; REGIONS; GAS; CS AB We present the results of combined NH3 (1,1) and (2,2) line emission observed with the Very Large Array and the Effelsberg 100 m telescope of the infrared dark cloud G14.225-0.506. The NH3 emission reveals a network of filaments constituting two hub-filament systems. Hubs are associated with gas of rotational temperature T-rot similar to 15 K, non-thermal velocity dispersion sigma(NT) similar to 1 km s(-1), and exhibit signs of star formation, while filaments appear to be more quiescent (T-rot similar to 11 K and sigma(NT) similar to 0.6 km s(-1)). Filaments are parallel in projection and distributed mainly along two directions, at P.A. similar to 10 degrees and 60 degrees, and appear to be coherent in velocity. The averaged projected separation between adjacent filaments is between 0.5 pc and 1 pc, and the mean width of filaments is 0.12 pc. Cores within filaments are separated by similar to 0.33 +/- 0.09 pc, which is consistent with the predicted fragmentation of an isothermal gas cylinder due to the "sausage"-type instability. The network of parallel filaments observed in G14.225-0.506 is consistent with the gravitational instability of a thin gas layer threaded by magnetic fields. Overall, our data suggest that magnetic fields might play an important role in the alignment of filaments, and polarization measurements in the entire cloud would lend further support to this scenario. C1 [Busquet, Gemma] INAF Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Busquet, Gemma; Estalella, Robert] Univ Barcelona IEEC UB, Dept Astron & Meteorol, ICC, E-08028 Barcelona, Catalunya, Spain. [Zhang, Qizhou; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Palau, Aina; Girart, Josep M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, E-08193 Barcelona, Catalunya, Spain. [Liu, Hauyu Baobab; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Sanchez-Monge, Alvaro] Osserv Astrofis Arcetri, INAF, I-05125 Florence, Italy. [de Gregorio-Monsalvo, Itziar] European So Observ, D-85748 Garching, Germany. [de Gregorio-Monsalvo, Itziar] Join ALMA Observ, Santiago, Chile. [Pillai, Thushara] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Wyrowski, Friedrich] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Santos, Fabio P.; Franco, Gabriel A. P.] Dept Fis ICEx UFMG, BR-30123970 Belo Horizonte, MG, Brazil. RP Busquet, G (reprint author), INAF Ist Astrofis & Planetol Spaziali, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM gemma.busquet@iaps.inaf.it RI Franco, Gabriel/A-8009-2011; Girart, Josep/O-1638-2014; OI Franco, Gabriel/0000-0003-2020-2649; Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU Italian Space Agency (ASI) fellowship [I/005/07/0]; Spanish MICINN grant [AYA2011-30228-C03]; FEDER funds; JAE-Doc CSIC fellowship; European Social Fund, under the program "Junta para la Ampliacion de Estudios"; AGAUR grant [2009SGR1172]; CNPq; FAPEMIG FX The authors are grateful to the anonymous referee for valuable comments. G.B. is deeply grateful to Eugenio Schisano for very fruitful discussion on filaments. G.B. is funded by an Italian Space Agency (ASI) fellowship under contract number I/005/07/0. A.P., R.E., and I.d.G.-M. are supported by the Spanish MICINN grant AYA2011-30228-C03 (co-funded with FEDER funds). A.P. is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund, under the program "Junta para la Ampliacion de Estudios," and by the AGAUR grant 2009SGR1172 (Catalonia). F.P.S. and G.A.P.F. are partially supported by CNPq and FAPEMIG. This work is partially based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. NR 45 TC 32 Z9 32 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 20 PY 2013 VL 764 IS 2 AR L26 DI 10.1088/2041-8205/764/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088EX UT WOS:000314817700008 ER PT J AU Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Baring, MG Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Busetto, G Buson, S Caliandro, GA Cameron, RA Caraveo, PA Casandjian, JM Cecchi, C Celik, O Charles, E Chaty, S Chaves, RCG Chekhtman, A Cheung, CC Chiang, J Chiaro, G Cillis, AN Ciprini, S Claus, R Cohen-Tanugi, J Cominsky, LR Conrad, J Corbel, S Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Falletti, L Favuzzi, C Ferrara, EC Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Germani, S Giglietto, N Giommi, P Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hayashi, K Hays, E Hewitt, JW Hill, AB Hughes, RE Jackson, MS Jogler, T Johannesson, G Johnson, AS Kamae, T Kataoka, J Katsuta, J Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lovellette, MN Lubrano, P Madejski, GM Massaro, F Mayer, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mignani, RP Mitthumsiri, W Mizuno, T Moiseev, AA Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nemmen, R Nuss, E Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Ritz, S Romoli, C Sanchez-Conde, M Schulz, A Sgro, C Simeon, PE Siskind, EJ Smith, DA Spandre, G Spinelli, P Stecker, FW Strong, AW Suson, DJ Tajima, H Takahashi, H Takahashi, T Tanaka, T Thayer, JG Thayer, JB Thompson, DJ Thorsett, SE Tibaldo, L Tibolla, O Tinivella, M Troja, E Uchiyama, Y Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Werner, M Winer, BL Wood, KS Wood, M Yamazaki, R Yang, Z Zimmer, S AF Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Baring, M. G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Busetto, G. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Casandjian, J. M. Cecchi, C. Celik, O. Charles, E. Chaty, S. Chaves, R. C. G. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Cillis, A. N. Ciprini, S. Claus, R. Cohen-Tanugi, J. Cominsky, L. R. Conrad, J. Corbel, S. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Falletti, L. Favuzzi, C. Ferrara, E. C. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Germani, S. Giglietto, N. Giommi, P. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hayashi, K. Hays, E. Hewitt, J. W. Hill, A. B. Hughes, R. E. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Kamae, T. Kataoka, J. Katsuta, J. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Madejski, G. M. Massaro, F. Mayer, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mignani, R. P. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nemmen, R. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Ritz, S. Romoli, C. Sanchez-Conde, M. Schulz, A. Sgro, C. Simeon, P. E. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Stecker, F. W. Strong, A. W. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Tanaka, T. Thayer, J. G. Thayer, J. B. Thompson, D. J. Thorsett, S. E. Tibaldo, L. Tibolla, O. Tinivella, M. Troja, E. Uchiyama, Y. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Werner, M. Winer, B. L. Wood, K. S. Wood, M. Yamazaki, R. Yang, Z. Zimmer, S. TI Detection of the Characteristic Pion-Decay Signature in Supernova Remnants SO SCIENCE LA English DT Article ID GAMMA-RAY EMISSION; LARGE-AREA TELESCOPE; IC 443; COSMIC-RAYS; FERMI LAT; SNR W44; ACCELERATION; CLOUDS; DISCOVERY; RADIATION AB Cosmic rays are particles (mostly protons) accelerated to relativistic speeds. Despite wide agreement that supernova remnants (SNRs) are the sources of galactic cosmic rays, unequivocal evidence for the acceleration of protons in these objects is still lacking. When accelerated protons encounter interstellar material, they produce neutral pions, which in turn decay into gamma rays. This offers a compelling way to detect the acceleration sites of protons. The identification of pion-decay gamma rays has been difficult because high-energy electrons also produce gamma rays via bremsstrahlung and inverse Compton scattering. We detected the characteristic pion-decay feature in the gamma-ray spectra of two SNRs, IC 443 and W44, with the Fermi Large Area Telescope. This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs. C1 [Ackermann, M.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Katsuta, J.; Lande, J.; Madejski, G. M.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Simeon, P. E.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Jogler, T.; Johnson, A. S.; Kamae, T.; Katsuta, J.; Lande, J.; Madejski, G. M.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Simeon, P. E.; Tajima, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Chaty, S.; Chaves, R. C. G.; Corbel, S.; Grenier, I. A.] Univ Paris Diderot, Serv Astrophys, Lab AIM, CEA Saclay,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sezione Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Busetto, G.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. 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[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Celik, O.; Moiseev, A. A.; Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Celik, O.; Moiseev, A. A.; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, O.; Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, O.; Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Chekhtman, A.; Cheung, C. C.; Razzaque, S.] USN, Res Lab, Washington, DC 20375 USA. [Cheung, C. C.] USN, Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Chiaro, G.] Ist Nazl Fis Nucl, I-35131 Padua, Italy. [Cillis, A. N.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Falletti, L.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, Montpellier, France. [Cominsky, L. R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Conrad, J.; Larsson, S.; Yang, Z.; Zimmer, S.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. 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[Grondin, M. -H.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.; Nakamori, T.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, F-31028 Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Lemoine-Goumard, M.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mignani, R. P.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Ohno, M.; Takahashi, T.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Ritz, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stecker, F. W.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Strong, A. W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tajima, H.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Tanaka, T.] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Thorsett, S. E.] Willamette Univ, Dept Phys, Salem, OR 97031 USA. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Troja, E.] NASA, Postdoctoral Program, Washington, DC USA. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Yamazaki, R.] Aoyama Gakuin Univ, Dept Phys & Math, Sagamihara, Kanagawa 2525258, Japan. RP Funk, S (reprint author), Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. EM funk@slac.stanford.edu; ttanaka@cr.scphys.kyoto-u.ac.jp; uchiyama@slac.stanford.edu RI Sgro, Carmelo/K-3395-2016; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Massaro, Francesco/L-9102-2016; Orlando, E/R-5594-2016; OI Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Massaro, Francesco/0000-0002-1704-9850; Thorsett, Stephen/0000-0002-2025-9613; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Baldini, Luca/0000-0002-9785-7726 FU NASA; U.S. Department of Energy (United States); CEA/Irfu; IN2P3/CNRS (France); ASI; INFN (Italy); MEXT; KEK; JAXA (Japan); K. A. Wallenberg Foundation; Swedish Research Council; National Space Board (Sweden) FX The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and the U.S. Department of Energy (United States); CEA/Irfu and IN2P3/CNRS (France); ASI and INFN (Italy); MEXT, KEK, and JAXA (Japan); and the K. A. Wallenberg Foundation, the Swedish Research Council, and the National Space Board (Sweden). Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. Fermi LAT data are available from the Fermi Science Support Center (http://fermi.gsfc.nasa.gov/ssc). NR 29 TC 185 Z9 190 U1 2 U2 76 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD FEB 15 PY 2013 VL 339 IS 6121 BP 807 EP 811 DI 10.1126/science.1231160 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 088YS UT WOS:000314874400045 PM 23413352 ER PT J AU Salvador, LA Taori, K Biggs, JS Jakoncic, J Ostrov, DA Paul, VJ Luesch, H AF Salvador, Lilibeth A. Taori, Kanchan Biggs, Jason S. Jakoncic, Jean Ostrov, David A. Paul, Valerie J. Luesch, Hendrik TI Potent Elastase Inhibitors from Cyanobacteria: Structural Basis and Mechanisms Mediating Cytoprotective and Anti-Inflammatory Effects in Bronchial Epithelial Cells SO JOURNAL OF MEDICINAL CHEMISTRY LA English DT Article ID INTERCELLULAR-ADHESION MOLECULE-1; OBSTRUCTIVE PULMONARY-DISEASE; PORCINE PANCREATIC ELASTASE; HUMAN NEUTROPHIL ELASTASE; LARGE GENE LISTS; MARINE CYANOBACTERIUM; ACTIVATED RECEPTORS; CYCLIC DEPSIPEPTIDE; CRYSTAL-STRUCTURES; CYSTIC-FIBROSIS AB We discovered new structural diversity to a prevalent, yet medicinally underappreciated, cyanobacterial protease inhibitor scaffold and undertook comprehensive protease profiling to reveal potent and selective elastase inhibition. Structure-activity relationship (SAR) studies and X-ray cocrystal structure analysis allowed a detailed assessment of critical and tunable structural elements. To realize the therapeutic potential of these cyclodepsipeptides, we probed the cellular effects of a novel and representative family member, symplostatin 5 (1), which attenuated the downstream cellular effects of elastase in an epithelial lung airway model system, alleviating clinical hallmarks of chronic pulmonary diseases such as cell death, cell detachment, and inflammation. This compound attenuated the effects of elastase on receptor activation, proteolytic processing of the adhesion protein ICAM-1, NF-kappa B activation, and transcriptomic changes, including the expression of pro-inflammatory cytokines IL1A, IL1B, and IL8. Compound 1 exhibited activity comparable to the clinically approved elastase inhibitor sivelestat in short-term assays and demonstrated superior sustained activity in longer-term assays. C1 [Salvador, Lilibeth A.; Taori, Kanchan; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Biggs, Jason S.] Univ Guam, Marine Lab, Mangilao, GU 96923 USA. [Jakoncic, Jean] Brookhaven Natl Lab, Upton, NY 11973 USA. [Ostrov, David A.] Univ Florida, Dept Pathol Immunol & Lab Med, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health, NIGMS [P41GM086210] FX We are grateful to J. Rocca (AMRIS) for assistance in obtaining the NMR spectra, J. Quinata of the Cetti Bay Ecostation (Agat, Guam) for collection access, X. Han and J. Yao (Bioinformatics Division, ICBR at UF) for assistance with the microarray analysis. This is contribution #901 from the Smithsonian Marine Station at Fort Pierce. This research was supported by the National Institutes of Health, NIGMS [Grant P41GM086210]. NR 62 TC 17 Z9 17 U1 1 U2 33 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0022-2623 J9 J MED CHEM JI J. Med. Chem. PD FEB 14 PY 2013 VL 56 IS 3 BP 1276 EP 1290 DI 10.1021/jm3017305 PG 15 WC Chemistry, Medicinal SC Pharmacology & Pharmacy GA 093HK UT WOS:000315182100053 PM 23350733 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Buckley, JH Bugaev, V Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Dumm, J Dwarkadas, VV Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Gotthelf, EV Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Hughes, G Humensky, TB Kaaret, P Kargaltsev, O Karlsson, N Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lee, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Roberts, M Saxon, DB Schroedter, M Sembroski, GH Slane, P Smith, AW Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vassiliev, VV Vincent, S Vivier, M Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Buckley, J. H. Bugaev, V. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Gotthelf, E. V. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Hughes, G. Humensky, T. B. Kaaret, P. Kargaltsev, O. Karlsson, N. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Roberts, M. Saxon, D. B. Schroedter, M. Sembroski, G. H. Slane, P. Smith, A. W. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Vivier, M. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI DISCOVERY OF TeV GAMMA-RAY EMISSION FROM CTA 1 BY VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-rays: stars; pulsars: individual (PSR J0007+7303); supernovae: individual (G119.5+10.2); X-rays: individual (RX J0007.0+7303) ID PULSAR-WIND NEBULAE; ATMOSPHERIC CHERENKOV TELESCOPES; SUPERNOVA REMNANT CTA-1; X-RAY; HESS J1825-137; CRAB-NEBULA; CATALOG; PULSATIONS; EVOLUTION; ASTRONOMY AB We report the discovery of TeV gamma-ray emission coincident with the shell-type radio supernova remnant (SNR) CTA 1 using the VERITAS gamma-ray observatory. The source, VER J0006+729, was detected as a 6.5 standard deviation excess over background and shows an extended morphology, approximated by a two-dimensional Gaussian of semimajor (semiminor) axis 0.degrees 30 (0.degrees 24) and a centroid 5' from the Fermi gamma-ray pulsar PSR J0007+7303 and its X-ray pulsar wind nebula (PWN). The photon spectrum is well described by a power-law dN/dE = N-0(E/3 TeV)(-Gamma), with a differential spectral index of Gamma = 2.2 +/- 0.2(stat) +/- 0.3(sys), and normalization N-0 = (9.1 +/- 1.3(stat) +/- 1.7(sys)) x 10(-14) cm(-2) s(-1) TeV-1. The integral flux, F-gamma = 4.0 x 10(-12) erg cm(-2) s(-1) above 1 TeV, corresponds to 0.2% of the pulsar spin-down power at 1.4 kpc. The energetics, colocation with the SNR, and the relatively small extent of the TeV emission strongly argue for the PWN origin of the TeV photons. We consider the origin of the TeV emission in CTA 1. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kargaltsev, O.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Kargaltsev, O.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Dept Astron, Baltimore, MD 21250 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Roberts, M.] Eureka Sci Inc, Oakland, CA 94602 USA. [Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM smcarthur@ulysses.uchicago.edu; muk@astro.columbia.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Roberts, Mallory/0000-0002-9396-9720; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K.; National Science Foundation [AST0908733]; NASA [NAS8-03060] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; O.K. was supported through the National Science Foundation grant No. AST0908733. P. S. acknowledges support from NASA contract NAS8-03060. NR 54 TC 10 Z9 10 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 38 DI 10.1088/0004-637X/764/1/38 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200038 ER PT J AU Bourdin, H Mazzotta, P Markevitch, M Giacintucci, S Brunetti, G AF Bourdin, H. Mazzotta, P. Markevitch, M. Giacintucci, S. Brunetti, G. TI SHOCK HEATING OF THE MERGING GALAXY CLUSTER A521 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A521); galaxies: clusters: intracluster medium; shock waves ID LARGE-SCALE STRUCTURE; XMM-NEWTON; X-RAY; RADIO HALO; CHANDRA OBSERVATION; BOW SHOCK; WAVES; ACCELERATION; SIMULATIONS; EMISSION AB A521 is an interacting galaxy cluster located at z = 0.247, hosting a low-frequency radio halo connected to an eastern radio relic. Previous Chandra observations hinted at the presence of an X-ray brightness edge at the position of the relic, which may be a shock front. We analyze a deep observation of A521 recently performed with XMM-Newton in order to probe the cluster structure up to the outermost regions covered by the radio emission. The cluster atmosphere exhibits various brightness and temperature anisotropies. In particular, two cluster cores appear to be separated by two cold fronts. We find two shock fronts, one that was suggested by Chandra and that is propagating to the east, and another to the southwestern cluster outskirt. The two main interacting clusters appear to be separated by a shock-heated region, which exhibits a spatial correlation with the radio halo. The outer edge of the radio relic coincides spatially with a shock front, suggesting that this shock is responsible for the generation of cosmic-ray electrons in the relic. The propagation direction and Mach number of the shock front derived from the gas density jump, M = 2.4 +/- 0.2, are consistent with expectations from the radio spectral index, under the assumption of Fermi I acceleration mechanism. C1 [Bourdin, H.; Mazzotta, P.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Mazzotta, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Markevitch, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Markevitch, M.; Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Brunetti, G.] INAF Ist Radioastron, I-40129 Bologna, Italy. RP Bourdin, H (reprint author), Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. EM herve.bourdin@roma2.infn.it RI Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Brunetti, Gianfranco/0000-0003-4195-8613 FU ESA Member States; USA (NASA); NASA [NNX09AP45G, NNX09AP36G]; ASI-INAF [I/088/06/0, I/009/10/0]; NASA through Einstein Postdoctoral Fellowship [PF0-110071]; Chandra X-ray Center; PRIN-INAF FX We thank the reviewer for constructive comments and suggestions aimed at improving the manuscript. H. B. thanks the Harvard-Smithsonian Centre for Astrophysics, where this work was initiated, for its hospitality. We thank Chiara Ferrari for providing us with a map of the projected galaxy density distribution in A521, derived from photometric observations performed at the CFH telescope. This work is based on observations obtained with XMM-Newton, an ESA science mission funded by ESA Member States and the USA (NASA). H. B and P. M. acknowledge support by grants NASA grant NNX09AP45G and NNX09AP36G grant ASI-INAF I/088/06/0 and ASI-INAF I/009/10/0. S. G. acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory. G. B. acknowledges partial support from PRIN-INAF2009. NR 44 TC 29 Z9 29 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 82 DI 10.1088/0004-637X/764/1/82 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200082 ER PT J AU Cyganowski, CJ Koda, J Rosolowsky, E Towers, S Meyer, JD Egusa, F Momose, R Robitaille, TP AF Cyganowski, C. J. Koda, J. Rosolowsky, E. Towers, S. Meyer, J. Donovan Egusa, F. Momose, R. Robitaille, T. P. TI A WATER MASER AND NH3 SURVEY OF GLIMPSE EXTENDED GREEN OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: jets and outflows; ISM: molecules; masers; stars: formation ID STAR-FORMING REGIONS; INFRARED DARK CLOUDS; GHZ METHANOL MASERS; ULTRACOMPACT HII-REGIONS; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; CLASS-I; TRIGONOMETRIC PARALLAXES; MOLECULAR CLOUD; ARRAY CAMERA AB We present the results of a Nobeyama 45 m H2O maser and NH3 survey of all 94 northern GLIMPSE extended green objects (EGOs), a sample of massive young stellar objects (MYSOs) identified based on their extended 4.5 mu m emission. We observed the NH3(1,1), (2,2), and (3,3) inversion lines, and detected emission toward 97%, 63%, and 46% of our sample, respectively (median rms similar to 50 mK). The H2O maser detection rate is 68% (median rms similar to 0.11 Jy). The derived H2O maser and clump-scale gas properties are consistent with the identification of EGOs as young MYSOs. To explore the degree of variation among EGOs, we analyze subsamples defined based on mid-infrared (MIR) properties or maser associations. H2O masers and warm dense gas, as indicated by emission in the higher-excitation NH3 transitions, are most frequently detected toward EGOs also associated with both Class I and II CH3OH masers. Ninety-five percent (81%) of such EGOs are detected in H2O (NH3(3,3)), compared to only 33% (7%) of EGOs without either CH3OH maser type. As populations, EGOs associated with Class I and/or II CH3OH masers have significantly higher NH3 line widths, column densities, and kinetic temperatures than EGOs undetected in CH3OH maser surveys. However, we find no evidence for statistically significant differences in H2O maser properties (such as maser luminosity) among any EGO subsamples. Combining our data with the 1.1 mm continuum Bolocam Galactic Plane Survey, we find no correlation between isotropic H2O maser luminosity and clump number density. H2O maser luminosity is weakly correlated with clump (gas) temperature and clump mass. C1 [Cyganowski, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koda, J.; Towers, S.; Meyer, J. Donovan] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Rosolowsky, E.] Univ British Columbia, Dept Phys & Astron, Kelowna BC, BC V1V 1V7, Canada. [Towers, S.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Egusa, F.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Egusa, F.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Momose, R.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Momose, R.] Natl Astron Observ Japan, Tokyo 1818588, Japan. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Cyganowski, CJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ccyganowski@cfa.harvard.edu FU NSF [AST-0808119]; National Science Foundation; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1003134]; NSERC of Canada FX We thank the staff at the Nobeyama Radio Observatory for their support during our observing runs. This research has made use of NASA's Astrophysics Data System Bibliographic Services and the SIMBAD database operated at CDS, Strasbourg, France. Support for this work was provided by NSF grant AST-0808119. C.J.C. was partially supported during this work by a National Science Foundation Graduate Research Fellowship, and is currently supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. C.J.C. thanks M. Reid for helpful discussions about kinematic distances, and J. Brown, L. Chomiuk, and H. Kirk for IDL insight. E. R. is supported by a Discovery Grant from NSERC of Canada. NR 101 TC 18 Z9 18 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 61 DI 10.1088/0004-637X/764/1/61 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200061 ER PT J AU Fragos, T Lehmer, B Tremmel, M Tzanavaris, P Basu-Zych, A Belczynski, K Hornschemeier, A Jenkins, L Kalogera, V Ptak, A Zezas, A AF Fragos, T. Lehmer, B. Tremmel, M. Tzanavaris, P. Basu-Zych, A. Belczynski, K. Hornschemeier, A. Jenkins, L. Kalogera, V. Ptak, A. Zezas, A. TI X-RAY BINARY EVOLUTION ACROSS COSMIC TIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; galaxies: stellar content; stars: evolution; X-rays: binaries; X-rays: diffuse background; X-rays: galaxies ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; BLACK-HOLE BINARIES; STELLAR MASS; LUMINOSITY FUNCTION; GLOBULAR-CLUSTERS; EXPLOSION MECHANISM; ELLIPTIC GALAXIES; FORMATION HISTORY; COMPACT BINARIES AB High-redshift galaxies permit the study of the formation and evolution of X-ray binary (XRB) populations on cosmological timescales, probing a wide range of metallicities and star formation rates (SFRs). In this paper, we present results from a large-scale population synthesis study that models the XRB populations from the first galaxies of the universe until today. We use as input to our modeling the Millennium II cosmological simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history and metallicity evolution of the universe. Our modeling, which is constrained by the observed X-ray properties of local galaxies, gives predictions about the global scaling of emission from XRB populations with properties such as SFR and stellar mass, and the evolution of these relations with redshift. Our simulations show that the X-ray luminosity density (X-ray luminosity per unit volume) from XRBs in our universe today is dominated by low-mass XRBs, and it is only at z greater than or similar to 2.5 that high-mass XRBs become dominant. We also find that there is a delay of similar to 1.1Gyr between the peak of X-ray emissivity from low-mass XRBs (at z similar to 2.1) and the peak of SFR density (at z similar to 3.1). The peak of the X-ray luminosity from high-mass XRBs (at z similar to 3.9) happens similar to 0.8Gyr before the peak of the SFR density, which is due to the metallicity evolution of the universe. C1 [Fragos, T.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lehmer, B.; Tzanavaris, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lehmer, B.; Tzanavaris, P.; Basu-Zych, A.; Hornschemeier, A.; Jenkins, L.; Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tremmel, M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Belczynski, K.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Belczynski, K.] Univ Texas Brownsville, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. RP Fragos, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tfragos@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU CfA; ITC; NASA ADAP [09-ADP09-0071]; Einstein Fellowship Program; NASA Postdoctoral Program Fellowship at Goddard Space Flight Center; MSHE [N203 404939] FX The authors thank the anonymous referee whose careful report has helped to improve this paper. T. F. acknowledges support from the CfA and the ITC prize fellowship programs. This work was partially supported from NASA ADAP grant 09-ADP09-0071 (PI: A. H.). B. L. thanks the Einstein Fellowship Program. P. T. acknowledges support through a NASA Postdoctoral Program Fellowship at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. K. B. acknowledges support from MSHE grant N203 404939. Computational resources supporting this work were provided by Northwestern University Quest HPC cluster and the NASA High-End Computing (HEC) Program through the NASA Center for Climate Simulation (NCCS) at Goddard Space Flight Center. NR 80 TC 54 Z9 54 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 41 DI 10.1088/0004-637X/764/1/41 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200041 ER PT J AU Garraffo, C Cohen, O Drake, JJ Downs, C AF Garraffo, C. Cohen, O. Drake, J. J. Downs, C. TI THE EFFECT OF LIMITED SPATIAL RESOLUTION OF STELLAR SURFACE MAGNETIC FIELD MAPS ON MAGNETOHYDRODYNAMIC WIND AND CORONAL X-RAY EMISSION MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: magnetic field ID GLOBAL SOLAR CORONA; LATE-TYPE STARS; AB-DORADUS; EM ALGORITHM; COOL STARS; DIFFERENTIAL ROTATION; MAXIMUM-LIKELIHOOD; ACTIVE STARS; EK DRACONIS; AD-LEO AB We study the influence of the spatial resolution on scales of 5 degrees and smaller of solar surface magnetic field maps on global magnetohydrodynamic solar wind models, and on a model of coronal heating and X-ray emission. We compare the solutions driven by a low-resolution Wilcox Solar Observatory magnetic map, the same map with spatial resolution artificially increased by a refinement algorithm, and a high-resolution Solar and Heliospheric Observatory Michelson Doppler Imager map. We find that both the wind structure and the X-ray morphology are affected by the fine-scale surface magnetic structure. Moreover, the X-ray morphology is dominated by the closed loop structure between mixed polarities on smaller scales and shows significant changes between high-and low-resolution maps. We conclude that three-dimensional modeling of coronal X-ray emission has greater surface magnetic field spatial resolution requirements than wind modeling, and can be unreliable unless the dominant mixed polarity magnetic flux is properly resolved. C1 [Garraffo, C.; Cohen, O.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Downs, C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RP Garraffo, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cohen, Ofer/0000-0003-3721-0215 FU NASA's CXC [TM2-13001X]; NASA [NAS8-39073]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX We thank the unknown referee for the valuable comments on our manuscript. O.C. is supported by NASA's CXC contract TM2-13001X. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center, and thanks the Director, H. Tananbaum, and the CXC science team for advice and support. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 83 TC 9 Z9 9 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 32 DI 10.1088/0004-637X/764/1/32 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200032 ER PT J AU Geller, MJ Diaferio, A Rines, KJ Serra, AL AF Geller, Margaret J. Diaferio, Antonaldo Rines, Kenneth J. Serra, Ana Laura TI MEASURING THE MASS DISTRIBUTION IN GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark matter; galaxies: clusters: individual (MS0906+11, A750); galaxies: kinematics and dynamics ID LARGE-SCALE STRUCTURE; STRONG LENSING CLUSTERS; DIGITAL SKY SURVEY; EQUATION-OF-STATE; X-RAY-PROPERTIES; DARK-MATTER; INFALL REGIONS; HALO CONCENTRATIONS; CHANDRA OBSERVATION; VIRIAL MASSES AB Cluster mass profiles are tests of models of structure formation. Only two current observational methods of determining the mass profile, gravitational lensing, and the caustic technique are independent of the assumption of dynamical equilibrium. Both techniques enable the determination of the extended mass profile at radii beyond the virial radius. For 19 clusters, we compare the mass profile based on the caustic technique with weak lensing measurements taken from the literature. This comparison offers a test of systematic issues in both techniques. Around the virial radius, the two methods of mass estimation agree to within similar to 30%, consistent with the expected errors in the individual techniques. At small radii, the caustic technique overestimates the mass as expected from numerical simulations. The ratio between the lensing profile and the caustic mass profile at these radii suggests that the weak lensing profiles are a good representation of the true mass profile. At radii larger than the virial radius, the extrapolated Navarro, Frenk & White fit to the lensing mass profile exceeds the caustic mass profile. Contamination of the lensing profile by unrelated structures within the lensing kernel may be an issue in some cases; we highlight the clusters MS0906+11 and A750, superposed along the line of sight, to illustrate the potential seriousness of contamination of the weak lensing signal by these unrelated structures. C1 [Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo; Serra, Ana Laura] Univ Turin, Dipartimento Fis, I-10125 Turin, Italy. [Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Serra, Ana Laura] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Serra, Ana Laura] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; diaferio@ph.unito.it; kenneth.rines@wwu.edu; serra@to.infn.it FU Smithsonian Institution; Cottrell College Science Award from the Research Corporation; PRIN INAF09 "Toward an Italian Network for Computational Cosmology"; INFN [PD51]; PRIN-MIUR FX We thank Ian Dell'Antonio and Scott Kenyon for insightful discussions that helped us clarify issues in this paper. We thank the referee for lucid, incisive comments enabling us to clarify our weak lensing discussion. The Smithsonian Institution partially supports M.J.G.'s research. K. R. was funded by a Cottrell College Science Award from the Research Corporation. A. L. S. acknowledges a fellowship by the PRIN INAF09 "Toward an Italian Network for Computational Cosmology." A. D. and A. L. S. acknowledge partial support from the INFN grant PD51 and the PRIN-MIUR-2008 grant "Matter-antimatter asymmetry, dark matter and dark energy in the LHC Era." NR 66 TC 29 Z9 29 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 58 DI 10.1088/0004-637X/764/1/58 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200058 ER PT J AU Kelly, BC Shen, Y AF Kelly, Brandon C. Shen, Yue TI THE DEMOGRAPHICS OF BROAD-LINE QUASARS IN THE MASS-LUMINOSITY PLANE. II. BLACK HOLE MASS AND EDDINGTON RATIO FUNCTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; AGN MONITORING PROJECT; HIGH-REDSHIFT QUASARS; SIMILAR-TO 1; VELOCITY DISPERSION CORRELATION; FALL EQUATORIAL STRIPE; HUBBLE-SPACE-TELESCOPE; SELF-REGULATED GROWTH; SINGLE-EPOCH SPECTRA AB We employ a flexible Bayesian technique to estimate the black hole (BH) mass and Eddington ratio functions for Type 1 (i.e., broad line) quasars from a uniformly selected data set of similar to 58,000 quasars from the Sloan Digital Sky Survey (SDSS) DR7. We find that the SDSS becomes significantly incomplete at M-BH less than or similar to 3 x 10(8) M-circle dot or L/L-Edd less than or similar to 0.07, and that the number densities of Type 1 quasars continue to increase down to these limits. Both the mass and Eddington ratio functions show evidence of downsizing, with the most massive and highest Eddington ratio BHs experiencing Type 1 quasar phases first, although the Eddington ratio number densities are flat at z < 2. We estimate the maximum Eddington ratio of Type 1 quasars in the observable universe to be L/L-Edd similar to 3. Consistent with our results in Shen & Kelly, we do not find statistical evidence for a so-called sub-Eddington boundary in the mass-luminosity plane of broad-line quasars, and demonstrate that such an apparent boundary in the observed distribution can be caused by selection effect and errors in virial BH mass estimates. Based on the typical Eddington ratio in a given mass bin, we estimate growth times for the BHs in Type 1 quasars and find that they are comparable to or longer than the age of the universe, implying an earlier phase of accelerated (i.e., with higher Eddington ratios) and possibly obscured growth. The large masses probed by our sample imply that most of our BHs reside in what are locally early-type galaxies, and we interpret our results within the context of models of self-regulated BH growth. C1 [Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93107 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kelly, BC (reprint author), Univ Calif Santa Barbara, Dept Phys, Broida Hall, Santa Barbara, CA 93107 USA. FU Southern California Center for Galaxy Evolution; University of California Office of Research; Smithsonian Astrophysical Observatory (SAO); Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Desika Narayanan, Marta Volonteri, and Benny Trakhtenbrot for helpful discussions, and Marianne Vestergaard, Tommaso Treu, Priya Natarajan, Marta Volonteri, Andreas Schulze, and Alister Graham for helpful comments on drafts of our manuscript. We also thank the anonymous referee for comments that helped improve our clarity, focus, and discussion. B. C. K. acknowledges support from the Southern California Center for Galaxy Evolution, a multi-campus research program funded by the University of California Office of Research. Y.S. acknowledges support from the Smithsonian Astrophysical Observatory (SAO) through a Clay Postdoctoral Fellowship.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 255 TC 55 Z9 55 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 45 DI 10.1088/0004-637X/764/1/45 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200045 ER PT J AU Kim, DW Fabbiano, G Ivanova, N Fragos, T Jordan, A Sivakoff, GR Voss, R AF Kim, D. -W. Fabbiano, G. Ivanova, N. Fragos, T. Jordan, A. Sivakoff, G. R. Voss, R. TI METALLICITY EFFECT ON LOW-MASS X-RAY BINARY FORMATION IN GLOBULAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; galaxies: elliptical and lenticular, cD; globular clusters: general; X-rays: binaries; X-rays: galaxies ID EARLY-TYPE GALAXIES; CHANDRA MULTIWAVELENGTH PROJECT; HUBBLE-SPACE-TELESCOPE; ELLIPTIC GALAXIES; STELLAR POPULATIONS; SOURCE CATALOG; DEEP CHANDRA; BLACK-HOLE; WIDE-FIELD; NGC 1399 AB We present comprehensive observational results of the metallicity effect on the fraction of globular clusters (GCs) that contain low-mass X-ray binaries (LMXB), by utilizing all available data obtained with Chandra for LMXBs and Hubble Space Telescope Advanced Camera for Surveys (ACS) for GCs. Our primary sample consists of old elliptical galaxies selected from the ACS Virgo and Fornax surveys. To improve statistics at both the lowest and highest X-ray luminosity, we also use previously reported results from other galaxies. It is well known that the fraction of GCs hosting LMXBs is considerably higher in red, metal-rich, GCs than in blue, metal-poor GCs. In this paper, we test whether this metallicity effect is X-ray luminosity-dependent and find that the effect holds uniformly in a wide luminosity range. This result is statistically significant (at >= 3 sigma) in LMXBs with luminosities in the range L-X = 2 x 10(37) to 5 x 10(38) erg s(-1), where the ratio of GC-LMXB fractions in metal-rich to metal-poor GCs is R = 3.4 +/- 0.5. A similar ratio is also found at lower (down to 10(36) erg s(-1)) and higher luminosities (up to the ULX regime), but with less significance (similar to 2 sigma confidence). Because different types of LMXBs dominate in different luminosities, our finding requires a new explanation for the metallicity effect in dynamically-formed LMXBs. We confirm that the metallicity effect is not affected by other factors such as stellar age, GC mass, stellar encounter rate, and galacto-centric distance. C1 [Kim, D. -W.; Fabbiano, G.; Fragos, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ivanova, N.; Sivakoff, G. R.] Univ Alberta, Dept Phys, Edmonton, AB, Canada. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Jordan, A.] Milky Way Millennium Nucl, Santiago, Chile. [Voss, R.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Sivakoff, Gregory/G-9602-2011; Fragos, Tassos/A-3581-2016; OI Sivakoff, Gregory/0000-0001-6682-916X; Fragos, Tassos/0000-0003-1474-1523; Jordan, Andres/0000-0002-5389-3944 FU NASA [NAS8-39073]; Chandra Guest Observer grant [GO1-12110X]; NSERC; CRC Program; CfA; ITC; Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio [P07-021-F]; BASAL CATA [PFB-06]; Anillo [ACT-086]; National Science Foundation [1066293] FX The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities, and have extracted archival data from the Chandra archives. This work was supported by NASA contract NAS8-39073 (CXC) and Chandra Guest Observer grant GO1-12110X (PI: Fabbiano). N.I. and G. R. S. acknowledge support by NSERC Discovery Grants, with additional support for NI by the CRC Program. T. F. acknowledges support from the CfA and the ITC prize fellowship programs. A.J. acknowledges support from the Chilean Ministry for the Economy, Development, and Tourism's Programa Iniciativa Cientifica Milenio through grant P07-021-F, awarded to The Milky Way Millennium Nucleus, from BASAL CATA PFB-06 and from Anillo ACT-086. This material is based upon work supported in part by the National Science Foundation Grant No. 1066293 and the hospitality of the Aspen Center for Physics. NR 61 TC 11 Z9 11 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 98 DI 10.1088/0004-637X/764/1/98 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200098 ER PT J AU Lal, DV Kraft, RP Randall, SW Forman, WR Nulsen, PEJ Roediger, E ZuHone, JA Hardcastle, MJ Jones, C Croston, JH AF Lal, Dharam V. Kraft, Ralph P. Randall, Scott W. Forman, William R. Nulsen, Paul E. J. Roediger, Elke ZuHone, John A. Hardcastle, Martin J. Jones, Christine Croston, Judith H. TI GAS SLOSHING AND RADIO GALAXY DYNAMICS IN THE CORE OF THE 3C 449 GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (3C 449); hydrodynamics; intergalactic medium; X-rays: galaxies: clusters ID XMM-NEWTON OBSERVATIONS; X-RAY; CHANDRA OBSERVATION; CENTAURUS-A; COLD-FRONT; INTERSTELLAR-MEDIUM; GASEOUS ATMOSPHERE; PERSEUS CLUSTER; VIRGO CLUSTER; SHOCKS AB We present results from a 140 ks Chandra/ACIS-S observation of the hot gas around the canonical FR I radio galaxy 3C 449. An earlier, shorter 30 ks Chandra observation of the group gas showed an unusual entropy distribution and a surface brightness edge in the gas that could be a strong shock around the inner radio lobes. In our deeper data we find no evidence for a temperature increase inside of the brightness edge, but a temperature decrease across part of the edge. This suggests that the edge is a "sloshing" cold front due to a merger within the last less than or similar to 1.3-1.6 Gyr. Both the northern and southern inner jets are bent slightly to the west in projection as they enter their respective lobes, suggesting that the sloshing core is moving to the east. The straight inner jet flares at approximately the position where it crosses the contact edge, suggesting that the jet is entraining and thermalizing some of the hot gas as it crosses the edge. We also detect filaments of X-ray emission around the southern inner radio jet and lobe which we attribute to low entropy entrained gas. The lobe flaring and gas entrainment were originally predicted in simulations of Loken et al. and are confirmed in our deep observation. C1 [Lal, Dharam V.; Kraft, Ralph P.; Randall, Scott W.; Forman, William R.; Nulsen, Paul E. J.; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roediger, Elke] Jacobs Univ Bremen, D-28725 Bremen, Germany. [ZuHone, John A.] NASA GSFC, Greenbelt, MD 20771 USA. [Hardcastle, Martin J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Croston, Judith H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1SJ, Hants, England. RP Lal, DV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Randall, Scott/0000-0002-3984-4337; Nulsen, Paul/0000-0003-0297-4493; Hardcastle, Martin/0000-0003-4223-1117 FU National Aeronautics and Space Administration through Chandra by the Chandra X-Ray Observatory Center [GO9-9111X]; National Aeronautics Space Administration [NAS8-03060]; South-East Physics Network (SEP-Net) FX D.V.L. thanks R. Johnson for many fruitful conversations and is grateful to N. P. Lee for repeated helpwith the "crude" temperature map. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO9-9111X issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. J.H.C. acknowledges support from the South-East Physics Network (SEP-Net). This research has made use of software provided by the Chandra X-Ray Center in the application packages CIAO and Sherpa. This research has made use of the NASA/IPAC Extra-galactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This research has made use of NASA's Astrophysics Data System. NR 48 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 83 DI 10.1088/0004-637X/764/1/83 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200083 ER PT J AU Palamara, DP Brown, MJI Jannuzi, BT Dey, A Stern, D Pimbblet, KA Weiner, BJ Ashby, MLN Kochanek, CS Gonzalez, A Brodwin, M Le Floc'h, E Rieke, M AF Palamara, David P. Brown, Michael J. I. Jannuzi, Buell T. Dey, Arjun Stern, Daniel Pimbblet, Kevin A. Weiner, Benjamin J. Ashby, Matthew L. N. Kochanek, C. S. Gonzalez, Anthony Brodwin, Mark Le Floc'h, Emeric Rieke, Marcia TI THE CLUSTERING OF EXTREMELY RED OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; galaxies: statistics; large-scale structure of universe ID GALAXY REDSHIFT SURVEY; HALO OCCUPATION DISTRIBUTION; WIDE-FIELD SURVEY; PHOTOMETRIC REDSHIFTS; STAR-FORMATION; HIERARCHICAL UNIVERSE; STATISTICAL-ANALYSIS; NUMBER COUNTS; LBDS 53W091; EVOLUTION AB We measure the clustering of extremely red objects (EROs) in approximate to 8 deg(2) of the NOAO Deep Wide Field Survey Bootes field in order to establish robust links between ERO(z approximate to 1.2) and local galaxy (z < 0.1) populations. Three different color selection criteria from the literature are analyzed to assess the consequences of using different criteria for selecting EROs. Specifically, our samples are (R - K-s) > 5.0 (28,724 galaxies), (I - K-s) > 4.0 (22,451 galaxies), and (I - [3.6]) > 5.0 (64,370 galaxies). Magnitude-limited samples show the correlation length (r(0)) to increase for more luminous EROs, implying a correlation with stellar mass. We can separate star-forming and passive ERO populations using the (K-s - [24]) and ([3.6]-[24]) colors to K-s = 18.4 and [3.6] = 17.5, respectively. Star-forming and passive EROs in magnitude-limited samples have different clustering properties and host dark halo masses and cannot be simply understood as a single population. Based on the clustering, we find that bright passive EROs are the likely progenitors of greater than or similar to 4L* elliptical galaxies. Bright EROs with ongoing star formation were found to occupy denser environments than star-forming galaxies in the local universe, making these the likely progenitors of greater than or similar to L* local ellipticals. This suggests that the progenitors of massive greater than or similar to 4L* local ellipticals had stopped forming stars by z greater than or similar to 1.2, but that the progenitors of less massive ellipticals (down to L*) can still show significant star formation at this epoch. C1 [Palamara, David P.; Brown, Michael J. I.; Pimbblet, Kevin A.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Palamara, David P.; Brown, Michael J. I.; Pimbblet, Kevin A.] Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia. [Jannuzi, Buell T.; Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jannuzi, Buell T.; Weiner, Benjamin J.; Rieke, Marcia] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Gonzalez, Anthony] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Le Floc'h, Emeric] Univ Paris Diderot, Lab AIM, CEA Saclay, CNRS,Serv Astrophys, F-91191 Gif Sur Yvette, France. RP Palamara, DP (reprint author), Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Weiner, Benjamin/0000-0001-6065-7483 FU National Optical Astronomy Observatory; Australian postgraduate award (APA); J.L. William postgraduate award; Australian Research Council (ARC) FX This work is based in part on observations made with the Spitzer Space Telescope, Spitzer/IRAC, and Spitzer/MIPS, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is based in part on observations made with the Kitt Peak National Observatory (KPNO). This research was supported by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation. We thank our colleagues on the NDWFS, SDWFS, and MAGES teams. We thank Renbin Yan for providing the DEEP2 EGS spectroscopic data used in this work, Mark Dickinson for providing the FIDEL EGS catalog used in this work, Xu Kong for providing the COSMOS ERO surface density data from Kong et al. (2009), and Chris Conselice for providing the DEEP2 ERO surface density data from Conselice et al. (2008). D. P. P. acknowledges support from an Australian postgraduate award (APA) and a J.L. William postgraduate award. M. J. I. B. acknowledges support from an Australian Research Council (ARC) Future Fellowship. NR 68 TC 4 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 31 DI 10.1088/0004-637X/764/1/31 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200031 ER PT J AU Roediger, E Kraft, RP Forman, WR Nulsen, PEJ Churazov, E AF Roediger, E. Kraft, R. P. Forman, W. R. Nulsen, P. E. J. Churazov, E. TI KELVIN-HELMHOLTZ INSTABILITIES AT THE SLOSHING COLD FRONTS IN THE VIRGO CLUSTER AS A MEASURE FOR THE EFFECTIVE INTRACLUSTER MEDIUM VISCOSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: clusters: intracluster medium; galaxies: individual (M87); hydrodynamics; instabilities; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; GALAXY CLUSTERS; BUOYANT BUBBLES; INTERGALACTIC MEDIUM; THERMAL CONDUCTION; ABUNDANCE PROFILES; MAGNETIC-FIELDS; PERSEUS CLUSTER; GAS; CORES AB Sloshing cold fronts (CFs) arise from minor merger triggered gas sloshing. Their detailed structure depends on the properties of the intracluster medium (ICM): hydrodynamical simulations predict the CFs to be distorted by Kelvin-Helmholtz instabilities (KHIs), but aligned magnetic fields, viscosity, or thermal conduction can suppress the KHIs. Thus, observing the detailed structure of sloshing CFs can be used to constrain these ICM properties. Both smooth and distorted sloshing CFs have been observed, indicating that the KHI is suppressed in some clusters, but not in all. Consequently, we need to address at least some sloshing clusters individually before drawing general conclusions about the ICM properties. We present the first detailed attempt to constrain the ICM properties in a specific cluster from the structure of its sloshing CF. Proximity and brightness make the Virgo Cluster an ideal target. We combine observations and Virgo-specific hydrodynamical sloshing simulations. Here, we focus on a Spitzer-like temperature-dependent viscosity as a mechanism to suppress the KHI, but discuss the alternative mechanisms in detail. We identify the CF at 90 kpc north and northeast of the Virgo center as the best location in the cluster to observe a possible KHI suppression. For viscosities greater than or similar to 10% of the Spitzer value KHIs at this CF are suppressed. We describe in detail the observable signatures at low and high viscosities, i.e., in the presence or the absence of KHIs. We find indications for a low ICM viscosity in archival XMM-Newton data and demonstrate the detectability of the predicted features in deep Chandra observations. C1 [Roediger, E.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Roediger, E.] Jacobs Univ Bremen, Sch Sci & Engn, D-28759 Bremen, Germany. [Roediger, E.; Kraft, R. P.; Forman, W. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churazov, E.] Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Roediger, E (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojensbergsweg 112, D-21029 Hamburg, Germany. EM eroediger@hs.uni-hamburg.de RI Churazov, Eugene/A-7783-2013; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU DFG (German Research Foundation) [1177, 1573]; Julich Supercomputing Center [NIC 4368, 5027]; Smithsonian Astrophysical Observatory; NASA [NAS8-03060] FX E. R. acknowledges support by the Priority Programmes 1177 ("Witnesses of Cosmic History") and 1573 ("Physics of the Interstellar Medium") of the DFG (German Research Foundation), the supercomputing grants NIC 4368 and 5027 at the Julich Supercomputing Center, a visiting scientist fellowship of the Smithsonian Astrophysical Observatory, and the hospitality of the Center for Astrophysics in Cambridge. We thank Marcus Bruggen for helpful discussions and the referee for useful suggestions. This work was supported by NASA grant NAS8-03060. NR 54 TC 22 Z9 22 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 60 DI 10.1088/0004-637X/764/1/60 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200060 ER PT J AU Sakamoto, K Aalto, S Costagliola, F Martin, S Ohyama, Y Wiedner, MC Wilner, DJ AF Sakamoto, Kazushi Aalto, Susanne Costagliola, Francesco Martin, Sergio Ohyama, Youichi Wiedner, Martina C. Wilner, David J. TI SUBMILLIMETER INTERFEROMETRY OF THE LUMINOUS INFRARED GALAXY NGC 4418: A HIDDEN HOT NUCLEUS WITH AN INFLOW AND AN OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: individual (NGC 4418); galaxies: ISM ID ACTIVE GALACTIC NUCLEUS; RESOLUTION MIDINFRARED OBSERVATIONS; STAR-FORMING GALAXIES; MOLECULAR GAS; STARBURST GALAXIES; RADIATION PRESSURE; NEARBY GALAXIES; BLACK-HOLES; CONTINUUM EMISSION; SEYFERT-GALAXIES AB We have observed the nucleus of the nearby luminous infrared galaxy NGC 4418 with subarcsec resolution at 860 and 450 mu m for the first time to characterize its hidden power source. A similar to 20 pc (0.'' 1) hot dusty core was found inside a 100 pc scale concentration of molecular gas at the galactic center. The 860 mu m continuum core has a deconvolved (peak) brightness temperature of 120-210 K. The CO(3-2) peak brightness temperature there is as high as 90 K at 50 pc resolution. The core has a bolometric luminosity of about 10(11) L-circle dot, which accounts for most of the galaxy luminosity. It is Compton thick (N-H greater than or similar to 10(25) cm(-2)) and has a high luminosity-to-mass ratio (L/M) similar to 500 L-circle dot M-circle dot(-1) as well as a high luminosity surface density 10(8.5+/ 0.5) L-circle dot pc(-2). These parameters are consistent with an active galactic nucleus to be the main luminosity source (with an Eddington ratio about 0.3), while they can be also due to a young starburst near its maximum L/M. We also found an optical color (reddening) feature that we attribute to an outflow cone emanating from the nucleus. The hidden hot nucleus thus shows evidence of both an inflow, previously seen with absorption lines, and the new outflow reported here in a different direction. The nucleus must be rapidly evolving with these gas flows. C1 [Sakamoto, Kazushi; Ohyama, Youichi] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Aalto, Susanne; Costagliola, Francesco] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43900 Onsala, Sweden. [Martin, Sergio] European So Observ, Santiago 19, Chile. [Wiedner, Martina C.] Observ Paris, LERMA, F-75014 Paris, France. [Wiedner, Martina C.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sakamoto, K (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. FU Taiwanese National Science Council [99-2112-M-001-011-MY3]; Marie Curie Actions of the European Commission (FP7-COFUND) FX We thank the SMA staff for making these observations possible and Mark Gurwell for helping flux calibration. K. S. thanks Dr. Eduardo Gonzalez-Alfonso for answering questions about his recent work on NGC 4418. This research made use of the NASA/IPAC Extragalactic Database (NED), NASA's Astrophysics Data System (ADS), the splatalogue database for astronomical spectroscopy, the Sloan Digital Sky Survey (SDSS), and the JPL HORIZONS system. K. S. was supported by the Taiwanese National Science Council grant 99-2112-M-001-011-MY3. S. M. acknowledges the co-funding of this work under the Marie Curie Actions of the European Commission (FP7-COFUND). NR 104 TC 26 Z9 26 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 42 DI 10.1088/0004-637X/764/1/42 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200042 ER PT J AU Su, YN van Ballegooijen, A AF Su, Yingna van Ballegooijen, Adriaan TI ROTATING MOTIONS AND MODELING OF THE ERUPTING SOLAR POLAR-CROWN PROMINENCE ON 2010 DECEMBER 6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: magnetic topology; Sun: rotation; Sun: UV radiation; Sun: X-rays, gamma rays ID CORONAL MASS EJECTIONS; X-RAY TELESCOPE; FLUX ROPES; DYNAMICAL EVOLUTION; MAGNETIC HELICITY; SLOW-RISE; FILAMENT; HINODE; FLARE; KINEMATICS AB A large polar-crown prominence composed of different segments spanning nearly the entire solar disk erupted on 2010 December 6. Prior to the eruption, the filament in the active region part split into two layers: a lower layer and an elevated layer. The eruption occurs in several episodes. Around 14: 12 UT, the lower layer of the active region filament breaks apart: One part ejects toward the west, while the other part ejects toward the east, which leads to the explosive eruption of the eastern quiescent filament. During the early rise phase, part of the quiescent filament sheet displays strong rolling motion (observed by STEREO-B) in the clockwise direction (viewed from east to west) around the filament axis. This rolling motion appears to start from the border of the active region, then propagates toward the east. The Atmospheric Imaging Assembly (AIA) observes another type of rotating motion: In some other parts of the erupting quiescent prominence, the vertical threads turn horizontal, then turn upside down. The elevated active region filament does not erupt until 18: 00 UT, when the erupting quiescent filament has already reached a very large height. We develop two simplified three-dimensional models that qualitatively reproduce the observed rolling and rotating motions. The prominence in the models is assumed to consist of a collection of discrete blobs that are tied to particular field lines of a helical flux rope. The observed rolling motion is reproduced by continuous twist injection into the flux rope in Model 1 from the active region side. Asymmetric reconnection induced by the asymmetric distribution of the magnetic fields on the two sides of the filament may cause the observed rolling motion. The rotating motion of the prominence threads observed by AIA is consistent with the removal of the field line dips in Model 2 from the top down during the eruption. C1 [Su, Yingna; van Ballegooijen, Adriaan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C, NNX12AI30G]; LMSAL [SP02H1701R] FX We acknowledge the anonymous referee for valuable comments to improve the paper. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and the NSC (Norway). We thank the teams of SDO/AIA, SDO/HMI, STEREO/EUVI, and Hinode/XRT for providing the valuable data. The STEREO and HMI data are downloaded via the Virtual Solar Observatory and the Joint Science Operations Center. This project is partially supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO as well as NASA grant NNX12AI30G. NR 58 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 91 DI 10.1088/0004-637X/764/1/91 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200091 ER PT J AU Van Loo, S Butler, MJ Tan, JC AF Van Loo, Sven Butler, Michael J. Tan, Jonathan C. TI KILOPARSEC-SCALE SIMULATIONS OF STAR FORMATION IN DISK GALAXIES. I. THE UNMAGNETIZED AND ZERO-FEEDBACK LIMIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: ISM; galaxies: star clusters: general; ISM: clouds; ISM: structure; methods: numerical; stars: formation ID MAGNETICALLY-DOMINATED CLOUDS; GALACTIC MOLECULAR CLOUDS; SHOCK-TRIGGERED FORMATION; ADAPTIVE MESH REFINEMENT; NEUTRAL ATOMIC PHASES; MODELING CO EMISSION; INTERSTELLAR-MEDIUM; SUPERSONIC TURBULENCE; THERMAL-INSTABILITY; PHYSICAL CONDITIONS AB We present hydrodynamic simulations of the evolution of self-gravitating dense gas on scales of 1 kpc down to less than or similar to parsec in a galactic disk, designed to study dense clump formation from giant molecular clouds (GMCs). These structures are expected to be the precursors to star clusters and this process may be the rate limiting step controlling star formation rates in galactic systems as described by the Kennicutt-Schmidt relation. We follow the thermal evolution of the gas down to similar to 5 K using extinction-dependent heating and cooling functions. We do not yet include magnetic fields or localized stellar feedback, so the evolution of the GMCs and clumps is determined solely by self-gravity balanced by thermal and turbulent pressure support and the large-scale galactic shear. While cloud structures and densities change significantly during the simulation, GMC virial parameters remain mostly above unity for timescales exceeding the free-fall time of GMCs indicating that energy from galactic shear and large-scale cloud motions continuously cascades down to and within the GMCs. We implement star formation at a slow, inefficient rate of 2% per local free-fall time, but even this yields global star formation rates that are about two orders of magnitude larger than the observed Kennicutt-Schmidt relation due to overproduction of dense gas clumps. We expect a combination of magnetic support and localized stellar feedback is required to inhibit dense clump formation to similar to 1% of the rate that results from the nonmagnetic, zero-feedback limit. C1 [Van Loo, Sven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Van Loo, Sven; Butler, Michael J.; Tan, Jonathan C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Van Loo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svanloo@cfa.harvard.edu OI Van Loo, Sven/0000-0003-4746-8500 FU UF Department of Astronomy; UF College of Liberal Arts and Sciences; SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory; NSF CAREER [AST-0645412]; NASA [ATP09-0094, ADAP10-0110] FX We thank the anonymous referee for his/her comments that improved the paper, Paola Caselli and Sam Falle for useful discussions, and Elizabeth Tasker for providing the initial conditions of our simulations. S. v. L. acknowledges support from the Theory Postdoctoral Fellowship from UF Department of Astronomy and College of Liberal Arts and Sciences and from the SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory. J.C.T. acknowledges support from NSF CAREER grant AST-0645412; NASA Astrophysics Theory and Fundamental Physics grant ATP09-0094; NASA Astrophysics Data Analysis Program ADAP10-0110. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 79 TC 9 Z9 9 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 2013 VL 764 IS 1 AR 36 DI 10.1088/0004-637X/764/1/36 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081PV UT WOS:000314335200036 ER PT J AU Jimenez-Serra, I Baez-Rubio, A Rivilla, VM Martin-Pintado, J Zhang, Q Dierickx, M Patel, N AF Jimenez-Serra, I. Baez-Rubio, A. Rivilla, V. M. Martin-Pintado, J. Zhang, Q. Dierickx, M. Patel, N. TI A NEW RADIO RECOMBINATION LINE MASER OBJECT TOWARD THE MonR2 H II REGION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects: (Mon R2); ISM: jets and outflows; masers; stars: formation ID MONOCEROS R2; MWC 349; MWC-349; DISK; STARS; ARRAY AB We report the detection of a new radio recombination line (RRL) maser object toward the IRS2 source in the MonR2 ultracompact H II region. The continuum emission at 1.3 mm and 0.85 mm and the H30 alpha and H26 alpha lines were observed with the Submillimeter Array (SMA) at angular resolutions of similar to 0 ''.5-3 ''. The SMA observations show that the MonR2-IRS2 source is very compact and remains unresolved at spatial scales <= 400 AU. Its continuum power spectrum at millimeter wavelengths is almost flat (alpha = - 0.16, with S-nu proportional to nu(alpha)), indicating that this source is dominated by optically thin free-free emission. The H30 alpha and H26 alpha RRL emission is also compact and peaks toward the position of the MonR2-IRS2 source. The measured RRL profiles are double peaked with the H26 alpha line showing a clear asymmetry in its spectrum. Since the derived line-to-continuum flux ratios (similar to 80 and 180 km s(-1) for H30 alpha and H26 alpha, respectively) exceed the LTE predictions, the RRLs toward MonR2-IRS2 are affected by maser amplification. The amplification factors are, however, smaller than those found toward the emission-line star MWC349A, indicating that MonR2-IRS2 is a weakly amplified maser. Radiative transfer modeling of the RRL emission toward this source shows that the RRL masers arise from a dense and collimated jet embedded in a cylindrical ionized wind, oriented nearly along the direction of the line of sight. High-angular resolution observations at submillimeter wavelengths are needed to unveil weakly amplified RRL masers in very young massive stars. C1 [Jimenez-Serra, I.; Zhang, Q.; Dierickx, M.; Patel, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Baez-Rubio, A.; Rivilla, V. M.; Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. RP Jimenez-Serra, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ijimenez-serra@cfa.harvard.edu; baezra@cab.inta-csic.es; ryvendel@gmail.com; jmartin@cab.inta-csic.es; qzhang@cfa.harvard.edu; mdierickx@cfa.harvard.edu; npatel@cfa.harvard.edu RI Baez Rubio, Alejandro/F-8184-2016; Martin-Pintado, Jesus/H-6107-2015; OI Baez Rubio, Alejandro/0000-0001-8125-5993; Martin-Pintado, Jesus/0000-0003-4561-3508; Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Astrophysical Observatory through an SMA fellowship; MICINN [ESP2007-65812-C02-C01, AYA2010-21697-C05-01]; AstroMadrid [CAM S2009/ESP-1496] FX We are grateful to the SMA director and staff for letting us carry out part of the SMA observations under the Harvard Astronomy Ay191 course, and to the Ay191 students for their enthusiasm during this course. We also acknowledge the anonymous referee for the constructive comments to the manuscript. I.J.-S. acknowledges the Smithsonian Astrophysical Observatory for the support provided through an SMA fellowship. J.M.-P. and I.J.-S. have been partially funded by MICINN grants ESP2007-65812-C02-C01 and AYA2010-21697-C05-01 and AstroMadrid (CAM S2009/ESP-1496). NR 28 TC 5 Z9 5 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD FEB 10 PY 2013 VL 764 IS 1 AR L4 DI 10.1088/2041-8205/764/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 081UA UT WOS:000314346700004 ER PT J AU Baker, DM Weigt, L Fogel, M Knowlton, N AF Baker, David M. Weigt, Lee Fogel, Marilyn Knowlton, Nancy TI Ancient DNA from Coral-Hosted Symbiodinium Reveal a Static Mutualism over the Last 172 Years SO PLOS ONE LA English DT Article ID ALGAL SYMBIONTS; GORGONIA-VENTALINA; REEF CORALS; MONTASTRAEA-ANNULARIS; SCLERACTINIAN CORALS; GENUS SYMBIODINIUM; CARIBBEAN CORALS; BLEACHING EVENT; CLIMATE-CHANGE; SPECIFICITY AB Ancient DNA (aDNA) provides powerful evidence for detecting the genetic basis for adaptation to environmental change in many taxa. Among the greatest of changes in our biosphere within the last century is rapid anthropogenic ocean warming. This phenomenon threatens corals with extinction, evidenced by the increasing observation of widespread mortality following mass bleaching events. There is some evidence and conjecture that coral-dinoflagellate symbioses change partnerships in response to changing external conditions over ecological and evolutionary timescales. Until now, we have been unable to ascertain the genetic identity of Symbiodinium hosted by corals prior to the rapid global change of the last century. Here, we show that Symbiodinium cells recovered from dry, century old specimens of 6 host species of octocorals contain sufficient DNA for amplification of the ITS2 subregion of the nuclear ribosomal DNA, commonly used for genotyping within this genus. Through comparisons with modern specimens sampled from similar locales we show that symbiotic associations among several species have been static over the last century, thereby suggesting that adaptive shifts to novel symbiont types is not common among these gorgonians, and perhaps, symbiotic corals in general. C1 [Baker, David M.] Smithsonian Inst, Marine Sci Network, Washington, DC 20560 USA. [Baker, David M.; Fogel, Marilyn] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Weigt, Lee] Smithsonian Inst, Museum Support Ctr, Labs Analyt Biol, Suitland, MD USA. [Knowlton, Nancy] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Baker, DM (reprint author), Smithsonian Inst, Marine Sci Network, Washington, DC 20560 USA. EM dmbaker@hku.hk RI Baker, David/B-2512-2010 OI Baker, David/0000-0002-0308-4954 FU Smithsonian's Marine Science Network Fellowship; Laboratories of Analytical Biology FX This work was funded by the Smithsonian's Marine Science Network Fellowship and the Laboratories of Analytical Biology. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 47 TC 5 Z9 5 U1 0 U2 38 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 6 PY 2013 VL 8 IS 2 AR e55057 DI 10.1371/journal.pone.0055057 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 092WJ UT WOS:000315153400055 PM 23405111 ER PT J AU Goheen, JR Palmer, TM Charles, GK Helgen, KM Kinyua, SN Maclean, JE Turner, BL Young, HS Pringle, RM AF Goheen, Jacob R. Palmer, Todd M. Charles, Grace K. Helgen, Kristofer M. Kinyua, Stephen N. Maclean, Janet E. Turner, Benjamin L. Young, Hillary S. Pringle, Robert M. TI Piecewise Disassembly of a Large-Herbivore Community across a Rainfall Gradient: The UHURU Experiment SO PLOS ONE LA English DT Article ID GRASSLAND PLANT DIVERSITY; AFRICAN SAVANNA; SEMIARID SAVANNA; WOODY COVER; PRODUCTIVITY; ECOSYSTEM; ECOLOGY; EXTINCTION; POPULATION; PREFERENCES AB Large mammalian herbivores (LMH) strongly influence plant communities, and these effects can propagate indirectly throughout food webs. Most existing large-scale manipulations of LMH presence/absence consist of a single exclusion treatment, and few are replicated across environmental gradients. Thus, important questions remain about the functional roles of different LMH, and how these roles depend on abiotic context. In September 2008, we constructed a series of 1-ha herbivore-exclusion plots across a 20-km rainfall gradient in central Kenya. Dubbed "UHURU" (Ungulate Herbivory Under Rainfall Uncertainty), this experiment aims to illuminate the ecological effects of three size classes of LMH, and how rainfall regimes shape the direction and magnitude of these effects. UHURU consists of four treatments: total-exclusion (all ungulate herbivores), mesoherbivore-exclusion (LMH >120-cm tall), megaherbivore-exclusion (elephants and giraffes), and unfenced open plots. Each treatment is replicated three times at three locations ("sites") along the rainfall gradient: low (440 mm/year), intermediate (580 mm/year), and high (640 mm/year). There was limited variation across sites in soil attributes and LMH activity levels. Understory-plant cover was greater in plots without mesoherbivores, but did not respond strongly to the exclusion of megaherbivores, or to the additional exclusion of dik-dik and warthog. Eleven of the thirteen understory plant species that responded significantly to exclusion treatment were more common in exclusion plots than open ones. Significant interactions between site and treatment on plant communities, although uncommon, suggested that differences between treatments may be greater at sites with lower rainfall. Browsers reduced densities of several common overstory species, along with growth rates of the three dominant Acacia species. Small-mammal densities were 2-3 times greater in total-exclusion than in open plots at all sites. Although we expect patterns to become clearer with time, results from 2008-2012 show that the effects of excluding successively smaller-bodied subsets of the LMH community are generally non-additive for a given response variable, and inconsistent across response variables, indicating that the different LMH size classes are not functionally redundant. Several response variables showed significant treatment-by-site interactions, suggesting that the nature of plant-herbivore interactions can vary across restricted spatial scales. C1 [Goheen, Jacob R.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. [Goheen, Jacob R.] Univ Wyoming, Dept Bot, Laramie, WY 82071 USA. [Goheen, Jacob R.; Palmer, Todd M.; Charles, Grace K.; Kinyua, Stephen N.; Maclean, Janet E.; Young, Hillary S.; Pringle, Robert M.] Mpala Res Ctr, Nanyuki, Kenya. [Palmer, Todd M.] Univ Florida, Dept Biol, Gainesville, FL USA. [Helgen, Kristofer M.] Natl Museum Nat Hist, Div Mammals, Washington, DE USA. [Kinyua, Stephen N.] Moi Univ, Dept Wildlife Management, Eldoret, Kenya. [Maclean, Janet E.] Univ British Columbia, Dept Zool, Vancouver, BC, Canada. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Young, Hillary S.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Pringle, Robert M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. RP Pringle, RM (reprint author), Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. EM rpringle@princeton.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Sherwood Family Foundation; National Sciences and Engineering Research Council of Canada; University of Florida; University of British Columbia; US National Science Foundation [DEB-0709880, OISE-0852961, DEB-0444071]; National Geographic Society; Stanford University's Woods Institute for the Environment; University of Wyoming; Harvard University FX The UHURU experiment was built with seed funding from the Sherwood Family Foundation, by grants from the National Sciences and Engineering Research Council of Canada (to JRG), and by the Universities of Florida, and British Columbia. Support for various portions of this study was contributed by the US National Science Foundation (DEB-0709880 and OISE-0852961 to RMP and DEB-0444071 to TMP), the National Geographic Society, Stanford University's Woods Institute for the Environment, the University of Wyoming, and the William F. Milton Fund of Harvard University. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 88 TC 23 Z9 23 U1 5 U2 62 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD FEB 6 PY 2013 VL 8 IS 2 AR e55192 DI 10.1371/journal.pone.0055192 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 092WJ UT WOS:000315153400067 PM 23405122 ER PT J AU Weimer, H Yao, NY Lukin, MD AF Weimer, Hendrik Yao, Norman Y. Lukin, Mikhail D. TI Collectively Enhanced Interactions in Solid-State Spin Qubits SO PHYSICAL REVIEW LETTERS LA English DT Article ID BOSE-EINSTEIN CONDENSATE; N-V CENTERS; RYDBERG BLOCKADE; QUANTUM REGISTER; DIAMOND; DYNAMICS; ELECTRON; ATOMS; RESOLUTION; COHERENCE AB We propose and analyze a technique to collectively enhance interactions between solid-state quantum registers composed from random networks of spin qubits. In such systems, disordered dipolar interactions generically result in localization. Here, we demonstrate the emergence of a single collective delocalized eigenmode as one turns on a transverse magnetic field. The interaction strength between this symmetric collective mode and a remote spin qubit is enhanced by the square root of the number of spins participating in the delocalized mode. Mediated by such collective enhancement, long-range quantum logic between remote spin registers can occur at distances consistent with optical addressing. A specific implementation utilizing nitrogen-vacancy defects in diamond is discussed and the effects of decoherence are considered. DOI: 10.1103/PhysRevLett.110.067601 C1 [Weimer, Hendrik; Yao, Norman Y.; Lukin, Mikhail D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Weimer, H (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM hweimer@cfa.harvard.edu RI Yao, Norman/A-3929-2009 OI Yao, Norman/0000-0003-0194-7266 FU DOE [FG02-97ER25308]; CUA; NSF; DARPA; AFOSR MURI; Packard Foundation; National Science Foundation (NSF) FX We acknowledge fruitful discussions with C. Laumann and S. Bennett. This work was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory, a fellowship within the Postdoc Program of the German Academic Exchange Service (DAAD), the DOE (FG02-97ER25308), CUA, NSF, DARPA, AFOSR MURI, and the Packard Foundation. NR 43 TC 13 Z9 13 U1 1 U2 30 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD FEB 4 PY 2013 VL 110 IS 6 AR 067601 DI 10.1103/PhysRevLett.110.067601 PG 5 WC Physics, Multidisciplinary SC Physics GA 086LY UT WOS:000314686700012 PM 23432308 ER PT J AU Torres, G AF Torres, G. TI Fundamental properties of lower main-sequence stars SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: evolution; stars: late-type; starspots ID LOW-MASS STARS; DWARF ECLIPSING BINARIES; ABSOLUTE DIMENSIONS; CM DRACONIS; EVOLUTIONARY MODELS; MOLECULAR INDEXES; MAGNETIC ACTIVITY; ACCURATE MASSES; RADII; METALLICITY AB The field of exoplanet research has revitalized interest in M dwarfs, which have become favorite targets of Doppler and transit surveys. Accurate measurements of their basic properties such as masses, radii, and effective temperatures have revealed significant disagreements with predictions from stellar evolution theory in the sense that stars are larger and cooler than expected. These anomalies are believed to be due to high levels of activity in these stars. The evidence for the radius discrepancies has grown over the years as more and more determinations have become available; however, fewer of these studies include accurate determinations of the temperatures. The ubiquitous mass-radius diagrams featured in many new discovery papers are becoming more confusing due to increased scatter, which may be due in part to larger than realized systematic errors affecting many of the published measurements. A discussion of these and other issues is given here from an observer's perspective, along with a summary of theoretical efforts to explain the radius and temperature anomalies. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu FU US National Science Foundation [AST-10-07992] FX The author wishes to thank the organizers of the meeting for the invitation to speak. This work was partially supported by grant AST-10-07992 from the US National Science Foundation. NR 52 TC 37 Z9 38 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 4 EP 9 DI 10.1002/asna.201211743 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900002 ER PT J AU Dupuy, TJ Allen, PR Kraus, AL Biller, B Blake, CH Davison, C Deacon, NR Duchene, G Geller, AM King, RR Law, NM Nguyen, DC Reipurth, B Winters, JG Zhang, ZH AF Dupuy, T. J. Allen, P. R. Kraus, A. L. Biller, B. Blake, C. H. Davison, C. Deacon, N. R. Duchene, G. Geller, A. M. King, R. R. Law, N. M. Nguyen, D. C. Reipurth, B. Winters, J. G. Zhang, Z. H. TI Multiplicity of cool dwarfs SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE binaries: eclipsing; stars: formation; stars: low-mass, brown dwarfs; techniques: spectroscopic ID STAR-FORMING REGIONS; WIYN OPEN CLUSTER; STELLAR RADIAL-VELOCITIES; BROWN DWARFS; UPPER-SCORPIUS; T DWARF; BINARIES; COMPANIONS; TAURUS; UNIVERSALITY AB Multiple systems have long been used to probe the origin and evolution of stars of all masses. Only in the past 10-15 years have such studies been extended to brown dwarfs and the lowest mass stars through binary surveys of both young star forming regions and the older field population. In addition, a groundswell of interest in M dwarfs in recent years has resulted in large, modern datasets for these most common stars in the Galaxy, thereby enabling renewed perspectives on their multiplicity properties. These latest observational results have in turn fueled the many theories competing to explain the formation of low-mass stars and brown dwarfs. This Cool Stars 17 splinter session examined the current state of this field by reviewing results from the numerous observational techniques - radial velocities, astrometry, direct imaging, and synoptic surveys - that have been used to study multiplicity from the earliest embedded protostars to objects in young star forming regions, old and intermediate-age clusters, as well as the more heterogeneous field population. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, P. R.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. [Kraus, A. L.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Biller, B.; Deacon, N. R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Blake, C. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Davison, C.; Winters, J. G.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Duchene, G.] UJF, CNRS INSU, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France. [Geller, A. M.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Geller, A. M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, R. R.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Law, N. M.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada. [Nguyen, D. C.] Univ Toronto, Toronto, ON M5S 3H4, Canada. [Nguyen, D. C.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Reipurth, B.] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Zhang, Z. H.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. RP Dupuy, TJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tdupuy@cfa.harvard.edu NR 34 TC 1 Z9 1 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 36 EP 39 DI 10.1002/asna.201211772 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900009 ER PT J AU Gunther, HM AF Guenther, H. M. TI Accretion, winds and outflows in young stars SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars: formation; stars: pre-main sequence; stars: winds, outflows; T Tauri stars ID T-TAURI-STARS; HUBBLE-SPACE-TELESCOPE; POWERED STELLAR WINDS; X-RAY SPECTROSCOPY; DG-TAURI; MAGNETOSPHERIC ACCRETION; MAGNETIC-FIELDS; ULTRAVIOLET-EXCESS; LAUNCHING REGION; OPTICAL OUTFLOW AB Young stars and planetary systems form in molecular clouds. After the initial radial infall an accretion disk develops. For classical T Tauri stars (CTTS, F-K type precursors) the accretion disk does not reach down to the central star, but it is truncated near the co-rotation radius by the stellar magnetic field. The inner edge of the disk is ionized by the stellar radiation, so that the accretion stream is funneled along the magnetic field lines. On the stellar surface an accretion shock develops, which is observed over a wide wavelength range as X-ray emission, UV excess, optical veiling and optical and IR emission lines. Some of the accretion tracers, e. g. Ha, can be calibrated to measure the accretion rate. This accretion process is variable on time scales of hours to years due to changing accretion rates, stellar rotation and reconfiguration of the magnetic field. Furthermore, many (if not all) accreting systems also drive strong outflows which are ultimately powered by accretion. However, the exact driving mechanism is still unclear. Several components could contribute to the outflows: slow, wide-angle disk winds, X-winds launched close to the inner disk rim, and thermally driven stellar winds. In any case, the outflows contain material of very different temperatures and speeds. The disk wind is cool and can have a molecular component with just a few tens of km s(-1), while the central component of the outflow can reach a few 100 km s(-1). In some cases the inner part of the outflow is collimated to a small-angle jet. These jets have an onion-like structure, where the inner components are consecutively hotter and faster. The jets can contain working surfaces, which show up as Herbig-Haro knots. Accretion and outflows in the CTTS phase do not only determine stellar parameters like the rotation rate on the main-sequence, they also can have a profound impact on the environment of young stars. This review concentrates on CTTS in near-by star forming regions where observations of high spatial and spectral resolution are available. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu OI Gunther, Hans Moritz/0000-0003-4243-2840 FU Space Telescope Science Institute [GO-12199.01-A]; NASA [NAS5-26555] FX HMG acknowledges support from grant GO-12199.01-A from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The author thanks Sean Matt for advice on how to show the different winds and magnetic fields in the figure. NR 80 TC 5 Z9 5 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 67 EP 72 DI 10.1002/asna.201211770 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900016 ER PT J AU Dupree, AK AF Dupree, A. K. TI New insights: The accretion process and variable wind from TW Hya SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars: individual (TW Hya); stars: mass-loss; stars: variables: T Tauri, Herbig Ae/Be; stars: winds, outflows; X-rays: stars ID TAURI STARS; LINE PROFILES; HYDRAE; MODELS; DISK AB For the first time in a classical T Tauri star, we are able to trace an accretion event signaled by an hour-long enhancement of X-rays from the accretion shock and revealed through substantial sequential changes in optical emission line profiles. Downflowing turbulent material appears in Ha and H beta emission. He D3 (5876 angstrom) broadens, coupled with an increase in flux. Two hours after the X-ray accretion event, the optical veiling increases due to continuum emission from the hot splashdown region. The response of the stellar coronal emission to the heated photosphere follows about 2.4 hours later, giving direct evidence that the stellar corona is heated in part by accretion. Then, the stellar wind becomes re-established. A model that incorporates the dynamics of this sequential series of events includes: an accretion shock, a cooling downflow in a supersonically turbulent region, followed by photospheric and later, coronal heating. This model naturally explains the presence of broad optical and ultraviolet lines, and affects the mass accretion rates currently determined from emission line profiles. These results, coupled with the large heated coronal region revealed from X-ray diagnostics, suggest that current models are not adequate to explain the accretion process in young stars. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dupree@cfa.harvard.edu NR 15 TC 1 Z9 1 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 73 EP 76 DI 10.1002/asna.201211748 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900017 ER PT J AU Liu, MC Dupuy, TJ Allers, KN AF Liu, M. C. Dupuy, T. J. Allers, K. N. TI Infrared parallaxes of young field brown dwarfs and connections to directly imaged gas-giant exoplanets SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE astrometry; stars: kinematics; stars: low-mass, brown dwarfs ID LOW-MASS STARS; SPECTROSCOPIC OBSERVATIONS; ULTRACOOL DWARFS; COOL NEIGHBORS; HR 8799; CLUSTER; DUSTY AB We have measured high-precision infrared parallaxes with the Canada-France-Hawaii Telescope for a large sample of candidate young (approximate to 10-100 Myr) and intermediate-age (approximate to 100-600 Myr) ultracool dwarfs, with spectral types ranging from M8 to T2.5. These objects are compelling benchmarks for substellar evolution and ultracool atmospheres at lower surface gravities (i.e., masses) than most of the field population. We find that the absolute magnitudes of our young sample can be systematically offset from ordinary (older) field dwarfs, with the young late-M objects being brighter and the young/dusty mid-L (L3-L6.5) objects being fainter, especially at J band. Thus, we conclude the "underluminosity" of the young planetary-mass companions HR 8799b and 2MASS J1207-39b compared to field dwarfs is also manifested in young free-floating brown dwarfs, though the effect is not as extreme. At the same time, some young objects over the full spectral type range of our sample are similar to field objects, and thus a simple correspondence between youth and magnitude offset relative to the field population appears to be lacking. Comparing the kinematics of our sample to nearby stellar associations and moving groups, we identify several new moving group members, including the first free-floating L dwarf in the AB Dor moving group, 2MASS J0355+11. Altogether, the effects of surface gravity (age) and dust content on the magnitudes and colors of substellar objects appear to be degenerate. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Liu, M. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allers, K. N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM mliu@ifa.hawii.edu FU NSF [AST-0507833, AST09-09222]; NASA [HF-51271.01-A] FX This research was supported by NSF grants AST-0507833 and AST09-09222 (awarded to MCL) and NASA grant #HF-51271.01-A (awarded to TJD). NR 24 TC 20 Z9 20 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 85 EP 88 DI 10.1002/asna.201211783 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900020 ER PT J AU Cushing, MC Kirkpatrick, JD Gelino, CR Wright, EL Gizis, JE Gomes, JI Leggett, SK Lodieu, N Mace, GN Dupuy, TJ AF Cushing, M. C. Kirkpatrick, J. D. Gelino, C. R. Wright, E. L. Gizis, J. E. Gomes, J. I. Leggett, S. K. Lodieu, N. Mace, G. N. Dupuy, T. J. TI Furthering our knowledge of the solar neighborhood using WISE SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE astrometry; stars: low-mass, brown dwarfs; stars: luminosity function, mass function; surveys ID INFRARED-SURVEY-EXPLORER; BROWN DWARF; T-DWARFS; L/T TRANSITION; FIELD; DISCOVERY; BINARIES; ATMOSPHERES; CLOUDS; NEARBY AB The launch of NASA's Wide-field Infrared Survey Explorer (WISE) in late 2009 ushered in an new era in the study of the solar neighborhood. Its mid-infrared capabilities have proven critical to the discovery of the bulk of the coolest (T-eff < 1000 K) brown dwarfs, including the new Y dwarfs, and its all-sky coverage lends itself to searches for high proper motions stars using other infrared surveys such as the Two Micron All Sky Survey (2MASS), UKIRT Infrared Deep Sky Survey (UKIDSS), and Visible and Infrared Survey Telescope for Astronomy (VISTA) surveys. This splinter session of the 17th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun was organized to bring together researchers working with WISE data to both identify brown dwarfs and characterize their properties. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Cushing, M. C.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Kirkpatrick, J. D.; Gelino, C. R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Wright, E. L.; Mace, G. N.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Gizis, J. E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Gomes, J. I.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Leggett, S. K.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Lodieu, N.] IAC, E-38205 Tenerife, Spain. [Dupuy, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cushing, MC (reprint author), Univ Toledo, Dept Phys & Astron, MS 111,2801 W Bancroft St, Toledo, OH 43606 USA. EM michael.cushing@utoledo.edu OI Gizis, John/0000-0002-8916-1972; Leggett, Sandy/0000-0002-3681-2989 FU National Aeronautics and Space Administration FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology; and the NEOWISE extension of WISE, both funded by the National Aeronautics and Space Administration. NR 28 TC 0 Z9 0 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 97 EP 100 DI 10.1002/asna.201211754 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900023 ER PT J AU Poppenhaeger, K Gunther, HM Beiersdorfer, P Brickhouse, NS Carter, JA Hudson, HS Kowalski, A Lalitha, S Miceli, M Wolk, SJ AF Poppenhaeger, K. Guenther, H. M. Beiersdorfer, P. Brickhouse, N. S. Carter, J. A. Hudson, H. S. Kowalski, A. Lalitha, S. Miceli, M. Wolk, S. J. TI Non-thermal processes in coronae and beyond SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE atomic data; methods: laboratory; radiation mechanism: non-thermal; stars: flare; Sun: flares ID ATOMIC DATABASE; EMISSION; CHIANTI; PLASMA; IONS AB This contribution summarizes the splinter session "Non-thermal processes in coronae and beyond" held at the Cool Stars 17 workshop in Barcelona in 2012. It covers new developments in high energy non-thermal effects in the Earth's exosphere, solar and stellar flares, the diffuse emission in star forming regions and reviews the state and the challenges of the underlying atomic databases. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Poppenhaeger, K.; Guenther, H. M.; Brickhouse, N. S.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beiersdorfer, P.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Carter, J. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Hudson, H. S.] Univ Calif Berkeley, SSL, Berkeley, CA USA. [Kowalski, A.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Lalitha, S.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Miceli, M.] Univ Palermo, Dipartimento Fis, I-90134 Palermo, Italy. RP Poppenhaeger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kpoppenhaeger@cfa.harvard.edu OI Poppenhaeger, Katja/0000-0003-1231-2194; Gunther, Hans Moritz/0000-0003-4243-2840; Brickhouse, Nancy/0000-0002-8704-4473; Miceli, Marco/0000-0003-0876-8391; Wolk, Scott/0000-0002-0826-9261 NR 19 TC 0 Z9 0 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 101 EP 104 DI 10.1002/asna.201211755 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900024 ER PT J AU Wright, NJ Drake, JJ Mamajek, EE Henry, GW AF Wright, N. J. Drake, J. J. Mamajek, E. E. Henry, G. W. TI The stellar activity-rotation relationship SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars: activity; stars: coronae; stars: late-type; stars: magnetic fields; stars: rotation; X-rays: stars ID X-RAY-EMISSION; MAIN-SEQUENCE STARS; SUPERSATURATION; DEPENDENCE; CONVECTION; EVOLUTION; EINSTEIN; DWARFS AB Using a new catalog of 824 solar and late-type stars with measured X-ray luminosities and rotation periods we have studied the relationship between rotation and stellar activity that is believed to be a probe of the underlying stellar dynamo. Using an unbiased subset of the sample we calculate the power law slope of the unsaturated regime of the activity-rotation relationship as L-X/L-bol proportional to Ro(beta), where beta = -2.70 +/- 0.13. Notably this is inconsistent with the canonical beta = -2 slope to a confidence of 5 sigma are argues for an interface-type dynamo. Super-saturation is observed for the fastest rotators in our sample and its parametric dependencies are explored. Significant correlations are found with both the corotation radius and the excess polar updraft, the latter theory being preferred as it is supported by other observations. We also present a new X-ray population synthesis model of the mature stellar component of our Galaxy and use it to reproduce deep observations of a high Galactic latitude field. The model, XStar, can be used to test models of stellar spin-down and dynamo decay, as well as for estimating stellar X-ray contamination rates for non-stellar studies. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Wright, N. J.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Henry, G. W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nwright@cfa.harvard.edu NR 21 TC 4 Z9 4 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 151 EP 154 DI 10.1002/asna.201211764 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900035 ER PT J AU Rojas-Ayala, B Hilton, EJ Mann, AW Lepine, S Gaidos, E Bonfils, X Helling, C Henry, TJ Rogers, LA von Braun, K Youdin, A AF Rojas-Ayala, B. Hilton, E. J. Mann, A. W. Lepine, S. Gaidos, E. Bonfils, X. Helling, Ch Henry, T. J. Rogers, L. A. von Braun, K. Youdin, A. TI M dwarf stars in the light of (future) exoplanet searches SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE stars: planetary systems; stars: late-type; stars: fundamental parameters ID EXTRASOLAR GIANT PLANETS; DISK TURBULENCE DRIVEN; LOW-MASS STARS; BROWN DWARFS; GRAVITATIONAL-INSTABILITY; ASTROPHYSICAL PARAMETERS; PLANETESIMAL FORMATION; STREAMING INSTABILITY; PHYSICAL-PROPERTIES; MODEL ATMOSPHERES AB We present a brief overview of a splinter session on M dwarf stars as planet hosts that was organized as part of the Cool Stars 17 conference. The session was devoted to reviewing our current knowledge of M dwarf stars and exoplanets in order to prepare for current and future exoplanet searches focusing in low mass stars. We review the observational and theoretical challenges to characterize M dwarf stars and the importance of accurate fundamental parameters for the proper characterization of their exoplanets and our understanding on planet formation. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Rojas-Ayala, B.; Lepine, S.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Hilton, E. J.; Mann, A. W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hilton, E. J.; Gaidos, E.] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Bonfils, X.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Helling, Ch] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Henry, T. J.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Rogers, L. A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [von Braun, K.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Youdin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rojas-Ayala, B (reprint author), Amer Museum Nat Hist, Dept Astrophys, Cent Pk West & 79th St, New York, NY 10024 USA. EM babs@amnh.org RI Rojas-Ayala, Barbara/G-4382-2015; OI Rojas-Ayala, Barbara/0000-0002-0149-1302; Youdin, Andrew/0000-0002-3644-8726; Bonfils, Xavier/0000-0001-9003-8894 FU European Community; ERC; NASA Astrobiology Institute FX The authors thank the CS17 SOC for the opportunity to hold this productive splinter session and the anonymous referee for her/his constructive comments. ChH highlights financial support of the European Community under the FP7 by an ERC starting grant. BR gratefully acknowledges the CS17 Early Career Travel Grant provided by the NASA Astrobiology Institute. NR 62 TC 3 Z9 3 U1 0 U2 6 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 155 EP 158 DI 10.1002/asna.201211760 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900036 ER PT J AU Meibom, S Barnes, SA Covey, K Jeffries, RD Matt, S Morin, J Palacios, A Reiners, A Sicilia-Aguilar, A Irwin, J AF Meibom, S. Barnes, S. A. Covey, K. Jeffries, R. D. Matt, S. Morin, J. Palacios, A. Reiners, A. Sicilia-Aguilar, A. Irwin, J. TI Angular momentum evolution of cool stars: Toward a synthesis of observations and theory before and after the ZAMS SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE circumstellar matter; stars: late-type; stars: magnetic fields; stars: pre-main sequence; stars: rotation ID LOW-MASS STARS; PRE-MAIN-SEQUENCE; STELLAR ROTATION; PROTOPLANETARY DISKS; YOUNG CLUSTERS; ACCRETION; DYNAMOS; GYROCHRONOLOGY; DIAGRAMS; DWARFS AB The coexistence of fast and slowly rotating cool stars in ZAMS clusters - forming distinct sequences in the color vs. rotation period plane - is providing clues to differences in their pre main-sequence angular momentum evolution. This Cool Stars 17 splinter was dedicated to a discussion of new observational and theoretical results that may help discriminate between proposed mechanisms for early angular momentum regulation and help us explain the observed ZAMS dichotomy. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Meibom, S.; Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnes, S. A.] Space Sci Inst, Boulder, CO USA. [Barnes, S. A.] Univ Potsdam, Potsdam, Germany. [Barnes, S. A.] Leibniz Inst Astrophys Potsdam, Potsdam, Germany. [Covey, K.] Lowell Observ, Flagstaff, AZ 86001 USA. [Jeffries, R. D.] Keele Univ, Keele, Staffs, England. [Matt, S.] Univ Paris Diderot, CNRS INSU, CEA Irfu, Lab AIM Paris Saclay, Paris, France. [Morin, J.; Reiners, A.] Univ Gottingen, Inst Astrophys, Gottingen, Germany. [Palacios, A.] Lab Univers & Particules Montpellier, Montpellier, France. [Sicilia-Aguilar, A.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu OI Morin, Julien/0000-0002-4996-6901; Covey, Kevin/0000-0001-6914-7797; Matt, Sean/0000-0001-9590-2274 NR 28 TC 4 Z9 4 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 168 EP 171 DI 10.1002/asna.201211777 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900039 ER PT J AU Rodler, F Kurster, M Lopez-Morales, M Ribas, I AF Rodler, F. Kuerster, M. Lopez-Morales, M. Ribas, I. TI The return of the mummy: Evidence for starlight reflected from the massive hot Jupiter tau Boo b? SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE planetary systems; stars: individual (tau Boo); techniques: radial velocities ID EXTRASOLAR GIANT PLANETS; SUN-LIKE STARS; SECONDARY ECLIPSE; UPPER LIMIT; LOW-ALBEDO; SPECTRA; CONSTRAINTS; ATMOSPHERES; EXOPLANETS; COROT-1B AB Very recently, we were able to measure CO absorption features in the atmosphere of the non-transiting planet tau Boo b for the very first time. This allowed us to unravel a long-term mystery in planet atmosphere studies, the determination of the orbital inclination of a non-transiting planet and the exact planetary mass, respectively being 46 degrees and 5.7 M-Jup. In light of these new results, we reanalyzed a UVES/VLT data set taken by us with the goal to detect starlight reflected from this hot Jupiter. In the previous analysis of these data, we found a candidate signal of low confidence (2 sigma), indicating a geometric albedo of the planetary atmosphere lower than 0.4 and an orbital inclination of 41 degrees, which is close to the recently measured value. We reanalyzed these data by adopting updated orbital parameters and find as result that the candidate signal of marginal significance now appears at an orbital inclination of 43 degrees. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 [Rodler, F.; Lopez-Morales, M.; Ribas, I.] Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Bellaterra 08193, Spain. [Kuerster, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodler, F (reprint author), Fac Ciencies, Inst Ciencies Espai CSIC IEEC, Campus UAB,Torre C5 Parell,2A Planta, Bellaterra 08193, Spain. EM rodler@ice.cat RI Ribas, Ignasi/M-2134-2014 OI Ribas, Ignasi/0000-0002-6689-0312 FU ESO Telescopes at the Paranal Observatory [079.C-0413]; NSF [AST-0908278] FX Based on observations made with ESO Telescopes at the Paranal Observatory under programme 079.C-0413 (A). This work has been partially supported by NSF's grant AST-0908278. FR is grateful to Friederike Elias und Stefan Walther for the hospitality in Heidelberg, where the first draft of the manuscript was written. NR 34 TC 4 Z9 4 U1 0 U2 3 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD FEB PY 2013 VL 334 IS 1-2 SI SI BP 188 EP 191 DI 10.1002/asna.201211744 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237HO UT WOS:000325859900044 ER PT J AU Marhold, K Stuessy, T Agababian, M Agosti, D Alford, MH Crespo, A Crisci, JV Dorr, LJ Ferencova, Z Frodin, D Geltman, DV Kilian, N Linder, HP Lohmann, LG Oberprieler, C Penev, L Smith, GF Thomas, W Tulig, M Turland, N Zhang, XC AF Marhold, Karol Stuessy, Tod Agababian, Mariam Agosti, Donat Alford, Mac H. Crespo, Ana Crisci, Jorge V. Dorr, Laurence J. Ferencova, Zuzana Frodin, David Geltman, Dmitry V. Kilian, Norbert Linder, H. Peter Lohmann, Lucia G. Oberprieler, Christoph Penev, Lyubomir Smith, Gideon F. Thomas, Wayt Tulig, Melissa Turland, Nicholas Zhang, Xian-Chun TI The Future of Botanical Monography: Report from an international workshop, 12-16 March 2012, Smolenice, Slovak Republic SO TAXON LA English DT Article DE classification; internet; monograph; nomenclature; phylogeny; revision; synopsis ID SPECIES IDENTIFICATION; DNA BARCODES; TAXONOMY; BIODIVERSITY; KNOWLEDGE; HERBARIA; DISCOVERY; SCIENCE; ACCESS; CRISIS AB Monographs are fundamental for progress in systematic botany. They are the vehicles for circumscribing and naming taxa, determining distributions and ecology, assessing relationships for formal classification, and interpreting long-term and short-term dimensions of the evolutionary process. Despite their importance, fewer monographs are now being prepared by the newer generation of systematic botanists, who are understandably involved principally with DNA data and analysis, especially for answering phylogenetic, biogeographic, and population genetic questions. As monographs provide hypotheses regarding species boundaries and plant relationships, new insights in many plant groups are urgently needed. Increasing pressures on biodiversity, especially in tropical and developing regions of the world, emphasize this point. The results from a workshop (with 21 participants) reaffirm the central role that monographs play in systematic botany. But, rather than advocating abbreviated models for monographic products, we recommend a full presentation of relevant information. Electronic publication offers numerous means of illustration of taxa, habitats, characters, and statistical and phylogenetic analyses, which previously would have been prohibitively costly. Open Access and semantically enhanced linked electronic publications provide instant access to content from anywhere in the world, and at the same time link this content to all underlying data and digital resources used in the work. Resources in support of monography, especially databases and widely and easily accessible digital literature and specimens, are now more powerful than ever before, but interfacing and interoperability of databases are much needed. Priorities for new resources to be developed include an index of type collections and an online global chromosome database. Funding for sabbaticals for monographers to work uninterrupted on major projects is strongly encouraged. We recommend that doctoral students be assigned smaller genera, or natural portions of larger ones (subgenera, sections, etc.), to gain the necessary expertise for producing a monograph, including training in a broad array of data collection (e.g., morphology, anatomy, palynology, cytogenetics, DNA techniques, ecology, biogeography), data analysis (e.g., statistics, phylogenetics, models), and nomenclature. Training programs, supported by institutes, associations, and agencies, provide means for passing on procedures and perspectives of challenging botanical monography to the next generation of young systematists. C1 [Marhold, Karol] Slovak Acad Sci, Inst Bot, Bratislava 84523, Slovakia. [Marhold, Karol] Charles Univ Prague, Fac Sci, Dept Bot, Prague 12801 2, Czech Republic. [Stuessy, Tod] Univ Vienna, Biodivers Ctr, Dept Systemat & Evolutionary Bot, A-1030 Vienna, Austria. [Marhold, Karol] Acad Sci, Inst Bot, Yerevan, Armenia. [Agosti, Donat] Plazi, CH-3007 Bern, Switzerland. [Alford, Mac H.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Crespo, Ana; Ferencova, Zuzana] Univ Complutense Madrid, Fac Farm, Dept Biol Vegetal 2, Madrid 28040, Spain. [Crisci, Jorge V.] Museo La Plata, Div Plantas Vasc, La Plata, Argentina. [Dorr, Laurence J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Frodin, David] Royal Bot Gardens, Herbarium, Richmond, Surrey, England. [Geltman, Dmitry V.] Russian Acad Sci, VL Komarov Bot Inst, St Petersburg 197376, Russia. [Kilian, Norbert] Free Univ Berlin, Bot Garten & Botan Museum Berlin Dahlem, D-14195 Berlin, Germany. [Linder, H. Peter] Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland. [Lohmann, Lucia G.] Univ Sao Paulo, Inst Biociencias, Dept Bot, BR-05508090 Sao Paulo, Brazil. [Oberprieler, Christoph] Univ Regensburg, Inst Bot, D-93053 Regensburg, Germany. [Penev, Lyubomir] Bulgarian Acad Sci & Pensoft Publishers, Inst Biodivers & Ecosyst Res, Sofia 1111, Bulgaria. [Smith, Gideon F.] South African Natl Biodivers Inst, Biosystemat Res & Biodivers Collect, ZA-001 Pretoria, South Africa. [Smith, Gideon F.] Univ Pretoria, Dept Bot, Schweickerdt Herbarium, ZA-0002 Pretoria, South Africa. [Smith, Gideon F.] Univ Coimbra, Dept Ciencias Vida, Ctr Funct Ecol, P-3001455 Coimbra, Portugal. [Thomas, Wayt; Tulig, Melissa] New York Bot Garden, Bronx, NY 10458 USA. [Tulig, Melissa] JSTOR, Bronx, NY 10458 USA. [Turland, Nicholas] Missouri Bot Garden, St Louis, MO 63166 USA. [Zhang, Xian-Chun] Chinese Acad Sci, Inst Bot, Beijing 100093, Peoples R China. RP Marhold, K (reprint author), Slovak Acad Sci, Inst Bot, Dubravskci Cesta 9, Bratislava 84523, Slovakia. EM karol.marhold@savba.sk RI Crespo, Ana/N-6236-2014; Marhold, Karol/B-4699-2011; Linder, Hans Peter/F-5316-2010 OI Crespo, Ana/0000-0002-5271-0157; Marhold, Karol/0000-0002-7658-0844; FU Andrew W. Mellon Foundation; International Association for Plant Taxonomy (IAPT) FX Appreciation is expressed to: the Andrew W. Mellon Foundation for financial support that allowed the workshop to be convened; the International Association for Plant Taxonomy (IAPT) for additional financial support for the workshop; the Slovak Academy of Sciences for facilitating use of Smolenice Castle for the meeting; Eva Senkova, Managing Secretary of IAPT for organizing the logistical aspects of the conference; Franz Stadler, production editor of Taxon, for critically reading Part Three; and all participants who took time from their busy schedules to focus on an important challenge in systematic botany. NR 79 TC 8 Z9 13 U1 2 U2 19 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD FEB PY 2013 VL 62 IS 1 BP 4 EP 20 PG 17 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 196CL UT WOS:000322750900002 ER PT J AU White, RB AF White, Roger B. TI 'An Exposition of Our Own': Corporate Identity, Consumer Advertising and Atlantic City's National Exhibits, 1898-1968 SO JOURNAL OF DESIGN HISTORY LA English DT Article DE 1920s; advertising; architecture; consumers; corporate identity; exhibitions AB This paper focuses on permanent displays of leading American manufacturers at the National Exhibits in Atlantic City, New Jersey, a major tourist resort on the east coast of the United States. Beginning in 1898, these displays expanded on corporate use of world's fair exhibits as advertising. Exhibits relocated from world's fairs to Atlantic City gradually were supplemented by original presentations. By the 1920s, the National Exhibits reflected a shift from celebrations of technological progress and corporate self-importance to public relations spectacles that promoted consumer products and the consumer lifestyle. Drawn by the millions of tourists who visited Atlantic City's famous Boardwalk each year, corporations in the 1920s spent lavishly on their Atlantic City projects. Working with architects and advertising professionals, corporations expressed their identities through individual pavilions and seductive showrooms that immersed visitors in the personal benefits and aesthetic allure of automobiles, appliances, bathroom fixtures and other consumer durables. The National Exhibits were important precursors to corporate displays at US-based world's fairs of the 1930s, where corporations demanded individual pavilions to convey their messages of economic redemption through applied science, technology and consumerism. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP White, RB (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. EM whiter@si.edu NR 82 TC 0 Z9 0 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0952-4649 J9 J DES HIST JI J. Des. Hist. PD FEB PY 2013 VL 26 IS 1 BP 47 EP 64 DI 10.1093/jdh/eps048 PG 18 WC Art SC Art GA 163XG UT WOS:000320371000003 ER PT J AU Small-Lorenz, SL Culp, LA Ryder, TB Will, TC Marra, PP AF Small-Lorenz, Stacy L. Culp, Leah A. Ryder, T. Brandt Will, Tom C. Marra, Peter P. TI A blind spot in climate change vulnerability assessments SO NATURE CLIMATE CHANGE LA English DT Editorial Material C1 [Small-Lorenz, Stacy L.] Environm Def Fund, Washington, DC 20009 USA. [Culp, Leah A.; Ryder, T. Brandt; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Will, Tom C.] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN 55437 USA. RP Small-Lorenz, SL (reprint author), Environm Def Fund, 1875 Connecticut Ave NW,Suite 600, Washington, DC 20009 USA. EM ssmall@edf.org NR 20 TC 31 Z9 31 U1 2 U2 41 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1758-678X J9 NAT CLIM CHANGE JI Nat. Clim. Chang. PD FEB PY 2013 VL 3 IS 2 BP 91 EP 93 PG 3 WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 150NK UT WOS:000319397500003 ER PT J AU Floyd, DJE Dunlop, JS Kukula, MJ Brown, MJI McLure, RJ Baum, SA O'Dea, CP AF Floyd, David J. E. Dunlop, James S. Kukula, Marek J. Brown, Michael J. I. McLure, Ross J. Baum, Stefi A. O'Dea, Christopher P. TI Star formation in luminous quasar host galaxies at z=1-2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: fundamental parameters; galaxies: high redshift; quasars: general ID ACTIVE GALACTIC NUCLEI; RADIO-QUIET QUASARS; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; INITIAL MASS FUNCTION; QSO REDSHIFT SURVEY; BLACK-HOLE; X-RAY; OPTICAL SPECTROSCOPY AB We present deep Hubble Space Telescope (HST)/Wide-Field Planetary Camera 2 (WFPC2), rest-frame U images of 17 similar to L* quasars at z approximate to 1 and 2 (V and I bands, respectively), designed to explore the host galaxies. We fit the images with simple axisymmetric galaxy models, including a point source, in order to separate nuclear and host-galaxy emission. We successfully model all of the host galaxies, with luminosities stable to within 0.3 mag. Combining with our earlier Near Infrared Camera and Multi-Object Spectrometer rest-frame optical study of the same sample, we provide the first rest-frame U - V colours for a sample of quasar host galaxies. While the optical luminosities of their host galaxies indicate that they are drawn purely from the most massive (greater than or similar to L*) early-type galaxy population, their colours are systematically bluer than those of comparably massive galaxies at the same redshift. The host galaxies of the radio-loud quasars (RLQs) in our sample are more luminous than their radio-quiet quasar (RQQ) counterparts at each epoch, but have indistinguishable colours, confirming that the RLQs are drawn from only the most massive galaxies (10(11)-10(12) M-circle dot even at z approximate to 2), while the RQQs are slightly less massive (similar to 10(11) M-circle dot). This is consistent with the well-known anticorrelation between radio-loudness and accretion rate. Using simple stellar population 'frosting' models, we estimate mean star formation rates of similar to 350 M-circle dot yr(-1) for the RLQs and similar to 100 M-circle dot yr(-1) for the RQQs at z approximate to 2. By z approximate to 1, these rates have fallen to similar to 150 M-circle dot yr(-1) for the RLQs and similar to 50 M-circle dot yr(-1) for the RQQs. We conclude that while the host galaxies are extremely massive, they remain actively star forming at, or close to, the epoch of the quasar. C1 [Floyd, David J. E.; Brown, Michael J. I.] Monash Univ, MoCA, Sch Phys, Clayton, Vic 3800, Australia. [Dunlop, James S.; McLure, Ross J.] Univ Edinburgh, Royal Observ, Sch Phys, Inst Astron,SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kukula, Marek J.] Royal Museums Greenwich, Royal Observ Greenwich, London SE10 9NF, England. [Baum, Stefi A.] Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, Stefi A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [O'Dea, Christopher P.] Dept Phys, Rochester, NY 14623 USA. [O'Dea, Christopher P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Floyd, DJE (reprint author), Monash Univ, MoCA, Sch Phys, Clayton, Vic 3800, Australia. EM david.floyd@monash.edu FU Australian Research Council [DP110102174]; Royal Society; European Research Council; Radcliffe Institute for Advanced Study at Harvard University; NASA/ESA Hubble Space Telescope [9085, 7447]; NASA [NAS5-26555] FX We thank the referee, Knud Jahnke, for his helpful critique of the paper, and in particular his suggestion to address the dependence of radio-loudness on accretion rate. DJEF and MJIB acknowledge support from the Australian Research Council via Discovery Project grant DP110102174. JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award, and also the support of the European Research Council via the award of an Advanced Grant. RJM acknowledges the support of the Royal Society via a University Research Fellowship. SAB acknowledges support from the Radcliffe Institute for Advanced Study at Harvard University. Based on observations with the NASA/ESA Hubble Space Telescope, (programme IDs 9085 and 7447) obtained at the Space Telescope Science Institute, which is operated by The Association of Universities for Research in Astronomy, Inc. under NASA contract No. NAS5-26555. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We wish to thank Peter Capak, Olivier Ilbert and the COSMOS team for access to their unpublished H-band catalogue and Victoria Bruce for her CANDELS galaxy scalelength data. DJEF would like to thank Ned Taylor, Chiara Tonini, Barry Rothberg and Darren Croton for helpful discussions and insights throughout the development of this work. NR 73 TC 19 Z9 19 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 2 EP 19 DI 10.1093/mnras/sts291 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300024 ER PT J AU Parejko, JK Sunayama, T Padmanabhan, N Wake, DA Berlind, AA Bizyaev, D Blanton, M Bolton, AS van den Bosch, F Brinkmann, J Brownstein, JR da Costa, LAN Eisenstein, DJ Guo, H Kazin, E Maia, M Malanushenko, E Maraston, C McBride, CK Nichol, RC Oravetz, DJ Pan, KK Percival, WJ Prada, F Ross, AJ Ross, NP Schlegel, DJ Schneider, D Simmons, AE Skibba, R Tinker, J Tojeiro, R Weaver, BA Wetzel, A White, M Weinberg, DH Thomas, D Zehavi, I Zheng, Z AF Parejko, John K. Sunayama, Tomomi Padmanabhan, Nikhil Wake, David A. Berlind, Andreas A. Bizyaev, Dmitry Blanton, Michael Bolton, Adam S. van den Bosch, Frank Brinkmann, Jon Brownstein, Joel R. Nicolaci da Costa, Luiz Alberto Eisenstein, Daniel J. Guo, Hong Kazin, Eyal Maia, Marcio Malanushenko, Elena Maraston, Claudia McBride, Cameron K. Nichol, Robert C. Oravetz, Daniel J. Pan, Kaike Percival, Will J. Prada, Francisco Ross, Ashley J. Ross, Nicholas P. Schlegel, David J. Schneider, Don Simmons, Audrey E. Skibba, Ramin Tinker, Jeremy Tojeiro, Rita Weaver, Benjamin A. Wetzel, Andrew White, Martin Weinberg, David H. Thomas, Daniel Zehavi, Idit Zheng, Zheng TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: the low-redshift sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE large-scale structure of Universe; galaxies: haloes; galaxies: evolution; galaxies: statistics; surveys ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; HALO OCCUPATION DISTRIBUTION; LARGE-SCALE STRUCTURE; PROBE WMAP OBSERVATIONS; COLD DARK-MATTER; REAL-SPACE; NUMERICAL SIMULATIONS; TARGET SELECTION; STELLAR SPECTRA AB We report on the small-scale (0.5 < r < 40 h(-1) Mpc) clustering of 78 895 massive (M-* similar to 10(11.3) M-circle dot) galaxies at 0.2 < z < 0.4 from the first two years of data from the Baryon Oscillation Spectroscopic Survey (BOSS), to be released as part of Sloan Digital Sky Survey (SDSS) Data Release 9 (DR9). We describe the sample selection, basic properties of the galaxies and caveats for working with the data. We calculate the real-and redshift-space two-point correlation functions of these galaxies, fit these measurements using halo occupation distribution (HOD) modelling within dark matter cosmological simulations, and estimate the errors using mock catalogues. These galaxies lie in massive haloes, with a mean halo mass of 5.2 x 10(13) h(-1) M-circle dot, a large-scale bias of similar to 2.0 and a satellite fraction of 12 +/- 2 per cent. Thus, these galaxies occupy haloes with average masses in between those of the higher redshift BOSS CMASS sample and the original SDSS I/II luminous red galaxy sample. C1 [Parejko, John K.; Sunayama, Tomomi; Padmanabhan, Nikhil; Wake, David A.; van den Bosch, Frank; Wetzel, Andrew] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Bizyaev, Dmitry; Brinkmann, Jon; Malanushenko, Elena; Oravetz, Daniel J.; Pan, Kaike; Simmons, Audrey E.] Apache Point Observ, Sunspot, NM 88349 USA. [Blanton, Michael; Tinker, Jeremy; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bolton, Adam S.; Brownstein, Joel R.; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Nicolaci da Costa, Luiz Alberto; Maia, Marcio] Observ Nacl, BR-20921400 Br Rio De Janeiro, RJ, Brazil. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Kazin, Eyal] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Maraston, Claudia; Nichol, Robert C.; Percival, Will J.; Ross, Ashley J.; Tojeiro, Rita; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor, CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Schneider, Don] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Skibba, Ramin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. RP Parejko, JK (reprint author), Yale Univ, Dept Phys, 260 Whitney Ave, New Haven, CT 06520 USA. EM john.parejko@yale.edu RI da Costa, Luiz Alberto/I-1326-2013; Guo, Hong/J-5797-2015; White, Martin/I-3880-2015; OI da Costa, Luiz Alberto/0000-0002-7731-277X; Guo, Hong/0000-0003-4936-8247; White, Martin/0000-0001-9912-5070; Wetzel, Andrew/0000-0003-0603-8942 FU Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University.; This work was supported in part by the facilities and staff of the Yale University Faculty of Arts and Sciences High Performance Computing Center, the National Energy Research Scientific Computing Center, the Shared Research Computing Services Pilot of the University of California and the Laboratory Research Computing project at Lawrence Berkeley Laboratory. NR 90 TC 36 Z9 36 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 98 EP 112 DI 10.1093/mnras/sts314 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300030 ER PT J AU Leonidaki, I Boumis, P Zezas, A AF Leonidaki, I. Boumis, P. Zezas, A. TI A multiwavelength study of supernova remnants in six nearby galaxies - II. New optically selected supernova remnants SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: supernova remnants; galaxies: star formation ID LARGE-MAGELLANIC-CLOUD; DWARF STARBURST GALAXY; X-RAY; SPIRAL GALAXIES; IRREGULAR GALAXIES; STAR-FORMATION; SHOCK-MODELS; IONIZED-GAS; EMISSION; CHANDRA AB We present results from a study of optically emitting supernova remnants (SNRs) in six nearby galaxies (NGC 2403, 3077, 4214, 4395, 4449 and 5204) based on deep narrow-band H alpha and [S II] images as well as spectroscopic observations. The SNR classification was based on the detected sources that fulfil the well-established emission-line flux criterion of [S II]/H alpha > 0.4. This study revealed similar to 400 photometric SNRs down to a limiting H alpha flux of 10(-15) erg s(-1) cm(-2). Spectroscopic observations confirmed the shock-excited nature of 56 out of the 96 sources with ([S II]/H alpha)(phot) > 0.3 (our limit for an SNR classification) for which we obtained spectra. 11 more sources were spectroscopically identified as SNRs although their photometric [S II]/H alpha ratio was below 0.3. We discuss the properties of the optically detected SNRs in our sample for different types of galaxies and hence different environments, in order to address their connection with the surrounding interstellar medium. We find that there is a difference in [N II]/H alpha line ratios of the SNR populations between different types of galaxies which indicates that this happens due to metallicity. We cross-correlate parameters of the optically detected SNRs ([S II]/H alpha ratio, luminosity) with parameters of coincident X- ray-emitting SNRs, resulted from our previous studies on the same sample of galaxies, in order to understand their evolution and investigate possible selection effects. We do not find a correlation between their H alpha and X-ray luminosities, which we attribute to the presence of material in a wide range of temperatures. We also find evidence for a linear relation between the number of luminous optical SNRs (10(37) erg s(-1)) and star formation rate in our sample of galaxies. C1 [Leonidaki, I.; Boumis, P.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Athens, Greece. [Leonidaki, I.] Univ Patras, Astron Lab, Dept Phys, GR-26500 Rio Patra, Greece. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Crete, Greece. RP Leonidaki, I (reprint author), Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, 1 Metaxa & Vas Pavlou St, GR-15236 Athens, Greece. EM ptb@astro.noa.gr RI Boumis, Panos/K-4653-2013; LEONIDAKI, IOANNA/K-4351-2013; Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X FU NASA [GO6-7086X]; NASA LTSA [G5-13056]; EU IRG [224878]; EU [206469] FX The authors would like to thank the referee John Danziger for providing constructive comments that have improved the clarity of this manuscript. We also thank M. Allen for the fruitful discussion and for providing us with different plots on the Mapping III shock model. This programme has been supported by NASA grant GO6-7086X and NASA LTSA grant G5-13056. AZ acknowledges support by the EU IRG grant 224878. Space Astrophysics at the University of Crete is supported by EU FP7-REGPOT grant 206469 (ASTROSPACE). The Skinakas Observatory is a collaborative project of the University of Crete, the Foundation for Research and Technology-Hellas and the Max Planck Institute. The Kitt Peak National Observatory, National Optical Astronomy Observatory, is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation. NR 70 TC 8 Z9 8 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 189 EP 220 DI 10.1093/mnras/sts324 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300039 ER PT J AU Curtis-Lake, E McLure, RJ Dunlop, JS Schenker, M Rogers, AB Targett, T Cirasuolo, M Almaini, O Ashby, MLN Bradshaw, EJ Finkelstein, SL Dickinson, M Ellis, RS Faber, SM Fazio, GG Ferguson, HC Fontana, A Grogin, NA Hartley, WG Kocevski, DD Koekemoer, AM Lai, K Robertson, BE Vanzella, E Willner, SP AF Curtis-Lake, E. McLure, R. J. Dunlop, J. S. Schenker, M. Rogers, A. B. Targett, T. Cirasuolo, M. Almaini, O. Ashby, M. L. N. Bradshaw, E. J. Finkelstein, S. L. Dickinson, M. Ellis, R. S. Faber, S. M. Fazio, G. G. Ferguson, H. C. Fontana, A. Grogin, N. A. Hartley, W. G. Kocevski, D. D. Koekemoer, A. M. Lai, K. Robertson, B. E. Vanzella, E. Willner, S. P. TI The ages, masses and star formation rates of spectroscopically confirmed z similar to 6 galaxies in CANDELS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID LYMAN-BREAK GALAXIES; LY-ALPHA EMITTERS; HIGH-REDSHIFT GALAXIES; EXTRAGALACTIC LEGACY SURVEY; SPITZER-SPACE-TELESCOPE; I'-DROP GALAXIES; ULTRA-DEEP-FIELD; STELLAR POPULATIONS; FORMATION HISTORIES; REIONIZATION EPOCH AB We report the results of a study exploring the stellar populations of 13 luminous (L > 1.2L*), spectroscopically confirmed, galaxies in the redshift interval 5.5 < z < 6.5, all with Hubble Space Telescope (HST) Wide Field Camera 3/infrared and Spitzer Infrared Array Camera imaging from the HST/Cosmic Assembly Near-infrared Deep Survey and Spitzer Extended Deep Survey. Based on fitting the observed photometry with galaxy spectral energy distribution (SED) templates covering a wide range of different star formation histories, including exponentially increasing star formation rates and a self-consistent treatment of Ly alpha emission, we find that the derived stellar masses lie within the range of 10(9) < M-* < 10(10) M-circle dot and are robust to within a factor of 2. In contrast, we confirm previous reports that the ages of the stellar populations are poorly constrained. Although the best-fitting models for 3/13 of the sample have ages of greater than or similar to 300 Myr, the degeneracies introduced by dust extinction mean that only two of these objects actually require a greater than or similar to 300 Myr old stellar population to reproduce the observed photometry. We also explore SED fitting with more general, two-component models (burst plus ongoing star formation), thereby relaxing the requirement that the current star formation rate and assembled stellar mass must be coupled, and allow for nebular line+continuum emission. On average, the inclusion of nebular emission leads to lower stellar mass estimates (median offset 0.18 dex), moderately higher specific star formation rates, and allows for a wider range of plausible stellar ages. However, based on our SED modelling, we find no strong evidence for extremely young ages in our sample (i.e. < 50 Myr). Finally, considering all of the different star formation histories explored, we find that the median best-fitting ages are of the order of similar or equal to 200-300 Myr and that the objects with the tightest constraints indicate ages in the range of 50-200 Myr. C1 [Curtis-Lake, E.; McLure, R. J.; Dunlop, J. S.; Rogers, A. B.; Targett, T.; Cirasuolo, M.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Schenker, M.; Ellis, R. S.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Almaini, O.; Bradshaw, E. J.; Hartley, W. G.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Ashby, M. L. N.; Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Finkelstein, S. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Faber, S. M.; Kocevski, D. D.; Lai, K.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Ferguson, H. C.; Grogin, N. A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fontana, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Robertson, B. E.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Vanzella, E.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. RP Curtis-Lake, E (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. EM efcl@roe.ac.uk OI Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 FU UK Science and Technology Facilities Council (STFC); Leverhulme Trust; Royal Society; European Research Council; STFC; STFC PD RA; NASA [NAS5-26555] FX First we would like to thank the anonymous referee who helped to improve this manuscript. EC-L would like to acknowledge financial support from the UK Science and Technology Facilities Council (STFC) and the Leverhulme Trust. RJM would like to acknowledge the funding of the Royal Society via the award of a University Research Fellowship and the Leverhulme Trust via the award of a Philip Leverhulme research prize. JSD acknowledges the support of the Royal Society via a Wolfson Research Merit award, and also the support of the European Research Council via the award of an Advanced Grant. MC acknowledges the award of an STFC Advanced Fellowship. ABR, and EJB acknowledge the award of STFC PhD studentships. WGH acknowledges the award of an STFC PD RA. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based (in part) on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 62 TC 32 Z9 32 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 302 EP 322 DI 10.1093/mnras/sts338 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300047 ER PT J AU Oguri, M Schrabback, T Jullo, E Ota, N Kochanek, CS Dai, XY Ofek, EO Richards, GT Blandford, RD Falco, EE Fohlmeister, J AF Oguri, Masamune Schrabback, Tim Jullo, Eric Ota, Naomi Kochanek, Christopher S. Dai, Xinyu Ofek, Eran O. Richards, Gordon T. Blandford, Roger D. Falco, Emilio E. Fohlmeister, Janine TI The Hidden Fortress: structure and substructure of the complex strong lensing cluster SDSS J1029+2623 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; gravitational lensing: weak; galaxies: clusters: individual: SDSS J1029+2623; quasars: individual: SDSS J1029+2623; dark matter; X-rays: galaxies: clusters ID GRAVITATIONALLY LENSED QUASAR; RELAXED GALAXY CLUSTERS; STEEP MASS PROFILE; DARK-MATTER; X-RAY; SCALING RELATIONS; DENSITY PROFILES; MERGING CLUSTERS; BULLET CLUSTER; TIME DELAYS AB We present Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3) observations of SDSS J1029+2623, a three-image quasar lens system produced by a foreground cluster at z = 0.584. Our strong lensing analysis reveals six additional multiply imaged galaxies in addition to the multiply imaged quasar. We confirm the complex nature of the mass distribution of the lensing cluster, with a bimodal dark matter distribution which deviates from the Chandra X-ray surface brightness distribution. The Einstein radius of the lensing cluster is estimated to be theta(E) = 15.2 +/- 0.5 arcsec for the quasar redshift of z = 2.197. We derive a radial mass distribution from the combination of strong lensing, HST/ACS weak lensing and Subaru/Suprime-cam weak lensing analysis results, finding a best-fitting virial mass of M-vir = 1.55(-0.35)(+0.40) x 10(14) h(-1) M-circle dot and a concentration parameter of c(vir) = 25.7(-7.5)(+14.1). The lensing mass estimate at the outer radius is smaller than the X-ray mass estimate by a factor of similar to 2. We ascribe this large mass discrepancy to shock heating of the intracluster gas during a merger, which is also suggested by the complex mass and gas distributions and the high value of the concentration parameter. In the HST image, we also identify a probable galaxy, GX, in the vicinity of the faintest quasar image C. In strong lens models, the inclusion of GX explains the anomalous flux ratios between the quasar images. The morphology of the highly elongated quasar host galaxy is also well reproduced. The best-fitting model suggests large total magnifications of 30 for the quasar and 35 for the quasar host galaxy, and has an AB time delay consistent with the measured value. C1 [Oguri, Masamune] Univ Tokyo, WPI, Kavli IPMU, Chiba 2778583, Japan. [Schrabback, Tim] Argelander Inst Astron, D-53121 Bonn, Germany. [Schrabback, Tim; Blandford, Roger D.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Jullo, Eric] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Ota, Naomi] Nara Womens Univ, Dept Phys, Nara 6308506, Japan. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Dai, Xinyu] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fohlmeister, Janine] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. RP Oguri, M (reprint author), Univ Tokyo, WPI, Kavli IPMU, Chiba 2778583, Japan. EM masamune.oguri@ipmu.jp RI Oguri, Masamune/C-6230-2011; Dai, Xinyu/B-5735-2011 OI Dai, Xinyu/0000-0001-9203-2808 FU FIRST program 'Subaru Measurements of Images and Redshifts (SuMIRe)'; World Premier International Research Center Initiative (WPI Initiative); MEXT, Japan; JSPS [23740161]; NSF [AST-0444059-001, AST-1009756]; Smithsonian Astrophysics Observatory [GO0-11147A]; NASA/SAO [GO011147B]; NASA/STScI [HST-GO-12915.07-A]; NASA [NAS 5-26555] FX We thank an anonymous referee for useful suggestions. This work was supported in part by the FIRST program 'Subaru Measurements of Images and Redshifts (SuMIRe)', World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). TS acknowledges support from NSF through grant AST-0444059-001, and the Smithsonian Astrophysics Observatory through grant GO0-11147A. CSK is supported by NSF grant AST-1009756. XD acknowledges financial support from NASA/SAO award GO011147B and NASA/STScI award HST-GO-12915.07-A. This paper is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, CHIPS and SHERPA. This paper is based on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. NR 71 TC 16 Z9 16 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 482 EP 493 DI 10.1093/mnras/sts351 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300059 ER PT J AU Jonker, PG Torres, MAP Steeghs, D Chakrabarty, D AF Jonker, Peter G. Torres, Manuel A. P. Steeghs, Danny Chakrabarty, Deepto TI Chandra X-ray and Gemini near-infrared observations of the eclipsing millisecond pulsar SWIFT J1749.4-2807 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; X-rays: binaries; X-rays: individual: SWIFT J1749.4-2807 ID NEUTRON-STAR; OPTICAL COUNTERPART; SAX J1808.4-3658; BINARY-SYSTEM; BLACK-HOLE; MASS; DISCOVERY; COMPANION; DONOR AB We report on Chandra X-ray and Gemini-North near-infrared K-band observations of the eclipsing accretion-powered millisecond X-ray pulsar SWIFT J1749.4-2807 in quiescence. Using the Chandra observation we derive a source position of right ascension 17:49:31.73 and declination -28:08:05.08. The position is accurate to 0.6 arcsec (90 per cent confidence). We find one source at a magnitude K = 18.44 +/- 0.03 with a position fully consistent with the accurate Chandra X-ray localization and a second source at K = 19.2 +/- 0.1 that falls close to the edge of the error circle in the deep K-band images. The presence of a few weaker sources as suggested by previous H-band observations presented in the literature cannot be ruled out. There is marginal evidence that the brighter of the these two sources is variable. Follow-up spectroscopy of this potential counterpart will show if this source is the true counterpart to SWIFT J1749.4-2807. If so, baring the presence of complicating effects such as heating of the mass-donor star, it would allow for the mass of the neutron star to be measured through the measurement of periodic radial velocity variations. C1 [Jonker, Peter G.; Torres, Manuel A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter G.; Torres, Manuel A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, Peter G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Steeghs, Danny] Univ Warwick, Dept Phys Astron & Astrophys, Coventry CV4 7AL, W Midlands, England. [Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU VIDI grant from the Netherlands Organization for Scientific Research FX The authors acknowledge the referee for providing useful comments that helped improve the manuscript. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. PGJ acknowledges Theo van Grunsven for discussions on the amplitude of the ellipsoidal variations and for producing Fig. 3. MAPT and PGJ acknowledge Knut Olsen for discussions on the NIRI data reduction. This research has made use of data obtained from the Chandra Source Catalogue, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive (ADS/Sa.CXO#CSC). NR 43 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP 523 EP 528 DI 10.1093/mnras/sts363 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300063 ER PT J AU Beardsley, AP Hazelton, BJ Morales, MF Arcus, W Barnes, D Bernardi, G Bowman, JD Briggs, FH Bunton, JD Cappallo, RJ Corey, BE Deshpande, A deSouza, L Emrich, D Gaensler, BM Goeke, R Greenhill, LJ Herne, D Hewitt, JN Johnston-Hollitt, M Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morgan, E Oberoi, D Ord, SM Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, A Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, J Subrahmanyan, R Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL Wyithe, JSB AF Beardsley, A. P. Hazelton, B. J. Morales, M. F. Arcus, W. Barnes, D. Bernardi, G. Bowman, J. D. Briggs, F. H. Bunton, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. deSouza, L. Emrich, D. Gaensler, B. M. Goeke, R. Greenhill, L. J. Herne, D. Hewitt, J. N. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morgan, E. Oberoi, D. Ord, S. M. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, A. Salah, J. E. Sault, R. J. Shankar, N. Udaya Srivani, K. S. Stevens, J. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wyithe, J. S. B. TI The EoR sensitivity of the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; cosmology: miscellaneous ID POWER SPECTRUM; REIONIZATION OBSERVATORIES; EPOCH; FLUCTUATIONS; COSMOLOGY; DESIGN AB Using the final 128 antenna locations of the Murchison Widefield Array (MWA), we calculate its sensitivity to the epoch of reionization (EoR) power spectrum of redshifted 21 cm emission for a fiducial model and provide the tools to calculate the sensitivity for any model. Our calculation takes into account synthesis rotation, chromatic and asymmetrical baseline effects, and excludes modes that will be contaminated by foreground subtraction. For the fiducial model, the MWA will be capable of a 14 sigma detection of the EoR signal with one full season of observation on two fields (900 and 700 h). C1 [Beardsley, A. P.; Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Arcus, W.; Emrich, D.; Herne, D.; Lynch, M. J.; Tingay, S. J.; Wayth, R. B.; Waterson, M.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Barnes, D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.; Ord, S. M.; Wayth, R. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F. H.; Waterson, M.] Australian Natl Univ, Weston, ACT 2611, Australia. [Briggs, F. H.; Gaensler, B. M.; Mitchell, D. A.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.; Wyithe, J. S. B.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Bunton, J. D.; deSouza, L.; Koenig, R.; Pathikulangara, J.; Stevens, J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Cappallo, R. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Oberoi, D.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A.; Prabu, T.; Roshi, A.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [deSouza, L.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Hewitt, J. N.; Morgan, E.; Remillard, R. A.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6012, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.; Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Stevens, J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Williams, A.] Perth Observ, Bickley, WA 6076, Australia. [Williams, A.] Univ Western Australia, Nedlands, WA 6009, Australia. RP Beardsley, AP (reprint author), Univ Washington, Dept Phys, Seattle, WA 98195 USA. EM mmorales@phys.washington.edu RI Bunton, John/A-4944-2008; Gaensler, Bryan/F-8655-2010; Kasper, Justin/D-1152-2010; Wayth, Randall/B-2444-2013; Williams, Andrew/K-2931-2013; Emrich, David/B-7002-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; Subrahmanyan, Ravi/D-4889-2012; OI Gaensler, Bryan/0000-0002-3382-9558; Kasper, Justin/0000-0002-7077-930X; Wayth, Randall/0000-0002-6995-4131; Williams, Andrew/0000-0001-9080-0105; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Wyithe, Stuart/0000-0001-7956-9758 FU US National Science Foundation [AST CAREER-0847753, AST-0457585, AST-0908884, PHY-0835713]; Australian Research Council [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE11E0001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Australian Federal government via the National Collaborative Research Infrastructure Strategy and Astronomy Australia Limited; iVEC Petabyte Data Store; Initiative in Innovative Computing; NVIDIA; International Centre for Radio Astronomy Research; Joint Venture of Curtin University of Technology; University of Western Australia; Western Australian State government FX Support came from the US National Science Foundation (grants AST CAREER-0847753, AST-0457585, AST-0908884 and PHY-0835713), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE11E0001020), the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, the Australian Federal government via the National Collaborative Research Infrastructure Strategy and Astronomy Australia Limited, under contract to Curtin University of Technology, the iVEC Petabyte Data Store, the Initiative in Innovative Computing and NVIDIA sponsored CUDA Center for Excellence at Harvard, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University of Technology and The University of Western Australia, funded by the Western Australian State government. NR 18 TC 42 Z9 42 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 1 BP L5 EP L9 DI 10.1093/mnrasl/sls013 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134TT UT WOS:000318238300002 ER PT J AU Koljonen, KII McCollough, ML Hannikainen, DC Droulans, R AF Koljonen, K. I. I. McCollough, M. L. Hannikainen, D. C. Droulans, R. TI 2006 May-July major radio flare episodes in Cygnus X-3: spectrotiming analysis of the X-ray data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; X-rays: binaries; X-rays: individual: Cygnus X-3; X-rays: stars ID CYG X-3; SPECTRAL VARIABILITY; VLBI OBSERVATIONS; RELATIVISTIC JET; EMISSION-LINES; ENERGY-SPECTRA; HARD STATE; GAMMA-RAYS; SCATTERING; OUTBURST AB We analyse in detail the X-ray data of the microquasar Cygnus X-3 obtained during major radio flaring episodes in 2006 with multiple observatories. The analysis consists of two parts: probing the fast (similar to 1 min) X-ray spectral evolution with principal component analysis followed by subsequent spectral fits to the time-averaged spectra (similar to 3 ks). Based on the analysis we find that the overall X-ray variability during major flaring episodes can be attributed to two principal components whose evolution based on spectral fits is best reproduced by a hybrid Comptonization component and a bremsstrahlung or saturated thermal Comptonization component. The variability of the thermal component is found to be linked to the change in the X-ray/radio spectral state. In addition, we find that the seed photons for the Comptonization originate in two seed photon populations that include the additional thermal emission and emission from the accretion disc. The Comptonization of the photons from the thermal component dominates, at least during the major radio flare episode in question, and the Comptonization of disc photons is intermittent and can be attributed to the phase interval 0.2-0.4. The most likely location for Comptonization is in the shocks in the jet. C1 [Koljonen, K. I. I.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [McCollough, M. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hannikainen, D. C.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Droulans, R.] LCE, L-6401 Echternach, Luxembourg. [Droulans, R.] IRAP, CNRS, F-31028 Toulouse 4, France. RP Koljonen, KII (reprint author), Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, FIN-02540 Kylmala, Finland. EM karri.koljonen@gmail.com OI Koljonen, Karri/0000-0002-9677-1533 FU Finnish Graduate School of Astronomy and Space Sciences; Jenny ja Antti Wihurin saatio; Academy of Finland [125189]; NASA [NNX06AB94G, NNG06GE72G, NAS8-03060] FX KIIK gratefully acknowledges support from the Finnish Graduate School of Astronomy and Space Sciences, a grant from Jenny ja Antti Wihurin saatio and Academy of Finland grant (project number 125189). This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. MLM acknowledges support from NASA under grant/contract NNX06AB94G, NNG06GE72G, and NAS8-03060. NR 51 TC 6 Z9 6 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 2 BP 1173 EP 1188 DI 10.1093/mnras/sts404 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134UC UT WOS:000318239300021 ER PT J AU Bartlett, ES Clark, JS Coe, MJ Garcia, MR Uttley, P AF Bartlett, E. S. Clark, J. S. Coe, M. J. Garcia, M. R. Uttley, P. TI Timing and spectral analysis of the unusual X-ray transient XTE J0421+560/CI Camelopardalis SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: miscellaneous; stars: emission-line; stars: individual: XTE J0421+560; X-rays: binaries ID ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; CI CAMELOPARDALIS; XMM-NEWTON; IGR J16318-4848; CLUSTER WESTERLUND-1; BINARY; LINE; SPECTROSCOPY; EMISSION AB We present a detailed X-ray study of the 2003 XMM-Newton observation of the high-mass X-ray binary XTE J0421+560/CI Camelopardalis. The continuum of the X-ray spectrum is well described by a flat power law (Gamma = 1.0 +/- 0.2) with a large intrinsic absorbing column (N-H = (4.4 +/- 0.5) x 10(23) cm(-2)). We have decomposed the broad iron line into three separate components: Fe I-K alpha, Fe I-K beta and Fe XXIV-XXVK alpha. It is unclear how both neutral and almost fully ionized iron can exist simultaneously; however, we suggest that this could be evidence that the compact object is embedded in the circumstellar material. This does not appear to be consistent with the X-ray flux and spectrum of the source, which has remained essentially unchanged since the initial outburst. The iron abundance implied by the ratio of the neutral Fe-K alpha and Fe-K beta is compatible with solar. We search for lags in the neutral Fe-K alpha with respect to the continuum and find marginal evidence for a lag at similar to 10 ks. We interpret this as the light crossing time of the torus which would suggest that the neutral iron is located at a radius of 10 au. This result depends on several assumptions including the distance to the system, the inclination, the mass of system and the orbital period, none of which are known with any great certainty. Better constraints on these system parameters and further observations of this system are required to confirm this result. We discuss the nature of this system in light of our results and place it in context with other binary B[e] stars. C1 [Bartlett, E. S.; Coe, M. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Clark, J. S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Garcia, M. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Uttley, P.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. RP Bartlett, ES (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM e.s.bartlett@soton.ac.uk OI Bartlett, Elizabeth/0000-0003-0634-4405 FU ESA; NASA; Science and Technology Facilities Council FX Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. ESB acknowledges support from a Science and Technology Facilities Council studentship. We would like to thank Arvind Parmar, the original PI of the data set. NR 45 TC 7 Z9 7 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 2 BP 1213 EP 1220 DI 10.1093/mnras/sts411 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134UC UT WOS:000318239300024 ER PT J AU Roseboom, IG Lawrence, A Elvis, M Petty, S Shen, Y Hao, H AF Roseboom, I. G. Lawrence, A. Elvis, M. Petty, S. Shen, Yue Hao, H. TI IR-derived covering factors for a large sample of quasars from WISE-UKIDSS-SDSS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE quasars: general; infrared: general ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; WIDE-FIELD CAMERA; SEYFERT-GALAXIES; STAR-FORMATION; DUSTY TORI; HOT-DUST; PHOTOMETRIC SYSTEM; TYPE-1 QUASARS; DATA RELEASE AB We investigate the range of covering factors (determined from the ratio of IR to UV/optical luminosity) seen in luminous type 1 quasars using a combination of data from the Wide-Field Infrared Survey Explorer, UKIDSS and SDSS surveys. Accretion disc (UV/optical) and obscuring dust (IR) luminosities are measured via the use of a simple three-component SED model. We use these estimates to investigate the distribution of covering factors and its relationship to both accretion luminosity and IR SED shape. The distribution of covering factors (f(C)) is observed to be log-normal, with a bias-corrected mean of < log(10) f(C) > = - 0.41 and standard deviation of sigma = 0.2. The fraction of IR luminosity emitted in the near-IR (1-5 mu m) is found to be high (similar to 40 per cent), and strongly dependant on covering factor. C1 [Roseboom, I. G.; Lawrence, A.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Elvis, M.; Shen, Yue; Hao, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petty, S.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Hao, H.] SISSA, I-34136 Trieste, Italy. RP Roseboom, IG (reprint author), Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM igr@roe.ac.uk FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. NR 77 TC 33 Z9 33 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 2 BP 1494 EP 1501 DI 10.1093/mnras/sts441 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134UC UT WOS:000318239300045 ER PT J AU Fornasa, M Zavala, J Sanchez-Conde, MA Siegal-Gaskins, JM Delahaye, T Prada, F Vogelsberger, M Zandanel, F Frenk, CS AF Fornasa, Mattia Zavala, Jesus Sanchez-Conde, Miguel A. Siegal-Gaskins, Jennifer M. Delahaye, Timur Prada, Francisco Vogelsberger, Mark Zandanel, Fabio Frenk, Carlos S. TI Characterization of dark-matter-induced anisotropies in the diffuse gamma-ray background SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astroparticle physics; methods: numerical; cosmology: dark matter; gamma-rays: diffuse background ID STAR-FORMING GALAXIES; LARGE-SCALE STRUCTURE; RADIO GALAXIES; FERMI-LAT; MILKY-WAY; ANNIHILATION SIGNAL; POWER SPECTRUM; RADIATION; HALOES; BLAZARS AB The Fermi-LAT collaboration has recently reported the detection of angular power above the photon noise level in the diffuse gamma-ray background between 1 and 50 GeV. Such signal can be used to constrain a possible contribution from dark matter (DM) induced photons. We estimate the intensity and features of the angular power spectrum (APS) of this potential DM signal, for both decaying and annihilating DM candidates, by constructing template all-sky gamma-ray maps for the emission produced in the galactic halo and its substructures, as well as in extragalactic (sub)haloes. The DM distribution is given by state-of-the-art N-body simulations of cosmic structure formation, namely Millennium-II for extragalactic (sub)haloes, and Aquarius for the galactic halo and its subhaloes. We use a hybrid method of extrapolation to account for (sub)structures that are below the resolution limit of the simulations, allowing us to estimate the total emission all the way down to the minimal self-bound halo mass. We describe in detail the features appearing in the APS of our template maps and we estimate the effect of various uncertainties such as the value of the minimal halo mass, the fraction of substructures hosted in a halo and the shape of the DM density profile. Our results indicate that the fluctuation APS of the DM-induced emission is of the same order as the Fermi-LAT APS, suggesting that one can constrain this hypothetical emission from the comparison with the measured anisotropy. We also quantify the uncertainties affecting our results, finding 'theoretical error bands' spanning more than two orders of magnitude and dominated (for a given particle physics model) by our lack of knowledge of the abundance of low-mass (sub)haloes. C1 [Fornasa, Mattia; Prada, Francisco; Zandanel, Fabio] Inst Astrofis Andalucia IAA CSIC, Granada, Spain. [Fornasa, Mattia] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Zavala, Jesus] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Zavala, Jesus] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Sanchez-Conde, Miguel A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Sanchez-Conde, Miguel A.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Siegal-Gaskins, Jennifer M.] CALTECH, Pasadena, CA 91125 USA. [Delahaye, Timur; Prada, Francisco] Univ Autonoma Madrid Cantoblanco, Inst Fis Teor, UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] UAM CSIC, E-28049 Madrid, Spain. [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frenk, Carlos S.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DM1 3LE, England. RP Fornasa, M (reprint author), Inst Astrofis Andalucia IAA CSIC, Granada, Spain. EM fornasam@gmail.com OI Delahaye, Timur/0000-0001-8134-1648; Fornasa, Mattia/0000-0002-2692-117X FU Consolider-Ingenio [CSD2009-00064]; University of Waterloo; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research Innovation; NASA [NNH09ZDA001N, PF1-120089, NAS8-03060]; CITA; Spanish MICINNs [CSD2007-00042]; MICINN [FPA2009-08958]; Community of Madrid [HEP-HACOSS2009/ESP-1473]; European Union [PITN-GA-2009-237920]; STFC; Large Facilities Capital Fund of BIS; Durham University; clusters at the Max-Planck Institute for Astrophysics FX We thank Alberto Dominguez for providing us with tables for the EBL attenuation factor and the referee, M. Kuhlen, for a thorough and constructive report. JZ thanks Niayesh Afshordi for fruitful discussions. We thank Alessandro Cuoco and Anne Green for useful comments and discussions. We also thank Chris Hirata and the support of the Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064. JZ is supported by the University of Waterloo and the Perimeter Institute for Theoretical Physics. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research & Innovation. The work of MASC is supported through the NASA grant NNH09ZDA001N for study of the Extragalactic Gamma-ray Background. JZ acknowledges financial support by a CITA National Fellowship. JSG acknowledges support from NASA through Einstein Postdoctoral Fellowship grant PF1-120089 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. TD was supported by the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant CPAN CSD2007-00042. We also thank the support of the MICINN under grant FPA2009-08958, the Community of Madrid under grant HEP-HACOSS2009/ESP-1473, and the European Union under the Marie Curie-ITN program PITN-GA-2009-237920. The calculations for this paper were performed on the ICC Cosmology Machine, which is part of the DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS, and Durham University, and the clusters at the Max-Planck Institute for Astrophysics. We acknowledge use of the facilities of the Shared Hierarchical Academic Research Computing Network (SHARCNET:www.sharcnet.ca) aCompute/Calcul Canada. NR 147 TC 32 Z9 32 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 429 IS 2 BP 1529 EP 1553 DI 10.1093/mnras/sts444 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134UC UT WOS:000318239300048 ER PT J AU Walton, DJ Nardini, E Fabian, AC Gallo, LC Reis, RC AF Walton, D. J. Nardini, E. Fabian, A. C. Gallo, L. C. Reis, R. C. TI Suzaku observations of 'bare' active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: active ID X-RAY REFLECTION; BLACK-HOLE SPIN; XMM-NEWTON OBSERVATION; LINE SEYFERT-1 GALAXY-1H-0707-495; BROAD IRON LINES; ACCRETION DISK; 1H 0707-495; SPECTRAL PROPERTIES; ABSORPTION ORIGIN; RADIO GALAXIES AB We present an X-ray spectral analysis of a large sample of 25 'bare' active galactic nuclei (AGN), sources with little or no complicating intrinsic absorption, observed with Suzaku. Our work focuses on studying the potential contribution from relativistic disc reflection and examining the implications of this interpretation for the intrinsic spectral complexities frequently displayed by AGN in the X-ray bandpass. During the analysis, we take the unique approach of attempting to simultaneously undertake a systematic analysis of the whole sample, as well as a detailed treatment of each individual source, and find that disc reflection has the required flexibility to successfully reproduce the broad-band spectrum observed for all of the sources considered. Where possible, we use the reflected emission to place constraints on the black hole spin for this sample of sources. Our analysis suggests a general preference for rapidly rotating black holes, which if taken at face value is most consistent with the scenario in which supermassive black hole growth is dominated by prolonged, ordered accretion. However, there may be observational biases towards AGN with high spin in the compiled sample, limiting our ability to draw strong conclusions for the general population at this stage. Finally, contrary to popular belief, our analysis also implies that the dichotomy between radio-loud/radio-quiet AGN is not solely related to black hole spin. C1 [Walton, D. J.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Walton, D. J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Nardini, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gallo, L. C.] St Marys Univ, Dept Astron & Phys, Halifax, NS B3H 3C3, Canada. [Reis, R. C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Walton, DJ (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM dwalton@ast.cam.ac.uk RI XRAY, SUZAKU/A-1808-2009; OI reis, rubens/0000-0002-6618-2412 FU STFC; NASA [GO2-13124X, NNX11AG99G, PF1-120087] FX This research has made use of data obtained from the Suzaku observatory, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). DJW acknowledges the financial support provided by STFC in the form of a PhD scholarship, EN is supported by NASA grants GO2-13124X and NNX11AG99G, and ACF thanks the Royal Society. RCR thanks the Michigan Society of Fellows, and is supported by NASA through the Einstein Fellowship Program, grant number PF1-120087. Special thanks go to both Jeremy Sanders and Jack Steiner for their computational assistance, which greatly aided in the publication of this research. The figures included in this work have been produced with the VEUSZ7 plotting package, written by Jeremy Sanders. Finally, the authors would like to thank the referee for their feedback, which helped improve the depth of this work. NR 97 TC 91 Z9 92 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 428 IS 4 BP 2901 EP 2920 DI 10.1093/mnras/sts227 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RM UT WOS:000318232000010 ER PT J AU Oliveira, JM van Loon, JT Sloan, GC Sewilo, M Kraemer, KE Wood, PR Indebetouw, R Filipovic, MD Crawford, EJ Wong, GF Hora, JL Meixner, M Robitaille, TP Shiao, B Simon, JD AF Oliveira, J. M. van Loon, J. Th Sloan, G. C. Sewilo, M. Kraemer, K. E. Wood, P. R. Indebetouw, R. Filipovic, M. D. Crawford, E. J. Wong, G. F. Hora, J. L. Meixner, M. Robitaille, T. P. Shiao, B. Simon, J. D. TI Early-stage young stellar objects in the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; circumstellar matter; stars: formation; stars: protostars; galaxies: individual: SMC; Magellanic Clouds ID SPITZER-SPACE-TELESCOPE; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AROMATIC-HYDROCARBON EMISSION; ARRAY CAMERA IRAC; PHOTODISSOCIATION REGIONS; GALAXY EVOLUTION; RADIO-CONTINUUM; LOW METALLICITY; IRS SPECTRA AB We present new observations of 34 young stellar object (YSO) candidates in the Small Magellanic Cloud (SMC). The photometric selection required sources to be bright at 24 and 70 mu m (to exclude evolved stars and galaxies). The anchor of the analysis is a set of Spitzer Infrared Spectrograph (IRS) spectra, supplemented by ground-based 3-5 mu m spectra, Spitzer Infrared Array Camera and Multiband Imaging Photometer for Spitzer photometry, near-infrared (IR) imaging and photometry, optical spectroscopy and radio data. The sources' spectral energy distributions and spectral indices are consistent with embedded YSOs; prominent silicate absorption is observed in the spectra of at least 10 sources, silicate emission is observed towards four sources. Polycyclic aromatic hydrocarbon (PAH) emission is detected towards all but two sources. Based on band ratios (in particular the strength of the 11.3-mu m and the weakness of the 8.6-mu m bands) PAH emission towards SMC YSOs is dominated by predominantly small neutral grains. Ice absorption is observed towards 14 sources in the SMC. The comparison of H2O and CO2 ice column densities for SMC, Large Magellanic Cloud and Galactic samples suggests that there is a significant H2O column density threshold for the detection of CO2 ice. This supports the scenario proposed by Oliveira et al., where the reduced shielding in metal-poor environments depletes the H2O column density in the outer regions of the YSO envelopes. No CO ice is detected towards the SMC sources. Emission due to pure rotational 0-0 transitions of molecular hydrogen is detected towards the majority of SMC sources, allowing us to estimate rotational temperatures and H-2 column densities. All but one source are spectroscopically confirmed as SMC YSOs. Based on the presence of ice absorption, silicate emission or absorption and PAH emission, the sources are classified and placed in an evolutionary sequence. Of the 33 YSOs identified in the SMC, 30 sources populate different stages of massive stellar evolution. The presence of ice- and/or silicate-absorption features indicates sources in the early embedded stages; as a source evolves, a compact H II region starts to emerge, and at the later stages the source's IR spectrum is completely dominated by PAH and fine-structure emission. The remaining three sources are classified as intermediate-mass YSOs with a thick dusty disc and a tenuous envelope still present. We propose one of the SMC sources is a D-type symbiotic system, based on the presence of Raman, H and He emission lines in the optical spectrum, and silicate emission in the IRS spectrum. This would be the first dust-rich symbiotic system identified in the SMC. C1 [Oliveira, J. M.; van Loon, J. Th] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Wood, P. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. [Filipovic, M. D.; Crawford, E. J.; Wong, G. F.] Univ Western Sydney, Penrith, NSW 1797, Australia. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meixner, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Simon, J. D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Oliveira, JM (reprint author), Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. EM j.oliveira@keele.ac.uk OI Crawford, Evan/0000-0001-5197-1091; Kraemer, Kathleen/0000-0002-2626-7155; Robitaille, Thomas/0000-0002-8642-1329 FU NASA FX We thank the staff at ESO's Paranal and La Silla Observatories for their support during the observations. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. We thank the referee for helpful comments. NR 81 TC 20 Z9 20 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 428 IS 4 BP 3001 EP 3033 DI 10.1093/mnras/sts250 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RM UT WOS:000318232000017 ER PT J AU Henshaw, JD Caselli, P Fontani, F Jimenez-Serra, I Tan, JC Hernandez, AK AF Henshaw, J. D. Caselli, P. Fontani, F. Jimenez-Serra, I. Tan, J. C. Hernandez, A. K. TI Complex, quiescent kinematics in a highly filamentary infrared dark cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: individual objects: G035.39-00.33; ISM: molecules ID MASSIVE-STAR-FORMATION; GRAIN-GRAIN COLLISIONS; INITIAL CONDITIONS; TEMPERATURE STRUCTURE; INTERSTELLAR SHOCKS; PHYSICAL-PROPERTIES; COLUMN DENSITY; CO DEPLETION; CORES; GAS AB Infrared dark clouds (IRDCs) host the initial conditions under which massive stars and stellar clusters form. It is therefore important to study the kinematics, as well as the physical and chemical properties of these regions. Their complex structure however posits challenges in the data interpretation. We have obtained high-sensitivity and high-spectral-resolution observations with the Instituto de Radioastronomia Milimetrica 30 m antenna, which allowed us to perform detailed analysis of the kinematics within one IRDC, G035.39-00.33. This cloud has been selected for its highly filamentary morphology and the presence of extended quiescent regions, characteristics of dynamical youth. We focus on the J = 1 -> 0 and J = 3 -> 2 transitions of N2H+, (CO)-O-18 (1-0), and make comparison with SiO (2-1) observations and extinction mapping. Three interacting filaments of gas are found. We report large-scale velocity coherence throughout the cloud, evidenced through small velocity gradients and relatively narrow line widths. This suggests that the merging of these filaments is somewhat 'gentle', possibly regulated by magnetic fields. This merging of filaments may be responsible for the production of weak, parsec-scale SiO emission, via grain mantle vaporization. A systematic velocity shift between the N2H+ (1-0) and (CO)-O-18 (1-0) gas throughout the cloud of 0.18 +/- 0.04 km s(-1) is also found, consistent with a scenario of collisions between filaments which is still ongoing. The N2H+ (1-0) is extended throughout the IRDC, in contrast to low-mass star forming regions, where N2H+ is known to trace only the dense cores. The average H-2 number density across the IRDC is similar or equal to 5 x 10(4) cm(-3), at least one order of magnitude larger than in nearby molecular clouds where low-mass stars are forming. A temperature gradient perpendicular to the filament is found. From our study, we conclude that G035.39-00.33 (clearly seen in the extinction map and in N2H+) has been formed via the collision between two relatively quiescent filaments with average densities of similar or equal to 5 x 10(3) cm(-3), moving with relative velocities of similar or equal to 5 km s(-1). The accumulation of material at the merging points started greater than or similar to 1 Myr ago and it is still ongoing. C1 [Henshaw, J. D.; Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Fontani, F.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tan, J. C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hernandez, A. K.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Henshaw, JD (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. EM phy5jh@leeds.ac.uk OI Fontani, Francesco/0000-0003-0348-3418 FU STFC rolling grant; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX We acknowledge the IRAM staff for the help provided during the observations. We thank Michael Butler and Jouni Kainulainen for providing the extinction maps for this work. We also thank Jaime E. Pineda for assistance with image processing. PC's work on star formation is supported by an STFC rolling grant.; Based on observations carried out with the IRAM 30 m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). NR 62 TC 24 Z9 24 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 428 IS 4 BP 3425 EP 3442 DI 10.1093/mnras/sts282 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RM UT WOS:000318232000048 ER PT J AU Ratti, EM van Grunsven, TFJ Jonker, PG Britt, CT Hynes, RI Steeghs, D Greiss, S Torres, MAP Maccarone, TJ Groot, PJ Knigge, C Gossen, L Mikles, V Villar, VA Collazzi, AC AF Ratti, E. M. van Grunsven, T. F. J. Jonker, P. G. Britt, C. T. Hynes, R. I. Steeghs, D. Greiss, S. Torres, M. A. P. Maccarone, T. J. Groot, P. J. Knigge, C. Gossen, L. Mikles, V. Villar, V. A. Collazzi, A. C. TI CXOGBS J174444.7-260330: a new long orbital period cataclysmic variable in a low state SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion: accretion discs; stars: dwarf novae; stars: individual: CXOGBS J174444.7-260330; novae, cataclysmic variables; X-rays: binaries ID IMAGE SUBTRACTION; ACCRETION DISKS; BLACK-HOLE; MASS; INTERMEDIATE; SPECTROSCOPY; EXTINCTION; EMISSION; A0620-00 AB We present phase-resolved spectroscopy and photometry of a source discovered with the Chandra Galactic Bulge Survey (GBS), CXOGBS J174444.7-260330 (aka CX93 and CX153 in the previously published GBS list). We find two possible values for the orbital period P, differing from each other by similar to 13 s. The most likely solution is P = 5.690 14(6) h. The optical lightcurves show ellipsoidal modulations, whose modelling provides an inclination of 32 +/- 1 degrees for the most likely P. The spectra are dominated by a K5 V companion star (the disc veiling is less than or similar to 5 per cent). Broad and structured emission from the Balmer lines is also detected, as well as fainter emission from He I. From the absorption lines we measure K-2 = 117 +/- 8 km s(-1) and upsilon sin i = 69 +/- 7 km s(-1). By solving the system mass function we find M-1 = 0.8 +/- 0.2 M-circle dot for the favoured P and i, consistent with a white dwarf accretor, and M-2 = 0.6 +/- 0.2 M-circle dot. We estimate a distance in the range 400-700 pc. Although in a low accretion state, both spectroscopy and photometry provide evidence of variability on a time-scale of months or faster. Besides finding a new, long orbital period cataclysmic variable (CV) in a low accretion state, this work shows that the design of the GBS works efficiently to find accreting X-ray binaries in quiescence, highlighting that the spectra of CVs in a low accretion state can at times appear suggestive of a quiescent neutron star or a black hole system. C1 [Ratti, E. M.; van Grunsven, T. F. J.; Jonker, P. G.; Torres, M. A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Steeghs, D.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Britt, C. T.; Hynes, R. I.; Collazzi, A. C.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Maccarone, T. J.; Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Gossen, L.; Mikles, V.] IM Syst Grp, Kensington, MD 20895 USA. [Villar, V. A.] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Ratti, EM (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM e.m.ratti@sron.nl RI Steeghs, Danny/C-5468-2009; Groot, Paul/K-4391-2016 OI Steeghs, Danny/0000-0003-0771-4746; Groot, Paul/0000-0002-4488-726X FU National Science Foundation [AST-0908789]; NASA/Louisiana Board of Regents [NNX07AT62A/LEQSF]; VIDI grant from the Netherlands Organisation for Scientific Research; STFC; Warwick Rolling grant FX RIH and CTB acknowledge support from the National Science Foundation under Grant No. AST-0908789. RIH also acknowledges support from NASA/Louisiana Board of Regents grant NNX07AT62A/LEQSF(2007-10) Phase3-02. PGJ acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. DS acknowledges support from STFC via an Advanced Fellowship and the Warwick Rolling grant. Tom Marsh is thanked for developing and sharing his packages PAMELA and MOLLY and E.L. Robinson for his XRBINARY code. We also acknowledge G. Nelemans for useful discussions and J.E. McClintock for his comments. NR 33 TC 10 Z9 10 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 428 IS 4 BP 3543 EP 3550 DI 10.1093/mnras/sts292 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RM UT WOS:000318232000056 ER PT J AU Vrtilek, SD Boroson, BS AF Vrtilek, Saeqa Dil Boroson, Bram Seth TI Model independent means of categorizing X-ray binaries - I. Colour-colour-intensity diagrams SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE pulsars: general; X-rays: binaries ID MULTIWAVELENGTH CAMPAIGN; UNIFIED MODEL; JETS; CATALOG; IUE AB The diverse behaviours displayed by X-ray binaries make it difficult to determine the nature of the underlying compact objects. In particular, identification of systems containing black holes is currently considered robust only if a dynamical mass is obtained. We explore a model-independent means of identifying the central bodies - neutron stars or black holes - of accreting binary systems. We find that four categories of object (classic black holes, GRS 1915-like black holes, pulsars and non-pulsing neutron stars) occupy distinct regions in a 3D colour-colour-intensity (CCI) diagram. Assuming that this clustering effect is due to intrinsic properties of the sources (such as mass-accretion rate, binary separation, mass ratio, magnetic field strength, etc.), we suggest possible physical effects that drive each object to its specific location in the CCI phase space. We also suggest a surface in this space which separates systems that produce jets from those which do not, and demonstrate the use of CCI for identifying X-ray pulsars where a period has not been established. This method can also be used to study subclustering within a category and may prove useful for other classes of objects, such as cataclysmic variables and active galactic nuclei. C1 [Vrtilek, Saeqa Dil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boroson, Bram Seth] Clayton State Univ, Dept Phys, Morrow, GA 30260 USA. RP Vrtilek, SD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svrtilek@cfa.harvard.edu NR 19 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD FEB PY 2013 VL 428 IS 4 BP 3693 EP 3714 DI 10.1093/mnras/sts312 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RM UT WOS:000318232000070 ER PT J AU Williams, NR Watters, TR Pritchard, ME Banks, ME Bell, JF AF Williams, N. R. Watters, T. R. Pritchard, M. E. Banks, M. E. Bell, J. F., III TI Fault dislocation modeled structure of lobate scarps from Lunar Reconnaissance Orbiter Camera digital terrain models SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID TOTALLY MOLTEN MOON; THRUST FAULTS; MARS; MERCURY; DEFORMATION; LITHOSPHERE; CONSTRAINTS; CONTRACTION; TOPOGRAPHY; DICHOTOMY AB [1] Before the launch of the Lunar Reconnaissance Orbiter, known characteristics of lobate scarps on the Moon were limited to studies of only a few dozen scarps revealed in Apollo-era photographs within similar to 20 degrees of the equator. The Lunar Reconnaissance Orbiter Camera now provides meter-scale images of more than 100 lobate scarps, as well as stereo-derived topography of about a dozen scarps. High-resolution digital terrain models (DTMs) provide unprecedented insight into scarp morphology and dimensions. Here, we analyze images and DTMs of the Slipher, Racah X-1, Mandel'shtam-1, Feoktistov, Simpelius-1, and Oppenheimer F lobate scarps. Parameters in fault dislocation models are iteratively varied to provide best fits to DTM topographic profiles to test previous interpretations that the observed landforms are the result of shallow, low-angle thrust faults. Results suggest that these faults occur from the surface down to depths of hundreds of meters, have dip angles of 35-40 degrees, and have typical maximum slips of tens of meters. These lunar scarp models are comparable to modeled geometries of lobate scarps on Mercury, Mars, and asteroid 433 Eros, but are shallower and similar to 10 degrees sleeper than geometries determined in studies with limited Apollo-era data. Frictional and rock mass strength criteria constrain the state of global differential stress between 3.5 and 18.6 MPa at the modeled maximum depths of faulting. Our results are consistent with thermal history models that predict relatively small compressional stresses that likely arise from cooling of a magma ocean. Citation: Williams, N. R., T. R. Watters, M. E. Pritchard, M. E. Banks, and J. F. Bell III (2013), Fault dislocation modeled structure of lobate scarps from Lunar Reconnaissance Orbiter Camera digital terrain models, J. Geophys. Res. Planets, 118, 224-233, doi: 10.1002/jgre.20051. C1 [Williams, N. R.; Bell, J. F., III] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Watters, T. R.; Banks, M. E.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Pritchard, M. E.] Cornell Univ, Dept Earth & Atmospher Sci, Ithaca, NY USA. RP Williams, NR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. EM Nathan.R.Williams@asu.edu RI Pritchard, Matthew/L-5892-2015 OI Pritchard, Matthew/0000-0003-3616-3373 FU LRO Project, Arizona State University School of Earth; Space Exploration; Smithsonian Institution National Air and Space Museum; Cornell University College of Engineering FX We gratefully acknowledge Mark Robinson, Thanh Tran, and the rest of the LRO and LROC teams. We also acknowledge the constructive comments of the two anonymous reviewers and the Associate Editor. This work was supported by the LRO Project, Arizona State University School of Earth and Space Exploration, Smithsonian Institution National Air and Space Museum, and the Cornell University College of Engineering. NR 52 TC 10 Z9 10 U1 0 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2013 VL 118 IS 2 BP 224 EP 233 DI 10.1002/jgre.20051 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 129MQ UT WOS:000317845100005 ER PT J AU Irwin, RP Tanaka, KL Robbins, SJ AF Irwin, Rossman P., III Tanaka, Kenneth L. Robbins, Stuart J. TI Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID IMPACT CRATERS; FLUVIAL PROCESSES; SINUS SABAEUS; MARS; EVOLUTION; DEGRADATION; HISTORY; ORIGIN; CONSTRAINTS; CHRONOLOGY AB Most of the geomorphic changes on Mars occurred during the Noachian Period, when the rates of impact crater degradation and valley network incision were highest. Fluvial erosion around the Noachian/Hesperian transition is better constrained than the longer-term landscape evolution throughout the Noachian Period, when the highland intercrater geomorphic surfaces developed. We interpret highland resurfacing events and processes using a new global geologic map of Mars (at 1: 20,000,000 scale), a crater data set that is complete down to 1 km in diameter, and Mars Orbiter Laser Altimeter topography. The Early Noachian highland (eNh) unit is nearly saturated with craters of 32-128 km diameter, the Middle Noachian highland (mNh) unit has a resurfacing age of similar to 4 Ga, and the Late Noachian highland unit (lNh) includes younger composite surfaces of basin fill and partially buried cratered terrain. These units have statistically distinct ages, and their distribution varies with elevation. The eNh unit is concentrated in the high-standing Hellas basin annulus and in highland terrain that was thinly mantled by basin ejecta near 180 degrees longitude. The mNh unit includes most of Arabia Terra, the Argyre vicinity, highland plateau areas between eNh outcrops, and the Thaumasia range. The lNh unit mostly occurs within highland basins. Crater depth/diameter ratios do not vary strongly between the eNh and mNh units, although crater losses to Noachian resurfacing appear greater in lower lying areas. Noachian resurfacing was spatially non-uniform, long-lived, and gravity-driven, more consistent with arid-zone fluvial and aeolian erosion and volcanism than with air fall mantling or mass wasting. Citation: Irwin, R. P., III, K. L. Tanaka, and S. J. Robbins (2013), Distribution of Early, Middle, and Late Noachian cratered surfaces in the Martian highlands: Implications for resurfacing events and processes, J. Geophys. Res. Planets, 118, 278-291, doi:10.1002/jgre.20053. C1 [Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Tanaka, Kenneth L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Robbins, Stuart J.] Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. RP Irwin, RP (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,6th St & Independence Ave SW, Washington, DC 20013 USA. EM irwinr@si.edu FU NASA Planetary Geology and Geophysics Program [NNH10AN97I]; U.S. Geological Survey; Mars Data Analysis Program; Planetary Science Institute [NNX10AE64G] FX This study was funded by grants from the NASA Planetary Geology and Geophysics Program (NNH10AN97I, U.S. Geological Survey, K. L. Tanaka, Principal Investigator) and Mars Data Analysis Program (NNX10AE64G, Planetary Science Institute, R. P. Irwin III, Principal Investigator). We are grateful to Nadine Barlow and Caleb Fassett for their detailed reviews. We also thank Colin Dundas, Alan Howard, and Bob Craddock for helpful discussions on technical details of the paper. NR 71 TC 13 Z9 13 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2013 VL 118 IS 2 BP 278 EP 291 DI 10.1002/jgre.20053 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 129MQ UT WOS:000317845100008 ER PT J AU McSween, HY Ammannito, E Reddy, V Prettyman, TH Beck, AW De Sanctis, MC Nathues, A Le Corre, L O'Brien, DP Yamashita, N McCoy, TJ Mittlefehldt, DW Toplis, MJ Schenk, P Palomba, E Turrini, D Tosi, F Zambon, F Longobardo, A Capaccioni, F Raymond, CA Russell, CT AF McSween, Harry Y. Ammannito, Eleonora Reddy, Vishnu Prettyman, Thomas H. Beck, Andrew W. De Sanctis, M. Cristina Nathues, Andreas Le Corre, Lucille O'Brien, David P. Yamashita, Naoyuki McCoy, Timothy J. Mittlefehldt, David W. Toplis, Michael J. Schenk, Paul Palomba, Ernesto Turrini, Diego Tosi, Federico Zambon, Francesca Longobardo, Andrea Capaccioni, Fabrizio Raymond, Carol A. Russell, Christopher T. TI Composition of the Rheasilvia basin, a window into Vesta's interior SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ASTEROID 4 VESTA; EUCRITE PARENT BODY; EARLY SOLAR-SYSTEM; ORTHO-PYROXENE; DIOGENITE METEORITES; REFLECTANCE SPECTRA; HED METEORITES; DAWN MISSION; ORIGIN; HOWARDITE AB The estimated excavation depth of the huge Rheasilvia impact basin is nearly twice the likely thickness of the Vestan basaltic crust, so the mantle should be exposed. Spectral mapping by the Dawn spacecraft reveals orthopyroxene-rich materials, similar to diogenite meteorites, in the deepest parts of the basin and within its walls. Significant amounts of olivine are predicted for the mantles of bulk-chondritic bodies like Vesta, and its occurrence is demonstrated by some diogenites that are harzburgite and dunite. However, olivine has so far escaped detection by Dawn's instruments. Spectral detection of olivine in the presence of orthopyroxene is difficult in samples with < 25% olivine, and olivine in Rheasilvia might have been diluted during impact mixing or covered by the collapse of basin walls. The distribution of diogenite inferred from its exposures in and around Rheasilvia provides a geologic context for the formation of these meteorites, but does not clearly distinguish between a magmatic cumulate versus partial melting restite origin for diogenites. The former is favored by geochemical arguments, and crystallization in either a magma ocean or multiple plutons emplaced near the crust-mantle boundary is permitted by Dawn observations. Citation: McSween, H. Y., et al. (2013), Composition of the Rheasilvia basin, a window into Vesta's interior, J. Geophys. Res. Planets, 118, 335-346, doi:10.1002/jgre.20057. C1 [McSween, Harry Y.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Ammannito, Eleonora; De Sanctis, M. Cristina; Palomba, Ernesto; Turrini, Diego; Tosi, Federico; Zambon, Francesca; Longobardo, Andrea; Capaccioni, Fabrizio] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Reddy, Vishnu; Nathues, Andreas; Le Corre, Lucille] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Reddy, Vishnu] Univ N Dakota, Dept Space Studies, Grand Forks, ND 58201 USA. [Prettyman, Thomas H.; O'Brien, David P.; Yamashita, Naoyuki] Planetary Sci Inst, Tucson, AZ USA. [Beck, Andrew W.; McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Mittlefehldt, David W.] NASA, Lyndon B Johnson Space Ctr, Astromat Res Off, Houston, TX 77058 USA. [Toplis, Michael J.] Univ Toulouse, Inst Rech Astrophys & Planetol, Toulouse, France. [Schenk, Paul] Lunar & Planetary Inst, Houston, TX 77058 USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Russell, Christopher T.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. RP McSween, HY (reprint author), Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. EM mcsween@utk.edu RI De Sanctis, Maria Cristina/G-5232-2013; Beck, Andrew/J-7215-2015; OI Turrini, Diego/0000-0002-1923-7740; Capaccioni, Fabrizio/0000-0003-1631-4314; De Sanctis, Maria Cristina/0000-0002-3463-4437; Beck, Andrew/0000-0003-4455-2299; Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932; Palomba, Ernesto/0000-0002-9101-6774; Tosi, Federico/0000-0003-4002-2434; Zambon, Francesca/0000-0002-4190-6592 FU NASA's Discovery Program; University of California, Los Angeles; NASA's Dawn at Vesta Participating Scientists Program; Italian Space Agency; Max Planck Society; German Space Agency (DLR); Planetary Science Institute under Jet Propulsion Laboratory FX This work was funded by NASA's Discovery Program through a contract to the University of California, Los Angeles, by NASA's Dawn at Vesta Participating Scientists Program, by the Italian Space Agency, by the Max Planck Society and German Space Agency (DLR), and by the Planetary Science Institute under contract with the Jet Propulsion Laboratory, California Institute of Technology. We appreciate reviews by K. Keil, K. Righter, and an unnamed reviewer. NR 79 TC 52 Z9 53 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB PY 2013 VL 118 IS 2 BP 335 EP 346 DI 10.1002/jgre.20057 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 129MQ UT WOS:000317845100012 ER PT J AU Guan, TP Ge, BM McShea, WJ Li, S Song, YL Stewart, CM AF Guan, Tian-Pei Ge, Bao-Ming McShea, William J. Li, Sheng Song, Yan-Ling Stewart, Chad M. TI Seasonal migration by a large forest ungulate: a study on takin (Budorcas taxicolor) in Sichuan Province, China SO EUROPEAN JOURNAL OF WILDLIFE RESEARCH LA English DT Article DE Elevation gradient; Budorcas taxicolor; Migration; Bamboo forest; Population estimation; Habitat availability analysis ID DETECTION PROBABILITY; QINLING MOUNTAINS; HABITAT SELECTION; NATURE-RESERVE; GRIZZLY BEARS; GOLDEN TAKIN; HOME-RANGE; POPULATION; CONSERVATION; MOVEMENTS AB Migration in large mammals is a biological phenomenon that involves seasonal movements over a vertical or horizontal scale that encompasses distances of more than several home ranges. Takin are large bovid herbivores that conduct seasonal migrations. From 2006 to 2009, we utilized data from 9 GPS-collared animals and 22 trail event recorders to describe takin migration pattern at the level of both individuals and population. We found seasonal migration of takin over an elevation gradient which contained two migration cycles, with takin inhabiting the highest elevations in summer, lowest elevations in spring and autumn, and intermediate elevations during winter. These movements did not involve expansion of home range size but rather shifts in distribution. Habitat availability analysis based on five forest types indicated that takin showed significant monthly forest preferences. Based on both telemetry and trail monitors, mature forest with bamboo understory was the habitat favored by takin for more than 8 months of the year. Both methods also indicated that not all individuals migrated to the highest elevations during summer or the lowest elevations in winter. We also found that individual takin do not necessarily follow the same annual movement, as three out of the four animals with at least 2 years of data changed their migration pattern between years. Current protocols for annual surveys conducted at highelevation meadows or low-elevation valleys are not adequate to detect all individuals. We suggest that surveys must include all potential habitats and include detection functions in order to accurately estimate takin numbers or relative changes in their density. C1 [Guan, Tian-Pei] Mianyang Normal Univ, Ecol Secur & Protect Key Lab Sichuan Prov, Mianyang 621000, Peoples R China. [Guan, Tian-Pei; Song, Yan-Ling] Beijing Normal Univ, Minist Educ, Key Lab Biodivers Sci & Ecol Engn, Coll Life Sci, Beijing 100875, Peoples R China. [Ge, Bao-Ming] Jiangsu Prov Key Lab Coastal Wetland Bioresources, Yancheng 224002, Jiangsu, Peoples R China. [McShea, William J.; Li, Sheng; Stewart, Chad M.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Song, Yan-Ling] Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conservat Biol, Beijing 100101, Peoples R China. RP Song, YL (reprint author), Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conservat Biol, 1 Beichen West Rd, Beijing 100101, Peoples R China. EM songyl@ioz.ac.cn RI Ge, Bao-Ming/F-4827-2011 FU Hong Kong Ocean Park Conservation Foundation; National Geographic Society; Smithsonian National Zoological Park; Wilds and Friends of the National Zoo FX We thank the Hong Kong Ocean Park Conservation Foundation, National Geographic Society, Smithsonian National Zoological Park, The Wilds and Friends of the National Zoo for funding and trials of these collars and takin capture procedure. We appreciate Sichuan Forestry Department and Administration of Tangjiahe Nature Reserve for research permissions and management support. We thank Shen XiaoLi for providing valuable suggestion on statistics. We also thank Chen Li Min, Ma Wen Hu, Yang Jun, and all other Tangjiahe staff for providing great help in the takin capture, radio tracking, and logistic support. We thank Rachael Weiss, Barbara Wolfe, and Evan Blumer for assistance with darting and veterinary care. NR 48 TC 1 Z9 6 U1 1 U2 45 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-4642 J9 EUR J WILDLIFE RES JI Eur. J. Wildl. Res. PD FEB PY 2013 VL 59 IS 1 BP 81 EP 91 DI 10.1007/s10344-012-0650-2 PG 11 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 108XL UT WOS:000316329500009 ER PT J AU Gingerich, O AF Gingerich, Owen TI CURTIS ALAN WILSON (1921-2012) SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Biographical-Item C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD FEB PY 2013 VL 44 BP 93 EP 94 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 099HB UT WOS:000315611000005 ER PT J AU Ogburn, MB Criales, MM Thompson, RT Browder, JA AF Ogburn, Matthew B. Criales, Maria M. Thompson, R. Tyler Browder, Joan A. TI Endogenous swimming activity rhythms of postlarvae and juveniles of the penaeid shrimp Farfantepenaeus aztecus, Farfantepenaeus duorarum, and Litopenaeus setiferus SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Farfantepenaeus aztecus; Farfantepenaeus duorarum; Litopenaeus setiferus; Endogenous rhythms; Selective tidal-stream transport; Recruitment ID CRAB CALLINECTES-SAPIDUS; TIDAL-STREAM TRANSPORT; CROSS-SHELF TRANSPORT; PINK SHRIMP; BROWN SHRIMP; FLORIDA BAY; WHITE SHRIMP; SECONDARY DISPERSAL; ESTUARINE WATERS; SOUTH-CAROLINA AB Selective tidal-stream transport is commonly used by marine animals to migrate between oceanic and estuarine habitats as they undergo ontogenetic migrations, but behaviors used to accomplish these migrations may differ among species, life history stages, or locations. The ecologically and commercially important brown shrimp, Farfantepenaeus aztecus, pink shrimp, Farfantepenaeus duorarum, and white shrimp, Litopenaeus setiferus, undergo ontogenetic migrations between spawning locations on the continental shelf and juvenile nursery habitats in estuaries. This study evaluated the role of endogenous rhythms in vertical swimming activity in Flood Tide Transport (FTT) of postlarvae entering estuaries and the potential for shifts in behavior between the postlarval and juvenile stages. Brown and pink shrimp postlarvae exhibited circatidal rhythms in vertical swimming activity with period lengths of approximately 12.4 h that coincided with the time of early flood tide in the field, whereas white shrimp postlarvae did not exhibit an endogenous rhythm in swimming activity. Pink shrimp juveniles (20-40 mm total length) exhibited a distinct circadian activity rhythm with a mean period length of 23.8 +/- 3.7 h and peak swimming during the time of night in the field. Juvenile brown and white shrimp exhibited relatively weak circatidal activity rhythms with peak vertical swimming around the times of ebb and early flood tide in the field, respectively. These results suggest that 1) brown and pink shrimp postlarvae exhibited endogenous activity rhythms that would enhance FTT, 2) white shrimp postlarvae likely depend on environmental cues associated with flood tide to accomplish FTT, and 3) pink shrimp are unique among these three species in exhibiting a shift from a circatidal to a nocturnal swimming activity rhythm between postlarval and juvenile stages. (C) 2013 Elsevier B.V. All rights reserved. C1 [Ogburn, Matthew B.; Thompson, R. Tyler] Savannah State Univ, Savannah, GA 31404 USA. [Criales, Maria M.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Browder, Joan A.] NOAA, Natl Marine Fisheries Serv, Miami, FL USA. RP Ogburn, MB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ogburnm@si.edu OI Ogburn, Matthew/0000-0001-5417-555X FU United States Department of Commerce; NOAA National Marine Fisheries Service [PL 88-309, 2-296-R]; NOM Living Marine Resources Cooperative Science Center [NA05OAR4811017]; NOM National Marine Fisheries Service Southeast Fisheries Science Center FX Technical assistance was provided by E. Buck, H. Cardenas, T. Jackson, A. Reyes, and I. Zink The manuscript was improved with comments by Z. Darnell, R. Forward, and N. Hawthorne and an anonymous reviewer. Funding for this study was provided by the United States Department of Commerce, NOAA National Marine Fisheries Service, under PL 88-309, Project 2-296-R, NOM Living Marine Resources Cooperative Science Center NA05OAR4811017 and by the NOM National Marine Fisheries Service Southeast Fisheries Science Center as part of the Habitat Conservation Program. [SS] NR 63 TC 5 Z9 5 U1 3 U2 27 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB PY 2013 VL 440 BP 149 EP 155 DI 10.1016/j.jembe.2012.12.007 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 105SJ UT WOS:000316092500021 ER PT J AU Bai, Y Su, M Zhao, Y AF Bai, Yang Su, Meng Zhao, Yue TI Dichromatic dark matter SO JOURNAL OF HIGH ENERGY PHYSICS LA English DT Article DE Beyond Standard Model; Cosmology of Theories beyond the SM ID GALACTIC-CENTER REGION; NEUTRALINO ANNIHILATION; GAMMA-RAYS; 2 PHOTONS; EMISSION; LINE; POSITRONS; RADIATION; SPECTRUM; HALO AB Both the robust INTEGRAL 511 keV gamma-ray line and the recent tentative hint of the 135 GeV gamma-ray line from Fermi-LAT have similar signal morphologies, and may be produced from the same dark matter annihilation. Motivated by this observation, we construct a dark matter model to explain both signals and to accommodate the two required annihilation cross sections that are different by more than six orders of magnitude. In our model, to generate the low-energy positrons for INTEGRAL, dark matter particles annihilate into a complex scalar that couples to photon via a charge-radius operator. The complex scalar contains an excited state decaying into the ground state plus an off-shell photon to generate a pair of positron and electron. Two charged particles with non-degenerate masses are necessary for generating this charge-radius operator. One charged particle is predicted to be long-lived and have a mass around 3.8 TeV to explain the dark matter thermal relic abundance from its late decay. The other charged particle is predicted to have a mass below 1 TeV given the ratio of the two signal cross sections. The 14 TeV LHC will concretely test the main parameter space of this lighter charged particle. C1 [Bai, Yang] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Bai, Yang; Zhao, Yue] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Zhao, Yue] Stanford Univ, Stanford Inst Theoret Phys, Varian Lab, Stanford, CA 94305 USA. [Su, Meng] MIT, Dept Phys, Cambridge, MA 02139 USA. [Su, Meng] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Su, Meng] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Bai, Y (reprint author), Univ Wisconsin, Dept Phys, 1150 Univ Ave, Madison, WI 53706 USA. EM yangbai@physics.wisc.edu; mengsu@space.mit.edu; zhaoyue@slac.stanford.edu RI Su, Meng/J-4211-2013 FU University of Wisconsin, Madison; ITS Department of Energy [DE-AC02-76SF00515]; Aspen Center for Physics, under NSF [1066293]; NASA [PF2-130102, NAS8-03060] FX We would like to thank James Cline, Tim Cohen, Douglas Finkbeiner, JoAnne Hewett, Dan Hooper, Jessie Shelton, Tracy Slatyer, Aaron Vincent and Jay Wacker for useful discussions and comments. YB is supported by start-up funds from the University of Wisconsin, Madison. YB thanks SLAC for their warm hospitality. SLAC is operated by Stanford University for the ITS Department of Energy under contract DE-AC02-76SF00515. We also thank the Aspen Center for Physics, under NSF Grant No. 1066293, where part of this work was completed. Support for the work of M.S. was provided by NASA through Einstein Postdoctoral Fellowship grant number PF2-130102 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 60 TC 6 Z9 6 U1 1 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1029-8479 J9 J HIGH ENERGY PHYS JI J. High Energy Phys. PD FEB PY 2013 IS 2 AR 097 DI 10.1007/JHEP02(2013)097 PG 20 WC Physics, Particles & Fields SC Physics GA 108EE UT WOS:000316273700020 ER PT J AU Toner, BM Lesniewski, RA Marlow, JJ Briscoe, LJ Santelli, CM Bach, W Orcutt, BN Edwards, KJ AF Toner, Brandy M. Lesniewski, Ryan A. Marlow, Jeffrey J. Briscoe, Lindsey J. Santelli, Cara M. Bach, Wolfgang Orcutt, Beth N. Edwards, Katrina J. TI Mineralogy Drives Bacterial Biogeography of Hydrothermally Inactive Seafloor Sulfide Deposits SO GEOMICROBIOLOGY JOURNAL LA English DT Article DE basalts; East Pacific Rise; microbial ecology; mid-ocean ridge; sulfides ID MID-ATLANTIC RIDGE; EAST PACIFIC RISE; MICROBIAL DIVERSITY; GEOCHEMICAL CONSTRAINTS; VENT; ABUNDANCE; CHIMNEY; FIELD; LIFE; MICROORGANISMS AB Mid-ocean ridge hydrothermal venting creates sulfide deposits containing gradients in mineralogy, fluid chemistry, and temperature. Even when hydrothermal circulation ceases, sulfides are known to host microbial communities. The relationship between mineralogy and microbial community composition in low-temperature, rock-hosted systems has not been resolved at any spatial scale, local or global. To examine the hypothesis that geochemistry of seafloor deposits is a dominant parameter driving environmental pressure for bacterial communities at low-temperature, the shared community membership, richness, and structure was measured using 16S rRNA gene sequences. The focus of the study was on hydrothermally inactive seafloor deposits from multiple locations within one deposit (e.g., single extinct chimney), within one vent field (intra-vent field), and among globally distributed vent fields from three ocean basins (inter-vent field). Distinct mineral substrates, such as hydrothermally inactive sulfides versus basalts, host different communities at low temperature in spite of close geographic proximity and contact with the same hydrothermally influenced deep-sea water. Furthermore, bacterial communities inhabiting hydrothermally inactive sulfide deposits from geographically distant locations cluster together in community cladograms to the exclusion of other deep-sea substrates and settings. From this study, we conclude that at low temperature, mineralogy was a more important variable determining microbial community composition than geographic factors. Supplemental materials are available for this article. Go to the publisher's online edition of Geomicrobiology Journal to view the supplemental file. C1 [Toner, Brandy M.; Lesniewski, Ryan A.; Briscoe, Lindsey J.] Univ Minnesota, Dept Soil Water & Climate, St Paul, MN 55108 USA. [Toner, Brandy M.; Marlow, Jeffrey J.; Santelli, Cara M.; Bach, Wolfgang; Edwards, Katrina J.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Santelli, Cara M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Bach, Wolfgang] Univ Bremen, Dept Geosci, D-28359 Bremen, Germany. [Orcutt, Beth N.; Edwards, Katrina J.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. [Orcutt, Beth N.] Aarhus Univ, Ctr Geomicrobiol, Aarhus, Denmark. RP Toner, BM (reprint author), Univ Minnesota, Dept Soil Water & Climate, 1991 Upper Buford Circle, St Paul, MN 55108 USA. EM toner@umn.edu RI Toner, Brandy/N-7911-2016; Bach, Wolfgang/D-3713-2017; OI Toner, Brandy/0000-0002-3681-3455; Bach, Wolfgang/0000-0002-3099-7142; Santelli, Cara/0000-0001-8617-0008 FU NASA Astrobiology Institute [NNA04CC04A]; National Research Council; NASA; RIDGE [OCE-0241791]; CFANS University of Minnesota; Woods Hole Oceanographic Institution's Summer Student Fellow program; DFG-Research Center/Excellence Cluster The Ocean in the Earth System; Danish National Research Foundation; Max Planck Society FX We thank PD Schloss and JA Huber for discussions regarding community comparisons and data treatment; JA Huber and WJ Brazelton for unpublished data; M. Manno and L. Sauer of the University of Minnesota Characterization Facility for assistance with X-ray diffraction; DR Rogers for sample collection. For financial support we thank the NASA Astrobiology Institute (NNA04CC04A); the National Research Council Associate and NASA Postdoctoral Programs (BMT); RIDGE 2000 (OCE-0241791; KJE and WB); CFANS University of Minnesota (BMT); Woods Hole Oceanographic Institution's Summer Student Fellow program (JJM); the DFG-Research Center/Excellence Cluster The Ocean in the Earth System (WB), and the Danish National Research Foundation and the Max Planck Society (BNO). Parts of this work were carried out in the Characterization Facility, University of Minnesota, which receives partial support from NSF through the MRSEC program. NR 45 TC 15 Z9 15 U1 1 U2 43 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0149-0451 J9 GEOMICROBIOL J JI Geomicrobiol. J. PD FEB 1 PY 2013 VL 30 IS 4 BP 313 EP 326 DI 10.1080/01490451.2012.688925 PG 14 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 100EQ UT WOS:000315679400004 ER PT J AU Meech, KJ Kleyna, J Hainaut, OR Lowry, SC Fuse, T A'Hearn, MF Chesley, S Yeomans, DK Fernandez, Y Lisse, C Reach, W Bauer, JM Mainzer, AK Pittichova, J Christensen, E Osip, D Brink, T Mateo, M Motta, V Challis, P Holman, M Ferrin, I AF Meech, K. J. Kleyna, J. Hainaut, O. R. Lowry, S. C. Fuse, T. A'Hearn, M. F. Chesley, S. Yeomans, D. K. Fernandez, Y. Lisse, C. Reach, W. Bauer, J. M. Mainzer, A. K. Pittichova, J. Christensen, E. Osip, D. Brink, T. Mateo, M. Motta, V. Challis, P. Holman, M. Ferrin, I. TI The demise of Comet 85P/Boethin, the first EPOXI mission target SO ICARUS LA English DT Article DE Comets; Data reduction techniques; Image processing ID MULTIBAND IMAGING PHOTOMETER; DEEP-IMPACT; SOLAR-SYSTEM; 9P/TEMPEL-1; SPITZER; JUPITER; NUCLEUS; 1P/HALLEY; CAMPAIGN; SCIENCE AB Comet 85P/Boethin was selected as the original comet target for the Deep Impact extended mission, EPOXI. Because this comet had been only observed at two apparitions in 1975 and 1986 and consequently had a large ephemeris error, an early intense recovery effort similar to that of 1P/Halley was undertaken beginning in 2005 using the ESO Very Large Telescopes (VLTs) in a distant comet program. These were challenging observations because of the low galactic latitude, and an error ellipse (the line of variations) that was larger than the CCD FOV, and the comet was not seen. Dedicated recovery observing time was awarded on the Subaru telescope in April and May 2006, and June 2007, in addition to time on the VLT and Canada France Hawaii telescopes during July August 2007 with wide field mosaics and mosaicing techniques. The limiting V magnitudes from these observing runs ranged between 25.7 and 27.3 and again the comet was not seen in the individual nights. A new image processing technique was developed to stack images over extended runs and runs after distorting them to account for dilations and rotations in the line of variations using modifications of the world coordinate system. A candidate at V 27.3 was found in the CFHT data along the LOV, 2.5' west of the nominal ephemeris position. The EPOXI mission was unwilling to re-target the spacecraft without a confirmation. Additional time was secured using the Spitzer Space Telescope, the Gemini South 8-m telescope, the Clay and Baade (Magellan 6.5 m), CTIO 4 m, and SOAR 4 m telescopes during 2007 September and October A composite image made by stacking the new data showed no plausible candidate nucleus to a limiting magnitude of V = 28.5, corresponding to a nucleus radius between 0.1 and 0.2 km (assuming an albedo of 0.04). The comet was declared lost, presumably having disintegrated. Searches in the WISE data set revealed no debris trail, but no constraints on the possible time of disruption can be made. NASA approved the trajectory correction maneuver to go to Comet 103P/Hartley 2 on 2007 November 1. Many observers searched for the comet as it came to its December 2008 perihelion, but no trace of the nucleus was found. Based on observations collected at the Very Large Telescope, Chile, in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, in part using data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile, in part on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l'Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii, in part using data collected at the Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which are operated by the Association for Research in Astronomy, under contract with the National Science Foundation, and in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This work is also based in part on observations taken with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. (c) 2012 Elsevier Inc. All rights reserved. C1 [Meech, K. J.; Kleyna, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Meech, K. J.; Kleyna, J.] UH NASA Astrobiol Inst, Moffett Field, CA 94035 USA. [Hainaut, O. R.] European So Observ, D-85748 Garching, Germany. [Lowry, S. C.] Univ Kent, Sch Phys Sci, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England. [Fuse, T.] Kashima Space Technol Ctr, Natl Inst Informat & Commun Technol, Kashima, Ibaraki 3148501, Japan. [A'Hearn, M. F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Chesley, S.; Yeomans, D. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fernandez, Y.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. [Lisse, C.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Reach, W.] USRA SOFIA, Moffett Field, CA 94035 USA. [Bauer, J. M.; Mainzer, A. K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Pittichova, J.] Slovak Acad Sci, Astron Inst, Bratislava 84504, Slovakia. [Christensen, E.] Univ Arizona, Catalina Sky Survey Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Osip, D.] Carnegie Inst Sci, Las Campanas Observ, La Serena, Chile. [Brink, T.; Mateo, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Motta, V.] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Challis, P.; Holman, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferrin, I.] Univ Antioquia, Fac Exact & Nat Sci, Inst Phys, Medellin, Colombia. RP Meech, KJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM meech@ifa.hawaii.edu RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Fernandez, Yanga/0000-0003-1156-9721; Reach, William/0000-0001-8362-4094 FU VLT, European Southern Observatory, Chile (ESO Programmes) [279.C-5016, 279.C-5062]; Gemini Observatory [GS-2007B-DD-2]; University of Maryland; University of Hawaii [Z667702]; NASA [NASW-00004]; National Aeronautics and Space Administration; Planetary Science Division of the National Aeronautics and Space Administration; Council for Scientific Development of the University of the Andes [C-1281-04-05-B]; UK Particle Physics and Astronomy Research Council FX This is based in part on observations collected at the VLT, European Southern Observatory, Chile (ESO Programmes 279.C-5016 and 279.C-5062), and in part on observations obtained at the Gemini Observatory (program GS-2007B-DD-2), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministrio da Cincia e Tecnologia (Brazil) and SECYT (Argentina). Image processing in this paper has been performed using the MIDAS software, developed by the European Southern Observatory, and is distributed with a general public license, and in part using the IRAF program. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. Support for this work was provided in part through University of Maryland and University of Hawaii subcontract Z667702, which was awarded under prime contract NASW-00004 from NASA (K.J.M., J.P., and C.M.L.), conducted in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (S.C. and D.K.Y.). Support for the work (C.M.L. and W.T.R.) was provided by NASA through an award issued by JPL/Caltech. This research made use of Tiny Tim/ Spitzer, developed by J.E. Krist for the Spitzer Space Center. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of the National Aeronautics and Space Administration. IF would like to thank the Council for Scientific Development of the University of the Andes, for their support through Grant C-1281-04-05-B, and S.C.L. acknowledges support from the UK Particle Physics and Astronomy Research Council. We would like to especially thank (1) the observatory directors who allocated director's time: M. Hayashi (Subaru), C. Cesarsky and T. de Zeeuw (ESO-V.L.T.), D. Simons and J.-R. Roy (Gemini), A. Walker (CTIO), S. Heathcote (SOAR); (2) the Observatory Science Operations Heads who were instrumental in helping execute our programs: P. Martin (Canada-France Telescope) and B. Rodgers (Gemini S.). Additionally we want to thank the observatory staff who helped with the observing: M. Takami and M. Ishii (Subaru), D. Maturana, L. Fraga and S. Points (SOAR). We would also like to thank J. Johnson and N. Cabrera who obtained UH2.2m images for us that enabled us to discount the spurious recovery report during July 2008. NR 43 TC 1 Z9 1 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 2013 VL 222 IS 2 SI SI BP 662 EP 678 DI 10.1016/j.icarus.2012.09.002 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 099ZZ UT WOS:000315665800022 ER PT J AU Lisse, CM Christian, DJ Wolk, SJ Dennerl, K Bodewits, D Combi, MR Lepri, ST Zurbuchen, TH Li, JY Dello-Russo, N Belton, MJS Knight, MM AF Lisse, C. M. Christian, D. J. Wolk, S. J. Dennerl, K. Bodewits, D. Combi, M. R. Lepri, S. T. Zurbuchen, T. H. Li, J. Y. Dello-Russo, N. Belton, M. J. S. Knight, M. M. TI Chandra ACIS-S imaging spectroscopy of anomalously faint X-ray emission from Comet 103P/Hartley 2 during the EPOXI encounter SO ICARUS LA English DT Article DE Comets; Solar wind; Spectroscopy ID EXTREME-ULTRAVIOLET EMISSION; SOLAR-WIND IONS; CHARGE-EXCHANGE; HALE-BOPP; VOLATILE COMPOSITION; PLASMA ENVIRONMENT; WATER PRODUCTION; DUSTY COMETARY; HOT GAS; SYSTEM AB We present results from the Chandra X-ray Observatory's characterization of the X-ray emission from Comet 103P/Hartley 2, in support of NASA's Deep Impact Extended close flyby of the comet on 04 November 2010. The comet was observed 4 times for a total on target time of similar to 60 ks between the 17th of October and 16th of November 2010, with two of the visits occurring during the EPOXI close approach on 04 November and 05 November 2010. X-ray emission from 103P was qualitatively similar to that observed for collisionally thin Comets 2P/Encke (Lisse, C.M. et al. [2005]. Astrophys. J. 635, 1329-1347) and 9P/Tempel 1 (Lisse, C.M. et al. [2007]. Icarus 190, 391-405). Emission morphology offset sunward but asymmetrical from the nucleus and emission lines produced by charge exchange between highly stripped C, N, and O solar wind minor ions and coma neutral gas species were found. The comet was very under-luminous in the X-ray at all times, representing the 3rd faintest comet ever detected (L-x = 1.1 +/- 0.3 x 10(14) erg s(-1)). The coma was collisionally thin to the solar wind at all times, allowing solar wind ions to flow into the inner coma and interact with the densest neutral coma gas. Localization of the X-ray emission in the regions of the major rotating gas jets was observed, consistent with the major source of cometary neutral gas species being icy coma dust particles. Variable spectral features due to changing solar wind flux densities and charge states were also seen. Modeling of the Chandra observations from the first three visits using observed gas production rates and ACE solar wind ion fluxes with a charge exchange mechanism for the emission is consistent with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma. The X-ray emission during the 4th visit on 16 November 2010 is similar to the unusual behavior seen for Comet 17P/Holmes in 2007 (Christian, D.J. et al. [2010]. Astrophys. J. Suppl. 187, 447-459) as the solar wind became dominated by a less ionized and faster plasma, more typical of outflow from polar coronal hole regions. We postulate that the overall faintness of the comet seen during all visits is due to the unusually well mixed dust and gas content of this hyperactive comet's coma producing Auger electrons rather than X-rays via charge exchange with the solar wind. An alternative possible explanation for the faintness of the comet's X-ray emission, and its unusual high CV and unusually low CVI emission, is that the impinging solar wind was drastically slowed in the inner coma, below 150 km s(-1), before charge exchanging with cometary neutrals. (c) 2012 Elsevier Inc. All rights reserved. C1 [Lisse, C. M.; Dello-Russo, N.; Knight, M. M.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Christian, D. J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. [Dennerl, K.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Bodewits, D.; Li, J. Y.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Combi, M. R.; Lepri, S. T.; Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Belton, M. J. S.] Belton Space Explorat Initiat, Tucson, AZ 85716 USA. [Knight, M. M.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Lisse, CM (reprint author), Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM carey.lisse@jhuapl.edu; damian.christian@csun.e-du; swolk@cfa.harvard.edu; kod@mpe.mpg.de; dennis@astro.umd.edu; mcombi@umich.edu; slepri@umich.edu; thomasz@umich.edu; jyli@as-tro.umd.edu; neil.dellorusso@jhuapl.edu; mbelton@dako-tacom.net; knight@lowell.edu RI Combi, Michael/J-1697-2012; Lepri, Susan/I-8611-2012; Dello Russo, Neil/G-2727-2015; Lisse, Carey/B-7772-2016; OI Combi, Michael/0000-0002-9805-0078; Dello Russo, Neil/0000-0002-8379-7304; Lisse, Carey/0000-0002-9548-1526; Knight, Matthew/0000-0003-2781-6897; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020 FU National Aeronautics and Space Administration through Chandra Award [GO1-12011A]; National Aeronautics Space Administration [NAS8-03060]; ACE Project [44A-1085637]; NSF Grant [AST 0707283]; NASA PATM Grant [NNX09AB58G] FX C.M. Lisse gratefully acknowledges support for this work provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-12011A issued by the Chandra X-ray Observatory Center (CXC). The CXC is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under Contract NAS8-03060. We would also like to thank the ACE Project, mission Grant 44A-1085637 for providing support for S.T Lepri to produce ACE trending data during the Chandra observations. M. Combi acknowledges support from NSF Grant AST 0707283 and NASA PATM Grant NNX09AB58G. NR 78 TC 3 Z9 3 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD FEB PY 2013 VL 222 IS 2 SI SI BP 752 EP 765 DI 10.1016/j.icarus.2012.09.025 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 099ZZ UT WOS:000315665800030 ER PT J AU Hagedorn, M Farrell, A Carter, VL AF Hagedorn, Mary Farrell, Ann Carter, Virginia L. TI Cryobiology of coral fragments SO CRYOBIOLOGY LA English DT Article DE Coral fragments; Cryobiology; Chilling; Zooxanthellae; Pocillopora damicornis ID CLIMATE-CHANGE; REEF CRISIS; CONSERVATION; TEMPERATURE; STRESS; MEMBRANES; DECLINE; DAMAGE; SPERM; MODEL AB Around the world, coral reefs are dying due to human influences, and saving habitat alone may not stop this destruction. This investigation focused on the biological processes that will provide the first steps in understanding the cryobiology of whole coral fragments. Coral fragments are a partnership of coral tissue and endosymbiotic algae, Symbiodinium sp., commonly called zooxanthellae. These data reflected their separate sensitivities to chilling and a cryoprotectant (dimethyl sulfoxide) for the coral Pocillopora damicornis, as measured by tissue loss and Pulse Amplitude Modulated fluorometry 3 weeks post-treatment. Five cryoprotectant treatments maintained the viability of the coral tissue and zooxanthellae at control values (1 M dimethyl sulfoxide at 1.0, 1.5 and 2.0 h exposures, and 1.5 M dimethyl sulfoxide at 1.0 and 1.5 h exposures, P > 0.05, ANOVA), whereas 2 M concentrations did not (P < 0.05, ANOVA). A seasonal response to chilling was observed in the coral tissue, but not in the zooxanthellae. During the winter when the fragments were chilled, the coral tissue remained relatively intact (similar to 25% loss) post-treatment, but the zooxanthellae numbers in the tissue declined after 5 min of chilling (P < 0.05, ANOVA). However, in the late spring, coral tissue (similar to 75% loss) and zooxanthellae numbers declined in response to chilling alone (P < 0.05, ANOVA). When a cryoprotectant (1 M dimethyl sulfoxide) was used in concert with chilling it protected the coral against tissue loss after 45 min of cryoprotectant exposure (P > 0.05, ANOVA), but it did not protect against the loss of zooxanthellae (P < 0.05, ANOVA). The zooxanthellae are the most sensitive element in the coral fragment complex and future cryopreservation protocols must be guided by their greater sensitivity. (c) 2012 Elsevier Inc. All rights reserved. C1 [Hagedorn, Mary; Farrell, Ann; Carter, Virginia L.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC 20008 USA. [Hagedorn, Mary; Farrell, Ann; Carter, Virginia L.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI 96744 USA. RP Hagedorn, M (reprint author), Hawaii Inst Marine Biol, Smithsonian Inst, 46-007 Lilipuna Rd, Kaneohe, HI 96744 USA. EM hagedornm@si.edu FU Anela Kolohe Foundation; Taronga Conservation Society Australia FX These experiments were funded through Grants from the Anela Kolohe Foundation and the Taronga Conservation Society Australia.; These experiments were funded through Grants from the Anela Kolohe Foundation and the Taronga Conservation Society Australia. We would like to thank Nikolas Zuchowicz and Erika Johnston for their comments on this manuscript, and the Gates Laboratory for the loan of the Diving PAM for these experiments. This manuscript has been approved for publication by the Hawaii Institute of Marine Biology as contribution # 1517. NR 33 TC 6 Z9 6 U1 3 U2 27 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD FEB PY 2013 VL 66 IS 1 BP 17 EP 23 DI 10.1016/j.cryobiol.2012.10.003 PG 7 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 098IY UT WOS:000315544100004 PM 23142722 ER PT J AU Orr, CM Tocheri, MW Burnett, SE Awe, RD Saptomo, EW Sutikna, T Jatmiko Wasisto, S Morwood, MJ Jungers, WL AF Orr, Caley M. Tocheri, Matthew W. Burnett, Scott E. Awe, Rokus Due Saptomo, E. Wahyu Sutikna, Thomas Jatmiko Wasisto, Sri Morwood, Michael J. Jungers, William L. TI New wrist bones of Homo floresiensis from Liang Bua (Flores, Indonesia) SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Hominin evolution; Carpal morphology; Cretinism; Australopithecus; Neandertals ID AUSTRALOPITHECUS-AFARENSIS; EASTERN INDONESIA; HOMININ EVOLUTION; LATE PLEISTOCENE; HADAR FORMATION; FOSSIL EVIDENCE; LARON-SYNDROME; OLDUVAI GORGE; TOOL BEHAVIOR; BODY-SIZE AB The carpals from the Homo floresiensis type specimen (LB1) lack features that compose the shared, derived complex of the radial side of the wrist in Neandertals and modern humans. This paper comprises a description and three-dimensional morphometric analysis of new carpals from at least one other individual at Liang Bua attributed to H. floresiensis: a right capitate and two hamates. The new capitate is smaller than that of LB1 but is nearly identical in morphology. As with capitates from extant apes, species of Australopithecus, and LB1, the newly described capitate displays a deeply-excavated nonarticular area along its radial aspect, a scaphoid facet that extends into a J-hook articulation on the neck, and a more radially-oriented second metacarpal facet; it also lacks an enlarged palmarly-positioned trapezoid facet. Because there is no accommodation for the derived, palmarly blocky trapezoid that characterizes Homo sapiens and Neandertals, this individual most likely had a plesiomorphically wedge-shaped trapezoid (like LB1). Morphometric analyses confirm the close similarity of the new capitate and that of LB1, and are consistent with previous findings of an overall primitive articular geometry. In general, hamate morphology is more conserved across hominins, and the H. floresiensis specimens fall at the far edge of the range of variation for H. sapiens in a number of metrics. However, the hamate of H. floresiensis is exceptionally small and exhibits a relatively long, stout hamulus lacking the oval-shaped cross-section characteristic of human and Neandertal hamuli (variably present in australopiths). Documentation of a second individual with primitive carpal anatomy from Liang Bua, along with further analysis of trapezoid scaling relative to the capitate in LB1, refutes claims that the wrist of the type specimen represents a modern human with pathology. In total, the carpal anatomy of H. floresiensis supports the hypothesis that the lineage leading to the evolution of this species originated prior to the cladogenetic event that gave rise to modern humans and Neandertals. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Orr, Caley M.; Jungers, William L.] SUNY Stony Brook, Dept Anat Sci, Hlth Sci Ctr T 8 040, Stony Brook, NY 11794 USA. [Tocheri, Matthew W.] Smithsonian Inst, Human Origins Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Burnett, Scott E.] Eckerd Coll, Comparat Cultures Coll, St Petersburg, FL 33711 USA. [Awe, Rokus Due; Saptomo, E. Wahyu; Sutikna, Thomas; Jatmiko; Wasisto, Sri] Plata Arkeol Nas, Jakarta 12510, Indonesia. [Morwood, Michael J.] Univ Wollongong, Sch Earth & Environm Sci, GeoQuEST Res Ctr, Wollongong, NSW, Australia. RP Orr, CM (reprint author), SUNY Stony Brook, Dept Anat Sci, Hlth Sci Ctr T 8 040, Stony Brook, NY 11794 USA. EM caley.orr@gmail.com OI Tocheri, Matthew/0000-0001-7600-8998 FU Smithsonian Institution Scholarly Studies Grant Program Award; Smithsonian Institution Postdoctoral Research Fellowship; Australian Research Council; University of New England FX Funding for the analysis of the new Homo floresiensis carpal remains was provided by a Smithsonian Institution Scholarly Studies Grant Program Award (MWT) and a Smithsonian Institution Postdoctoral Research Fellowship (CMO). The excavations of Sectors VII and XI at Liang Bua were funded by a Discovery Project Grant from the Australian Research Council (MJM) and grants from the University of New England (MJM). We thank the following individuals and institutions for curatorial assistance and access to specimens in their care: Eileen Westwig (American Museum of Natural History), William Kimbel and Donald Johanson (Arizona State University's Institute of Human Origins), Emma Mbua (National Museum of Nairobi), Richard Thorington, Richard Potts, David Hunt and Linda Gordon (National Museum of Natural History), Judith Chupasko (Museum of Comparative Zoology), Emmanuel Gilissen and Wim Wendelen (Royal Museum for Central Africa), Patrick Semal and Georges Lenglet (Royal Belgian Institute of Natural Sciences), Erik Trinkaus (Washington University in St. Louis), Tony Djubiantono (National Research and Development Center for Archaeology in Indonesia), and Ned Gilmore (Academy of Natural Sciences in Philadelphia). In addition, we thank Jessica Arrott who kindly provided assistance with data collection. Finally, we appreciate the many helpful comments and suggestions provided by the editor (Mark Teaford), the associate editor, and the anonymous reviewers. NR 102 TC 24 Z9 25 U1 7 U2 75 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD FEB PY 2013 VL 64 IS 2 BP 109 EP 129 DI 10.1016/j.jhevol.2012.10.003 PG 21 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 100AC UT WOS:000315666100001 PM 23290261 ER PT J AU Birnstiel, T Dullemond, CP Pinilla, P AF Birnstiel, T. Dullemond, C. P. Pinilla, P. TI Lopsided dust rings in transition disks SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: pre-main sequence; planets and satellites: formation; submillimeter: planetary systems; circumstellar matter ID TURBULENT PROTOPLANETARY DISKS; PLANETESIMAL FORMATION; SNOW LINE; MAGNETOROTATIONAL TURBULENCE; SOLAR NEBULA; GROWTH; PARTICLES; EVOLUTION; VORTICES; SOLIDS AB Context. Particle trapping in local or global pressure maxima in protoplanetary disks is one of the new paradigms in the theory of the first stages of planet formation. However, finding observational evidence for this effect is not easy. Recent work suggests that the large ring-shaped outer disks observed in transition disk sources may in fact be lopsided and constitute large banana-shaped vortices. Aims. We wish to investigate how effectively dust can accumulate along the azimuthal direction. We also want to find out if the size-sorting resulting from this accumulation can produce detectable signatures at millimeter wavelengths. Methods. To keep the numerical cost under control we developed a 1 + 1D method in which the azimuthal variations are treated separately from the radial variations. The azimuthal structure was calculated analytically for a steady-state between mixing and azimuthal drift. We derived equilibration time scales and compared the analytical solutions to time-dependent numerical simulations. Results. We found that weak, but long-lived azimuthal density gradients in the gas can induce very strong azimuthal accumulations of dust. The strength of the accumulations depends on the Peclet number, which describes the relative importance of advection and diffusion. We applied our model to transition disks and our simulated observations show that this effect would be easily observable with the Atacama Large Millimeter / submillimeter Array (ALMA) and could be used to put constraints on the strength of turbulence and the local gas density. C1 [Birnstiel, T.] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dullemond, C. P.; Pinilla, P.] Heidelberg Univ, Inst Theoret Astrophys, Ctr Astron ZAH, D-69120 Heidelberg, Germany. RP Birnstiel, T (reprint author), Tech Univ Munich, Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. EM tbirnstiel@cfa.harvard.edu OI Dullemond, Cornelis/0000-0002-7078-5910; Birnstiel, Tilman/0000-0002-1899-8783 NR 44 TC 56 Z9 56 U1 4 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2013 VL 550 AR L8 DI 10.1051/0004-6361/201220847 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089AJ UT WOS:000314879700146 ER PT J AU Liu, FC Parise, B Wyrowski, F Zhang, Q Gusten, R AF Liu, F. -C. Parise, B. Wyrowski, F. Zhang, Q. Guesten, R. TI Water deuterium fractionation in the high-mass hot core G34.26+0.15 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: massive; stars: protostars; HII regions; ISM: molecules ID STAR-FORMING REGIONS; H-II-REGIONS; MOLECULAR LINE EMISSION; GRAIN SURFACE-CHEMISTRY; DEUTERATED WATER; COLLISIONAL EXCITATION; ROTATIONAL-EXCITATION; HERSCHEL OBSERVATIONS; PHYSICAL-PROPERTIES; PROTOSTELLAR CORES AB Context. Water is an essential molecule in oxygen chemistry and the main constituent of grain icy mantles. The formation of water can be studied through the HDO/H2O ratio. Thanks to the launch of the Herschel satellite and the advance of sensitive submillimeter receivers on ground telescopes, many H2O and HDO transitions can now be observed, enabling more accurate studies of the level of water fractionation. Aims. Using these new technologies, we aim at revisiting the water fractionation studies toward massive star-forming regions. We present here a detailed study toward G34.26+0.15, a massive star-forming region associated with compact HII regions. Methods. We present observations of five HDO lines obtained with the APEX telescope. Two of those transitions are ground-state transitions. Two of the three high-excitation lines were additionally observed at higher angular resolution with the SMA. We analyzed these observations using the 1D radiative transfer code RATRAN and adopting different physical profiles from two different models. Results. Although the inner and outer fractional abundances relative to H-2 can be best constrained to be X-in(HDO) (T > 100 K) = (5-7) x 10(-8)(3 sigma) and X-out(HDO) (T <= 100 K) = (0.3-2) x 10(-11)(3 sigma), the line profile of the 893 GHz ground transition cannot be well reproduced. This line profile is shown to be very sensitive to the velocity field. To better constrain the velocity field, it is necessary to observe the HDO line at 893 GHz with high angular resolution. The H2O abundance is deduced from one high-excitation and one ground transition (H2O)-O-18 line. The D/H ratios of water are 3.0 x 10(-4) in the inner region and (1.9-4.9) x 10(-4) in the outer region of the core. The HDO fractional abundance in the inner and outer regions are different by more than four orders, which implies that the sublimation is very similar in low-and high-mass protostars. The D/H ratios of water in G34.26 + 0.15 are close to the value obtained for the same source in a previous study, and similar to those in other high-mass sources, but lower than those in low-mass protostars, suggesting the possibility that the dense and cold pre-collapse phase is shorter for high-mass star-forming regions. C1 [Liu, F. -C.; Parise, B.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, FC (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM fliu@mpifr-bonn.mpg.de OI Zhang, Qizhou/0000-0003-2384-6589 FU German Deutsche Forschungsgemeinschaft, DFG Emmy Noether project [PA1692/1-1] FX The authors warmly thank the anonymous referee and M. Walmsley for very constructive comments and suggestions, which greatly improved this paper. We are grateful to R. Rolffs for many fruitful discussions as well as to F. Herpin for some interesting ideas. We also would like to thank M. Hogerheijde and F. van der Tak for their help in dealing with RATRAN. The authors are grateful to the WISH team for providing access to the H2O data. F.-C. Liu and B. Parise are funded by the German Deutsche Forschungsgemeinschaft, DFG Emmy Noether project number PA1692/1-1. NR 70 TC 3 Z9 3 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2013 VL 550 AR A37 DI 10.1051/0004-6361/201219905 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089AJ UT WOS:000314879700037 ER PT J AU Schneider, PC Eisloffel, J Gudel, M Gunther, HM Herczeg, G Robrade, J Schmitt, JHMM AF Schneider, P. C. Eisloeffel, J. Guedel, M. Guenther, H. M. Herczeg, G. Robrade, J. Schmitt, J. H. M. M. TI HST FUV C IV observations of the hot DG Tauri jet SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: winds, outflows; stars: pre-main sequence; ISM: jets and outflows; ultraviolet: stars; stars: individual: DG Tauri ID HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; STARS; ACCRETION; KINEMATICS; DISCOVERY; OBJECTS; LINES; SHOCK AB Protostellar jets are tightly connected to the accretion process and regulate the angular momentum balance of accreting star-disk systems. The DG Tau jet is one of the best-studied protostellar jets and contains plasma with temperatures ranging over three orders of magnitude within the innermost 50AU of the jet. We present new Hubble Space Telescope (HST) far-ultraviolet (FUV) long-slit spectra spatially resolving the C IV emission (T similar to 10(5) K) from the jet for the first time, in addition to quasi-simultaneous HST observations of optical forbidden emission lines ([O I], [N II], [S II], and [O III]) and fluorescent H-2 lines. The C iv emission peaks at approximate to 42AU from the stellar position and has a FWHM of approximate to 52AU along the jet. Its deprojected velocity of around 200 km s(-1) decreases monotonically away from the driving source. In addition, we compare our HST data with the X-ray emission from the DG Tau jet. We investigate the requirements to explain the data by an initially hot jet compared to local heating. Both scenarios indicate a mass loss by the T similar to 10(5) K jet of similar to 10(-9) M-circle dot yr(-1), i.e., between the values for the lower temperature jet (T approximate to 10(4) K) and the hotter X- ray emitting part (T greater than or similar to 10(6) K). However, a simple initially hot wind requires a large launching region (similar to 1 AU), and we therefore favor local heating. C1 [Schneider, P. C.; Robrade, J.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Eisloeffel, J.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Guedel, M.] Univ Vienna, A-1010 Vienna, Austria. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herczeg, G.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Schneider, PC (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM cschneider@hs.uni-hamburg.de RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Gunther, Hans Moritz/0000-0003-4243-2840 FU DLR [50OR1112]; NASA through Chandra Award [GO1-12067X, NAS8-03060] FX P.C.S. is supported by the DLR under grant 50OR1112. HMG is supported by NASA through Chandra Award Number GO1-12067X on behalf of NASA under contract NAS8-03060. This paper is based on observations made with the NASA/ESA Hubble Space Telescope. NR 29 TC 13 Z9 13 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2013 VL 550 AR L1 DI 10.1051/0004-6361/201118592 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089AJ UT WOS:000314879700139 ER PT J AU Yatawatta, S de Bruyn, AG Brentjens, MA Labropoulos, P Pandey, VN Kazemi, S Zaroubi, S Koopmans, LVE Offringa, AR Jelic, V Rubi, OM Veligatla, V Wijnholds, SJ Brouw, WN Bernardi, G Ciardi, B Daiboo, S Harker, G Mellema, G Schaye, J Thomas, R Vedantham, H Chapman, E Abdalla, FB Alexov, A Anderson, J Avruch, IM Batejat, F Bell, ME Bell, MR Bentum, M Best, P Bonafede, A Bregman, J Breitling, F van de Brink, RH Broderick, JW Bruggen, M Conway, J de Gasperin, F de Geus, E Duscha, S Falcke, H Fallows, RA Ferrari, C Frieswijk, W Garrett, MA Griessmeier, JM Gunst, AW Hassall, TE Hessels, JWT Hoeft, M Iacobelli, M Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P Mann, G McKean, JP Mevius, M Mol, JD Munk, H Nijboer, R Noordam, JE Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Rottgering, HJA Sluman, J Smirnov, O Stappers, B Steinmetz, M Tagger, M Tang, Y Tasse, C ter Veen, S Vermeulen, R van Weeren, RJ Wise, M Wucknitz, O Zarka, P AF Yatawatta, S. de Bruyn, A. G. Brentjens, M. A. Labropoulos, P. Pandey, V. N. Kazemi, S. Zaroubi, S. Koopmans, L. V. E. Offringa, A. R. Jelic, V. Rubi, O. Martinez Veligatla, V. Wijnholds, S. J. Brouw, W. N. Bernardi, G. Ciardi, B. Daiboo, S. Harker, G. Mellema, G. Schaye, J. Thomas, R. Vedantham, H. Chapman, E. Abdalla, F. B. Alexov, A. Anderson, J. Avruch, I. M. Batejat, F. Bell, M. E. Bell, M. R. Bentum, M. Best, P. Bonafede, A. Bregman, J. Breitling, F. van de Brink, R. H. Broderick, J. W. Brueggen, M. Conway, J. de Gasperin, F. de Geus, E. Duscha, S. Falcke, H. Fallows, R. A. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. M. Gunst, A. W. Hassall, T. E. Hessels, J. W. T. Hoeft, M. Iacobelli, M. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. Mann, G. McKean, J. P. Mevius, M. Mol, J. D. Munk, H. Nijboer, R. Noordam, J. E. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. J. A. Sluman, J. Smirnov, O. Stappers, B. Steinmetz, M. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Vermeulen, R. van Weeren, R. J. Wise, M. Wucknitz, O. Zarka, P. TI Initial deep LOFAR observations of epoch of reionization windows I. The north celestial pole SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dark ages, reionization, first stars; instrumentation: interferometers; techniques: interferometric; methods: data analysis ID SKY SURVEY; RADIO; FOREGROUNDS; TOMOGRAPHY; ALGORITHM; LATITUDE; FIELDS; ARRAY; MHZ AB Aims. The aim of the LOFAR epoch of reionization (EoR) project is to detect the spectral fluctuations of the redshifted HI 21 cm signal. This signal is weaker by several orders of magnitude than the astrophysical foreground signals and hence, in order to achieve this, very long integrations, accurate calibration for stations and ionosphere and reliable foreground removal are essential. Methods. One of the prospective observing windows for the LOFAR EoR project will be centered at the north celestial pole (NCP). We present results from observations of the NCP window using the LOFAR highband antenna (HBA) array in the frequency range 115 MHz to 163 MHz. The data were obtained in April 2011 during the commissioning phase of LOFAR. We used baselines up to about 30 km. The data was processed using a dedicated processing pipeline which is an enhanced version of the standard LOFAR processing pipeline. Results. With about 3 nights, of 6 h each, effective integration we have achieved a noise level of about 100 mu Jy/PSF in the NCP window. Close to the NCP, the noise level increases to about 180 mu Jy/PSF, mainly due to additional contamination from unsubtracted nearby sources. We estimate that in our best night, we have reached a noise level only a factor of 1.4 above the thermal limit set by the noise from our Galaxy and the receivers. Our continuum images are several times deeper than have been achieved previously using the WSRT and GMRT arrays. We derive an analytical explanation for the excess noise that we believe to be mainly due to sources at large angular separation from the NCP. We present some details of the data processing challenges and how we solved them. Conclusions. Although many LOFAR stations were, at the time of the observations, in a still poorly calibrated state we have seen no artefacts in our images which would prevent us from producing deeper images in much longer integrations on the NCP window which are about to commence. The limitations present in our current results are mainly due to sidelobe noise from the large number of distant sources, as well as errors related to station beam variations and rapid ionospheric phase fluctuations acting on bright sources. We are confident that we can improve our results with refined processing. C1 [de Bruyn, A. G.; Kazemi, S.; Zaroubi, S.; Koopmans, L. V. E.; Offringa, A. R.; Jelic, V.; Rubi, O. Martinez; Veligatla, V.; Bernardi, G.; Daiboo, S.; Thomas, R.; Vedantham, H.; Avruch, I. M.; Mevius, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Yatawatta, S.; de Bruyn, A. G.; Brentjens, M. A.; Labropoulos, P.; Pandey, V. N.; Wijnholds, S. J.; Brouw, W. N.; Bentum, M.; Bregman, J.; van de Brink, R. H.; de Geus, E.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Griessmeier, J. M.; Gunst, A. W.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; McKean, J. P.; Mevius, M.; Mol, J. D.; Munk, H.; Nijboer, R.; Noordam, J. E.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Vermeulen, R.; van Weeren, R. J.; Wise, M.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Ciardi, B.; Bell, M. R.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Harker, G.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Mellema, G.] Stockholm Univ, AlbaNova, Dept Astron, S-10691 Stockholm, Sweden. [Mellema, G.] Stockholm Univ, AlbaNova, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Schaye, J.; Garrett, M. A.; Iacobelli, M.; Pandey-Pommier, M.; Rottgering, H. J. A.; van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Tasse, C.; Zarka, P.] Observ Paris, F-92195 Meudon, France. [Hessels, J. W. T.; van Leeuwen, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Anderson, J.; Kramer, M.; Kuniyoshi, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Astrophys, D-53010 Bonn, Germany. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, Sch Phys A28, Sydney, NSW 2006, Australia. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.] Jacobs Univ Bremen, D-28759 Bremen, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Bell, M. E.; Broderick, J. W.; Hassall, T. E.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Hoeft, M.] Tautenburg Observ, Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.; Orru, E.; ter Veen, S.] Radboud Univ Nijmegen, Fac NWI, NL-6500 GL Nijmegen, Netherlands. [Griessmeier, J. M.; Tagger, M.] CNRS, F-75794 Paris 16, France. [Hassall, T. E.; Kramer, M.; Stappers, B.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Karastergiou, A.] Univ Oxford, Oxford OX1 2JD, England. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Smirnov, O.] Rhodes Univ, RATT, Dep Phys & Elect, ZA-6140 Grahamstown, South Africa. [Wucknitz, O.] Argelander Inst Astron, D-53121 Bonn, Germany. [Chapman, E.; Abdalla, F. B.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Batejat, F.; Conway, J.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Paas, H.] Univ Groningen, CIT, NL-9700 AV Groningen, Netherlands. [Offringa, A. R.] RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. RP Yatawatta, S (reprint author), ASTRON, POB 2, NL-7990 AA Dwingeloo, Netherlands. EM yatawatta@astron.nl RI Tagger, Michel/O-6615-2014; Jelic, Vibor/B-2938-2014; Mellema, Garrelt/K-4962-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Falcke, Heino/H-5262-2012; Yatawatta, Sarod/E-6037-2013; OI de Gasperin, Francesco/0000-0003-4439-2627; Abdalla, Filipe/0000-0003-2063-4345; van Weeren, Reinout/0000-0002-0587-1660; Schaye, Joop/0000-0002-0668-5560; Tagger, Michel/0000-0003-2962-3220; Jelic, Vibor/0000-0002-6034-8610; Mellema, Garrelt/0000-0002-2512-6748; Kondratiev, Vladislav/0000-0001-8864-7471; Falcke, Heino/0000-0002-2526-6724; Yatawatta, Sarod/0000-0001-5619-4017; Harker, Geraint/0000-0002-7894-4082 FU Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX LOFAR, designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. Chiara Ferrari acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. NR 29 TC 57 Z9 57 U1 0 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD FEB PY 2013 VL 550 AR A136 DI 10.1051/0004-6361/201220874 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 089AJ UT WOS:000314879700136 ER PT J AU Sargis, EJ Woodman, N Reese, AT Olson, LE AF Sargis, Eric J. Woodman, Neal Reese, Aspen T. Olson, Link E. TI Using hand proportions to test taxonomic boundaries within the Tupaia glis species complex (Scandentia, Tupaiidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE digits; manus; morphology; postcranium; rays; skeleton; Southeast Asia; treeshrews ID COMMON TREE SHREW; PHYLOGENETIC IMPLICATIONS; FUNCTIONAL-MORPHOLOGY; TREESHREWS MAMMALIA; SORICIDAE; PLESIADAPIFORMS; DIVERSIFICATION; BIODIVERSITY; GUATEMALA; CRYPTOTIS AB Treeshrews (order Scandentia) comprise 2 families of squirrel-sized terrestrial, arboreal, and scansorial mammals distributed throughout much of tropical South and Southeast Asia. The last comprehensive taxonomic revision of treeshrews was published in 1913, and a well-supported phylogeny clarifying relationships among all currently recognized extant species within the order has only recently been published. Within the family Tupaiidae, 2 widely distributed species, the northern treeshrew, Tupaia belangeri (Wagner, 1841), and the common treeshrew, T. glis (Diard, 1820), represent a particularly vexing taxonomic complex. These 2 species are currently distinguished primarily based on their respective distributions north and south of the Isthmus of Kra on the Malay Peninsula and on their different mammae counts. This problematic species complex includes 54 published synonyms, many of which represent putative island endemics. The widespread T. glis and T. belangeri collectively comprise a monophyletic assemblage representing the sister lineage to a clade composed of the golden-bellied treeshrew, T. chrysogaster Miller, 1903 (Mentawai Islands), and the long-footed treeshrew, T. longipes (Thomas, 1893) (Borneo). As part of a morphological investigation of the T. glis T. belangeri complex, we studied the proportions of hand bones, which have previously been shown to be useful in discriminating species of soricids (true shrews). We measured 38 variables from digital X-ray images of 148 museum study skins representing several subspecies of T. glis, T. belangeri, T. chrysogaster, and T. longipes and analyzed these data using principal components and cluster analyses. Manus proportions among these 4 species readily distinguish them, particularly in the cases of T. chrysogaster and T. longipes. We then tested the distinctiveness of several of the populations comprising T. glis and T. longipes. T. longipes longipes and T. l. salatana Lyon, 1913, are distinguishable from each other, and populations of T. "glis" from Bangka Island and Sumatra are distinct from those on the Malay Peninsula, supporting the recognition of T. salatana, T. discolor Lyon, 1906, and T. ferruginea Raffles, 1821 as distinct species in Indonesia. These relatively small, potentially vulnerable treeshrew populations occur in the Sundaland biodiversity hotspot and will require additional study to determine their appropriate conservation status. C1 [Sargis, Eric J.] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Sargis, Eric J.; Reese, Aspen T.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Sargis, Eric J.; Reese, Aspen T.] Yale Peabody Museum Nat Hist, Div Vertebrate Zool, New Haven, CT 06520 USA. [Woodman, Neal] Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. [Olson, Link E.] Univ Alaska Fairbanks, Univ Alaska Museum, Fairbanks, AK 99775 USA. RP Sargis, EJ (reprint author), Yale Univ, Dept Anthropol, POB 208277, New Haven, CT 06520 USA. EM eric.sargis@yale.edu OI Woodman, Neal/0000-0003-2689-7373 FU National Science Foundation [DEB-0542532/0542725]; Alaska EPSCoR grant; United States Geological Survey's Patuxent Wildlife Research Center; Yale Institute for Biospheric Studies FX This research was supported by National Science Foundation grant DEB-0542532/0542725 and an Alaska EPSCoR grant to EJS and LEO. Additional support was provided to NW from the United States Geological Survey's Patuxent Wildlife Research Center. We are grateful to S. Raredon, Division of Fishes, Museum Support Center, USNM, for help with the digital X-ray system. This manuscript was completed when LEO was supported by an Edward P. Bass Distinguished Visiting Environmental Scholarship from the Yale Institute for Biospheric Studies. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. We thank R. M. Timm and an anonymous reviewer for comments that improved the manuscript. NR 66 TC 6 Z9 6 U1 0 U2 15 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD FEB PY 2013 VL 94 IS 1 BP 183 EP 201 DI 10.1644/11-MAMM-A-343.1 PG 19 WC Zoology SC Zoology GA 095WY UT WOS:000315366900019 ER PT J AU Bakos, GA Csubry, Z Penev, K Bayliss, D Jordan, A Afonso, C Hartman, JD Henning, T Kovacs, G Noyes, RW Beky, B Suc, V Csak, B Rabus, M Lazar, J Papp, I Sari, P Conroy, P Zhou, G Sackett, PD Schmidt, B Mancini, L Sasselov, DD Ueltzhoeffer, K AF Bakos, G. A. Csubry, Z. Penev, K. Bayliss, D. Jordan, A. Afonso, C. Hartman, J. D. Henning, T. Kovacs, G. Noyes, R. W. Beky, B. Suc, V. Csak, B. Rabus, M. Lazar, J. Papp, I. Sari, P. Conroy, P. Zhou, G. Sackett, P. D. Schmidt, B. Mancini, L. Sasselov, D. D. Ueltzhoeffer, K. TI HATSouth: A Global Network of Fully Automated Identical Wide-Field Telescopes SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID WHOLE EARTH TELESCOPE; OPEN CLUSTER M37; MICROLENSING EVENTS; PLANET-DETECTION; VARIABLE-STARS; TRANSIT SURVEY; LIGHT CURVES; SUPER-EARTHS; SYSTEM; SEARCH AB HATSouth is the world's first network of automated and homogeneous telescopes that is capable of year-round 24 hr monitoring of positions over an entire hemisphere of the sky. The primary scientific goal of the network is to discover and characterize a large number of transiting extrasolar planets, reaching out to long periods and down to small planetary radii. HATSouth achieves this by monitoring extended areas on the sky, deriving high precision light curves for a large number of stars, searching for the signature of planetary transits, and confirming planetary candidates with larger telescopes. HATSouth employs six telescope units spread over three prime locations with large longitude separation in the southern hemisphere (Las Campanas Observatory, Chile; HESS site, Namibia; Siding Spring Observatory, Australia). Each of the HATSouth units holds four 0.18 m diameter f/2.8 focal ratio telescope tubes on a common mount producing an 8.2 degrees x 8.2 degrees field of view on the sky, imaged using four 4 K x 4 K CCD cameras and Sloan r filters, to give a pixel scale of 3.7 '' pixel(-1). The HATSouth network is capable of continuously monitoring 128 square arc degrees at celestial positions moderately close to the anti-solar direction. We present the technical details of the network, summarize operations, and present detailed weather statistics for the three sites. Robust operations have meant that on average each of the six HATSouth units has conducted observations on similar to 500 nights over a 2 years time period, yielding a total of more than 1 million science frames at a 4 minute integration time and observing similar to 10.65 hr day(-1) on average. We describe the scheme of our data transfer and reduction from raw pixel images to trend-filtered light curves and transiting planet candidates. Photometric precision reaches similar to 6 mmag at 4 minute cadence for the brightest non-saturated stars at r approximate to 10.5. We present detailed transit recovery simulations to determine the expected yield of transiting planets from HATSouth. We highlight the advantages of networked operations, namely, a threefold increase in the expected number of detected planets, as compared to all telescopes operating from the same site. C1 [Bakos, G. A.; Csubry, Z.; Penev, K.; Hartman, J. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bakos, G. A.; Csubry, Z.; Penev, K.; Hartman, J. D.; Noyes, R. W.; Beky, B.; Sasselov, D. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, D.; Conroy, P.; Zhou, G.; Sackett, P. D.; Schmidt, B.] Australian Natl Univ, Canberra, ACT, Australia. [Jordan, A.; Suc, V.; Rabus, M.] Catholic Univ Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Afonso, C.; Henning, T.; Csak, B.; Mancini, L.] Max Planck Inst Astron, D-69120 Heidelberg, Germany. [Kovacs, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. [Ueltzhoeffer, K.] Goethe Univ Frankfurt, Bernstein Ctr Computat Neurosci Heidelberg Mannhe, Frankfurt, Germany. RP Bakos, GA (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM gbakos@astro.princeton.edu RI Bayliss, Daniel/I-4635-2012; OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287 FU NSF MRI grant [NSF/AST-0723074]; MPIA; ANU; NASA [NNX09AB29G]; Fondecyt [1095213, 3120097]; Ministry of Economy ICM Nuclei [P07-021-F, P10-022-F]; Anillo [ACT-086]; BASAL CATA [PFB-06]; FONDAP CFA [15010003]; ALMA-CONICYT [31090015, 31080021]; RoPACS, a Marie Curie Initial Training Network; European Commissions Seventh Framework Programme FX Hardware costs for the HATSouth project were funded by NSF MRI grant NSF/AST-0723074. Construction of the infrastructure at the HESS site was funded by MPIA, and similar costs at SSO enjoyed partial funding from the ANU. We thank the Smithsonian Astrophysical Observatory for the Internal Research and Development (IR&D) funds that supported visiting students Gabor Kovacs and Zoltan Csubry during the 2008-2009 development phase of the project. Following the installation and calibration, the overall operation of the HATSouth network has been supported by NASA grant NNX09AB29G.; Installation to the respective HATSouth sites required teamwork in a hectic schedule. We thank F. Rozsa for joining our installation team to Namibia and Australia. At Las Campanas, we are indebted to the whole staff for their help in installation, and particularly so to Francisco Figueroa, Marc Leroy, Juan Espoz, Juan Espoz, Jr., Andres Rivera, Patricio Pinto, and Henry Cortes for their very generous support. Don Hector and the kitchen staff at LCO provided delicious meals that kept us going through the long installation days. We also thank Earl Harris (Carnegie) for his assistance in the transportation of telescope components to the site. At the HESS site, we are most grateful for the help of Toni Hanke, site manager, technical support Albert Jahnke, and our hosts Adele and Joachim Cranz. We greatly benefited from discussions with Michael Panther and German Herman (MPIK) in the initial planning phase of the project. At ANU's Siding Springs Observatory, we thank Geoff White for his help during installation and the first 2 year's of operation. Tammy Roderick at ANU helped identify many issues in relation to the first set of HATSouth images, and we thank her very much for her contribution to the project. We greatly appreciate the help we received from Gabe Bloxham at ANU in relation to the telescope optics. We also thank Colin Vest at ANU for his help in servicing the Australian telescopes. We appreciate Vince O'Connor's help in administrative matters regarding the installation. G. A. B. was supported as an NSF Fellow (AST-0702843) by SAO during the development of this project. G. A. B. is extremely thankful for the family of P. Sari for hosting and operating the prototype instrument in their garden at Pecel, Hungary, for an extended period of almost 1 year. G. A. B. also wishes to thank the SAO administration for the swift management of the relevant grants, in particular to P. Sozanski, J. Lendall, N. Rathle, L. Linarte and E. Dotts. We thank T. Szklenar for his expert help in the system management of computers during 2011 at the remote sites and at Princeton. We also thank Gy. Medgyesi for his help in the mechanical design of the HATSouth units. We thank P. Jonas and his family for their help in the Australian installation. A. J. acknowledges support from Fondecyt project 1095213, Ministry of Economy ICM Nuclei P07-021-F and P10-022-F, Anillo ACT-086, BASAL CATA PFB-06, and FONDAP CFA 15010003. V. S. acknowledges support form BASAL CATA PFB-06. M. R. has been supported by ALMA-CONICYT projects 31090015 and 31080021 and by a FONDECYT postdoctoral project 3120097. G. K. is supported by RoPACS, a Marie Curie Initial Training Network funded by the European Commissions Seventh Framework Programme. We thank the anonymous referee for the critical review that improved the quality of the manuscript. NR 66 TC 51 Z9 51 U1 2 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD FEB PY 2013 VL 125 IS 924 BP 154 EP 182 DI 10.1086/669529 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 094ON UT WOS:000315273800004 ER PT J AU Batalha, NM Rowe, JF Bryson, ST Barclay, T Burke, CJ Caldwell, DA Christiansen, JL Mullally, F Thompson, SE Brown, TM Dupree, AK Fabrycky, DC Ford, EB Fortney, JJ Gilliland, RL Isaacson, H Latham, DW Marcy, GW Quinn, SN Ragozzine, D Shporer, A Borucki, WJ Ciardi, DR Gautier, TN Haas, MR Jenkins, JM Koch, DG Lissauer, JJ Rapin, W Basri, GS Boss, AP Buchhave, LA Carter, JA Charbonneau, D Christensen-Dalsgaard, J Clarke, BD Cochran, WD Demory, BO Desert, JM Devore, E Doyle, LR Esquerdo, GA Everett, M Fressin, F Geary, JC Girouard, FR Gould, A Hall, JR Holman, MJ Howard, AW Howell, SB Ibrahim, KA Kinemuchi, K Kjeldsen, H Klaus, TC Li, J Lucas, PW Meibom, S Morris, RL Prsa, A Quintana, E Sanderfer, DT Sasselov, D Seader, SE Smith, JC Steffen, JH Still, M Stumpe, MC Tarter, JC Tenenbaum, P Torres, G Twicken, JD Uddin, K Van Cleve, J Walkowicz, L Welsh, WF AF Batalha, Natalie M. Rowe, Jason F. Bryson, Stephen T. Barclay, Thomas Burke, Christopher J. Caldwell, Douglas A. Christiansen, Jessie L. Mullally, Fergal Thompson, Susan E. Brown, Timothy M. Dupree, Andrea K. Fabrycky, Daniel C. Ford, Eric B. Fortney, Jonathan J. Gilliland, Ronald L. Isaacson, Howard Latham, David W. Marcy, Geoffrey W. Quinn, Samuel N. Ragozzine, Darin Shporer, Avi Borucki, William J. Ciardi, David R. Gautier, Thomas N., III Haas, Michael R. Jenkins, Jon M. Koch, David G. Lissauer, Jack J. Rapin, William Basri, Gibor S. Boss, Alan P. Buchhave, Lars A. Carter, Joshua A. Charbonneau, David Christensen-Dalsgaard, Joergen Clarke, Bruce D. Cochran, William D. Demory, Brice-Olivier Desert, Jean-Michel Devore, Edna Doyle, Laurance R. Esquerdo, Gilbert A. Everett, Mark Fressin, Francois Geary, John C. Girouard, Forrest R. Gould, Alan Hall, Jennifer R. Holman, Matthew J. Howard, Andrew W. Howell, Steve B. Ibrahim, Khadeejah A. Kinemuchi, Karen Kjeldsen, Hans Klaus, Todd C. Li, Jie Lucas, Philip W. Meibom, Soren Morris, Robert L. Prsa, Andrej Quintana, Elisa Sanderfer, Dwight T. Sasselov, Dimitar Seader, Shawn E. Smith, Jeffrey C. Steffen, Jason H. Still, Martin Stumpe, Martin C. Tarter, Jill C. Tenenbaum, Peter Torres, Guillermo Twicken, Joseph D. Uddin, Kamal Van Cleve, Jeffrey Walkowicz, Lucianne Welsh, William F. TI PLANETARY CANDIDATES OBSERVED BY KEPLER. III. ANALYSIS OF THE FIRST 16 MONTHS OF DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; eclipses; planetary systems; space vehicles; techniques: photometric ID SOLAR-TYPE STARS; SUN-LIKE STAR; TARGET STARS; ECLIPSING BINARIES; HABITABLE PLANETS; INPUT CATALOG; DATA RELEASE; LOW-MASS; SYSTEMS; METALLICITIES AB New transiting planet candidates are identified in 16 months (2009 May-2010 September) of data from the Kepler spacecraft. Nearly 5000 periodic transit-like signals are vetted against astrophysical and instrumental false positives yielding 1108 viable new planet candidates, bringing the total count up to over 2300. Improved vetting metrics are employed, contributing to higher catalog reliability. Most notable is the noise-weighted robust averaging of multiquarter photo-center offsets derived from difference image analysis that identifies likely background eclipsing binaries. Twenty-two months of photometry are used for the purpose of characterizing each of the candidates. Ephemerides (transit epoch, T-0, and orbital period, P) are tabulated as well as the products of light curve modeling: reduced radius (R-P / R-star), reduced semimajor axis (d / R-star), and impact parameter (b). The largest fractional increases are seen for the smallest planet candidates (201% for candidates smaller than 2R(circle plus). compared to 53% for candidates larger than 2R.) and those at longer orbital periods (124% for candidates outside of 50 day orbits versus 86% for candidates inside of 50 day orbits). The gains are larger than expected from increasing the observing window from 13 months (Quarters 1-5) to 16 months (Quarters 1-6) even in regions of parameter space where one would have expected the previous catalogs to be complete. Analyses of planet frequencies based on previous catalogs will be affected by such incompleteness. The fraction of all planet candidate host stars with multiple candidates has grown from 17% to 20%, and the paucity of short-period giant planets in multiple systems is still evident. The progression toward smaller planets at longer orbital periods with each new catalog release suggests that Earth-size planets in the habitable zone are forthcoming if, indeed, such planets are abundant. C1 [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Batalha, Natalie M.; Bryson, Stephen T.; Christiansen, Jessie L.; Borucki, William J.; Haas, Michael R.; Koch, David G.; Lissauer, Jack J.; Rapin, William; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Burke, Christopher J.; Caldwell, Douglas A.; Mullally, Fergal; Thompson, Susan E.; Jenkins, Jon M.; Li, Jie; Quintana, Elisa; Seader, Shawn E.; Smith, Jeffrey C.; Stumpe, Martin C.; Tenenbaum, Peter; Twicken, Joseph D.; Van Cleve, Jeffrey] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas; Kinemuchi, Karen; Still, Martin] NASA, Bay Area Environm Res Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Timothy M.; Shporer, Avi] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA. [Dupree, Andrea K.; Latham, David W.; Quinn, Samuel N.; Ragozzine, Darin; Carter, Joshua A.; Charbonneau, David; Desert, Jean-Michel; Esquerdo, Gilbert A.; Fressin, Francois; Geary, John C.; Holman, Matthew J.; Meibom, Soren; Sasselov, Dimitar; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Isaacson, Howard; Marcy, Geoffrey W.; Basri, Gibor S.; Howard, Andrew W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gautier, Thomas N., III; Clarke, Bruce D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Boss, Alan P.] Carnegie Inst Sci, Washington, DC 20015 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Christensen-Dalsgaard, Joergen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Demory, Brice-Olivier] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Devore, Edna; Doyle, Laurance R.; Tarter, Jill C.] SETI Inst, Mountain View, CA 94043 USA. [Everett, Mark] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Girouard, Forrest R.; Hall, Jennifer R.; Ibrahim, Khadeejah A.; Klaus, Todd C.; Morris, Robert L.; Sanderfer, Dwight T.; Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Steffen, Jason H.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Walkowicz, Lucianne] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Batalha, NM (reprint author), San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. EM Natalie.Batalha@nasa.gov RI Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Demory, Brice-Olivier/0000-0002-9355-5165; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate.; National Aeronautics and Space Administration [NNX08AR04G] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This material is based on work supported by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program. NR 59 TC 434 Z9 434 U1 6 U2 65 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2013 VL 204 IS 2 AR 24 DI 10.1088/0067-0049/204/2/24 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088BZ UT WOS:000314810100011 ER PT J AU Luo, B Fabbiano, G Strader, J Kim, DW Brodie, JP Fragos, T Gallagher, JS King, A Zezas, A AF Luo, B. Fabbiano, G. Strader, J. Kim, D. -W. Brodie, J. P. Fragos, T. Gallagher, J. S. King, A. Zezas, A. TI DEEP CHANDRA MONITORING OBSERVATIONS OF NGC 4649. I. CATALOG OF SOURCE PROPERTIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: individual (NGC 4649); globular clusters: general; X-rays: binaries; X-rays: galaxies ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; MS SOURCE CATALOGS; DIGITAL SKY SURVEY; GLOBULAR-CLUSTERS; ELLIPTIC GALAXIES; MULTIWAVELENGTH PROJECT; LUMINOSITY FUNCTION; CONFIDENCE-LIMITS AB We present the X-ray source catalog for the Chandra monitoring observations of the elliptical galaxy, NGC 4649. The galaxy has been observed with Chandra ACIS-S3 in six separate pointings, reaching a total exposure of 299 ks. There are 501 X-ray sources detected in the 0.3-8.0 keV band in the merged observation or in one of the six individual observations; 399 sources are located within the D-25 ellipse. The observed 0.3-8.0 keV luminosities of these 501 sources range from 9.3 x 10(36) erg s(-1) to 5.4 x 10(39) erg s(-1). The 90% detection completeness limit within the D-25 ellipse is 5.5x10(37) erg s-1. Based on the surface density of background active galactic nuclei (AGNs) and detection completeness, we expect approximate to 45 background AGNs among the catalog sources (approximate to 15 within the D25 ellipse). There are nine sources with luminosities greater than 1039 erg s-1, which are candidates for ultraluminous X-ray sources. The nuclear source of NGC 4649 is a low-luminosity AGN, with an intrinsic 2.0-8.0 keV X-ray luminosity of 1.5x10(38) erg s(-1). The X-ray colors suggest that the majority of the catalog sources are low-mass X-ray binaries (LMXBs). We find that 164 of the 501 X-ray sources show long-term variability, indicating that they are accreting compact objects. We discover four transient candidates and another four potential transients. We also identify 173 X-ray sources (141 within the D-25 ellipse) that are associated with globular clusters (GCs) based on Hubble Space Telescope and ground-based data; these LMXBs tend to be hosted by red GCs. Although NGC 4649 has a much larger population of X-ray sources than the structurally similar early-type galaxies, NGC 3379 and NGC 4278, the X-ray source properties are comparable in all three systems. C1 [Luo, B.; Fabbiano, G.; Strader, J.; Kim, D. -W.; Fragos, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brodie, J. P.] UCO Lick Observ, Santa Cruz, CA 95064 USA. [Gallagher, J. S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [King, A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Luo, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Fragos, Tassos/0000-0003-1474-1523 FU NASA HST [GO-12369.01-A]; CXC [GO1-12110X]; NSF [AST-0808099]; CXC; Smithsonian Astrophysical Observatory (SAO) [NAS8-03060]; CfA; ITC FX We acknowledge financial support from NASA HST grant GO-12369.01-A (B.L., G.F.), CXC grant GO1-12110X (B.L., G.F.), and NSF grant AST-0808099 (J.P.B.). We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under Contract NAS8-03060. G.F. and T.F. thank the Aspen Center for Physics. T.F. acknowledges support from the CfA and the ITC prize fellowship programs, and J.S.G. thanks the University of Wisconsin Graduate School and College of Letters NR 66 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD FEB PY 2013 VL 204 IS 2 AR 14 DI 10.1088/0067-0049/204/2/14 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 088BZ UT WOS:000314810100001 ER PT J AU Greenberg, R Etterson, M Danner, RM AF Greenberg, Russell Etterson, Matthew Danner, Raymond M. TI Seasonal dimorphism in the horny bills of sparrows SO ECOLOGY AND EVOLUTION LA English DT Article DE Bill size; bird beaks; emberizidae; rhamphotheca; salt marsh birds; sexual selection; tidal marsh birds ID SEXUAL SIZE DIMORPHISM; POECILE-ATRICAPILLUS; NATURAL-SELECTION; DARWINS FINCHES; MARSH SPARROWS; NORTH-AMERICA; BODY-SIZE; GROWTH; EVOLUTION; BEAK AB Bill size is often viewed as a species-specific adaptation for feeding, but it sometimes varies between sexes, suggesting that sexual selection or intersexual competition may also be important. Hypotheses to explain sexual dimorphism in avian bill size include divergence in feeding niche or thermoregulatory demands, intrasexual selection based on increased competition among males, or female preference. Birds also show seasonal changes in bill size due to shifts in the balance between growth rate and wear, which may be due to diet or endogenous rhythms in growth. Insight into the function of dimorphism can be gained using the novel approach of digital x-ray imaging of museum skins to examine the degree to which the skeletal core or the rhamphotheca contribute to overall dimorphism. The rhamphotheca is ever-growing and ever-wearing, varying in size throughout life; whereas the skeletal core shows determinant growth. Because tidal marsh sparrows are more dimorphic in bill size than related taxa, we selected two marsh taxa to investigate dimorphism and seasonality in the size of the overall bill, the skeletal core, and the rhamphotheca. Bill size varied by sex and season, with males having larger bills than females, and bill size increasing from nonbreeding to breeding season more in males. Skeletal bill size varied with season, but not sex. The rhamphotheca varied primarily with sex; males had a larger rhamphotheca (corrected for skeletal bill size), which showed a greater seasonal increase than females. The rhamphotheca, rather than the skeletal bill, was responsible for sexual dimorphism in overall bill size, which was particularly well developed in the breeding season. The size of the rhamphotheca may be a condition-based character that is shaped by sexual selection. These results are consistent with the evidence that bill size is influenced by sexual selection as well as trophic ecology. C1 [Greenberg, Russell; Danner, Raymond M.] Smithsonian Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Etterson, Matthew] US EPA, Off Res & Dev, Natl Hlth & Environm Effects Res Lab, Midcontinent Ecol Div, Duluth, MN 55804 USA. RP Greenberg, R (reprint author), Smithsonian Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. EM greenbergr@si.edu RI Danner, Raymond/J-8350-2013 OI Danner, Raymond/0000-0002-3999-8141 NR 57 TC 9 Z9 9 U1 5 U2 49 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD FEB PY 2013 VL 3 IS 2 BP 389 EP 398 DI 10.1002/ece3.474 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 091BZ UT WOS:000315025200019 PM 23467758 ER PT J AU Boomer, KMB Weller, DE Jordan, TE Linker, L Liu, ZJ Reilly, J Shenk, G Voinov, AA AF Boomer, Kathleen M. B. Weller, Donald E. Jordan, Thomas E. Linker, Lewis Liu, Zhi-Jun Reilly, James Shenk, Gary Voinov, Alexey A. TI Using Multiple Watershed Models to Predict Water, Nitrogen, and Phosphorus Discharges to the Patuxent Estuary SO JOURNAL OF THE AMERICAN WATER RESOURCES ASSOCIATION LA English DT Review DE watersheds; watershed management; nonpoint source pollution; simulation; hydrological modeling; ensemble modeling; model comparison; model average; land use; model structure; model performance ID LAND-USE CHANGE; CONTERMINOUS UNITED-STATES; CHESAPEAKE BAY; ENVIRONMENTAL-MODELS; NUTRIENT DISCHARGES; SUSPENDED-SEDIMENT; CONSTITUENT LOADS; SCENARIO ANALYSIS; COVER DATABASE; RIVER ESTUARY AB Boomer, Kathleen M.B., Donald E. Weller, Thomas E. Jordan, Lewis Linker, Zhi-Jun Liu, James Reilly, Gary Shenk, and Alexey A. Voinov, 2012. Using Multiple Watershed Models to Predict Water, Nitrogen, and Phosphorus Discharges to the Patuxent Estuary. Journal of the American Water Resources Association (JAWRA) 1-25. DOI: 10.1111/j.1752-1688.2012.00689.x Abstract: We analyzed an ensemble of watershed models that predict flow, nitrogen, and phosphorus discharges. The models differed in scope and complexity and used different input data, but all had been applied to evaluate human impacts on discharges to the Patuxent River or to the Chesapeake Bay. We compared predictions to observations of average annual, annual time series, and monthly discharge leaving three basins. No model consistently matched observed discharges better than the others, and predictions differed as much as 150% for every basin. Models that agreed best with the observations in one basin often were among the worst models for another material or basin. Combining model predictions into a model average improved overall reliability in matching observations, and the range of predictions helped describe uncertainty. The model average was not the closest to the observed discharge for every material, basin, and time frame, but the model average had the highest NashSutcliffe performance across all combinations. Consistently poor performance in predicting phosphorus loads suggests that none of the models capture major controls. Differences among model predictions came from differences in model structures, input data, and the time period considered, and also to errors in the observed discharge. Ensemble watershed modeling helped identify research needs and quantify the uncertainties that should be considered when using the models in management decisions. C1 [Boomer, Kathleen M. B.; Weller, Donald E.; Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Linker, Lewis; Shenk, Gary] US EPA, Chesapeake Bay Program, Annapolis, MD 21403 USA. [Liu, Zhi-Jun] Univ N Carolina, Dept Geog, Greensboro, NC 27402 USA. [Reilly, James] Maryland Dept Planning, Baltimore, MD 21201 USA. [Voinov, Alexey A.] Univ Vermont, Gund Inst Ecol Econ, Burlington, VT 05405 USA. RP Boomer, KMB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM boomerk@si.edu RI Voinov, Alexey/F-7397-2010; OI Voinov, Alexey/0000-0002-2985-4574; Weller, Donald/0000-0002-7629-5437 FU National Oceanic and Atmospheric Administration Coastal Oceans Program [NA66RG0129, NA03NOS4780008]; National Science Foundation [BSR-9085219, DEB-9317968]; Smithsonian Institution Environmental Sciences Program FX This research was funded by the National Oceanic and Atmospheric Administration Coastal Oceans Program (grant numbers NA66RG0129 and NA03NOS4780008), National Science Foundation (grant numbers BSR-9085219 and DEB-9317968), and the Smithsonian Institution Environmental Sciences Program. John Brakebill of the U. S. Geological Survey provided information and model output for the SPARROW models. NR 118 TC 9 Z9 9 U1 2 U2 56 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1093-474X EI 1752-1688 J9 J AM WATER RESOUR AS JI J. Am. Water Resour. Assoc. PD FEB PY 2013 VL 49 IS 1 BP 15 EP 39 DI 10.1111/j.1752-1688.2012.00689.x PG 25 WC Engineering, Environmental; Geosciences, Multidisciplinary; Water Resources SC Engineering; Geology; Water Resources GA 087IU UT WOS:000314755700002 ER PT J AU Metcalf, CJE McMahon, SM Salguero-Gomez, R Jongejans, E AF Metcalf, C. Jessica E. McMahon, Sean M. Salguero-Gomez, Roberto Jongejans, Eelke TI IPMpack: an R package for integral projection models SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE demography; elasticity; integral projection model; passage time; sensitivity ID MATRIX MODELS; HYPERICUM-CUMULICOLA; ENVIRONMENTAL-CHANGE; POPULATION-DYNAMICS; DEMOGRAPHY; SIZE; SENSITIVITY; EVOLUTION; TREES; SCRUB AB Structured demographic models offer powerful methods for addressing important questions in ecology and evolution. Integral Projection Models (IPMs) are related to classic matrix models, but are more appropriate for modelling structured populations when the variable describing individuals' demography is continuous (e.g. size, weight, etc.). We present IPMpack, a free open-source software (R) package for building IPMs. The package estimates key population characteristics from IPMs, such as population growth rate in both deterministic and stochastic environments, age-specific trajectories of survival and reproduction, and sensitivities and elasticities to changes in underlying vital rates. IPMpack can be used for species across a range of life cycle complexity and can include continuous and discrete (e.g. seed bank, hibernation) state variables, as well as environmental covariates of interest. Methods for diagnostics, sensitivity analyses, plotting, model comparison and many other features allow users to move from data input through analysis to inference using an array of internal functions. IPMpack fills a need for readily usable tools for constructing and analysing IPMs and is designed to facilitate their use for experts and open up their use for those researchers who have little experience in the details of population models. A standardized IPM modelling framework will also facilitate cross-study and cross-species comparative demography, encouraging the exploration of broader ecological and evolutionary questions that can be addressed by population models. C1 [Metcalf, C. Jessica E.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [McMahon, Sean M.] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. [Salguero-Gomez, Roberto] Max Planck Inst Demog Res, Evolutionary Biodemog Lab, D-18057 Rostock, Germany. [Jongejans, Eelke] Radboud Univ Nijmegen, Dept Anim Ecol & Ecophysiol, Inst Water & Wetland Res, NL-6525 AJ Nijmegen, Netherlands. RP Metcalf, CJE (reprint author), Univ Oxford, Dept Zool, S Parks Rd, Oxford OX1 3PS, England. EM charlotte.metcalf@zoo.ox.ac.uk RI Salguero-Gomez, Roberto/F-9071-2013; Jongejans, Eelke/B-4832-2008; Salguero-Gomez, Roberto/N-6016-2016 OI Salguero-Gomez, Roberto/0000-0002-6085-4433; Jongejans, Eelke/0000-0003-1148-7419; Salguero-Gomez, Roberto/0000-0002-6085-4433 FU Evolutionary Biodemography Laboratory; Modeling the Evolution of Ageing Independent Group of the Max Planck Society for Demographic Research (Rostock, Germany) FX We thank Justin Lessler for guidance on S4 objects and Cory Merow for helpful discussions and comments on previous versions of IPMpack and this manuscript. P. F. Quintana-Ascencio (University of Central Florida) and E. Menges (Archbold Biological Station) kindly provided Hypericum cumulicola individual data used here to illustrate the use of the R package. We thank the Evolutionary Biodemography Laboratory and the Modeling the Evolution of Ageing Independent Group of the Max Planck Society for Demographic Research (Rostock, Germany) for supporting the working group where this package was finished. NR 21 TC 33 Z9 33 U1 3 U2 101 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD FEB PY 2013 VL 4 IS 2 BP 195 EP 200 DI 10.1111/2041-210x.12001 PG 6 WC Ecology SC Environmental Sciences & Ecology GA 090JH UT WOS:000314974800011 ER PT J AU Dalling, JW Winter, K Andersen, KM Turner, BL AF Dalling, J. W. Winter, K. Andersen, K. M. Turner, B. L. TI Artefacts of the pot environment on soil nutrient availability: implications for the interpretation of ecological studies SO PLANT ECOLOGY LA English DT Article DE Nutrient availability; Soil conditioner; Plant growth; Pot artifacts ID LYCOPERSICON-ESCULENTUM MILL; BUSH PLANT-RESPONSE; ROOT RESTRICTION; ELEVATED CO2; GROWTH; NITROGEN; FOREST; MINERALIZATION; ENHANCEMENT; VERMICULITE AB Pot experiments are frequently used to examine plant, soil, and microbial interactions that cannot be studied in situ. Although impacts of the pot environment on seedling growth have long been recognized, they are rarely addressed directly in current ecological studies. Here we examine how commonly used soil conditioners, often necessary to maintain adequate drainage in pots, can influence nutrient availability and seedling growth. Balsawood (Ochroma pyramidalis) seedlings were grown in central Panama in soil combined in a 50:50 mix with one of the following soil conditioners: marine sand, pure sand, perlite, vermiculite, or rice husks. Soil nutrient availability, foliar N and P, and seedling growth were compared after 1 month. Rice husks dramatically reduced soil nitrate, seedling growth, and foliar N. Other conditioners had smaller effects on growth, although vermiculite may be a significant source of base cations in infertile soils. Marine sand had a strong neutralizing effect on acidic soil due to the presence of calcareous shell fragments. Effects of soil conditioners need to be added to other known artifacts of the pot environment influencing nutrient availability, including alterations to N mineralization rates relative to bulk soil, and pot-size effects on N:P availability. These artifacts can strongly influence plant performance and therefore the interpretation of ecological studies. C1 [Dalling, J. W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, J. W.; Winter, K.; Andersen, K. M.; Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM dallingj@life.illinois.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Smithsonian Tropical Research Institute FX We thank Milton Garcia, Jorge Aranda, Aurelio Virgo, and Tania Romero for technical assistance in carrying out the experiment, and the Smithsonian Tropical Research Institute for financial and logistic support. NR 45 TC 5 Z9 5 U1 1 U2 53 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD FEB PY 2013 VL 214 IS 2 BP 329 EP 338 DI 10.1007/s11258-013-0172-3 PG 10 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 087SB UT WOS:000314781600014 ER PT J AU Godfrey, SJ Geisler, J Fitzgerald, EMG AF Godfrey, Stephen J. Geisler, Jonathan Fitzgerald, Erich M. G. TI On the Olfactory Anatomy in an Archaic Whale (Protocetidae, Cetacea) and the Minke Whale Balaenoptera acutorostrata (Balaenopteridae, Cetacea) SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE Cetacea; olfactory apparatus Protocetidae; Balaenopteridae; Virginia; ethmoturbinates; Pamunkey River ID MIDDLE EOCENE; ARCHAEOCETE WHALE; TOOTHED MYSTICETE; RORQUAL WHALES; EOCETUS-WARDII; FLOW PATTERNS; BALEEN WHALES; AIR-FLOW; MAMMALIA; LUNGE AB The structure of the olfactory apparatus is not well known in both archaic and extant whales; the result of poor preservation in most fossils and locational isolation deep within the skulls in both fossil and Recent taxa. Several specimens now shed additional light on the subject. A partial skull of an archaic cetacean is reported from the Pamunkey River, Virginia, USA. The specimen probably derives from the upper middle Eocene (Piney Point Formation) and is tentatively assigned to the Protocetidae. Uncrushed cranial cavities associated with the olfactory apparatus were devoid of sediment. CT scans clearly reveal the dorsal nasal meatus, ethmoturbinates within the olfactory recess, the cribriform plate, the area occupied by the olfactory bulbs, and the olfactory nerve tract. Several sectioned skulls of the minke whale (Balaenoptera acutorostrata) were also examined, and olfactory structures are remarkably similar to those observed in the fossil skull from the Pamunkey River. One important difference between the two is that the fossil specimen has an elongate olfactory nerve tract. The more forward position of the external nares in extant balaenopterids when compared with those of extant odontocetes is interpreted to be the result of the need to retain a functional olfactory apparatus and the forward position of the supraoccipital/cranial vertex. An increase in the distance between the occipital condyles and the vertex in balaenopterids enhances the mechanical advantage of the epaxial musculature that inserts on the occiput, a specialization that likely stabilizes the head of these enormous mammals during lunge feeding. Anat Rec, 2013. (c) 2012 Wiley Periodicals, Inc. C1 [Godfrey, Stephen J.] Calvert Marine Museum, Dept Paleontol, Solomons, MD 20688 USA. [Godfrey, Stephen J.; Geisler, Jonathan; Fitzgerald, Erich M. G.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Geisler, Jonathan] New York Coll Osteopath Med, Dept Anat, Old Westbury, NY USA. [Fitzgerald, Erich M. G.] Museum Victoria, Melbourne, Vic, Australia. RP Godfrey, SJ (reprint author), Calvert Marine Museum, Dept Paleontol, POB 97, Solomons, MD 20688 USA. EM godfresj@co.cal.md.us FU Board of Calvert County; Citizens of Calvert County, MD; Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum FX Grant sponsors: Board of Calvert County Commissioners, The Citizens of Calvert County, MD, and The Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum. NR 78 TC 17 Z9 18 U1 2 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 EI 1932-8494 J9 ANAT REC JI Anat. Rec. PD FEB PY 2013 VL 296 IS 2 BP 257 EP 272 DI 10.1002/ar.22637 PG 16 WC Anatomy & Morphology SC Anatomy & Morphology GA 086BA UT WOS:000314656800009 PM 23233318 ER PT J AU Hirsch, BT Prange, S Hauver, SA Gehrt, SD AF Hirsch, Ben T. Prange, Suzanne Hauver, Stephanie A. Gehrt, Stanley D. TI Genetic relatedness does not predict racoon social network structure SO ANIMAL BEHAVIOUR LA English DT Article DE association; home range overlap; homophily; kinship; Procyon lotor; rabies; racoon; relatedness; social network; socioecology ID RACCOON PROCYON-LOTOR; BROWN CAPUCHIN MONKEYS; ANTHROPOGENIC RESOURCES; CENTRAL MISSISSIPPI; SOLITARY CARNIVORE; HABITAT SELECTION; ADULT RACCOONS; KIN SELECTION; CONTACT RATES; CEBUS-APELLA AB Social assortativity, preferentially associating with certain individuals, is a widespread behaviour among a diverse range of taxa. Animals often choose to associate with other individuals based on characteristics such as sex, age, body size, rank and genetic relatedness. These preferences can scale up to shape the overall social structure of an animal group or population. We investigated possible factors that might shape the social network structure of common racoons, Procyon lotor, in a high-density urban population in Cook County, Illinois, U. S. A. Racoon associations were recorded using proximity detecting radiocollars that recorded when individuals came within 1-1.5 m of each other. In addition, dyadic measures of home range overlap and genetic relatedness were calculated for all individuals included in our study. We used multiple regression quadratic assignment procedures to determine what factors influenced the structure of racoon association networks. The only variable that positively influenced racoon social structure was male-male homophily, which is consistent with previous studies that documented frequent social interactions between adult male racoons. Genetic relatedness had no effect on racoon social networks and there was no evidence that males or females preferentially associated with close relatives, despite the presence of kin in the population. This pattern, that kinship does not play a significant role in shaping social structure, is strikingly unusual among mammals and is not consistent with many socioecological models. Although racoon individuals showed strong social partner preferences, it is unclear what factors drove these choices. This unpredictability in partner choice shaped the structure of the racoon social networks and has important implications for disease transfer in this widespread animal vector. (C) 2012 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Hirsch, Ben T.; Gehrt, Stanley D.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Hirsch, Ben T.] Smithsonian Trop Res Inst, Balboa, Panama. [Prange, Suzanne] Ohio Div Wildlife, Athens, OH USA. [Hauver, Stephanie A.] SUNY Binghamton, Sch Educ, Binghamton, NY USA. RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, 2021 Coffey Rd, Columbus, OH 43210 USA. EM hirschb@si.edu FU National Science Foundation [ID-0425203]; Cook County Animal and Rabies Control; Max McGraw Wildlife Foundation; Ohio State University's Terrestrial Wildlife Ecology Lab FX This project was funded in part by the National Science Foundation (ID-0425203), Cook County Animal and Rabies Control and the Max McGraw Wildlife Foundation. We thank the Cook County Forest Preserve District and C. Anchor for access to our study site, and are especially grateful for the support of D. Parmer (deceased). We also thank The Ohio State University's Terrestrial Wildlife Ecology Lab for support. Genetic analysis was conducted at the Brookfield Zoo in Chicago, IL under the supervision of J. Dubach. We thank Maggie Stanton, Nancy Solomon and two anonymous referees for giving us useful comments on an earlier version of this manuscript. We are deeply indebted to all of the technicians who assisted on this project. NR 92 TC 21 Z9 23 U1 8 U2 110 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD FEB PY 2013 VL 85 IS 2 BP 463 EP 470 DI 10.1016/j.anbehav.2012.12.011 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 086KR UT WOS:000314683000021 ER PT J AU Paretas-Martinez, J Forshage, M Buffington, M Fisher, N La Salle, J Pujade-Villar, J AF Paretas-Martinez, Jordi Forshage, Mattias Buffington, Matthew Fisher, Nicole La Salle, John Pujade-Villar, Juli TI Overview of Australian Cynipoidea (Hymenoptera) SO AUSTRALIAN JOURNAL OF ENTOMOLOGY LA English DT Article DE Australia; Austrocynipidae; Cynipidae; Figitidae; Ibaliidae; Liopteridae ID FAMILY IBALIIDAE HYMENOPTERA; SP N. HYMENOPTERA; OAK GALL WASPS; EUCOILINAE HYMENOPTERA; CHARIPINAE HYMENOPTERA; FIGITIDAE HYMENOPTERA; FORSTER HYMENOPTERA; BIOLOGICAL-CONTROL; PUJADE-VILLAR; SOUTH-AFRICA AB An overview of all families, subfamilies, genera and species of Cynipoidea present in Australia is presented. The Australian cynipoid fauna is very poorly known, with 37 genera recorded: one each for Austrocynipidae, Ibaliidae and Liopteridae; two for Cynipidae; and 32 for Figitidae. The first Australian records are given for the following genera of Eucoilinae: Aganaspis Lin, Areaspis Lin, Chrestosema Forster, Didyctium Riley, Endecameris Yoshimoto, Ganaspis Forster, Leptolamina Yoshimoto, Micreriodes Yoshimoto, Pseudodiranchis Yoshimoto, Sinochresta Lin and Weldia Yoshimoto. Nine new combinations, two new synonymies and one reinstatement are made: Eucoilinae (Figitidae): Hexacola aemilia comb. n., Hexacola florentia comb. n., Hexacola julia comb. n., Hexacola mozarti comb. n., Hexacola thoreauini comb. n., Kleidotoma marguerita comb. n., Leptopilina lonchaeae comb. n., Leptopilina maria comb. n., Trybliographa australiensis stat. rev. (Rhoptromeris unimaculus syn. n.); Thrasorinae (Figitidae): Thrasorus berlesi comb. n. (Thrasorus rieki Paretas-Martinez & Pujade-Villar 2011 syn. n.). Aspects on the systematics, distribution, biology and morphology of all cynipoid families and figitid subfamilies in Australia are given. A multi-character online key to the genera of Australian Cynipoidea can be found at http://www.ces.csiro.au/keys/Hymenoptera/Australian_Cynipoidea/Australian-Cynipoidea-Keys.html. C1 [Paretas-Martinez, Jordi; Pujade-Villar, Juli] Univ Barcelona, Fac Biol, Dept Anim Biol, E-08028 Barcelona, Spain. [Forshage, Mattias] Swedish Museum Nat Hist, Dept Entomol, SE-10405 Stockholm, Sweden. [Buffington, Matthew] NMNH, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Fisher, Nicole] CSIRO Ecosyst Sci, Australian Natl Insect Collect, Canberra, ACT 2601, Australia. [La Salle, John] CSIRO Ecosyst Sci, Atlas Living Australia, Canberra, ACT 2601, Australia. RP Paretas-Martinez, J (reprint author), Univ Barcelona, Fac Biol, Dept Anim Biol, Avda Diagonal 645, E-08028 Barcelona, Spain. EM jordi.paretas.martinez@gmail.com RI La Salle, John/B-9544-2008; Fisher, Nicole/B-3616-2009; Pujade-Villar, Juli/K-9838-2014 OI La Salle, John/0000-0002-8816-9569; NR 89 TC 5 Z9 6 U1 1 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1326-6756 EI 1440-6055 J9 AUST J ENTOMOL JI Aust. J. Entomol. PD FEB PY 2013 VL 52 IS 1 BP 73 EP 86 DI 10.1111/j.1440-6055.2012.00877.x PG 14 WC Entomology SC Entomology GA 084LN UT WOS:000314540900010 ER PT J AU Soon, W Legates, DR AF Soon, Willie Legates, David R. TI Solar irradiance modulation of Equator-to-Pole (Arctic) temperature gradients: Empirical evidence for climate variation on multi-decadal timescales SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article DE Total solar irradiance variability; Equator-to-Pole temperature gradient; Climate dynamics; Multi-decadal timescales ID SURFACE AIR-TEMPERATURE; LATITUDINAL INSOLATION/TEMPERATURE GRADIENT; INTERNETWORK MAGNETIC-FIELDS; NORTH-ATLANTIC; QUIET-SUN; THERMOHALINE CIRCULATION; ENERGY TRANSPORTS; KENDALLS TAU; HEAT-FLUX; SEA-ICE AB Using thermometer-based air temperature records for the period 1850-2010, we present empirical evidence for a direct relationship between total solar irradiance (TSI) and the Equator-to-Pole (Arctic) surface temperature gradient (EPTG). Modulation of the EPTG by TSI is also shown to exist, in variable ways, for each of the four seasons. Interpretation of the positive relationship between the TSI and EPTG indices suggests that solar-forced changes in the EPTG may represent a hemispheric-scale relaxation response of the system to a reduced Equator-to-Pole temperature gradient, which occurs in response to an increasing gradient of incoming solar insolation. Physical bases for the TSI-EPTG relationship are discussed with respect to their connections with large-scale climate dynamics, especially a critical relationship with the total meridional poleward energy transport. Overall, evidence suggests that a net increase in the TSI, or in the projected solar insolation gradient which reflects any net increase in solar radiation, has caused an increase in both oceanic and atmospheric heat transport to the Arctic in the warm period since the 1970s, resulting in a reduced temperature gradient between the Equator and the Arctic. We suggest that this new interpretative framework, which involves the extrinsic modulation of the total meridional energy flux beyond the implicit assumptions of the Bjerknes Compensation rule, may lead to a better understanding of how global and regional climate has varied through the Holocene and even the Quaternary (the most recent 2.6 million years of Earth's history). Similarly, a reassessment is now required of the underlying mechanisms that may have governed the equable climate dynamics of the Eocene (35-55 million years ago) and late Cretaceous (65-100 million years ago), both of which were warm geological epochs. This newly discovered relationship between TSI and the EPTG represents the "missing link" that was implicit in the empirical relationship that Soon (2009) recently demonstrated to exist between multi-decadal TSI and Arctic and North Atlantic climatic change. (c) 2012 Elsevier Ltd. All rights reserved. C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Legates, David R.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. RP Legates, DR (reprint author), Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. EM wsoon@cfa.harvard.edu; legates@udel.edu NR 130 TC 18 Z9 18 U1 1 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD FEB PY 2013 VL 93 BP 45 EP 56 DI 10.1016/j.jastp.2012.11.015 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 083SX UT WOS:000314486600005 ER PT J AU Murphy, KR Boehme, JR Brown, C Noble, M Smith, G Sparks, D Ruiz, GM AF Murphy, Kathleen R. Boehme, Jennifer R. Brown, Christopher Noble, Monaca Smith, George Sparks, Darrick Ruiz, Gregory M. TI Exploring the limits of dissolved organic matter fluorescence for determining seawater sources and ballast water exchange on the US Pacific coast SO JOURNAL OF MARINE SYSTEMS LA English DT Article DE Fluorescence; EEM; Dissolved organic matter; Ballast water; Ballast water exchange ID CALIFORNIA CURRENT SYSTEM; OCEAN; MARINE; SHIPS; INVASIONS; ENVIRONMENTS; SPECTROSCOPY; VERIFICATION; TERRESTRIAL; PARAFAC AB To minimize the risk of biological invasions associated with commercial shipping, vessels are required to conduct ballast water exchange (BWE)>= 200 nautical miles offshore when arriving in the US from foreign ports, and some states require coastal BWE >= 50 miles offshore along domestic routes. Previous research suggests that the intensity of fluorescent dissolved organic matter (fDOM) can be used to verify whether BWE was implemented. This study examined seasonal and spatial variability of fDOM in Pacific rim ports and the adjacent seas, using the North American coast as a model system to test whether regional fluorescence intensity thresholds consistently distinguish port sites from coastal and oceanic sites at increasing distances from shore. Over 2000 samples from major port systems on the US Pacific coast and along offshore (perpendicular) and alongshore (parallel) transects were analyzed. Overall, humic fDOM fluorescence intensity (C3* = 370/494 nm) effectively discriminated port versus oceanic sites located further than 100 miles from shore, but discriminated only a subset of coastal versus oceanic sources within the northeastern Pacific. Data from additional global ports are needed to predict the frequency of false positive or false negative ballast source determinations using fDOM for foreign vessel traffic. (C) 2012 Elsevier B.V. All rights reserved. C1 [Murphy, Kathleen R.; Boehme, Jennifer R.; Brown, Christopher; Noble, Monaca; Smith, George; Sparks, Darrick; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Murphy, Kathleen R.] Univ New S Wales, Sch Civil & Environm Engn, Water Res Ctr, Sydney, NSW 2052, Australia. RP Murphy, KR (reprint author), Univ New S Wales, Sch Civil & Environm Engn, Water Res Ctr, Sydney, NSW 2052, Australia. EM krm@unsw.edu.au; ruizg@si.edu RI Murphy, Kathleen/B-8217-2009; OI Murphy, Kathleen/0000-0001-5715-3604; Noble, Monaca/0000-0002-0284-5395; Ruiz, Gregory/0000-0003-2499-441X FU California State Lands Commission; National Sea Grant Program; Smithsonian Institution; US Coast Guard FX The authors thank the SERC staff, interns and volunteers who contributed to sample collection and analyses. L Takata, N. Dobroski, J. Menkel, B. Peterson, E. Devers, M. Wells, B. Hickey, J. Cordell and N. Fermi helped with the coordination and sampling on west coast transects. We gratefully acknowledge the research vessels and crew from the University of Washington (Friday Harbor Laboratory), Oregon State University, UC Davis (Bodega Marine Laboratory) and Moss Landing Marine Laboratory and owners and crew of the merchant vessels Alaskan Navigator (Alaska Tanker Company), MV Kate Maersk (Maersk Shipping Inc.), Sine Maersk (Maersk Shipping Inc.), MV Svendborg Maersk (Maersk Shipping Inc.), SS Polar Eagle (Marathon Oil Inc.), SS Arctic Sun (Marathon Oil Inc.), MV Ciclope (Ership International), and NRC Columbia (National Response Corporation) for hosting and assisting research efforts. This research was supported by California State Lands Commission, National Sea Grant Program, Smithsonian Institution, and the US Coast Guard. NR 38 TC 5 Z9 5 U1 5 U2 45 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0924-7963 J9 J MARINE SYST JI J. Mar. Syst. PD FEB PY 2013 VL 111 BP 157 EP 166 DI 10.1016/j.jmarsys.2012.10.010 PG 10 WC Geosciences, Multidisciplinary; Marine & Freshwater Biology; Oceanography SC Geology; Marine & Freshwater Biology; Oceanography GA 082EQ UT WOS:000314375500013 ER PT J AU Molina, JE Wen, J Struwe, L AF Molina, Jeanmaire E. Wen, Jun Struwe, Lena TI Systematics and biogeography of the non-viny grape relative Leea (Vitaceae) SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE 5S-NTS; cryptic species; internal transcribed spacer; Leeaceae; morphological evolution; Old World tropics; phylogeny; secondary structure; species complex; taxonomy; Vitales ID DISPERSAL-VICARIANCE ANALYSIS; RNA SECONDARY STRUCTURE; NUCLEAR RIBOSOMAL DNA; PHYLOGENY GROUP CLASSIFICATION; INTERNAL TRANSCRIBED SPACER-1; FREE-ENERGY MINIMIZATION; FLOWERING PLANTS; ANGIOSPERM PHYLOGENY; SEQUENCE DATA; HISTORICAL BIOGEOGRAPHY AB Leea, sometimes treated as the monogeneric family Leeaceae, is sister to the rest of the grape family, Vitaceae, but its systematics is poorly known. Phylogenetic relationships in Leea were reconstructed with parsimony and Bayesian methods using nuclear ribosomal sequences to assess species circumscriptions, morphological evolution and biogeography. The internal transcribed spacer secondary structure model for Leea facilitated homology assessments during sequence alignment. Nine morphological characters were mapped onto the phylogenetic tree. Four major clades in Leea were supported, with L. asiatica s.l. (=clade I) as the earliest diverging clade and having plesiomorphic free stamens. Clade II, which includes the prickle-bearing species, is sister to clade III, which includes species with comparatively large flowers. Clade IV, sister to clade II +/- III, was resolved into four subclades. Each subclade included accessions of L. indica and L. guineensis intermixed with six other morphologically distinct species, showing the polyphyly of these two species as currently circumscribed. Flower colour, previously used to characterize species, was shown to be unreliable for species identification. Dating analyses estimated that Leea originated in Indochina in the Late Cretaceous (65-86.19 Mya, 95% highest posterior density). The members of the major clades later spread to India, Africa, Madagascar, South-East (SE) Asia and tropical Australasia. Major species diversification occurred in the Neogene, when dynamic environmental and geological changes in SE Asia presented new ecological niches. (C) 2012 The Linnean Society of London, Botanical Journal of the Linnean Society, 2013, 171, 354-375. C1 [Molina, Jeanmaire E.; Struwe, Lena] Rutgers State Univ, Dept Ecol Evolut & Nat Resources, New Brunswick, NJ 08901 USA. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Struwe, Lena] Rutgers State Univ, Dept Plant Biol & Pathol, New Brunswick, NJ 08901 USA. RP Molina, JE (reprint author), Long Isl Univ, Dept Biol, 1 Univ Plaza, Brooklyn, NY 11201 USA. EM jeanmaire.molina@liu.edu FU Rutgers Ecology & Evolution Academic Excellence Award; Systematics Research Fund (from the Linnean Society and the Systematics Association); US Department of Agriculture [USDA/NJAES-NJ17112] FX We thank Stuart Davies, Ed Green, Steven Handel, Karl Kjer and Pete Lowry for providing comments on the first drafts of this manuscript. We would like to thank the herbaria A, CANB, CHRB, DBG, F, K, L, MICH, MO, NY, PUH, UC and US for loan of specimens and/or allowing destructive sampling for DNA extraction. We also thank Leonard Co, Sandra Yap and Ulysses Ferreras for providing plant material and Cynthia Frasier for her technical support. We are also grateful to the Smithsonian Institution for allowing us to conduct part of the molecular work in their labs. This work would have not been possible without the financial support from the Rutgers Ecology & Evolution Academic Excellence Award and the Systematics Research Fund (from the Linnean Society and the Systematics Association). L. S. was also funded by US Department of Agriculture award USDA/NJAES-NJ17112. This paper is dedicated to the memory of Leonard Co, whose mentorship in botany has been invaluable to J.M. NR 96 TC 7 Z9 7 U1 0 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD FEB PY 2013 VL 171 IS 2 BP 354 EP 376 DI 10.1111/j.1095-8339.2012.01320.x PG 23 WC Plant Sciences SC Plant Sciences GA 074AL UT WOS:000313784100004 ER PT J AU Zhu, WD Nie, ZL Wen, J Sun, H AF Zhu, Wei-Dong Nie, Ze-Long Wen, Jun Sun, Hang TI Molecular phylogeny and biogeography of Astilbe (Saxifragaceae) in Asia and eastern North America SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Beringian migration; intercontinental disjunction; south-western China; tropical Asia ID HEUCHERA GROUP SAXIFRAGACEAE; CHLOROPLAST DNA; CLIMATE-CHANGE; SENSU-STRICTO; SEQUENCE DATA; EVOLUTION; INFERENCE; PHYLOGEOGRAPHY; DISJUNCTION; HEMISPHERE AB Phylogenetic analyses were conducted for Astilbe (Saxifragaceae), an Asian/eastern North American disjunct genus, using sequences of nuclear ribosomal internal transcribed spacer (ITS) and plastid matK, trnL-trnF and psbA-trnH regions. The monophyly of Astilbe is well supported by both ITS and plastid sequences. Topological incongruence was detected between the plastid and the ITS trees, particularly concerning the placement of the single North American species, A. biternata, which may be most probably explained by its origin involving hybridization and/or allopolyploidy with plastid capture. In Astilbe, all species with hermaphroditic flowers constitute a well-supported clade; dioecious species form a basal grade to the hermaphroditic clade. Astilbe was estimated to have split with Saxifragopsis from western North America at 20.69 Ma (95% HPD: 12.1430.22 Ma) in the early Miocene. This intercontinental disjunction between Astilbe and Saxifragopsis most likely occurred via the Bering land bridge. The major clade of Astilbe (all species of the genus excluding A. platyphylla) was inferred to have a continental Asian origin. At least three subsequent migrations or dispersals were hypothesized to explain the expansion of Astilbe into North America, Japan and tropical Asian islands. The intercontinental disjunct lineage in Astilbe invokes a hybridization event either in eastern Asia or in North America. This disjunction in Astilbe may be explained by a Beringian migration around 3.54 Ma (95% high posterior density: 1.296.18 Ma) in the late Tertiary, although long-distance dispersal from eastern Asia to North America is also likely. The biogeographical connection between continental Asia, Taiwan, the Philippines and other tropical Asian islands in Astilbe provides evidence for the close floristic affinity between temperate or alpine south-western China and tropical Asia. (C) 2012 The Linnean Society of London, Botanical Journal of the Linnean Society, 2013, 171, 377-394. C1 [Zhu, Wei-Dong; Nie, Ze-Long; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650201, Yunnan, Peoples R China. [Zhu, Wei-Dong] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu; hsun@mail.kib.ac.cn RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU Natural Science Foundation of China [40930209, U1136601, 31129001]; Hundred Talents Program of the Chinese Academy of Sciences [2011312D11022]; NSFC-International (Region) Cooperation Project [31061160184]; Innovation Project of Chinese Academy of Sciences [KSCX2-YW-Z-1019]; John D. and Catherine T. MacArthur Foundation FX This study was supported by grants from the Natural Science Foundation of China (40930209 and U1136601 to H. S., and 31129001 to J.W.), Hundred Talents Program of the Chinese Academy of Sciences (2011312D11022 to H. S.) and NSFC-International (Region) Cooperation Project (31061160184 to H. S.), Innovation Project of Chinese Academy of Sciences (KSCX2-YW-Z-1019 to H. S.), and the John D. and Catherine T. MacArthur Foundation to J.W., R. R. and G. Mueller. We thank Aleck T. Y. Yang and Lawrence Janeway for collecting samples; Nikko Botanical Garden and the Royal Botanical Garden, Edinburgh, for providing leaf materials; Jianwen Zhang, Dengmei Fan and Ying Meng for field assistance; and Rong Li and Jimmy K. Triplett for assistance with data analysis. NR 105 TC 12 Z9 12 U1 4 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD FEB PY 2013 VL 171 IS 2 BP 377 EP 394 DI 10.1111/j.1095-8339.2012.01318.x PG 18 WC Plant Sciences SC Plant Sciences GA 074AL UT WOS:000313784100005 ER PT J AU Huang, WP Sun, H Deng, T Razafimandimbison, SG Nie, ZL Wen, J AF Huang, Wei-Ping Sun, Hang Deng, Tao Razafimandimbison, Sylvain G. Nie, Ze-Long Wen, Jun TI Molecular phylogenetics and biogeography of the eastern Asian-eastern North American disjunct Mitchella and its close relative Damnacanthus (Rubiaceae, Mitchelleae) SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Bering land bridge; intercontinental disjunction ID SUBFAMILY IXOROIDEAE RUBIACEAE; RBCL SEQUENCE DATA; TRNT-F; RPS16 INTRON; COLLETOECEMA RUBIACEAE; RUBIOIDEAE RUBIACEAE; ALLIANCE RUBIACEAE; TRIBE SPERMACOCEAE; MORPHOLOGICAL DATA; POLLEN DIMORPHISM AB Mitchella is a small genus of the Rubiaceae with only two species. It is the only herbaceous semishrub of the family showing a disjunct distribution in eastern Asia and eastern North America, extending to Central America. Its phylogeny and biogeographical diversification remain poorly understood. In this study, we conducted phylogenetic and biogeographical analyses for Mitchella and its close relative Damnacanthus based on sequences of the nuclear internal transcribed spacer (ITS) and four plastid markers (rbcL, atpB-rbcL, rps16 and trnL-F). Mitchella is monophyletic, consisting of an eastern Asian M. undulata clade and a New World M. repens clade. Our results also support Michella as the closest relative to the eastern Asian Damnacanthus. The divergence time between the two intercontinental disjunct Mitchella species was dated to 7.73 Mya, with a 95% highest posterior density (HPD) of 3.14-12.53 Mya, using the Bayesian relaxed clock estimation. Ancestral area reconstructions suggest that the genus originated in eastern Asia. The semishrub Mitchella appears to have arisen from its woody ancestor in eastern Asia and then migrated to North America via the Bering land bridge in the late Miocene. (C) 2013 The Linnean Society of London Botanical Journal of the Linnean Society, 2013, 171, 395-412. C1 [Huang, Wei-Ping; Sun, Hang; Deng, Tao; Nie, Ze-Long] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. [Huang, Wei-Ping] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Razafimandimbison, Sylvain G.] Stockholm Univ, Royal Swedish Acad Sci, Bergius Fdn, SE-10691 Stockholm, Sweden. [Razafimandimbison, Sylvain G.] Stockholm Univ, Dept Bot, SE-10691 Stockholm, Sweden. RP Nie, ZL (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan, Peoples R China. EM niezl@mail.kib.ac.cn; wenj@si.edu RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU Natural Sciences Foundation of China [NSFC 30970193, 30828001, 30625004, 40930209, 31061160184]; One Hundred Talents Program of the Chinese Academy of Sciences [2011312D11022]; NSFC; Yunnan Natural Science Foundation [U1136601]; John D. and Catherine T. MacArthur Foundation; Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution FX This study was supported by grants from the Natural Sciences Foundation of China (NSFC 30970193 to Z.-L. Nie, 30828001 and 30625004 to J. Wen and T. Yi, 40930209 and 31061160184 to H. Sun), the One Hundred Talents Program of the Chinese Academy of Sciences (2011312D11022 to H. Sun), the United Fund of the NSFC and Yunnan Natural Science Foundation (U1136601 to H. Sun) and the John D. and Catherine T. MacArthur Foundation to J. Wen, R. Ree and G. Mueller. Laboratory work was performed at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. Fieldwork in North America was supported by the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. We thank the MEXU herbarium for loaning the sampled Mexican Mitchella repens used in this study. NR 118 TC 8 Z9 8 U1 3 U2 43 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD FEB PY 2013 VL 171 IS 2 BP 395 EP 412 DI 10.1111/j.1095-8339.2012.01321.x PG 18 WC Plant Sciences SC Plant Sciences GA 074AL UT WOS:000313784100006 ER PT J AU Shockey, KM Zimbelman, JR AF Shockey, K. M. Zimbelman, J. R. TI Analysis of transverse aeolian ridge profiles derived from HiRISE images of Mars SO EARTH SURFACE PROCESSES AND LANDFORMS LA English DT Article DE reversing dunes; megaripples; photoclinometry; TARs; geomorphology ID DUNES; PHOTOCLINOMETRY AB Photoclinometry was used to analyze selected High Resolution Imaging Science Experiment (HiRISE) images of Transverse Aeolian Ridges (TARs) on Mars. Sixty Mars profiles have been assessed and a summary of their morphologic characteristics compiled. Measurements collected quantified the symmetry of the feature, the curvature of the crest, flank slopes, width, height and several comparative ratios. Results show that small TARs have physical characteristics generally similar to measurements obtained from lower resolution images of Mars. The HiRISE image data allow for much improved sampling along each feature; the improved resolution reveals relatively few features not seen in earlier studies, but is well suited for topographic sampling. Measured TAR profiles, when scaled by the width of the feature, can be compared to similarly scaled profiles for terrestrial dunes and megaripples. Published 2012. This article is a U.S. Government work and is in the public domain in the USA. C1 [Shockey, K. M.; Zimbelman, J. R.] Smithsonian Inst, Natl Air Space Museum, Ctr Earth Planetary Studies, Washington, DC 20013 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20013 USA. EM zimbelmanj@si.edu FU NASA [NNX08AK90G] FX The comments of Simone Silvestro, an anonymous reviewer, and the Special Issue Editor Mark Bishop were very helpful during revision of the manuscript. This work was supported by NASA Mars Data Analysis Program grant NNX08AK90G (JRZ, PI). NR 21 TC 7 Z9 7 U1 2 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0197-9337 J9 EARTH SURF PROC LAND JI Earth Surf. Process. Landf. PD FEB PY 2013 VL 38 IS 2 BP 179 EP 182 DI 10.1002/esp.3316 PG 4 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 076TP UT WOS:000313981200007 ER PT J AU Maurer, KD Bohrer, G Medvigy, D Wright, SJ AF Maurer, Kyle D. Bohrer, Gil Medvigy, David Joseph Wright, S. TI The timing of abscission affects dispersal distance in a wind-dispersed tropical tree SO FUNCTIONAL ECOLOGY LA English DT Article DE abscission; dispersal; long-distance dispersal; mechanistic modelling; meteorology; seed trap; tropical forest; updraft; wind dispersal ID SEED DISPERSAL; INVASIVE THISTLES; DRIVEN DISPERSAL; PLANT; MECHANISMS; FORESTS; MODEL; TIME; PATTERNS; HABITAT AB Seed dispersal is a short-term phenomenon with long-term consequences for population survival and spread. Physiological mechanisms that target the release of seeds to particular sets of environmental conditions that maximize the probability of long-distance dispersal should evolve if long dispersal distance enhances fitness. In this study, we use high-frequency censuses of seeds actually dispersed, high-frequency within-canopy meteorological observations and long-term measurements of above-canopy wind to investigate the environmental conditions that control the timing of seed abscission at different time-scales for a wind-dispersed tropical tree, Luehea seemannii. We show that seed abscission follows a typical seasonal pattern, is rare at night and is most prevalent during periods of prolonged updrafts, higher temperature, with negative feedback when the heat canopy flux is relatively high. We use phenomenological (super-WALD) and mechanistic (coupled EulerianLagrangian closure) models to estimate the relative effects of the timing of seed release at different subannual temporal scales (secondshours) on the resulting long-term (seasondecade) dispersal kernels. We find that periods of high wind speed increase the probability of long-distance dispersal between 1001000 m, but decrease the probability at distances further than 1000 m relative to unbiased environmental conditions. We also find abscission during updrafts to increase the probability of long-distance dispersal at distances greater than 100 m. Synthesis: We observe preferential abscission during updrafts in a tropical wind-dispersed tree. We use mechanistic models and long-term wind statistics to estimate the dispersal consequences of preferential seed release in specific environmental conditions. We find that the timing of the dispersal season may be influenced by wind conditions that maximize long-distance dispersal; however, there are likely other environmental factors essential for their determination. Our approach provides a method to bridge between small turbulence scales and large ecosystem scales to predict dispersal kernels. These findings shed light on the evolutionary processes that drive optimization of the timing of seed abscission and may be incorporated into plant population movement models to increase their accuracy and predictive power. C1 [Maurer, Kyle D.; Bohrer, Gil] Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA. [Medvigy, David] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Panama. RP Maurer, KD (reprint author), Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA. EM maurer.189@osu.edu RI Bohrer, Gil/A-9731-2008; Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Bohrer, Gil/0000-0002-9209-9540 FU Smithsonian Tropical Research Institute (STRI); French Graduate Fellowship through the Department of Civil, Environmental & Geodetic Engineering; Ohio State University; NSF IGERT through the University of Michigan Biosphere-Atmosphere Research Training (BART) program [DGE-0504552]; NSF [DEB-0918869] FX We thank Ran Nathan for early discussion that helped inspire this study. We thank Mirna Samaniego for data collection assistance. KM was supported by the Smithsonian Tropical Research Institute (STRI), a French Graduate Fellowship through the Department of Civil, Environmental & Geodetic Engineering, an Ohio State University Fellowship and an NSF IGERT Fellowship #DGE-0504552 awarded through the University of Michigan Biosphere-Atmosphere Research Training (BART) program. GB was supported by NSF grant #DEB-0918869. Any opinions, findings and conclusions expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 40 TC 10 Z9 10 U1 3 U2 43 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2013 VL 27 IS 1 BP 208 EP 218 DI 10.1111/1365-2435.12028 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 079JN UT WOS:000314166500022 ER PT J AU Sapir, N Dudley, R AF Sapir, Nir Dudley, Robert TI Implications of floral orientation for flight kinematics and metabolic expenditure of hover-feeding hummingbirds SO FUNCTIONAL ECOLOGY LA English DT Article DE body angle; Calypte anna; head flexion; mass-specific metabolic rate; pendent flowers; respirometry; wingbeat kinematics ID MALE REPRODUCTIVE SUCCESS; POLEMONIUM-VISCOSUM; OXYGEN-CONSUMPTION; POLLEN DISPERSAL; FLOWER SHAPE; HYBRID ZONE; SELECTION; POLLINATION; PLANT; EVOLUTION AB Nectar-bearing flowers are characterized by many different shapes, sizes and orientations, which may affect the way hummingbirds feed from them. Many hummingbird-pollinated flowers are oriented downwards, thereby requiring that trochilids feed while hovering with the bill oriented vertically upward. We measured body orientations, wingbeat kinematics and hovering metabolic rates for Anna's Hummingbirds (Calypte anna) feeding from artificial flowers that were oriented horizontally, tilted 45 degrees downwards and pointing vertically downwards. When feeding from vertically oriented flowers, hummingbirds employed an upright body position combined with dorsal head flexion. Additional kinematic adjustments included an increased stroke plane angle relative to the longitudinal body axis and an increased stroke amplitude deriving from increases in the minimum positional angle of the wingbeat. By contrast, wingbeat frequency, the stroke plane angle relative to horizontal, the ratio of the minimum to maximum positional angles of the wingbeat and the upstroke/downstroke ratio did not vary during feeding from different flower orientations. Metabolic rates increased by an average (+/-SD) of 10.8 (+/-8.8)% for feeding from vertically compared to horizontally oriented flowers. Feeding from pendent flowers comes with a substantial metabolic cost that may influence floral selection by hummingbirds and thus the evolution of associated pollination syndromes. C1 [Sapir, Nir; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Sapir, N (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM nir.sapir@mail.huji.ac.il OI Sapir, Nir/0000-0002-2477-0515 FU NSF [IOS-0837866] FX We thank Yen K. Nguyen and members of the Animal Flight Laboratory at UC Berkeley for their assistance. Bird trapping and housing were under permits from the United States Fish and Wildlife Service (permit no. MB054440-0) and California Department of Fish and Game (permit no. SC-006627). All hummingbird husbandry and research were conducted in compliance with the University of California, Berkeley's Animal Use Protocol R282-0310. This study was supported by an NSF grant (IOS-0837866). The authors declare no conflict of interest. NR 84 TC 5 Z9 5 U1 0 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD FEB PY 2013 VL 27 IS 1 BP 227 EP 235 DI 10.1111/1365-2435.12024 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 079JN UT WOS:000314166500024 ER PT J AU Wright, SJ AF Wright, Stuart Joseph TI The carbon sink in intact tropical forests SO GLOBAL CHANGE BIOLOGY LA English DT Letter ID RESPONSES; BIOMASS; ECOLOGY; LITTER; CO2 C1 Smithsonian Trop Res Inst, Balboa 03092, Panama. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843, Balboa 03092, Panama. EM wrightj@si.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 NR 17 TC 22 Z9 24 U1 3 U2 75 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD FEB PY 2013 VL 19 IS 2 BP 337 EP 339 DI 10.1111/gcb.12052 PG 3 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 080CQ UT WOS:000314219200001 PM 23504773 ER PT J AU Weldon, PJ Cardoza, YJ Vander Meer, RK Hoffmann, WC Daly, JW Spande, TF AF Weldon, Paul J. Cardoza, Yasmin J. Vander Meer, Robert K. Hoffmann, W. Clint Daly, John W. Spande, Thomas F. TI Contact toxicities of anuran skin alkaloids against the fire ant (Solenopsis invicta) SO NATURWISSENSCHAFTEN LA English DT Article DE Alkaloid; Allomone; Ant; Defense; Frog; Toxicity ID DENDROBATID POISON FROGS; PUMILIOTOXIN 251D; DECAHYDROQUINOLINES; MELANOPHRYNISCUS; QUINOLIZIDINES; PYRROLIZIDINES; INDOLIZIDINES; BUFONIDAE; DEFENSE; COMMON AB Nearly 500 alkaloids, representing over 20 structural classes, have been identified from the skin of neotropical poison frogs (Dendrobatidae). These cutaneous compounds, which are derived from arthropod prey of the frogs, generally are believed to deter predators. We tested the red imported fire ant (Solenopsis invicta) for toxicosis following contact with 20 alkaloids (12 structural classes) identified from dendrobatids or other anurans. Individual ants forced to contact the dried residues of 13 compounds exhibited convulsions and/or reduced ambulation. We estimated the cutaneous concentrations of several compounds based on their reported recoveries from skin extracts of free-ranging frogs and our measurements of the skin surface areas of museum specimens. Pumiliotoxin 251D exhibited contact toxicity below its estimated cutaneous concentration in the Ecuadorian frog, Epipedobates anthonyi, an observation consistent with the hypothesized role of this compound in anuran chemical defense. Our results and those of a previous study of mosquitoes indicate that some anuran skin compounds function defensively as contact toxins against arthropods, permeating their exoskeleton. C1 [Weldon, Paul J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Cardoza, Yasmin J.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Vander Meer, Robert K.] ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL 32608 USA. [Hoffmann, W. Clint] ARS, So Plains Agr Res Ctr, USDA, College Stn, TX 77845 USA. [Daly, John W.; Spande, Thomas F.] NIDDKD, Dept Hlth & Human Serv, Bioorgan Chem Lab, NIH, Bethesda, MD 20892 USA. RP Vander Meer, RK (reprint author), ARS, Ctr Med Agr & Vet Entomol, USDA, Gainesville, FL 32608 USA. EM bob.vandermeer@ars.usda.gov NR 41 TC 5 Z9 5 U1 1 U2 56 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD FEB PY 2013 VL 100 IS 2 BP 185 EP 192 DI 10.1007/s00114-013-1010-0 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 080WT UT WOS:000314275500008 PM 23340579 ER PT J AU Bochanski, JJ Savcheva, A West, AA Hawley, SL AF Bochanski, John J. Savcheva, Antonia West, Andrew A. Hawley, Suzanne L. TI MAPPING THE LOCAL HALO: STATISTICAL PARALLAX ANALYSIS OF SDSS LOW-MASS SUBDWARFS SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: kinematics and dynamics; methods: statistical; solar neighborhood; stars: kinematics and dynamics; stars: low-mass; subdwarfs ID DIGITAL SKY SURVEY; STAR SPECTROSCOPIC SURVEY; MILKY-WAY TOMOGRAPHY; RR-LYRAE STARS; PROPER MOTION STARS; 7TH DATA RELEASE; M-DWARFS; SOLAR NEIGHBORHOOD; ABSOLUTE MAGNITUDES; KINEMATIC PROPERTIES AB We present a statistical parallax study of nearly 2000 M subdwarfs with photometry and spectroscopy from the Sloan Digital Sky Survey (SDSS). Statistical parallax analysis yields the mean absolute magnitudes, mean velocities, and velocity ellipsoids for homogenous samples of stars. We selected homogeneous groups of subdwarfs based on their photometric colors and spectral appearance. We examined the color-magnitude relations of low-mass subdwarfs and quantified their dependence on the newly refined metallicity parameter, zeta. We also developed a photometric metallicity parameter, delta((g-r)), based on the g - r and r - z colors of low-mass stars and used it to select stars with similar metallicities. The kinematics of low-mass subdwarfs as a function of color and metallicity were also examined and compared to main-sequence M dwarfs. We find that the SDSS subdwarfs share similar kinematics to the inner halo and thick disk. The color-magnitude relations derived in this analysis will be a powerful tool for identifying and characterizing low-mass metal-poor subdwarfs in future surveys such as Gaia and LSST, making them important and plentiful tracers of the stellar halo. C1 [Bochanski, John J.] Haverford Coll, Haverford, PA 19041 USA. [Bochanski, John J.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Savcheva, Antonia; West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Savcheva, Antonia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hawley, Suzanne L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Bochanski, JJ (reprint author), Haverford Coll, 370 Lancaster Ave, Haverford, PA 19041 USA. EM jbochans@haverford.edu RI West, Andrew/H-3717-2014 FU NSF [AST 11-09273, AST 02-05875, AST 06-07644, AST 1151462]; NASA ADP [NAG5-13111]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank Beth Willman, Steve Boughn, and Pat Boeshaar for helpful discussions. We kindly thank the referee, Ata Sarajedini, for his insightful and helpful suggestions. A. A. W. acknowledges the financial support of NSF grant AST 11-09273. We also gratefully acknowledge the support of NSF grants AST 02-05875, AST 06-07644, and AST 1151462, and NASA ADP grant NAG5-13111.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.; The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 87 TC 17 Z9 17 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 2013 VL 145 IS 2 AR 40 DI 10.1088/0004-6256/145/2/40 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 071FB UT WOS:000313571600014 ER PT J AU Ackermann, M Ajello, M Asano, K Baldini, L Barbiellini, G Baring, MG Bastieri, D Bellazzini, R Blandford, RD Bonamente, E Borgland, AW Bottacini, E Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S D'Ammando, F de Angelis, A de Palma, F Dermer, CD Silva, EDE Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Focke, WB Franckowiak, A Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Granot, J Greiner, J Grenier, IA Grove, JE Guiriec, S Hadasch, D Hanabata, Y Hayashida, M Hays, E Hughes, RE Jackson, MS Jogler, T Johannesson, G Johnson, AS Knodlseder, J Kocevski, D Kuss, M Lande, J Larsson, S Latronico, L Longo, F Loparco, F Lovellette, MN Lubrano, P Mazziotta, MN McEnery, JE Mehault, J Meszaros, P Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Moretti, E Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Norris, JP Nuss, E Nymark, T Ohno, M Ohsugi, T Omodei, N Orienti, M Orlando, E Paneque, D Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Racusin, JL Raino, S Rando, R Razzano, M Razzaque, S Reimer, A Reimer, O Romoli, C Roth, M Ryde, F Sanchez, DA Sgro, C Siskind, EJ Sonbas, E Spinelli, P Stamatikos, M Takahashi, H Tanaka, T Thayer, JG Thayer, JB Tibaldo, L Tinivella, M Tosti, G Troja, E Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Yang, Z Gruber, D Bhat, PN Bissaldi, E Briggs, MS Burgess, JM Connaughton, V Foley, S Kippen, RM Kouveliotou, C McBreen, S McGlynn, S Paciesas, WS Pelassa, V Preece, R Rau, A van der Horst, AJ von Kienlin, A Kann, DA Filgas, R Klose, S Kruhler, T Fukui, A Sako, T Tristram, PJ Oates, SR Ukwatta, TN Littlejohns, O AF Ackermann, M. Ajello, M. Asano, K. Baldini, L. Barbiellini, G. Baring, M. G. Bastieri, D. Bellazzini, R. Blandford, R. D. Bonamente, E. Borgland, A. W. Bottacini, E. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Focke, W. B. Franckowiak, A. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Granot, J. Greiner, J. Grenier, I. A. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Hayashida, M. Hays, E. Hughes, R. E. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Knoedlseder, J. Kocevski, D. Kuss, M. Lande, J. Larsson, S. Latronico, L. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Mazziotta, M. N. McEnery, J. E. Mehault, J. Meszaros, P. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Moretti, E. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Norris, J. P. Nuss, E. Nymark, T. Ohno, M. Ohsugi, T. Omodei, N. Orienti, M. Orlando, E. Paneque, D. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Racusin, J. L. Raino, S. Rando, R. Razzano, M. Razzaque, S. Reimer, A. Reimer, O. Romoli, C. Roth, M. Ryde, F. Sanchez, D. A. Sgro, C. Siskind, E. J. Sonbas, E. Spinelli, P. Stamatikos, M. Takahashi, H. Tanaka, T. Thayer, J. G. Thayer, J. B. Tibaldo, L. Tinivella, M. Tosti, G. Troja, E. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Yang, Z. Gruber, D. Bhat, P. N. Bissaldi, E. Briggs, M. S. Burgess, J. M. Connaughton, V. Foley, S. Kippen, R. M. Kouveliotou, C. McBreen, S. McGlynn, S. Paciesas, W. S. Pelassa, V. Preece, R. Rau, A. van der Horst, A. J. von Kienlin, A. Kann, D. A. Filgas, R. Klose, S. Kruhler, T. Fukui, A. Sako, T. Tristram, P. J. Oates, S. R. Ukwatta, T. N. Littlejohns, O. TI MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB110731A) ID GAMMA-RAY BURST; HIGH-ENERGY EMISSION; LARGE-AREA TELESCOPE; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; INTERNAL SHOCK MODEL; LIGHT CURVES; OPTICAL AFTERGLOWS; FERMI OBSERVATIONS; SPECTRAL CATALOG; PEAK LUMINOSITY AB We report on the multiwavelength observations of the bright, long gamma-ray burst GRB 110731A, by the Fermi and Swift observatories, and by the MOA and GROND optical telescopes. The analysis of the prompt phase reveals that GRB 110731A shares many features with bright Large Area Telescope bursts observed by Fermi during the first three years on-orbit: a light curve with short time variability across the whole energy range during the prompt phase, delayed onset of the emission above 100 MeV, extra power-law component and temporally extended high-energy emission. In addition, this is the first GRB for which simultaneous GeV, X-ray, and optical data are available over multiple epochs beginning just after the trigger time and extending for more than 800 s, allowing temporal and spectral analysis in different epochs that favor emission from the forward shock in a wind-type medium. The observed temporally extended GeV emission is most likely part of the high-energy end of the afterglow emission. Both the single-zone pair transparency constraint for the prompt signal and the spectral and temporal analysis of the forward-shock afterglow emission independently lead to an estimate of the bulk Lorentz factor of the jet Gamma similar to 500-550. C1 [Ackermann, M.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.; Blandford, R. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Johnson, A. S.; Kocevski, D.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Ajello, M.; Blandford, R. D.; Borgland, A. W.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Jogler, T.; Johnson, A. S.; Kocevski, D.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Omodei, N.; Orlando, E.; Paneque, D.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Asano, K.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro, Tokyo 1528551, Japan. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Pivato, G.; Rando, R.; Romoli, C.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; D'Ammando, F.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Ciprini, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.] IEEE CSIC, Inst Ciencies Espai, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chaves, R. C. G.; Grenier, I. A.; Naumann-Godo, M.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Cohen-Tanugi, J.; Mehault, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Moretti, E.; Nymark, T.; Ryde, F.; Yang, Z.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Hanabata, Y.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Gehrels, N.; Hays, E.; McEnery, J. E.; Perkins, J. S.; Racusin, J. L.; Sonbas, E.; Stamatikos, M.; Troja, E.; Ukwatta, T. N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Granot, J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Greiner, J.; Gruber, D.; Foley, S.; McBreen, S.; Rau, A.; von Kienlin, A.; Kann, D. A.; Filgas, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Guiriec, S.; Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Connaughton, V.; Paciesas, W. S.; Pelassa, V.; Preece, R.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hughes, R. E.; Stamatikos, M.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Jackson, M. S.; Moretti, E.; Nymark, T.; Ryde, F.] AlbaNova, Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Knoedlseder, J.] Univ Toulouse, UPS OMP, IRAP, GAHEC, Toulouse, France. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Meszaros, P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Norris, J. P.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.] Boise State Univ, Dept Phys, Boise, ID 83725 USA. [Ohno, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Sonbas, E.] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey. [Sonbas, E.] USRA, Columbia, MD 21044 USA. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-10133 Turin, Italy. [Foley, S.; McBreen, S.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kouveliotou, C.; van der Horst, A. J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [McGlynn, S.; Kann, D. A.] Tech Univ Munich, Exzellenzcluster Universe, D-85748 Garching, Germany. [Kann, D. A.; Klose, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Filgas, R.] Czech Tech Univ, Inst Expt & Appl Phys, Prague 12800, Czech Republic. [Kruhler, T.] Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Fukui, A.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Sako, T.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Tristram, P. J.] Victoria Univ Wellington, SCPS, Wellington Nz, New Zealand. [Oates, S. R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Ukwatta, T. N.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Littlejohns, O.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM johan.bregeon@pi.infn.it; kocevski@slac.stanford.edu; srazzaque@ssd5.nrl.navy.mil; eleonora.troja@nasa.gov; dgruber@mpe.mpg.de RI Bissaldi, Elisabetta/K-7911-2016; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Orlando, E/R-5594-2016 OI Moretti, Elena/0000-0001-5477-9097; Gasparrini, Dario/0000-0002-5064-9495; Kruehler, Thomas/0000-0002-8682-2384; Baldini, Luca/0000-0002-9785-7726; Giordano, Francesco/0000-0002-8651-2394; Preece, Robert/0000-0003-1626-7335; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Burgess, James/0000-0003-3345-9515; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; McBreen, Sheila/0000-0002-1477-618X; Bissaldi, Elisabetta/0000-0001-9935-8106; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; FU K. A. Wallenberg Foundation; UK Space Agency; DFG [HA 1850/28-1, Kl 766/16-1]; European Commission under the Marie Curie Intra-European Fellowship Programme; MPE; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; We gratefully acknowledge the contributions of dozens of members of the Swift team at OAB, PSU, UL, GSFC, ASDC, and MSSL and our subcontractors, who helped make these instruments possible. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. S.R.O. acknowledges support from the UK Space Agency.; Part of the funding for GROND (both hardware and personnel) was generously granted from the Leibniz-Prize to Professor G. Hasinger (DFG grant HA 1850/28-1). T. K. acknowledges support by the European Commission under the Marie Curie Intra-European Fellowship Programme. D. A. K. and S. K. acknowledge support by grant DFG Kl 766/16-1. D. A. K. is grateful for travel funding support through the MPE.; We acknowledge the MOA collaboration to permit target of opportunity observations for GRB afterglow. We also acknowledge the University of Canterbury for allowing MOA to use the B&C telescope. This work was partially supported by the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. NR 99 TC 28 Z9 28 U1 0 U2 30 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 71 DI 10.1088/0004-637X/763/2/71 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800002 ER PT J AU Benson, BA de Haan, T Dudley, JP Reichardt, CL Aird, KA Andersson, K Armstrong, R Ashby, MLN Bautz, M Bayliss, M Bazin, G Bleem, LE Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S Dobbs, MA Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, N High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Padin, S Plagge, T Pryke, C Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K Stubbs, CW Suhada, R van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Benson, B. A. de Haan, T. Dudley, J. P. Reichardt, C. L. Aird, K. A. Andersson, K. Armstrong, R. Ashby, M. L. N. Bautz, M. Bayliss, M. Bazin, G. Bleem, L. E. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Padin, S. Plagge, T. Pryke, C. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Suhada, R. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI COSMOLOGICAL CONSTRAINTS FROM SUNYAEV-ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg(2) OF THE SOUTH POLE TELESCOPE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; large-scale structure of universe ID MASSIVE GALAXY CLUSTERS; MICROWAVE BACKGROUND ANISOTROPIES; HUBBLE-SPACE-TELESCOPE; WEAK-LENSING MASSES; GREATER-THAN 1; SCALING RELATIONS; OBSERVED GROWTH; POWER SPECTRUM; STAR-FORMATION; DARK ENERGY AB We usemeasurements from the South Pole Telescope (SPT) Sunyaev-Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z > 0.3 from the first 178 deg(2) of the 2500 deg(2) SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM-Newton. Assuming a spatially flat Lambda CDM cosmological model, we find the SPT cluster sample constrains sigma(8)(Omega(m)/0.25)(0.30) = 0.785 +/- 0.037. In combination with measurements of the cosmic microwave background (CMB) power spectrum from the SPT and the seven-year Wilkinson Microwave Anisotropy Probe data, the SPT cluster sample constrains sigma(8) = 0.795 +/- 0.016 and Omega(m) = 0.255 +/- 0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the Lambda CDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (Sigma m(nu)), the effective number of relativistic species (N-eff), and a primordial non-Gaussianity (f(NL)). We find that adding the SPT cluster data significantly improves the constraints on w and Sigma m(nu) beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w = -0.973 +/- 0.063 and the sum of neutrino masses Sigma m(nu) < 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. Assuming a Lambda CDM model with a free N-eff and Sigma m(nu), we measure N-eff = 3.91 +/- 0.42 and constrain Sigma m(nu) < 0.63 eV at 95% confidence. We also use the SPT cluster sample to constrain f(NL) = -220 +/- 317, consistent with zero primordial non-Gaussianity. Finally, we discuss the current systematic limitations due to the cluster mass calibration, and future improvements for the recently completed 2500 deg(2) SPT-SZ survey. The survey has detected similar to 500 clusters with a median redshift of similar to 0.5 and a median mass of similar to 2.3 x 10(14) M-circle dot h(-1) and, when combined with an improved cluster mass calibration and existing external cosmological data sets will significantly improve constraints on w. C1 [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [de Haan, T.; Dudley, J. P.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Reichardt, C. L.; George, E. M.; Harrington, N.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Andersson, K.; Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Andersson, K.; Bautz, M.; McDonald, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Ashby, M. L. N.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Suhada, R.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Brodwin, M.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Marrone, D. P.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] PUC, Dept Astron & Astrofs, Santiago 22, Chile. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Marrone, D. P.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Benson, BA (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. EM bbenson@kicp.uchicago.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA [12800071, 12800088, 13800883, NAS8-03060, NAS 8-03060]; Chandra X-ray Observatory Center; Blanco 4 m at Cerro Tololo Interamerican Observatories [2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598]; VLT programs [086.A-0741, 286.A-5021]; Gemini program [GS-2009B-Q-16]; NASA Office of Space Science; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA; Excellence Cluster Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation; JPL/Caltech FX The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile. Support for X-ray analysis was provided by NASA through Chandra Award Numbers 12800071, 12800088, and 13800883 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. Optical imaging data from the Blanco 4 m at Cerro Tololo Interamerican Observatories (programs 2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598) and spectroscopic observations from VLT programs 086.A-0741 and 286.A-5021 and Gemini program GS-2009B-Q-16 were included in this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. R.J.F. is supported by a Clay Fellowship. B.A.B. is supported by a KICP Fellowship, M.B. acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M.D. acknowledges support from an Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support from the Smithsonian Institution, and B.S. acknowledges support from the Brinson Foundation. NR 98 TC 132 Z9 132 U1 2 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 147 DI 10.1088/0004-637X/763/2/147 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800078 ER PT J AU Binder, B Williams, BF Eracleous, M Gaetz, TJ Kong, AKH Skillman, ED Weisz, DR AF Binder, B. Williams, B. F. Eracleous, M. Gaetz, T. J. Kong, A. K. H. Skillman, E. D. Weisz, D. R. TI THE CHANDRA LOCAL VOLUME SURVEY: THE X-RAY POINT-SOURCE POPULATION OF NGC 404 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; galaxies: individual (NGC 404); surveys; X-rays: galaxies ID EARLY-TYPE GALAXIES; ALL-SKY SURVEY; LUMINOSITY FUNCTION; SOURCE CATALOG; ELLIPTIC GALAXIES; DEEP CHANDRA; CENTRAL REGION; M33 CHASEM33; ACIS SURVEY; BLACK-HOLE AB We present a comprehensive X-ray point-source catalog of NGC 404 obtained as part of the Chandra Local Volume Survey. A new 97 ks Chandra ACIS-S observation of NGC 404 was combined with archival observations for a total exposure of similar to 123 ks. Our survey yields 74 highly significant X-ray point sources and is sensitive to a limiting unabsorbed luminosity of similar to 6 x 10(35) erg s(-1) in the 0.35-8 keV band. To constrain the nature of each X-ray source, cross-correlations with multi-wavelength data were generated. We searched overlapping Hubble Space Telescope observations for optical counterparts to our X-ray detections, but find only two X-ray sources with candidate optical counterparts. We find 21 likely low-mass X-ray binaries (LMXBs), although this number is a lower limit due to the difficulties in separating LMXBs from background active galactic nuclei. The X-ray luminosity functions (XLFs) in both the soft and hard energy bands are presented. The XLFs in the soft band (0.5-2 keV) and the hard band (2-8 keV) have a limiting luminosity at the 90% completeness limit of 10(35) erg s(-1) and 10(36) erg s(-1), respectively, significantly lower than previous X-ray studies of NGC 404. We find the XLFs to be consistent with those of other X-ray populations dominated by LMXBs. However, the number of luminous (>10(37) erg s(-1)) X-ray sources per unit stellar mass in NGC 404 is lower than is observed for other galaxies. The relative lack of luminous XRBs may be due to a population of LMXBs with main-sequence companions formed during an epoch of elevated star formation similar to 0.5 Gyr ago. C1 [Binder, B.; Williams, B. F.; Weisz, D. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Eracleous, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Eracleous, M.] Penn State Univ, Ctr Gravitat Wave Phys, Davey Lab 525, University Pk, PA 16802 USA. [Gaetz, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Skillman, E. D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Binder, B (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. FU National Aeronautics and Space Administration through Chandra Award [G01-12118X]; Chandra X-Ray Observatory Center; National Aeronautics Space Administration [NAS8-03060]; NASA [NAS8-03060] FX We thank the anonymous referee for numerous detailed and thoughtful comments and suggestions. We also thank the editor, Eric Feigelson, for helpful comments. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G01-12118X issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. T.J.G acknowledges support under NASA contract NAS8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 68 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 128 DI 10.1088/0004-637X/763/2/128 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800059 ER PT J AU Campbell, H D'Andrea, CB Nichol, RC Sako, M Smith, M Lampeitl, H Olmstead, MD Bassett, B Biswas, R Brown, P Cinabro, D Dawson, KS Dilday, B Foley, RJ Frieman, JA Garnavich, P Hlozek, R Jha, SW Kuhlmann, S Kunz, M Marriner, J Miquel, R Richmond, M Riess, A Schneider, DP Sollerman, J Taylor, M Zhao, GB AF Campbell, Heather D'Andrea, Chris B. Nichol, Robert C. Sako, Masao Smith, Mathew Lampeitl, Hubert Olmstead, Matthew D. Bassett, Bruce Biswas, Rahul Brown, Peter Cinabro, David Dawson, Kyle S. Dilday, Ben Foley, Ryan J. Frieman, Joshua A. Garnavich, Peter Hlozek, Renee Jha, Saurabh W. Kuhlmann, Steve Kunz, Martin Marriner, John Miquel, Ramon Richmond, Michael Riess, Adam Schneider, Donald P. Sollerman, Jesper Taylor, Matt Zhao, Gong-Bo TI COSMOLOGY WITH PHOTOMETRICALLY CLASSIFIED TYPE Ia SUPERNOVAE FROM THE SDSS-II SUPERNOVA SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; distance scale; supernovae: general; surveys ID DIGITAL SKY SURVEY; HUBBLE-SPACE-TELESCOPE; OSCILLATION SPECTROSCOPIC SURVEY; HIGH-REDSHIFT SUPERNOVAE; BVRI LIGHT CURVES; DARK-ENERGY CONSTRAINTS; HOST GALAXIES; LEGACY SURVEY; ULTRAVIOLET-SPECTRA; DATA RELEASE AB We present the cosmological analysis of 752 photometrically classified Type Ia Supernovae (SNe Ia) obtained from the full Sloan Digital Sky Survey II (SDSS-II) Supernova (SN) Survey, supplemented with host-galaxy spectroscopy from the SDSS-III Baryon Oscillation Spectroscopic Survey. Our photometric-classification method is based on the SN classification technique of Sako et al., aided by host-galaxy redshifts (0.05 < z < 0.55). SuperNova ANAlysis simulations of our methodology estimate that we have an SN Ia classification efficiency of 70.8%, with only 3.9% contamination from core-collapse (non-Ia) SNe. We demonstrate that this level of contamination has no effect on our cosmological constraints. We quantify and correct for our selection effects (e. g., Malmquist bias) using simulations. When fitting to a flat.CDM cosmological model, we find that our photometric sample alone gives Omega(m) = 0.24(-0.05)(+0.07) (statistical errors only). If we relax the constraint on flatness, then our sample provides competitive joint statistical constraints on Omega(m) and Omega(Lambda), comparable to those derived from the spectroscopically confirmed Three-year Supernova Legacy Survey (SNLS3). Using only our data, the statistics-only result favors an accelerating universe at 99.96% confidence. Assuming a constant wCDM cosmological model, and combining with H-0, cosmic microwave background, and luminous red galaxy data, we obtain w = -0.96(-0.10)(+0.10), Omega(m) = 0.29(-0.02)(+0.02), and Omega(k) = 0.00(-0.02)(+0.03)(statistical errors only), which is competitive with similar spectroscopically confirmed SNe Ia analyses. Overall this comparison is reassuring, considering the lower redshift leverage of the SDSS-II SN sample (z < 0.55) and the lack of spectroscopic confirmation used herein. These results demonstrate the potential of photometrically classified SN Ia samples in improving cosmological constraints. C1 [Campbell, Heather; D'Andrea, Chris B.; Nichol, Robert C.; Smith, Mathew; Lampeitl, Hubert; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Smith, Mathew] Univ Western Cape, Dept Phys, ZA-7530 Cape Town, South Africa. [Olmstead, Matthew D.; Brown, Peter; Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Bassett, Bruce] Univ Cape Town, Dept Math, ZA-7925 Cape Town, South Africa. [Bassett, Bruce] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Bassett, Bruce; Kunz, Martin] African Inst Math Sci, ZA-7945 Cape Town, South Africa. [Biswas, Rahul; Kuhlmann, Steve] Argonne Natl Lab, Argonne, IL 60439 USA. [Brown, Peter] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Cinabro, David; Taylor, Matt] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48126 USA. [Dilday, Ben] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Dilday, Ben] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, Joshua A.; Marriner, John] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Hlozek, Renee] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Kunz, Martin] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland. [Kunz, Martin] Univ Geneva, Ctr Astroparticle Phys, CH-1211 Geneva 4, Switzerland. [Miquel, Ramon] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Bellaterra, Barcelona, Spain. [Miquel, Ramon] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Richmond, Michael] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Riess, Adam] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Riess, Adam] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Sollerman, Jesper] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Campbell, H (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. EM Heather.Campbell@port.ac.uk OI Bassett, Bruce/0000-0001-7700-1069; Sollerman, Jesper/0000-0003-1546-6615 FU ICG; SEPNet; University of Portsmouth; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; Cambridge University; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; Princeton University; United States Naval Observatory; University of Washington; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; University of Florida; French Participation Group; German Participation Group; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New York University; Pennsylvania State University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; Yale University FX We thank the referee, whose diligent but friendly review greatly improved the quality of this paper. We thank Mark Sullivan for many helpful discussions during the lifetime of this project and analysis. We thank Julien Guy for sending us the data plotted in Figure 24, and Alex Conley for his advice with the simple_cosfitter. We thank Michael Wood-Vasey and Raffaele Flaminio for helpful discussions on earlier drafts of the paper. Additionally, we thank Alex Kim and Rick Kessler for their useful inputs on advanced draft of the paper. We thank Marisa March for her comments on grid versus MCMC search methods. We thank Emma Beynon for her advice with ComsoMC, Rob Crittenden, and David Bacon for useful discussions on statistics. Numerical computations were done on the Sciama High Performance Computer (HPC) cluster, which is supported by the ICG, SEPNet and the University of Portsmouth. We thank Gary Burton for his help in using Sciama HPC; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 147 TC 39 Z9 39 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 88 DI 10.1088/0004-637X/763/2/88 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800019 ER PT J AU Kirkpatrick, A Pope, A Charmandaris, V Daddi, E Elbaz, D Hwang, HS Pannella, M Scott, D Altieri, B Aussel, H Coia, D Dannerbauer, H Dasyra, K Dickinson, M Kartaltepe, J Leiton, R Magdis, G Magnelli, B Popesso, P Valtchanov, I AF Kirkpatrick, Allison Pope, Alexandra Charmandaris, Vassilis Daddi, Emmanuele Elbaz, David Hwang, Ho Seong Pannella, Maurilio Scott, Douglas Altieri, Bruno Aussel, Herve Coia, Daniela Dannerbauer, Helmut Dasyra, Kalliopi Dickinson, Mark Kartaltepe, Jeyhan Leiton, Roger Magdis, Georgios Magnelli, Benjamin Popesso, Paola Valtchanov, Ivan TI GOODS-HERSCHEL: SEPARATING HIGH-REDSHIFT ACTIVE GALACTIC NUCLEI AND STAR-FORMING GALAXIES USING INFRARED COLOR DIAGNOSTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: high-redshift; galaxies: star formation; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; MS SOURCE CATALOGS; FIELD NORTH SURVEY; SIMILAR-TO 2; MIDINFRARED SELECTION; STARBURST GALAXIES; CHANDRA; POPULATION; SOUTH; VIEW AB We have compiled a large sample of 151 high-redshift (z = 0.5-4) galaxies selected at 24 mu m (S-24 > 100 mu Jy) in the GOODS-N and ECDFS fields for which we have deep Spitzer IRS spectroscopy, allowing us to decompose the mid-infrared spectrum into contributions from star formation and activity in the galactic nuclei. In addition, we have a wealth of photometric data from Spitzer IRAC/MIPS and Herschel PACS/SPIRE. We explore how effective different infrared color combinations are at separating our mid-IR spectroscopically determined active galactic nuclei from our star-forming galaxies. We look in depth at existing IRAC color diagnostics, and we explore new color-color diagnostics combining mid-IR, far-IR, and near-IR photometry, since these combinations provide the most detail about the shape of a source's IR spectrum. An added benefit of using a color that combines far-IR and mid-IR photometry is that it is indicative of the power source driving the IR luminosity. For our data set, the optimal color selections are S-250/S-24 versus S-8/S-3.6 and S-100/S-24 versus S-8/S-3.6; both diagnostics have similar to 10% contamination rate in the regions occupied primarily by star-forming galaxies and active galactic nuclei, respectively. Based on the low contamination rate, these two new IR color-color diagnostics are ideal for estimating both the mid-IR power source of a galaxy when spectroscopy is unavailable and the dominant power source contributing to the IR luminosity. In the absence of far-IR data, we present color diagnostics using the Wide-field Infrared Survey Explorer mid-IR bands which can efficiently select out high-z (z similar to 2) star-forming galaxies. C1 [Kirkpatrick, Allison; Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Charmandaris, Vassilis] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Charmandaris, Vassilis] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Greece. [Charmandaris, Vassilis] Fdn Res & Technol Hellas, IESL, GR-71110 Iraklion, Greece. [Charmandaris, Vassilis] Observ Paris, F-75014 Paris, France. [Daddi, Emmanuele; Elbaz, David; Pannella, Maurilio; Aussel, Herve; Dasyra, Kalliopi; Leiton, Roger] Univ Paris Diderot, CEA DSM CNRS, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Scott, Douglas; Magnelli, Benjamin; Popesso, Paola] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Altieri, Bruno; Coia, Daniela; Valtchanov, Ivan] European Space Astron Ctr, Herschel Sci Ctr, E-28691 Madrid, Spain. [Dannerbauer, Helmut] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Dickinson, Mark; Kartaltepe, Jeyhan] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Leiton, Roger] Univ Concepcion, Dept Astron, Concepcion, Chile. [Magdis, Georgios] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Kirkpatrick, A (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. RI Charmandaris, Vassilis/A-7196-2008; Magdis, Georgios/C-7295-2014; Daddi, Emanuele/D-1649-2012; OI Charmandaris, Vassilis/0000-0002-2688-1956; Magdis, Georgios/0000-0002-4872-2294; Daddi, Emanuele/0000-0002-3331-9590; Leiton, Roger/0000-0002-0744-489X; Dasyra, Kalliopi/0000-0002-1482-2203; Scott, Douglas/0000-0002-6878-9840; Pannella, Maurilio/0000-0003-3738-3976; Altieri, Bruno/0000-0003-3936-0284 FU NASA through JPL/Caltech FX We thank the anonymous referee for the careful reading of this paper and the insightful comments provided. This work is based in part on observations made with Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA, and the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 42 TC 19 Z9 19 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 123 DI 10.1088/0004-637X/763/2/123 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800054 ER PT J AU Kocsis, B AF Kocsis, Bence TI HIGH-FREQUENCY GRAVITATIONAL WAVES FROM SUPERMASSIVE BLACK HOLES: PROSPECTS FOR LIGO-VIRGO DETECTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitational lensing: strong; gravitational waves; relativistic processes ID ACTIVE GALACTIC NUCLEI; QUASI-NORMAL MODES; BASE-LINE ARRAY; STANDARD SIRENS; ELECTROMAGNETIC COUNTERPARTS; ACCRETION DISC; RADIATION; BINARIES; SEARCH; JETS AB It is commonly assumed that ground-based gravitational wave (GW) instruments will not be sensitive to supermassive black holes (SMBHs) because the characteristic GW frequencies are far below the similar to 10-1000 Hz sensitivity bands of terrestrial detectors. Here, however, we explore the possibility of SMBH GWs to leak to higher frequencies. In particular, if the high-frequency spectral tail asymptotes to (h) over tilde (f) proportional to f(-alpha), where alpha <= 2, then the spectral amplitude is a constant or increasing function of the mass M at a fixed frequency f >> c(3)/GM. This will happen if the time-domain waveform or its derivative exhibits a discontinuity. Ground-based instruments could search for these universal spectral tails to detect or rule out such features irrespective of their origin. We identify the following processes which may generate high-frequency signals: (1) gravitational bremsstrahlung of ultrarelativistic objects in the vicinity of an SMBH, (2) ringdown modes excited by an external process that has a high-frequency component or terminates abruptly, and (3) gravitational lensing echoes and diffraction. We estimate the order of magnitude of the detection signal-to-noise ratio for each mechanism (1, 2, and 3) as a function of the waveform parameters. In particular for (3), SMBHs produce GW echoes of inspiraling stellar mass binaries in galactic nuclei with a delay of a few minutes to hours. The lensed primary signal and GW echo are both amplified if the binary is within a similar to 10 deg (r/100M)(-1/2) cone behind the SMBH relative to the line of sight at a distance r from the SMBH. For the rest of the binaries near SMBHs, the amplitude of the GW echo is similar to 0.1(r/100M)(-1) of the primary signal on average. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bkocsis@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NASA [PF9-00063]; Chandra X-ray Center [NAS8-03060] FX I thank Emanuele Berti, Ryan O'Leary, Dan Holz, Lorenzo Sironi, Zoltan Haiman, and Scott Tremaine for discussions, and Nico Yunes and Cole Miller for useful comments after carefully reading the manuscript. The author acknowledges support by NASA through Einstein Postdoctoral Fellowship grant number PF9-00063 awarded by the Chandra X-ray Center (operated by the SAO, contract NAS8-03060). NR 81 TC 1 Z9 1 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 122 DI 10.1088/0004-637X/763/2/122 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800053 ER PT J AU Reichardt, CL Stalder, B Bleem, LE Montroy, TE Aird, KA Andersson, K Armstrong, R Ashby, MLN Bautz, M Bayliss, M Bazin, G Benson, BA Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Murray, SS Natoli, T Padin, S Plagge, T Pryke, C Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Staniszewski, Z Stark, AA Story, K Stubbs, CW Suhada, R van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Reichardt, C. L. Stalder, B. Bleem, L. E. Montroy, T. E. Aird, K. A. Andersson, K. Armstrong, R. Ashby, M. L. N. Bautz, M. Bayliss, M. Bazin, G. Benson, B. A. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Murray, S. S. Natoli, T. Padin, S. Plagge, T. Pryke, C. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Suhada, R. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV-ZEL'DOVICH EFFECT IN THE FIRST 720 SQUARE DEGREES OF THE SOUTH POLE TELESCOPE SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: individual; large-scale structure of universe ID MICROWAVE BACKGROUND ANISOTROPIES; ALL-SKY SURVEY; BLANCO COSMOLOGY SURVEY; HUBBLE-SPACE-TELESCOPE; GREATER-THAN 1; DATA RELEASE; POWER SPECTRUM; SOURCE CATALOG; RICH CLUSTERS; SAMPLE AB We present a catalog of galaxy cluster candidates, selected through their Sunyaev-Zel'dovich (SZ) effect signature in the first 720 deg(2) of the South Pole Telescope (SPT) survey. This area was mapped with the SPT in the 2008 and 2009 austral winters to a depth of similar to 18 mu K-CMB-arcmin at 150 GHz; 550 deg(2) of it was also mapped to similar to 44 mu K-CMB-arcmin at 95 GHz. Based on optical imaging of all 224 candidates and near-infrared imaging of the majority of candidates, we have found optical and/or infrared counterparts for 158, which we then classify as confirmed galaxy clusters. Of these 158 clusters, 135 were first identified as clusters in SPT data, including 117 new discoveries reported in this work. This catalog triples the number of confirmed galaxy clusters discovered through the SZ effect. We report photometrically derived (and in some cases spectroscopic) redshifts for confirmed clusters and redshift lower limits for the remaining candidates. The catalog extends to high redshift with a median redshift of z = 0.55 and maximum confirmed redshift of z = 1.37. Forty-five of the clusters have counterparts in the ROSAT bright or faint source catalogs from which we estimate X-ray fluxes. Based on simulations, we expect the catalog to be nearly 100% complete above M-500 approximate to 5 x 10(14) M-circle dot h(70)(-1) at z greater than or similar to 0.6. There are 121 candidates detected at signal-to-noise ratio greater than five, at which the catalog purity is measured to be 95%. From this high-purity subsample, we exclude the z < 0.3 clusters and use the remaining 100 candidates to improve cosmological constraints following the method presented by Benson et al. Adding the cluster data to CMB + BAO + H-0 data leads to a preference for non-zero neutrino masses while only slightly reducing the upper limit on the sum of neutrino masses to Sigma m(nu) < 0.38 eV (95% CL). For a spatially flat wCDM cosmological model, the addition of this catalog to the CMB + BAO + H-0 + SNe results yields sigma(8) = 0.807 +/- 0.027 and w = -1.010 +/- 0.058, improving the constraints on these parameters by a factor of 1.4 and 1.3, respectively. The larger cluster catalog presented in this work leads to slight improvements in cosmological constraints from those presented by Benson et al. These cosmological constraints are currently limited by uncertainty in the cluster mass calibration, not the size or quality of the cluster catalog. A multi-wavelength observation program to improve the cluster mass calibration will make it possible to realize the full potential of the final 2500 deg(2) SPT cluster catalog to constrain cosmology. C1 [Stalder, B.; Ashby, M. L. N.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bleem, L. E.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Andersson, K.; Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Andersson, K.; Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] PUC, Dept Astron & Astrofis, Santiago 22, Chile. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Reichardt, C. L.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RP Reichardt, CL (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. EM cr@bolo.berkeley.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012 OI Marrone, Daniel/0000-0002-2367-1080; Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996; Stubbs, Christopher/0000-0003-0347-1724 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA [NAS 8-03060, NAS8-03060]; NASA through JPL/Caltech; Excellence Cluster Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation; NASA through Chandra Award [12800071, 12800088, G02-13006A]; Chandra X-ray Observatory Center; Blanco 4 m at Cerro Tololo Inter-American Observatories [2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598]; VLT programs [086.A-0741, 286.A-5021]; Gemini program [GS-2009B-Q-16]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. R.J.F. is supported by a Clay Fellowship. B. A. B is supported by a KICP Fellowship, M. Bautz acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship, W. F. and C.J. acknowledge support from the Smithsonian Institution, and B. S. acknowledges support from the Brinson Foundation.; Support for X-ray analysis was provided by NASA through Chandra Award Numbers 12800071, 12800088, and G02-13006A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. Optical imaging data from the Blanco 4 m at Cerro Tololo Inter-American Observatories (programs 2005B-0043, 2009B-0400, 2010A-0441, and 2010B-0598) and spectroscopic observations from VLT programs 086.A-0741 and 286.A-5021 and Gemini program GS-2009B-Q-16 were included in this work. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile.; We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 93 TC 150 Z9 150 U1 2 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 127 DI 10.1088/0004-637X/763/2/127 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800058 ER PT J AU Stalder, B Ruel, J Suhada, R Brodwin, M Aird, KA Andersson, K Armstrong, R Ashby, MLN Bautz, M Bayliss, M Bazin, G Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gettings, D Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Nurgaliev, D Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Stalder, B. Ruel, J. Suhada, R. Brodwin, M. Aird, K. A. Andersson, K. Armstrong, R. Ashby, M. L. N. Bautz, M. Bayliss, M. Bazin, G. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gettings, D. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Nurgaliev, D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI SPT-CL J0205-5829: A z=1.32 EVOLVED MASSIVE GALAXY CLUSTER IN THE SOUTH POLE TELESCOPE SUNYAEV-ZEL'DOVICH EFFECT SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies: clusters: individual (SPT-CL J0205-5829); galaxies: evolution; galaxies: formation; large-scale structure of universe ID IRAC SHALLOW SURVEY; GREATER-THAN 1; HIGH-REDSHIFT; RED-SEQUENCE; XMM-NEWTON; SPECTROSCOPIC CONFIRMATION; COOLING FLOWS; COSMOLOGY; EVOLUTION; SAMPLE AB The galaxy cluster SPT-CL J0205-5829 currently has the highest spectroscopically confirmed redshift, z = 1.322, in the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. XMM-Newton observations measure a core-excluded temperature of T-X = 8.7(-0.8)(+1.0) keV producing a mass estimate that is consistent with the Sunyaev-Zel'dovich-derived mass. The combined SZ and X-ray mass estimate of M-500 = (4.8+/-0.8) x 10(14)h(70)(-1) M-circle dot makes it the most massive known SZ-selected galaxy cluster at z > 1.2 and the second most massive at z > 1. Using optical and infrared observations, we find that the brightest galaxies in SPT-CL J0205-5829 are already well evolved by the time the universe was < 5 Gyr old, with stellar population ages greater than or similar to 3 Gyr, and low rates of star formation (< 0.5 M-circle dot yr(-1)). We find that, despite the high redshift and mass, the existence of SPT-CL J0205-5829 is not surprising given a flat Lambda CDM cosmology with Gaussian initial perturbations. The a priori chance of finding a cluster of similar rarity (or rarer) in a survey the size of the 2500 deg(2) SPT-SZ survey is 69%. C1 [Stalder, B.; Ashby, M. L. N.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ruel, J.; Bayliss, M.; Nurgaliev, D.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Suhada, R.; Andersson, K.; Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Brodwin, M.] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Andersson, K.; Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrosif, Santiago, Chile. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Gettings, D.; Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RP Stalder, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bstalder@cfa.harvard.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA [NAS 8-03060]; Excellence Cluster Universe; DFG [TR33]; NASA by JPL/Caltech; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution FX The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. This work is based in part on observations obtained with the Spitzer Space Telescope (PID 60099), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile and the Blanco 4 m Telescope at Cerro Tololo Inter-American Observatories in Chile. R.J.F. is supported by a Clay Fellowship. B. A. B is supported by a KICP Fellowship, M. Bautz acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship, W. F. and C.J. acknowledge support from the Smithsonian Institution. NR 86 TC 23 Z9 23 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 93 DI 10.1088/0004-637X/763/2/93 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800024 ER PT J AU Su, KYL Rieke, GH Malhotra, R Stapelfeldt, KR Hughes, AM Bonsor, A Wilner, DJ Balog, Z Watson, DM Werner, MW Misselt, KA AF Su, Kate Y. L. Rieke, George H. Malhotra, Renu Stapelfeldt, Karl R. Hughes, A. Meredith Bonsor, Amy Wilner, David J. Balog, Zoltan Watson, Dan M. Werner, Michael W. Misselt, Karl A. TI ASTEROID BELTS IN DEBRIS DISK TWINS: VEGA AND FOMALHAUT SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems; stars: individual (Vega, Fomalhaut) ID INFRARED INTERFEROMETRIC SURVEY; SPITZER-SPACE-TELESCOPE; EPSILON-ERIDANI; SOLAR-SYSTEM; HR 8799; KUIPER-BELT; HOT DUST; PLANET; STARS; HERSCHEL AB Vega and Fomalhaut are similar in terms of mass, ages, and global debris disk properties; therefore, they are often referred to as "debris disk twins." We present Spitzer 10-35 mu m spectroscopic data centered at both stars and identify warm, unresolved excess emission in the close vicinity of Vega for the first time. The properties of the warm excess in Vega are further characterized with ancillary photometry in the mid-infrared and resolved images in the far-infrared and submillimeter wavelengths. The Vega warm excess shares many similar properties with the one found around Fomalhaut. The emission shortward of similar to 30 mu m from both warm components is well described as a blackbody emission of similar to 170 K. Interestingly, two other systems, epsilon Eri and HR 8799, also show such an unresolved warm dust using the same approach. These warm components may be analogous to the solar system's zodiacal dust cloud, but of far greater mass (fractional luminosity of similar to 10(-5) to 10(-6) compared to 10(-8) to 10(-7)). The dust temperature and tentative detections in the submillimeter suggest that the warm excess arises from dust associated with a planetesimal ring located near the water-frost line and presumably created by processes occurring at similar locations in other debris systems as well. We also review the properties of the 2 mu m hot excess around Vega and Fomalhaut, showing that the dust responsible for the hot excess is not spatially associated with the dust we detected in the warm belt. We suggest it may arise from hot nano grains trapped in the magnetic field of the star. Finally, the separation between the warm and cold belt is rather large with an orbital ratio greater than or similar to 10 in all four systems. In light of the current upper limits on the masses of planetary objects and the large gap, we discuss the possible implications for their underlying planetary architecture and suggest that multiple, low-mass planets likely reside between the two belts in Vega and Fomalhaut. C1 [Su, Kate Y. L.; Rieke, George H.; Misselt, Karl A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Malhotra, Renu] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Stapelfeldt, Karl R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bonsor, Amy] UJF Grenoble 1, CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG, UMR 5274, F-38041 Grenoble, France. [Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Balog, Zoltan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Werner, Michael W.] JPL Caltech, Pasadena, CA 91109 USA. RP Su, KYL (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM ksu@as.arizona.edu OI Malhotra, Renu/0000-0002-1226-3305; Su, Kate/0000-0002-3532-5580 FU NASA's ADAP program [NNX11AF73G]; NASA issued by JPL/Caltech [1255094, 1256424]; Miller Institute for Basic Research in Science; EXEXOZODI [ANR-2010 BLAN-0505-01]; Deutsches Zentrum fur Luf- und Raumfahrt (DLR); Hungarian OTKA [K81966] FX We thank the anonymous referee for prompt and constructive comments. K.Y.L.S. thanks Denis Defrere for his helpful discussion of the hot excesses. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology. K.Y.L.S. and K. R. S. are grateful for funding from NASA's ADAP program (grant No. NNX11AF73G). Support for G. H. R. is provided by NASA through contracts 1255094 and 1256424 issued by JPL/Caltech to the University of Arizona. A. M. H. is supported by a fellowship from the Miller Institute for Basic Research in Science. A. B. is supported by the ANR-2010 BLAN-0505-01 (EXEXOZODI) program. Z.B. is funded by the Deutsches Zentrum fur Luf- und Raumfahrt (DLR). Partial support for this work was also provided for Z.B. through Hungarian OTKA grant No. K81966. NR 87 TC 52 Z9 52 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 118 DI 10.1088/0004-637X/763/2/118 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800049 ER PT J AU Wu, JF Brandt, WN Miller, BP Garmire, GP Schneider, DP Vignali, C AF Wu, Jianfeng Brandt, W. N. Miller, Brendan P. Garmire, Gordon P. Schneider, Donald P. Vignali, Cristian TI AN X-RAY AND MULTIWAVELENGTH SURVEY OF HIGHLY RADIO-LOUD QUASARS AT z > 4: JET-LINKED EMISSION IN THE BRIGHTEST RADIO BEACONS OF THE EARLY UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: jets; galaxies: nuclei; X-rays: galaxies ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; HIGHEST-REDSHIFT QUASARS; XMM-NEWTON OBSERVATIONS; STAR-FORMATION HISTORY; EXTREME Z=4.72 BLAZAR; INVERSE-COMPTON MODEL; 7TH DATA RELEASE AB We present a systematic study of the X-ray and multiwavelength properties of a sample of 17 highly radio-loud quasars (HRLQs) at z > 4 with sensitive X-ray coverage from new Chandra and archival Chandra, XMM-Newton, and Swift observations. Eight of the new and archival observations are reported in this work for the first time. New Chandra observations of two moderately radio-loud and highly optically luminous quasars at z greater than or similar to 4 are also reported. Our HRLQ sample represents the top similar to 5% of radio-loud quasars (RLQs) in terms of radio loudness. We found that our HRLQs have an X-ray emission enhancement over HRLQs at lower redshifts (by a typical factor of approximate to 3), and this effect, after controlling for several factors which may introduce biases, has been solidly estimated to be significant at the 3 sigma-4 sigma level. HRLQs at z = 3-4 are also found to have a similar X-ray emission enhancement over z < 3 HRLQs, which further supports the robustness of our results. We discuss models for the X-ray enhancement's origin including a fractional contribution from inverse Compton scattering of cosmic microwave background photons. No strong correlations are found between the relative X-ray brightness and optical/UV emission-line rest-frame equivalent widths (REWs) for RLQs. However, the line REWs are positively correlated with radio loudness, which suggests that relativistic jets make a negligible contribution to the optical/UV continua of these HRLQs (contrary to the case where the emission lines are diluted by the relativistically boosted continuum). Our HRLQs are generally consistent with the known anti-correlation between radio loudness and X-ray power-law photon index. We also found that the two moderately radio-loud quasars appear to have the hardest X-ray spectra among our objects, suggesting that intrinsic X-ray absorption (N-H similar to 10(23) cm(-2)) may be present. Our z > 4 HRLQs generally have higher X-ray luminosities than those for the composite broadband spectral energy distributions of HRLQs at lower redshift, which further illustrates and supports the X-ray emission enhancement of z > 4 HRLQs. Some of our HRLQs also show an excess of mid-infrared emission which may originate from the synchrotron emission of the relativistic jets. None of our z > 4 HRLQs is detected by the Fermi-LAT two-year survey, which provides constraints on jet-emission models. C1 [Wu, Jianfeng; Brandt, W. N.; Garmire, Gordon P.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wu, Jianfeng; Brandt, W. N.; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, Brendan P.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Vignali, Cristian] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Vignali, Cristian] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. RP Wu, JF (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM jfwu@astro.psu.edu RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015 OI Vignali, Cristian/0000-0002-8853-9611; Brandt, William/0000-0002-0167-2453 FU ACIS Instrument Team [SV4-74018]; NASA ADP [NNX10AC99G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank the anonymous referee for constructive comments. We thank M. S. Brotherton, A. C. Fabian, M. J. Hardcastle, R. F. Mushotzky, E. S. Perlman, G. T. Richards, R. W. Romani, and Z. Shang for helpful discussions. We gratefully acknowledge the support of the ACIS Instrument Team contract SV4-74018 (PI: G. P. Garmire) and NASA ADP grant NNX10AC99G (J. W., W.N.B). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 150 TC 6 Z9 6 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 109 DI 10.1088/0004-637X/763/2/109 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800040 ER PT J AU Zahid, HJ Yates, RM Kewley, LJ Kudritzki, RP AF Zahid, H. J. Yates, R. M. Kewley, L. J. Kudritzki, R. P. TI THE OBSERVED RELATION BETWEEN STELLAR MASS, DUST EXTINCTION, AND STAR FORMATION RATE IN LOCAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: abundances; galaxies: ISM; galaxies: star formation; ISM: abundances ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; FORMING GALAXIES; METALLICITY RELATION; HIGH-REDSHIFT; HOST GALAXIES; DATA RELEASE; EVOLUTION; UNIVERSE; DISKS AB In this study, we investigate the relation between stellar mass, dust extinction, and star formation rate (SFR) using similar to 150,000 star-forming galaxies from SDSS DR7. We show that the relation between dust extinction and SFR changes with stellar mass. For galaxies at the same stellar mass, dust extinction is anti-correlated with the SFR at stellar masses <10(10) M-circle dot. There is a sharp transition in the relation at a stellar mass of 10(10) M-circle dot. At larger stellar masses, dust extinction is positively correlated with the SFR for galaxies at the same stellar mass. The observed relation between stellar mass, dust extinction, and SFR presented in this study helps to confirm similar trends observed in the relation between stellar mass, metallicity, and SFR. The relation reported in this study provides important new constraints on the physical processes governing the chemical evolution of galaxies. The correlation between SFR and dust extinction for galaxies with stellar masses >10(10) M-circle dot is shown to extend to the population of quiescent galaxies suggesting that the physical processes responsible for the observed relation between stellar mass, dust extinction, and SFR may be related to the processes leading to the shutdown of star formation in galaxies. C1 [Zahid, H. J.; Kewley, L. J.; Kudritzki, R. P.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Yates, R. M.; Kudritzki, R. P.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Kewley, L. J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Zahid, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF EARLY CAREER AWARD [AST07-48559]; Deutsche Forschungsgesellshaft (DFG); Alexander-von-Humboldt Foundation FX We thank the anonymous referee for careful reading of the manuscript and G. Cresci for useful comments. H.J.Z. and L.J.K. gratefully acknowledge support by NSF EARLY CAREER AWARD AST07-48559. R.M.Y. acknowledges the financial support of the Deutsche Forschungsgesellshaft (DFG). R. P. K. acknowledges support by the Alexander-von-Humboldt Foundation and the hospitality of the Max Planck Institute for Astrophysics in Garching where part of this work was carried out. NR 54 TC 33 Z9 33 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 2013 VL 763 IS 2 AR 92 DI 10.1088/0004-637X/763/2/92 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 075FR UT WOS:000313869800023 ER PT J AU Dinerstein, E Varma, K Wikramanayake, E Powell, G Lumpkin, S Naidoo, R Korchinsky, M Del Valle, C Lohani, S Seidensticker, J Joldersma, D Lovejoy, T Kushlin, A AF Dinerstein, Eric Varma, Keshav Wikramanayake, Eric Powell, George Lumpkin, Susan Naidoo, Robin Korchinsky, Mike Del Valle, Christian Lohani, Shubash Seidensticker, John Joldersma, Dirk Lovejoy, Thomas Kushlin, Andrey TI Enhancing Conservation, Ecosystem Services, and Local Livelihoods through a Wildlife Premium Mechanism SO CONSERVATION BIOLOGY LA English DT Article DE community based conservation; landscape conservation; large mammals; PES; REDD - Reduction of Emissions for Deforestation and Degradation; species conservation; sustainable financing for conservation; wildlife premium mechanism ID REDD+ GAME; BIODIVERSITY; DEFORESTATION; VALUATION; BENEFITS; PAYMENTS; ECOLOGY AB We propose the wildlife premium mechanism as an innovation to conserve endangered large vertebrates. The performance-based payment scheme would allow stakeholders in lower-income countries to generate revenue by recovering and maintaining threatened fauna that can also serve as umbrella species (i.e., species whose protection benefits other species with which they co-occur). There are 3 possible options for applying the premium: option 1, embed premiums in a carbon payment; option 2, link premiums to a related carbon payment, but as independent and legally separate transactions; option 3, link premiums to noncarbon payments for conserving ecosystem services (PES). Each option presents advantages, such as incentive payments to improve livelihoods of rural poor who reside in or near areas harboring umbrella species, and challenges, such as the establishment of a subnational carbon credit scheme. In Kenya, Peru, and Nepal pilot premium projects are now underway or being finalized that largely follow option 1. The Kasigau (Kenya) project is the first voluntary carbon credit project to win approval from the 2 leading groups sanctioning such protocols and has already sold carbon credits totaling over $1.2 million since June 2011. A portion of the earnings is divided among community landowners and projects that support community members and has added over 350 jobs to the local economy. All 3 projects involve extensive community management because they occur on lands where locals hold the title or have a long-term lease from the government. The monitoring, reporting, and verification required to make premium payments credible to investors include transparent methods for collecting data on key indices by trained community members and verification of their reporting by a biologist. A wildlife premium readiness fund would enable expansion of pilot programs needed to test options beyond those presented here. C1 [Dinerstein, Eric; Wikramanayake, Eric; Powell, George; Naidoo, Robin] World Wildlife Fund, Conservat Sci Program, US, Washington, DC 20037 USA. [Varma, Keshav; Lumpkin, Susan; Kushlin, Andrey] World Bank Grp, Global Tiger Initiat, Washington, DC 20433 USA. [Korchinsky, Mike] Wildlife Works Carbon LLC, Mill Valley, CA 94941 USA. [Del Valle, Christian] Althelia Climate Fund, L-1882 Luxembourg, Luxembourg. [Lumpkin, Susan; Lohani, Shubash] World Wildlife Fund, Eastern Himalayas Program, US, Washington, DC 20037 USA. [Seidensticker, John] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Joldersma, Dirk] World Wildlife Fund, Macroecon & Policy Program, Washington, DC 20037 USA. [Lovejoy, Thomas] George Mason Univ, Environm Sci & Policy Program, Fairfax, VA 22030 USA. [Lovejoy, Thomas] Heinz Ctr Sci Econ & Environm, Washington, DC 20004 USA. RP Dinerstein, E (reprint author), World Wildlife Fund, Conservat Sci Program, US, 1250 24th St,NW, Washington, DC 20037 USA. EM eric.dinerstein@wwfus.org NR 38 TC 14 Z9 14 U1 4 U2 150 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2013 VL 27 IS 1 BP 14 EP 23 DI 10.1111/j.1523-1739.2012.01959.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 073ZM UT WOS:000313781600003 PM 23181423 ER PT J AU Rick, TC Lockwood, R AF Rick, Torben C. Lockwood, Rowan TI Integrating Paleobiology, Archeology, and History to Inform Biological Conservation SO CONSERVATION BIOLOGY LA English DT Article DE applied paleozoology; Chesapeake Bay; conservation paleobiology; environmental history; historical ecology; restoration; shifting baselines ID BASE-LINE SYNDROME; CHESAPEAKE BAY; CRASSOSTREA-VIRGINICA; OYSTER REEF; JAMES RIVER; ECOLOGICAL RESTORATION; PERKINSUS-MARINUS; FISHERIES; PERSPECTIVE; FUTURE AB The search for novel approaches to establishing ecological baselines (reference conditions) is constrained by the fact that most ecological studies span the past few decades, at most, and investigate ecosystems that have been substantially altered by human activities for decades, centuries, or more. Paleobiology, archeology, and history provide historical ecological context for biological conservation, remediation, and restoration. We argue that linking historical ecology explicitly with conservation can help unify related disciplines of conservation paleobiology, conservation archeobiology, and environmental history. Differences in the spatial and temporal resolution and extent (scale) of prehistoric, historic, and modern ecological data remain obstacles to integrating historical ecology and conservation biology, but the prolonged temporal extents of historical ecological data can help establish more complete baselines for restoration, document a historical range of ecological variability, and assist in determining desired future conditions. We used the eastern oyster (Crassostrea virginica) fishery of the Chesapeake Bay (U.S.A.) to demonstrate the utility of historical ecological data for elucidating oyster conservation and the need for an approach to conservation that transcends disciplinary boundaries. Historical ecological studies from the Chesapeake have documented dramatic declines (as much as 99%) in oyster abundance since the early to mid-1800s, changes in oyster size in response to different nutrient levels from the sixteenth to nineteenth centuries, and substantial reductions in oyster accretion rates (from 10 mm/year to effectively 0 mm/year) from the Late Holocene to modern times. Better integration of different historical ecological data sets and increased collaboration between paleobiologists, geologists, archeologists, environmental historians, and ecologists to create standardized research designs and methodologies will help unify prehistoric, historic, and modern time perspectives on biological conservation. C1 [Rick, Torben C.] Smithsonian Inst, Program Human Ecol & Archaeobiol, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Lockwood, Rowan] Coll William & Mary, Dept Geol, Williamsburg, VA 23187 USA. RP Rick, TC (reprint author), Smithsonian Inst, Program Human Ecol & Archaeobiol, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. EM rickt@si.edu NR 86 TC 36 Z9 36 U1 7 U2 101 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2013 VL 27 IS 1 BP 45 EP 54 DI 10.1111/j.1523-1739.2012.01920.x PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 073ZM UT WOS:000313781600006 PM 22979917 ER PT J AU Lebuhn, G Droege, S Connor, EF Gemmill-Herren, B Potts, SG Minckley, RL Griswold, T Jean, R Kula, E Roubik, DW Cane, J Wright, KW Frankie, G Parker, F AF Lebuhn, Gretchen Droege, Sam Connor, Edward F. Gemmill-Herren, Barbara Potts, Simon G. Minckley, Robert L. Griswold, Terry Jean, Robert Kula, Emanuel Roubik, David W. Cane, Jim Wright, Karen W. Frankie, Gordon Parker, Frank TI Detecting Insect Pollinator Declines on Regional and Global Scales SO CONSERVATION BIOLOGY LA English DT Article DE Apiformes; Apoidea; bees; monitoring; power analysis ID BEES; POPULATIONS; ANIMALS; PLANTS; POWER AB Recently there has been considerable concern about declines in bee communities in agricultural and natural habitats. The value of pollination to agriculture, provided primarily by bees, is >$200 billion/year worldwide, and in natural ecosystems it is thought to be even greater. However, no monitoring program exists to accurately detect declines in abundance of insect pollinators; thus, it is difficult to quantify the status of bee communities or estimate the extent of declines. We used data from 11 multiyear studies of bee communities to devise a program to monitor pollinators at regional, national, or international scales. In these studies, 7 different methods for sampling bees were used and bees were sampled on 3 different continents. We estimated that a monitoring program with 200250 sampling locations each sampled twice over 5 years would provide sufficient power to detect small (25%) annual declines in the number of species and in total abundance and would cost U.S.$2,000,000. To detect declines as small as 1% annually over the same period would require >300 sampling locations. Given the role of pollinators in food security and ecosystem function, we recommend establishment of integrated regional and international monitoring programs to detect changes in pollinator communities. C1 [Lebuhn, Gretchen; Connor, Edward F.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. [Droege, Sam] USGS Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Gemmill-Herren, Barbara] Food & Agr Org United Nat, I-00100 Rome, Italy. [Potts, Simon G.] Univ Reading, CAER, Sch Agr Policy & Dev, Reading RG6 6AR, Berks, England. [Minckley, Robert L.] Univ Rochester, Dept Biol, Rochester, NY 14627 USA. [Griswold, Terry; Cane, Jim; Parker, Frank] Utah State Univ, USDA ARS Bee Biol & Systemat Lab, Logan, UT 84322 USA. [Jean, Robert] Indiana State Univ, Dept Biol, Terre Haute, IN 47809 USA. [Kula, Emanuel] Mendel Univ Brno, Fac Forestry & Wood Technol, CZ-61300 Brno, Czech Republic. [Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Wright, Karen W.] Univ New Mexico, Sevilleta LTER, Dept Biol, Albuquerque, NM 87131 USA. [Frankie, Gordon] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. RP Lebuhn, G (reprint author), San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. EM lebuhn@sfsu.edu RI Kula, Emanuel/A-9984-2014 FU Food and Agriculture Organization of the United Nations; Integrated Hardwoods Range Management Program; Nature Conservancy through the Robert Johnson Stewardship Endowment; European Union [GOCE-CT-2003-506675]; National Science Foundation [DEB 0418871]; Nature Conservancy through the Katherine Ordway Stewardship Endowment; [MSM 6215648902] FX This manuscript benefited from insightful comments by B. Steidl, E. Fleishman, and an anonymous reviewer. G.L. and E.F.C. were supported by a grant from the Food and Agriculture Organization of the United Nations. G.L. was also funded by the Integrated Hardwoods Range Management Program. R.J. was funded by a grant to P. E. Scott, Indiana State University, from The Nature Conservancy through the Robert Johnson and Katherine Ordway Stewardship Endowments. S.G.P. was supported by the ALARM project (European Union's Sixth Framework Program, GOCE-CT-2003-506675). R.L.M. was supported by the National Science Foundation (grant DEB 0418871). E.K. was supported by the grant MSM 6215648902. NR 29 TC 35 Z9 37 U1 13 U2 378 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD FEB PY 2013 VL 27 IS 1 BP 113 EP 120 DI 10.1111/j.1523-1739.2012.01962.x PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 073ZM UT WOS:000313781600013 PM 23240651 ER PT J AU Inanez, JG Madrid-Fernandez, M Molera, J Speakman, RJ Pradell, T AF Inanez, Javier G. Madrid-Fernandez, Marisol Molera, Judit Speakman, Robert J. Pradell, Trinitat TI Potters and pigments: preliminary technological assessment of pigment recipes of American majolica by synchrotron radiation micro-X-ray diffraction (Sr-mu ARD) SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Editorial Material DE Majolica; Pigments; Synchrotron micro-X-ray diffraction (mu-XRD); Scanning electron microscopy ID NEUTRON-ACTIVATION ANALYSIS; RAMAN-SCATTERING FEATURES; CHEMICAL-CHARACTERIZATION; IBERIAN PENINSULA; YELLOW PIGMENTS; LEAD-TIN; RENAISSANCE; IDENTIFICATION; CERAMICS; GLAZES AB This paper assesses the impact of European ceramics on preexisting American potting technologies. Specifically we investigate the technological features of pigments used for production of colonial American majolica. In order to achieve this goal, majolica sherds from Puebla (4), and Oaxaca (2), both in Mexico, from Antigua (Guatemala) (2), from Panama (1), and from Mission San Luis (Florida) (5) were analyzed by synchrotron micro-X-ray diffraction (mu-XRD). Eleven out of these fourteen samples were also analyzed by scanning electron microscopy (SEM). The combination of micro-chemical and micro-structural techniques provides a cross sectional profile of the constituent minerals present ultimately providing information about the nature and distribution of the pigments used in their decorations, their dissolution in the glassy matrix, and the formation of crystalline compounds. Our results reveal significant differences among productions. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Inanez, Javier G.] Univ Basque Country, Ctr Invest & Estudios Avanzados, Grp Invest Patrimonio Construido GPAC, Vitoria 01006, Spain. [Inanez, Javier G.] Basque Fdn Sci, IKERBASQUE, Bilbao 48011, Spain. [Inanez, Javier G.; Madrid-Fernandez, Marisol] Univ Barcelona, Dept Prehist Hist Antiga & Arqueol, GRACPE, Cultura Mat & Arqueometria UB ARQ UB, Barcelona 08001, Catalonia, Spain. [Molera, Judit] Univ Vic, Escola Politecn Super, GRTD, Vic 08500, Catalonia, Spain. [Inanez, Javier G.; Speakman, Robert J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Speakman, Robert J.] Univ Georgia, Ctr Appl Isotope Studies, Athens, GA 30602 USA. [Pradell, Trinitat] Univ Politecn Cataluna, GCM, Dept Fis & Engn Nucl, Castelldefels 08860, Catalonia, Spain. RP Inanez, JG (reprint author), Univ Basque Country, Ctr Invest & Estudios Avanzados, Grp Invest Patrimonio Construido GPAC, Miguel de Unamuno 3, Vitoria 01006, Spain. EM javiergarcia@ub.edu; mmadrid@ub.edu; judit.molera@uvic.cat; archsci@uga.edu; Trinitat.Pradell@upc.edu RI Molera, Judit/K-9474-2013; Pradell, Trinitat/D-4765-2014; OI Molera, Judit/0000-0003-3116-0456; Pradell, Trinitat/0000-0002-8720-5492; Inanez, Javier/0000-0002-1411-8099 NR 28 TC 2 Z9 2 U1 0 U2 20 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD FEB PY 2013 VL 40 IS 2 BP 1408 EP 1415 DI 10.1016/j.jas.2012.09.015 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 065MO UT WOS:000313152800059 ER PT J AU McMichael, CH Bush, MB Silman, MR Piperno, DR Raczka, M Lobato, LC Zimmerman, M Hagen, S Palace, M AF McMichael, Crystal H. Bush, Mark B. Silman, Miles R. Piperno, Dolores R. Raczka, Marco Lobato, Luiz C. Zimmerman, Monica Hagen, Stephen Palace, Michael TI Historical fire and bamboo dynamics in western Amazonia SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Amazonia; bamboo dynamics; fire; forest stability; persistence; phytoliths; soil charcoal ID MADRE-DE-DIOS; CLIMATE-CHANGE; CHARCOAL PRODUCTION; CYCLE HYPOTHESIS; HOLOCENE CLIMATE; RAIN-FORESTS; LAND-USE; DISTURBANCE; DIEBACK; PERU AB Aim To determine if recurrent fire accounts for bamboo-dominated forests that cover about 180,000 km2 of western Amazonia. Location Western Amazonia, including Los Amigos and Cocha Cashu, Peru, and Acre, Brazil. Methods We identified bamboo (B+) and closed-canopy forests (B-) using a combination of MODIS imagery, Landsat TM imagery and field surveys. Local-scale and landscape-scale patterns of historical bamboo dynamics were analysed by collecting soil cores from B+ and B- sites across three regions. Soil charcoal within cores was used to document previous fire, and phytoliths were employed to reconstruct vegetational patterns through time. Results Fire occurred in B+ and B- sites with approximately equal frequencies in each region sampled. Between regions, fire signals were most prevalent at Los Amigos, with Cocha Cashu and Acre sites typically containing only trace amounts of charcoal. Vegetational state remained constant through time in both B+ and B- forests of Cocha Cashu and Acre. The persistence of bamboo through time is less clear at Los Amigos, with bamboo presence changing both spatially and temporally. Main conclusions Fire does not appear to be the driving mechanism behind current bamboo distributions, although it may facilitate bamboo invasion. Once established in an area, bamboo persistently dominates the vegetation structure over historical time-scales at some sites (Cocha Cashu and Acre), but not at others (Los Amigos), which is likely to be a function of patch origin. Increasing human activity, including fire and deforestation, combined with predicted Amazonian drought, may allow bamboo to expand from its current distribution and replace typical Amazonian closed-canopy forests. These structural changes in the forests have important implications for carbon storage, as Amazonian forests are currently the largest terrestrial carbon sink in the world. C1 [McMichael, Crystal H.; Bush, Mark B.; Raczka, Marco; Zimmerman, Monica] Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. [McMichael, Crystal H.; Palace, Michael] Univ New Hampshire, Earth Syst Res Ctr, Durham, NH 03824 USA. [Silman, Miles R.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27106 USA. [Silman, Miles R.] Ctr Energy Environm & Sustainabil, Winston Salem, NC 27106 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Washington, DC 20560 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. [Lobato, Luiz C.] Univ Fed Rondonia, Lab Geog Humana & Planejamento Ambiental, Nucleo Ciencia & Tecnol, Porto Velho, Brazil. [Hagen, Stephen] Appl GeoSolut, Durham, NH 03824 USA. RP McMichael, CH (reprint author), Florida Inst Technol, Dept Biol Sci, Melbourne, FL 32901 USA. EM cmcmicha@my.fit.edu OI Bush, Mark/0000-0001-6894-8613 FU National Science Foundation (NSF) Ecology Program [DEB 0742301, DEB 0743666]; Florida Institute of Technology; Smithsonian National Museum of Natural History; Smithsonian Tropical Research Institute; NASA [NNX10AM14G] FX Fieldwork and 14C dating of charcoal fragments was funded by National Science Foundation (NSF) Ecology Program: award DEB 0742301 and DEB 0743666. Other funding was provided by the Florida Institute of Technology, the Smithsonian National Museum of Natural History, including a Restricted Endowment and Small Grant Award, and the Smithsonian Tropical Research Institute. Remote sensing data were funded by NASA Grant NNX10AM14G. All data will be deposited in the Neotoma Database (http://www.neotomadb.org/). We thank Benjamin McMichael and Bryan Rado for field assistance, William Farfan, Karina Garcia, and Nigel and Renata Pitman for logistical assistance, and Noah Yavit for insightful comments on the manuscript. We thank Peter Linder and three anonymous referees for their comments and suggestions on improving the manuscript. This is publication number 77 from the Climate Change Institute of Florida Institute of Technology. NR 74 TC 12 Z9 13 U1 2 U2 40 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD FEB PY 2013 VL 40 IS 2 BP 299 EP 309 DI 10.1111/jbi.12002 PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 074LD UT WOS:000313813100008 ER PT J AU Temeles, EJ Rah, YJ Andicoechea, J Byanova, KL Giller, GSJ Stolk, SB Kress, WJ AF Temeles, E. J. Rah, Y. J. Andicoechea, J. Byanova, K. L. Giller, G. S. J. Stolk, S. B. Kress, W. J. TI Pollinator-mediated selection in a specialized hummingbird-Heliconia system in the Eastern Caribbean SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Dominica; Eastern Caribbean; floral polymorphisms; Heliconia; hummingbird; Lesser Antilles; natural selection; pollination ID PURPLE-THROATED CARIBS; PHENOTYPIC SELECTION; SEXUAL-DIMORPHISM; TROPICAL HUMMINGBIRD; IPOMOPSIS-AGGREGATA; PLATANTHERA-BIFOLIA; GLADIOLUS IRIDACEAE; EULAMPIS-JUGULARIS; FLORAL DISPLAY; COROLLA TUBES AB Phenotypic matches between plants and their pollinators often are interpreted as examples of reciprocal selection and adaptation. For the two co-occurring plant species, Heliconia bihai and H. caribaea in the Eastern Caribbean, we evaluated for five populations over 2 years the strength and direction of natural selection on corolla length and number of bracts per inflorescence. These plant traits correspond closely to the bill lengths and body masses of their primary pollinators, female or male purple-throated carib hummingbirds (Eulampis jugularis). In H. bihai, directional selection for longer corollas was always significant with the exception of one population in 1 year, whereas selection on bract numbers was rare and found only in one population in 1 year. In contrast, significant directional selection for more bracts per inflorescence occurred in all three populations of the yellow morph and in two populations of the red morph of H. caribaea, whereas significant directional selection on corolla length occurred in only one population of the red morph and one population of the yellow morph. Selection for longer corollas in H. bihai may result from better mechanical fit, and hence pollination, by the long bills of female E. jugularis, their sole pollinator. In contrast, competition between males of E. jugularis for territories may drive selection for more bracts in H. caribaea. Competitive exclusion of female E. jugularis by territorial males also implicates pollinator competition as a possible ecological mechanism for trait diversification in these plants. C1 [Temeles, E. J.; Rah, Y. J.; Andicoechea, J.; Byanova, K. L.; Giller, G. S. J.; Stolk, S. B.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA. [Kress, W. J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA. EM ejtemeles@amherst.edu FU Amherst College; Smithsonian Institution; NSF [DEB-0614218] FX We thank A. Kamath for field assistance, E. Williams, A. James and J. Andre of the Forestry Service of the Commonwealth of Dominica for advice and cooperation, S. and A. Peyner-Loehner and A. Jno Baptiste for accommodations and hospitality and two anonymous reviewers for comments on the manuscript. Our research was supported by Amherst College, the Smithsonian Institution and NSF grant DEB-0614218. NR 53 TC 5 Z9 5 U1 4 U2 89 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD FEB PY 2013 VL 26 IS 2 BP 347 EP 356 DI 10.1111/jeb.12053 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 073MR UT WOS:000313747600021 PM 23199234 ER PT J AU Escobar, J Whitmore, TJ Kamenov, GD Riedinger-Whitmore, MA AF Escobar, Jaime Whitmore, Thomas J. Kamenov, George D. Riedinger-Whitmore, Melanie A. TI Isotope record of anthropogenic lead pollution in lake sediments of Florida, USA SO JOURNAL OF PALEOLIMNOLOGY LA English DT Article DE Lead isotope; Alkyl lead; Florida; Sediment; Lead arsenate ID ATMOSPHERIC LEAD; DEPOSITION; GREENLAND; PB; AD; CONTAMINATION; NORTHERN; HISTORY; BC; ATLANTIC AB We examined the anthropogenic lead (Pb) burden that accumulated in sediment of lakes in the southeastern USA during the last similar to 150 years. Mining, smelting, agriculture, and fossil-fuel combustion are known to have contributed to Pb pollution in lakes of other regions. Few studies, however, have examined Pb sequestered in lakes of the southeastern USA, particulary peninsular Florida, which is subject to less continental atmospheric influence than other regions of the eastern USA. We obtained sediment cores from Little Lake Jackson and Little Lake Bonnet in Highlands County, Florida and used Pb isotopes in the records to identify principal sources of Pb contamination. The sediment records showed that changes in Pb concentration and isotope ratios correspond temporally with gasoline consumption in the USA, as well as with changes in lead ores used to produce leaded gasoline. Lead concentrations in the study lakes showed temporal variations that were similar to those found in peat records from east-central Florida. Isotope trends were similar to the mean USA atmospheric Pb deposition record, and to Pb isotope records from Bermuda and Atlantic corals. We modeled the isotopic composition of the anthropogenic Pb in lake sediments and found that the overall trend is controlled by Pb that was released during leaded gasoline combustion. There is, however, additional Pb at each site that comes from sources that are not fully represented by the natural, background Pb. Lead isotope ratios and Pb/arsenic (As) ratios provide evidence that Pb deposition in lakes during the middle 1900s might have been influenced by lead arsenate applications to golf courses, a source that is often ignored in Pb isotope studies. Isotope evidence confirms, however, that following cessation of commercial lead arsenate use in the 1960s, atmospheric alkyl lead was again the primary influence on Pb in sediments of the study lakes. C1 [Escobar, Jaime] Univ Norte Uninorte, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. [Whitmore, Thomas J.; Kamenov, George D.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Riedinger-Whitmore, Melanie A.] Univ S Florida, Dept Biol Sci, St Petersburg, FL 33701 USA. RP Escobar, J (reprint author), Univ Norte Uninorte, Dept Ingn Civil & Ambiental, Km 5 Via Puerto Colombia, Barranquilla, Colombia. EM jhescobar@uninorte.edu.co OI Kamenov, George/0000-0002-6041-6687 FU U.S. Environmental Protection Agency STAR grant FX Funding for this project was provided in part by a U.S. Environmental Protection Agency STAR grant to the University of South Florida-St. Petersburg. We thank Keith Dominey and Jessica Moss at Waters Agricultural Laboratory in Camilla, Georgia for analytical assistance with total Pb content. Natalia Hoyos assisted with figures. NR 47 TC 6 Z9 6 U1 3 U2 43 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2728 J9 J PALEOLIMNOL JI J. Paleolimn. PD FEB PY 2013 VL 49 IS 2 BP 237 EP 252 DI 10.1007/s10933-012-9671-9 PG 16 WC Environmental Sciences; Geosciences, Multidisciplinary; Limnology SC Environmental Sciences & Ecology; Geology; Marine & Freshwater Biology GA 074EJ UT WOS:000313795300009 ER PT J AU Avila-Arcos, MC Ho, SYW Ishida, Y Nikolaidis, N Tsangaras, K Honig, K Medina, R Rasmussen, M Fordyce, SL Calvignac-Spencer, S Willerslev, E Gilbert, MTP Helgen, KM Roca, AL Greenwood, AD AF Avila-Arcos, Maria C. Ho, Simon Y. W. Ishida, Yasuko Nikolaidis, Nikolas Tsangaras, Kyriakos Hoenig, Karin Medina, Rebeca Rasmussen, Morten Fordyce, Sarah L. Calvignac-Spencer, Sebastien Willerslev, Eske Gilbert, M. Thomas P. Helgen, Kristofer M. Roca, Alfred L. Greenwood, Alex D. TI One Hundred Twenty Years of Koala Retrovirus Evolution Determined from Museum Skins SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE KoRV; Phascolarctos cinereus; endogenous retroviruses; ancient DNA ID RECEPTOR-BINDING; LEUKEMIA-VIRUS; PROTEIN; SEQUENCE; GENOME AB Although endogenous retroviruses are common across vertebrate genomes, the koala retrovirus (KoRV) is the only retrovirus known to be currently invading the germ line of its host. KoRV is believed to have first infected koalas in northern Australia less than two centuries ago. We examined KoRV in 28 koala museum skins collected in the late 19th and 20th centuries and deep sequenced the complete proviral envelope region from five northern Australian specimens. Strikingly, KoRV env sequences were conserved among koalas collected over the span of a century, and two functional motifs that affect viral infectivity were fixed across the museum koala specimens. We detected only 20 env polymorphisms among the koalas, likely representing derived mutations subject to purifying selection. Among northern Australian koalas, KoRV was already ubiquitous by the late 19th century, suggesting that KoRV evolved and spread among koala populations more slowly than previously believed. Given that museum and modern koalas share nearly identical KoRV sequences, it is likely that koala populations, for more than a century, have experienced increased susceptibility to diseases caused by viral pathogenesis. C1 [Avila-Arcos, Maria C.; Rasmussen, Morten; Fordyce, Sarah L.; Willerslev, Eske; Gilbert, M. Thomas P.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Copenhagen, Denmark. [Ho, Simon Y. W.] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia. [Ishida, Yasuko; Roca, Alfred L.] Univ Illinois, Dept Anim Sci, Urbana, IL 61801 USA. [Nikolaidis, Nikolas; Medina, Rebeca] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92634 USA. [Nikolaidis, Nikolas; Medina, Rebeca] Calif State Univ Fullerton, Ctr Appl Biotechnol Studies, Fullerton, CA 92634 USA. [Tsangaras, Kyriakos; Hoenig, Karin; Greenwood, Alex D.] Leibniz Inst Zoo & Wildlife Res, Berlin, Germany. [Calvignac-Spencer, Sebastien] Robert Koch Inst, Berlin, Germany. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Roca, AL (reprint author), Univ Illinois, Dept Anim Sci, 328 Mumford Hall, Urbana, IL 61801 USA. EM roca@illinois.edu; greenwood@izw-berlin.de RI Ho, Simon/A-8417-2008; Gilbert, Marcus/A-8936-2013; OI Ho, Simon/0000-0002-0361-2307; Gilbert, Marcus/0000-0002-5805-7195; Avila-Arcos, Maria C./0000-0003-1691-1696; Calvignac-Spencer, Sebastien/0000-0003-4834-0509 FU Australian Research Council; Lundbeck Foundation "Pathogen Palaeogenomes"; Danish National Research Foundation "GeoGenetics"; California State University, Fullerton (CSUF); CSUF; Smithsonian Institution; National Institute of General Medical Sciences (NIGMS) [R01GM092706] FX The authors are grateful to the institutions and individuals listed in table 1 for museum specimens of koalas. They also thank G. Gordon, K. Aplin, and S. Jackson for helpful discussions; M. Farag for technical help; M. Malasky, R. Hanson, S. O'Brien, M. Bush, J. Graves, W. Sherwin, D. Wildt; and the Columbus, San Diego, and San Francisco zoos for modern koala samples. This work was supported by The Australian Research Council, Lundbeck Foundation "Pathogen Palaeogenomes," and the Danish National Research Foundation "GeoGenetics" grants to M. A. A., S. H., M. R., S. F., E. W., and M. T. P. G.; by start-up funds and a state-mini grant from California State University, Fullerton (CSUF) and a Faculty-Student research grant from CSUF to N.N. and R. M.; by an Equity Scholarship from CSUF to R. M.; and by the Smithsonian Institution to K. H. The project described was supported by grant number R01GM092706 from the National Institute of General Medical Sciences (NIGMS). The content is solely the responsibility of the authors and does not necessarily represent the official views of the NIGMS or the National Institutes of Health. NR 24 TC 31 Z9 32 U1 2 U2 61 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0737-4038 J9 MOL BIOL EVOL JI Mol. Biol. Evol. PD FEB PY 2013 VL 30 IS 2 BP 299 EP 304 DI 10.1093/molbev/mss223 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 078TI UT WOS:000314122000007 PM 22983950 ER PT J AU Hamilton, AJ Novotny, V Waters, EK Basset, Y Benke, KK Grimbacher, PS Miller, SE Samuelson, GA Weiblen, GD Yen, JDL Stork, NE AF Hamilton, Andrew J. Novotny, Vojtech Waters, Edward K. Basset, Yves Benke, Kurt K. Grimbacher, Peter S. Miller, Scott E. Samuelson, G. Allan Weiblen, George D. Yen, Jian D. L. Stork, Nigel E. TI Estimating global arthropod species richness: refining probabilistic models using probability bounds analysis SO OECOLOGIA LA English DT Article DE Host specificity; Model; Monte Carlo; Uncertainty ID RISK; DIVERSITY; UNCERTAINTY; VARIABLES; FOREST; TREES AB A key challenge in the estimation of tropical arthropod species richness is the appropriate management of the large uncertainties associated with any model. Such uncertainties had largely been ignored until recently, when we attempted to account for uncertainty associated with model variables, using Monte Carlo analysis. This model is restricted by various assumptions. Here, we use a technique known as probability bounds analysis to assess the influence of assumptions about (1) distributional form and (2) dependencies between variables, and to construct probability bounds around the original model prediction distribution. The original Monte Carlo model yielded a median estimate of 6.1 million species, with a 90 % confidence interval of [3.6, 11.4]. Here we found that the probability bounds (p-bounds) surrounding this cumulative distribution were very broad, owing to uncertainties in distributional form and dependencies between variables. Replacing the implicit assumption of pure statistical independence between variables in the model with no dependency assumptions resulted in lower and upper p-bounds at 0.5 cumulative probability (i.e., at the median estimate) of 2.9-12.7 million. From here, replacing probability distributions with probability boxes, which represent classes of distributions, led to even wider bounds (2.4-20.0 million at 0.5 cumulative probability). Even the 100th percentile of the uppermost bound produced (i.e., the absolutely most conservative scenario) did not encompass the well-known hyper-estimate of 30 million species of tropical arthropods. This supports the lower estimates made by several authors over the last two decades. C1 [Hamilton, Andrew J.; Grimbacher, Peter S.] Univ Melbourne, Melbourne Sch Land & Environm, Dept Agr & Food Syst, Dookie Coll, Vic 3647, Australia. [Novotny, Vojtech] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice, Czech Republic. [Novotny, Vojtech] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Waters, Edward K.] Univ Notre Dame Australia, Broadway, NSW 2007, Australia. [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Benke, Kurt K.] Parkville Ctr, Dept Primary Ind, Parkville, Vic 3052, Australia. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Samuelson, G. Allan] Bernice P Bishop Museum, Honolulu, HI USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, Biol Sci Ctr 220, St Paul, MN 55108 USA. [Yen, Jian D. L.] Monash Univ, Sch Biol Sci, Clayton, Vic 3800, Australia. [Stork, Nigel E.] Griffith Univ, Griffith Sch Environm, Nathan, Qld 4111, Australia. RP Hamilton, AJ (reprint author), Univ Melbourne, Melbourne Sch Land & Environm, Dept Agr & Food Syst, Dookie Campus,940 Dookie Nalinga Rd, Dookie Coll, Vic 3647, Australia. EM andrewjh@unimelb.edu.au; Novotny@entu.cas.cz; edward.waters@nd.edu.au; bassety@si.edu; kurt.benke@dpi.vic.gov.au; petersg@unimelb.edu.au; millers@si.edu; alsam@bishopmuseum.org; gweiblen@umn.edu; jdyen@iinet.net.au; nigel.stork@griffith.edu.au RI Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Yen, Jian/0000-0001-7964-923X; Benke, Kurt/0000-0002-7812-3671; Miller, Scott/0000-0002-4138-1378 FU National Science Foundation (USA) [DEB-0841885]; Christensen Fund (USA); Grant Agency of the Czech Republic [206/09/0115]; Czech Academy of Sciences; Swedish Natural Science Research Council; Czech Ministry of Education [CZ.1.07/2.3.00/20.0064, LH11008]; Otto Kinne Foundation; Darwin Initiative (UK) [19-008]; International Centre of Insect Physiology and Ecology (ICIPE); Bishop Museum FX Cindy Hauser provided useful technical comments on a draft of this manuscript. The host specificity studies in New Guinea, upon which this model draws substantially, were supported by the National Science Foundation (USA) (DEB-0841885), Christensen Fund (USA), Grant Agency of the Czech Republic (206/09/0115), Czech Academy of Sciences, the Swedish Natural Science Research Council, Czech Ministry of Education (CZ.1.07/2.3.00/20.0064, LH11008), Otto Kinne Foundation, Darwin Initiative (UK) (19-008), International Centre of Insect Physiology and Ecology (ICIPE) and Bishop Museum. Parataxonomists in New Guinea are thanked for their assistance and are listed in Novotny et al. (2002). This paper is dedicated to the late Ken Hamilton, the consummate logician and giver. NR 48 TC 23 Z9 23 U1 2 U2 57 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD FEB PY 2013 VL 171 IS 2 BP 357 EP 365 DI 10.1007/s00442-012-2434-5 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 074GJ UT WOS:000313800600006 PM 22968292 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD FEB PY 2013 VL 43 IS 10 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 078ZB UT WOS:000314138500002 ER PT J AU Kapheim, KM Smith, AR Nonacs, P Wcislo, WT Wayne, RK AF Kapheim, Karen M. Smith, Adam R. Nonacs, Peter Wcislo, William T. Wayne, Robert K. TI Foundress polyphenism and the origins of eusociality in a facultatively eusocial sweat bee, Megalopta genalis (Halictidae) SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Alternative reproductive behavior; Facultative eusociality; Maternal manipulation; Social evolution; Polyphenism ID ASSURED FITNESS RETURNS; SPLIT SEX-RATIOS; RUBICUNDUS HYMENOPTERA; ECUADORIA HYMENOPTERA; EVOLUTION; ALLOCATION; BEHAVIOR; POPULATION; SOLITARY; SIZE AB The reproductive (queen) and nonreproductive (worker) castes of eusocial insect colonies are a classic example of insect polyphenism. A complementary polyphenism may also exist entirely among females in the reproductive caste. Although less studied, reproductive females may vary in behavior based on size-associated attributes leading to the production of daughter workers. We studied a bee with flexible social behavior, Megalopta genalis, to better understand the potential of this polyphenism to shape the social organization of bee colonies and, by extension, its role in the evolution of eusociality. Our experimental design reduced variation among nest foundresses in life history variables that could influence reproductive decisions, such as nesting quality and early adulthood experience. Within our study population, approximately one third of M. genalis nests were eusocial and the remaining nests never produced workers. Though they do not differ in survival, nest-founding females who do not attempt to produce workers (which we refer to as the solitary phenotype) are significantly smaller and become reproductive later than females who attempt to recruit workers (the social phenotype). Females with the social phenotype are more likely to produce additional broods but at a cost of having some of their first offspring become nonreproductive workers. The likelihood of eusocial organization varies with body size across females of the social phenotype. Thus, fitness consequences associated with size-based plasticity in foundress behavior has colony level effects on eusociality. The potential for size-based polyphenisms among reproductive females may be an important factor to consider in the evolutionary origins of eusociality. C1 [Kapheim, Karen M.; Nonacs, Peter; Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Kapheim, Karen M.; Smith, Adam R.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Panama. [Kapheim, Karen M.] Inst Genom Biol, Dept Entomol, Urbana, IL 61801 USA. RP Kapheim, KM (reprint author), Inst Genom Biol, Dept Entomol, 1206 W Gregory, Urbana, IL 61801 USA. EM kapheimk@illinois.edu FU STRI; Smithsonian Institution; UCLA EEB; American Women in Science; US Department of Education; UCLA graduate division; Center for Society and Genetics; NSF; NSF [IOS-0642085]; Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama [COL 06-030]; NSF International Research Fellowship Program; Smithsonian Institution post-doctoral fellowship FX KMK was supported by a short-term fellowship from STRI, a 10-week and pre-doctoral fellowship from the Smithsonian Institution, a Holmes O. Miller grant and a George Bartholomew fellowship from UCLA EEB, a Joan Wright Goodman award from American Women in Science, a GAANN fellowship from the US Department of Education, a graduate mentor fellowship from the UCLA graduate division, a graduate fellowship from the Center for Society and Genetics, and an NSF doctoral dissertation improvement grant. KMK and PN were also supported by NSF grant IOS-0642085. ARS was supported by grant COL 06-030 from the Secretaria Nacional de Ciencia, Tecnologia e Innovacion (SENACYT) of Panama to WTW and ARS, a fellowship to ARS from the NSF International Research Fellowship Program, and a Smithsonian Institution post-doctoral fellowship. STRI provided additional support through general research funds to WTW. We would like to thank Margarita Lopez-Uribe, Michael Reiser, Ricardo Cossio, Dyana La Rosa, Julian Medina Gutierrez, Sandra Bernal, Damien Ramirez Garcia, and Tim Alvey for the assistance in the field. Oris Acevedo, Belkys Jimenez, and Orelis Arosemena and the rest of the STRI staff provided valuable logistic support. Research on BCI was conducted with permission from the Autoridad Nacional del Ambiente under permit # SEX/A-34-09, in accordance with the laws of the Republic of Panama. We are thankful to Greg Grether, Torrey Rodgers, Simon Tierney, and Smadar Gilboa for the helpful comments on the manuscript. Earlier drafts of this manuscript were greatly improved by suggestions from Andrew Bourke and two anonymous reviewers. NR 59 TC 8 Z9 8 U1 3 U2 72 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 2013 VL 67 IS 2 BP 331 EP 340 DI 10.1007/s00265-012-1453-x PG 10 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 072DZ UT WOS:000313650600017 ER PT J AU Baccaro, FB Ferraz, G AF Baccaro, F. B. Ferraz, G. TI Estimating density of ant nests using distance sampling SO INSECTES SOCIAUX LA English DT Article DE Distance sampling; Species density; Formicidae; Litter; Tropical forest ID SPECIES RICHNESS; FOOD; COMMUNITIES; POPULATION; DISCOVERY; FOREST; SIZE AB The quantification of ant nest densities is a useful but challenging task given the group's high abundance and diversity of nesting sites. We present a new application of a distance-sampling method which follows standard distance analytical procedures, but introduces a sampling innovation that is particularly useful for ants; instead of having an observer look for ants we let ants find a bait station and measure the distances covered between nest and station. We test this method by estimating the density of epigaeic ant nests in an Amazon tropical forest site near Manaus, Brazil. We distributed 220 baits of canned sardine mixed with cassava flour among 10, 210-m long transects in old-growth upland forest. Forty-five minutes after baiting, we followed the ants' trails and measured the linear distance between the bait and each nest's entrance. We then used the freely available program DISTANCE to estimate the number of nests per unit area while accounting for the effect of distance on the probability that a colony will find a bait. There were found 38 species nesting in 287 different colonies, with an estimated 2.66 nests/m(2). This estimate fell within the 95 % confidence bounds of nest density predicted for a similar number of species based on a literature survey of ant species richness and nest density. Our sampling solution, however, takes less than 30 % of the time used by conventional sampling approaches for a similar area, with the advantage that it produces not only a point estimate but also a quantification of uncertainty about density. C1 [Baccaro, F. B.] Inst Nacl Pesquisas Amazonia INPA, Programa Posgrad Ecol, BR-69060020 Manaus, Amazonas, Brazil. [Ferraz, G.] Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, Inst Nacl Pesquisas Amazonia, Manaus, Amazonas, Brazil. [Ferraz, G.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Baccaro, FB (reprint author), Inst Nacl Pesquisas Amazonia INPA, Programa Posgrad Ecol, CP 478, BR-69060020 Manaus, Amazonas, Brazil. EM fabricera@gmail.com RI Ferraz, Goncalo/C-3860-2008; Baccaro, Fabricio/H-3885-2012 OI Ferraz, Goncalo/0000-0001-8748-0462; Baccaro, Fabricio/0000-0003-4747-1857 FU Instituto Internacional de Educacao do Brasil-IEB-Beca scholarship; PPBio/MCT FX This paper was stimulated by conversations with J.D. Nichols, J.E. Hines and B.K. Williams during a 2007 workshop on Analysis and Management of Animal Populations at the Universidade Federal de Mato Grosso, Brazil. We are thankful to M. Kaspari for kindly providing site-specific data to the species density model, to Ricardo Braga-Neto for collecting and sharing litter depth measurements, and to Juliana Schietti for preparation of Fig. 1. Thiago Izzo, Alexander Christianini, Stephen Buckland and two anonymous reviewers offered valuable suggestions for improving the analysis and manuscript. F. Baccaro was supported by an Instituto Internacional de Educacao do Brasil-IEB-Beca scholarship and fieldwork was supported by PPBio/MCT grants. NR 35 TC 2 Z9 2 U1 1 U2 50 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD FEB PY 2013 VL 60 IS 1 BP 103 EP 110 DI 10.1007/s00040-012-0274-2 PG 8 WC Entomology SC Entomology GA 070CV UT WOS:000313484500014 ER PT J AU Foster, BL Soenjaya, Y Nociti, FH Holm, E Zerfas, PM Wimer, HF Holdsworth, DW Aubin, JE Hunter, GK Goldberga, HA Somermana, MJ AF Foster, B. L. Soenjaya, Y. Nociti, F. H., Jr. Holm, E. Zerfas, P. M. Wimer, H. F. Holdsworth, D. W. Aubin, J. E. Hunter, G. K. Goldberga, H. A. Somermana, M. J. TI Deficiency in Acellular Cementum and Periodontal Attachment in Bsp Null Mice SO JOURNAL OF DENTAL RESEARCH LA English DT Article DE bone sialoprotein; cementum; periodontal ligament; bone; alkaline phosphatase; extracellular matrix ID BONE SIALOPROTEIN; ELECTRON-MICROSCOPY; HYDROXYAPATITE; OSTEOPONTIN; CEMENTOGENESIS; PROTEINS; IDENTIFICATION; INHIBITION; EXPRESSION; NUCLEATION AB Bone sialoprotein (BSP) is an extracellular matrix protein found in mineralized tissues of the skeleton and dentition. BSP is multifunctional, affecting cell attachment and signaling through an RGD integrin-binding region, and acting as a positive regulator for mineral precipitation by nucleating hydroxyapatite crystals. BSP is present in cementum, the hard tissue covering the tooth root that anchors periodontal ligament (PDL) attachment. To test our hypothesis that BSP plays an important role in cementogenesis, we analyzed tooth development in a Bsp null ((-/-)) mouse model. Developmental analysis by histology, histochemistry, and SEM revealed a significant reduction in acellular cementum formation on Bsp(-/-) mouse molar and incisor roots, and the cementum deposited appeared hypomineralized. Structural defects in cementum-PDL interfaces in Bsp(-/-) mice caused PDL detachment, likely contributing to the high incidence of incisor malocclusion. Loss of BSP caused progressively disorganized PDL and significantly increased epithelial down-growth with aging. Bsp(-/-) mice displayed extensive root and alveolar bone resorption, mediated by increased RANKL and the presence of osteoclasts. Results collected here suggest that BSP plays a non-redundant role in acellular cementum formation, likely involved in initiating mineralization on the root surface. Through its importance to cementum integrity, BSP is essential for periodontal function. C1 [Foster, B. L.; Nociti, F. H., Jr.; Somermana, M. J.] NIAMSD, NIH, Bethesda, MD 20892 USA. [Soenjaya, Y.; Hunter, G. K.; Goldberga, H. A.] Univ Western Ontario, Schulich Sch Med & Dent, Biomed Engn Program, London, ON, Canada. [Nociti, F. H., Jr.] Univ Estadual Campinas, Sch Dent, Div Periodont, Dept Prosthodont & Periodont, Piracicaba, SP, Brazil. [Holm, E.; Goldberga, H. A.] Univ Western Ontario, Sch Med & Dent, Dept Biochem, London, ON, Canada. [Zerfas, P. M.] NIH, Div Vet Resources, Off Res Serv, Bethesda, MD 20892 USA. [Wimer, H. F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Holdsworth, D. W.] Robarts Res Inst, Imaging Res Labs, London, ON N6A 5C1, Canada. [Aubin, J. E.] Univ Toronto, Dept Mol Genet, Toronto, ON, Canada. [Aubin, J. E.] Univ Toronto, Fac Dent, Toronto, ON, Canada. [Hunter, G. K.; Goldberga, H. A.] Univ Western Ontario, Sch Dent, Schulich Sch Med & Dent, London, ON, Canada. RP Foster, BL (reprint author), NIAMSD, NIH, Bethesda, MD 20892 USA. EM brian.foster@nih.gov RI Holdsworth, David/F-6315-2012; Goldberg, Harvey/B-5742-2015; Nociti, Francisco/G-4907-2015; Foster, Brian/H-8375-2015; OI Foster, Brian/0000-0003-3444-0576; Aubin, Jane E./0000-0002-7268-5235 FU National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS) of the National Institutes of Health (NIH); Canadian Institutes of Health Research [FRN83704-JEA, FRN93598-HAG/GKH]; CIHR; AO Foundation (Switzerland) FX We thank Jirawan Wade and Daisy Matsa-Dunn (UW, Seattle, WA, USA) for histological procedures, Simrandeep Sidhu (NIAMS) for IHC assistance, Frank Beier and Vasek Pitelka (UWO) for assistance with animal studies, Cristiane Salmon (UNICAMP, Piracicaba, SP, Brazil) for mouse ligature-periodontitis tissues, and Marc McKee (McGill University, Montreal, Quebec, Canada) for technical advice on sectioning undecalcified tissues. This research was supported by the Intramural Research Program of the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS) of the National Institutes of Health (NIH), and by the Canadian Institutes of Health Research (FRN83704-JEA, FRN93598-HAG/GKH). YS is supported by The Joint Motion Program, a CIHR Training Program and the AO Foundation (Switzerland). The authors declare no potential conflicts of interest with respect to the authorship and/or publication of this article. NR 30 TC 24 Z9 24 U1 0 U2 18 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0022-0345 J9 J DENT RES JI J. Dent. Res. PD FEB PY 2013 VL 92 IS 2 BP 166 EP 172 DI 10.1177/0022034512469026 PG 7 WC Dentistry, Oral Surgery & Medicine SC Dentistry, Oral Surgery & Medicine GA 071XE UT WOS:000313629700012 PM 23183644 ER PT J AU Nadeau, NJ Martin, SH Kozak, KM Salazar, C Dasmahapatra, KK Davey, JW Baxter, SW Blaxter, ML Mallet, J Jiggins, CD AF Nadeau, Nicola J. Martin, Simon H. Kozak, Krzysztof M. Salazar, Camilo Dasmahapatra, Kanchon K. Davey, John W. Baxter, Simon W. Blaxter, Mark L. Mallet, James Jiggins, Chris D. TI Genome-wide patterns of divergence and gene flow across a butterfly radiation SO MOLECULAR ECOLOGY LA English DT Article DE divergence; genome; Heliconius; phylogeny; speciation ID MITOCHONDRIAL-DNA SEQUENCES; HELICONIUS-BUTTERFLIES; ECOLOGICAL SPECIATION; MULLERIAN MIMICRY; MIMETIC BUTTERFLIES; WARNING-COLOR; EVOLUTION; DISCOVERY; SELECTION; DIFFERENTIATION AB The Heliconius butterflies are a diverse recent radiation comprising multiple levels of divergence with ongoing gene flow between species. The recently sequenced genome of Heliconius melpomene allowed us to investigate the genomic evolution of this group using dense RAD marker sequencing. Phylogenetic analysis of 54 individuals robustly supported reciprocal monophyly of H. melpomene and Heliconius cydno and refuted previous phylogenetic hypotheses that H. melpomene may be paraphylectic with respect to H. cydno. Heliconius timareta also formed a monophyletic clade closely related but distinct from H. cydno with Heliconius heurippa falling within this clade. We find evidence for genetic admixture between sympatric populations of the sister clades H. melpomene and H. cydno/timareta, particularly between H. cydno and H. melpomene from Central America and between H. timareta and H. melpomene from the eastern slopes of the Andes. Between races, divergence is primarily explained by isolation by distance and there is no detectable genetic population structure between parapatric races, suggesting that hybrid zones between races are not zones of secondary contact. Our results also support previous findings that colour pattern loci are shared between populations and species with similar colour pattern elements. Furthermore, this pattern is almost unique to these genomic regions, with only a very small number of other loci showing significant similarity between populations and species with similar colour patterns. C1 [Nadeau, Nicola J.; Martin, Simon H.; Kozak, Krzysztof M.; Salazar, Camilo; Baxter, Simon W.; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Salazar, Camilo] Smithsonian Trop Res Inst, Naos Isl, Causeway Amador, Panama. [Salazar, Camilo] Univ Nacl Rosario, Fac Ciencias Nat & Matemat, Bogota, Colombia. [Dasmahapatra, Kanchon K.; Mallet, James] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England. [Davey, John W.; Blaxter, Mark L.] Univ Edinburgh, Ashworth Labs, Inst Evolutionary Biol, Edinburgh EH9 3JT, Midlothian, Scotland. [Baxter, Simon W.] Univ Adelaide, Sch Mol & Biomed Sci, Adelaide, SA 5005, Australia. [Mallet, James] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. RP Nadeau, NJ (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM njn27@cam.ac.uk RI Jiggins, Chris/B-9960-2008; Davey, John/B-5075-2013; Nadeau, Nicola/E-1149-2011; Salazar, camilo/A-1647-2010; mallet, james/B-5114-2008; Martin, Simon/D-1410-2011; Blaxter, Mark/B-4113-2010 OI Dasmahapatra, Kanchon Kumar/0000-0002-2840-7019; Jiggins, Chris/0000-0002-7809-062X; Kozak, Krzysztof/0000-0001-8980-3173; Davey, John/0000-0002-1017-9775; Nadeau, Nicola/0000-0002-9319-921X; Salazar, camilo/0000-0001-9217-6588; Martin, Simon/0000-0002-0747-7456; Blaxter, Mark/0000-0003-2861-949X FU Leverhulme Trust; BBSRC FX We thank the governments of Colombia, Peru and Panama for permission to collect and export butterflies and Mauricio Linares for collecting and providing us will samples of H. cydno cordula. This work was funded primarily by a Leverhulme Trust award to CDJ and a BBSRC grant to JM, CDJ and MB. Sequencing of the RAD libraries was performed at the GenePool, Edinburgh. NR 61 TC 58 Z9 58 U1 3 U2 203 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 2013 VL 22 IS 3 BP 814 EP 826 DI 10.1111/j.1365-294X.2012.05730.x PG 13 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 073EM UT WOS:000313726300020 PM 22924870 ER PT J AU Kornis, MS Sharma, S Vander Zanden, MJ AF Kornis, Matthew S. Sharma, Sapna Vander Zanden, M. Jake TI Invasion success and impact of an invasive fish, round goby, in Great Lakes tributaries SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Biodiversity; biological invasions; community composition; environmental characteristics; Great Lakes; Neogobius melanostomus; round goby ID GOBIES NEOGOBIUS-MELANOSTOMUS; RIVER CONTINUUM CONCEPT; BIOLOGICAL INVASIONS; SPECIES INVASIONS; APOLLONIA-MELANOSTOMA; COMMUNITY STRUCTURE; MOTTLED SCULPIN; NORTH-AMERICA; ENEMY RELEASE; DIVERSITY AB Aim Environmental and biological characteristics interact in complex ways to determine ecosystem susceptibility to invasive species, and a greater understanding of their relative roles in invader spread and impact is needed. We evaluated relationships between environmental characteristics, biodiversity of indigenous species, and the abundance and ecological impact of an invasive fish, round goby (Neogobius melanostomus). Location Tributaries to Lake Michigan, WI, USA. Methods We assessed the distribution and abundance of round gobies and native fishes in tributaries via electrofishing. We compared fish community composition and diversity in streams with (n = 30) and without (n = 52) round gobies and examined how trends in round goby abundance from 2007 to 2010 correlated with changes in abundance of five native benthic fishes. We used redundancy analysis to determine how indigenous stream communities related to environmental characteristics and round goby abundance. Results Round goby abundance was best explained by environmental characteristics, with watershed area and temperature explaining 22.4% of the variation. Species richness and Shannon diversity only explained 6.9% of the variation in round goby abundance and only an additional 2.3% after considering environmental characteristics. Round goby abundance was not a significant predictor of fish community composition, which was best explained by seven environmental variables (30.3% of the variation). Invaded communities had significantly higher indigenous species richness than uninvaded communities (8.38 vs. 6.54). Round goby abundance was low compared with estimates from other studies, but showed an increasing trend in many tributaries (average 10.8-fold increase from 2007 to 2010). Surprisingly, there were no temporal trends in native benthic fish abundance despite increases in round goby abundance. Main conclusions Environmental characteristics favouring high fish diversity (e.g. resource availability and warm water temperature) were positively associated with round goby abundance. However, round goby density and impact are relatively low in most tributaries at present, emphasizing the importance of considering heterogeneity in an invader's abundance when assessing invasion success. C1 [Kornis, Matthew S.; Sharma, Sapna; Vander Zanden, M. Jake] Univ Wisconsin, Ctr Limnol, Madison, WI 53706 USA. RP Kornis, MS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM kornism@si.edu FU University of Wisconsin Sea Grant Institute [NA06OAR4170011, R/AI-3] FX We thank Erika Nilsson for her estimates of round goby density in select tributaries through 3x depletion sampling. Our gratitude also extends to Emily Stanley, Anthony Ives, Brian Weidel and our three anonymous peer reviewers for their insightful comments on this manuscript. We greatly appreciate Erik Kopperud, Jedchada Carlson, Hans Martin and Gabrielle Lehrer-Brey for aiding in field collections. This work was funded by a grant from the University of Wisconsin Sea Grant Institute, federal grant number NA06OAR4170011 project number R/AI-3, to Jake Vander Zanden. NR 84 TC 17 Z9 18 U1 12 U2 212 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD FEB PY 2013 VL 19 IS 2 BP 184 EP 198 DI 10.1111/ddi.12001 PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 067AV UT WOS:000313265100007 ER PT J AU Maloney, KO Weller, DE Michaelson, DE Ciccotto, PJ AF Maloney, Kelly O. Weller, Donald E. Michaelson, Daniel E. Ciccotto, Patrick J. TI Species Distribution Models of Freshwater Stream Fishes in Maryland and Their Implications for Management SO ENVIRONMENTAL MODELING & ASSESSMENT LA English DT Article DE Conditional random forests; Landscape; Prediction; Classification; Habitat suitability ID MULTIPLE SPATIAL SCALES; UNITED-STATES; LAND-USE; ECOLOGICAL THEORY; BIOTIC INTEGRITY; HABITAT; CLASSIFICATION; ASSEMBLAGES; ECOSYSTEMS; PREDICTION AB Species distribution models (SDMs) are often used in conservation planning, but their utility can be improved by assessing the relationships between environmental and species response variables. We constructed SDMs for 30 stream fishes of Maryland, USA, using watershed attributes as environmental variables and presence/absence as species responses. SDMs showed substantial agreement between observed and predicted values for 17 species. Most important variables were natural attributes (e.g., ecoregion, watershed area, latitude/longitude); land cover (e.g., %impervious, %row crop) was important for three species. Focused analyses on four representative species (central stoneroller, creek chub, largemouth bass, and white sucker) showed the probability of presence of each species increased non-linearly with watershed area. For these species, SDMs built to predict absent, low, and high densities were similar to presence/absence predictions but provided probable locations of high densities (e.g., probability of high-density creek chub decreased rapidly with watershed area). We applied SDMs to predict suitability of watersheds within the study area for each species. Maps of suitability and the environmental and species response relationships can help develop better management plans. C1 [Maloney, Kelly O.] US Geol Survey, No Appalachian Res Lab, Leetown Sci Ctr, Wellsboro, PA 16901 USA. [Maloney, Kelly O.; Weller, Donald E.; Michaelson, Daniel E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ciccotto, Patrick J.] Maryland Dept Nat Resources, Annapolis, MD 21401 USA. RP Maloney, KO (reprint author), US Geol Survey, No Appalachian Res Lab, Leetown Sci Ctr, 176 Straight Run Rd, Wellsboro, PA 16901 USA. EM kmaloney@usgs.gov; wellerd@si.edu; dem2k@virginia.edu; PCiccotto@dnr.state.md.us OI Weller, Donald/0000-0002-7629-5437 FU REU fellowship; Smithsonian Post-Doctoral Research Fellowship FX We thank the Maryland Department of Natural Resources and the MBSS field crew members for providing the MBSS data and Matt Baker for watershed boundaries. We thank Lori Davias and an anonymous reviewer for constructive feedback on an earlier version of this manuscript. This research was partly funded by an REU fellowship to DEM. Additional support was provided by a Smithsonian Post-Doctoral Research Fellowship awarded to KOM. NR 73 TC 8 Z9 8 U1 2 U2 65 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1420-2026 J9 ENVIRON MODEL ASSESS JI Environ. Model. Assess. PD FEB PY 2013 VL 18 IS 1 BP 1 EP 12 DI 10.1007/s10666-012-9325-3 PG 12 WC Environmental Sciences SC Environmental Sciences & Ecology GA 063RO UT WOS:000313017800001 ER PT J AU Roper, CFE Shea, EK AF Roper, Clyde F. E. Shea, Elizabeth K. TI Unanswered questions about the giant squid Architeuthis (Architeuthidae) illustrate our incomplete knowledge of coleoid cephalopods SO AMERICAN MALACOLOGICAL BULLETIN LA English DT Article; Proceedings Paper CT James H. Lee Symposium on Great Unanswered Questions in Malacology held at the 77th Annual Meeting of the American-Malacological-Society CY JUL 23-27, 2011 CL Pittsburgh, PA SP Amer Malacol Soc DE oegopsid; natural history; biology ID WHALES PHYSETER-MACROCEPHALUS; WESTERN NORTH-ATLANTIC; IN-SITU OBSERVATIONS; SPAWNING EGG CARE; SPERM-WHALES; DEEP-SEA; VERTICAL-DISTRIBUTION; STOMACH CONTENTS; DECAPODIFORMES MOLLUSCA; FUNCTIONAL-MORPHOLOGY AB The giant squid, Architeuthis Steenstrup, 1857, serves as a model for what we know and do not know about the broad biological aspects of the coleoid cephalopods. Gaps in our knowledge of taxonomy and systematics, distribution, population size, habitat use, age and growth, predation and feeding, reproduction and life cycles, and functional morphology all are examined by our review of Architeuthis natural history. Continued Architeuthis research improves our understanding of all coleoid cephalopods, and provides an avenue to engage the public in the process of science. C1 [Roper, Clyde F. E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Shea, Elizabeth K.] Delaware Museum Nat Hist, Dept Mollusks, Wilmington, DE 19807 USA. RP Shea, EK (reprint author), Delaware Museum Nat Hist, Dept Mollusks, 4840 Kennett Pike, Wilmington, DE 19807 USA. EM eshea@delmnh.org NR 145 TC 3 Z9 4 U1 8 U2 27 PU AMER MALACOLOGICAL SOC, INC PI WILMINGTON PA DELAWARE MUSEUM NATURAL HISTORY, BOX 3937, WILMINGTON, DE 19807-0937 USA SN 0740-2783 EI 2162-2698 J9 AM MALACOL BULL JI Am. Malacol. Bull. PD FEB PY 2013 VL 31 IS 1 BP 109 EP 122 DI 10.4003/006.031.0104 PG 14 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AK9TL UT WOS:000338769900014 ER PT J AU Accomazzi, A Budavari, T Fluke, C Gray, N Mann, RG O'Mullane, W Wicenec, A Wise, M AF Accomazzi, Alberto Budavari, Tamas Fluke, Christopher Gray, Norman Mann, Robert G. O'Mullane, William Wicenec, Andreas Wise, Michael TI Astronomy and Computing: A new journal for the astronomical computing community SO ASTRONOMY AND COMPUTING LA English DT Article AB We introduce Astronomy and Computing, a new journal for the growing population of people working in the domain where astronomy overlaps with computer science and information technology. The journal aims to provide a new communication channel within that community, which is not well served by current journals, and to help secure recognition of its true importance within modern astronomy. In this inaugural editorial, we describe the rationale for creating the journal, outline its scope and ambitions, and seek input from the community in defining in detail how the journal should work towards its high-level goals. (c) 2013 Published by Elsevier B.V. C1 [Accomazzi, Alberto] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Budavari, Tamas] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Fluke, Christopher] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Gray, Norman] Univ Glasgow, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Mann, Robert G.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [O'Mullane, William] European Space Astron Ctr, European Space Agcy, E-28691 Madrid, Spain. [Wicenec, Andreas] Univ Western Australia, Int Ctr Radio Astron Res, Nedlands, WA 6009, Australia. [Wise, Michael] ASTRON Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. RP Accomazzi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aaccomazzi@cfa.harvard.edu; tamas.budavari@jhu.edu; cfluke@astro.swin.edu.au; norman@astro.gla.ac.uk; rgm@roe.ac.uk; womullan@sciops.esa.int; andreas.wicenec@uwa.edu.au; wise@astron.nl OI Gray, Norman/0000-0002-1941-9202; Accomazzi, Alberto/0000-0002-4110-3511 NR 8 TC 2 Z9 2 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD FEB PY 2013 VL 1 BP 1 EP 4 DI 10.1016/j.ascom.2012.10.001 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA V39BC UT WOS:000209385500001 ER PT J AU Shamir, L Wallin, JF Allen, A Berriman, B Teuben, P Nemiroff, RJ Mink, J Hanisch, RJ DuPrie, K AF Shamir, Lior Wallin, John F. Allen, Alice Berriman, Bruce Teuben, Peter Nemiroff, Robert J. Mink, Jessica Hanisch, Robert J. DuPrie, Kimberly TI Practices in source code sharing in astrophysics SO ASTRONOMY AND COMPUTING LA English DT Article DE Source code; Scientific software; Open source; Software sharing; Software validation AB While software and algorithms have become increasingly important in astronomy, the majority of authors who publish computational astronomy research do not share the source code they develop, making it difficult to replicate and reuse the work. In this paper we discuss the importance of sharing scientific source code with the entire astrophysics community, and propose that journals require authors to make their code publicly available when a paper is published. That is, we suggest that a paper that involves a computer program not be accepted for publication unless the source code becomes publicly available. The adoption of such a policy by editors, editorial boards, and reviewers will improve the ability to replicate scientific results, and will also make computational astronomy methods more available to other researchers who wish to apply them to their data. (C) 2013 Elsevier B.V. All rights reserved. C1 [Shamir, Lior] Lawrence Technol Univ, Southfield, MI 48075 USA. [Wallin, John F.] Middle Tennessee State Univ, Murfreesboro, TN USA. [Allen, Alice; DuPrie, Kimberly] ASCL, Baltimore, MD USA. [Berriman, Bruce] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Teuben, Peter] Univ Maryland, Baltimore, MD USA. [Nemiroff, Robert J.] Michigan Technol Univ, Houghton, MI 49931 USA. [Mink, Jessica] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Hanisch, Robert J.] Space Telescope Sci Inst, Baltimore, MD USA. RP Shamir, L (reprint author), Lawrence Technol Univ, Southfield, MI 48075 USA. EM Ishamir@mtu.edu OI Mink, Jessica/0000-0003-3594-1823 NR 29 TC 10 Z9 10 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD FEB PY 2013 VL 1 BP 54 EP 58 DI 10.1016/j.ascom.2013.04.001 PG 5 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA V39BC UT WOS:000209385500008 ER PT J AU Foster, B Soenjaya, Y Nociti, F Holm, E Kantovitz, K Wimer, H Zerfas, P Aubin, J Hunter, G Goldberg, H Somerman, M AF Foster, Brian Soenjaya, Yohannes Nociti, Francisco, Jr. Holm, Erik Kantovitz, Kamila Wimer, Helen Zerfas, Patricia Aubin, Jane Hunter, Graeme Goldberg, Harvey Somerman, Martha TI Defective Mineralization in Craniofacial Bone and Cementum in Bsp Null Mice SO JOURNAL OF BONE AND MINERAL RESEARCH LA English DT Meeting Abstract CT Annual Meeting of the American-Society-for-Bone-and-Mineral-Research CY OCT 04-07, 2013 CL Baltimore, MD SP Amer Soc Bone & Mineral Res C1 [Soenjaya, Yohannes] Univ Western Ontario, Schulich Sch Med & Dent, Biomed Engn Program, London, ON N6A 3K7, Canada. [Nociti, Francisco, Jr.; Kantovitz, Kamila; Somerman, Martha] Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bethesda, MD USA. [Holm, Erik] Univ Western Ontario, Schulich Sch Med & Dent, Dept Biochem, London, ON N6A 3K7, Canada. [Wimer, Helen] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Zerfas, Patricia] NIH, Dept Res Serv, Div Vet Resources, Bethesda, MD USA. [Aubin, Jane] Univ Toronto, Fac Med, Toronto, ON M5S 1A1, Canada. [Hunter, Graeme] Univ Western Ontario, Schulich Sch Med & Dent, Sch Dent, London, ON N6A 3K7, Canada. [Goldberg, Harvey] Univ Western Ontario, London, ON N6A 3K7, Canada. RI Nociti, Francisco/G-4907-2015; Foster, Brian/H-8375-2015 OI Foster, Brian/0000-0003-3444-0576 NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0884-0431 EI 1523-4681 J9 J BONE MINER RES JI J. Bone Miner. Res. PD FEB PY 2013 VL 28 SU 1 MA SA0112 PG 3 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA AB8JI UT WOS:000332035803043 ER PT J AU Jarcho, MR Power, ML Layne-Colon, DG Tardif, SD AF Jarcho, Michael R. Power, Michael L. Layne-Colon, Donna G. Tardif, Suzette D. TI Digestive Efficiency Mediated by Serum Calcium Predicts Bone Mineral Density in the Common Marmoset (Callithrix jacchus) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE common marmoset; marmoset wasting syndrome; metabolic bone disease; digestive efficiency; calcium ID TAMARINS SAGUINUS-OEDIPUS; WASTING SYNDROME; ABSORPTION; NUTRITION; PRIMATE; DISEASE AB Two health problems have plagued captive common marmoset (Callithrix jacchus) colonies for nearly as long as those colonies have existed: marmoset wasting syndrome and metabolic bone disease. While marmoset wasting syndrome is explicitly linked to nutrient malabsorption, we propose metabolic bone disease is also linked to nutrient malabsorption, although indirectly. If animals experience negative nutrient balance chronically, critical nutrients may be taken from mineral stores such as the skeleton, thus leaving those stores depleted. We indirectly tested this prediction through an initial investigation of digestive efficiency, as measured by apparent energy digestibility, and serum parameters known to play a part in metabolic bone mineral density of captive common marmoset monkeys. In our initial study on 12 clinically healthy animals, we found a wide range of digestive efficiencies, and subjects with lower digestive efficiency had lower serum vitamin D despite having higher food intakes. A second experiment on 23 subjects including several with suspected bone disease was undertaken to measure digestive and serum parameters, with the addition of a measure of bone mineral density by dual-energy X-ray absorptiometry (DEXA). Bone mineral density was positively associated with apparent digestibility of energy, vitamin D, and serum calcium. Further, digestive efficiency was found to predict bone mineral density when mediated by serum calcium. These data indicate that a poor ability to digest and absorb nutrients leads to calcium and vitamin D insufficiency. Vitamin D absorption may be particularly critical for indoor-housed animals, as opposed to animals in a more natural setting, because vitamin D that would otherwise be synthesized via exposure to sunlight must be absorbed from their diet. If malabsorption persists, metabolic bone disease is a possible consequence in common marmosets. These findings support our hypothesis that both wasting syndrome and metabolic bone disease in captive common marmosets are consequences of inefficient nutrient absorption. Am. J. Primatol. 75:153-160, 2013. (c) 2012 Wiley Periodicals, Inc. C1 [Jarcho, Michael R.] Univ Calif Davis, Dept Psychol, Davis, CA 95616 USA. [Jarcho, Michael R.] Univ Calif Los Angeles, Cousins Ctr Psychoneuroimmunol, Los Angeles, CA USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Washington, DC 20024 USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC USA. [Power, Michael L.] Smithsonian Inst, Natl Zool Pk, Conservat Ecol Ctr, Washington, DC 20008 USA. [Layne-Colon, Donna G.; Tardif, Suzette D.] SW Natl Primate Res Ctr, San Antonio, TX USA. [Tardif, Suzette D.] Univ Texas Hlth Sci Ctr San Antonio, San Antonio, TX 78229 USA. RP Jarcho, MR (reprint author), Loras Coll, Dept Neurosci, 1450 Alta Vista St, Dubuque, IA 52001 USA. EM michael.jarcho@loras.edu OI Power, Michael/0000-0002-6120-3528 FU PHS [R01-RR02022]; National Institutes of Health/National Center for Research Resources (NIH/NCRR) [P51 RR013986] FX Contract grant sponsor: PHS; Contract grant number: R01-RR02022 (SDT); Contract grant sponsor: National Institutes of Health/National Center for Research Resources (NIH/NCRR); Contract grant number: P51 RR013986. NR 21 TC 4 Z9 4 U1 0 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD FEB PY 2013 VL 75 IS 2 BP 153 EP 160 DI 10.1002/ajp.22093 PG 8 WC Zoology SC Zoology GA 057CK UT WOS:000312539300006 PM 23169342 ER PT J AU Sohn, JC Regier, JC Mitter, C Davis, D Landry, JF Zwick, A Cummings, MP AF Sohn, Jae-Cheon Regier, Jerome C. Mitter, Charles Davis, Donald Landry, Jean-Francois Zwick, Andreas Cummings, Michael P. TI A Molecular Phylogeny for Yponomeutoidea (Insecta, Lepidoptera, Ditrysia) and Its Implications for Classification, Biogeography and the Evolution of Host Plant Use SO PLOS ONE LA English DT Article ID CONSENSUS TREES; ADVANCED MOTHS; ERMINE MOTH; GENE; BUTTERFLIES; SUPPORT; DISTRIBUTIONS; SELECTION; HISTORY; BIOLOGY AB Background: Yponomeutoidea, one of the early-diverging lineages of ditrysian Lepidoptera, comprise about 1,800 species worldwide, including notable pests and insect-plant interaction models. Yponomeutoids were one of the earliest lepidopteran clades to evolve external feeding and to extensively colonize herbaceous angiosperms. Despite the group's economic importance, and its value for tracing early lepidopteran evolution, the biodiversity and phylogeny of Yponomeutoidea have been relatively little studied. Methodology/Principal Findings: Eight nuclear genes (8 kb) were initially sequenced for 86 putative yponomeutoid species, spanning all previously recognized suprageneric groups, and 53 outgroups representing 22 families and 12 superfamilies. Eleven to 19 additional genes, yielding a total of 14.8 to 18.9 kb, were then sampled for a subset of taxa, including 28 yponomeutoids and 43 outgroups. Maximum likelihood analyses were conducted on data sets differing in numbers of genes, matrix completeness, inclusion/weighting of synonymous substitutions, and inclusion/exclusion of "rogue" taxa. Monophyly for Yponomeutoidea was supported very strongly when the 18 "rogue" taxa were excluded, and moderately otherwise. Results from different analyses are highly congruent and relationships within Yponomeutoidea are well supported overall. There is strong support overall for monophyly of families previously recognized on morphological grounds, including Yponomeutidae, Ypsolophidae, Plutellidae, Glyphipterigidae, Argyresthiidae, Attevidae, Praydidae, Heliodinidae, and Bedelliidae. We also assign family rank to Scythropiinae (Scythropiidae stat. rev.), which in our trees are strongly grouped with Bedelliidae, in contrast to all previous proposals. We present a working hypothesis of among-family relationships, and an informal higher classification. Host plant family associations of yponomeutoid subfamilies and families are non-random, but show no trends suggesting parallel phylogenesis. Our analyses suggest that previous characterizations of yponomeutoids as predominantly Holarctic were based on insufficient sampling. Conclusions/Significance: We provide the first robust molecular phylogeny for Yponomeutoidea, together with a revised classification and new insights into their life history evolution and biogeography. C1 [Sohn, Jae-Cheon; Regier, Jerome C.; Mitter, Charles] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Davis, Donald] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Landry, Jean-Francois] Agr & Agri Food Canada, Eastern Cereal & Oilseed Res Ctr, CEF, Ottawa, ON, Canada. [Zwick, Andreas] State Museum Nat Hist, Dept Entomol, Stuttgart, Germany. [Cummings, Michael P.] Univ Maryland, Lab Mol Evolut, Ctr Bioinformat & Computat Biol, College Pk, MD 20742 USA. RP Sohn, JC (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. EM jsohn@umd.edu RI Yakovlev, Roman/J-7243-2013; Zwick, Andreas/A-5735-2015 FU U.S. National Science Foundation's Assembling the Tree of Life program [0531769]; Maryland Agricultural Experiment Station FX Financial support was provided by the U.S. National Science Foundation's Assembling the Tree of Life program, award number 0531769, and the Maryland Agricultural Experiment Station. This is contribution 244 of the Evolution of Terrestrial Ecosystems consortium of the National Museum of Natural History, in Washington, D.C. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 101 TC 21 Z9 23 U1 2 U2 48 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 31 PY 2013 VL 8 IS 1 AR e55066 DI 10.1371/journal.pone.0055066 PG 23 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 085JH UT WOS:000314610600063 PM 23383061 ER PT J AU Bergin, EA Cleeves, LI Gorti, U Zhang, K Blake, GA Green, JD Andrews, SM Evans, NJ Henning, T Oberg, K Pontoppidan, K Qi, CH Salyk, C van Dishoeck, EF AF Bergin, Edwin A. Cleeves, L. Ilsedore Gorti, Uma Zhang, Ke Blake, Geoffrey A. Green, Joel D. Andrews, Sean M. Evans, Neal J., II Henning, Thomas Oeberg, Karin Pontoppidan, Klaus Qi, Chunhua Salyk, Colette van Dishoeck, Ewine F. TI An old disk still capable of forming a planetary system SO NATURE LA English DT Article ID T-TAURI; PROTOPLANETARY DISKS; SOLAR NEBULA; GAS; HYA; EMISSION; SEARCH; PACS; LINE; MASS AB From the masses of the planets orbiting the Sun, and the abundance of elements relative to hydrogen, it is estimated that when the Solar System formed, the circumstellar disk must have had a minimum mass of around 0.01 solar masses within about 100 astronomical units of the star(1-4). (One astronomical unit is the EarthSun distance.) The main constituent of the disk, gaseous molecular hydrogen, does not efficiently emit radiation from the disk mass reservoir(5), and so the most common measure of the disk mass is dust thermal emission and lines of gaseous carbon monoxide(6). Carbon monoxide emission generally indicates properties of the disk surface, and the conversion from dust emission to gas mass requires knowledge of the grain properties and the gas-to-dust mass ratio, which probably differ from their interstellar values(7,8). As a result, mass estimates vary by orders of magnitude, as exemplified by the relatively old (3-10 million years) star TW Hydrae(9,10), for which the range is 0.0005-0.06 solar masses(11-14). Here we report the detection of the fundamental rotational transition of hydrogen deuteride from the direction of TW Hydrae. Hydrogen deuteride is a good tracer of disk gas because it follows the distribution of molecular hydrogen and its emission is sensitive to the total mass. The detection of hydrogen deuteride, combined with existing observations and detailed models, implies a disk mass of more than 0.05 solar masses, which is enough to form a planetary system like our own. C1 [Bergin, Edwin A.; Cleeves, L. Ilsedore] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gorti, Uma] SETI Inst, Mountain View, CA 94043 USA. [Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Zhang, Ke] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Green, Joel D.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Andrews, Sean M.; Oeberg, Karin; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pontoppidan, Klaus] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Salyk, Colette] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI zhang, ke/A-3898-2009; OI zhang, ke/0000-0002-0661-7517; Cleeves, L. Ilsedore/0000-0003-2076-8001 FU NASA through JPL/Caltech; US National Science Foundation [1008800] FX Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech and by the US National Science Foundation under grant 1008800. This paper makes use of the following Atacama Large Millimeter/submillimeter Array (ALMA) data: ADS/JAO.ALMA#2011.0.00001.SV. ALMA is a partnership of ESO (representing its member states), the NSF (USA) and NINS (Japan), together with the NRC (Canada) and the NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 30 TC 82 Z9 82 U1 1 U2 14 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 31 PY 2013 VL 493 IS 7434 BP 644 EP 646 DI 10.1038/nature11805 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 080CU UT WOS:000314219600050 PM 23364742 ER PT J AU Arai, K Le Sage, D DeVience, SJ Glenn, DR Pham, LM Rahn-Lee, L Lukin, MD Yacoby, A Komeili, A Walsworth, RL AF Arai, Keigo Le Sage, David DeVience, Stephen J. Glenn, David R. Pham, Linh M. Rahn-Lee, Lilah Lukin, Mikhail D. Yacoby, Amir Komeili, Arash Walsworth, Ronald L. TI Wide-Field Magnetic Imaging using Nitrogen-Vacancy Color Centers in Diamond SO BIOPHYSICAL JOURNAL LA English DT Meeting Abstract CT 57th Annual Meeting of the Biophysical-Society CY FEB 02-06, 2013 CL Philadelphia, PA SP Biophys Soc C1 [Arai, Keigo] MIT, Cambridge, MA 02139 USA. [Le Sage, David; Glenn, David R.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Le Sage, David; DeVience, Stephen J.; Glenn, David R.; Pham, Linh M.; Lukin, Mikhail D.; Yacoby, Amir; Walsworth, Ronald L.] Harvard Univ, Cambridge, MA 02138 USA. [Rahn-Lee, Lilah; Komeili, Arash] Univ Calif Berkeley, Berkeley, CA 94720 USA. RI DeVience, Stephen/D-7274-2012 OI DeVience, Stephen/0000-0003-3142-7296 NR 0 TC 1 Z9 1 U1 0 U2 27 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0006-3495 J9 BIOPHYS J JI Biophys. J. PD JAN 29 PY 2013 VL 104 IS 2 SU 1 BP 193A EP 193A PG 1 WC Biophysics SC Biophysics GA 105MI UT WOS:000316074301487 ER PT J AU Lauterbach, R Wells, K O'Hara, RB Kalko, EKV Renner, SC AF Lauterbach, Ralf Wells, Konstans O'Hara, Robert B. Kalko, Elisabeth K. V. Renner, Swen C. TI Variable Strength of Forest Stand Attributes and Weather Conditions on the Questing Activity of Ixodes ricinus Ticks over Years in Managed Forests SO PLOS ONE LA English DT Article ID LYME-DISEASE VECTOR; CLIMATE-CHANGE; POPULATION-DYNAMICS; SATURATION DEFICIT; RANGE EXPANSION; LOCAL CLIMATE; RISK; ABUNDANCE; SCAPULARIS; IXODIDAE AB Given the ever-increasing human impact through land use and climate change on the environment, we crucially need to achieve a better understanding of those factors that influence the questing activity of ixodid ticks, a major disease-transmitting vector in temperate forests. We investigated variation in the relative questing nymph densities of Ixodes ricinus in differently managed forest types for three years (2008-2010) in SW Germany by drag sampling. We used a hierarchical Bayesian modeling approach to examine the relative effects of habitat and weather and to consider possible nested structures of habitat and climate forces. The questing activity of nymphs was considerably larger in young forest successional stages of thicket compared with pole wood and timber stages. Questing nymph density increased markedly with milder winter temperatures. Generally, the relative strength of the various environmental forces on questing nymph density differed across years. In particular, winter temperature had a negative effect on tick activity across sites in 2008 in contrast to the overall effect of temperature across years. Our results suggest that forest management practices have important impacts on questing nymph density. Variable weather conditions, however, might override the effects of forest management practices on the fluctuations and dynamics of tick populations and activity over years, in particular, the preceding winter temperatures. Therefore, robust predictions and the detection of possible interactions and nested structures of habitat and climate forces can only be quantified through the collection of long-term data. Such data are particularly important with regard to future scenarios of forest management and climate warming. C1 [Lauterbach, Ralf; Wells, Konstans; Kalko, Elisabeth K. V.; Renner, Swen C.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Wells, Konstans; O'Hara, Robert B.] Biodivers & Climate Res Ctr, Frankfurt, Germany. [Renner, Swen C.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Renner, SC (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM swen.renner@uni-ulm.de RI O'Hara, Robert/A-7499-2008; Wells, Konstans/A-7232-2010; Renner, Swen/J-3502-2014 OI O'Hara, Robert/0000-0001-9737-3724; Wells, Konstans/0000-0003-0377-2463; Renner, Swen/0000-0002-6893-4219 FU DFG [KA 1241/15-1] FX The work has been funded by the DFG Priority Program 1374 "Infrastructure-Biodiversity-Exploratories" (KA 1241/15-1). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 5 Z9 7 U1 3 U2 31 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 25 PY 2013 VL 8 IS 1 AR e55365 DI 10.1371/journal.pone.0055365 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 093RV UT WOS:000315210400092 PM 23372852 ER PT J AU Robertson, DR AF Robertson, D. Ross TI Who Resembles Whom? Mimetic and Coincidental Look-Alikes among Tropical Reef Fishes SO PLOS ONE LA English DT Article ID INTERSPECIFIC FEEDING ASSOCIATIONS; CORAL-REEF; AGGRESSIVE MIMICRY; IMPERFECT MIMICRY; HAMLETS HYPOPLECTRUS; MARINE FISHES; COLOR MORPHS; PUERTO-RICO; RED-SEA; EVOLUTION AB Studies of mimicry among tropical reef-fishes usually give little or no consideration to alternative explanations for behavioral associations between unrelated, look-alike species that benefit the supposed mimic. I propose and assess such an alternative explanation. With mimicry the mimic resembles its model, evolved to do so in response to selection by the mimicry target, and gains evolved benefits from that resemblance. In the alternative, the social-trap hypothesis, a coincidental resemblance of the model to the "mimic" inadvertently attracts the latter to it, and reinforcement of this social trapping by learned benefits leads to the "mimic" regularly associating with the model. I examine three well known cases of supposed aggressive mimicry among reef-fishes in relation to nine predictions from these hypotheses, and assess which hypothesis offers a better explanation for each. One case, involving precise and complex morphological and behavioral resemblance, is strongly consistent with mimicry, one is inconclusive, and one is more consistent with a social-trap based on coincidental, imprecise resemblance. Few cases of supposed interspecific mimicry among tropical reef fishes have been examined in depth, and many such associations may involve social traps arising from generalized, coincidental resemblance. Mimicry may be much less common among these fishes than is generally thought. C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Robertson, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM drr@stri.org NR 73 TC 6 Z9 6 U1 3 U2 49 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 25 PY 2013 VL 8 IS 1 AR e54939 DI 10.1371/journal.pone.0054939 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 093RV UT WOS:000315210400041 PM 23372795 ER PT J AU Wilson, S Marra, PP Sillett, TS AF Wilson, Scott Marra, Peter P. Sillett, T. Scott TI The Effects of Experimental Irrigation on Plant Productivity, Insect Abundance and the Non-Breeding Season Performance of a Migratory Songbird SO PLOS ONE LA English DT Article ID TROPICAL DRY FOREST; NONBREEDING-SEASON; HABITAT QUALITY; SETOPHAGA-RUTICILLA; NEOTROPICAL MIGRANT; AMERICAN REDSTARTS; DECIDUOUS FOREST; LEAF PHENOLOGY; COSTA-RICA; BIRD AB Migratory bird populations are often limited by food during the non-breeding season. Correlative evidence suggests that food abundance on territories varies among years in relation to rainfall, which affects plant productivity and arthropod biomass. At the Font Hill Nature Preserve in Jamaica, we used an irrigation experiment to test the hypothesis that rainfall affects the condition of wintering American redstarts (Setophaga ruticilla) via intermediate effects on plant productivity and arthropod abundance. Experimental plots were irrigated in late February and early March to simulate a mid-season pulse of 200 mm of rain. Irrigation maintained soil moisture levels near saturation and had immediate effects on plant productivity. Cumulative leaf abscission over the dry season was 50% lower on experimental plots resulting in greater canopy cover, and we observed significantly higher ground level shoot growth and the flushing of new leaves on about 58% of logwood (Haematoxylon campechianum) individuals. Arthropod biomass was 1.5 times higher on irrigated plots, but there was considerable inter-plot variability within a treatment and a strong seasonal decline in biomass. Consequently, we found no significant effect of irrigation on arthropod abundance or redstart condition. We suspect that the lack of an irrigation effect for taxa higher on the trophic chain was due to the small spatial scale of the treatment relative to the scale at which these taxa operate. Although redstart condition was not affected, we did observe turnover from subordinate to dominant territorial individuals on experimental plots suggesting a perceived difference in habitat quality that influenced individual behavior. C1 [Wilson, Scott; Marra, Peter P.; Sillett, T. Scott] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC USA. RP Wilson, S (reprint author), Environm Canada, Canadian Wildlife Serv, Saskatoon, SK, Canada. EM scottd.wilson@ec.gc.ca FU National Science Foundation [DEB 0717243]; Smithsonian Institution; Canadian Natural Sciences and Engineering Research Council FX This work was funded by the National Science Foundation (grant DEB 0717243) to PPM and TSS, the Smithsonian Institution, and a Canadian Natural Sciences and Engineering Research Council grant to SW. The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. NR 48 TC 5 Z9 5 U1 1 U2 35 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 25 PY 2013 VL 8 IS 1 AR e55114 DI 10.1371/journal.pone.0055114 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 093RV UT WOS:000315210400067 PM 23372825 ER PT J AU Hermsen, W Hessels, JWT Kuiper, L van Leeuwen, J Mitra, D de Plaa, J Rankin, JM Stappers, BW Wright, GAE Basu, R Alexov, A Coenen, T Griessmeier, JM Hassall, TE Karastergiou, A Keane, E Kondratiev, VI Kramer, M Kuniyoshi, M Noutsos, A Serylak, M Pilia, M Sobey, C Weltevrede, P Zagkouris, K Asgekar, A Avruch, IM Batejat, F Bell, ME Bell, MR Bentum, MJ Bernardi, G Best, P Birzan, L Bonafede, A Breitling, F Broderick, J Brueggen, M Butcher, HR Ciardi, B Duscha, S Eisloffel, J Falcke, H Fender, R Ferrari, C Frieswijk, W Garrett, MA de Gasperin, F de Geus, E Gunst, AW Heald, G Hoeft, M Horneffer, A Iacobelli, M Kuper, G Maat, P Macario, G Markoff, S McKean, JP Mevius, M Miller-Jones, JCA Morganti, R Munk, H Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pizzo, R Polatidis, AG Rawlings, S Reich, W Rottgering, H Scaife, AMM Schoenmakers, A Shulevski, A Sluman, J Steinmetz, M Tagger, M Tang, Y Tasse, C ter Veen, S Vermeulen, R van de Brink, RH van Weeren, RJ Wijers, RAMJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P AF Hermsen, W. Hessels, J. W. T. Kuiper, L. van Leeuwen, J. Mitra, D. de Plaa, J. Rankin, J. M. Stappers, B. W. Wright, G. A. E. Basu, R. Alexov, A. Coenen, T. Griessmeier, J. -M. Hassall, T. E. Karastergiou, A. Keane, E. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Noutsos, A. Serylak, M. Pilia, M. Sobey, C. Weltevrede, P. Zagkouris, K. Asgekar, A. Avruch, I. M. Batejat, F. Bell, M. E. Bell, M. R. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bonafede, A. Breitling, F. Broderick, J. Brueggen, M. Butcher, H. R. Ciardi, B. Duscha, S. Eisloeffel, J. Falcke, H. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. de Gasperin, F. de Geus, E. Gunst, A. W. Heald, G. Hoeft, M. Horneffer, A. Iacobelli, M. Kuper, G. Maat, P. Macario, G. Markoff, S. McKean, J. P. Mevius, M. Miller-Jones, J. C. A. Morganti, R. Munk, H. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pizzo, R. Polatidis, A. G. Rawlings, S. Reich, W. Roettgering, H. Scaife, A. M. M. Schoenmakers, A. Shulevski, A. Sluman, J. Steinmetz, M. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Vermeulen, R. van de Brink, R. H. van Weeren, R. J. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. TI Synchronous X-ray and Radio Mode Switches: A Rapid Global Transformation of the Pulsar Magnetosphere SO SCIENCE LA English DT Article ID XMM-NEWTON OBSERVATIONS; PHOTON IMAGING CAMERA; DRIFTING SUBPULSES; EMPIRICAL-THEORY; POWERED PULSARS; GAMMA-RAY; EMISSION; B0943+10; RADIATION; POLARIZATION AB Pulsars emit from low-frequency radio waves up to high-energy gamma-rays, generated anywhere from the stellar surface out to the edge of the magnetosphere. Detecting correlated mode changes across the electromagnetic spectrum is therefore key to understanding the physical relationship among the emission sites. Through simultaneous observations, we detected synchronous switching in the radio and x-ray emission properties of PSR B0943+10. When the pulsar is in a sustained radio-"bright" mode, the x-rays show only an unpulsed, nonthermal component. Conversely, when the pulsar is in a radio-"quiet" mode, the x-ray luminosity more than doubles and a 100% pulsed thermal component is observed along with the nonthermal component. This indicates rapid, global changes to the conditions in the magnetosphere, which challenge all proposed pulsar emission theories. C1 [Hermsen, W.; Kuiper, L.; de Plaa, J.; Avruch, I. M.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Hermsen, W.; Hessels, J. W. T.; van Leeuwen, J.; Rankin, J. M.; Coenen, T.; Markoff, S.; Miller-Jones, J. C. A.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Hessels, J. W. T.; van Leeuwen, J.; Kondratiev, V. I.; Pilia, M.; Asgekar, A.; Avruch, I. M.; Bentum, M. J.; Butcher, H. R.; Duscha, S.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; de Geus, E.; Gunst, A. W.; Heald, G.; Kuper, G.; Maat, P.; McKean, J. P.; Mevius, M.; Morganti, R.; Munk, H.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Schoenmakers, A.; Sluman, J.; Tang, Y.; Vermeulen, R.; van de Brink, R. H.; van Weeren, R. J.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Mitra, D.; Basu, R.] Natl Ctr Radio Astrophys NCFRA TIFR, Pune 411007, Maharashtra, India. [Rankin, J. M.] Univ Vermont, Dept Phys, Burlington, VT 05405 USA. [Stappers, B. W.; Hassall, T. E.; Kramer, M.; Weltevrede, P.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Wright, G. A. E.] Univ Sussex, Ctr Astron, Brighton BN1 9QJ, E Sussex, England. [Alexov, A.] Space Telescope Sci Inst STScI, Baltimore, MD 21218 USA. [Griessmeier, J. -M.; Serylak, M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 02, France. [Griessmeier, J. -M.; Serylak, M.] CNRS, INSU, Observ Paris, Stn Radioastron Nancay, F-18330 Nancay, France. [Hassall, T. E.; Bell, M. E.; Broderick, J.; Fender, R.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Karastergiou, A.; Zagkouris, K.; Rawlings, S.] Univ Oxford, Oxford OX1 3RH, England. [Keane, E.; Kramer, M.; Kuniyoshi, M.; Noutsos, A.; Sobey, C.; Falcke, H.; Horneffer, A.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kondratiev, V. I.] Ctr Astro Space, Lebedev Phys Inst, Moscow 117997, Russia. [Avruch, I. M.; Mevius, M.; Morganti, R.; Shulevski, A.] Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Batejat, F.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Bell, M. E.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bell, M. R.; Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Bentum, M. J.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Birzan, L.; Garrett, M. A.; Iacobelli, M.; Pandey-Pommier, M.; Roettgering, H.; van Weeren, R. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Breitling, F.; Steinmetz, M.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Butcher, H. R.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.; Orru, E.; ter Veen, S.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Ferrari, C.; Macario, G.] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Paas, H.] Univ Groningen, CIT, NL-9747 AJ Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Pandey, V. N.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Tasse, C.; Zarka, P.] UPMC Univ Paris Diderot, CNRS, LESIA Observ Paris, F-92190 Meudon, France. [Tasse, C.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Tasse, C.] SKA S Africa, ZA-7405 Pinelands, South Africa. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Hermsen, W (reprint author), SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM w.hermsen@sron.nl RI Miller-Jones, James/B-2411-2013; Tagger, Michel/O-6615-2014; Shulevski, Aleksandar/E-5591-2015; Ciardi, Benedetta/N-7625-2015; Melrose, Don/O-8766-2014; Kondratiev, Vladislav/N-1105-2015; van Leeuwen, John/G-3155-2011; Falcke, Heino/H-5262-2012; Yatawatta, Sarod/E-6037-2013; OI van Weeren, Reinout/0000-0002-0587-1660; Miller-Jones, James/0000-0003-3124-2814; Tagger, Michel/0000-0003-2962-3220; Shulevski, Aleksandar/0000-0002-1827-0469; Kondratiev, Vladislav/0000-0001-8864-7471; van Leeuwen, John/0000-0003-1175-5161; Falcke, Heino/0000-0002-2526-6724; Yatawatta, Sarod/0000-0001-5619-4017; Wijers, Ralph/0000-0002-3101-1808; de Gasperin, Francesco/0000-0003-4439-2627 FU ESA member states; NASA; Netherlands Organization for Scientific Research (NWO); Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank the staff of XMM-Newton, GMRT, and LOFAR for making these observations possible. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA member states and by NASA. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries that are owned by various parties (each with their own funding sources) and are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. ASTRON and SRON are supported financially by the Netherlands Organization for Scientific Research (NWO). Two of us (J.M.R., G. A. E. W.) thank NWO and ASTRON for visitor grants. C. F. was supported by Agence Nationale de la Recherche grant ANR-09-JCJC-0001-01. The used x-ray data can be retrieved from the XMM-Newton Science Archive at xmm.esac.esa.int/xsa. The applied B-and Q-mode window selections, derived from the GMRT and LOFAR observations, are listed in table S2. NR 33 TC 45 Z9 45 U1 0 U2 15 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 25 PY 2013 VL 339 IS 6118 BP 436 EP 439 DI 10.1126/science.1230960 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 076MN UT WOS:000313960700040 PM 23349288 ER PT J AU Manchester, RN Hobbs, G Bailes, M Coles, WA Straten, W Keith, MJ Shannon, RM Bhat, NDR Brown, A Burke-Spolaor, SG Champion, DJ Chaudhary, A Edwards, RT Hampson, G Hotan, AW Jameson, A Jenet, FA Kesteven, MJ Khoo, J Kocz, J Maciesiak, K Oslowski, S Ravi, V Reynolds, JR Sarkissian, JM Verbiest, JPW Wen, ZL Wilson, WE Yardley, D Yan, WM You, XP AF Manchester, R. N. Hobbs, G. Bailes, M. Coles, W. A. van Straten, W. Keith, M. J. Shannon, R. M. Bhat, N. D. R. Brown, A. Burke-Spolaor, S. G. Champion, D. J. Chaudhary, A. Edwards, R. T. Hampson, G. Hotan, A. W. Jameson, A. Jenet, F. A. Kesteven, M. J. Khoo, J. Kocz, J. Maciesiak, K. Oslowski, S. Ravi, V. Reynolds, J. R. Sarkissian, J. M. Verbiest, J. P. W. Wen, Z. L. Wilson, W. E. Yardley, D. Yan, W. M. You, X. P. TI The Parkes Pulsar Timing Array Project SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE gravitational waves; instrumentation: miscellaneous; methods: observational; pulsars: general ID BLACK-HOLE BINARIES; RADIO ASTRONOMICAL POLARIMETRY; GRAVITATIONAL-WAVE DETECTION; MILLISECOND PULSARS; GENERAL-RELATIVITY; ELECTRON-DENSITY; COALESCENCE RATE; PSR J1022+1001; SYSTEM; DISCOVERY AB A 'pulsar timing array' (PTA), in which observations of a large sample of pulsars spread across the celestial sphere are combined, allows investigation of 'global' phenomena such as a background of gravitational waves or instabilities in atomic timescales that produce correlated timing residuals in the pulsars of the array. The Parkes Pulsar Timing Array (PPTA) is an implementation of the PTA concept based on observations with the Parkes 64-m radio telescope. A sample of 20 ms pulsars is being observed at three radio-frequency bands, 50 cm (similar to 700MHz), 20 cm (similar to 1400 MHz), and 10 cm (similar to 3100 MHz), with observations at intervals of two to three weeks. Regular observations commenced in early 2005. This paper describes the systems used for the PPTA observations and data processing, including calibration and timing analysis. The strategy behind the choice of pulsars, observing parameters, and analysis methods is discussed. Results are presented for PPTA data in the three bands taken between 2005 March and 2011 March. For 10 of the 20 pulsars, rms timing residuals are less than 1 mu s for the best band after fitting for pulse frequency and its first time derivative. Significant 'red' timing noise is detected in about half of the sample. We discuss the implications of these results on future projects including the International Pulsar Timing Array and a PTA based on the Square Kilometre Array. We also present an 'extended PPTA' data set that combines PPTA data with earlier Parkes timing data for these pulsars. C1 [Manchester, R. N.; Hobbs, G.; Keith, M. J.; Shannon, R. M.; Brown, A.; Burke-Spolaor, S. G.; Champion, D. J.; Chaudhary, A.; Hampson, G.; Hotan, A. W.; Kesteven, M. J.; Khoo, J.; Maciesiak, K.; Oslowski, S.; Ravi, V.; Reynolds, J. R.; Sarkissian, J. M.; Wilson, W. E.; Yardley, D.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Bailes, M.; van Straten, W.; Bhat, N. D. R.; Hotan, A. W.; Jameson, A.; Kocz, J.; Oslowski, S.; Verbiest, J. P. W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Coles, W. A.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Bhat, N. D. R.] Curtin Univ Technol, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Burke-Spolaor, S. G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Champion, D. J.; Verbiest, J. P. W.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Jenet, F. A.] Univ Texas Brownsville, Ctr Adv Radio Astron, Brownsville, TX 78520 USA. [Kocz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maciesiak, K.] Univ Zielona Gora, Kepler Inst Astron, PL-65265 Zielona Gora, Poland. [Ravi, V.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Wen, Z. L.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Yardley, D.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Yan, W. M.] Chinese Acad Sci, Xinjiang Astron Observ, Xinjiang 830011, Peoples R China. [You, X. P.] Southwest Univ, Sch Phys Sci & Technol, Chongqing 400715, Peoples R China. RP Manchester, RN (reprint author), CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia. EM dick.manchester@csiro.au OI Champion, David/0000-0003-1361-7723; Shannon, Ryan/0000-0002-7285-6348; Kocz, Jonathon/0000-0003-0249-7586; van Straten, Willem/0000-0003-2519-7375; Oslowski, Stefan/0000-0003-0289-0732 FU RNM's Australian Research Council (ARC) Federation Fellowship [FF0348478]; CSIRO; ARC Discovery Project grant [DP0985272]; ARC QEII Fellowship [DP0878388]; John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund; National Aeronautics and Space Administration; Commonwealth Government FX The PPTA project was initiated with support from RNM's Australian Research Council (ARC) Federation Fellowship (FF0348478) and from the CSIRO under this Fellowship program. It has also received support from ARC Discovery Project grant DP0985272. GH is the recipient of an ARC QEII Fellowship (DP0878388) and VR is a recipient of a John Stocker Postgraduate Scholarship from the Science and Industry Endowment Fund. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We acknowledge contributions to the project from L. Kedziora-Chudczer, K. J. Lee, A. N. Lommen, D. Smith, and Ding Chen. The Parkes telescope is part of the Australia Telescope which is funded by the Commonwealth Government for operation as a National Facility managed by CSIRO. NR 118 TC 46 Z9 46 U1 0 U2 9 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD JAN 24 PY 2013 VL 30 AR UNSP e017 DI 10.1017/pasa.2012.017 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161ZV UT WOS:000320234700001 ER PT J AU Tingay, SJ Goeke, R Bowman, JD Emrich, D Ord, SM Mitchell, DA Morales, MF Booler, T Crosse, B Wayth, RB Lonsdale, CJ Tremblay, S Pallot, D Colegate, T Wicenec, A Kudryavtseva, N Arcus, W Barnes, D Bernardi, G Briggs, F Burns, S Bunton, JD Cappallo, RJ Corey, BE Deshpande, A Desouza, L Gaensler, BM Greenhill, LJ Hall, PJ Hazelton, BJ Herne, D Hewitt, JN Johnston-Hollitt, M Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lynch, MJ Mckinley, B Mcwhirter, SR Morgan, E Oberoi, D Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, A Salah, JE Sault, RJ Udaya-Shankar, N Schlagenhaufer, F Srivani, KS Stevens, J Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL Wyithe, JSB AF Tingay, S. J. Goeke, R. Bowman, J. D. Emrich, D. Ord, S. M. Mitchell, D. A. Morales, M. F. Booler, T. Crosse, B. Wayth, R. B. Lonsdale, C. J. Tremblay, S. Pallot, D. Colegate, T. Wicenec, A. Kudryavtseva, N. Arcus, W. Barnes, D. Bernardi, G. Briggs, F. Burns, S. Bunton, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. Desouza, L. Gaensler, B. M. Greenhill, L. J. Hall, P. J. Hazelton, B. J. Herne, D. Hewitt, J. N. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lynch, M. J. Mckinley, B. Mcwhirter, S. R. Morgan, E. Oberoi, D. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, A. Salah, J. E. Sault, R. J. Udaya-Shankar, N. Schlagenhaufer, F. Srivani, K. S. Stevens, J. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wyithe, J. S. B. TI The Murchison Widefield Array: The Square Kilometre Array Precursor at Low Radio Frequencies SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE instrumentation: interferometers; techniques: image processing; techniques: interferometric-radio continuum: general; radio lines: general; early Universe ID WIDE-FIELD ARRAY; SOFTWARE CORRELATOR; NONCOPLANAR ARRAYS; POINT SOURCES; IMAGES; REIONIZATION; SUBTRACTION; CALIBRATION; CHALLENGES; TRANSIENTS AB The Murchison Widefield Array (MWA) is one of three Square Kilometre Array Precursor telescopes and is located at the Murchison Radio-astronomy Observatory in the Murchison Shire of the mid-west of Western Australia, a location chosen for its extremely low levels of radio frequency interference. The MWA operates at low radio frequencies, 80-300 MHz, with a processed bandwidth of 30.72 MHz for both linear polarisations, and consists of 128 aperture arrays (known as tiles) distributed over a similar to 3-km diameter area. Novel hybrid hardware/software correlation and a real-time imaging and calibration systems comprise the MWA signal processing backend. In this paper, the as-built MWA is described both at a system and sub-system level, the expected performance of the array is presented, and the science goals of the instrument are summarised. C1 [Tingay, S. J.; Emrich, D.; Ord, S. M.; Booler, T.; Crosse, B.; Wayth, R. B.; Tremblay, S.; Pallot, D.; Colegate, T.; Kudryavtseva, N.; Arcus, W.; Hall, P. J.; Herne, D.; Lynch, M. J.; Schlagenhaufer, F.; Waterson, M.] Curtin Univ Technol, ICRAR, Perth, WA, Australia. [Tingay, S. J.; Mitchell, D. A.; Wayth, R. B.; Tremblay, S.; Briggs, F.; Gaensler, B. M.; Mckinley, B.; Subrahmanyan, R.; Webster, R. L.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Remillard, R. A.; Williams, C. L.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Mitchell, D. A.; Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Melbourne, Vic, Australia. [Morales, M. F.; Hazelton, B. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Lonsdale, C. J.; Cappallo, R. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; Mcwhirter, S. R.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT Haystack Observ, Westford, MA USA. [Wicenec, A.; Williams, A.] Univ Western Australia, ICRAR, Perth, WA 6009, Australia. [Barnes, D.] Monash Univ, Monash E Res Ctr, Melbourne, Vic 3004, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, F.; Mckinley, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Burns, S.] Burns Ind, Nashua, NH USA. [Deshpande, A.; Prabu, T.; Udaya-Shankar, N.; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Oberoi, D.] Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, WV USA. RP Tingay, SJ (reprint author), Curtin Univ Technol, ICRAR, Perth, WA, Australia. EM s.tingay@curtin.edu.au RI Bunton, John/A-4944-2008; Gaensler, Bryan/F-8655-2010; Kasper, Justin/D-1152-2010; Wayth, Randall/B-2444-2013; Subrahmanyan, Ravi/D-4889-2012; Williams, Andrew/K-2931-2013; Emrich, David/B-7002-2013; Kudryavtseva, Nadezhda/F-2472-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; OI Kasper, Justin/0000-0002-7077-930X; Wayth, Randall/0000-0002-6995-4131; Wyithe, Stuart/0000-0001-7956-9758; Williams, Andrew/0000-0001-9080-0105; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Gaensler, Bryan/0000-0002-3382-9558; Kudryavtseva, Nadia/0000-0002-1372-0942 FU U.S. National Science Foundation [AST CAREER-0847753, AST-0457585, AST-0908884, PHY-0835713]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; New Zealand Ministry of Economic Development [MED-E1799]; IBM Shared University Research Grant (via VUW); Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington; Australian Federal government via the National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia-India Strategic Research Fund; Astronomy Australia Limited; iVEC Petabyte Data Store; Initiative in Innovative Computing; NVIDIA; International Centre for Radio Astronomy Research; Joint Venture of Curtin University; The University of Western Australia; Western Australian State government; IBM Shared University Research Grant (via Curtin) FX We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST CAREER-0847753, AST-0457585, AST-0908884, and PHY-0835713), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020), New Zealand Ministry of Economic Development (grant MED-E1799), an IBM Shared University Research Grant (via VUW and Curtin), the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, the Victoria University of Wellington, the Australian Federal government via the National Collaborative Research Infrastructure Strategy, Education Investment Fund and the Australia-India Strategic Research Fund and Astronomy Australia Limited, under contract to Curtin University, the iVEC Petabyte Data Store, the Initiative in Innovative Computing and NVIDIA sponsored CUDA Center for Excellence at Harvard, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 49 TC 82 Z9 82 U1 0 U2 15 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD JAN 24 PY 2013 VL 30 AR UNSP e007 DI 10.1017/pasa.2012.007 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 161ZN UT WOS:000320233700001 ER PT J AU Cirtain, JW Golub, L Winebarger, AR De Pontieu, B Kobayashi, K Moore, RL Walsh, RW Korreck, KE Weber, M McCauley, P Title, A Kuzin, S DeForest, CE AF Cirtain, J. W. Golub, L. Winebarger, A. R. De Pontieu, B. Kobayashi, K. Moore, R. L. Walsh, R. W. Korreck, K. E. Weber, M. McCauley, P. Title, A. Kuzin, S. DeForest, C. E. TI Energy release in the solar corona from spatially resolved magnetic braids SO NATURE LA English DT Article ID EVOLVING FIELDS; HEATING PROBLEM; NEUTRAL SHEETS; ALFVENIC WAVES; ACTIVE-REGION; CHROMOSPHERE; LOOPS; POWER; WIND AB It is now apparent that there are at least two heating mechanisms in the Sun's outer atmosphere, or corona(1-5). Wave heating may be the prevalent mechanism in quiet solar periods and may contribute to heating the corona to 1,500,000K (refs 1-3). The active corona needs additional heating to reach 2,000,000-4,000,000 K; this heat has been theoretically proposed(6-12) to come from the reconnection and unravelling of magnetic 'braids'. Evidence favouring that process has been inferred(13,14), but has not been generally accepted because observations are sparse and, in general, the braided magnetic strands that are thought(1-3,15-17) to have an angular width of about 0.2 arc seconds have not been resolved(10,18-20). Fine-scale braiding has been seen(21,22) in the chromosphere but not, until now, in the corona. Here we report observations, at a resolution of 0.2 arc seconds, of magnetic braids in a coronal active region that are reconnecting, relaxing and dissipating sufficient energy to heat the structures to about 4,000,000K. Although our 5-minute observations cannot unambiguously identify the field reconnection and subsequent relaxation as the dominant heating mechanism throughout active regions, the energy available from the observed field relaxation in our example is ample for the observed heating. C1 [Golub, L.; Korreck, K. E.; Weber, M.; McCauley, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Title, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Kobayashi, K.] Univ Alabama Huntsville, Ctr Space & Aeronaut Res, Huntsville, AL 35812 USA. [Walsh, R. W.] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [Kuzin, S.] PN Lebedev Phys Inst, Moscow 119991, Russia. [DeForest, C. E.] SW Res Inst, Instrumentat & Space Res Div, Boulder, CO 80302 USA. EM jonathan.w.cirtain@nasa.gov RI Kuzin, Sergey/M-3435-2015; McCauley, Patrick/P-7747-2015 OI McCauley, Patrick/0000-0002-1450-7350 FU Russian Foundation for Basic Research [11-02-01079-a]; Presidium of the Russian Academy of Sciences [22] FX We thank the NASA Low-Cost Access to Space programme for supporting the development of the Hi-C instrument, the NASA Sounding Rocket Office for the launch of the instrument and the NASA Marshall Space Flight Center for instrument development support. This LPI work was supported in part by the Russian Foundation for Basic Research (project 11-02-01079-a), Program No. 22 of the Presidium of the Russian Academy of Sciences. NR 24 TC 96 Z9 96 U1 1 U2 28 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 24 PY 2013 VL 493 IS 7433 BP 501 EP 503 DI 10.1038/nature11772 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 075GF UT WOS:000313871400031 PM 23344359 ER PT J AU Hill, MS Hill, AL Lopez, J Peterson, KJ Pomponi, S Diaz, MC Thacker, RW Adamska, M Boury-Esnault, N Cardenas, P Chaves-Fonnegra, A Danka, E De Laine, BO Formica, D Hajdu, E Lobo-Hajdu, G Klontz, S Morrow, CC Patel, J Picton, B Pisani, D Pohlmann, D Redmond, NE Reed, J Richey, S Riesgo, A Rubin, E Russell, Z Rutzler, K Sperling, EA di Stefano, M Tarver, JE Collins, AG AF Hill, Malcolm S. Hill, April L. Lopez, Jose Peterson, Kevin J. Pomponi, Shirley Diaz, Maria C. Thacker, Robert W. Adamska, Maja Boury-Esnault, Nicole Cardenas, Paco Chaves-Fonnegra, Andia Danka, Elizabeth De laine, Bre-Onna Formica, Dawn Hajdu, Eduardo Lobo-Hajdu, Gisele Klontz, Sarah Morrow, Christine C. Patel, Jignasa Picton, Bernard Pisani, Davide Pohlmann, Deborah Redmond, Niamh E. Reed, John Richey, Stacy Riesgo, Ana Rubin, Ewelina Russell, Zach Ruetzler, Klaus Sperling, Erik A. di Stefano, Michael Tarver, James E. Collins, Allen G. TI Reconstruction of Family-Level Phylogenetic Relationships within Demospongiae (Porifera) Using Nuclear Encoded Housekeeping Genes SO PLOS ONE LA English DT Article ID 18S RIBOSOMAL-RNA; SPONGES PORIFERA; SEQUENCE ALIGNMENT; PHYLUM PORIFERA; MARINE SPONGES; CALCAREOUS SPONGES; MOLECULAR CLOCKS; FOSSIL RECORD; FRESH-WATER; EVOLUTION AB Background: Demosponges are challenging for phylogenetic systematics because of their plastic and relatively simple morphologies and many deep divergences between major clades. To improve understanding of the phylogenetic relationships within Demospongiae, we sequenced and analyzed seven nuclear housekeeping genes involved in a variety of cellular functions from a diverse group of sponges. Methodology/Principal Findings: We generated data from each of the four sponge classes (i.e., Calcarea, Demospongiae, Hexactinellida, and Homoscleromorpha), but focused on family-level relationships within demosponges. With data for 21 newly sampled families, our Maximum Likelihood and Bayesian-based approaches recovered previously phylogenetically defined taxa: Keratosa(p), Myxospongiae(p), Spongillida(p), Haploscleromorpha(p) (the marine haplosclerids) and Democlavia(p). We found conflicting results concerning the relationships of Keratosa(p) and Myxospongiae(p) to the remaining demosponges, but our results strongly supported a clade of Haploscleromorpha(p)+Spongillida(p)+Democlavia(p). In contrast to hypotheses based on mitochondrial genome and ribosomal data, nuclear housekeeping gene data suggested that freshwater sponges (Spongillida(p)) are sister to Haploscleromorpha(p) rather than part of Democlavia(p). Within Keratosa(p), we found equivocal results as to the monophyly of Dictyoceratida. Within Myxospongiae(p), Chondrosida and Verongida were monophyletic. A well-supported clade within Democlavia(p), Tetractinellida(p), composed of all sampled members of Astrophorina and Spirophorina (including the only lithistid in our analysis), was consistently revealed as the sister group to all other members of Democlavia(p). Within Tetractinellida(p), we did not recover monophyletic Astrophorina or Spirophorina. Our results also reaffirmed the monophyly of order Poecilosclerida (excluding Desmacellidae and Raspailiidae), and polyphyly of Hadromerida and Halichondrida. Conclusions/Significance: These results, using an independent nuclear gene set, confirmed many hypotheses based on ribosomal and/or mitochondrial genes, and they also identified clades with low statistical support or clades that conflicted with traditional morphological classification. Our results will serve as a basis for future exploration of these outstanding questions using more taxon- and gene-rich datasets. C1 [Hill, Malcolm S.; Hill, April L.; Danka, Elizabeth; De laine, Bre-Onna; Pohlmann, Deborah; Richey, Stacy; Russell, Zach; di Stefano, Michael] Univ Richmond, Gottwald Sci Ctr, Richmond, VA 23173 USA. [Lopez, Jose; Chaves-Fonnegra, Andia; Formica, Dawn; Patel, Jignasa; Rubin, Ewelina] Nova SE Univ, Oceanog Ctr, Dania, FL USA. [Peterson, Kevin J.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Pomponi, Shirley; Reed, John] Florida Atlantic Univ, Oceanog Inst, Harbor Branch, Ft Pierce, FL USA. [Diaz, Maria C.] Museo Marino de Margarita, Boca Del Rio, Nueva Esparta, Venezuela. [Thacker, Robert W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Adamska, Maja] Sars Int Ctr Marine Mol Biol, Bergen, Norway. [Boury-Esnault, Nicole] Univ Aix Marseille, CNRS, IMBE, UMR7263,Stn Marine Endoume, Marseille, France. [Cardenas, Paco] Uppsala Univ, Evolutionary Biol Ctr, Dept Systemat Biol, Uppsala, Sweden. [Hajdu, Eduardo] Univ Fed Rio de Janeiro, Museu Nacl, Dept Invertebrados, Rio De Janeiro, Brazil. [Lobo-Hajdu, Gisele] Univ Estado Rio de Janeiro, IBRAG, Dept Genet, BR-20550011 Rio De Janeiro, Brazil. [Klontz, Sarah; Redmond, Niamh E.; Ruetzler, Klaus; Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Morrow, Christine C.] Queens Univ Belfast, Sch Biol Sci, MBC, Belfast, Antrim, North Ireland. [Picton, Bernard] Natl Museums No Ireland, Holywood, North Ireland. [Pisani, Davide; Tarver, James E.] Univ Bristol, Sch Earth Sci, Bristol, Avon, England. [Pisani, Davide] Univ Bristol, Sch Biol Sci, Bristol, Avon, England. [Riesgo, Ana] Harvard Univ, Museum Comparat Zool, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Sperling, Erik A.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab NOAAs Fisheries Serv, Washington, DC 20560 USA. RP Collins, AG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM collinsa@si.edu RI Lobo-Hajdu, G/A-6709-2008; Lopez, Jose/F-8809-2011; Inca, Inct/K-2204-2013; Riesgo, Ana/E-3341-2014; Adamska, Maja/M-4128-2014; Hill, Malcolm/B-6204-2015; Hajdu, Eduardo/C-3863-2009; Adamska, Maja/L-3306-2015; OI Lobo-Hajdu, G/0000-0001-7792-9609; Lopez, Jose/0000-0002-1637-4125; Riesgo, Ana/0000-0002-7993-1523; Adamska, Maja/0000-0002-4223-8450; Danka, Elizabeth/0000-0001-5705-9466; Picton, Bernard/0000-0002-1500-2215 FU National Science Foundation's Assembling the Tree of Life Program; DEB award [0829763, 0829783, 0829791, 0829986] FX This work was supported by the National Science Foundation's Assembling the Tree of Life Program (http://www.nsf.gov/funding/pgm_summ.jsp?pims_ id = 5129; DEB awards 0829763, 0829783, 0829791, and 0829986). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 89 TC 19 Z9 19 U1 2 U2 48 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 23 PY 2013 VL 8 IS 1 AR e50437 DI 10.1371/journal.pone.0050437 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 077IQ UT WOS:000314021500004 PM 23372644 ER PT J AU Loreau, J Kharchenko, V Dalgarno, A AF Loreau, J. Kharchenko, V. Dalgarno, A. TI Index of refraction of molecular nitrogen for sodium matter waves SO PHYSICAL REVIEW A LA English DT Article ID INTERFEROMETRY; SCATTERING; COLLISIONS; OPTICS; GASES AB We calculate the index of refraction of sodium matter waves propagating through a gas of nitrogen molecules. We use a recent ab initio potential for the ground state of the NaN2 van der Waals complex to perform quantal close-coupling calculations and compute the index of refraction as a function of the projectile velocity. We obtain good agreement with the available experimental data. We show that the refractive index contains glory oscillations but that they are damped by the averaging over the thermal motion of the N-2 molecules. These oscillations appear at lower temperatures and projectile velocity. We also investigate the behavior of the refractive index at low temperature and low projectile velocity to show its dependence on the rotational state of N-2 and discuss the advantage of using diatomic molecules as projectiles. DOI: 10.1103/PhysRevA.87.012708 C1 [Loreau, J.; Kharchenko, V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RP Loreau, J (reprint author), Univ Libre Brussels, Serv Chim Quant & Photophys, Brussels, Belgium. OI Loreau, Jerome/0000-0002-6142-1509 FU US Department of Energy FX We thank T. Tscherbul for his help with computational issues as well as D. Pritchard and A. Cronin for discussions. This work was supported by the US Department of Energy. NR 26 TC 1 Z9 1 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JAN 22 PY 2013 VL 87 IS 1 AR 012708 DI 10.1103/PhysRevA.87.012708 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 076EI UT WOS:000313938900007 ER PT J AU Ewing, I Christian, DJ Bodewits, D Dennerl, K Lisse, CM Wolk, SJ AF Ewing, Ian Christian, Damian J. Bodewits, Dennis Dennerl, Konrad Lisse, Carey M. Wolk, Scott J. TI EMISSION LINES BETWEEN 1 AND 2 keV IN COMETARY X-RAY SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: general; comets: individual (C/1999 S4 (LINEAR), C/1999 T1 (McNaught-Hartley), 153P/2002 (Ikeya-Zhang), 2P/2003 (Encke), C/2008 8P (Tuttle)); solar wind; techniques: spectroscopic; X-rays: general ID CHARGE-EXCHANGE EMISSION; CORONAL MASS EJECTION; CHANDRA OBSERVATIONS; XMM-NEWTON; IONS; SPECTROMETER; SYSTEM; M82 AB We present the detection of new cometary X-ray emission lines in the 1.0-2.0 keV range using a sample of comets observed with the Chandra X-Ray Observatory and ACIS spectrometer. We have selected five comets from the Chandra sample with good signal-to-noise spectra. The surveyed comets are C/1999 S4 (LINEAR), C/1999 T1 (McNaught-Hartley), 153P/2002 (Ikeya-Zhang), 2P/2003 (Encke), and C/2008 8P (Tuttle). We modeled the spectra with an extended version of our solar wind charge exchange (SWCX) emission model. Above 1 keV, we find Ikeya-Zhang to have strong emission lines at 1340 and 1850 eV which we identify as being created by SWCX lines of Mg XI and Si XIII, respectively, and weaker emission lines at 1470, 1600, and 1950 eV formed by SWCX of Mg XII, Mg XI, and Si XIV, respectively. The Mg XI and XII and Si XIII and XIV lines are detected at a significant level for the other comets in our sample (LS4, MH, Encke, 8P), and these lines promise additional diagnostics to be included in SWCX models. The silicon lines in the 1700-2000 eV range are detected for all comets, but with the rising background and decreasing cometary emission, we caution that these detections need further confirmation with higher resolution instruments. C1 [Ewing, Ian; Christian, Damian J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Bodewits, Dennis] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Dennerl, Konrad] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Planetary Explorat Grp, Dept Space, Laurel, MD 20723 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ewing, I (reprint author), Calif State Univ Northridge, Dept Phys & Astron, 18111 Nordhoff St, Northridge, CA 91330 USA. EM ian.ewing.794@my.csun.edu; daman.christian@csun.edu RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020 FU Chandra archival grants [CXO-09100455, CXO-13100089]; CSUN Department of Physics and Astronomy FX This research was supported by Chandra archival grants CXO-09100455 and CXO-13100089. D.C. also thanks the CSUN Department of Physics and Astronomy for start-up funds in support of this research. We thank an anonymous referee for suggested improvements. We thank S. Lepri for useful discussion on solar wind abundances, and we thank an anonymous referee for suggested improvements. NR 40 TC 5 Z9 5 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2013 VL 763 IS 1 AR 66 DI 10.1088/0004-637X/763/1/66 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 069SH UT WOS:000313456700066 ER PT J AU Ma, CJ McNamara, BR Nulsen, PEJ AF Ma, C. -J. McNamara, B. R. Nulsen, P. E. J. TI RADIO ACTIVE GALAXY NUCLEI IN GALAXY CLUSTERS: HEATING HOT ATMOSPHERES AND DRIVING SUPERMASSIVE BLACK HOLE GROWTH OVER COSMIC TIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; quasars: general; radio continuum: galaxies; X-rays: galaxies: clusters ID SKY SURVEY DATA; X-RAY-CLUSTERS; GALACTIC NUCLEI; COOLING FLOWS; JET POWER; LUMINOSITY FUNCTION; INTRACLUSTER MEDIUM; CHANDRA OBSERVATION; ELLIPTIC GALAXIES; NEARBY CLUSTERS AB We estimate the average radio active galactic nucleus (AGN, mechanical) power deposited into the hot atmospheres of galaxy clusters over more than three quarters of the age of the Universe. Our sample was drawn from eight major X-ray cluster surveys and includes 685 clusters in the redshift range 0.1 < z < 0.6 that overlap the area covered by the NRAO VLA Sky Survey (NVSS). The radio-AGN mechanical power was estimated from the radio luminosity of central NVSS sources, using the relation of Cavagnolo et al. that is based on mechanical powers determined from the enthalpies of X-ray cavities. We find only a weak correlation between radio luminosity and cluster X-ray luminosity, although the most powerful radio sources reside in luminous clusters. The average AGN mechanical power of 3 x 10(44) erg s(-1) exceeds the X-ray luminosity of 44% of the clusters, indicating that the accumulation of radio-AGN energy is significant in these clusters. Integrating the AGN mechanical power to redshift z = 2.0, using simple models for its evolution and disregarding the hierarchical growth of clusters, we find that the AGN energy accumulated per particle in low luminosity X-ray clusters exceeds 1 keV per particle. This result represents a conservative lower limit to the accumulated thermal energy. The estimate is comparable to the level of energy needed to "preheat" clusters, indicating that continual outbursts from radio-AGN are a significant source of gas energy in hot atmospheres. Assuming an average mass conversion efficiency of eta = 0.1, our result implies that the supermassive black holes that released this energy did so by accreting an average of similar to 10(9) M-circle dot over time, which is comparable to the level of growth expected during the quasar era. C1 [Ma, C. -J.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Ma, C. -J.; McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. RP Ma, CJ (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. OI Nulsen, Paul/0000-0003-0297-4493 FU Chandra Large Project Grant [G09-0140X]; Natural Sciences and Engineering Research Council of Canada; NASA [NAS8-03060] FX C.-J.M. and B.R.M. are supported by Chandra Large Project Grant: G09-0140X. B. R. M. acknowledges generous support from the Natural Sciences and Engineering Research Council of Canada. P.E.J.N. was supported by NASA grant NAS8-03060. C.-J.M. thanks Harald Ebeling for his comments to improve the draft. This research makes use of the FIRST and NVSS radio surveys. This research has made use of the archived data and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. NR 95 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2013 VL 763 IS 1 AR 63 DI 10.1088/0004-637X/763/1/63 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 069SH UT WOS:000313456700063 ER PT J AU Naoz, S Yoshida, N Gnedin, NY AF Naoz, Smadar Yoshida, Naoki Gnedin, Nickolay Y. TI SIMULATIONS OF EARLY BARYONIC STRUCTURE FORMATION WITH STREAM VELOCITY. II. THE GAS FRACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; early universe; galaxies: formation; galaxies: halos ID HIGH-REDSHIFT GALAXIES; COSMIC DARK-AGES; COSMOLOGICAL SIMULATIONS; 1ST GALAXIES; STAR-FORMATION; INTERGALACTIC MEDIUM; CHEMICAL ENRICHMENT; PRIMORDIAL GAS; MASS FUNCTION; REIONIZATION AB Understanding the gas content of high-redshift halos is crucial for studying the formation of the first generation of galaxies and reionization. Recently, Tseliakhovich & Hirata showed that the relative "stream" velocity between the dark matter and baryons at the time of recombination-formally a second-order effect, but an unusually large one-can influence the later structure formation history of the universe. We quantify the effect of the stream velocity on the so-called characteristic mass-the minimum mass of a dark matter halo capable of retaining most of its baryons throughout its formation epoch-using three different high-resolution sets of cosmological simulations (with separate transfer functions for baryons and dark matter) that vary in box size, particle number, and the value of the relative velocity between the dark matter and baryons. In order to understand this effect theoretically, we generalize the linear theory filtering mass to properly account for the difference between the dark matter and baryonic density fluctuation evolution induced by the stream velocity. We show that the new filtering mass provides an accurate estimate for the characteristic mass, while other theoretical ansatzes for the characteristic mass are substantially less precise. C1 [Naoz, Smadar] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Yoshida, Naoki] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Gnedin, Nickolay Y.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Gnedin, Nickolay Y.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Gnedin, Nickolay Y.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Gnedin, Nickolay Y.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM snaoz@cfa.harvard.edu OI Naoz, Smadar/0000-0002-9802-9279 FU Information Technology at Northwestern University; NASA; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [PF2-130096] FX We thank Avi Loeb, Rennan Barkana, Andrey Kravtsov, Neal Dalal, Will Farr, Matt McQuinn, and Dmitriy Tseliakhovich for useful discussions. We thank Dmitriy Tseliakhovich for providing his code. We also thank Yoram Lithwick for the use of his allocation time on the computer cluster Quest. This research was supported in part through the computational resources and staff contributions provided by Information Technology at Northwestern University as part of its shared cluster program, Quest. S.N. is supported by NASA through a Einstein Postdoctoral Fellowship awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract PF2-130096. NR 63 TC 24 Z9 24 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2013 VL 763 IS 1 AR 27 DI 10.1088/0004-637X/763/1/27 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 069SH UT WOS:000313456700027 ER PT J AU Takahashi, S Ho, PTP Teixeira, PS Zapata, LA Su, YN AF Takahashi, Satoko Ho, Paul T. P. Teixeira, Paula S. Zapata, Luis A. Su, Yu-Nung TI HIERARCHICAL FRAGMENTATION OF THE ORION MOLECULAR FILAMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (OMC-3, Orion A); ISM: structure; stars: formation; stars: protostars ID SUBMILLIMETER-WAVE OBSERVATIONS; STAR-FORMING REGIONS; MAGNETIC-FIELDS; ANGULAR-MOMENTUM; CARBON-MONOXIDE; HIGH-RESOLUTION; NEBULA-CLUSTER; OMC-2/3 REGION; DENSE CORES; CLOUD CORES AB We present a high angular resolution map of the 850 mu m continuum emission of the Orion Molecular Cloud-3 (OMC 3) obtained with the Submillimeter Array (SMA); the map is a mosaic of 85 pointings covering an approximate area of 6'.5 x 2'.0 (0.88 x 0.27 pc). We detect 12 spatially resolved continuum sources, each with an H-2 mass between 0.3-5.7 M-circle dot and a projected source size between 1400-8200 AU. All the detected sources are on the filamentary main ridge (n(H2) >= 10(6) cm(-3)), and analysis based on the Jeans theorem suggests that they are most likely gravitationally unstable. Comparison of multi-wavelength data sets indicates that of the continuum sources, 6/12 (50%) are associated with molecular outflows, 8/12 (67%) are associated with infrared sources, and 3/12 (25%) are associated with ionized jets. The evolutionary status of these sources ranges from prestellar cores to protostar phase, confirming that OMC-3 is an active region with ongoing embedded star formation. We detect quasi-periodical separations between the OMC-3 sources of approximate to 17 ''/0.035 pc. This spatial distribution is part of a large hierarchical structure that also includes fragmentation scales of giant molecular cloud (approximate to 35 pc), large-scale clumps (approximate to 1.3 pc), and small-scale clumps (approximate to 0.3 pc), suggesting that hierarchical fragmentation operates within the Orion A molecular cloud. The fragmentation spacings are roughly consistent with the thermal fragmentation length in large-scale clumps, while for small-scale cores it is smaller than the local fragmentation length. These smaller spacings observed with the SMA can be explained by either a helical magnetic field, cloud rotation, or/and global filament collapse. Finally, possible evidence for sequential fragmentation is suggested in the northern part of the OMC-3 filament. C1 [Takahashi, Satoko; Ho, Paul T. P.; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teixeira, Paula S.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Teixeira, Paula S.] Univ Lisbon, Inst D Luiz SIM, Lab Associado, P-1749016 Lisbon, Portugal. [Zapata, Luis A.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. RP Takahashi, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM satoko_t@asiaa.sinica.edu.tw RI Teixeira, Paula Stella/O-2289-2013 OI Teixeira, Paula Stella/0000-0002-3665-5784 FU Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan; ESO (Garching); MPIfR FX We acknowledge the staff at the Submillimeter Array and the Very Large Array for assistance with operations and helpful comments related to data reduction. S. T. acknowledges K. Asada, B.-C. Hsieh, Z.-W. Zhang, A. Hacar, K. Saigo, and H. Hirashita, D. Johnstone for fruitful comments. We also thank D. Johnstone for providing us the submillimeter continuum data taken with the JCMT/SCUBA. S.T. is financially supported by a postdoctoral fellowship at the Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan, and was supported by visitor programs at ESO (Garching) and MPIfR, while visiting co-authors P. S. Teixeira and L. A. Zapata, respectively. NR 97 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 2013 VL 763 IS 1 AR 57 DI 10.1088/0004-637X/763/1/57 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 069SH UT WOS:000313456700057 ER PT J AU Hinkley, S Hillenbrand, L Oppenheimer, BR Rice, EL Pueyo, L Vasisht, G Zimmerman, N Kraus, AL Ireland, MJ Brenner, D Beichman, C Dekany, R Roberts, JE Parry, IR Roberts, LC Crepp, JR Burruss, R Wallace, JK Cady, E Zhai, CX Shao, M Lockhart, T Soummer, R Sivaramakrishnan, A AF Hinkley, Sasha Hillenbrand, Lynne Oppenheimer, Ben R. Rice, Emily L. Pueyo, Laurent Vasisht, Gautam Zimmerman, Neil Kraus, Adam L. Ireland, Michael J. Brenner, Douglas Beichman, Charles Dekany, Richard Roberts, Jennifer E. Parry, Ian R. Roberts, Lewis C., Jr. Crepp, Justin R. Burruss, Rick Wallace, J. Kent Cady, Eric Zhai, Chengxing Shao, Michael Lockhart, Thomas Soummer, Remi Sivaramakrishnan, Anand TI HIGH-RESOLUTION INFRARED IMAGING AND SPECTROSCOPY OF THE Z CANIS MAJORIS SYSTEM DURING QUIESCENCE AND OUTBURST SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; instrumentation: adaptive optics; stars: individual (Z CMa); stars: pre-main sequence ID Z-CMA; ADAPTIVE OPTICS; COMPANION; OBJECTS; HERBIG; SCALE; DISK; ACCRETION; EVOLUTION; DISCOVERY AB We present adaptive optics photometry and spectra in the JHKL bands along with high spectral resolution K-band spectroscopy for each component of the Z Canis Majoris system. Our high angular resolution photometry of this very young (less than or similar to 1 Myr) binary, comprised of an FU Ori object and a Herbig Ae/Be star, was gathered shortly after the 2008 outburst while our high-resolution spectroscopy was gathered during a quiescent phase. Our photometry conclusively determines that the outburst was due solely to the embedded Herbig Ae/Be member, supporting results from earlier works, and that the optically visible FU Ori component decreased slightly (similar to 30%) in luminosity during the same period, consistent with previous works on the variability of FU Ori type systems. Further, our high-resolution K-band spectra definitively demonstrate that the 2.294 mu m CO absorption feature seen in composite spectra of the system is due solely to the FU Ori component, while a prominent CO emission feature at the same wavelength, long suspected to be associated with the innermost regions of a circumstellar accretion disk, can be assigned to the Herbig Ae/Be member. These findings clarify previous analyses of the origin of the CO emission in this complex system. C1 [Hinkley, Sasha; Hillenbrand, Lynne; Crepp, Justin R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Oppenheimer, Ben R.; Rice, Emily L.; Zimmerman, Neil; Brenner, Douglas] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Rice, Emily L.] CUNY Coll Staten Isl, Dept Engn Sci & Phys, Staten Isl, NY 10314 USA. [Pueyo, Laurent; Soummer, Remi; Sivaramakrishnan, Anand] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Vasisht, Gautam; Roberts, Jennifer E.; Roberts, Lewis C., Jr.; Burruss, Rick; Wallace, J. Kent; Cady, Eric; Zhai, Chengxing; Shao, Michael; Lockhart, Thomas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zimmerman, Neil] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kraus, Adam L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, Macquarie Pk, NSW 2109, Australia. [Ireland, Michael J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Beichman, Charles] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Dekany, Richard] CALTECH, Caltech Opt Observ, Pasadena, CA 91125 USA. [Parry, Ian R.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Hinkley, S (reprint author), CALTECH, Dept Astron, 1200 E Calif Blvd,MC 249-17, Pasadena, CA 91125 USA. RI Rice, Emily/G-4446-2013; OI Rice, Emily/0000-0002-3252-5886; Zimmerman, Neil/0000-0001-5484-1516 FU NASA through the Sagan Fellowship Program; National Science Foundation [AST-1203023, AST-0804417, 0334916, 0215793, 0520822, 1245018]; internal Research and Technology Development funds; W. M. Keck Foundation FX This work was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. A portion of this work was supported by the National Science Foundation under grant Nos. AST-1203023, AST-0804417, 0334916, 0215793, 0520822, and 1245018. A portion of the research in this Letter was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration, and was funded by internal Research and Technology Development funds. The authors thank Pat Hartigan for his help obtaining the Keck/NIRSPEC observations. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 46 TC 11 Z9 11 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 20 PY 2013 VL 763 IS 1 AR L9 DI 10.1088/2041-8205/763/1/L9 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 071CY UT WOS:000313564500009 ER PT J AU Knapp, LW AF Knapp, Leslie W. TI Descriptions of four new species of Thysanophrys (Scorpaeniformes: Platycephalidae) from the Western Indian Ocean SO ZOOTAXA LA English DT Article DE Thysanophrys randalli sp nov.; T. rarita sp nov.; T. springeri sp nov.; T. tricaudata sp nov.; T. chiltonae; Platycephalidae; western Indian Ocean AB Four new species of Thysanophrys are described from the Western Indian Ocean (WIO). T. rarita, known from a single specimen taken off Somalia, is provisionally placed in Thysanophrys and is distinguished by its color pattern and number of preocular and suborbital spines. T. tricaudata is described from three specimens taken at SCUBA stations off southwestern Sri Lanka. They differ from other western Indian Ocean (WIO) Thysanophrys in color pattern, lack of ocular flaps, number of dorsal fin spines and scale counts. The remaining two new species are somewhat similar to the widespread Indo-Pacific species, T. chiltonae Schultz (1966). T. randalli is described from specimens taken at the Amirante Islands and Mauritius. It may also be widespread in the Indo-Pacific, but differs from T. chiltonae in nasal spine structure, color pattern, type of iris lappet margin, and in having a much shorter maximum size. T. springeri also appears to be a smaller species than T. chiltonae and, aside from one record off Djibouti, is restricted to Red Sea. It also differs from T. chiltonae in color pattern, in having fewer pectoral rays and fewer scale rows between the second dorsal-fin insertion and the lateral line. Although T. chiltonae is relatively common in the northern Indian Ocean, it does not appear to have entered the Red Sea. C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20013 USA. RP Knapp, LW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 534,POB 37012, Washington, DC 20013 USA. EM knappl@si.edu NR 12 TC 0 Z9 0 U1 0 U2 7 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD JAN 17 PY 2013 VL 3608 IS 2 BP 127 EP 136 PG 10 WC Zoology SC Zoology GA 074GS UT WOS:000313801500003 PM 24614455 ER PT J AU Safavi-Naini, A Soyler, SG Pupillo, G Sadeghpour, HR Capogrosso-Sansone, B AF Safavi-Naini, A. Soeyler, S. G. Pupillo, G. Sadeghpour, H. R. Capogrosso-Sansone, B. TI Quantum phases of dipolar bosons in bilayer geometry SO NEW JOURNAL OF PHYSICS LA English DT Article ID POLAR-MOLECULES; SIMULATION; CHAINS AB We investigate the quantum phases of hard-core dipolar bosons confined to a square lattice in a bilayer geometry. Using exact theoretical techniques, we discuss the many-body effects resulting from the pairing of particles across layers at finite density, including a novel pair supersolid, superfluid and solid phases. These results are of direct relevance to experiments with polar molecules and atoms with large magnetic dipole moments trapped in optical lattices. C1 [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Safavi-Naini, A.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Soeyler, S. G.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy. [Pupillo, G.] Univ Strasbourg, ISIS UMR 7006, Strasbourg, France. [Pupillo, G.] Univ Strasbourg, IPCMS UMR 7504, Strasbourg, France. [Pupillo, G.] CNRS, Strasbourg, France. [Capogrosso-Sansone, B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. RP Safavi-Naini, A (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM safavin@mit.edu FU ERC-St Grant (ColDSIM) [307688]; EOARD; NSF FX BC-S and, SGS thank A Kuklov for enlightening discussions. GP is supported by an ERC-St Grant 2012 (ColDSIM, 307688) and EOARD. This work was supported by the NSF through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. NR 45 TC 7 Z9 7 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JAN 17 PY 2013 VL 15 AR 013036 DI 10.1088/1367-2630/15/1/013036 PG 11 WC Physics, Multidisciplinary SC Physics GA 071TJ UT WOS:000313617000003 ER PT J AU Deng, LW Seagle, C Fei, YW Shahar, A AF Deng, Liwei Seagle, Christopher Fei, Yingwei Shahar, Anat TI High pressure and temperature electrical resistivity of iron and implications for planetary cores SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MERCURYS MAGNETIC-FIELD; THERMAL-CONDUCTIVITY; TIME VARIATIONS; EARTHS CORE; LIQUID FE; MARS; EVOLUTION; GRAVITY; TRANSITION; INTERIOR AB Electrical resistivity measurements of polycrystalline iron have been performed at 5, 7, and 15 GPa and in the temperature range 293-2200 K by employing a four-wired method. The kinks in electrical resistivity associated with solid iron phase transitions and the solid to liquid transition were clearly observed upon increasing temperature. Geometry corrections due to volume variations with pressure and temperature were applied to the entire data set. High pressure and temperature thermal conductivity were calculated by fitting resistivity data through the Wiedemann-Franz law. The temperature dependences of electrical resistivity and thermal conductivity for alpha, gamma, and epsilon solid iron have been determined at high-pressure conditions. Our study provides the first experimental constraint on the heat flux conducted at Mercury's outmost core, estimated to be 0.29-0.36 TW, assuming an adiabatic core. Extrapolations of our data to Martian outer core conditions yield a series of heat transport parameters (e. g., electrical resistivity, thermal conductivity, and heat flux), which are in reasonable comparison with various geophysical estimates. Citation: Deng, L., C. Seagle, Y. Fei, and A. Shahar (2013), High pressure and temperature electrical resistivity of iron and implications for planetary cores, Geophys. Res. Lett., 40, 33-37, doi: 10.1029/2012GL054347. C1 [Deng, Liwei; Seagle, Christopher; Fei, Yingwei; Shahar, Anat] Carnegie Inst Sci, Geophys Lab, Washington, DC USA. [Seagle, Christopher] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Deng, LW (reprint author), 19 Beitucheng Western Rd, Beijing 100029, Peoples R China. EM dengliwei@mail.iggcas.ac.cn RI 中国科学院, 地球深部研究重点实验室/E-2300-2014; Fei, Yingwei/F-3709-2011; OI Fei, Yingwei/0000-0001-9955-5353; Shahar, Anat/0000-0002-0794-2717 FU NASA [NNX11AC68G]; NSF [EAR0948131]; Carnegie Postdoctoral Fellowship FX The synchrotron radiation experiments were performed at the BL04B1 of Spring-8 with the approval of the Japan Synchrotron Radiation Research Institute (JASRI) (Proposal No. 2011B1550). We thank T. Komabayashi at Tokyo Institute of Technology and Y. Higo at the Spring 8 for experiment assistance. We are indebted to Viktor Struzhkin and Haijun Huang for resistance measurements assisting. This research was supported by NASA grant to YF (NNX11AC68G), NSF grant to AS (EAR0948131), and the Carnegie Postdoctoral Fellowship. NR 35 TC 15 Z9 15 U1 0 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JAN 16 PY 2013 VL 40 IS 1 BP 33 EP 37 DI 10.1029/2012GL054347 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 129GF UT WOS:000317826300007 ER PT J AU Kraus, MJ McInerney, FA Wing, SL Secord, R Baczynski, AA Bloch, JI AF Kraus, Mary J. McInerney, Francesca A. Wing, Scott L. Secord, Ross Baczynski, Allison A. Bloch, Jonathan I. TI Paleohydrologic response to continental warming during the Paleocene-Eocene Thermal Maximum, Bighorn Basin, Wyoming SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE PETM; Paleoclimate; Precipitation; Paleosol; Global warming ID OXYGEN-ISOTOPE; CLIMATE-CHANGE; WILLWOOD FORMATION; SURFACE-TEMPERATURE; BURIAL ALTERATION; SOIL DEVELOPMENT; NORTH-AMERICA; FOSSIL LEAVES; CENTRAL UTAH; EBRO BASIN AB Geologically rapid global warming occurred during the Paleocene-Eocene Thermal Maximum (PETM) similar to 56 Ma. Several studies have argued that important changes occurred in the hydrological cycle during the PETM, but results have been inconsistent, ranging from global increases in humidity to drier conditions. Changes in paleosols during the PETM in the southeastern Bighorn Basin document major drying during the body of the event. Paleosol changes also suggest transitional episodes of climate change that both preceded and followed the PETM. Qualitative, semi-quantitative, and fully quantitative analyses of a similar to 70 m thick interval of paleosols provide a high-resolution record of changes in soil moisture and precipitation. Those changes are compared to changes in temperature determined from 6180 values of tooth enamel from the mammal Coryphodon. A distinct shift to drier soils occurred just prior to the PETM, a conclusion that is consistent with Previous observations that warming began before the onset of the negative carbon isotope excursion associated with the PETM. Paleosols show a progressive drying trend into the lower part of the PETM and become even drier in the upper part of the body of the PETM. Purple-red paleosols that appear during the recovery phase of the PETM indicate wetter soils, although they are better drained than paleosols below the onset. The purple-red paleosols continue for similar to 15 m above the recovery and indicate that wetter soil conditions persisted after the recovery. It is not clear whether changes in the paleosols that preceded and followed the PETM reflect global forcing factors like orbital cycles or release of carbon that lacks an isotopic label; however, such mechanisms would provide a unifying explanation for shifts seen in continental and marine environments. (c) 2012 Elsevier B.V. All rights reserved. C1 [Kraus, Mary J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [McInerney, Francesca A.; Baczynski, Allison A.] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 USA. [Wing, Scott L.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Secord, Ross] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Bloch, Jonathan I.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [McInerney, Francesca A.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. RP Kraus, MJ (reprint author), Univ Colorado, Dept Geol Sci, UCB 399,2200 Colorado Ave, Boulder, CO 80309 USA. EM mary.kraus@colorado.edu RI Kraus, Mary/C-3323-2008; McInerney, Francesca/B-7894-2009; OI Kraus, Mary/0000-0002-1721-2566; McInerney, Francesca/0000-0002-2020-6650; Bloch, Jonathan/0000-0003-1484-6931; Wing, Scott/0000-0002-2954-8905 FU NSF [EAR-0718740, EAR-0717892, EAR-0720268, EAR-0719941, EAR-0640076] FX This research was supported by NSF Awards EAR-0718740 (MJK), EAR-0717892 (SLW), EAR-0720268 (FAM), EAR-0719941 (JIB), and EAR-0640076 (JIB, RS). We are grateful to Douglas Boyer, Stephen Chester, and Paul Morse for their help with DGPS work and fossil collecting, and to the many students and volunteers who helped with field work related to this project. John Krigbaum provided lab support. We thank two anonymous reviewers for constructive reviews that improved the manuscript. NR 104 TC 22 Z9 23 U1 6 U2 52 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD JAN 15 PY 2013 VL 370 BP 196 EP 208 DI 10.1016/j.palaeo.2012.12.008 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 101GB UT WOS:000315762100016 ER PT J AU Jewgenow, K Pukazhenthi, BS Schoen, J AF Jewgenow, K. Pukazhenthi, B. S. Schoen, J. TI Analysis of Sertoli cell efficiency allows the differentiation between two fundamentally different forms of feline teratospermia SO THERIOGENOLOGY LA English DT Article DE Spermatogenesis; Teratospermia; Cat ID DOMESTIC CAT; QUALITY; SPERMATOGENESIS; MORPHOLOGY; MOTILITY AB Teratospermia is a common phenomenon within felid species and has been attributed to reduction in genetic diversity. Testes from teratospermic domestic cats show enhanced spermatogenesis accompanied by remarkably reduced germ cell apoptosis. In the present study we investigated whether free-range teratospermic torn cats exhibit a similar testicular phenotype as proven permanently teratospermic males. Randomly collected teratospermic cats were compared with normal (normospermic; >60% morphologically normal sperm per ejaculate) and a well-characterized population of permanently teratospermic domestic cats, with respect to their spermatogenic potential. Histomorphologic assessment of testes from randomly collected teratospermic cats revealed no differences compared with normospermic donors. These two groups, however, were both different from permanently teratospermic cats, which exhibit fewer Sertoli cells and increased numbers of round spermatids per tubule cross-section resulting in a remarkably increased Sertoli cell efficiency (ratio of round spermatids to Sertoli cells). In conclusion, we can distinguish at least two fundamentally different forms of feline teratospermia. One subtype, found in most of the randomly collected tom cats, but not associated with altered quantitative spermatogenic parameters. Another subtype, found in all permanently teratospermic felids, is manifested by an impairment of Sertoli cell efficiency. We suggest that spermatogenic output should be analyzed before using random source domestic cats to study the phenomenon of teratospermia. (C) 2013 Elsevier Inc. All rights reserved. C1 [Jewgenow, K.] Leibniz Inst Zoo Biol & Wildlife Res IZW, Dept Reprod Biol, Berlin, Germany. [Pukazhenthi, B. S.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA USA. [Schoen, J.] Free Univ Berlin, Inst Vet Biochem, Berlin, Germany. RP Jewgenow, K (reprint author), Leibniz Inst Zoo Biol & Wildlife Res IZW, Dept Reprod Biol, Berlin, Germany. EM jewgenow@izw-berlin.de FU Deutsche Forschungsgemeinschaft [DFG Je 163/9-1, Scho 1231/2-1] FX The authors thank Christiane Franz and Sigrid Holz for their technical assistance, the German Zoos for contributing to the Felid Gametes rescue project, and the Deutsche Forschungsgemeinschaft for funding (DFG Je 163/9-1, Scho 1231/2-1). NR 17 TC 3 Z9 3 U1 0 U2 6 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JAN 15 PY 2013 VL 79 IS 2 BP 261 EP 266 DI 10.1016/j.theriogenology.2012.08.014 PG 6 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 067QX UT WOS:000313311300008 PM 23174773 ER PT J AU Taylor, ML Cairns, SD Agnew, DJ Rogers, AD AF Taylor, M. L. Cairns, S. D. Agnew, D. J. Rogers, A. D. TI A revision of the genus Thouarella Gray, 1870 (Octocorallia: Primnoidae), including an illustrated dichotomous key, a new species description, and comments on Plumarella Gray, 1870 and Dasystenella, Versluys, 1906 SO ZOOTAXA LA English DT Article DE Cnidaria; taxonomic revision; sub-Antarctic; octocoral ID GORGONIANS COELENTERATA; PHYLOGENETIC ANALYSIS; ALEUTIAN ISLANDS; ANTARCTIC WATERS; SOUTHERN-OCEAN; WEDDELL SEA; ANTHOZOA; REPRODUCTION; CNIDARIA; ALCYONACEA AB A comprehensive revision of the genus Thouarella is presented. Thirty-five holotypes of the 38 nominal Thouarella species, two varieties, and one form were examined. The number of original Thouarella species has been reduced to 25, mostly through synonymy or new genus combinations. In the process several new species have also been identified, one of which is described here as Thouarella parachilensis nov. sp. The genus is split into two groups based on polyp arrangement: Group 1 with isolated polyps and Group 2 with polyps in pairs or whorls. An illustrated dichotomous key and detailed character table of the 25 Thouarella species are presented alongside an up-to-date account of all species described in the 19th and 20th centuries and summaries of the few described from 2000 onwards. We propose that Thouarella longispinosa is synonymous with Dasystenella acanthina, T. versluysi with T. brucei, and, T. tenuisquamis, T. flabellata, and T. carinata are synonymous with T. laxa. Lastly, we propose that T. bayeri and T. undulata be placed in Plumarella and support recent suggestions that T. alternata, T. recta, T. superba, and T. diadema are also Plumarella. C1 [Taylor, M. L.] Zool Soc London, Inst Zool, London NW1 4RY, England. [Taylor, M. L.; Agnew, D. J.] Univ London Imperial Coll Sci Technol & Med, Dept Nat Sci, Ascot SL5 7PY, Berks, England. [Taylor, M. L.; Rogers, A. D.] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Cairns, S. D.] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20560 USA. [Agnew, D. J.] Marine Resources Assessment Grp LtD, London, England. RP Taylor, ML (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM michelle.taylor@zoo.ox.ac.uk RI Taylor, Michelle/C-3918-2015 OI Taylor, Michelle/0000-0001-7271-4385 FU Smithsonian Fellowship; NERC CASE Studentship [NE/F00785X/1]; Marine Resources Assessment Group (MRAG) Ltd, London FX This work was sponsored by a Smithsonian Fellowship and NERC CASE Studentship, NE/F00785X/1, in partnership with the Marine Resources Assessment Group (MRAG) Ltd, London. Many useful discussions were had by the first author with Dr Manfred Grasshoff and Rebeca Zapata-Guardiola, for which we are grateful. We would also like to thank the support of individuals at several museums and institutes without whose help in providing holotypes this paper would have been impossible: Andrew Cabrinovic, NHM; Aude Andouche, MNHMP; Elly Beglinger, ZUMA; Rei Ueshima, UMUT; Yukimitsu Imahara, Biological Institute on Kuroshio; Beata M. Pokryszko, MNHWU; Carsten Lueter, ZMB; Dr. Andreas Schmidt-Rhaesa, Zoological Museum, University of Hamburg. At the Smithsonian Institution, where the majority of this work was undertaken, we are indebted to Tim Coffer, Jennifer Hammock, Paul Greenhall and Scott Whittaker. Special thanks are again due to Rebeca Zapata-Guardiola for kindly allowing us to use some of her SEM images and photos; James Soda for preparing stubs and taking some SEM images; Diane Wyse for sclerite measurements and species identifications; and Jon Schleyer for specimen photographs. We reserve special mention and thanks for the late, great Dr F. M. Bayer, whose beautiful SEM images also grace these pages. And, of course, we appreciated the three anonymous reviewers' very useful comments which ultimately improved the manuscript. NR 87 TC 4 Z9 6 U1 1 U2 8 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 14 PY 2013 VL 3602 IS 1 BP 1 EP 105 PG 105 WC Zoology SC Zoology GA 074EO UT WOS:000313795900001 PM 24614121 ER PT J AU Webb, DW Gaimari, SD Hauser, M Holston, KC Metz, MA Irwin, ME Kampmeier, GE Algmin, K AF Webb, Donald W. Gaimari, Stephen D. Hauser, Martin Holston, Kevin C. Metz, Mark A. Irwin, Michael E. Kampmeier, Gail E. Algmin, Kristin TI An annotated catalogue of the New World Therevidae (Insecta: Diptera: Asiloidea) SO ZOOTAXA LA English DT Article DE Asiloidea; distribution; generic combinations; nomenclature; primary type deposition; recent revisions; synonymy; type locality ID LYNEBORG DIPTERA; PHYLOGENETIC REVISION; STILETTO-FLIES; BOMBYLIIDAE DIPTERA; AUSTRALIA DIPTERA; NEARCTIC REGION; IRWIN DIPTERA; NORTH-AMERICA; GENUS; GENERA AB The genera and species of New World stiletto flies (Diptera: Therevidae) are listed, with annotated references to nomenclature, synonymies and generic combinations, type localities, the primary type depositories, distribution, and citations for the most recent revisions. The genus Cyclotelus Walker, 1850 (along with its synonyms Furcifera Krober, 1911, and Epomyia Cole, 1923a) is synonymized under Cerocatus Rondani, 1848. Ectinorhynchus fascipennis Krober, 1911 is given the new name Cerocatus rondanii Gaimari, and Phycus rufiventris Krober, 1911 is given the new name Cerocatus raspii Hauser. Phycus analis Krober, 1911 and Phycus bicolor Krober, 1911, are placed as new combinations in Cerocatus Rondani, as are the following species that were previously in combination with Cyclotelus: Furcifera achaeta Malloch, 1932, Cyclotelus badicrusus Irwin and Webb, 1992, Phycus beckeri Krober, 1911, Epomyia bella Cole, 1923a, Furcifera braziliana Cole, 1960a, Cyclotelus colei Irwin and Lyneborg, 1981a, Thereva diversipes Krober, 1911, Thereva fascipennis Macquart, 1846a, Psilocephala femorata Krober, 1911, Furcifera flavipes Krober, 1928b, Furcifera hardyi Cole, 1960a, Furcifera kroeberi Cole, 1960a, Cyclotelus laetus Walker, 1850, Furcifera longicornis Korber, 1911, Cyclotelus nigroflammus Walker, 1850, Psilocephala nigrifrons Krober, 1914a, Thereva pictipennis Wiedemann, 1821, Furcifera polita Krober, 1911, Cyclotelus pruinosus Walker, 1850, Thereva ruficornis Macquart, 1841a, Psilocephala rufiventris Loew, 1869, Thereva scutellaris Walker, 1857, Cyclotelus silacrusus Irwin and Webb, 1992, Cyclotelus socius Walker, 1850 and Psilocephala sumichrasti Bellardi, 1861. Dialineura pallidiventris Malloch, 1932, Melanothereva blackmani Oldroyd, 1968, Thereva maculicornis Jaennicke, 1867 and Thereva notabilis Macquart, 1841a are placed as new combinations in Entesia Oldroyd. Henicomyia amazonica Irwin and Webb, 1992 is a new synonym of Henicomyia flava Lyneborg, 1972. Henicomyia varipes Krober, 1912a is given revised species status from former synonymy with Henicomyia hubbardii Coquillett, 1898. C1 [Webb, Donald W.; Kampmeier, Gail E.; Algmin, Kristin] Univ Illinois, Illinois Nat Hist Survey, Prairie Res Inst, Champaign, IL 61820 USA. [Gaimari, Stephen D.; Hauser, Martin] Calif Dept Food & Agr, Plant Pest Diagnost Ctr, Sacramento, CA 95832 USA. [Holston, Kevin C.] Swedish Museum Nat Hist, Dept Biodivers Informat, S-10405 Stockholm, Sweden. [Metz, Mark A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM stephen.gaimari@cdfa.ca.gov; martin.hauser@cdfa.ca.gov; kevin.holston@nrm.se; mametz@aol.com; meirwin@illinois.edu; gkamp@illinois.edu; mrozinsk@illinois.edu FU National Science Foundation under PEET [9977958]; Schlinger Foundation; Sequoia Foundation FX We thank the following colleagues for their assistance in the preparation of this catalogue: Dr. R. Rakitov for his assistance in the translation of Russian papers; Illinois Natural History Survey librarians Beth Wohlgemuth and Susan Braxton for their assistance in chasing down obscure references; and the following curators, Dr. Sergio Ibanez-Bernal (IEXA), Dr. Christophe Daugeron (MNHN), Dr. Zachary Falin and Dr. Michael Engel (SEMC), Fritz Geller-Grimm (Museum Wiesbaden, Wiesbaden, Germany), Dr. Nicola Maio (MZUN), Dr. Uwe Kallweit and Dr. Christian Kehlmaier (Museum fur Tierkunde, Dresden, Germany), Dr. Nicola Maio (MZUN), Dr. Erica McAlister (BMNH), Dr. Frank Menzel (DEI), Dr. Adrian Pont (Oxford University), Dr. Norman Penny and Vincent Lee (CAS), Professor Alfio Raspi (Universita di Pisa, Pisa, Italy), Dr. Hans Riefenstahl (ZMUH), Dr. Peter Sehnal (NHMW), Dr. F. Christian Thompson and Dr. David Furth (USNM), Dr. Hans-Peter Tschorsnig (SMNS), Dr. Joachim Ziegler and Dr. Michael Ohl (ZMHB), Dr. Thomas Pape (ZMUC), Dr. Karla Schneider, (MLUH), Dr. Jan E. Raastad (ZMUH), and Dr. Richard Zack (WSUC) for their assistance in verifying information on location of type specimens. Thanks also go to Dr. Shaun Winterton (California Department of Food and Agriculture, Sacramento California, USA) for examining the type of Melanothereva blackmani Oldroyd and letting us know it belongs in Entesia, to Dr. Irina Brake (BMNH) for help with literature, and to Dr. Neal Evenhuis (Bishop Museum, Honolulu, Hawaii, USA), Thomas Pape (ZMUC) and F. Christian Thompson (USNM) for help with some nomenclatural issues. Special thanks to Drs. Alfio Raspi and Nicola Maio for locating and photographing the type of Cerocatus tarsalis Rondani. Thanks are also extended to the following people for permission to use their excellent photographs: Alice Abela (California USA), Stephen Marshall (DEBU), Lynette Schimming (Washington, USA), Shaun Winterton (California Department of Food and Agriculture, Sacramento, California, USA), Harmut Wisch (California, USA). This paper is based upon work supported by the National Science Foundation under PEET Award Number 9977958 (to M.E. Irwin) and support provided by the Schlinger Foundation and the Sequoia Foundation. Any opinions, findings, and conclusions or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of NSF, the Schlinger Foundation or the Sequioa Foundation. NR 314 TC 3 Z9 3 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JAN 11 PY 2013 VL 3600 IS 1 BP 1 EP + PG 95 WC Zoology SC Zoology GA 074DY UT WOS:000313794000001 PM 24614059 ER PT J AU MacGregor, MA Wilner, DJ Rosenfeld, KA Andrews, SM Matthews, B Hughes, AM Booth, M Chiang, E Graham, JR Kalas, P Kennedy, G Sibthorpe, B AF MacGregor, Meredith A. Wilner, David J. Rosenfeld, Katherine A. Andrews, Sean M. Matthews, Brenda Hughes, A. Meredith Booth, Mark Chiang, Eugene Graham, James R. Kalas, Paul Kennedy, Grant Sibthorpe, Bruce TI MILLIMETER EMISSION STRUCTURE IN THE FIRST ALMA IMAGE OF THE AU Mic DEBRIS DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; planet-disk interactions; stars: individual (AU Microscopii); submillimeter: planetary systems ID LOW-MASS STARS; CIRCUMSTELLAR DISK; KUIPER-BELT; DUST DYNAMICS; GRAIN-SIZE; DME STARS; HR 8799; MICROSCOPII; NEARBY; CONSTRAINTS AB We present 1.3 mm ALMA Cycle 0 observations of the edge-on debris disk around the nearby, similar to 10 Myr old, M-type star AU Mic. These observations obtain 0 ''.6 (6 AU) resolution and reveal two distinct emission components: (1) the previously known dust belt that extends to a radius of 40 AU and (2) a newly recognized central peak that remains unresolved. The cold dust belt of mass similar to 1 M-Moon is resolved in the radial direction with a rising emission profile that peaks sharply at the location of the outer edge of the "birth ring" of planetesimals hypothesized to explain the midplane scattered light gradients. No significant asymmetries are discerned in the structure or position of this dust belt. The central peak identified in the ALMA image is similar to 6 times brighter than the stellar photosphere, which indicates an additional emission process in the inner regions of the system. Emission from a stellar corona or activity may contribute, but the observations show no signs of temporal variations characteristic of radio-wave flares. We suggest that this central component may be dominated by dust emission from an inner planetesimal belt of mass similar to 0.01 M-Moon, consistent with a lack of emission shortward of 25 mu m and a location less than or similar to 3 AU from the star. Future millimeter observations can test this assertion, as an inner dust belt should be readily separated from the central star at higher angular resolution. C1 [MacGregor, Meredith A.; Wilner, David J.; Rosenfeld, Katherine A.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matthews, Brenda; Booth, Mark] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Hughes, A. Meredith; Chiang, Eugene; Graham, James R.; Kalas, Paul] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Booth, Mark] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Graham, James R.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Kalas, Paul] SETI Inst, Mountain View, CA 94043 USA. [Kennedy, Grant] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, Bruce] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Booth, Mark/0000-0001-8568-6336; MacGregor, Meredith/0000-0001-7891-8143; Kennedy, Grant/0000-0001-6831-7547 FU NRAO; Miller Institute for Basic Research in Science; Canadian Space Agency; NSERC; NSF [AST-0909210, 0909188]; NASA [NNX11AD21G] FX M.A.M. thanks NRAO for Student Observing Support funds. A. M. H. is supported by a fellowship from the Miller Institute for Basic Research in Science. M. B. is funded through a Space Science Enhancement Program grant from the Canadian Space Agency and an NSERC Discovery Accelerator Supplement. E. C. acknowledges NSF grant AST-0909210. P. K. and J.R.G. acknowledge support from NSF Award 0909188 and NASA Award NNX11AD21G. This Letter makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00142.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 38 TC 21 Z9 21 U1 2 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2013 VL 762 IS 2 AR L21 DI 10.1088/2041-8205/762/2/L21 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237ND UT WOS:000325876300006 ER PT J AU Meijerink, R Kristensen, LE Weiss, A van der Werf, PP Walter, F Spaans, M Loenen, AF Fischer, J Israel, FP Isaak, K Papadopoulos, PP Aalto, S Armus, L Charmandaris, V Dasyra, KM Diaz-Santos, T Evans, A Gao, Y Gonzalez-Alfonso, E Gusten, R Henkel, C Kramer, C Lord, S Martin-Pintado, J Naylor, D Sanders, DB Smith, H Spinoglio, L Stacey, G Veilleux, S Wiedner, MC AF Meijerink, R. Kristensen, L. E. Weiss, A. van der Werf, P. P. Walter, F. Spaans, M. Loenen, A. F. Fischer, J. Israel, F. P. Isaak, K. Papadopoulos, P. P. Aalto, S. Armus, L. Charmandaris, V. Dasyra, K. M. Diaz-Santos, T. Evans, A. Gao, Y. Gonzalez-Alfonso, E. Guesten, R. Henkel, C. Kramer, C. Lord, S. Martin-Pintado, J. Naylor, D. Sanders, D. B. Smith, H. Spinoglio, L. Stacey, G. Veilleux, S. Wiedner, M. C. TI EVIDENCE FOR CO SHOCK EXCITATION IN NGC 6240 FROM HERSCHEL SPIRE SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (NGC 6240); galaxies: nuclei; galaxies: starburst; infrared: galaxies ID LUMINOUS INFRARED GALAXIES; MOLECULAR GAS; STAR-FORMATION; ARP 220; MARKARIAN 231; NGC-6240; DIAGNOSTICS; NUCLEI; DENSE; ENVIRONMENTS AB We present Herschel SPIRE FTS spectroscopy of the nearby luminous infrared galaxy NGC 6240. In total 20 lines are detected, including CO J = 4-3 through J = 13-12, 6 H2O rotational lines, and [C I] and [N II] fine-structure lines. The CO to continuum luminosity ratio is 10 times higher in NGC 6240 than Mrk 231. Although the CO ladders of NGC 6240 and Mrk 231 are very similar, UV and/or X-ray irradiation are unlikely to be responsible for the excitation of the gas in NGC 6240. We applied both C and J shock models to the H-2 v = 1-0 S(1) and v = 2-1 S(1) lines and the CO rotational ladder. The CO ladder is best reproduced by a model with shock velocity v(s) = 10 km s(-1) and a pre-shock density n(H) = 5 x 10(4) cm(-3). We find that the solution best fitting the H-2 lines is degenerate. The shock velocities and number densities range between v(s) = 17-47 km s(-1) and n(H) = 10(7)-5x10(4) cm(-3), respectively. The H-2 lines thus need a much more powerful shock than the CO lines. We deduce that most of the gas is currently moderately stirred up by slow (10 km s(-1)) shocks while only a small fraction (less than or similar to 1%) of the interstellar medium is exposed to the high-velocity shocks. This implies that the gas is rapidly losing its highly turbulent motions. We argue that a high CO line-to-continuum ratio is a key diagnostic for the presence of shocks. C1 [Meijerink, R.; Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Meijerink, R.; Kristensen, L. E.; van der Werf, P. P.; Loenen, A. F.; Israel, F. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Weiss, A.; Papadopoulos, P. P.; Guesten, R.; Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fischer, J.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Isaak, K.] Estec, ESA Astrophys Miss Div, NL-2200 AG Noordwijk, Netherlands. [Aalto, S.] Chalmers, Onsala Observ, Dept Radio & Space Sci, SE-43992 Onsala, Sweden. [Armus, L.; Diaz-Santos, T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Charmandaris, V.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Dasyra, K. M.] Observ Paris, LERMA CNRS UMR8112, F-75014 Paris, France. [Evans, A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Gao, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, E-28871 Madrid, Spain. [Henkel, C.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia. [Kramer, C.] IRAM, E-18012 Granada, Spain. [Lord, S.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Martin-Pintado, J.] CSIC, Inst Estruct Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. [Naylor, D.] Univ Lethbridge, Dept Phys & Astron, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Smith, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spinoglio, L.] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Stacey, G.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Wiedner, M. C.] Observ Paris, LERMA, CNRS, F-75014 Paris, France. RP Meijerink, R (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. RI Charmandaris, Vassilis/A-7196-2008; Kristensen, Lars/F-4774-2011; Martin-Pintado, Jesus/H-6107-2015; OI Charmandaris, Vassilis/0000-0002-2688-1956; Kristensen, Lars/0000-0003-1159-3721; Martin-Pintado, Jesus/0000-0003-4561-3508; Meijerink, Rowin/0000-0001-7584-9293; Dasyra, Kalliopi/0000-0002-1482-2203; Spinoglio, Luigi/0000-0001-8840-1551 FU CSA in Canada; NAOC in China; CNES in France; CNRS in France; CEA in France; ASI in Italy; MEC in Spain; Stockholm Observatory in Sweden; STFC in the UK; NASA in the USA; ESA; NHSC; US ONR FX We acknowledge the constructive comments by the referee Christine Wilson. The following institutes have provided hardware and software elements to the SPIRE project: University of Lethbridge, Canada; NAOC, Beijing, China; CEA Saclay, CEA Grenoble and LAM in France; IFSI, Rome, and University of Padua, Italy; IAC, Tenerife, Spain; Stockholm Observatory, Sweden; Cardiff University, Imperial College London, UCL-MSSL, STFCRAL, UK ATC Edinburgh, and the University of Sussex in the UK. Funding for SPIRE has been provided by the national agencies of the participating countries and by internal institute funding: CSA in Canada; NAOC in China; CNES, CNRS, and CEA in France; ASI in Italy; MEC in Spain; Stockholm Observatory in Sweden; STFC in the UK; and NASA in the USA. Additional funding support for some instrument activities has been provided by ESA. US authors acknowledge support from the NHSC. Basic research in IR astronomy at NRL is funded by the US ONR. NR 29 TC 47 Z9 47 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JAN 10 PY 2013 VL 762 IS 2 AR L16 DI 10.1088/2041-8205/762/2/L16 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237ND UT WOS:000325876300001 ER PT J AU Middleton, MJ Miller-Jones, JCA Markoff, S Fender, R Henze, M Hurley-Walker, N Scaife, AMM Roberts, TP Walton, D Carpenter, J Macquart, JP Bower, GC Gurwell, M Pietsch, W Haberl, F Harris, J Daniel, M Miah, J Done, C Morgan, JS Dickinson, H Charles, P Burwitz, V Della Valle, M Freyberg, M Greiner, J Hernanz, M Hartmann, DH Hatzidimitriou, D Riffeser, A Sala, G Seitz, S Reig, P Rau, A Orio, M Titterington, D Grainge, K AF Middleton, Matthew J. Miller-Jones, James C. A. Markoff, Sera Fender, Rob Henze, Martin Hurley-Walker, Natasha Scaife, Anna M. M. Roberts, Timothy P. Walton, Dominic Carpenter, John Macquart, Jean-Pierre Bower, Geoffrey C. Gurwell, Mark Pietsch, Wolfgang Haberl, Frank Harris, Jonathan Daniel, Michael Miah, Junayd Done, Chris Morgan, John S. Dickinson, Hugh Charles, Phil Burwitz, Vadim Della Valle, Massimo Freyberg, Michael Greiner, Jochen Hernanz, Margarita Hartmann, Dieter H. Hatzidimitriou, Despina Riffeser, Arno Sala, Gloria Seitz, Stella Reig, Pablo Rau, Arne Orio, Marina Titterington, David Grainge, Keith TI Bright radio emission from an ultraluminous stellar-mass microquasar in M 31 SO NATURE LA English DT Article ID X-RAY SOURCE; BLACK-HOLE BINARIES; SUPERLUMINAL SOURCE; GRS 1915+105; J1819.3-2525; EVOLUTION; SYSTEMS; CHANDRA; GALAXY; MODEL AB A subset of ultraluminous X-ray sources (those with luminosities of less than 10(40) erg s(-1); ref. 1) are thought to be powered by the accretion of gas onto black holes with masses of similar to 5-20M(circle dot), probably by means of an accretion disk(2,3). The X-ray and radio emission are coupled in such Galactic sources; the radio emission originates in a relativistic jet thought to be launched from the innermost regions near the black hole(4,5), with the most powerful emission occurring when the rate of infalling matter approaches a theoretical maximum (the Eddington limit). Only four such maximal sources are known in the Milky Way(6), and the absorption of soft X-rays in the interstellar medium hinders the determination of the causal sequence of events that leads to the ejection of the jet. Here we report radio and X-ray observations of a bright new X-ray source in the nearby galaxy M 31, whose peak luminosity exceeded 10(39) erg s(-1). The radio luminosity is extremely high and shows variability on a timescale of tens of minutes, arguing that the source is highly compact and powered by accretion close to the Eddington limit onto a black hole of stellar mass. Continued radio and X-ray monitoring of such sources should reveal the causal relationship between the accretion flow and the powerful jet emission. C1 [Middleton, Matthew J.; Roberts, Timothy P.; Harris, Jonathan; Daniel, Michael; Miah, Junayd; Done, Chris] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Middleton, Matthew J.; Markoff, Sera] Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Miller-Jones, James C. A.; Hurley-Walker, Natasha; Macquart, Jean-Pierre; Morgan, John S.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Fender, Rob; Scaife, Anna M. M.; Charles, Phil] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Henze, Martin; Pietsch, Wolfgang; Haberl, Frank; Burwitz, Vadim; Freyberg, Michael; Greiner, Jochen; Rau, Arne] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Walton, Dominic] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Walton, Dominic; Carpenter, John] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Macquart, Jean-Pierre] Curtin Univ Technol, ARC Ctr Excellence All Sky Astrophys CAASTRO, Perth, WA 6845, Australia. [Bower, Geoffrey C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dickinson, Hugh] Stockholm Univ, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Charles, Phil] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Della Valle, Massimo] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Della Valle, Massimo] Int Ctr Relativist Astrophys, I-65122 Pescara, Italy. [Hernanz, Margarita] Fac Ciencies, Inst Space Sci CSIC IEEC, Barcelona 08193, Spain. [Hartmann, Dieter H.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29631 USA. [Hatzidimitriou, Despina] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, Athens 15784, Greece. [Riffeser, Arno; Seitz, Stella] Univ Munich, Univ Observ Munich, D-81679 Munich, Germany. [Sala, Gloria] EUETIB UPC IEEC, Dept Phys & Nucl Engn, Barcelona 08036, Spain. [Reig, Pablo] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. [Orio, Marina] Osserv Astron Padova, I-35122 Padua, Italy. [Titterington, David; Grainge, Keith] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. RP Middleton, MJ (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England. EM m.j.middleton@durham.ac.uk RI Daniel, Michael/A-2903-2010; Miller-Jones, James/B-2411-2013; Macquart, Jean-Pierre/B-5306-2013; Hurley-Walker, Natasha/B-9520-2013; Morgan, John/B-9505-2013; Reig, Pablo/A-1198-2014; Hernanz, Margarita/K-1770-2014; Hatzidimitriou, Despina/A-3732-2015; done, chris/D-4605-2016 OI Della Valle, Massimo/0000-0003-3142-5020; Haberl, Frank/0000-0002-0107-5237; Henze, Martin/0000-0001-9985-3406; Daniel, Michael/0000-0002-8053-7910; Miller-Jones, James/0000-0003-3124-2814; Hurley-Walker, Natasha/0000-0002-5119-4808; Reig, Pablo/0000-0002-6446-3050; Hernanz, Margarita/0000-0002-8651-7910; done, chris/0000-0002-1065-7239 FU Science and Technology Facilities Council (STFC); Netherlands Organization for Scientific Research Vidi Fellowship; European Research Council; Cambridge University; STFC; [BMWI/DLR]; [FKZ 50 OR 1010] FX We thank C. Trott and R. Soria for discussions, and C. Gough for making his code available. This work was supported by a Science and Technology Facilities Council (STFC) standard grant (M.J.M.), Netherlands Organization for Scientific Research Vidi Fellowship (S. M.), European Research Council partial funding (R. F.) and grant number BMWI/DLR, FKZ 50 OR 1010 (M. Henze). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank the staff of the Mullard Radio Astronomy Observatory for their assistance in the commissioning and operation of AMI, which is supported by Cambridge University and the STFC. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data obtained from NASA's Swift and Chandra satellites. NR 30 TC 58 Z9 58 U1 0 U2 21 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 10 PY 2013 VL 493 IS 7431 BP 187 EP 190 DI 10.1038/nature11697 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 066YY UT WOS:000313259600032 PM 23235823 ER PT J AU Casassus, S van der Plas, G Perez, MS Dent, WRF Fomalont, E Hagelberg, J Hales, A Jordan, A Mawet, D Menard, F Wootten, A Wilner, D Hughes, AM Schreiber, MR Girard, JH Ercolano, B Canovas, H Roman, PE Salinas, V AF Casassus, Simon van der Plas, Gerrit Sebastian Perez, M. Dent, William R. F. Fomalont, Ed Hagelberg, Janis Hales, Antonio Jordan, Andres Mawet, Dimitri Menard, Francois Wootten, Al Wilner, David Hughes, A. Meredith Schreiber, Matthias R. Girard, Julien H. Ercolano, Barbara Canovas, Hector Roman, Pablo E. Salinas, Vachail TI Flows of gas through a protoplanetary gap SO NATURE LA English DT Article ID DISK SURROUNDING HD-142527; CO FUNDAMENTAL EMISSION; HERBIG AE/BE STARS; T-TAURI; TRANSITIONAL DISKS; PLANET FORMATION; MOLECULAR GAS; AE STARS; SPECTROSCOPY; ACCRETION AB The formation of gaseous giant planets is thought to occur in the first few million years after stellar birth. Models(1) predict that the process produces a deep gap in the dust component (shallower in the gas(2-4)). Infrared observations of the disk around the young star HD 142527 (at a distance of about 140 parsecs from Earth) found an inner disk about 10 astronomical units (AU) in radius(5) (1 AU is the Earth-Sun distance), surrounded by a particularly large gap(6) and a disrupted(7) outer disk beyond 140 AU. This disruption is indicative of a perturbing planetary-mass body at about 90 AU. Radio observations(8,9) indicate that the bulk mass is molecular and lies in the outer disk, whose continuum emission has a horseshoe morphology(8). The high stellar accretion rate(10) would deplete the inner disk(11) in less than one year, and to sustain the observed accretion matter must therefore flow from the outer disk and cross the gap. In dynamical models, the putative protoplanets channel outer-disk material into gap-crossing bridges that feed stellar accretion through the inner disk(12). Here we report observations of diffuse CO gas inside the gap, with denser HCO+ gas along gap-crossing filaments. The estimated flow rate of the gas is in the range of 7 x 10(-9) to 2 x 10(-7) solar masses per year, which is sufficient to maintain accretion onto the star at the present rate. C1 [Casassus, Simon; van der Plas, Gerrit; Sebastian Perez, M.; Menard, Francois; Salinas, Vachail] Univ Chile, Dept Astron, Santiago, Chile. [Dent, William R. F.; Hales, Antonio] Joint ALMA Observ, Santiago 7630355, Chile. [Dent, William R. F.; Mawet, Dimitri; Girard, Julien H.] European So Observ, Santiago 19, Chile. [Fomalont, Ed; Hales, Antonio; Wootten, Al] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Hagelberg, Janis] Univ Geneva, Observ Geneve, CH-1290 Versoix, Switzerland. [Jordan, Andres] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Menard, Francois] CNRS INSU France UMI 3386, UMI FCA, Grenoble, France. [Menard, Francois] UJF Grenoble 1, CNRS, UMR 5274, IPAG, F-48041 Grenoble 9, France. [Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. Meredith] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Schreiber, Matthias R.; Canovas, Hector] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile. [Ercolano, Barbara] Univ Munich, Univ Observ, D-81679 Munich, Germany. [Roman, Pablo E.] Univ Chile, Ctr Math Modeling, Santiago, Chile. RP Casassus, S (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM scasassus@u.uchile.cl RI Roman, Pablo/G-1960-2011; Casassus, Simon/I-8609-2016; OI Roman, Pablo/0000-0002-7105-9371; Hagelberg, Janis/0000-0002-1096-1433; Canovas, Hector/0000-0001-7668-8022; Jordan, Andres/0000-0002-5389-3944; Girard, Julien/0000-0001-8627-0404; van der Plas, Gerrit/0000-0001-5688-187X FU Millennium Nucleus [P10-022-F]; European Union [FONDECYT 1100221, 284405] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00465. S. ALMA is a partnership of the ESO, NSF, NINS, NRC, NSC and ASIAA. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO and NAOJ. This work was also based on observations obtained at the Gemini Observatory. Financial support was provided by Millennium Nucleus P10-022-F (Chilean Ministry of Economy) and additionally by grant FONDECYT 1100221 and grant 284405 from the European Union FP7 programme. NR 30 TC 148 Z9 148 U1 1 U2 25 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 10 PY 2013 VL 493 IS 7431 BP 191 EP 194 DI 10.1038/nature11769 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 066YY UT WOS:000313259600033 PM 23283173 ER PT J AU Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Buckley, JH Bugaev, V Cesarini, A Ciupik, L Connolly, MP Cui, W Dickherber, R Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Humensky, TB Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Maier, G Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Park, N Perkins, JS Pichel, A Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Saxon, DB Schroedter, M Sembroski, GH Staszak, D Telezhinsky, I Tesic, G Theiling, M Tsurusaki, K Varlotta, A Vincent, S Wakely, SP Weekes, TC Weinstein, A Welsing, R Williams, DA Zitzer, B Jorstad, SG MacDonald, NR Marscher, AP Smith, PS Walker, RC Hovatta, T Richards, J Max-Moerbeck, W Readhead, A Lister, ML Kovalev, YY Pushkarev, AB Gurwell, MA Lahteenmaki, A Nieppola, E Tornikoski, M Jarvela, E AF Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Buckley, J. H. Bugaev, V. Cesarini, A. Ciupik, L. Connolly, M. P. Cui, W. Dickherber, R. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Maier, G. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Saxon, D. B. Schroedter, M. Sembroski, G. H. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Tsurusaki, K. Varlotta, A. Vincent, S. Wakely, S. P. Weekes, T. C. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Jorstad, S. G. MacDonald, N. R. Marscher, A. P. Smith, P. S. Walker, R. C. Hovatta, T. Richards, J. Max-Moerbeck, W. Readhead, A. Lister, M. L. Kovalev, Y. Y. Pushkarev, A. B. Gurwell, M. A. Lahteenmaki, A. Nieppola, E. Tornikoski, M. Jarvela, E. CA VERITAS Collaboration TI RAPID TeV GAMMA-RAY FLARING OF BL LACERTAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (BL Lacertae, VER J2202+422); gamma rays: galaxies ID ACTIVE GALACTIC NUCLEI; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; POLARIMETRIC OBSERVATIONS; RELATIVISTIC JETS; HIGH-FREQUENCIES; RADIO-SOURCES; PKS 1222+216; BLAZARS; VARIABILITY AB We report on the detection of a very rapid TeV gamma-ray flare from BL Lacertae on 2011 June 28 with the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The flaring activity was observed during a 34.6 minute exposure, when the integral flux above 200 GeV reached (3.4 +/- 0.6) x 10(-6) photons m(-2) s(-1), roughly 125% of the Crab Nebula flux measured by VERITAS. The light curve indicates that the observations missed the rising phase of the flare but covered a significant portion of the decaying phase. The exponential decay time was determined to be 13 +/- 4 minutes, making it one of the most rapid gamma-ray flares seen from a TeV blazar. The gamma-ray spectrum of BL Lacertae during the flare was soft, with a photon index of 3.6 +/- 0.4, which is in agreement with the measurement made previously by MAGIC in a lower flaring state. Contemporaneous radio observations of the source with the Very Long Baseline Array revealed the emergence of a new, superluminal component from the core around the time of the TeV gamma-ray flare, accompanied by changes in the optical polarization angle. Changes in flux also appear to have occurred at optical, UV, and GeV gamma-ray wavelengths at the time of the flare, although they are difficult to quantify precisely due to sparse coverage. A strong flare was seen at radio wavelengths roughly four months later, which might be related to the gamma-ray flaring activities. We discuss the implications of these multiwavelength results. C1 [Arlen, T.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Cesarini, A.; Connolly, M. P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Errando, M.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Federici, S.; Maier, G.; Pohl, M.; Prokoph, H.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Griffin, S.; Hanna, D.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Krennrich, F.; Orr, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Park, N.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Jorstad, S. G.; MacDonald, N. R.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, S. G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85716 USA. [Walker, R. C.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hovatta, T.; Max-Moerbeck, W.; Readhead, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kovalev, Y. Y.] Russian Acad Sci, Astro Space Ctr Lebedev Phys Inst, Moscow, Russia. [Kovalev, Y. Y.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. [Pushkarev, A. B.] Pulkovo Astron Observ, St Petersburg 196140, Russia. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Ukraine. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lahteenmaki, A.; Nieppola, E.; Tornikoski, M.; Jarvela, E.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. RP Arlen, T (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM cui@purdue.edu; qfeng@purdue.edu RI Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Khassen, Yerbol/I-3806-2015; Jorstad, Svetlana/H-6913-2013; Pushkarev, Alexander/M-9997-2015; OI Kovalev, Yuri/0000-0001-9303-3263; Khassen, Yerbol/0000-0002-7296-3100; Jorstad, Svetlana/0000-0001-9522-5453; Smith, Paul/0000-0002-5083-3663; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Errando, Manel/0000-0002-1853-863X FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; NASA [NNX08AV65G, NNX08AV61G, NNX09AT99G, NNX11AQ03G, NNX08AW31G, NNX11A043G, NNX08AV67G]; NSF [AST-0907893, AST-0808050, AST-1109911]; Russian Foundation for Basic Research [11-02-00368, 12-02-33101]; Physical Sciences Division of the Russian Academy of Sciences; Dynasty Foundation; Academia Sinica; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G]; Academy of Finland [212656, 210338, 121148] FX Q.F. and W.C. thank Dimitrios Giannios for useful comments on the manuscript. The work of the VERITAS Collaboration was supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; The Boston University effort was supported in part by NASA through Fermi grants NNX08AV65G, NNX08AV61G, NNX09AT99G, and NNX11AQ03G, and by NSF grant AST-0907893.; The OVRO 40 m monitoring program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911.; The MOJAVE project is supported under NASA-Fermi grant NNX08AV67G. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Y.Y.K. and K. V. S. were partly supported by the Russian Foundation for Basic Research (project 11-02-00368, 12-02-33101) and the basic research program "Active processes in galactic and extragalactic objects" of the Physical Sciences Division of the Russian Academy of Sciences. Y.Y.K. was supported by the Dynasty Foundation.; The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.; The Steward Observatory spectropolarimetric monitoring project is supported by Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G.; The Metsahovi team acknowledges the support from the Academy of Finland to observing projects (numbers 212656, 210338, 121148, and others). NR 72 TC 29 Z9 29 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 92 DI 10.1088/0004-637X/762/2/92 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900026 ER PT J AU King, AL Miller, JM Raymond, J Fabian, AC Reynolds, CS Gultekin, K Cackett, EM Allen, SW Proga, D Kallman, TR AF King, A. L. Miller, J. M. Raymond, J. Fabian, A. C. Reynolds, C. S. Gueltekin, K. Cackett, E. M. Allen, S. W. Proga, D. Kallman, T. R. TI REGULATION OF BLACK HOLE WINDS AND JETS ACROSS THE MASS SCALE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: jets ID ACTIVE GALACTIC NUCLEI; QUASAR OUTFLOW CONTRIBUTION; GALAXY IRAS 18325-5926; ACCRETION DISK WIND; X-RAY ABSORBERS; GRO J1655-40; XMM-NEWTON; WARM ABSORBERS; AGN FEEDBACK; MICROQUASAR H1743-322 AB We present a study of the mechanical power generated by both winds and jets across the black hole mass scale. We begin with the study of ionized X-ray winds and present a uniform analysis using Chandra grating spectra. The high-quality grating spectra facilitate the characterization of the outflow velocity, ionization, and column density of the absorbing gas. We find that the kinetic power of the winds, derived from these observed quantities, scales with increasing bolometric luminosity as log(L-wind,L-42/C-v) = (1.58 +/- 0.07) log(L-Bol,L-42) - (3.19 +/- 0.19). This suggests that supermassive black holes may be more efficient than stellar-mass black holes in launching winds, per unit filling factor, C-v. If the black hole binary (BHB) and active galactic nucleus (AGN) samples are fit individually, the slopes flatten to alpha(BHB) = 0.91 +/- 0.31 and alpha(AGN) = 0.63 +/- 0.30 (formally consistent within errors). The broad fit and individual fits both characterize the data fairly well, and the possibility of common slopes may point to common driving mechanisms across the mass scale. For comparison, we examine jet production, estimating jet power based on the energy required to inflate local bubbles. The jet relation is log(L-Jet,L-42) = (1.18 +/- 0.24) log(L-Bondi,L-42) - (0.96 +/- 0.43). The energetics of the bubble associated with Cygnus X-1 are particularly difficult to determine, and the bubble could be a background supernova remnant. If we exclude Cygnus X-1 from our fits, then the jets follow a relation consistent with the winds, but with a higher intercept, log(L-Jet,L-42) = (1.34 +/- 0.50) log(L-Bondi,L-42) - (0.80 +/- 0.82). The formal consistency in the wind and jet scaling relations, when assuming that L-Bol and L-Bondi are both proxies for mass accretion rate, suggests that a common launching mechanism may drive both flows; magnetic processes, such as magnetohydrodynamics and magnetocentrifugal forces, are viable possibilities. We also examine winds that are moving at especially high velocities, v > 0.01c. These ultra-fast outflows tend to resemble the jets more than the winds in terms of outflow power, indicating that we may be observing a regime in which winds become jets. A transition at approximately L-Bol approximate to 10(-2) L-Edd is apparent when outflow power is plotted versus Eddington fraction. At low Eddington fractions, the jet power is dominant, and at high Eddington fractions, the wind power is dominant. This study allows for the total power from black hole accretion, both mechanical and radiative, to be characterized in a simple manner and suggests possible connections between winds and jets. X-ray wind data and jet cavity data will enable stronger tests. C1 [King, A. L.; Miller, J. M.; Gueltekin, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Raymond, J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Fabian, A. C.; Cackett, E. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48120 USA. [Allen, S. W.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophysiccs & Cosmol, Stanford, CA 94305 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Proga, D.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. [Proga, D.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP King, AL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ashking@umich.edu OI Gultekin, Kayhan/0000-0002-1146-0198 FU NASA through the NESSF program; NASA FX The authors thank the anonymous referee for their invaluable comments to improve this paper. A. L. K. acknowledges support from NASA through the NESSF program. J.M.M. thanks NASA for support through its guest observer programs. NR 106 TC 41 Z9 41 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 103 DI 10.1088/0004-637X/762/2/103 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900037 ER PT J AU Liu, T Xue, L Gu, WM Lu, JF AF Liu, Tong Xue, Li Gu, Wei-Min Lu, Ju-Fu TI THE VERTICAL COMPOSITION OF NEUTRINO-DOMINATED ACCRETION DISKS IN GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; gamma-ray burst: general; nuclear reactions, nucleosynthesis, abundances ID ENERGY COSMIC-RAYS; BLACK-HOLES; SUPERNOVA EXPLOSIONS; JET PRECESSION; NUCLEOSYNTHESIS; OUTFLOWS; DRIVEN; FLOWS; LINES; SIMULATIONS AB We investigate the vertical structure and element distribution of neutrino-dominated accretion flows around black holes in spherical coordinates using the reasonable nuclear statistical equilibrium. According to our calculations, heavy nuclei tend to be produced in a thin region near the disk surface, whose mass fractions are primarily determined by the accretion rate and vertical distribution of temperature and density. In this thin region, we find that Ni-56 is dominant for the flow with a low accretion rate (e. g., 0.05 M-circle dot s(-1)), but Fe-56 is dominant for the flow with a high accretion rate (e. g., 1 M-circle dot s(-1)). The dominant Ni-56 in the aforementioned region may provide a clue to understanding the bumps in the optical light curve of core-collapse supernovae. C1 [Liu, Tong; Xue, Li; Gu, Wei-Min; Lu, Ju-Fu] Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China. [Liu, Tong; Xue, Li; Gu, Wei-Min; Lu, Ju-Fu] Xiamen Univ, Inst Theoret Phys & Astrophys, Xiamen 361005, Fujian, Peoples R China. [Xue, Li] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Gu, Wei-Min] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, T (reprint author), Xiamen Univ, Dept Phys, Xiamen 361005, Fujian, Peoples R China. EM tongliu@xmu.edu.cn RI Gu, WM/G-3984-2010 FU National Basic Research Program (973 Program) of China [2009CB824800]; National Natural Science Foundation of China [10833002, 11003016, 11073015, 11103015, 11222328, 11233006]; Natural Science Foundation of Fujian Province of China [2010J01017] FX We thank the anonymous referee for a careful and constructive review and Xue-Feng Wu and Shu-Jin Hou for beneficial discussion. T. L. thanks Ang Li for the invitation to visit RIKEN. This work was supported by the National Basic Research Program (973 Program) of China under grant 2009CB824800, the National Natural Science Foundation of China under grants 10833002, 11003016, 11073015, 11103015, 11222328, and 11233006, and the Natural Science Foundation of Fujian Province of China under grant 2010J01017. NR 46 TC 15 Z9 15 U1 0 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 102 DI 10.1088/0004-637X/762/2/102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900036 ER PT J AU Liu, X Civano, F Shen, Y Green, P Greene, JE Strauss, MA AF Liu, Xin Civano, Francesca Shen, Yue Green, Paul Greene, Jenny E. Strauss, Michael A. TI CHANDRA X-RAY AND HUBBLE SPACE TELESCOPE IMAGING OF OPTICALLY SELECTED KILOPARSEC-SCALE BINARY ACTIVE GALACTIC NUCLEI. I. NATURE OF THE NUCLEAR IONIZING SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: Seyfert; quasars: general; X-rays: galaxies ID DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES; NARROW-LINE REGION; SEYFERT 2 GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE INDICATOR; INITIAL MASS FUNCTION; STAR-FORMATION RATES; SIMILAR-TO 3-4 AB Kiloparsec-scale binary active galactic nuclei (AGNs) signal active supermassive black hole (SMBH) pairs in merging galaxies. Despite their significance, unambiguously confirmed cases remain scarce and most have been discovered serendipitously. In a previous systematic search, we optically identified four kpc-scale binary AGNs from candidates selected with double-peaked narrow emission lines at z = 0.1-0.2. Here, we present Chandra and Hubble Space Telescope Wide Field Camera 3 (WFC3) imaging of these four systems. We critically examine and confirm the binary-AGN scenario for two of the four targets, by combining high angular resolution X-ray imaging spectroscopy with Chandra ACIS-S, better nuclear position constraints from WFC3 F105W imaging, and direct starburst estimates from WFC3 F336W imaging; for the other two targets, the existing data are still consistent with the binary-AGN scenario, but we cannot rule out the possibility of only one AGN ionizing gas in both merging galaxies. We find tentative evidence for a systematically smaller X-ray-to-[O III] luminosity ratio and/or higher Compton-thick fraction in optically selected kpc-scale binary AGNs than in single AGNs, possibly caused by a higher nuclear gas column due to mergers and/or a viewing angle bias related to the double-peak narrow-line selection. While our result lends some further support to the general approach of optically identifying kpc-scale binary AGNs, it also highlights the challenge and ambiguity of X-ray confirmation. C1 [Liu, Xin; Civano, Francesca; Shen, Yue; Green, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Greene, Jenny E.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS 5-26555]; [GO 12363] FX Based, in part, on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program number GO 12363. NR 174 TC 32 Z9 32 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 110 DI 10.1088/0004-637X/762/2/110 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900044 ER PT J AU Palau, A Fuente, A Girart, JM Estalella, R Ho, PTP Sanchez-Monge, A Fontani, F Busquet, G Commercon, B Hennebelle, P Boissier, J Zhang, QZ Cesaroni, R Zapata, LA AF Palau, Aina Fuente, Asuncion Girart, Josep M. Estalella, Robert Ho, Paul T. P. Sanchez-Monge, Alvaro Fontani, Francesco Busquet, Gemma Commercon, Benoit Hennebelle, Patrick Boissier, Jeremie Zhang, Qizhou Cesaroni, Riccardo Zapata, Luis A. TI EARLY STAGES OF CLUSTER FORMATION: FRAGMENTATION OF MASSIVE DENSE CORES DOWN TO less than or similar to 1000 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (IRAS 22172+5549, IRAS 22134+5834; IRAS 22198+6336, AFGL5142); radio continuum: ISM; stars: formation ID STAR-FORMING REGION; FAR-INFRARED OBSERVATIONS; ADAPTIVE MESH REFINEMENT; MOLECULAR CLOUD CORES; HERBIG AE/BE STARS; 1333 IRAS 4A; INTERMEDIATE-MASS; MAGNETIC-FIELDS; HIGH-RESOLUTION; GRAVOTURBULENT FRAGMENTATION AB In order to study the fragmentation of massive dense cores, which constitute the cluster cradles, we observed the continuum at 1.3 mm and the CO (2-1) emission of four massive cores with the Plateau de Bure Interferometer in the most extended configuration. We detected dust condensations down to similar to 0.3 M-circle dot and separate millimeter sources down to 0.'' 4 or less than or similar to 1000 AU, comparable to the sensitivities and separations reached in optical/infrared studies of clusters. The CO (2-1) high angular resolution images reveal high-velocity knots usually aligned with previously known outflow directions. This, in combination with additional cores from the literature observed at similar mass sensitivity and spatial resolution, allowed us to build a sample of 18 protoclusters with luminosities spanning three orders of magnitude. Among the 18 regions, similar to 30% show no signs of fragmentation, while 50% split up into greater than or similar to 4 millimeter sources. We compiled a list of properties for the 18 massive dense cores, such as bolometric luminosity, total mass, and mean density, and found no correlation of any of these parameters with the fragmentation level. In order to investigate the combined effects of the magnetic field, radiative feedback, and turbulence in the fragmentation process, we compared our observations to radiation magnetohydrodynamic simulations and found that the low-fragmented regions are reproduced well in the magnetized core case, while the highly fragmented regions are consistent with cores where turbulence dominates over the magnetic field. Overall, our study suggests that the fragmentation in massive dense cores could be determined by the initial magnetic field/turbulence balance in each particular core. C1 [Palau, Aina; Girart, Josep M.] Inst Ciencies Espai CSIC IEEC, Fac Ciencias, E-08193 Bellaterra, Catalunya, Spain. [Fuente, Asuncion] Observ Astron Nacl, E-28803 Madrid, Spain. [Estalella, Robert] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol IEEC UB, E-08028 Barcelona, Spain. [Ho, Paul T. P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Busquet, Gemma] INAF Ist Astrofis & Planetol Spaziali, Area Recerca Tor Vergata, I-00133 Rome, Italy. [Commercon, Benoit; Hennebelle, Patrick] Ecole Normale Super, UMR CNRS 8112, Lab Radioastron, F-75231 Paris 05, France. [Boissier, Jeremie] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Boissier, Jeremie] ESO, D-85748 Garching Muenchen, Germany. [Zapata, Luis A.] Univ Nacl Autonoma Mexico, Centro Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Commercon, Benoit; Hennebelle, Patrick] Observ Paris, F-75231 Paris 05, France. [Sanchez-Monge, Alvaro; Fontani, Francesco; Cesaroni, Riccardo] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Palau, A (reprint author), Inst Ciencies Espai CSIC IEEC, Fac Ciencias, Campus UAB,Torre C5 Parell 2, E-08193 Bellaterra, Catalunya, Spain. EM palau@ieec.uab.es RI Girart, Josep/O-1638-2014; Fuente, Asuncion/G-1468-2016; OI Girart, Josep/0000-0002-3829-5591; Fuente, Asuncion/0000-0001-6317-6343; Zhang, Qizhou/0000-0003-2384-6589 FU INSU/CNRS (France); MPG (Germany); IGN (Spain) FX Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 128 TC 29 Z9 29 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 120 DI 10.1088/0004-637X/762/2/120 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900054 ER PT J AU Steiner, JF McClintock, JE Narayan, R AF Steiner, James F. McClintock, Jeffrey E. Narayan, Ramesh TI JET POWER AND BLACK HOLE SPIN: TESTING AN EMPIRICAL RELATIONSHIP AND USING IT TO PREDICT THE SPINS OF SIX BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; stars: winds, outflows; X-rays: binaries ID X-RAY TRANSIENT; NOVA-MUSCAE 1991; MICROQUASAR XTE J1550-564; RXTE SPECTRAL OBSERVATIONS; GRO J1655-40; RELATIVISTIC JETS; MASS-DISTRIBUTION; GX 339-4; INFRARED PHOTOMETRY; LOW/HARD STATE AB Using 5 GHz radio luminosity at light-curve maximum as a proxy for jet power and black hole spin measurements obtained via the continuum-fitting method, Narayan & McClintock presented the first direct evidence for a relationship between jet power and black hole spin for four transient black hole binaries. We test and confirm their empirical relationship using a fifth source, H1743-322, whose spin was recently measured. We show that this relationship is consistent with Fe-line spin measurements provided that the black hole spin axis is assumed to be aligned with the binary angular momentum axis. We also show that, during a major outburst of a black hole transient, the system reasonably approximates an X-ray standard candle. We further show, using the standard synchrotron bubble model, that the radio luminosity at light-curve maximum is a good proxy for jet kinetic energy. Thus, the observed tight correlation between radio power and black hole spin indicates a strong underlying link between mechanical jet power and black hole spin. Using the fitted correlation between radio power and spin for the above five calibration sources, we predict the spins of six other black holes in X-ray/radio transient systems with low-mass companions. Remarkably, these predicted spins are all relatively low, especially when compared to the high measured spins of black holes in persistent, wind-fed systems with massive companions. C1 [Steiner, James F.] Univ Cambridge, Dept Astron, Cambridge CB3 0HA, England. [Steiner, James F.; McClintock, Jeffrey E.; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steiner, JF (reprint author), Univ Cambridge, Dept Astron, Madingley Rd, Cambridge CB3 0HA, England. EM jsteiner@ast.cam.ac.uk OI Narayan, Ramesh/0000-0002-1919-2730 FU Smithsonian Institution Endowment Funds; NASA Hubble Fellowship [HST-HF-51315.01]; NASA [NNX11AD08G, NNX11AE16G] FX J.F.S. was supported by the Smithsonian Institution Endowment Funds and NASA Hubble Fellowship grant HST-HF-51315.01. J.E.M. acknowledges support from NASA grant NNX11AD08G, and R.N. acknowledges support from NASA grant NNX11AE16G. We thank Robert Dunn for input on his work, Rubens Reis, Chris Done, and Tom Maccarone for constructive discussions, and appreciate feedback on this manuscript from Laura Brenneman and Andy Fabian. We are grateful to Pawan Kumar for helpful discussions on jet emission. NR 92 TC 52 Z9 52 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 2013 VL 762 IS 2 AR 104 DI 10.1088/0004-637X/762/2/104 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 063OH UT WOS:000313008900038 ER PT J AU Kayal, E Roure, B Philippe, H Collins, AG Lavrov, DV AF Kayal, Ehsan Roure, Beatrice Philippe, Herve Collins, Allen G. Lavrov, Dennis V. TI Cnidarian phylogenetic relationships as revealed by mitogenomics SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Cnidaria; Medusozoa; Acraspeda; Anthozoa; mito-phylogenomics ID 18S RDNA SEQUENCES; GROUP-I INTRON; MITOCHONDRIAL GENOME; PHYLUM-CNIDARIA; MOLECULAR PHYLOGENETICS; SCLERACTINIA CONTAINS; SARCOPHYTON-GLAUCUM; HYDROZOA CNIDARIA; ANIMAL EVOLUTION; CLASS ANTHOZOA AB Background: Cnidaria (corals, sea anemones, hydroids, jellyfish) is a phylum of relatively simple aquatic animals characterized by the presence of the cnidocyst: a cell containing a giant capsular organelle with an eversible tubule (cnida). Species within Cnidaria have life cycles that involve one or both of the two distinct body forms, a typically benthic polyp, which may or may not be colonial, and a typically pelagic mostly solitary medusa. The currently accepted taxonomic scheme subdivides Cnidaria into two main assemblages: Anthozoa (Hexacorallia + Octocorallia) -cnidarians with a reproductive polyp and the absence of a medusa stage -and Medusozoa (Cubozoa, Hydrozoa, Scyphozoa, Staurozoa) -cnidarians that usually possess a reproductive medusa stage. Hypothesized relationships among these taxa greatly impact interpretations of cnidarian character evolution. Results: We expanded the sampling of cnidarian mitochondrial genomes, particularly from Medusozoa, to reevaluate phylogenetic relationships within Cnidaria. Our phylogenetic analyses based on a mitochogenomic dataset support many prior hypotheses, including monophyly of Hexacorallia, Octocorallia, Medusozoa, Cubozoa, Staurozoa, Hydrozoa, Carybdeida, Chirodropida, and Hydroidolina, but reject the monophyly of Anthozoa, indicating that the Octocorallia + Medusozoa relationship is not the result of sampling bias, as proposed earlier. Further, our analyses contradict Scyphozoa [Discomedusae + Coronatae], Acraspeda [Cubozoa + Scyphozoa], as well as the hypothesis that Staurozoa is the sister group to all the other medusozoans. Conclusions: Cnidarian mitochondrial genomic data contain phylogenetic signal informative for understanding the evolutionary history of this phylum. Mitogenome-based phylogenies, which reject the monophyly of Anthozoa, provide further evidence for the polyp-first hypothesis. By rejecting the traditional Acraspeda and Scyphozoa hypotheses, these analyses suggest that the shared morphological characters in these groups are plesiomorphies, originated in the branch leading to Medusozoa. The expansion of mitogenomic data along with improvements in phylogenetic inference methods and use of additional nuclear markers will further enhance our understanding of the phylogenetic relationships and character evolution within Cnidaria. C1 [Kayal, Ehsan; Lavrov, Dennis V.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. [Kayal, Ehsan] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Roure, Beatrice; Philippe, Herve] Univ Montreal, Fac Med, Dept Biochim, Montreal, PQ H3C 3J7, Canada. [Collins, Allen G.] Smithsonian Inst, Natl Systemat Lab, NOAAs Fisheries Serv, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kayal, E (reprint author), Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. EM kayale@si.edu OI Lavrov, Dennis/0000-0002-2745-1704 FU National Science Foundation [DEB-0829783]; Iowa State University; Smithsonian Predoctoral Fellow grant; NSF [EF-0531779] FX We would like to thank Matthew Palen for his wonderful drawings of cnidarians. We would also like to thank Niamh Redmond and Henner Brinkmann for their highly insightful comments on this manuscript. We also want to thank Omar Rota Stabelli, Corrinne Grover and Emmanuel Szadkowski for their help with the construction of the nucleotide alignments and analyses. This work was supported by a grant from the National Science Foundation to DVL [DEB-0829783] and by funding from Iowa State University. EK wishes to acknowledge funding through the Smithsonian Predoctoral Fellow grant. Some samples used in this study came from work supported by the NSF-funded Cnidarian Tree of Life Project (EF-0531779 to P. Cartwright, D. Fautin and AGC). NR 100 TC 53 Z9 56 U1 5 U2 136 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JAN 9 PY 2013 VL 13 AR 5 DI 10.1186/1471-2148-13-5 PG 18 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 102CO UT WOS:000315821200001 PM 23302374 ER PT J AU Costello, MJ Bouchet, P Boxshall, G Fauchald, K Gordon, D Hoeksema, BW Poore, GCB van Soest, RWM Stohr, S Walter, TC Vanhoorne, B Decock, W Appeltans, W AF Costello, Mark J. Bouchet, Philippe Boxshall, Geoff Fauchald, Kristian Gordon, Dennis Hoeksema, Bert W. Poore, Gary C. B. van Soest, Rob W. M. Stohr, Sabine Walter, T. Chad Vanhoorne, Bart Decock, Wim Appeltans, Ward TI Global Coordination and Standardisation in Marine Biodiversity through the World Register of Marine Species (WoRMS) and Related Databases SO PLOS ONE LA English DT Article ID CLIMATE-CHANGE; SEED PLANTS; DEEP-SEA; INFORMATION; TAXONOMY; COLLECTIONS; DIVERSITY; KNOWLEDGE; IMPACT; RATES AB The World Register of Marine Species is an over 90% complete open-access inventory of all marine species names. Here we illustrate the scale of the problems with species names, synonyms, and their classification, and describe how WoRMS publishes online quality assured information on marine species. Within WoRMS, over 100 global, 12 regional and 4 thematic species databases are integrated with a common taxonomy. Over 240 editors from 133 institutions and 31 countries manage the content. To avoid duplication of effort, content is exchanged with 10 external databases. At present WoRMS contains 460,000 taxonomic names (from Kingdom to subspecies), 368,000 species level combinations of which 215,000 are currently accepted marine species names, and 26,000 related but non-marine species. Associated information includes 150,000 literature sources, 20,000 images, and locations of 44,000 specimens. Usage has grown linearly since its launch in 2007, with about 600,000 unique visitors to the website in 2011, and at least 90 organisations from 12 countries using WoRMS for their data management. By providing easy access to expert-validated content, WoRMS improves quality control in the use of species names, with consequent benefits to taxonomy, ecology, conservation and marine biodiversity research and management. The service manages information on species names that would otherwise be overly costly for individuals, and thus minimises errors in the application of nomenclature standards. WoRMS' content is expanding to include host-parasite relationships, additional literature sources, locations of specimens, images, distribution range, ecological, and biological data. Species are being categorised as introduced (alien, invasive), of conservation importance, and on other attributes. These developments have a multiplier effect on its potential as a resource for biodiversity research and management. As a consequence of WoRMS, we are witnessing improved communication within the scientific community, and anticipate increased taxonomic efficiency and quality control in marine biodiversity research and management. C1 [Costello, Mark J.] Univ Auckland, Leigh Marine Lab, Auckland 1, New Zealand. [Bouchet, Philippe] Museum Natl Hist Nat, F-75231 Paris, France. [Boxshall, Geoff] Nat Hist Museum, London SW7 5BD, England. [Fauchald, Kristian; Walter, T. Chad] Smithsonian Inst, Washington, DC 20560 USA. [Gordon, Dennis] Natl Inst Water & Atmospher Res, Wellington, New Zealand. [Hoeksema, Bert W.; van Soest, Rob W. M.] Nat Biodivers Ctr, Leiden, Netherlands. [Poore, Gary C. B.] Museum Victoria, Melbourne, Vic, Australia. [Stohr, Sabine] Swedish Museum Nat Hist, Dept Invertebrate Zool, S-10405 Stockholm, Sweden. [Vanhoorne, Bart; Decock, Wim; Appeltans, Ward] Flanders Marine Inst, Oostende, Belgium. [Appeltans, Ward] Intergovt Oceanog Commiss UNESCO, IOC Project Off IODE, Oostende, Belgium. RP Costello, MJ (reprint author), Univ Auckland, Leigh Marine Lab, Auckland 1, New Zealand. EM m.costello@auckland.ac.nz RI Hoeksema, Bert/B-2973-2010; Stohr, Sabine/B-8629-2011; OI Hoeksema, Bert/0000-0001-8259-3783; Stohr, Sabine/0000-0002-2586-7239; Boxshall, Geoffrey/0000-0001-8170-7734; Costello, Mark/0000-0003-2362-0328 FU European commission research programme: FP4 Marine Science and Technology programme for ERMS [MAS3-CT97-0146]; Species 2000 europa; FP6 Marine biodiversity and Ecosystem Function (MarBEF) network of excellence; FP6 PESI; FP7 4D4 life; National Science Foundation CORONA project; Ocean Biogeographic Information system; Census of Marine Life Synthesis project; Global Biodiversity Information Facility; Musee Cantonal de Zoologie (Switzerland); Universite Pierre & Marie Curie(France); School of computer Science & Statitics, Lloyds Institute; Trinity College, Dublin(Ireland); Academia Sinica; Biodiversity Research Centre (Taiwan); Future of Marine Animal Program, Department of Biological Sciences, Dalhousie University (Canada); University of Aucklan's Leigh Marine Laboratory (New Zealand) FX The development of WoRMS has benefited from major funding from the European commission research programme: FP4 Marine Science and Technology programme for ERMS(MAS3-CT97-0146), Species 2000 europa, FP6 Marine biodiversity and Ecosystem Function (MarBEF) network of excellence, FP6 PESI and FP7 4D4 life. Funding has also been provided by the National Science Foundation CORONA project, Ocean Biogeographic Information system, Census of Marine Life Synthesis project and Global Biodiversity Information Facility. SMEBD acknowledges financial contributions from Musee Cantonal de Zoologie (Switzerland); Universite Pierre & Marie Curie(France); School of computer Science & Statitics, Lloyds Institute; Trinity College, Dublin(Ireland), Academia Sinica, Biodiversity Research Centre (Taiwan); Future of Marine Animal Program, Department of Biological Sciences, Dalhousie University (Canada); and the University of Aucklan's Leigh Marine Laboratory (New Zealand). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 113 TC 46 Z9 46 U1 3 U2 74 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 9 PY 2013 VL 8 IS 1 AR e51629 DI 10.1371/journal.pone.0051629 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 070YR UT WOS:000313551500006 PM 23505408 ER PT J AU Hatala, KG Dingwall, HL Wunderlich, RE Richmond, BG AF Hatala, Kevin G. Dingwall, Heather L. Wunderlich, Roshna E. Richmond, Brian G. TI Variation in Foot Strike Patterns during Running among Habitually Barefoot Populations SO PLOS ONE LA English DT Article ID HUMAN FOOTPRINTS; EVOLUTION; HYPOTHESIS; RUNNERS; HOMINID; FORCES; KENYA AB Endurance running may have a long evolutionary history in the hominin clade but it was not until very recently that humans ran wearing shoes. Research on modern habitually unshod runners has suggested that they utilize a different biomechanical strategy than runners who wear shoes, namely that barefoot runners typically use a forefoot strike in order to avoid generating the high impact forces that would be experienced if they were to strike the ground with their heels first. This finding suggests that our habitually unshod ancestors may have run in a similar way. However, this research was conducted on a single population and we know little about variation in running form among habitually barefoot people, including the effects of running speed, which has been shown to affect strike patterns in shod runners. Here, we present the results of our investigation into the selection of running foot strike patterns among another modern habitually unshod group, the Daasanach of northern Kenya. Data were collected from 38 consenting adults as they ran along a trackway with a plantar pressure pad placed midway along its length. Subjects ran at self-selected endurance running and sprinting speeds. Our data support the hypothesis that a forefoot strike reduces the magnitude of impact loading, but the majority of subjects instead used a rearfoot strike at endurance running speeds. Their percentages of midfoot and forefoot strikes increased significantly with speed. These results indicate that not all habitually barefoot people prefer running with a forefoot strike, and suggest that other factors such as running speed, training level, substrate mechanical properties, running distance, and running frequency, influence the selection of foot strike patterns. C1 [Hatala, Kevin G.] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Hatala, Kevin G.; Dingwall, Heather L.; Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC USA. [Wunderlich, Roshna E.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Hatala, KG (reprint author), George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. EM kghatala@gwmail.gwu.edu FU National Science Foundation [BCS-0924476, DGE-0801634]; George Washington University Lewis N. Cotlow Fund FX This research was funded by the National Science Foundation, grants BCS-0924476 and DGE-0801634, and the George Washington University Lewis N. Cotlow Fund. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 28 TC 31 Z9 31 U1 5 U2 135 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 9 PY 2013 VL 8 IS 1 AR e52548 DI 10.1371/journal.pone.0052548 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 070YR UT WOS:000313551500018 PM 23326341 ER PT J AU Karanth, KU Gopalaswamy, AM Karanth, KK Goodrich, J Seidensticker, J Robinson, JG AF Karanth, K. Ullas Gopalaswamy, Arjun M. Karanth, Krithi K. Goodrich, John Seidensticker, John Robinson, John G. TI Sinks as saviors: Why flawed inference cannot assist tiger recovery SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Karanth, K. Ullas; Robinson, John G.] Wildlife Conservat Soc, Global Conservat Program, Bronx, NY 10460 USA. [Karanth, K. Ullas; Gopalaswamy, Arjun M.; Karanth, Krithi K.] Ctr Wildlife Studies, Bangalore 560042, Karnataka, India. [Gopalaswamy, Arjun M.] Univ Oxford, Dept Zool, Wildlife Conservat Res Unit, Oxford OX1 3PS, England. [Karanth, Krithi K.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Goodrich, John] Panthera, Tiger Program, New York, NY 10018 USA. [Seidensticker, John] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Karanth, KU (reprint author), Wildlife Conservat Soc, Global Conservat Program, Bronx, NY 10460 USA. EM ukaranth@gmail.com NR 5 TC 10 Z9 10 U1 1 U2 46 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JAN 8 PY 2013 VL 110 IS 2 BP E110 EP E110 DI 10.1073/pnas.1216623110 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 075SK UT WOS:000313906600003 PM 23284176 ER PT J AU Garcia-Robledo, C Erickson, DL Staines, CL Erwin, TL Kress, WJ AF Garcia-Robledo, Carlos Erickson, David L. Staines, Charles L. Erwin, Terry L. Kress, W. John TI Tropical Plant-Herbivore Networks: Reconstructing Species Interactions Using DNA Barcodes SO PLOS ONE LA English DT Article ID COLEOPTERA-CHRYSOMELIDAE CASSIDINAE; ROLLED-LEAF BEETLES; HOST PLANTS; INSECT HERBIVORES; ENVIRONMENTAL DNA; HISPINE BEETLES; RAIN-FOREST; COSTA-RICA; GINGERS; COEVOLUTION AB Plants and their associated insect herbivores, represent more than 50% of all known species on earth. The first step in understanding the mechanisms generating and maintaining this important component of biodiversity is to identify plant-herbivore associations. In this study we determined insect-host plant associations for an entire guild of insect herbivores using plant DNA extracted from insect gut contents. Over two years, in a tropical rain forest in Costa Rica (La Selva Biological Station), we recorded the full diet breadth of rolled-leaf beetles, a group of herbivores that feed on plants in the order Zingiberales. Field observations were used to determine the accuracy of diet identifications using a three-locus DNA barcode (rbcL, trnH-psbA and ITS2). Using extraction techniques for ancient DNA, we obtained high-quality sequences for two of these loci from gut contents (rbcL and ITS2). Sequences were then compared to a comprehensive DNA barcode library of the Zingiberales. The rbcL locus identified host plants to family (success/sequence = 58.8%) and genus (success/sequence = 47%). For all Zingiberales except Heliconiaceae, ITS2 successfully identified host plants to genus (success/sequence = 67.1%) and species (success/sequence = 61.6%). Kindt's sampling estimates suggest that by collecting ca. four individuals representing each plant-herbivore interaction, 99% of all host associations included in this study can be identified to genus. For plants that amplified ITS2, 99% of the hosts can be identified to species after collecting at least four individuals representing each interaction. Our study demonstrates that host plant identifications at the species-level using DNA barcodes are feasible, cost-effective, and reliable, and that reconstructing plant-herbivore networks with these methods will become the standard for a detailed understanding of these interactions. C1 [Garcia-Robledo, Carlos; Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Garcia-Robledo, Carlos; Staines, Charles L.; Erwin, Terry L.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM garciac@si.edu FU Smithsonian Postdoctoral Fellowship; National Geographic-Waitt Institute [W149-11]; Heliconia Society; Rubenstein Fellowship - Encyclopedia of Life FX This research was funded by the Smithsonian Postdoctoral Fellowship, the National Geographic-Waitt Institute grant (W149-11), Heliconia Society Grant and the Rubenstein Fellowship - Encyclopedia of Life to CG. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 48 TC 38 Z9 44 U1 5 U2 132 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 8 PY 2013 VL 8 IS 1 AR e52967 DI 10.1371/journal.pone.0052967 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 069IY UT WOS:000313429800023 PM 23308128 ER PT J AU Haselhorst, DS Moreno, JE Punyasena, SW AF Haselhorst, Derek S. Enrique Moreno, J. Punyasena, Surangi W. TI Variability within the 10-Year Pollen Rain of a Seasonal Neotropical Forest and Its Implications for Paleoenvironmental and Phenological Research SO PLOS ONE LA English DT Article ID TROPICAL FOREST; COSTA-RICA; EL-NINO; TREES; VEGETATION; CLIMATE; RECORD; PANAMA; REPRESENTATION; DISPERSAL AB Tropical paleoecologists use a combination of mud-water interface and modern pollen rain samples (local samples of airborne pollen) to interpret compositional changes within fossil pollen records. Taxonomic similarities between the composition of modern assemblages and fossil samples are the basis of reconstructing paleoclimates and paleoenvironments. Surface sediment samples reflect a time-averaged accumulation of pollen spanning several years or more. Due to experimental constraints, modern pollen rain samples are generally collected over shorter timeframes (1-3 years) and are therefore less likely to capture the full range of natural variability in pollen rain composition and abundance. This potentially biases paleoenvironmental interpretations based on modern pollen rain transfer functions. To determine the degree to which short-term environmental change affects the composition of the aerial pollen flux of Neotropical forests, we sampled ten years of the seasonal pollen rain from Barro Colorado Island, Panama and compared it to climatic and environmental data over the same ten-year span. We establish that the pollen rain effectively captured the strong seasonality and stratification of pollen flow within the forest canopy and that individual taxa had variable sensitivity to seasonal and annual changes in environmental conditions, manifested as changes in pollen productivity. We conclude that modern pollen rain samples capture the reproductive response of moist tropical plants to short-term environmental change, but that consequently, pollen rain-based calibrations need to include longer sampling periods (>= 7 years) to reflect the full range of natural variability in the pollen output of a forest and simulate the time-averaging present in sediment samples. Our results also demonstrate that over the long-term, pollen traps placed in the forest understory are representative samples of the pollen output of both canopy and understory vegetation. Aerial pollen traps, therefore, also represent an underutilized means of monitoring the pollen productivity and reproductive behavior of moist tropical forests. C1 [Haselhorst, Derek S.; Punyasena, Surangi W.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Enrique Moreno, J.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Panama City, Panama. [Punyasena, Surangi W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Punyasena, SW (reprint author), Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. EM punyasena@life.illinois.edu RI Punyasena, Surangi/C-9134-2011 FU University of Illinois Campus Research Board [09236, 11239]; University of Illinois Center for Latin American and Caribbean Studies Tinker Travel Grant; U.S. National Science Foundation [NSF EF-1137396] FX Funding was provided by the University of Illinois Campus Research Board (Grants #09236 and #11239) to SWP and a University of Illinois Center for Latin American and Caribbean Studies Tinker Travel Grant to DSH. SWP acknowledges additional support from the U.S. National Science Foundation (NSF EF-1137396). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 53 TC 5 Z9 5 U1 0 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JAN 8 PY 2013 VL 8 IS 1 AR e53485 DI 10.1371/journal.pone.0053485 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 069IY UT WOS:000313429800054 PM 23320089 ER PT J AU Holt, B Lessard, JP Borregaard, MK Fritz, SA Araujo, MB Dimitrov, D Fabre, PH Graham, CH Graves, GR Jonsson, KA Nogues-Bravo, D Wang, ZH Whittaker, RJ Fjeldsa, J Rahbek, C AF Holt, Ben G. Lessard, Jean-Philippe Borregaard, Michael K. Fritz, Susanne A. Araujo, Miguel B. Dimitrov, Dimitar Fabre, Pierre-Henri Graham, Catherine H. Graves, Gary R. Jonsson, Knud A. Nogues-Bravo, David Wang, Zhiheng Whittaker, Robert J. Fjeldsa, Jon Rahbek, Carsten TI An Update of Wallace's Zoogeographic Regions of the World SO SCIENCE LA English DT Article ID GLOBAL PATTERNS; CLIMATE-CHANGE; DISTRIBUTIONS; CONSERVATION; DIVERSITY; VELOCITY; ENDEMISM AB Modern attempts to produce biogeographic maps focus on the distribution of species, and the maps are typically drawn without phylogenetic considerations. Here, we generate a global map of zoogeographic regions by combining data on the distributions and phylogenetic relationships of 21,037 species of amphibians, birds, and mammals. We identify 20 distinct zoogeographic regions, which are grouped into 11 larger realms. We document the lack of support for several regions previously defined based on distributional data and show that spatial turnover in the phylogenetic composition of vertebrate assemblages is higher in the Southern than in the Northern Hemisphere. We further show that the integration of phylogenetic information provides valuable insight on historical relationships among regions, permitting the identification of evolutionarily unique regions of the world. C1 [Holt, Ben G.; Lessard, Jean-Philippe; Borregaard, Michael K.; Fritz, Susanne A.; Araujo, Miguel B.; Graves, Gary R.; Nogues-Bravo, David; Wang, Zhiheng; Whittaker, Robert J.; Rahbek, Carsten] Univ Copenhagen, Ctr Macroecol Evolut & Climate, Dept Biol, DK-2100 Copenhagen O, Denmark. [Fritz, Susanne A.] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Fritz, Susanne A.] Senckenberg Gesell Nat Forsch, D-60325 Frankfurt, Germany. [Araujo, Miguel B.] CSIC, Dept Biogeog & Global Change, Natl Museum Nat Sci, Madrid 28006, Spain. [Araujo, Miguel B.] Univ Evora, Ctr Invest Biodiversidade & Recursos Genet, P-7000 Evora, Portugal. [Dimitrov, Dimitar; Fabre, Pierre-Henri; Jonsson, Knud A.; Fjeldsa, Jon] Univ Copenhagen, Ctr Macroecol Evolut & Climate, Nat Hist Museum Denmark, DK-2100 Copenhagen O, Denmark. [Graham, Catherine H.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. [Graves, Gary R.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Whittaker, Robert J.] Univ Oxford, Biodivers Res Grp, Sch Geog & Environm, Ctr Environm, Oxford OX1 3QY, England. RP Lessard, JP (reprint author), Univ Copenhagen, Ctr Macroecol Evolut & Climate, Dept Biol, DK-2100 Copenhagen O, Denmark. EM jplessard@bio.ku.dk RI Fjeldsa, Jon/A-9699-2013; Borregaard, Michael/B-8442-2008; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017; Rahbek, Carsten/D-9372-2013; Rahbek, Carsten/L-1129-2013; Dimitrov, Dimitar/A-9563-2009; Graham, Catherine/A-9560-2011; Whittaker, Robert/H-1548-2015; Araujo, Miguel/B-6117-2008; Fritz, Susanne/M-9872-2014; Wang, Zhiheng/G-1750-2010 OI Jonsson, Knud/0000-0002-1875-9504; Fjeldsa, Jon/0000-0003-0790-3600; Borregaard, Michael/0000-0002-8146-8435; Holt, Ben G./0000-0003-0831-9684; Dimitrov, Dimitar/0000-0001-5830-5702; Whittaker, Robert/0000-0001-7775-3383; Araujo, Miguel/0000-0002-5107-7265; Fritz, Susanne/0000-0002-4085-636X; FU Danish National Research Foundation; Marie Curie Actions under the Seventh Framework Programme [PIEF-GA-2009-252888]; Spanish Research Council (CSIC) FX We thank the Danish National Research Foundation for its support of the Center for Macroecology, Evolution, and Climate. B.G.H. also thanks the Marie Curie Actions under the Seventh Framework Programme (PIEF-GA-2009-252888). M.B.A. also thanks the Spanish Research Council (CSIC) for support, and S.A.F. thanks the Landes-Offensive zur Entwicklung Wissenschaftlich-Okonomischer Exzellenz program of Hesse's Ministry of Higher Education, Research, and the Arts. We thank L. Hansen for help with data and reference compilations. We thank the International Union for Conservation of Nature and Natural Resources for making the amphibian and mammal range data available. Data are archived at http://macroecology.ku.dk/resources/wallace. NR 26 TC 232 Z9 255 U1 22 U2 379 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 4 PY 2013 VL 339 IS 6115 BP 74 EP 78 DI 10.1126/science.1228282 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 063HC UT WOS:000312985800054 PM 23258408 ER PT J AU Carretti, E Crocker, RM Staveley-Smith, L Haverkorn, M Purcell, C Gaensler, BM Bernardi, G Kesteven, MJ Poppi, S AF Carretti, Ettore Crocker, Roland M. Staveley-Smith, Lister Haverkorn, Marijke Purcell, Cormac Gaensler, B. M. Bernardi, Gianni Kesteven, Michael J. Poppi, Sergio TI Giant magnetized outflows from the centre of the Milky Way SO NATURE LA English DT Article ID X-RAY-EMISSION; GALACTIC-CENTER; FERMI BUBBLES; COSMIC-RAYS; GAMMA-RAYS; FIELD; WIND; NUCLEUS; GALAXY; BULGE AB The nucleus of the Milky Way is known to harbour regions of intense star formation activity as well as a supermassive black hole(1). Recent observations have revealed regions of gamma-ray emission reaching far above and below the Galactic Centre (relative to the Galactic plane), the so-called 'Fermi bubbles'(2). It is uncertain whether these were generated by nuclear star formation or by quasar-like outbursts of the central black hole(3-6) and no information on the structures' magnetic field has been reported. Here we report observations of two giant, linearly polarized radio lobes, containing three ridgelike substructures, emanating from the Galactic Centre. The lobes each extend about 60 degrees in the Galactic bulge, closely corresponding to the Fermi bubbles, and are permeated by strong magnetic fields of up to 15 microgauss. We conclude that the radio lobes originate in a biconical, star-formation-driven (rather than black-hole-driven) outflow from the Galaxy's central 200 parsecs that transports a huge amount of magnetic energy, about 10(55) ergs, into the Galactic halo. The ridges wind around this outflow and, we suggest, constitute a 'phonographic' record of nuclear star formation activity over at least ten million years. C1 [Carretti, Ettore] CSIRO Astron & Space Sci, Parkes, NSW 2870, Australia. [Crocker, Roland M.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Crocker, Roland M.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Staveley-Smith, Lister] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Staveley-Smith, Lister] Univ Western Australia, ARC Ctr Excellence All sky Astrophys CAASTRO, Crawley, WA 6009, Australia. [Haverkorn, Marijke] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Haverkorn, Marijke] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Purcell, Cormac; Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kesteven, Michael J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Poppi, Sergio] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. RP Carretti, E (reprint author), CSIRO Astron & Space Sci, POB 276, Parkes, NSW 2870, Australia. EM Ettore.Carretti@csiro.au RI Gaensler, Bryan/F-8655-2010; Staveley-Smith, Lister/A-1683-2011; OI Purcell, Cormac/0000-0002-7491-7386; Staveley-Smith, Lister/0000-0002-8057-0294; Carretti, Ettore/0000-0002-3973-8403; Poppi, Sergio/0000-0002-4698-2607; Gaensler, Bryan/0000-0002-3382-9558 FU Max-Planck-Institut fur Kernphysik; Australian Research Council [FT110100108]; Australian Laureate Fellowship from the Australian Research Council [FL100100114]; Netherlands Organisation for Scientific Research (NWO) [639.042.915] FX This work has been carried out in the framework of the S-band Polarization All Sky Survey collaboration (S-PASS). We thank the Parkes Telescope staff for support, both while setting up the non-standard observing mode and during the observing runs. R. M. C. thanks F. Aharonian, R. Beck, G. Bicknell, D. Jones, C. Law, M. Morris, C. Pfrommer, W. Reich, A. Stolte, T. Porter and H. Volk for discussions, and the Max-Planck-Institut fur Kernphysik for supporting his research. R. M. C. also acknowledges the support of a Future Fellowship from the Australian Research Council through grant FT110100108. B. M. G. and C. P. acknowledge the support of an Australian Laureate Fellowship from the Australian Research Council through grant FL100100114. M. H. acknowledges the support of research programme 639.042.915, which is partly financed by the Netherlands Organisation for Scientific Research (NWO). The Parkes Radio Telescope is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We acknowledge the use of WMAP data and the HEALPix software package. NR 29 TC 73 Z9 73 U1 1 U2 21 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 3 PY 2013 VL 493 IS 7430 BP 66 EP 69 DI 10.1038/nature11734 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 062QC UT WOS:000312933800031 PM 23282363 ER PT B AU Gonzales, AA Evans, TQ AF Gonzales, Angela A. Evans, Timotothy Q. BE DenOuden, AE OBrien, JM TI The Imposition of Law The Federal Acknowledgment Process and the Legal De/Construction of Tribal Identity SO RECOGNITION, SOVEREIGNTY STRUGGLES, & INDIGENOUS RIGHTS IN THE UNITED STATES: A SOURCEBOOK LA English DT Article; Book Chapter C1 [Gonzales, Angela A.] Cornell Univ, Dept Dev Sociol, Amer Indian Studies Program, Ithaca, NY 14853 USA. [Gonzales, Angela A.] NMAI, Washington, DC USA. [Gonzales, Angela A.] Natl Museum African Amer Hist & Culture, Washington, DC USA. [Gonzales, Angela A.] Smithsonian Inst, Traveling Serv, Washington, DC 20560 USA. [Evans, Timotothy Q.] Princeton Univ, Woodrow Wilson Sch Publ & Int Affairs, Princeton, NJ 08544 USA. RP Gonzales, AA (reprint author), Cornell Univ, Dept Dev Sociol, Amer Indian Studies Program, Ithaca, NY 14853 USA. NR 40 TC 0 Z9 0 U1 0 U2 0 PU UNIV NORTH CAROLINA PRESS PI CHAPEL HILL PA BOX 2288, CHAPEL HILL, NC 27514 USA BN 978-1-4696-0216-5; 978-1-4696-0217-2; 978-1-4696-0215-8 PY 2013 BP 37 EP 63 PG 27 WC Ethnic Studies; Law SC Ethnic Studies; Government & Law GA BB6DT UT WOS:000344698900002 ER PT S AU Braje, TJ Erlandson, JM Rick, TC AF Braje, Todd J. Erlandson, Jon M. Rick, Torben C. BE Ono, R Morrison, A Addison, D TI Red Abalone, Sea Otters, and Kelp Forest Ecosystems on Historic Period San Miguel Island, California SO PREHISTORIC MARINE RESOURCE USE IN THE INDO-PACIFIC REGIONS SE Terra Australis LA English DT Proceedings Paper CT 19th Congress of the Indo-Pacific-Prehistory-Association (IPPA) CY 2009 CL Hanoi, VIETNAM SP Indo Pacific Prehist Assoc ID CHANNEL-ISLANDS; COMMUNITIES; BIODIVERSITY; SUBSISTENCE; RESILIENCE; FISHERY; IMPACTS C1 [Braje, Todd J.] San Diego State Univ, San Diego, CA 92182 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 40 TC 0 Z9 0 U1 0 U2 4 PU AUSTRALIAN NATL UNIV PI CANBERRA ACT PA P O BOX 4, 2600 CANBERRA ACT, AUSTRALIA SN 0725-9018 BN 978-1-925021-25-7; 978-1-925021-26-4 J9 TERRA AUSTRALIS PY 2013 VL 39 BP 85 EP 96 PG 12 WC Anthropology; Environmental Studies SC Anthropology; Environmental Sciences & Ecology GA BB6YU UT WOS:000345152000004 ER PT S AU Sues, HD Desojo, JB Ezcurra, MD AF Sues, Hans-Dieter Desojo, Julia B. Ezcurra, Martin D. BE Nesbitt, SJ Desojo, JB Irmis, RB TI Doswelliidae: a clade of unusual armoured archosauriforms from the Middle and Late Triassic SO ANATOMY, PHYLOGENY AND PALAEOBIOLOGY OF EARLY ARCHOSAURS AND THEIR KIN SE Geological Society Special Publication LA English DT Proceedings Paper CT 1st Symposium of Early Archosaur Evolution at the IV Congreso Latinoamericano de Paleontologia de de Vertebrados CY SEP, 2011 CL San Juan, ARGENTINA ID ENIGMATIC ARCHOSAUROMORPH DOSWELLIA; BLUEWATER CREEK FORMATION; NEW-MEXICO; ARGENTINA; USA AB Doswelliidae is a clade of armoured non-archosaurian archosauriform reptiles more closely related to Archosauria than are Proterosuchidae, Erythrosuchidae and possibly Euparkeria capensis. It is currently known from the late Middle Triassic (Ladinian) of Germany, the late Middle to early Late Triassic (Ladinian-Carnian) of Argentina and Brazil, and the Late Triassic (Carnian-Norian) of the USA. To date, two unambiguous synapomorphies diagnose Doswelliidae: (i) osteoderm ornamentation coarse, incised, and composed of central regular pits of subequal size and shape, and (ii) osteoderms with anterior articular lamina. Five taxa are currently recognized: Archeopelta arborensis, Doswellia kaltenbachi, Doswellia sixmilensis, Tarjadia ruthae and a new taxon from Germany. Based on skeletal features and occurrence, doswelliid archosauriforms may have had a semi-aquatic mode of life. C1 [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. [Ezcurra, Martin D.] Ludwig Maximilian-Univ, GeoBio-Ctr, D-80333 Munich, Germany. [Desojo, Julia B.] Museo Argentino de Ciencias, Buenos Aires, DF, Argentina. RP Sues, HD (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu NR 22 TC 1 Z9 1 U1 0 U2 2 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-361-5 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2013 VL 379 BP 49 EP 58 DI 10.1144/SP379.13 PG 10 WC Geology; Paleontology SC Geology; Paleontology GA BB5EM UT WOS:000343734500004 ER PT J AU Bucher, KE Norris, JN Sears, JR AF Bucher, Katina E. Norris, James N. Sears, James R. TI Gloiotrichus vermiculatus sp. nov. (Liagoraceae, Rhodophyta), a new species from the Caribbean Sea SO CARIBBEAN JOURNAL OF SCIENCE LA English DT Article DE Belize; marine algae; morphology; reproduction; seaweed; St. John (US Virgin Islands); taxonomy ID REPRODUCTIVE MORPHOLOGY; NEMALIALES AB Gloiotrichus (Liagoraceae; Nemaliales), a red algal genus originally described from Western Australia and later found in Hawaii, is reported for the first time in the western Atlantic Ocean, from the Caribbean Sea. A new species, G. vermiculatus, is described based on specimens collected from subtidal waters near Carrie Bow Cay, Belize and off St. John, U.S. Virgin Islands. Features of the new species are compared with G. fractalis Huisman et Kraft (1994), the generitype, and only other species presently in the genus. Gloiotrichus vermiculatus differs reproductively; in having fewer cells in its carpogonial branch, (3-) 4 (-5) cells versus 5-8 cells for G. fractalis; and dioecious gametophytes while those of G. fractalis are monoecious. The timing of sterile lateral filament initiation from carpogonial branch cells varies between the two species, with G. fractalis generally initiating them before the first transverse division of the zygote, while those of G. vermiculatus are typically initiated concurrently or after the first division. The basal cell or other proximal cells of the sterile lateral filaments occasionally issue rhizoid-like filaments that can develop to a higher degree in G. vermiculatus, where they may loosely drape or encircle carpogonial branch cells. The new species differs vegetatively from G. fractalis in its longer (290-500 mu m) and more complex primary cortical fascicles, which are trichotomously to polychotomously branched, not only at the basal division but at several inner divisions, thereafter the cortical filaments are subdichotomously branched outward, while those of G. fractalis are described as subdichotomously branched throughout. C1 [Bucher, Katina E.; Norris, James N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Sears, James R.] Univ Massachusetts Dartmouth, Dept Biol, N Dartmouth, MA 02747 USA. RP Bucher, KE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB 166,POB 37012, Washington, DC 20013 USA. EM norrisj@si.edu; jsears@umassd.edu FU Smithsonian Caribbean Coral Reef Ecosystem Program [904] FX JN and KB are grateful for support from the Smithsonian Caribbean Coral Reef Ecosystem Program [Klaus Rutzler, CCRE Program Director]; this study represents CCRE contribution # 904). Diving and collecting assistance of W. Fenical, R. H. Sims, S. Fredericq, C. F. D. Gurgel, M. E. Hay, A.R. Sears and R.R. Sears, and Chip Clark is appreciated. We three authors thank I. A. Abbott for pointing out that we may have been independently working on the same alga. Early discussions with Izzie Abbott, Gerald Kraft, Suzanne Fredericq, and Max Hommersand were helpful in understanding the relationship between Gloiotrichus vermiculatus and related taxa in the Liagoraceae and we appreciate their interest and assistance. We are also grateful to I. A. Abbott and S. Fredericq for reviewing earlier versions of the manuscript; S. Fredericq for photomicrographs of the St. John specimen; Chip Clark for the photograph of the holotype; R. H. Sims for assistance with Adobe Photoshop CS-3; and D. H. Nicolson for discussion on specific names. We thank Prof. Alex George (Murdoch University, Perth, WA) for translation of the diagnosis into latin. NR 19 TC 0 Z9 0 U1 1 U2 1 PU UNIV PUERTO RICO, PI MAYAGUEZ PA COLLEGE ARTS SCIENCES, MAYAGUEZ, PR 00680 USA SN 0008-6452 J9 CARIBB J SCI JI Caribb. J. Sci. PY 2013 VL 47 IS 1 BP 98 EP 113 PG 16 WC Biodiversity Conservation SC Biodiversity & Conservation GA AR7TF UT WOS:000343782000008 ER PT S AU Ebbestad, JOR Fryda, J Wagner, PJ Horny, RJ Isakar, M Stewart, S Percival, IG Bertero, V Rohr, DM Peel, JS Blodgett, RB Hogstrom, AES AF Ebbestad, Jan Ove R. Fryda, Jiri Wagner, Peter J. Horny, Radvan J. Isakar, Mare Stewart, Sarah Percival, Ian G. Bertero, Veronica Rohr, David M. Peel, John S. Blodgett, Robert B. Hogstrom, Anette E. S. BE Harper, DAT Servais, T TI Biogeography of Ordovician and Silurian gastropods, monoplacophorans and mimospirids SO EARLY PALAEOZOIC BIOGEOGRAPHY AND PALAEOGEOGRAPHY SE Geological Society Memoirs LA English DT Proceedings Paper CT Meeting of IGCP 503 on Ordovician Palaeogeography and Palaeoclimate CY SEP, 2009 CL Copenhagen, DENMARK SP IGCP ID LOWER-MIDDLE ORDOVICIAN; ARGENTINE PRECORDILLERA; BRACHIOPOD FAUNAS; DIVERSITY; AUSTRALIA; TERRANES; PALEOECOLOGY; SOUTHEASTERN; NOMENCLATURE; COMMUNITIES AB The biogeographical distribution of Ordovician and Silurian gastropods, monoplacophorans and mimospirids has been analysed on a generic level. The dataset contains 334 genera and 2769 species, yielding 1231 records of genera with 2274 occurrences worldwide. There is a bias towards eastern Laurentia, Baltica and Perunica records. Some 53.1% of the records are Ordovician. The study demonstrates that these molluscs are well suited to being used to improve understanding of Ordovician and Silurian biogeographical provinciality. Specific points are that: a Lower Ordovician assemblage is evident in Laurentia; the fauna of the Argentinean Precordillera is Laurentian until the Darriwilian, when taxa are shared with North China; Late Silurian gastropods from the Alexander terrane (SE Alaska) are unknown in Laurentia, but support a rift origin of this terrane from NE Siberia; Perunica, Ibero-Armorica and Morocco cluster together throughout the Ordovician but Perunica and Morocco are closer; Darriwilian-Sandbian deep-water Bohemian taxa occur in Baltica; a Laurentian-Baltica proximity is unsupported until the Silurian; Siberia clusters with North China and eastern Laurentia during the Tremadocian-Darriwilian; during the Gorstian-Pridoli Siberia clusters with the Farewell and Alexander terranes; North China may have been close to Laurentia and the Argentinean margin of Gondwana; and the affinity of Tarim taxa is problematic. C1 [Ebbestad, Jan Ove R.] Uppsala Univ, Museum Evolut, SE-75236 Uppsala, Sweden. [Fryda, Jiri] Czech Geol Survey, Prague 15000, Czech Republic. [Wagner, Peter J.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Horny, Radvan J.] Natl Museum, Dept Palaeontol, Prague 11579 1, Czech Republic. [Isakar, Mare] Univ Tartu, Museum Geol, EE-51014 Tartu, Estonia. [Stewart, Sarah] Natl Museum Scotland, Edinburgh EH1 1JF, Midlothian, Scotland. [Percival, Ian G.] Geol Survey New South Wales, WB Clarke Geosci Ctr, Londonderry, NSW 2753, Australia. [Bertero, Veronica] Univ Nacl Cordoba, Fac Ciencias Exactas Fis & Nat, CICTERRA CONICET, Ctr Invest Paleobiol, RA-5000 Cordoba, Argentina. [Rohr, David M.] Sul Ross State Univ, Dept Earth & Phys Sci, Alpine, TX 79832 USA. [Peel, John S.] Uppsala Univ, Dept Earth Sci Palaeobiol, SE-75236 Uppsala, Sweden. [Hogstrom, Anette E. S.] Tromso Univ Museum, N-9037 Tromso, Norway. RP Ebbestad, JOR (reprint author), Uppsala Univ, Museum Evolut, Norbyvagen 16, SE-75236 Uppsala, Sweden. EM jan-ove.ebbestad@em.uu.se OI Percival, Ian/0000-0001-5161-2021; Ebbestad, Jan Ove/0000-0001-8769-3572 NR 107 TC 5 Z9 5 U1 0 U2 3 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0435-4052 BN 978-1-86239-373-8 J9 GEOL SOC MEM PY 2013 VL 38 BP 199 EP 220 DI 10.1144/M38.15 PG 22 WC Geography, Physical; Geology; Paleontology SC Physical Geography; Geology; Paleontology GA BB5EJ UT WOS:000343729900015 ER PT S AU Nakamura, M Algaba, JC Asada, K Chen, B Chen, MT Han, J Ho, PHP Hsieh, SN Huang, T Inoue, M Koch, P Kuo, CY Martin-Cocher, P Matsushita, S Meyer-Zhao, Z Nishioka, H Nystrom, G Pradel, N Pu, HY Raffin, P Shen, HY Tseng, CY AF Nakamura, M. Algaba, J. C. Asada, K. Chen, B. Chen, M. -T. Han, J. Ho, P. H. P. Hsieh, S. -N. Huang, T. Inoue, M. Koch, P. Kuo, C. -Y. Martin-Cocher, P. Matsushita, S. Meyer-Zhao, Z. Nishioka, H. Nystrom, G. Pradel, N. Pu, H. -Y. Raffin, P. Shen, H. -Y. Tseng, C. -Y. CA Greenland Telescope Project Team BE Gomez, JL TI Greenland Telescope (GLT) Project "A Direct Confirmation of Black Hole with Submillimeter VLBI" SO INNERMOST REGIONS OF RELATIVISTIC JETS AND THEIR MAGNETIC FIELDS SE EPJ Web of Conferences LA English DT Proceedings Paper CT International Symposium on Innermost Regions of Relativistic Jets and their Magnetic Field CY JUN 10-14, 2013 CL CSIC, Inst Astrofisica Andalucia, Granada, SPAIN SP RadioNet, Consejo Super Investigaciones Cientificas, Junta Andalucia HO CSIC, Inst Astrofisica Andalucia ID GALACTIC-CENTER; M87 AB The GLT project is deploying a new submillimeter (submm) VLBI station in Greenland. Our primary scientific goal is to image a shadow of the supermassive black hole (SMBH) of six billion solar masses in M87 at the center of the Virgo cluster of galaxies. The expected SMBH shadow size of 40-50 mu as requires superbly high angular resolution, suggesting that the submm VLBI would be the only way to obtain the shadow image. The Summit station in Greenland enables us to establish baselines longer than 9,000 km with ALMA in Chile and SMA in Hawaii as well as providing a unique u-v coverage for imaging M87. Our VLBI network will achieve a superior angular resolution of about 20 mu as at 350 GHz, corresponding to similar to 2.5 times of the Schwarzschild radius of the supermassive black hole in M87. We have been monitoring the atmospheric opacity at 230 GHz since August. 2011; we have confirmed the value on site during the winter season is comparable to the ALMA site thanks to high altitude of 3,200 m and low temperature of -50 degrees C. We will report current status and future plan of the GLT project towards our expected first light on 2015-2016. C1 [Nakamura, M.; Algaba, J. C.; Asada, K.; Chen, B.; Chen, M. -T.; Han, J.; Ho, P. H. P.; Hsieh, S. -N.; Huang, T.; Inoue, M.; Koch, P.; Kuo, C. -Y.; Martin-Cocher, P.; Matsushita, S.; Meyer-Zhao, Z.; Nishioka, H.; Pradel, N.; Pu, H. -Y.; Raffin, P.; Shen, H. -Y.; Tseng, C. -Y.] Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. [Nystrom, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. MIT, Haystack Observ, Westford, MA 01886 USA. [Greenland Telescope Project Team] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Nakamura, M (reprint author), Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,AS NTU 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. OI Pu, Hung-Yi/0000-0001-9270-8812 NR 11 TC 0 Z9 0 U1 0 U2 2 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X J9 EPJ WEB CONF PY 2013 VL 61 AR UNSP 01008 DI 10.1051/epjconf/20136101008 PG 4 WC Physics, Applied; Physics, Multidisciplinary SC Physics GA BB5CU UT WOS:000343671600008 ER PT S AU Tabor, NJ Romanchock, CM Looy, CV Hotton, CL Dimichele, WA Chaney, DS AF Tabor, Neil J. Romanchock, Charles M. Looy, Cynthia V. Hotton, Carol L. Dimichele, William A. Chaney, Dan S. BE Gasiewicz, A Slowakiewicz, M TI Conservatism of Late Pennsylvanian vegetational patterns during short-term cyclic and long-term directional environmental change, western equatorial Pangea SO PALAEOZOIC CLIMATE CYCLES: THEIR EVOLUTIONARY AND SEDIMENTOLOGICAL IMPACT SE Geological Society Special Publication LA English DT Article; Book Chapter ID LATE PALEOZOIC CONIFERS; NORTH-AMERICA; SEA-LEVEL; PALYNOLOGICAL EVIDENCE; APPALACHIAN BASIN; TROPICAL LOWLANDS; ATLANTIC CANADA; GEOLOGICAL TIME; GLACIAL PHASES; CLIMATE-CHANGE AB Patterns of plant distribution by palaeoenvironment were examined across the Pennsylvanian- Permian transition in North-Central Texas. Stratigraphically recurrent packages of distinct lithofacies, representing different habitats, contain qualitatively and quantitatively different macrofloras and microfloras. The species pools demonstrate niche conservatism, remaining closely tied to specific habitats, during both short-term cyclic environmental change and a long-term trend of increasing aridity. The deposits examined principally comprise the terrestrial Markley and its approximate marine equivalent, the Harpersville Formation and parts of lower Archer City Formation. Fossiliferous deposits are lens-like, likely representing fill sequences of channels formed during abandonment phases. Palaeosols, represented by blocky mudstones, comprise a large fraction of the deposits. They suggest progressive climate change from minimally seasonal humid to seasonal subhumid to seasonal dry subhumid. Five lithofacies yielded plants: kaolinite-dominated siltstone, organic shale, mudstone beds within organic shale, coarsening upward mudstone-sandstone interbeds and channel sandstone. Both macro-and microflora were examined. Lithofacies proved compositionally distinct, with different patterns of dominance diversity. Organic shales (swamp deposits), mudstone partings (swamp drainages) and coarsening upward mudstone-sandstone interbeds (floodplains) typically contain Pennsylvanian wetland vegetation. Kaolinite-dominated siltstones and (to the extent known) sandstones contain taxa indicative of seasonally dry substrates. Some kaolinite-dominated siltstones and organic shales/coals yielded palynomorphs. Microfloras are more diverse, with greater wetland-dryland overlap than macrofloras. It appears that these two floras were coexistent at times on the regional landscape. C1 [Tabor, Neil J.] Huffington Dept Earth Sci, Dallas, TX 75275 USA. [Romanchock, Charles M.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. [Looy, Cynthia V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Looy, Cynthia V.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. [Hotton, Carol L.; Dimichele, William A.; Chaney, Dan S.] NMNH Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Hotton, Carol L.] NIH, Natl Ctr Biotechnol Informat, Natl Lib Med, Bethesda, MD 20892 USA. RP Tabor, NJ (reprint author), Huffington Dept Earth Sci, POB 750395, Dallas, TX 75275 USA. EM ntabor@smu.edu FU Intramural NIH HHS [Z99 LM999999] NR 120 TC 8 Z9 8 U1 0 U2 2 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-357-8 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2013 VL 376 BP 201 EP 234 DI 10.1144/SP376.14 PG 34 WC Geology; Paleontology SC Geology; Paleontology GA BB3VR UT WOS:000343084000010 PM 25339793 ER PT S AU Bayona, G Cardona, A Jaramillo, C Mora, A Montes, C Caballero, V Mahecha, H Lamus, F Montenegro, O Jimenez, G Mesa, A Valencia, V AF Bayona, German Cardona, Agustin Jaramillo, Carlos Mora, Andres Montes, Camilo Caballero, Victor Mahecha, Hernando Lamus, Felipe Montenegro, Omar Jimenez, Giovanny Mesa, Andres Valencia, Victor BE Nemcok, M Mora, A Cosgrove, JW TI Onset of fault reactivation in the Eastern Cordillera of Colombia and proximal Llanos Basin; response to Caribbean-South American convergence in early Palaeogene time SO THICK-SKIN-DOMINATED OROGENS: FROM INITIAL INVERSION TO FULL ACCRETION SE Geological Society Special Publication LA English DT Article; Book Chapter ID MIDDLE MAGDALENA VALLEY; FORELAND-BASIN; NORTHERN ANDES; STRATIGRAPHIC MODEL; TECTONIC HISTORY; UNITED-STATES; ILANOS BASIN; DEFORMATION; EVOLUTION; EXHUMATION AB The inversion of Mesozoic extensional structures in the Northern Andes has controlled the location of syn-orogenic successions and the dispersal of detritus since latest Maastrichtian time. Our results are supported by detailed geological mapping, integrated provenance (petrography, heavy minerals, geochronology) analysis and chronostratigraphical correlation (palynological and geochronology data) of 13 areas with Palaeogene strata across the central segment of the Eastern Cordillera. Spatial and temporal variation of sedimentation rates and provenance data indicate that mechanisms driving the location of marginal and intraplate uplifts and tectonic subsidence vary among syn-orogenic depocentres. In the late Maastrichtian-mid-Palaeocene time, crustal tilting of the Central Cordillera favoured reverse reactivation of the western border of the former extensional Cretaceous basin. The hanging wall of the reactivated fault separated two depocentres: a western depocentre (in the Magdalena Valley) and an eastern depocentre (presently along the axial zone of the Eastern Cordillera, Llanos foothills and Llanos Basin). In late Palaeocene-early Eocene time, as eastern subduction of the Caribbean Plate and intraplate magmatics advanced eastwards, reactivation of older structures migrated eastwards up to the Llanos Basin and disrupted the eastern depocentre. In early Eocene time, these three depocentres were separated by two low-amplitude uplifts that exposed dominantly Cretaceous sedimentary cover. Synorogenic detrital sediments supplied from the eastwards-tilted Central Cordillera reached areas of the axial domain of the Eastern Cordillera, whereas unstable metamorphic and sedimentary fragments recorded in the easternmost depocentre were supplied by basement-cored uplifts with Cretaceous and Palaeozoic sedimentary cover reported in the southern Llanos Basin. This tectonic configuration of low-amplitude uplifts separating intraplate syn-orogenic depocentres and intraplate magmatic activity in Palaeocene time was primary controlled by subduction of the Caribbean Plate. C1 [Bayona, German; Cardona, Agustin; Jaramillo, Carlos; Montes, Camilo; Mahecha, Hernando; Lamus, Felipe; Montenegro, Omar; Jimenez, Giovanny] Corp Geol ARES, Bogota, Colombia. [Cardona, Agustin] Univ Nacl Colombia, Medellin, Colombia. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Ciudad De Panama, Panama. [Mora, Andres; Caballero, Victor] Inst Colombiano Petr, Bucaramanga, Colombia. [Montes, Camilo] Univ Los Andes, Bogota, Colombia. [Mesa, Andres] Hocol SA, Bogota, Colombia. [Valencia, Victor] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA. RP Bayona, G (reprint author), Corp Geol ARES, Calle 44A,53-96, Bogota, Colombia. EM gbayona@cgares.org OI Caballero, Victor/0000-0002-8403-3883; Montes, Camilo/0000-0002-3553-0787 NR 91 TC 11 Z9 11 U1 0 U2 1 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND SN 0305-8719 BN 978-1-86239-358-5 J9 GEOL SOC SPEC PUBL JI Geol. Soc. Spec. Publ. PY 2013 VL 377 BP 285 EP 314 DI 10.1144/SP377.5 PG 30 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BB3UJ UT WOS:000343054600013 ER PT B AU Sanjek, D AF Sanjek, David BE Carr, P TI Zappa and the Freaks: Recording Wild Man Fischer SO FRANK ZAPPA AND THE AND SE Ashgate Popular and Folk Music Series LA English DT Article; Book Chapter C1 [Sanjek, David] Univ Salford, Salford M5 4WT, Lancs, England. [Sanjek, David] Natl Acad Recording Arts & Sci, Lib Congress, Santa Monica, CA USA. [Sanjek, David] Smithsonian, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASHGATE PUBLISHING LTD PI ALDERSHOT PA GOWER HOUSE, CROFT ROAD, ALDERSHOT GU11 3HR, ENGLAND BN 978-1-4094-3338-5; 978-1-4094-3337-8 J9 ASHG POP FOLK MUSIC PY 2013 BP 149 EP 165 PG 17 WC Music SC Music GA BA8TY UT WOS:000338686700011 ER PT S AU Zusi, RL AF Zusi, Richard L. BA Zusi, RL BF Zusi, RL TI INTRODUCTION TO THE SKELETON OF HUMMINGBIRDS (AVES: APODIFORMES, TROCHILIDAE) IN FUNCTIONAL AND PHYLOGENETIC CONTEXTS SO INTRODUCTION TO THE SKELETON OF HUMMINGBIRDS (AVES: APODIFORMES, TROCHILIDAE) IN FUNCTIONAL AND PHYLOGENETIC CONTEXTS SE Ornithological Monographs LA English DT Article; Book Chapter DE Trochilidae; Apodiformes; comparative osteology; myology; inter- and intraspecific variation; nectarivory; hovering; Eurotrochilus ID DNA HYBRIDIZATION EVIDENCE; HERMIT RAMPHODON-NAEVIUS; OLD-WORLD HUMMINGBIRD; NECTAR-FEEDING BIRDS; SWIFT-LIKE BIRD; HOVERING HUMMINGBIRD; TROPICAL HUMMINGBIRD; ECOLOGICAL CAUSATION; SEXUAL-DIMORPHISM; FLAPPING FLIGHT AB Historically, comparative study of the skeleton of hummingbirds has focused on systematics, emphasizing differences between hummingbirds and other birds and only rarely addressing differences within Trochilidae. This monograph covers both approaches, and comparisons within Trochilidae are framed within recently published, plausible phylogenetic hypotheses. The data are derived mainly from museum collections of anatomical specimens, covering similar to 256 species of 102 genera of hummingbirds, and 11 genera of other Apodiformes. Although the syringeal skeleton is included, emphasis is on the axial and appendicular skeletons. The first section deals with the syrinx and with skeletal features mainly associated with nectarivory and hovering, emphasizing characters that are unique to hummingbirds within Apodiformes. The syrinx of hummingbirds lies in the neck rather than the thorax and displays a unique bony knob on the surface of the tympanic membrane. During posthatching development, the upper jaw of hummingbirds undergoes metamorphic changes that produce a morphology uniquely adapted for nectarivory within Ayes. The ventral bars of the upper jaw lengthen and rotate to become lateral walls of an incompletely tubular bill that is completed by the closed mandibula, and lateral bowing (streptognathism) of the mandibula helps to seal the tube while a bird drinks nectar. Streptognathism of the opened jaw is used in display by some Hermits. The lamellar tip of the tongue required for nectar uptake also develops after fledging, while young are still fed by the parent. In Trochilines the nasal region changes from its configuration by bone resorption during posthatching development. Cranial kinesis in hummingbirds is poorly documented, but structural differences in the upper jaw of Hermits and Trochilines imply differences in cranial kinesis. The palatum of hummingbirds is distinguished from that of other apodiforms by extreme reduction of the lateral part of the palatinum, greater width of the ventral choanal region, and by a median spine on the vomer. Otherwise the vomer is variable in shape and not compatible with aegithognathism. Among cranial features, the basipterygoid process, lacrimale, and jugale are absent, and the interorbital septum is complete. The hyobranchial apparatus differs from that of other apodiforms in having an epibranchiale that is longer than the ceratobranchiale, and variably elongate in relation to body size. I hypothesize two modes of hyobranchial function-one applicable to moderate protrusion of the tongue (typical nectar eating), and another to extreme protrusion. The pelvis is less strongly supported by the synsacrum, and the proximal portion of the hind limb is more reduced than in other Apodiformes. By contrast, the tarsometatarsus and flexor muscles of the toes are well developed in association with perching and clinging. In the flight mechanism, features uniquely pertinent to hovering are distinguished from those that support stiff-winged flight-the latter common to both swifts and hummingbirds. Hovering is especially dependent on adaptations for axial rotation of the wing at all major joints, and on extreme development in hummingbirds of the unusual wing proportions (short humerus and forearm, and long hand) and enlarged breast muscles found in swifts. Osteological characters of the Oligocene fossil Eurotrochilus that can be compared with modern hummingbirds do not indicate nectarivory or sustained hovering in that taxon. In the second section, variations within Trochilidae are described and their distributions within the major clades (Hermits, Topazes, Mangoes, Brilliants, Coquettes, Patagona, Mountain Gems, Bees, and Emeralds) are specified. Most diverse are the jaw mechanism, nasal region and conchae, hyobranchial apparatus, cranial proportions, crests, and pneumatic inflation, structure of the ribcage based on number of ribs attached to the sternum, pectoral girdle, and various humeral characters. Other noteworthy but largely unexplained variation characterizes the hyobranchial apparatus of Heliodoxa, the humerus of the "Pygmornis group" of Phaethornis, sexual dimorphism in numbers of thoracic ribs, and synostosis of phalanges of the foot. Although Hermits display distinctive characters, their subfamily status is uncertain for lack of informative outgroups. Major trochilid clades are either weakly supported or unsupported by uniquely derived characters, but apomorphic variation within Mangoes suggests recognition of an Anthracothorax group of genera, and within Emeralds, a large Amazilia group. Each of the major trochilid clades displays considerable diversity in body size and skeletal characters, and numerous characters show parallel evolution within the family. Intraspecific variation is widespread, and selected examples are highlighted. Patterns of skeletal variations at multiple levels of phylogerty suggest that some variations characterizing higher levels had their origins at the intraspecific level. A list of unsolved problems of functional morphology of the skeleton in hummingbirds is offered. Especially intriguing are the many posthatchirtg changes in development of the feeding mechanism and the challenge of incorporating morphological data and their implications into models of evolution of hummingbird communities. Received 17 September 2012, accepted 8 February 2013. C1 [Zusi, Richard L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. RP Zusi, RL (reprint author), 802 NE 62nd Ave,Apt F, Hillsboro, OR 97124 USA. EM zusirl@yahoo.com NR 221 TC 5 Z9 5 U1 8 U2 26 PU AMER ORNITHOLOGISTS UNION PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY, WASHINGTON, DC 20560 USA SN 0078-6594 BN 978-0-943610-96-2 J9 ORNITHOL MONOGR JI Ornithol. Monogr. PY 2013 IS 77 BP 1 EP 94 DI 10.1525/om.2013.77.1.1 PG 94 WC Ornithology SC Zoology GA BA8OP UT WOS:000338385600001 ER PT J AU Pastorini, J Janaka, HK Nishantha, HG Prasad, T Leimgruber, P Fernando, P AF Pastorini, Jennifer Janaka, H. K. Nishantha, H. G. Prasad, Tharaka Leimgruber, Peter Fernando, Prithiviraj TI A preliminary study on the impact of changing shifting cultivation practices on dry season forage for Asian elephants in Sri Lanka SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE Asian elephant; Elephas maximus; shifting cultivation; succession; pioneer species ID AGRICULTURE; ECOLOGY AB Shifting cultivation, in which fields are traditionally cultivated for two or three consecutive years and left fallow for four to five years, is an ancient practice still prevalent in the dry zone of Sri Lanka. Traditionally, shifting agriculture is rain dependent and is limited to the wet season. However, traditional patterns are now changing due to population pressures. We assessed the use of shifting agriculture areas by Asian elephants (Elephas maximus) and the availability of fodder in active fields during the dry season, to evaluate the impact of changing cultivation practices on elephants. We radio-tracked a juvenile and an adult male, representative of the two social groupings of herds and adult males respectively, based on the sexually dimorphic social structure of elephants. Although the small sample size precluded definitive conclusions, the tracking data were consistent with extensive elephant use of shifting cultivation areas during the dry season. We conducted line transects and plots in fields cultivated continuously for 1-20 years, assessing the growth of grasses and four browse species selected as indicators of elephant food. Grass was plentiful in early dry season, representing an important but transient food source. Browse density and volume remained constant through the dry season. Browse density but not volume decreased with increasing number of consecutive years of cultivation. We conclude that shifting agriculture fields under active cultivation are a significant dry season food source for elephants. This benefit is likely to decrease with additional years of continued cultivation and/or longer cultivation seasons. C1 [Pastorini, Jennifer; Janaka, H. K.; Nishantha, H. G.; Fernando, Prithiviraj] Ctr Conservat & Res, Rajagiriya, Sri Lanka. [Pastorini, Jennifer] Univ Zurich, Inst Anthropol, CH-8057 Zurich, Switzerland. [Prasad, Tharaka] Dept Wildlife Conservat, Battaramulla, Sri Lanka. [Leimgruber, Peter] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Pastorini, J (reprint author), Ctr Conservat & Res, 35 Gunasekara Gardens,Nawala Rd, Rajagiriya, Sri Lanka. EM jenny@aim.uzh.ch RI Pastorini, Jennifer/A-9959-2012 OI Pastorini, Jennifer/0000-0001-5883-0208 FU U.S. Fish and Wildlife Service Asian Elephant Conservation; Friends of the National Zoo (FONZ) FX We are grateful to L.K.A. Jayasinghe, M. Gunawardena, Chaminda, Roshan and Prasanga for helping with the fieldwork. We are thankful to the team of the Department of Wildlife Conservation Sri Lanka for collaring the elephants. Financial support from U.S. Fish and Wildlife Service Asian Elephant Conservation Fund, and Friends of the National Zoo (FONZ) is gratefully acknowledged. NR 17 TC 0 Z9 0 U1 0 U2 5 PU TROPICAL CONSERVATION SCIENCE PI MENLO PARK PA PO BOX 0291, MENLO PARK, CA 94026-0291 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PY 2013 VL 6 IS 6 BP 770 EP 780 PG 11 WC Biodiversity Conservation SC Biodiversity & Conservation GA AK7YM UT WOS:000338643800006 ER PT B AU Ropret, P Legan, L Rosi, F Miliani, C AF Ropret, P. Legan, L. Rosi, F. Miliani, C. BE RogerioCandelera, MA Lazzari, M Cano, E TI A novel approach for micro FTIR reflection absorption analysis of artworks' surface SO SCIENCE AND TECHNOLOGY FOR THE CONSERVATION OF CULTURAL HERITAGE LA English DT Proceedings Paper CT International Congress on Science and Technology for the Conservation of Cultural Heritage CY OCT 02-05, 2012 CL Santiago de Compostela, SPAIN SP Univ Santiago de Compostela AB Non invasive reflection FTIR measurements provide valuable information about the chemical composition and degradation processes taking place at the surface of works of art. However, band assignments and the identification of components can often be complicated by the fact that the IR reflection response of artworks' surface is rather complex. In order to overcome this problem, a novel approach of mu-transflection analysis of artworks' surface is proposed. The obtained transflection spectra are very similar to the transmission ones, offering an easier interpretation. Although micro sampling is required, the sample removal leaves barely visible traces. In addition to the identification of the components present at the surface of the work of art, the technique can also be applied for monitoring of the chemical cleaning. Some examples of the identification of the surface of a Baroque easel painting are presented. C1 [Ropret, P.] Inst Protect Cultural Heritage Slovenia, Ljubljana, Slovenia. [Legan, L.] Smithsonian Inst, Museum Conservat Inst, Suitland, ME USA. [Rosi, F.; Miliani, C.] Univ Perugia, CNR ISTM, I-06100 Perugia, Italy. [Rosi, F.; Miliani, C.] Univ Perugia, SMAArt Dipartimento Chim, I-06100 Perugia, Italy. RP Ropret, P (reprint author), Inst Protect Cultural Heritage Slovenia, Ljubljana, Slovenia. RI Miliani, Costanza/O-2888-2015; Rosi, Francesca/P-5396-2015 OI Miliani, Costanza/0000-0001-6091-9922; Rosi, Francesca/0000-0002-1518-4784 NR 10 TC 0 Z9 0 U1 1 U2 4 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA BN 978-0-203-50801-5; 978-1-138-00009-4 PY 2013 BP 189 EP 192 PG 4 WC Cultural Studies; Environmental Studies; Multidisciplinary Sciences SC Cultural Studies; Environmental Sciences & Ecology; Science & Technology - Other Topics GA BA8LH UT WOS:000338265800044 ER PT J AU Diazgranados, M Sanchez, LR AF Diazgranados, Mauricio Roberto Sanchez, Luis TI A new species of Espeletiopsis (Millerieae, Asteraceae) from Colombia SO PHYTOKEYS LA English DT Article AB A new species of Espeletiopsis was found in two small paramos of Norte de Santander, Colombia. The species is named Erpeletiopsis diazii honoring the contributions of Santiago Diaz-Piedrahita in recognition of his vast knowledge of the Compositae in Colombia. This is a very distinctive species, markedly different from most of the Espeletiopsis present in Colombia. The new species is closely related to Espeletiopsis caldasii and E. santanderensis, but differs in having (1)4-6(-7) capitula, with very short peduncles, and capitula arranged in a compact or densely glomerate cyme. With a total distribution area of less than 75 km2, this species is probably critically endangered or imperiled. RP Diazgranados, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM espeletias@gmail.com NR 34 TC 2 Z9 2 U1 0 U2 0 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 32 BP 37 EP 48 DI 10.3897/phytokeys.32.6387 PG 12 WC Plant Sciences SC Plant Sciences GA AC1PX UT WOS:000332269600003 ER PT J AU Wagner, WL Wagner, AJ Lorence, DH AF Wagner, Warren L. Wagner, Anthony J. Lorence, David H. TI Revision of Cyrtandra (Gesneriaceae) in the Marquesas Islands SO PHYTOKEYS LA English DT Article AB During the preparation of the Vascular Flora of the Marquesas Islands three new species of Cyrtandra (Gesneriaceae) have come to light and are described herein: C. uapouensis W. L. Wagner & Lorence, C. uahukaensis W. L. Wagner & Lorence, and C. kenwoodii W. L. Wagner & A. J. Wagner. Amended descriptions of the eight previously described Marquesan species are also provided as well as a key to the species. With the description of these the new species Cyrtandra in the Marquesas Islands consists of 11 species, six of which have been included in recent molecular phylogenetic studies of Pacific Cyrtandra, and appear to have arisen from one original introduction. If the other five species are members of this Marquesas clade then Cyrtandra would represent the largest lineage of Marquesas vascular plants. Psychotria is largest genus in the Marquesas Islands with 13 species, but is thought to consist of three separate lineages. RP Wagner, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, POB 37012, Washington, DC 20013 USA. EM wagnerw@si.edu NR 15 TC 1 Z9 1 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 30 BP 33 EP 64 DI 10.3897/phytokeys.30.6147 PG 32 WC Plant Sciences SC Plant Sciences GA 284RK UT WOS:000329337800003 ER PT J AU Funk, VA Robinson, H Tangerini, AR AF Funk, Vicki A. Robinson, Harold Tangerini, Alice R. TI Whatever happened to Bishopanthus (Compositae, Liabeae)? SO PHYTOKEYS LA English DT Article ID GENUS; ANDES AB The enigmatic monospecific Bishopanthus of the tribe Liabeae (Compostiae/Asteraceae) has never been fully understood. It has not been possible to examine it in detail since it was described, because most of the type material was destroyed shortly after it arrived at the US National Herbarium, the morphology is insufficient to assign it to a subtribe, and the small amount of leaf material that remains is unsuitable for DNA extraction. A detailed description in English, image of the type specimen, photograph, and original illustration are included along with an estimation of where it was collected in the hopes that this information will encourage other field botanists who collect in northern Peru to search for it. RP Funk, VA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, POB 37012, Washington, DC 20013 USA. EM funkv@si.edu NR 10 TC 0 Z9 0 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 30 BP 65 EP 73 DI 10.3897/phytokeys.30.6652 PG 9 WC Plant Sciences SC Plant Sciences GA 284RK UT WOS:000329337800004 ER PT J AU Tornabene, MW Wagner, WL AF Tornabene, Michael W. Wagner, Warren L. TI New combinations for Pacific endemic species: Marquesan Poaceae, and Micronesian Myrtaceae SO PHYTOKEYS LA English DT Article ID SYZYGIUM AB As part of the preparation for a comprehensive online flora of Pacific oceanic islands, numerous taxonomic changes have been necessary, primarily due to a new wealth of global molecular phylogenetic studies on genera that include Pacific islands species. In order to compile an accurate checklist of the Pacific island flora with up-to-date taxonomies, we are moving several species to their currently accepted genera. Two Marquesan Pennisetum Rich, are transferred to Cenchrus L. with the new combinations Cenchrus articularis (Trin.) M. Tornabene & W.L. Wagner, and Cenchrus henryanus (F. Br.) M. Tornabene & W.L. Wagner. A key to Marquesas Cenchrus is also provided to differentiate the two species. Additionally, one species of Eugenia L. is transferred to Syzygium Gaertn. with the new combination Syzygium stelechanthoides (Kaneh.) M. Tornabene & W.L. Wagner in accord with the aforementioned studies. RP Wagner, WL (reprint author), Smithsonian Inst, Dept Bot, MRC-166,POB 37012, Washington, DC 20013 USA. EM wagnerw@si.edu NR 12 TC 0 Z9 0 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 28 BP 1 EP 7 DI 10.3897/phytokeys.28.6139 PG 7 WC Plant Sciences SC Plant Sciences GA 273JG UT WOS:000328530500001 ER PT J AU Diazgranados, M Morillo, G AF Diazgranados, Mauricio Morillo, Gilberto TI A new species of Coespeletia (Asteraceae, Millerieae) from Venezuela SO PHYTOKEYS LA English DT Article AB A new species of Coespeletia from the paramos of Merida (Venezuela) is described here. This species, named Coespeletia palustris, is found in a few marshy areas of the paramo. It is closely related to C. moritziana, but differs from it in a smaller number of florets in the capitula, larger ray flowers with longer ligulae and longer linguiform appendages, smaller pollen grains, larger cypselae, ebracteate scapes, leaves and inflorescences with more whitish indumentum, larger leaf sheaths, and marshy habitat. RP Diazgranados, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM espeletias@gmail.com NR 4 TC 2 Z9 2 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 28 BP 9 EP 18 DI 10.3897/phytokeys.28.6378 PG 10 WC Plant Sciences SC Plant Sciences GA 273JG UT WOS:000328530500002 ER PT J AU Wagner, WL Krakos, KN Hoch, PC AF Wagner, Warren L. Krakos, Kyra N. Hoch, Peter C. TI Taxonomic changes in Oenothera sections Gaura and Calylophus (Onagraceae) SO PHYTOKEYS LA English DT Article ID SEQUENCE DATA AB The long-recognized genus Gaura was shown recently to be deeply nested within one of two major clades of Oenothera. New molecular data indicate further taxonomic changes are necessary in Oenothera sect. Gaura. We make these changes here, including three new combinations, in advance of the Onagraceae treatment for the Flora of North America. The new phylogenetic studies show that several pairs of taxa treated as subspecies in the most recent revision by Raven and Gregory (1972) had independent origins within sect. Gaura, and are here elevated to species level (Oenothera nealleyi for Gaura suffulta subsp. nealleyi; Oenothera dodgeniana for Gaura neomexicana subsp. neomexicana; and Oenothera podocarpa for Gaura hexandra subsp. gracilis). Also, a nomenclatural problem in Oenothera sect. Calylophus is corrected by adopting the name Oenothera capillifolia Scheele for the species known previously, and nomenclaturally correct, as Calylophus berlandieri Spach. This problem necessitates a new combination Oenothera capillifolia subsp. berlandieri. RP Wagner, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM wagnerw@si.edu NR 11 TC 1 Z9 1 U1 1 U2 7 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 28 BP 61 EP 72 DI 10.3897/phytokeys.28.6143 PG 12 WC Plant Sciences SC Plant Sciences GA 273JG UT WOS:000328530500004 ER PT J AU Diazgranados, M Funk, VA AF Diazgranados, Mauricio Funk, Vicki A. TI Utility of QR codes in biological collections SO PHYTOKEYS LA English DT Article AB The popularity of QR codes for encoding information such as Urns has increased exponentially in step with the technological advances and availability of smartphones, digital tablets, and other electronic devices. We propose using QR codes on specimens in biological collections to facilitate linking vouchers' electronic information with their associated collections. QR codes can efficiently provide such links for connecting collections, photographs, maps, ecosystem notes, citations, and even GenBank sequences. QR codes have numerous advantages over barcodes, including their small size, superior security mechanisms, increased complexity and quantity of information, and low implementation cost. The scope of this paper is to initiate an academic discussion about using QR codes on specimens in biological collections. RP Diazgranados, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM DiazgranadosM@si.edu NR 20 TC 4 Z9 4 U1 2 U2 8 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 25 BP 21 EP 34 DI 10.3897/phytokeys.25.5175 PG 14 WC Plant Sciences SC Plant Sciences GA 229DW UT WOS:000325243000003 ER PT J AU Robinson, H Skvarla, JJ AF Robinson, Harold Skvarla, John J. TI Lettowia, a new genus of Vernonieae from East Africa (Asteraceae) SO PHYTOKEYS LA English DT Article AB A new genus, Lettowia H. Rob. & Skvarla is named for the single East African species originally described. as Vernonia nyassae Oliv. Its pollen is lophate and triporate, with a perforated tectum restricted to the muri. The new genus is placed near Vernoniastrum in the subtribe Erlangeinae. RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu NR 11 TC 2 Z9 2 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 25 BP 47 EP 53 DI 10.3897/phytokeys.25.5556 PG 7 WC Plant Sciences SC Plant Sciences GA 229DW UT WOS:000325243000005 ER PT J AU Feuillet, C AF Feuillet, Christian TI The typification of Cordia flavescens Aubl., the transfer of Firensia Scop. from Cordia L. (Cordiaceae, Boraginales) to the synonymy of Ocotea Aubl. (Lauraceae), and the identity of the species of Firensia SO PHYTOKEYS LA English DT Article AB Firensia Scop. was based on Cordia flavescens Aubl., a species described and illustrated from a mixed collection that Scopoli never transferred to Firensia. The genus included three additional species formally named by Rafinesque. Currently the four species are placed in three different families and none retained the epithet accepted by Scopoli or given by Rafinesque for reason of priority. A lectotype is designated for Cordia flavescens that places Firensia in the synonymy of Ocotea (Lauraceae). RP Feuillet, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM feuillec@si.edu NR 18 TC 1 Z9 1 U1 1 U2 4 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 23 BP 19 EP 24 DI 10.3897/phytokeys.23.4827 PG 6 WC Plant Sciences SC Plant Sciences GA 178YK UT WOS:000321483100002 ER PT J AU Wen, J Kiapranis, R Lovave, M AF Wen, Jun Kiapranis, Robert Lovave, Michael TI Ampelocissus asekii J.Wen, R. Kiapranis & M. Lovave, a new species of Vitaceae from Papua New Guinea SO PHYTOKEYS LA English DT Article AB A new species Ampelocissus asekii J.Wen, R.Kiapranis & M.Lovave of Vitaceae is described from Morobe Province of Papua New Guinea. It is a close relative of A. muelleriana Planch., another endemic of New Guinea and differs from the latter by its densely woolly tomentose lower leaflet surface and much thicker leaflets. The new species is from the mid montane forests, whereas A. muelleriana occurs in the lowland rain forests. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu NR 5 TC 0 Z9 0 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1314-2011 EI 1314-2003 J9 PHYTOKEYS JI PhytoKeys PY 2013 VL 21 BP 1 EP 6 DI 10.3897/phytokeys.21.4512 PG 6 WC Plant Sciences SC Plant Sciences GA 172DI UT WOS:000320979800001 ER PT J AU Mozdzer, TJ Brisson, J Hazelton, ELG AF Mozdzer, Thomas J. Brisson, Jacques Hazelton, Eric L. G. TI Physiological ecology and functional traits of North American native and Eurasian introduced Phragmites australis lineages SO AOB PLANTS LA English DT Article DE Conspecific; global change; invasive; nitrogen; nitrogen productivity; phenotypic plasticity; relative growth rate; specific leaf area; wetland ID CLONE-SPECIFIC DIFFERENCES; BRACKISH TIDAL MARSH; COMMON REED; CHESAPEAKE BAY; PLANT INVASION; PHENOTYPIC PLASTICITY; NITROGEN ASSIMILATION; GENETIC-VARIATION; CRYPTIC INVASION; SALT MARSHES AB Physiological ecology and plant functional traits are often used to explain plant invasion. To gain a better understanding of how traits influence invasion, studies usually compare the invasive plant to a native congener, but there are few conspecific examples in the literature. In North America, the presence of native and introduced genetic lineages of the common reed, Phragmites australis, presents a unique example to evaluate how traits influence plant invasion. We reviewed the literature on functional traits of P. australis lineages in North America, specifically contrasting lineages present on the Atlantic Coast. We focused on differences in physiology between the lineage introduced from Eurasia and the lineage native to North America, specifically seeking to identify the causes underlying the recent expansion of the introduced lineage. Our goals were to better understand which traits may confer invasiveness, provide predictions of how these lineages may respond to interspecific competition or imminent global change, and provide guidance for future research. We reviewed published studies and articles in press, and conducted personal communications with appropriate researchers and managers to develop a comparative dataset. We compared the native and introduced lineages and focused on plant physiological ecology and functional traits. Under both stressful and favourable conditions, our review showed that introduced P. australis consistently exhibited greater ramet density, height and biomass, higher and more plastic relative growth rate, nitrogen productivity and specific leaf area, higher mass specific nitrogen uptake rates, as well as greater phenotypic plasticity compared with the native lineage. We suggest that eco-physiological and other plant functional traits elucidate potential-mechanisms for the introduced lineage's invasiveness under current and predicted global change conditions. However, our review identified a disconnect between field surveys, experiments, natural competition and plant ecophysiology that must be addressed in future field studies. Given the likelihood of hybridization between lineages, a better understanding of plant traits in native, non-native and hybrid lineages is needed to manage current invasions and to predict the outcome of interactions among novel genotypes. Comparative physiology and other plant functional traits may provide additional tools to predict the trajectory of current and potential future invasions. C1 [Mozdzer, Thomas J.] Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. [Brisson, Jacques] Univ Montreal, Inst Rech Biol Vegetale, Dept Sci Biol, Montreal, PQ H1X 2B2, Canada. [Hazelton, Eric L. G.] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Hazelton, Eric L. G.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA. [Hazelton, Eric L. G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Mozdzer, TJ (reprint author), Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. EM tmozdzer@brynmawr.edu OI Mozdzer, Thomas/0000-0002-1053-0967 FU AoB PLANTS; MD Sea Grant [SA7528114-WW]; NSF [DEB-0950080]; NOAA [NA09NO S4780214]; Smithsonian Predoctoral Fellowship; Utah State University Ecology Center; Society of Wetland Scientists; Delta Waterfowl FX This manuscript is an outcome of a Phragmites symposium at the 2011 meeting of the Society of Wetland Scientists with travel funding provided by AoB PLANTS to both T.J.M. and E.L.G.H. Funding support for T.J.M. was provided from MD Sea Grant Award SA7528114-WW and NSF DEB-0950080. E.L.G.H. was funded by NOAA NA09NO S4780214, a Smithsonian Predoctoral Fellowship, Utah State University Ecology Center, the Society of Wetland Scientists and Delta Waterfowl. NR 80 TC 15 Z9 15 U1 8 U2 51 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 2041-2851 J9 AOB PLANTS JI Aob Plants PY 2013 VL 5 AR plt048 DI 10.1093/aobpla/plt048 PG 14 WC Plant Sciences SC Plant Sciences GA AJ2LQ UT WOS:000337487800001 ER PT J AU Karlstrom, PJ AF Karlstrom, Paul J. TI PHENOMENAL: CALIFORNIA LIGHT, SPACE, AND SURFACE SO CALIFORNIA HISTORY LA English DT Book Review C1 [Karlstrom, Paul J.] Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. RP Karlstrom, PJ (reprint author), Smithsonian Inst, Archives Amer Art, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU CALIFORNIA HISTORICAL SOC PI SAN FRANCISCO PA 678 MISSION ST, SAN FRANCISCO, CA 94105-4014 USA SN 0162-2897 J9 CALIF HIST JI Calif. Hist. PY 2013 VL 90 IS 2 BP 78 EP 82 PG 5 WC History SC History GA AI4WO UT WOS:000336865700006 ER PT S AU Blakeslee, AMH Fowler, AE Keogh, CL AF Blakeslee, April M. H. Fowler, Amy E. Keogh, Carolyn L. BE Lesser, M TI Marine Invasions and Parasite Escape: Updates and New Perspectives SO ADVANCES IN MARINE BIOLOGY, VOL 66 SE Advances in Marine Biology LA English DT Review; Book Chapter DE Marine; Invasion; Biogeography; Parasite; Trematode; Parasite escape; Enemy release; Introduction vector ID ENEMY RELEASE HYPOTHESIS; HETEROSACCUS-DOLLFUSI BOSCHMA; CLAM RUDITAPES-PHILIPPINARUM; CHARYBDIS-LONGICOLLIS LEENE; BIRD FINAL HOSTS; RED KING CRAB; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; CRASSOSTREA-GIGAS; CARCINUS-MAENAS AB Marine invasions have risen over time with enhanced globalization, and so has the introduction of non-native hosts and their parasites. An important and well-supported paradigm of invasion biology is the significant loss of parasites that hosts enjoy in introduced regions compared to native regions (i.e. parasite escape), yet less is known about the factors that influence parasite escape in marine systems. Here, we compile an up-to-date review of marine parasite invasions and test several hypotheses related to host invasion pathway that we suspected could influence parasite escape across the 31 host parasite systems included in our investigation. In general, we continued to show significant support for parasite escape; however, escape varied among parasite taxa, with most taxa demonstrating moderate levels of escape and a few showing complete or no escape. Moreover, we revealed several important factors related to host taxa, geography, time, and vector of introduction that influenced parasite escape, and in some cases demonstrated significant interactions, revealing the complexity of the invasion pathway in filtering parasites from native to introduced regions. In some (but not all) cases, there was also evidence of invasive host advantages due to parasite escape, but more evidence is required to demonstrate clear support for the enemy release hypothesis. In general, our study revealed the need for further research across systems, especially in understudied regions of the world. C1 [Blakeslee, April M. H.] Long Isl Univ Post, Dept Biol, Brookville, NY 11548 USA. [Blakeslee, April M. H.; Fowler, Amy E.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Fowler, Amy E.] Marine Resources Res Inst, South Carolina Dept Nat Resources, Charleston, SC 29412 USA. [Keogh, Carolyn L.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. RP Blakeslee, AMH (reprint author), Long Isl Univ Post, Dept Biol, Brookville, NY 11548 USA. EM april.blakeslee@liu.edu NR 163 TC 10 Z9 10 U1 1 U2 47 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 0065-2881 BN 978-0-12-408096-6 J9 ADV MAR BIOL JI Adv. Mar. Biol. PY 2013 VL 66 BP 87 EP 169 DI 10.1016/B978-0-12-408096-6.00002-X PG 83 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA BA1FJ UT WOS:000332424000002 PM 24182900 ER PT B AU Huber, BT Buzas, MA Drew, A Jett, JA AF Huber, Brian T. Buzas, Martin A. Drew, Alice Jett, Jennifer A. BE Bowden, AJ Gregory, FJ Henderson, AS TI History of foraminiferal collections at the Smithsonian Institution SO LANDMARKS IN FORAMINIFERAL MICROPALAEONTOLOGY: HISTORY AND DEVELOPMENT SE Micropaleaeontological Society Special Publications LA English DT Article; Book Chapter ID PLANKTONIC FORAMINIFERA; ATLANTIC AB The Smithsonian Institution's foraminiferal collections, collectively identified as the Cushman Collection, consist of nearly 17 000 primary type slides, more than 240 000 secondary type and identified slides and thousands of bulk samples and washed residue samples from important type localities, stratigraphic sections and land-based and deep-sea boreholes. The collection grew slowly from its beginning in the late 1800s, but acquisition of Joseph A. Cushman's entire research collection in 1950 dramatically increased its size and international prominence. Following Cushman's gift, the collection grew over three times larger during the late twentieth century as additional foraminiferal slides and samples were added. Biographical profiles are presented here for key research scientists who were particularly influential in the collection's growth and/ or curation at the Smithsonian Institution. These researchers include T. Wayland Vaughan, Joseph A. Cushman, Lloyd G. Henbest, Ruth Todd, Alfred R. Loeblich Jr, Thomas Gibson and Raymond C. Douglass. C1 [Huber, Brian T.; Buzas, Martin A.; Drew, Alice; Jett, Jennifer A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Huber, BT (reprint author), Smithsonian Inst, Dept Paleobiol, MRC-121, Washington, DC 20560 USA. EM huberb@si.edu NR 23 TC 2 Z9 2 U1 0 U2 0 PU GEOLOGICAL SOC PUBLISHING HOUSE PI BATH PA UNIT 7, BRASSMILL ENTERPRISE CTR, BRASSMILL LANE, BATH BA1 3JN, AVON, ENGLAND BN 978-1-86239-371-4 J9 MICROPALEAEONTOLOGIC PY 2013 BP 71 EP 83 PG 13 WC Geology; Microbiology; Paleontology SC Geology; Microbiology; Paleontology GA BA1FL UT WOS:000332424200008 ER PT B AU Noyes, RW AF Noyes, R. W. BE Jain, K Tripathy, SC Hill, F Leibacher, JW Pevtsov, AA TI Robert Leighton and the Dawn of Helioseismology SO FIFTY YEARS OF SEISMOLOGY OF THE SUN AND STARS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 27th Workshop on Fifty Years of Seismology of the Sun and Stars CY MAY 06-10, 2013 CL Tucson, AZ SP Natl Solar Observ, NSF, ESA, NISP Program ID SOLAR GRANULATION; MAGNETIC FIELDS; VELOCITY FIELDS; ATMOSPHERE AB We review the events leading up to and including the discovery in 1960 by Robert Leighton of the solar 5-minute oscillation, which may be characterized as the dawn of helioseismology. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Noyes, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnoyes@cfa.harvard.edu NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-840-4 J9 ASTR SOC P PY 2013 VL 478 BP 5 EP 18 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BA2MN UT WOS:000333656200001 ER PT B AU Korzennik, SG AF Korzennik, S. G. BE Jain, K Tripathy, SC Hill, F Leibacher, JW Pevtsov, AA TI Mode Frequencies from GONG, MDI, and HMI Data SO FIFTY YEARS OF SEISMOLOGY OF THE SUN AND STARS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 27th Workshop on Fifty Years of Seismology of the Sun and Stars CY MAY 06-10, 2013 CL Tucson, AZ SP Natl Solar Observ, NSF, ESA, NISP Program AB I present recent results from fitting all the available data from the three major helioseismic instruments: GONG, MDI and HMI using my independent methodology. This method not only fits individual singlets, but: fits them simultaneously for a given multiplet; uses an optimal multi-taper spectral estimator; includes the full leakage matrix and the effect of mode distortion by differential rotation; and fits an asymmetric mode profile. The mode fitting was carried out on time series of varying lengths (1x, 2x, 4x, 8x, 16x, 32x, 64x 72 days long), using co-eval epochs for all three instruments. By fitting time series of varying lengths, one trades off some temporal resolution for a better precision. I present these results, compare them and discuss the potential sources of the discrepancies. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skorzennik@cfa.harvard.edu NR 3 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-840-4 J9 ASTR SOC P PY 2013 VL 478 BP 137 EP 144 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BA2MN UT WOS:000333656200015 ER PT B AU Korzennik, SG Eff-Darwich, A Larson, TP Rabello-Soares, MC Schou, J AF Korzennik, S. G. Eff-Darwich, A. Larson, T. P. Rabello-Soares, M. C. Schou, J. BE Jain, K Tripathy, SC Hill, F Leibacher, JW Pevtsov, AA TI Characterization of High-Degree Modes using MDI, HMI and GONG Data SO FIFTY YEARS OF SEISMOLOGY OF THE SUN AND STARS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 27th Workshop on Fifty Years of Seismology of the Sun and Stars CY MAY 06-10, 2013 CL Tucson, AZ SP Natl Solar Observ, NSF, ESA, NISP Program AB We present the first characterization of high-degree modes (i.e., up to 900 or 1000), using three instruments and three epochs corresponding to the 2001, 2002 and 2010 MDI Dynamics runs. For 2001, we analyzed MDI full-disk Dopplergrams, while for 2002, we analyzed MDI and GONG full-disk Dopplergrams, and for 2010 we analyzed MDI, GONG and HMI full-disk Dopplergrams. These Dopplergrams were spatially decomposed up to l = 900 or 1000, and power spectra for all degrees and all azimuthal orders were computed using a high-order multi-taper, power spectrum estimator. These spectra were then fitted for all degrees and all azimuthal orders, above = 100, and for all orders with substantial amplitude. Fitting at high degrees generates ridge characteristics, characteristics that do not correspond to the underlying mode characteristics. We used a sophisticated forward modeling to recover the best possible estimate of the underlying mode characteristics (mode frequencies, as well as linewidths, amplitudes and asymmetries). We present the first attempt to apply this method to three instruments and three epochs. The derived sets of corrected mode characteristics (frequencies, line widths, asymmetries and amplitudes) are presented and compared. C1 [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rabello Soares, Maria Cristina/C-3207-2013 NR 4 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-840-4 J9 ASTR SOC P PY 2013 VL 478 BP 173 EP 178 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BA2MN UT WOS:000333656200021 ER PT B AU Munoz-Jaramillo, A Martens, PCH Nandy, D AF Munoz-Jaramillo, A. Martens, P. C. H. Nandy, D. BE Jain, K Tripathy, SC Hill, F Leibacher, JW Pevtsov, AA TI Helioseismic Perspective of the Solar Dynamo SO FIFTY YEARS OF SEISMOLOGY OF THE SUN AND STARS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 27th Workshop on Fifty Years of Seismology of the Sun and Stars CY MAY 06-10, 2013 CL Tucson, AZ SP Natl Solar Observ, NSF, ESA, NISP Program ID MAGNETIC-FLUX TUBES; CONVECTION ZONE; MERIDIONAL FLOW; DIFFERENTIAL ROTATION; CYCLE; MODEL; INTERIOR; FIELD; CIRCULATION; TRANSPORT AB Helioseismology has been, without a doubt, one of the greatest contributors to our understanding of the solar cycle. In particular, its results have been critical in the development of solar dynamo models, by providing modelers with detailed information about the internal, large scale flows of solar plasma. This review will give a historical overview of the evolution of our understanding of the solar cycle, placing special emphasis on advances driven by helioseismic results. We will discuss some of the outstanding modeling issues, and discuss how Helioseismology can help push our understanding forward during the next decade. C1 [Munoz-Jaramillo, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Munoz-Jaramillo, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amunoz@cfa.harvard.edu NR 51 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-840-4 J9 ASTR SOC P PY 2013 VL 478 BP 271 EP 282 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BA2MN UT WOS:000333656200036 ER PT S AU Li, ZH Wu, F Crofoot, MC AF Li, Zhenhui Wu, Fei Crofoot, Margaret C. BE Xiong, H Karypis, G Thuraisingham, B Cook, D Wu, X TI Mining Following Relationships in Movement Data SO 2013 IEEE 13TH INTERNATIONAL CONFERENCE ON DATA MINING (ICDM) SE IEEE International Conference on Data Mining LA English DT Proceedings Paper CT IEEE 13th International Conference on Data Mining (ICDM) CY DEC 07-10, 2013 CL Dallas, TX SP IEEE, IEEE Comp Soc, NSF, Toshiba, KNIME, TechMatrix, Univ Texas Dallas, Univ Texas Dallas, Erik Jonsson Sch Engn & Comp Sci, Dept Comp Sci ID MOVING POINT OBJECTS; TRAJECTORIES AB Movement data have been widely collected from GPS and sensors, allowing us to analyze how moving objects interact in terms of space and time and to learn about the relationships that exist among the objects. In this paper, we investigate an interesting relationship that has not been adequately studied so far: the following relationship. Intuitively, a follower has similar trajectories as its leader but always arrives at a location with some time lag. The challenges in mining the following relationship are: (1) the following time lag is usually unknown and varying; (2) the trajectories of the follower and leader are not identical; and (3) the relationship is subtle and only occurs in a short period of time. In this paper, we propose a simple but practical method that addresses all these challenges. It requires only two intuitive parameters and is able to mine following time intervals between two trajectories in linear time. We conduct comprehensive experiments on both synthetic and real datasets to demonstrate the effectiveness of our method. C1 [Li, Zhenhui; Wu, Fei] Penn State Univ, Coll Informat Sci & Technol, University Pk, PA 16802 USA. [Crofoot, Margaret C.] Univ Calif Davis, Davis, CA USA. [Crofoot, Margaret C.] Max Plank Inst Ornithol, Radford, VA 78315 USA. [Crofoot, Margaret C.] Smithsonian Trop Res Inst, Redmond, WA USA. RP Li, ZH (reprint author), Penn State Univ, Coll Informat Sci & Technol, University Pk, PA 16802 USA. EM jessieli@ist.psu.edu; fxw133@ist.psu.edu; mccrofoot@ucdavis.edu NR 26 TC 3 Z9 3 U1 0 U2 2 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 1550-4786 J9 IEEE DATA MINING PY 2013 BP 458 EP 467 DI 10.1109/ICDM.2013.98 PG 10 WC Computer Science, Artificial Intelligence SC Computer Science GA BA1QI UT WOS:000332874200047 ER PT J AU McCormick, MK Parker, KL Szlavecz, K Whigham, DF AF McCormick, Melissa K. Parker, Kenneth L. Szlavecz, Katalin Whigham, Dennis F. TI Native and exotic earthworms affect orchid seed loss SO AOB PLANTS LA English DT Article DE Earthworms; forest succession; mycorrhizae; orchids; seed burial; seed viability ID TERRESTRIAL ORCHIDS; PLANT-COMMUNITIES; SOIL; POPULATIONS; FORESTS; RECRUITMENT; ECOSYSTEMS; DIVERSITY; INVASIONS; FIELD AB Non-native earthworms have invaded ecosystems around the world but have recently received increased attention as they invaded previously earthworm-free habitats in northern North America. Earthworms can affect plants by ingesting seeds and burying them in the soil. These effects can be negative or positive but are expected to become increasingly negative with decreasing seed size. Orchids have some of the smallest seeds of any plants, so we hypothesized that earthworm consumption of seeds would decrease seed viability and lead to burial of ingested seeds. We used a combination of mesocosms and field measurements to determine whether native and non-native earthworms would affect Goodyera pubescens seed germination by decreasing seed viability through digestion or burial. To determine soil depths at which seed burial would decrease chances of germination, we used field measurements of the abundance of mycorrhizal fungi needed for G. pubescens germination at different soil depths. We found that the combined effects of earthworm ingestion and burial would be expected to result in a loss of 49 % of orchid seeds in mature forests and 68 % of those in successional forests over an average year. Differences in seed ingestion and burial among soils from mature and successional forests were probably driven by differences in their ability to support earthworm biomass and not by differences in earthworm behaviour as a function of soil type. The combined effects of earthworm ingestion and burial have the potential to result in substantial loss of orchid seeds, particularly in successional forests. This effect may slow the ability of orchids to recolonize forests as they proceed through succession. Determining whether this strong effect of earthworms on G. pubescens viability and germination also applies to other orchid species awaits further testing. C1 [McCormick, Melissa K.; Parker, Kenneth L.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Szlavecz, Katalin] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. RP McCormick, MK (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM mccormickm@si.edu OI Szlavecz, Katalin/0000-0003-2504-0298; Whigham, Dennis/0000-0003-1488-820X FU United States Department of Agriculture [USDA-CSREES NRI 2007-35320-18375]; National Science Foundation [EAR-0748442]; REU [REU-0353759] FX M.K.M. and K.S. were supported by grants from the United States Department of Agriculture (USDA-CSREES NRI 2007-35320-18375) and the National Science Foundation (EAR-0748442). This study and K.L.P. were supported by an REU grant (REU-0353759) to the Smithsonian Environmental Research Center. NR 51 TC 6 Z9 6 U1 1 U2 17 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 2041-2851 J9 AOB PLANTS JI Aob Plants PY 2013 VL 5 AR plt018 DI 10.1093/aobpla/plt018 PG 11 WC Plant Sciences SC Plant Sciences GA AD5XZ UT WOS:000333327800001 ER PT S AU Rots, AH AF Rots, Arnold H. BE Seago, JH Seaman, RL Seidelmann, PK Allen, SL TI UTC IN ASTRONOMICAL METADATA STANDARDS SO REQUIREMENTS FOR UTC AND CIVIL TIMEKEEPING ON EARTH SE Science and Technology Series LA English DT Proceedings Paper CT Colloquium on Requirements for UTC and Civil Timekeeping on Earth CY MAY 29-30, 2013 CL Jefferson Scholars Fdn, Charlottesville, VA SP Amer Inst Aeronaut & Astronaut HO Jefferson Scholars Fdn ID REPRESENTATIONS; FITS AB There are a number of data and data-format standards in use in the astronomical community that include a high level of specificity regarding the metadata information that they require to describe the astronomical coordinates of the data, including time. For FITS the metadata standards are defined in a series of World Coordinate System (WCS) papers, the latest of which is on Time. Within the Virtual Observatory community there is a Space-Time Coordinate metadata standard which is very similar. This paper presents how UTC is dealt with in these standards. In actual coding implementations the leap second file published by USNO is an essential resource. C1 Smithsonian Astrophys Observ, Chandra Xray Ctr, Cambridge, MA 02138 USA. RP Rots, AH (reprint author), Smithsonian Astrophys Observ, Chandra Xray Ctr, 60 Garden St MS 67, Cambridge, MA 02138 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU AMER ASTRONAUTICAL SOC PI SAN DIEGO PA PUBLICATIONS OFFICE PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 978-0-87703-603-6 J9 SCI TECH PY 2013 VL 115 BP 271 EP 277 PG 7 WC Astronomy & Astrophysics; Instruments & Instrumentation; Telecommunications SC Astronomy & Astrophysics; Instruments & Instrumentation; Telecommunications GA BA0UD UT WOS:000332260900021 ER PT B AU Glotfelty, KJ AF Glotfelty, Kenny J. BE Friedel, DN TI One Hop: In The Right Direction SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois AB Accelerated by the ease of access to data triggered by growing archive registries and common search protocols, many more application than before are now directly interfacing with archives. Gone and going are the days when data sat behind proprietary archive interfaces. What were once exclusively considered analysis tools designed to consume files on disk are now becoming first-class front ends to archives to discover and retrieve remote data-sets. More than that, whether by saving files to disk or sending and servicing SAMP messages, these applications are themselves now local data service providers for other local applications. The problem is that often data that are retrieve remotely are directly cast into the applications internal data model likely altering the data in the process. Content may be added (e.g. new columns), nonessential information (to the current application) may be purged, provenance altered, or content directly modified (e.g. WCS conventions). This possibly insufficient or incompatible view of the data is then what is presented to postliminary tools in the work-flow. The remote data have in essence become trapped in the application that retrieved it from the remote service. In this paper we will discuss this "one hop" effect and the strain it imposes on application developers. We will showcase a current example of this problem and discuss why a "return to source" model of sending all applications back to the original remote source is, in general, insufficient. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Glotfelty, KJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 59 EP 67 PG 9 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500014 ER PT B AU Winkelman, S Rots, A AF Winkelman, Sherry Rots, Arnold BE Friedel, DN TI An Observation-Centric View of the Chandra Data Archive SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois AB The Chandra Data Archive is more than Chandra data. It also includes proposal abstracts, observation parameters, and a bibliography. In addition, there are logs and databases which record user interactions with archive. It's the data which tie these seemingly disparate snapshots of the archive together. By examining the interdependence between the various facets of the archive we can better visualize how our data is being utilized within the astronomical community and perhaps discover new or improved ways to serve the science needs of the community. C1 [Winkelman, Sherry; Rots, Arnold] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Winkelman, S (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 139 EP 142 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500031 ER PT B AU Becker, G Winkelman, S Rots, A AF Becker, Glenn Winkelman, Sherry Rots, Arnold BE Friedel, DN TI Better Living Through Metadata: Examining Archive Usage SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois AB The primary purpose of an observatory's archive is to provide access to the data through various interfaces. User interactions with the archive are recorded in server logs, which can be used to answer basic questions like: Who has downloaded dataset X? When did she do this? Which tools did she use? The answers to questions like these fill in patterns of data access (e.g., how many times dataset X has been downloaded in the past three years). Analysis of server logs provides metrics of archive usage and provides feedback on interface use which can be used to guide future interface development. The Chandra X-ray Observatory is fortunate in that a database to track data access and downloads has been continuously recording such transactions for years; however, it is overdue for an update. We will detail changes we hope to effect and the differences the changes may make to our usage metadata picture. We plan to gather more information about the geographic location of users without compromising privacy; create improved archive statistics; and track and assess the impact of web "crawlers" and other scripted access methods on the archive. With the improvements to our download tracking we hope to gain a better understanding of the dissemination of Chandra's data; how effectively it is being done; and perhaps discover ideas for new services. C1 [Becker, Glenn; Winkelman, Sherry; Rots, Arnold] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Becker, G (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 167 EP 170 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500038 ER PT B AU Chilingarian, I Brown, W Fabricant, D McLeod, B Roll, J Szentgyorgyi, A AF Chilingarian, Igor Brown, Warren Fabricant, Daniel McLeod, Brian Roll, John Szentgyorgyi, Andrew BE Friedel, DN TI Data Reduction Pipeline for the MMT Magellan Infrared Spectrograph SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois AB We describe principal components of the new spectroscopic data pipeline for the multi-object MMT/Magellan Infrared Spectrograph (MMIRS). The pipeline is implemented in mm. and C++. The performance of the data processing algorithms are sufficient to reduce a single dataset in 2-3 mm on a modern PC workstation, so that one can use the pipeline as a quick-look tool during the observations. We provide an example of the spectral data processed by our pipeline and demonstrate that the sky subtraction quality get close to the limits set by the Poisson photon statistics. C1 [Chilingarian, Igor; Brown, Warren; Fabricant, Daniel; McLeod, Brian; Roll, John; Szentgyorgyi, Andrew] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Chilingarian, I (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Chilingarian, Igor/N-5117-2016 OI Chilingarian, Igor/0000-0002-7924-3253 NR 5 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 189 EP 192 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500043 ER PT B AU Tibbetts, M Elvis, M Galache, JL Harbo, P McDowell, JC Rudenko, M Van Stone, D Zografou, P AF Tibbetts, M. Elvis, M. Galache, J. L. Harbo, P. McDowell, J. C. Rudenko, M. Van Stone, D. Zografou, P. BE Friedel, DN TI NEOview: Near Earth Object Data Discovery and Query SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois AB Missions to Near Earth Objects (NEOs) figure prominently in NASA's Flexible Path approach to human space exploration. NEOs offer insight into both the origins of the Solar System and of life, as well as a source of materials for future missions. With NEOview scientists can locate NEO datasets, explore metadata provided by the archives, and query or combine disparate NEO datasets in the search for NEO candidates for exploration. NEOview is a software system that illustrates how standards-based interfaces facilitate NEO data discovery and research. NEOview software follows a client-server architecture. The server is a configurable implementation of the International Virtual Observatory Alliance (IVOA) Table Access Protocol (TAP), a general interface for tabular data access, that can be deployed as a front end to existing NEO datasets. The TAP client, seleste, is a graphical interface that provides intuitive means of discovering NEO providers, exploring dataset metadata to identify fields of interest, and constructing queries to retrieve or combine data. It features a powerful, graphical query builder capable of easing the user's introduction to table searches. Through science use cases, NEOview demonstrates how potential targets for NEO rendezvous could be identified by combining data from complementary sources. Through deployment and operations, it has been shown that the software components are data independent and configurable to many different data servers. As such, NEOview's TAP server and seleste TAP client can be used to create a seamless environment for data discovery and exploration for tabular data in any astronomical archive. C1 [Tibbetts, M.; Elvis, M.; Galache, J. L.; Harbo, P.; McDowell, J. C.; Rudenko, M.; Van Stone, D.; Zografou, P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Tibbetts, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 259 EP 262 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500060 ER PT B AU Mink, J AF Mink, Jessica BE Friedel, DN TI The Past 15 Years of RVSAO SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS XXII SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 22nd Annual Conference on Astronomical Data Analysis Software and Systems (ADASS XXII) CY NOV 04-08, 2012 CL Univ Illinois, Champaign, IL SP Natl Ctr Supercomput Applicat, NASA Infrared Process & Anal Ctr, Univ Illinois, Dept Astron, Natl Radio Astron Observ, Australian Astron Observ, Natl Opt Astron Observ, Canada France Hawaii Telescope, Observ Paris, Elsevier Publish, Smithsonian Astrophys Observ, European Space Astron Ctr, Space Telescope Sci Inst, European So Observ HO Univ Illinois ID RADIAL-VELOCITIES AB Since the last paper describing the IRAF RVSAO radial velocity package was published almost 15 years ago, this collection of tasks dealing with wavelength-shifted spectra has continued to grow and evolve. Many changes have been made to improve robustness and accuracy in the xcsao cross-correlation and emsao emission line fitting tasks. Two new tasks, pxcsao and pemsao, find radial velocities using the same methods, but save the results as task parameters, making them easier to use in CL scripts. Spectra can now be cross-correlated in pixel or wavelenth space as well as velocity space. A major task, eqwidth, based on the TRAF bands task, computes equivalent widths in redshifted spectra. sumspec, which rebins, normalizes, re-redshifts, sums, and/or stacks spectra, has proven to be useful in multi-fiber spectrograph reduction pipelines. listspec lists spectra in a variety of user-selected formats, and several CL scripts plot spectra with labeled emission and absorption lines. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Mink, J (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-834-3 J9 ASTR SOC P PY 2013 VL 475 BP 291 EP 294 PG 4 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA BA0YC UT WOS:000332346500068 ER PT S AU Rothman, LS Gordon, IE AF Rothman, Laurence S. Gordon, Iouli E. BE Gillaspy, JD Wiese, WL Podpaly, YA TI The HITRAN Molecular Database SO EIGHTH INTERNATIONAL CONFERENCE ON ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS (ICAMDATA-2012) SE AIP Conference Proceedings LA English DT Proceedings Paper CT 8th International Conference on Atomic and Molecular Data and Their Applications (ICAMDATA) CY SEP 30-OCT 04, 2012 CL Gaithersburg, MD DE HITRAN; molecular absorption; spectroscopic database AB This presentation provides an overview of the updates and extensions of the HITRAN molecular spectroscopic absorption database. The new significantly improved parameters for the major atmospheric absorbers (for instance H2O and O-2) have been given particular attention. For most of the molecules, spectral parameters have been revised and updated. The new edition also features many new spectral bands and new isotopic species. The cross-section part of the database has also been significantly extended by adding new species as well as more temperature-pressure sets for existing species. In addition, HITRAN now provides the collision-induced absorption parameters, including those relevant to the terrestrial atmosphere: N-2-N-2, N-2-O-2, O-2-O-2. The study of the spectroscopic signatures of planetary atmospheres is a powerful tool for extracting detailed information concerning their constituents and thermodynamic properties. The HITRAN molecular spectroscopic database has traditionally served researchers involved with terrestrial atmospheric problems, such as remote sensing of constituents in the atmosphere, pollution monitoring at the surface, and numerous environmental issues. In collaboration with laboratories across the globe, an extensive effort is currently underway to extend the HITRAN database to have capabilities for investigating a variety of planetary atmospheres. Spectroscopic parameters for gases and spectral bands of molecules that are germane to the studies of planetary atmospheres are being assembled. These parameters include the types of data that have already been considered for transmission and radiance algorithms, such as line position, intensity, broadening coefficients, lower-state energies, and temperature dependence values. A number of new molecules, including H-2, CS, C4H2, HC3N, and C2N2, are being incorporated into HITRAN, while several other molecules are pending. For some of the molecules, additional parameters, beyond those currently considered for the terrestrial atmosphere, are being archived. Examples are collision-broadened half widths due to various foreign partners, collision-induced absorption, and temperature dependence factors. Collision-induced absorption data for H-2-H-2, H-2-N-2, H-2-He, H-2-CH4, CH4-CH4, O-2-CO2 and N-2-CH4 were recently released. Partition sums that are necessary for applications at a wide range of temperatures have also been calculated for a variety of molecules of planetary interest, and form an integral part of the HITRAN compilation. C1 [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. OI Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 NR 9 TC 2 Z9 2 U1 3 U2 17 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-1170-8 J9 AIP CONF PROC PY 2013 VL 1545 BP 223 EP 231 DI 10.1063/1.4815858 PG 9 WC Physics, Applied; Physics, Atomic, Molecular & Chemical SC Physics GA BA0HJ UT WOS:000331261500023 ER PT S AU Foster, AR Ji, L Yamaguchi, H Smith, RK Brickhouse, NS AF Foster, Adam R. Ji, Li Yamaguchi, Hiroya Smith, Randall K. Brickhouse, Nancy S. BE Gillaspy, JD Wiese, WL Podpaly, YA TI AtomDB: Atomic Data for X-ray Astronomy SO EIGHTH INTERNATIONAL CONFERENCE ON ATOMIC AND MOLECULAR DATA AND THEIR APPLICATIONS (ICAMDATA-2012) SE AIP Conference Proceedings LA English DT Proceedings Paper CT 8th International Conference on Atomic and Molecular Data and Their Applications (ICAMDATA) CY SEP 30-OCT 04, 2012 CL Gaithersburg, MD ID PHOTOIONIZATION CROSS-SECTIONS; OPTICALLY THIN PLASMAS; LOW-DENSITY PLASMA; IONIZATION EQUILIBRIUM; RECOMBINATION RATES; FLUORESCENCE YIELDS; IONS; EMISSION; ELEMENTS; FITS AB This paper outlines some of the progress in the AtomDB project, which aims to model X-ray emission from hot, collisionally ionized plasmas. We define data formats for ionization, recombination, photo-ionization and autoionization. We discuss the inclusion of the XSTAR database in AtomDB, in particular using the photoionization data, and the progress in preparing a full non-equilibrium ionization model for use by modelers and observers. C1 [Foster, Adam R.; Yamaguchi, Hiroya; Smith, Randall K.; Brickhouse, Nancy S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Foster, AR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 30 TC 0 Z9 0 U1 2 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-1170-8 J9 AIP CONF PROC PY 2013 VL 1545 BP 252 EP 259 DI 10.1063/1.4815861 PG 8 WC Physics, Applied; Physics, Atomic, Molecular & Chemical SC Physics GA BA0HJ UT WOS:000331261500026 ER PT S AU Herrick, JA Siebert, L Rose, WI AF Herrick, Julie A. Siebert, Lee Rose, William I. BE Rose, WI Palma, JL Granados, HD Varley, N TI Large-volume Barriles and Caisan debris avalanche deposits from Volcan Baru, Panama SO UNDERSTANDING OPEN-VENT VOLCANISM AND RELATED HAZARDS SE Geological Society of America Special Papers LA English DT Article; Book Chapter ID COSTA-RICA; EMPLACEMENT MECHANISMS; FOREST DISTURBANCE; EDIFICE FAILURES; SECTOR COLLAPSE; WESTERN PANAMA; HISTORY; RECORD; AGRICULTURE; CONSTRAINTS AB Geologic mapping at the base of Volcan Baru, Panama, characterizes two large andesitic volcanic debris avalanche deposits attributed to sector collapse at Volcan Baru. The older Caisan debris avalanche deposit is at or beyond the radiocarbon dating range, >43,500 yr B.P., whereas the younger Barriles debris avalanche deposit is constrained by two radiocarbon ages that are ca. 9000 yr B. P. The total runout length of the Caisan deposit was similar to 50 km, covering nearly 1200 km(2). The Barriles deposit extended to similar to 45 km and covered >990 km(2), overlapping most of the Caisan. Over 4000 hummocks from these deposits were digitized, and statistical analysis of hummock location and geometry depicts flow patterns of highly fragmented material affected by underlying topography and also helps to define the shorter runout limit of the Barriles deposit. The Barriles and Caisan deposits are primarily unconfined deposits that are among the world's most voluminous subaerial debris avalanche deposits. Two different geospatial procedures, utilizing deposit thicknesses and edifice reconstruction, yield calculated volumes similar to 30 km(3) and larger for both deposits. Subaerial deposits of comparable scale include those from Mount Shasta, Socompa, and Shiveluch. Currently, the modern edifice is 200-400 m lower than the estimated pre-collapse Barriles and Caisan summits, and only 16%-25% of the former edifice has been replaced since the last failure. The similar to 10 km(3) postcollapse lava-dome complex, however, implies a Holocene magma production rate of 1.1 km(3)/k.y., comparable to elevated eruptive pulses documented at other stratovolcanoes, underscoring the importance of hazards assessment and monitoring of this active volcano. C1 [Herrick, Julie A.; Rose, William I.] Michigan Technol Univ, Dept Geol Engn & Sci, Houghton, MI 49931 USA. [Siebert, Lee] Smithsonian Inst, Global Volcanism Program, Washington, DC 20013 USA. RP Herrick, JA (reprint author), Michigan Technol Univ, Dept Geol Engn & Sci, Houghton, MI 49931 USA. NR 59 TC 2 Z9 2 U1 0 U2 1 PU GEOLOGICAL SOC AMER INC PI BOULDER PA 3300 PENROSE PL, PO BOX 9140, BOULDER, CO 80301 USA SN 0072-1077 BN 978-0-8137-2498-0 J9 GEOL SOC AM SPEC PAP PY 2013 VL 498 BP 141 EP 162 DI 10.1130/2013.2498(09) D2 10.1130/9780813724980 PG 22 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA BJR96 UT WOS:000329862300010 ER PT S AU Ryan, MJ Cummings, ME AF Ryan, Michael J. Cummings, Molly E. BE Futuyma, DJ TI Perceptual Biases and Mate Choice SO ANNUAL REVIEW OF ECOLOGY, EVOLUTION, AND SYSTEMATICS, VOL 44 SE Annual Review of Ecology Evolution and Systematics LA English DT Review; Book Chapter DE sensory drive; receiver biases; sexual selection; sensory traps; sensory exploitation ID AWAY SEXUAL SELECTION; FEMALE MATING PREFERENCES; SIGNAL EVOLUTION; VISUAL PIGMENTS; SENSORY DRIVE; COLOR PATTERNS; TUNGARA FROGS; SURFPERCH EMBIOTOCIDAE; PHYSALAEMUS-PUSTULOSUS; ANIMAL COMMUNICATION AB Our view of the evolution of sexually selected traits and preferences was influenced radically in the 1990s by studies that emphasized how signals interact with sensory properties of receivers. Here, twenty-five years later, we review evidence that has accumulated in support of this idea. We replace the term sensory biases with perceptual biases to emphasize the growing knowledge of how cognitive processes generate selection on sexual traits. We show that mating preferences among conspecifics (e.g., sexual selection by mate choice) often are influenced by perceptual adaptations and constraints that have evolved in other contexts. We suggest that these perceptual biases need not be costly to females when they influence mate choice because in many cases they generate direct benefits. Although we do not reject a role for indirect benefits in mate choice, such as good genes, exclusive focus on eugenic mate choice limits our understanding of the evolution of the remarkable diversity of sexually selected traits. C1 [Ryan, Michael J.; Cummings, Molly E.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. RP Ryan, MJ (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM mryan@utexas.edu; mcummings@austin.utexas.edu NR 129 TC 56 Z9 57 U1 20 U2 119 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 1543-592X BN 978-0-8243-1444-6 J9 ANNU REV ECOL EVOL S JI Annu. Rev. Ecol. Evol. Syst. PY 2013 VL 44 BP 437 EP + DI 10.1146/annurev-ecolsys-110512-135901 PG 46 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA BJR54 UT WOS:000329821800021 ER PT J AU Barrantes, G Aisenberg, A Eberhard, WG AF Barrantes, Gilbert Aisenberg, Anita Eberhard, William G. TI Functional aspects of genital differences in Leucauge argyra and L. mariana (Araneae: Tetragnathidae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Copulatory plugs; genital movements; genital evolution ID SPIDERS ARANEAE; FEMALE CHOICE; COPULATION; COURTSHIP AB Morphological studies have documented the tendency for male genitalia to diverge rapidly compared to other body parts in many animal groups, including spiders. But documentation of how differences in genital structures of closely related species correlate with differences in the behavior of their genitalia during copulation is rare. This study describes how the genitalia of the spider Leucauge argyra (Walckenaer 1841), a species in which both male and female have unusual derived structures, are used during copulation and compares their sexual behavior with previous descriptions of genital behavior in the congener L. mariana (Taczanowski 1881) and the genital morphology of other Leucauge species. Males of L. argyra have two prominent derived genital structures, both of which interact directly with the female; one of them apparently locks against a modified female structure, while the other is inserted into the female atrium. On the other hand, the most prominent derived female structure does not lock against or receive any male structure and may serve to sense movements of the male palp, perhaps to trigger deposition of a strong copulatory plug by the female. The female atrium is unusual in that it receives insertions of both the male's conductor and his cymbial hook. Both derived male structures of L. argyra may have evolved to stabilize the male's genitalia during intromission, perhaps in response to violent and dangerous female resistance or to perforate the strong plug that is probably produced or at least moved into place by the female. The rotating and projecting movements executed by male genitalia in L. argyra, which as in other spiders are presumably produced by the hydraulic unfolding of complex membranes in the palp, are quite different from the movements of the male genitalia of L. mariana. We speculate that in spiders in general, changes in palpal sclerites are often accompanied by changes in the movements of the sclerites, and thus by changes in the unstudied internal membranes of the palp. C1 [Barrantes, Gilbert; Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. [Aisenberg, Anita] Inst Invest Biol Clemente Estable, Lab Etol Ecol & Evoluc, Montevideo, Uruguay. [Eberhard, William G.] Smithsonian Trop Res Inst, Panama City, Panama. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute (STRI); Stanley Rand Fellowship; Universidad de Costa Rica; STRI FX We thank Pedro Gaspar for kindly allowing us to work in his plantation, J. Moya-Ramirez, A. Rojas, M. Solis Del Valle and Ju-Lin Weng for help with fieldwork, Maribelle Vargas Montero for help with the SEM, Nubia Caballero, Rosannette Quesada and Emilia Triana for sharing unpublished data, and Bernhard Huber for two rounds of constructive comments on preliminary versions of the manuscript. The Smithsonian Tropical Research Institute (STRI) supported AA with a Stanley Rand Fellowship; the Universidad de Costa Rica and STRI provided financial support for GB and WGE. NR 29 TC 1 Z9 3 U1 0 U2 3 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2013 VL 41 IS 1 BP 59 EP 69 PG 11 WC Entomology SC Entomology GA AA3YB UT WOS:000331030000009 ER PT J AU Eberhard, WG Hazzi, NA AF Eberhard, William G. Hazzi, Nicolas A. TI Web construction of Linothele macrothelifera (Araneae: Dipluridae) SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Mygalomorph; sheet web construction behavior ID EVOLUTION; BEHAVIOR; SPIDERS AB Direct behavioral observations, plus deductions made from studying the lines in recently built webs, showed that Linothele macrothelifera Strand 1908 lays swaths of lines in relatively stereotypic ways that differ during sheet web and tube construction. Sheet construction occurs in brief bursts interspersed with returns to the retreat. The legs are not used to manipulate lines; the spinnerets attach lines to the substrate and are probably used as sense organs. Asymmetrical use of the spinnerets during sheet construction results in an increase in the variety of orientations of lines in the sheet. C1 [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. [Hazzi, Nicolas A.] Univ Valle, Programa Acad Biol, Cali, Colombia. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Universidad de Costa Rica FX It is a pleasure to thank Eduardo Florez for arranging the logistics of the trip to the Reserva Forestal de Yotoco and managing the specimens, and Ligia Benavides for much additional help of various sorts (including locating spiders in the field). Martin Ramirez and Matias Izquierdo provided pleasant company in the field. We thank the Director Carlos Alberto Jaramillo and also Valentin Hidalgo of the Reserva Forestal de Yotoco for permission to work there. We are especially grateful to Laura Santamaria for identifying the spiders. Financial support was provided by the Smithsonian Tropical Research Institute and the Universidad de Costa Rica. NR 17 TC 2 Z9 2 U1 0 U2 4 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2013 VL 41 IS 1 BP 70 EP 75 PG 6 WC Entomology SC Entomology GA AA3YB UT WOS:000331030000010 ER PT J AU Eberhard, WG AF Eberhard, William G. TI The rare large prey hypothesis for orb web evolution: a critique SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Orb web evolution; rare large prey hypothesis ID WEAVING SPIDERS; VISIBILITY; ARANEIDAE; BEHAVIOR; CAPTURE; ARANEAE; SILK AB Several recent studies emphasize, correctly, that the biomass of prey captured by an orb web is likely more important than the number of prey in driving the evolution of web designs. Using equations that estimate prey mass from the lengths of captured prey, one study concluded that rare, long-bodied prey contribute the large majority of energy obtained by orb weavers in general, and thus that the designs of orb webs should generally reflect selection favoring the capture of larger insects, especially the ability to absorb high-energy impacts. I show here that the weights of long prey have sometimes been seriously overestimated by these equations. In addition, the longer prey captured by spiders probably represent highly biased samples, in terms of both low weight/body length and low momentum/body weight, of the longer prey available in the environment, leading to overestimates of the kinetic energy that the orb needed to absorb to stop them. Deductions concerning how selection acts on orb designs that have been based on the prey captured are also flawed, because additional data on prey availabilities and prey escapes are needed to evaluate the possible gains and losses from different orb designs. Still another complication is that data on prey abundances in natural rather than altered environments are needed to understand past selection pressures that produced present-day web forms. I conclude that a dominant importance for rare large prey in orb web evolution has not been conclusively demonstrated to be a general rule for orb weavers. A more inclusive approach regarding orb functions is prudent, especially because many traits that improve some functions have opposite effects on others. C1 [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad Univ, San Jose, Costa Rica. EM william.eberhard@gmail.com NR 31 TC 5 Z9 5 U1 2 U2 10 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2013 VL 41 IS 1 BP 76 EP 80 PG 5 WC Entomology SC Entomology GA AA3YB UT WOS:000331030000011 ER PT J AU Lapinski, W Tschapka, M AF Lapinski, Witold Tschapka, Marco TI Habitat use in an assemblage of Central American wandering spiders SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Coexistence; habitat preference; natural prey; niche; sympatry; Ctenidae; Trechaleidae ID RAIN-FOREST; ARANEAE; CTENIDAE; ABUNDANCE; PATTERNS; PISAURIDAE; CUPIENNIUS; NICHE; REVISION; RANGE AB The sympatric occurrence of species is thought to be based mainly on the differences in their use of habitat and of limiting resources. Segregating parameters may be of spatial or temporal character and may include behavioral differences. We hypothesized that species of large hunting spider living sympatrically in a Costa Rican lowland rain forest should differ in their habitat and/or hunting microhabitat preferences, in daily activity pattern, and, as an adaptation to the preferred hunting microhabitat, in their specific ability to adhere to smooth surfaces. We found an assemblage of eight large species of the families Ctenidae and Trechaleidae, consisting of three subguilds: 1) two semi-aquatic species with low adhesion ability, 2) three forest-floor dwelling species with good adhesion ability, and 3) three vegetation dwelling species showing very good adhesion ability. The species were partially segregated by habitat type, with two of the vegetation dwelling species preferring the treeless area of a temporary swamp. We found no species-specific differences in daily activity patterns. The similarity in community structure between this Costa Rican and a central Amazonian assemblage suggests the existence of similar structuring mechanisms in wandering spider assemblages in climatically similar biomes. C1 [Lapinski, Witold; Tschapka, Marco] Univ Ulm, Inst Expt Biol, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Lapinski, W (reprint author), Univ Ulm, Inst Expt Biol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM witold.lapinski@uni-ulm.de FU German Academic Exchange Service (DAAD) FX We thank the German Academic Exchange Service (DAAD) for a scholarship supporting fieldwork of WL in Costa Rica. Hubert Hofer (State Museum of Natural History, Karlsruhe, Germany) provided us with valuable unpublished Masters and Doctoral theses. M. Pfeiffer (University of Ulm, Germany) helped with the multivariate statistical analysis. The MINAET (Ministerio de Ambiente, Energia y Telecomunicaciones, Costa Rica) kindly gave us the permit to conduct field work in Costa Rica. The friendly assistance of Javier Guevara (MINAET) is greatly appreciated. We are very grateful to Bernal Rodriguez-Herrera (RBT and UCR) and all staff members at the Reserva Biologica Tirimbina for all their friendliness and support, and for allowing us to complete this project at the station. NR 43 TC 7 Z9 8 U1 1 U2 6 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2013 VL 41 IS 2 BP 151 EP 159 PG 9 WC Entomology SC Entomology GA AA3YC UT WOS:000331030100007 ER PT J AU Kralj-Fiser, S Gregoric, M Lokovsek, T Celik, T Kuntner, M AF Kralj-Fiser, Simona Gregoric, Matjaz Lokovsek, Tjasa Celik, Tatjana Kuntner, Matjaz TI A glimpse into the sexual biology of the "zygiellid" spider genus Leviellus SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Mating system; genital plugging; mate guarding; sexual-size dimorphism; eunuchs ID ORB-WEB SPIDER; CANNIBALISTIC SPIDER; SPERM COMPETITION; MATING-BEHAVIOR; NEPHILID SPIDERS; MALE ADAPTATION; WEAVING SPIDER; GENITAL DAMAGE; DESERT SPIDER; ARANEAE AB We investigated the mating biology of the previously unstudied central European spider Leviellus thorelli (Ausserer 1871) by staging laboratory mating trials using males and females of varying mating histories. Our aim was to seek common themes in sexual behaviors of the sexually size-monomorphic "zygiellid" spiders with their putatively close relatives, araneids and nephilids, which are relatively well studied with respect to sexual biology. We found L. thorelli mating biology to more closely resemble that of sexually size-monomorphic araneids than that of dimorphic nephilids. Unlike in nephilids with sexually conflicted adaptations, we found no evidence for genital damage or plugging in Leviellus Wunderlich 2004, although we found rare cases of half-eunuchs. We suggest that the mating system of L. thorelli spiders is determined by short female sexual attractiveness, reduced receptivity after mating and/or intensive mate guarding. C1 [Kralj-Fiser, Simona; Gregoric, Matjaz; Lokovsek, Tjasa; Celik, Tatjana; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Jovan Hadzi Inst Biol, SI-1001 Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Kralj-Fiser, S (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Jovan Hadzi Inst Biol, Novi Trg 2, SI-1001 Ljubljana, Slovenia. EM simonakf@gmail.com FU Slovenian Research Agency [J12063] FX We thank Eva and Irena Kuntner and Cene Fiser for logistic help, Jutta Schneider for comments on the early manuscript version, and Martin Marzidovsek for making available the video on male antagonism. This work was funded by the Slovenian Research Agency (grant J12063 to M. Kuntner). NR 54 TC 3 Z9 3 U1 0 U2 3 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PY 2013 VL 41 IS 3 BP 387 EP 391 PG 5 WC Entomology SC Entomology GA AA3YD UT WOS:000331030200013 ER PT J AU Smith, DR Janzen, DH Hallwachs, W AF Smith, David R. Janzen, Daniel H. Hallwachs, Winnie TI Food plants and life histories of sawflies of the families Argidae and Tenthredinidae (Hymenoptera) in Costa Rica, a supplement SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Symphyta; Area de Conservacion Guanacaste; ACG; fern; tropical dry forest; tropical rain forest AB Food plants and information on life history are presented for six species of Argidae and four species of Tenthredinidae in Costa Rica. The Argidae include cocoons of Atomacera josefernandezi Smith, sp. n., found on Hampea appendiculata (Donn. Sm.) Standl. (Malvaceae) and likely feeding on its leaves before pupation, and larvae of Eriglenum tristum Smith feeding on Machaerium seemanii Benth. Ex Seem. (Fabaceae), Ptenos leucopodus (Cameron) feeding on Inga oerstediana Benth. and I. vera Wild. (Fabaceae), Ptilia peleterii (Gray) feeding on Cnestidium rufescens (Connaraceae), and Scobina lepida (Klug) and S. notaticollis (Konow) feeding on Sida rhombifolia L. (Malvaceae). The Tenthredinidae include larvae of Dochmioglene crassa (Cameron) feeding on the fern Lomariopsis vestita E. Fourn. (Lomariopsidaceeae), Dochmiogleme Smith03 feeding on Blechnum occidentale L. (Blechnaceae), Waldheimia laeta (Cameron) feeding on Cissus alata Jacq. (Vitaceae), and Waldheimia lucianocapellii Smith, sp. n., feeding on Davilla nitida (Vahl) Kubitzki (Dilleniaceae). Waldheimia lucianocapellii is described from specimens from both Panama and Costa Rica. Selandria crassa Cameron, 1883 is a comb. n. in Dochmioglene. C1 [Smith, David R.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. RP Smith, DR (reprint author), USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com FU U.S. National Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; Wege Foundation; International Conservation Fund of Canada; Jessie B. Cox Charitable Trust; Blue Moon Fund; Guanacaste Dry Forest Conservation Fund; Area de Conservacion Guanacaste; University of Pennsylvania (DHJ); Government of Canada through Genome Canada; Ontario Genomics Institute [2008-OGI-ICI-03] FX Michele Touchet, Systematic Entomology Laboratory, USDA, Washington, DC, helped with Figures 1-15. We gratefully acknowledge the team of ACG parataxonomists (Janzen et al. 2009) who found and reared the specimens used in this study, and the team of biodiversity managers who keep alive the ACG forests that host these sawflies. The study has been supported by U.S. National Science Foundation grants BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, 0515699, and grants from the Wege Foundation, International Conservation Fund of Canada, Jessie B. Cox Charitable Trust, Blue Moon Fund, Guanacaste Dry Forest Conservation Fund, Area de Conservacion Guanacaste, and University of Pennsylvania (DHJ). Laboratory analyses of the DNA barcode sequences were funded by the Government of Canada through Genome Canada and the Ontario Genomics Institute (2008-OGI-ICI-03), thanks to P. D.N. Hebert, M. Hajobabae, and S. Naik. USDA is an equal opportunity provider and employer. NR 17 TC 1 Z9 1 U1 1 U2 6 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2013 VL 35 BP 17 EP 31 DI 10.3897/JHR.35.5496 PG 15 WC Entomology SC Entomology GA 300UA UT WOS:000330488300002 ER PT J AU Sharma, S Dutta, T Maldonado, JE Wood, TC Panwar, HS Seidensticker, J AF Sharma, Sandeep Dutta, Trishna Maldonado, Jesus E. Wood, Thomas C. Panwar, Hemendra Singh Seidensticker, John TI Selection of microsatellite loci for genetic monitoring of sloth bears SO URSUS LA English DT Article DE DNA; individual identification; Melursus ursinus; microsatellite; noninvasive sampling; sloth bear ID INDIVIDUAL IDENTIFICATION; COMPUTER-PROGRAM; PANTHERA-PARDUS; POLAR BEARS; POPULATION; SOFTWARE; ALASKA; INDIA; FLOW AB The sloth bear (Melursus ursinus) is a threatened species endemic to the Indian subcontinent. To date, no reliable method has been developed for identifying individuals or monitoring their populations. Here we describe a non-invasive genetic monitoring technique for individual identification of sloth bears. After testing 18 micro satellites developed for other carnivore species, including ursids, we optimized a panel of 7 highly polymorphic microsatellite loci that yielded a cumulative Probability of Identity between siblings value of 2.15E-03. We used this panel to identify 55 individual sloth bears from 190 fecal and 4 hair samples collected in tiger reserves in central India. This panel can be used for population genetic studies and population monitoring of sloth bears. C1 [Sharma, Sandeep] Clemson Univ, Clemson Inst Pk, Clemson, SC 29634 USA. [Sharma, Sandeep; Dutta, Trishna; Maldonado, Jesus E.; Seidensticker, John] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Dutta, Trishna] Clemson Univ, Sch Agr Forest & Environm Sci, Clemson, SC 29634 USA. [Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Sharma, S (reprint author), Clemson Univ, Clemson Inst Pk, Clemson, SC 29634 USA. EM sandeeps17@gmail.com FU International Bear Association; Smithsonian Conservation Biology Institute; Friends of the National Zoo; Kathryn Fuller Science for Nature Fund of World Wildlife Fund FX We thank the Principal Chief Conservator of Forests (Wildlife) Madhya Pradesh and Maharashtra for granting research permission. We are grateful to the Field Directors of all the tiger reserves (Kanha, Satpura, Melghat, Pench-MP, Pench-Mh) for providing logistical help. We thank Y.S. Shouche and H. Munot of the National Center for Cell Sciences, Pune, India, for providing laboratory space and facilitating lab work. We thank the Rajiv Gandhi Zoological Park, Pune, for providing us samples from captive sloth bears and S. Pawar for facilitation. At the Smithsonian Conservation Biology Institute (SCBI), R. Fleischer and N. Rotzel of the Center for Conservation and Evolutionary Genetics and L. Dougan of the Conservation Ecology Center offered logistical support. S. Lumpkin provided useful suggestions and editorial input to improve the manuscript. Funding for this study was provided by the International Bear Association, Smithsonian Conservation Biology Institute, Friends of the National Zoo, and Kathryn Fuller Science for Nature Fund of World Wildlife Fund. We thank the editor and an anonymous reviewer for comments that greatly improved the quality of this manuscript. NR 30 TC 2 Z9 2 U1 0 U2 8 PU INT ASSOC BEAR RESEARCH & MANAGEMENT-IBA PI KNOXVILLE PA C/O TERRY WHITE, UNIV TENNESSEE, DEPT FORESTRY, WILDLIFE & FISHERIES, PO BOX 1071, KNOXVILLE, TN 37901-1071 USA SN 1537-6176 J9 URSUS JI Ursus PY 2013 VL 24 IS 2 BP 164 EP 169 PG 6 WC Zoology SC Zoology GA 299SE UT WOS:000330415200007 ER PT J AU Gorzelak, P Zamora, S AF Gorzelak, Przemyslaw Zamora, Samuel TI Stereom microstructures of Cambrian echinoderms revealed by cathodoluminescence (CL) SO PALAEONTOLOGIA ELECTRONICA LA English DT Article DE skeleton; biomineralization; Cambrian; echinoderms; stereom; cathodoluminescence ID BIOMINERALIZATION; SPAIN; AFFINITIES; MORPHOLOGY; EVOLUTION; OSSICLES; PLATES AB Echinoderms possess a skeleton with a unique and distinctive meshlike microstructure called stereom that is underpinned by a specific family of genes. Stereom is thus considered the major echinoderm synapomorphy and is recognized already in some Cambrian echinoderm clades. However, data on the skeletal microstructures of early echinoderms are still sparse and come only from isolated ossicles of limited taxonomic value in which the primary calcium carbonate has been replaced or thinly coated by phosphates, silica or iron oxides. Here, we applied cathodoluminescence (CL) to reveal stereom microstructures of the diagenetically altered calcitic skeletons of some Cambrian echinoderms (in particular Protocinctus, Stromatocystites and Dibrachicystidae). CL not only provides insights into the diagenesis of their skeletons but also reveals primary microstructural details that are not visible under transmitted light or SEM. Different stereom types (resembling labyrinthic, fascicular, galleried, microperforate and imperforate microfabrics) comparable to those observed in extant echinoderms have been recognized for the first time in these Cambrian taxa. Our results show that the stereom microstructures widely occur in various Cambrian echinoderm clades which suggest that they likely evolved the same genetically controlled biomineralization mechanisms as those observed in modern echinoderms. These results underline that the CL technique can be a powerful tool in the detection of the microstructural organization in even severely recrystallized echinoderm specimens. Given the close association between the skeletal microstructure and the investing soft tissues, the method presented here opens new possibilites for revealing skeletal growth and soft tissue palaeoanatomy of fossil echinoderms. C1 [Gorzelak, Przemyslaw] Polish Acad Sci, Inst Paleobiol, Dept Biogeol, PL-00818 Warsaw, Poland. [Zamora, Samuel] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Gorzelak, P (reprint author), Polish Acad Sci, Inst Paleobiol, Dept Biogeol, Twarda Str 51-55, PL-00818 Warsaw, Poland. EM pgorzelak@twarda.pan.pl; samuel@unizar.es RI Gorzelak, Przemyslaw/B-6329-2015 OI Gorzelak, Przemyslaw/0000-0001-5706-1881 FU National Science Centre (NCN) [DEC-2011/03/N/ST10/04798]; European Regional Development Fund [POIG.02.02.00-00-025/09]; Spanish Project [CGL2011-24516] FX This work was funded by the National Science Centre (NCN) grant no DEC-2011/03/N/ST10/04798 and was performed in the NanoFun laboratory co-financed by the European Regional Development Fund within the Innovation Economy Operational Programme POIG.02.02.00-00-025/09. SZ was funded by the Spanish Project CGL2011-24516) and a Post Doctoral grant at the Smithsonian Institution. We are grateful to O. Elicki (Germany) and S. Clausen (France) for allowing us to use some of their photographies. We thank the editor S. Gerber (France) and two anonymous reviewers for their constructive comments. Additional comments by A. B. Smith (United Kingdom) and J. Stolarski (Poland) greatly helped to improve the resulting manuscript. I. Perez (Spain) provided help in preparing Figure 1. NR 49 TC 4 Z9 4 U1 0 U2 2 PU COQUINA PRESS PI AMHERST PA C/O WHITEY HAGADORN, EXECUTIVE EDITOR, AMHERST COLLEGE, DEPT GEOLOGY, AMHERST, MA 01002 USA SN 1935-3952 EI 1094-8074 J9 PALAEONTOL ELECTRON JI Palaeontol. electron. PY 2013 VL 16 IS 3 AR 32A PG 17 WC Paleontology SC Paleontology GA 293QA UT WOS:000329987100012 ER PT J AU Chaisson, EJ AF Chaisson, Eric J. BE Lineweaver, CH Davies, PCW Ruse, M TI Using complexity science to search for unity in the natural sciences SO COMPLEXITY AND THE ARROW OF TIME LA English DT Article; Book Chapter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chaisson, EJ (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 7 TC 4 Z9 4 U1 0 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND BN 978-1-107-02725-1 PY 2013 BP 68 EP 79 D2 10.1017/CBO9781139225700 PG 12 WC History & Philosophy Of Science SC History & Philosophy of Science GA BJL26 UT WOS:000328818100004 ER PT B AU Boyle, SA Lenz, BB Gilbert, KA Sprionello, WR Gomez, MS Setz, EZF dos Reis, AM da Silva, OF Keuroghlian, A Pinto, F AF Boyle, Sarah A. Lenz, Bryan B. Gilbert, Kellen A. Sprionello, Wilson R. Gomez, Marcela Santamaria Setz, Eleonore Z. F. dos Reis, Alaercio Marajo da Silva, Osmaildo Ferreira Keuroghlian, Alexine Pinto, Flavia BE Marsh, LK Chapman, CA TI Primates of the Biological Dynamics of Forest Fragments Project: A History SO PRIMATES IN FRAGMENTS: COMPLEXITY AND RESILIENCE SE Developments in Primatology-Progress and Prospects LA English DT Article; Book Chapter ID PITHECIA-PITHECIA-CHRYSOCEPHALA; PRIMARY SEED DISPERSAL; AMAZONIAN FOREST; SAKI MONKEYS; CHIROPOTES; PATTERNS; FATE; DUNG AB The Biological Dynamics of Forest Fragments Project (BDFFP), located approximately 80 km north of Manaus, Brazil, is the longest-running study of forest fragmentation in the world. The BDFFP was created in 1979 and the first primate census occurred in 1980. Six primate species inhabit the study area: red howler (Alouatta macconnelli), black spider (Ateles paniscus), brown capuchin (Sapajus apella), northern bearded saki (Chiropotes satanas chiropotes), golden-faced saki (Pithecia chrysocephala), and golden-handed tamarin (Saguinus midas). The distribution of these six species throughout the forest fragments has varied during the past three decades with some species (i.e., howler monkeys) being more prevalent than others (i.e., spider monkeys), particularly in the smaller fragments. Researchers did not find primates in some of the 1-ha forest fragments prior to 2007. Here we present a history of primate research at the BDFFP, including findings from three decades of primate censuses and behavioral and ecological studies of several species in the forest fragments, the surrounding matrix, and the continuous forest. These primate studies have provided information on seed dispersal in forest fragments, parasite infections, use of the matrix, and changes in group size, activity budget, and diet of groups in the forest fragments. Many of the once-cleared pastures surrounded by continuous primary forest are now dominated by various stages of secondary growth. Unfortunately, deforestation continues in many areas of the continuous forest north of Manaus. We discuss the implications of these land-cover changes on the primate community and suggest avenues for future primate research at the BDFFP. C1 [Boyle, Sarah A.] Rhodes Coll, Dept Biol, Memphis, TN 38112 USA. [Lenz, Bryan B.] Tulane Univ, Dept Anthropol, New Orleans, LA 70118 USA. [Gilbert, Kellen A.] SE Louisiana Univ, Dept Sociol, Hammond, LA 70402 USA. [Sprionello, Wilson R.] Inst Nacl de Pesquisas da Amazonia, BR-69080971 Manaus, Amazonas, Brazil. [Gomez, Marcela Santamaria; dos Reis, Alaercio Marajo; da Silva, Osmaildo Ferreira; Pinto, Flavia] Inst Nacl de Pesquisas da Amazonia, BR-69060001 Manaus, Amazonas, Brazil. [Gomez, Marcela Santamaria; dos Reis, Alaercio Marajo; da Silva, Osmaildo Ferreira; Pinto, Flavia] Smithsonian Trop Res Inst, BR-69060001 Manaus, Amazonas, Brazil. [Setz, Eleonore Z. F.] Univ Estadual Campinas, Inst Biol, UNICAMP, BR-13083970 Campinas, SP, Brazil. [Keuroghlian, Alexine] Wildlife Conservat Soc Brazil, BR-79052070 Campo Grande, MS, Brazil. RP Boyle, SA (reprint author), Rhodes Coll, Dept Biol, 2000 North Pkwy, Memphis, TN 38112 USA. EM sarahannboyle@gmail.com; bblenz@gmail.com; kgilbert@selu.edu; wilson@inpa.gov.br; marcesantagomez@gmail.com; setz@unicamp.br; alexinek@hotmail.com; flaviasantospinto@gmail.com NR 44 TC 4 Z9 4 U1 0 U2 11 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-1-4614-8838-5; 978-1-4614-8839-2 J9 DEV PRIMATOL-PROG PR JI Dev Primatol PY 2013 BP 57 EP 74 DI 10.1007/978-1-4614-8839-2_5 D2 10.1007/978-1-4614-8839-2 PG 18 WC Zoology SC Zoology GA BJN10 UT WOS:000329209700008 ER PT J AU Marquez, MA Skog, LE Kvist, LP AF Amaya Marquez, Marisol Skog, Laurence E. Kvist, Lars Peter TI COLUMNEA CAUDATA AND COLUMNEA MEGAFOLIA, TWO NEW SPECIES OF GESNERIACEAE SO CALDASIA LA English DT Article DE Collandra; Columnea; Colombia; Flora of Colombia; Gesneriaceae; Biogeographical Choco; Plant Taxonomy ID BIOTIC INTERACTIONS; COLOMBIAN ANDES; COSTA-RICA AB Two new species of Columnea belonging to section Collandra (Gesneriaceae) from the "cordillera Occidental" in the Colombian Andes are described and illustrated. Columnea caudata is distributed along the Biogeographical Choco in the Departments of Antioquia, Choco, Risaralda, and Valle del Cauca, whereas Columnea megafolia is restricted to Antioquia, and probably is an endemic species of the National Natural Park Las Orquideas. C1 [Amaya Marquez, Marisol] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Skog, Laurence E.] Smithsonian Inst, Dept Bot MRC 166, Washington, DC 20013 USA. [Kvist, Lars Peter] Univ Aarhus, Inst Biol Sci, DK-8000 Aarhus C, Denmark. RP Marquez, MA (reprint author), Univ Nacl Colombia, Inst Ciencias Nat, Apartado 7495, Bogota, Colombia. EM mamayam@unal.edu.co; SKOGL@si.edu; larskvist@biology.au.dk NR 23 TC 2 Z9 2 U1 0 U2 1 PU INST CIENCIAS NATURALES, MUSEO HISTORIA NATURAL PI BOGOTA PA FAC CIENCIAS, UNIV NACIONAL COLOMBIA, APARTADO 7495, BOGOTA, 00000, COLOMBIA SN 0366-5232 J9 CALDASIA JI Caldasia PY 2013 VL 35 IS 2 BP 273 EP 280 PG 8 WC Plant Sciences; Multidisciplinary Sciences; Zoology SC Plant Sciences; Science & Technology - Other Topics; Zoology GA 287UN UT WOS:000329567800004 ER PT S AU Howard, J Babij, E Griffis, R Helmuth, B Himes-Cornell, A Niemier, P Orbach, M Petes, L Allen, S Auad, G Auer, C Beard, R Boatman, M Bond, N Boyer, T Brown, D Clay, P Crane, K Cross, S Dalton, M Diamond, J Diaz, R Dortch, Q Duffy, E Fauquier, D Fisher, W Graham, M Halpern, B Hansen, L Hayum, B Herrick, S Hollowed, A Hutchins, D Jewett, E Jin, D Knowlton, N Kotowicz, D Kristiansen, T Little, P Lopez, C Loring, P Lumpkin, R Mace, A Mengerink, K Morrison, JR Murray, J Norman, K O'Donnell, J Overland, J Parsons, R Pettigrew, N Pfeiffer, L Pidgeon, E Plummer, M Polovina, J Quintrell, J Rowles, T Runge, J Rust, M Sanford, E Send, U Singer, M Speir, C Stanitski, D Thornber, C Wilson, C Xue, Y AF Howard, Jennifer Babij, Eleanora Griffis, Roger Helmuth, Brian Himes-Cornell, Amber Niemier, Paul Orbach, Michael Petes, Laura Allen, Stewart Auad, Guillermo Auer, Carol Beard, Russell Boatman, Mary Bond, Nicholas Boyer, Timothy Brown, David Clay, Patricia Crane, Katherine Cross, Scott Dalton, Michael Diamond, Jordan Diaz, Robert Dortch, Quay Duffy, Emmett Fauquier, Deborah Fisher, William Graham, Michael Halpern, Benjamin Hansen, Lara Hayum, Bryan Herrick, Samuel Hollowed, Anne Hutchins, David Jewett, Elizabeth Jin, Di Knowlton, Nancy Kotowicz, Dawn Kristiansen, Trond Little, Peter Lopez, Cary Loring, Philip Lumpkin, Rick Mace, Amber Mengerink, Kathryn Morrison, J. Ru Murray, Jason Norman, Karma O'Donnell, James Overland, James Parsons, Rost Pettigrew, Neal Pfeiffer, Lisa Pidgeon, Emily Plummer, Mark Polovina, Jeffrey Quintrell, Josie Rowles, Teressa Runge, Jeffrey Rust, Michael Sanford, Eric Send, Uwe Singer, Merrill Speir, Cameron Stanitski, Diane Thornber, Carol Wilson, Cara Xue, Yan BA Smith, IP BF Smith, IP BE Hughes, RN Hughes, DJ TI OCEANS AND MARINE RESOURCES IN A CHANGING CLIMATE SO OCEANOGRAPHY AND MARINE BIOLOGY: AN ANNUAL REVIEW, VOL 51 SE Oceanography and Marine Biology LA English DT Article; Book Chapter ID HARMFUL ALGAL BLOOMS; GULF-OF-MEXICO; SEA-SURFACE TEMPERATURE; SOUTHWESTERN UNITED-STATES; CALIFORNIA CURRENT SYSTEM; NORTHWESTERN HAWAIIAN-ISLANDS; HANTAVIRUS PULMONARY SYNDROME; DOLPHINS TURSIOPS-TRUNCATUS; CARBONATE ION CONCENTRATION; NORTH-ATLANTIC OSCILLATION AB The United States is an ocean nation-our past, present, and future are inextricably connected to and dependent on oceans and marine resources. Marine ecosystems provide many important services, including jobs, food, transportation routes, recreational opportunities, health benefits, climate regulation, and cultural heritage that affect people, communities, and economies across the United States and internationally every day. There is a wealth of information documenting the strong linkages between the planet's climate and ocean systems, as well as how changes in the climate system can produce changes in the physical, chemical, and biological characteristics of ocean ecosystems on a variety of spatial and temporal scales. There is relatively little information on how these climate-driven changes in ocean ecosystems may have an impact on ocean services and uses, although it is predicted that ocean-dependent users, communities, and economies will likely become increasingly vulnerable in a changing climate. Based on our current understanding and future projections of the planet's ocean systems, it is likely that Marine ecosystems will continue to be affected by anthropogenic-driven climate change into the future. This review describes how these impacts are set in motion through a suite of changes in ocean physical, chemical, and biological components and processes in US waters and the significant implications of these changes for ocean users and the communities and economies that depend on healthy oceans. US international partnerships, management challenges, opportunities, and knowledge gaps are also discussed. Effectively preparing for and responding to climate-driven changes in the ocean will require both limiting future change through reductions of greenhouse gases and adapting to the changes that we can no longer avoid. C1 [Howard, Jennifer; Griffis, Roger; Niemier, Paul; Petes, Laura; Auer, Carol; Boyer, Timothy; Clay, Patricia; Fauquier, Deborah; Jewett, Elizabeth; Kristiansen, Trond; Lopez, Cary; Rowles, Teressa] NOAA, Silver Spring, MD 20910 USA. [Babij, Eleanora; Hayum, Bryan] US Fish & Wildlife Serv, Arlington, VA 22203 USA. [Helmuth, Brian] Northeastern Univ, Ctr Marine Sci, Nahant, MA 01908 USA. [Himes-Cornell, Amber; Dalton, Michael; Hollowed, Anne; Little, Peter; Overland, James; Pfeiffer, Lisa] NOAA, Seattle, WA 98115 USA. [Orbach, Michael] Duke Univ, Beaufort, NC 28516 USA. [Allen, Stewart; Kotowicz, Dawn; Pettigrew, Neal] NOAA, Honolulu, HI 96814 USA. [Auad, Guillermo; Boatman, Mary] Bur Ocean Energy Management, Washington, DC 20240 USA. [Beard, Russell; Parsons, Rost] NOAA, Natl Coastal Data Dev Ctr, Stennis Space Ctr, MS 39529 USA. [Bond, Nicholas] Univ Washington, Seattle, WA 98115 USA. [Brown, David] NOAA, Ft Worth, TX 76102 USA. [Crane, Katherine; Stanitski, Diane] NOAA, Silver Spring, MD 20910 USA. [Cross, Scott] NOAA, Charleston, SC 29412 USA. [Diamond, Jordan; Mengerink, Kathryn] Environm Law Inst, Washington, DC 20036 USA. [Diaz, Robert; Duffy, Emmett] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Dortch, Quay] NOAA, Silver Spring, MD 20910 USA. [Fisher, William] US EPA, Natl Hlth & Environm Effects Res Lab, Gulf Breeze, FL 32561 USA. [Graham, Michael] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Halpern, Benjamin] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA. [Hansen, Lara] EcoAdapt, Bainbridge Isl, WA 98110 USA. [Herrick, Samuel] NOAA, La Jolla, CA 92037 USA. [Hutchins, David] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. [Jin, Di] Woods Hole Oceanog Inst, Woods Hole, MA 02543 USA. [Knowlton, Nancy] Smithsonian Inst, Washington, DC 20013 USA. [Kristiansen, Trond] Inst Marine Res, N-5817 Bergen, Norway. [Loring, Philip] Univ Alaska Fairbanks, Fairbanks, AK 99775 USA. [Lumpkin, Rick] NOAA, Miami, FL 33149 USA. [Mace, Amber] Univ Calif Davis, Davis, CA 95616 USA. [Morrison, J. Ru] North East Reg Assoc Coastal & Ocean Observing Sy, Rye, NH 03870 USA. [Murray, Jason] Univ S Carolina, Columbia, SC 29208 USA. [Norman, Karma; Plummer, Mark; Rust, Michael] NOAA, Seattle, WA 98112 USA. [O'Donnell, James] Univ Connecticut, Groton, CT 06340 USA. [Pidgeon, Emily] Conservat Int, Arlington, VA 22202 USA. [Polovina, Jeffrey] NOAA, Honolulu, HI 96822 USA. [Quintrell, Josie; Runge, Jeffrey] Natl Federat Reg Assoc Coastal Observing, Harpswell, ME 04079 USA. [Quintrell, Josie; Runge, Jeffrey] Univ Maine, Portland, ME 04101 USA. [Sanford, Eric] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Send, Uwe] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Singer, Merrill] Univ Connecticut, Storrs, CT 06269 USA. [Speir, Cameron] NOAA, Santa Cruz, CA 95060 USA. [Thornber, Carol] Univ Rhode Isl, Kingston, RI 02881 USA. [Wilson, Cara] NOAA, Pacific Grove, CA 93950 USA. [Xue, Yan] NOAA, Suitland, MD 20746 USA. RP Howard, J (reprint author), NOAA, 1315 East West Hwy, Silver Spring, MD 20910 USA. EM Jennifer.Howard@noaa.gov RI Lumpkin, Rick/C-9615-2009 OI Lumpkin, Rick/0000-0002-6690-1704 NR 771 TC 18 Z9 18 U1 7 U2 59 PU CRC PRESS-TAYLOR & FRANCIS GROUP PI BOCA RATON PA 6000 BROKEN SOUND PARKWAY NW, STE 300, BOCA RATON, FL 33487-2742 USA SN 0078-3218 BN 978-1-4665-6866-2 J9 OCEANOGR MAR BIOL JI Oceanogr. Mar. Biol. PY 2013 VL 51 BP 71 EP 192 PG 122 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA BIF30 UT WOS:000328002700002 ER PT B AU Furlow, NE AF Furlow, Nancy E. BE Wankel, C Pate, L TI STORYTELLING THROUGH INTEGRATED MARKETING COMMUNICATION SO SOCIAL ENTREPRENEURSHIP AS A CATALYST FOR SOCIAL CHANGE SE Research in Management Education and Development LA English DT Article; Book Chapter ID CORPORATE SOCIAL-RESPONSIBILITY; CONSUMERS; FRAMEWORK AB The art of storytelling has been around as long as humans have been able to communicate. From telling stories around a campfire to reading fairy tales at bedtime, we all have an affinity for a good story. We grew up watching children's television programs and sitcoms that, for a short time, held our attention and captivated us while drawing us into the lives of the characters. Just as stories connect us emotionally to television, stories help to develop an emotional bond between social entrepreneur and consumers. For a social enterprise, being able to convey your vision, mission, and values in a compelling way sets you apart from the competition and increases your chance for success. The best way to connect and ultimately bond with consumers is through storytelling. By telling your story you can unite with your customers, donors, clients, and employees on a deeper level and ultimately write your own tale of success. C1 [Furlow, Nancy E.] Marymount Univ, Sch Business Adm, Arlington, VA 22207 USA. [Furlow, Nancy E.] Univ So Mississippi, Hattiesburg, MS 39406 USA. [Furlow, Nancy E.] World Wildlife Fund, Washington, DC 20037 USA. [Furlow, Nancy E.] Smithsonian Inst Natl Zoo, Washington, DC USA. RP Furlow, NE (reprint author), Marymount Univ, Sch Business Adm, Arlington, VA 22207 USA. NR 27 TC 0 Z9 0 U1 0 U2 5 PU INFORMATION AGE PUBLISHING-IAP PI CHARLOTTE PA PO BOX 79049, CHARLOTTE, NC 28271-7047 USA BN 978-1-62396-445-0; 978-1-62396-446-7 J9 RES MANAG EDUC DEV PY 2013 BP 207 EP 221 PG 15 WC Social Issues SC Social Issues GA BJH26 UT WOS:000328172200010 ER PT B AU Udomprasert, PS Goodman, AA Wong, C AF Udomprasert, Patricia S. Goodman, Alyssa A. Wong, Curtis BE Barnes, J Shupla, C Manning, JG Gibbs, MG TI WorldWide Telescope Ambassadors: A Year 3 Update SO COMMUNICATING SCIENCE: A NATIONAL CONFERENCE ON SCIENCE EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Communicating Science - A National Conference on Science Education and Public Outreach CY AUG 04-08, 2012 CL Tucson, AZ SP Astronom Soc Pacific AB We give a brief overview of some key features of WorldWide Telescope and its Ambassadors Program, and we describe two goals for expanding the program in the coming year: scaling up training efforts; and developing "plug and play" Visualization Lab modules that teach key Earth and Space Science concepts to students while emphasizing important scientific processes and skills. We discuss several different ways that members of the astronomy education and outreach community can incorporate WWT-based materials into their work. C1 [Udomprasert, Patricia S.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Udomprasert, PS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 3 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-830-5 J9 ASTR SOC P PY 2013 VL 473 BP 137 EP 140 PG 4 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BJH30 UT WOS:000328179100016 ER PT B AU Henneken, EA AF Henneken, Edwin A. BE Barnes, J Shupla, C Manning, JG Gibbs, MG TI ADS Labs: Supporting Information Discovery in Science Education SO COMMUNICATING SCIENCE: A NATIONAL CONFERENCE ON SCIENCE EDUCATION AND PUBLIC OUTREACH SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Communicating Science - A National Conference on Science Education and Public Outreach CY AUG 04-08, 2012 CL Tucson, AZ SP Astronom Soc Pacific AB The SAO/NASA Astrophysics Data System (ADS) is an open access digital library portal for researchers in astronomy and physics, operated by the Smithsonian Astrophysical Observatory (SAO) under a NASA grant, successfully serving the professional science community for two decades. Currently there are about 55,000 frequent users (100+ queries per year), and up to 10 million infrequent users per year. Access by the general public now accounts for about half of all ADS use, demonstrating the vast reach of the content in our databases. The visibility and use of content in the ADS can be measured by the fact that there are over 17,000 links from Wikipedia pages to ADS content, a figure comparable to the number of links that Wikipedia has to OCLC's WorldCat catalog. The ADS, through its holdings and innovative techniques available in ADS Labs,(1) offers an environment for information discovery that is unlike any other service currently available to the astrophysics community. Literature discovery and review are important components of science education, aiding the process of preparing for a class, project, or presentation. The ADS has been recognized as a rich source of information for the science education community in astronomy, thanks to its collaborations within the astronomy community, publishers and projects like ComPADRE. One element that makes the ADS uniquely relevant for the science education community is the availability of powerful tools to explore aspects of the astronomy literature as well as the relationship between topics, people, observations and scientific papers. The other element is the extensive repository of scanned literature, a significant fraction of which consists of historical literature. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Henneken, EA (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 5 TC 0 Z9 0 U1 0 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-830-5 J9 ASTR SOC P PY 2013 VL 473 BP 207 EP 212 PG 6 WC Astronomy & Astrophysics; Education, Scientific Disciplines SC Astronomy & Astrophysics; Education & Educational Research GA BJH30 UT WOS:000328179100028 ER PT J AU Krupnick, GA McCormick, MK Mirenda, T Whigham, DF AF Krupnick, Gary A. McCormick, Melissa K. Mirenda, Thomas Whigham, Dennis F. TI THE STATUS AND FUTURE OF ORCHID CONSERVATION IN NORTH AMERICA SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article DE Endangered species; Global Strategy for Plant Conservation (GSPC); North American Orchid Conservation Center (NAOCC); Orchidaceae; restoration ID PRAIRIE FRINGED ORCHID; PLATANTHERA-LEUCOPHAEA ORCHIDACEAE; NUTT. LINDLEY; NATIONAL-PARK; POPULATION; DIVERSITY; SEEDLINGS AB The status and trends of issues related to the conservation of orchids native to the United States, Canada, and Greenland are considered. We focus on nine of the 16 Targets of the Global Strategy for Plant Conservation (GSPC). The first two targets, which all other targets rely upon, appear to have been adequately achieved, in addition to Target 11. Limited progress has been made on six other GSPC targets. Three case studies of efforts to conserve the native threatened orchids, Platanthera leucophaea (Nutt.) Lindl., Isotria medeoloides (Pursh) Raf., and Tolumnia bahamensis (Nash) Braem, are presented to demonstrate the difficulties as well as the issues associated with effective conservation. We describe our efforts to establish an international program to conserve all native orchids in the United States and Canada. The North American Orchid Conservation Center (NAOCC) is an internationally focused effort that is based on public-private partnerships. The goal of NAOCC is to conserve the genetic diversity of all native orchids through efforts to develop an international collection of seeds and orchid fungi. The NAOCC also focuses on the cultivation of all native orchids in an international network of botanic gardens, and they partner with private and public landowners to develop techniques to conserve and restore all native orchid species. C1 [Krupnick, Gary A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [McCormick, Melissa K.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Mirenda, Thomas] Smithsonian Inst, Smithsonian Gardens, Washington, DC 20013 USA. RP Krupnick, GA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012,MRC 166, Washington, DC 20013 USA. EM krupnickg@si.edu; mccormickm@si.edu; mirendat@si.edu; whighamd@si.edu OI Krupnick, Gary/0000-0002-1357-4826; Whigham, Dennis/0000-0003-1488-820X FU United States Botanic Garden; Smithsonian Institution; National Park Service [H399207001/J370010018] FX We are thankful to the United States Botanic Garden and the Smithsonian Institution for financial support of the North American Orchid Conservation Center (NAOCC) through a Smithsonian Grand Challenges Award grant. Frank Clements, Vickie Dibella, Tony Dove, Barbara Faust, Christine Flanagan, Jim Kaufmann, John Kress, William McLaughlin, Ray Mims, Jay O'Neill, Holly Shimizu, Teresa Vetick, and Kyle Wallick contributed substantially to discussions about the structure and development of NAOCC. Intern Jean Linsky assisted in collecting data. Information related to the case study description of Isotria medeoloides was obtained during a research project funded by Contract Number H399207001/ J370010018 from the National Park Service. NR 43 TC 2 Z9 2 U1 9 U2 41 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2013 VL 99 IS 2 BP 180 EP 198 DI 10.3417/2011108 PG 19 WC Plant Sciences SC Plant Sciences GA 275FW UT WOS:000328662700008 ER PT J AU Miller, JS Krupnick, GA Stevens, H Porter-Morgan, H Boom, B Acevedo-Rodriguez, P Ackerman, J Kolterman, D Santiago, E Torres, C Velez, J AF Miller, James S. Krupnick, Gary A. Stevens, Hannah Porter-Morgan, Holly Boom, Brian Acevedo-Rodriguez, Pedro Ackerman, James Kolterman, Duane Santiago, Eugenio Torres, Christian Velez, Jeanine TI TOWARD TARGET 2 OF THE GLOBAL STRATEGY FOR PLANT CONSERVATION: AN EXPERT ANALYSIS OF THE PUERTO RICAN FLORA TO VALIDATE NEW STREAMLINED METHODS FOR ASSESSING CONSERVATION STATUS SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article DE Global Strategy for Plant Conservation (GSPC); IUCN Red List; Puerto Rico ID RED LIST; DIVERSITY AB Target 2 of the 2020 Global Strategy for Plant Conservation (GSPC) calls for a comprehensive list of the world's threatened plant species. The lack of such a list is one of the greatest impediments to protecting the full complement of the world's plant species, and work to achieve this has been slow. An efficient system for identifying those species that are at risk of extinction could help to achieve this goal in a timeframe sensitive to today's conservation needs. Two systems that efficiently use available data to assess conservation status were tested against a provisional International Union for Conservation of Nature and Natural Resources (IUCN) Red List analysis to evaluate the native seed plant species of Puerto Rico. It was demonstrated that both systems efficiently identify species at risk, which is a step toward both the GSPC Target 2 and a more comprehensive IUCN Red List for plants. Both systems were effective at identifying plant species at risk, with the New York analysis identifying 98% and the Smithsonian analysis 85% of the plant species considered Threatened in the IUCN Red List. Both analyses to some extent overestimated those plants at risk, but the species identified are all range restricted and, thus, of some conservation interest. C1 [Miller, James S.; Stevens, Hannah; Porter-Morgan, Holly; Boom, Brian] New York Bot Garden, Bronx, NY 10458 USA. [Krupnick, Gary A.; Acevedo-Rodriguez, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Porter-Morgan, Holly] LaGuardia Community Coll, Long Isl City, NY 11101 USA. [Ackerman, James; Santiago, Eugenio] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. [Kolterman, Duane; Velez, Jeanine] Univ Puerto Rico, Dept Biol, Mayaguez, PR 00681 USA. [Santiago, Eugenio] Univ Puerto Rico, San Juan, PR 00936 USA. [Torres, Christian] Forest Serv, USDA, Int Inst Trop Forestry, San Juan, PR 00926 USA. RP Miller, JS (reprint author), New York Bot Garden, 2900 Southern Blvd, Bronx, NY 10458 USA. EM jmiller@nybg.org; krupnickg@si.edu; hannah.i.stevens@gmail.com; hporter-morgan@lagcc.cuny.edu; bboom@nybg.org; acevedop@si.edu; ackennan.upr@hotmail.com; dkolterman@hotmail.com; esantiagoupr@gmail.com; cwtorressantana@fs.fed.us; jeanine.velez@upr.edu OI Krupnick, Gary/0000-0002-1357-4826 FU Prospect Hill Foundation FX We are thankful to Robert and Encarnita Quinlan and the Prospect Hill Foundation for financial support of The New York Botanical Garden's GIS laboratory where some of these analyses were performed. We thank the University of Puerto Rico's Botanical Garden, especially Johanna Delgado, Rafael Davila, and Eugenio Santiago, for hosting the meetings of the expert panels that led to these analyses. The Puerto Rico Department of Natural and Environmental Resources, the Fideicomiso de Conservacion, and Pedro Jimenez were very supportive of these efforts. Our colleagues Alberto Areces, Frank Axelrod, and Peter Weaver contributed substantially to discussions about Puerto Rican endangered plants. We also thank the group of interns at The New York Botanical Garden, Elvio Almonte, James Fleming, Micah Gensler, Angeleta Johnson, Jubril Lawal, and Kristen MacFarlane, and at the Smithsonian Institution, Marie Balboa, John Bly, Anna Braum, Kelsey Brooks, Dana Gadeken, Matthew Johnson, Grace Liu, Holly Markley, Melissa Marshall, Eleanor Moran, Siddharth Rajagopalan, Brittany Roger, Marie lle Saums, Ashley Sullivan, and Linda Yi. NR 30 TC 2 Z9 2 U1 0 U2 3 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 2013 VL 99 IS 2 BP 199 EP 205 DI 10.3417/2011121 PG 7 WC Plant Sciences SC Plant Sciences GA 275FW UT WOS:000328662700009 ER PT S AU Guarcello, MG Drake, JJ Wright, NJ Garcia-Alvarez, D Drew, JE Aldcroft, T Fruscione, A Kashyap, VL AF Guarcello, M. G. Drake, J. J. Wright, N. J. Garcia-Alvarez, D. Drew, J. E. Aldcroft, T. Fruscione, A. Kashyap, V. L. BE MunozTunon, C RodriguezEspinosa, JM TI OSIRIS DEEP IMAGING OF CYGNUS OB2: THE STELLAR POPULATION OF THE CYGNUS X CENTRAL ENGINE SO FOURTH SCIENCE MEETING WITH THE GTC SE Revista Mexicana de Astronomia y Astrofisica-Serie de Conferencias LA English DT Proceedings Paper CT 4th Science with the GTC Meeting CY NOV 16-18, 2011 CL Santa Cruz La Palma, SPAIN DE catalogs; stars: formation; stars: pre-main sequence AB The young massive cluster Cyg OB2 is the closest massive star forming region to the Sun, with hundreds of OB members, and then the best target in the Milky Way to study the feedback of massive stars on the star formation process. To study in detail the stellar population of such a unique target, Cyg OB2 has been observed with GTC/OSIRIS and Chandra/ACIS-I. We present the OSIRIS observations, the catalog and the preliminary scientific results. C1 [Guarcello, M. G.; Drake, J. J.; Wright, N. J.; Aldcroft, T.; Fruscione, A.; Kashyap, V. L.] Smithsonian Astron Observ, Cambridge, MA 02318 USA. RP Guarcello, MG (reprint author), Smithsonian Astron Observ, MS-67,60 Garden St, Cambridge, MA 02318 USA. OI Drew, Janet/0000-0003-1192-7082 NR 7 TC 1 Z9 1 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-607-02-4281-6 J9 REV MEX AST ASTR PY 2013 VL 42 BP 5 EP 7 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BJJ85 UT WOS:000328518900003 ER PT J AU Matte, EM Castilho, CS Miotto, RA Sana, DA Johnson, WE O'Brien, SJ de Freitas, TRO Eizirik, E AF Matte, Eunice M. Castilho, Camila S. Miotto, Renata A. Sana, Denis A. Johnson, Warren E. O'Brien, Stephen J. de Freitas, Thales R. O. Eizirik, Eduardo TI Molecular evidence for a recent demographic expansion in the puma (Puma concolor) (Mammalia, Felidae) SO GENETICS AND MOLECULAR BIOLOGY LA English DT Article DE conservation genetics; mammals; mitochondrial DNA; molecular time estimate; phylogeography ID HUMAN MITOCHONDRIAL-DNA; PHYLOGEOGRAPHIC PATTERNS; POPULATION HISTORY; NEOTROPICAL CATS; SOUTHERN BRAZIL; EVOLUTION; GENETICS; DISPERSAL; SOFTWARE; CONSERVATION AB The puma is an iconic predator that ranges throughout the Americas, occupying diverse habitats. Previous phylogeographic analyses have revealed that it exhibits moderate levels of genetic structure across its range, with few of the classically recognized subspecies being supported as distinct demographic units. Moreover, most of the species' molecular diversity was found to be in South America. To further investigate the phylogeographic structure and demographic history of pumas we analyzed mtDNA sequences from 186 individuals sampled throughout their range, with emphasis on South America. Our objectives were to refine the phylogeographic assessment within South America and to investigate the demographic history of pumas using a coalescent approach. Our results extend previous phylogeographic findings, reassessing the delimitation of historical population units in South America and demonstrating that this species experienced a considerable demographic expansion in the Holocene, ca. 8,000 years ago. Our analyses indicate that this expansion occurred in South America, prior to the hypothesized re-colonization of North America, which was therefore inferred to be even more recent. The estimated demographic history supports the interpretation that pumas suffered a severe demographic decline in the Late Pleistocene throughout their distribution, followed by population expansion and re-colonization of the range, initiating from South America. C1 [Matte, Eunice M.; de Freitas, Thales R. O.] Univ Fed Rio Grande do Sul, Dept Genet, Lab Citogenet & Evolucao, Porto Alegre, RS, Brazil. [Matte, Eunice M.; Eizirik, Eduardo] Pontificia Univ Catolica Rio Grande do Sul, Fac Biociencias, Lab Biol Genom & Mol, BR-90619900 Porto Alegre, RS, Brazil. [Castilho, Camila S.] Univ Sao Paulo, Lab Ecol Paisagem & Conservacao, Sao Paulo, Brazil. [Miotto, Renata A.] Univ Fed Sao Carlos, Dept Genet & Evolucao, Lab Biodiversidade Mol & Citogenet, BR-13560 Sao Carlos, SP, Brazil. [Miotto, Renata A.] Univ Sao Paulo, Escola Super Agr Luiz de Queiroz, Piracicaba, SP, Brazil. [Sana, Denis A.; Eizirik, Eduardo] Inst Procarnivoros, Atibaia, SP, Brazil. [Sana, Denis A.] Univ Fed Rio Grande do Sul, Programa Posgrad Ecol, Porto Alegre, RS, Brazil. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. RP Eizirik, E (reprint author), Pontificia Univ Catolica Rio Grande do Sul, Fac Biociencias, Av Ipiranga 6681,Predio 12, BR-90619900 Porto Alegre, RS, Brazil. EM eduardo.eizirik@pucrs.br RI Eizirik, Eduardo/K-8034-2012; Johnson, Warren/D-4149-2016; OI Eizirik, Eduardo/0000-0002-9658-0999; Johnson, Warren/0000-0002-5954-186X; O'Brien, Stephen J./0000-0001-7353-8301 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil; Companhia Energetica de Sao Paulo (CESP), Brazil; Intramural Research Program of the National Institutes of Health, National Cancer Institute, USA FX We thank C.R. Sarturi, A. Schnorr, A.C.G. Escobar, C.B. Pires, A.T. Hahn, F. Britto, F.G. Grazziotin, T. Haag, T.C. Trigo and T.L.L. Simao for laboratory assistance and helpful discussions regarding data analysis and interpretation, as well as J. Schiefelbain and M.G. da Silva for additional support. This work was funded by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Brazil, and Companhia Energetica de Sao Paulo (CESP), Brazil. Part of this research was also supported by funds from the Intramural Research Program of the National Institutes of Health, National Cancer Institute, USA awarded to WEJ and SJO. NR 49 TC 3 Z9 3 U1 1 U2 25 PU SOC BRASIL GENETICA PI RIBEIRAO PRET PA RUA CAP ADELMIO NORBET DA SILVA, 736, ALTO DA BOA VISTA, 14025-670 RIBEIRAO PRET, BRAZIL SN 1415-4757 EI 1678-4685 J9 GENET MOL BIOL JI Genet. Mol. Biol. PY 2013 VL 36 IS 4 BP 586 EP U164 PG 26 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA 275UI UT WOS:000328702800018 PM 24385863 ER PT J AU Zimmermann, B Zimmermann, A Scheckenbach, HL Schmid, T Hall, JS van Breugel, M AF Zimmermann, B. Zimmermann, A. Scheckenbach, H. L. Schmid, T. Hall, J. S. van Breugel, M. TI Changes in rainfall interception along a secondary forest succession gradient in lowland Panama SO HYDROLOGY AND EARTH SYSTEM SCIENCES LA English DT Article ID LAND-USE CHANGE; CENTRAL KALIMANTAN; HUMID TROPICS; PASTURE; THROUGHFALL; VEGETATION; INDONESIA; RECOVERY; STEMFLOW; CLIMATE AB Secondary forests are rapidly expanding in tropical regions. Yet, despite the importance of understanding the hydrological consequences of land-cover dynamics, the relationship between forest succession and canopy interception is poorly understood. This lack of knowledge is unfortunate because rainfall interception plays an important role in regional water cycles and needs to be quantified for many modeling purposes. To help close this knowledge gap, we designed a throughfall monitoring study along a secondary succession gradient in a tropical forest region of Panama. The investigated gradient comprised 20 forest patches 3 to 130 yr old. We sampled each patch with a minimum of 20 funnel-type throughfall collectors over a continuous 2month period that had nearly 900 mm of rain. During the same period, we acquired forest inventory data and derived several forest structural attributes. We then applied simple and multiple regression models (Bayesian model averaging, BMA) and identified those vegetation parameters that had the strongest influence on the variation of canopy interception. Our analyses yielded three main findings. First, canopy interception changed rapidly during forest succession. After only a decade, throughfall volumes approached levels that are typical for mature forests. Second, a parsimonious (simple linear regression) model based on the ratio of the basal area of small stems to the total basal area outperformed more complex multivariate models (BMA approach). Third, based on complementary forest inventory data, we show that the influence of young secondary forests on interception in realworld fragmented landscapes might be detectable only in regions with a substantial fraction of young forests. Our re-sults suggest that where entire catchments undergo forest regrowth, initial stages of succession may be associated with a substantial decrease of streamflow generation. Our results further highlight the need to study hydrological processes in all forest succession stages, including early ones. C1 [Zimmermann, B.; Zimmermann, A.; Scheckenbach, H. L.] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Golm, Germany. [Schmid, T.] Univ Tubingen, Dept Geosci, D-72074 Tubingen, Germany. [Hall, J. S.; van Breugel, M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zimmermann, A (reprint author), Univ Potsdam, Inst Earth & Environm Sci, Karl Liebknecht Str 24-25, D-14476 Golm, Germany. EM alexander.zimmermann.ii@uni-potsdam.de RI Zimmermann, Alexander/B-6831-2011 FU German Research Foundation [ZI 1300/1-1]; German Academic Exchange Service; HSBC climate partnership; Smithsonian Tropical Research Institute (STRI); Panama Canal Authority (ACP); Frank Levinson Family Foundation; Motta Family Foundation. FX This research was funded by the German Research Foundation (ZI 1300/1-1); additional support came from the German Academic Exchange Service. The Agua Salud Project, where most of the field work was done, was financially supported by the HSBC climate partnership, with additional funding from the Smithsonian Tropical Research Institute (STRI), the Panama Canal Authority (ACP), the Frank Levinson Family Foundation, and the Motta Family Foundation. We wish to thank our team of botanists, technicians, and field assistants. Furthermore, we are grateful to O. Acevedo (STRI), Daniela Weber (STRI), and F. Davies (STRI) for logistical and administrative support. Finally, we appreciate the constructive comments of C. Lenhart, F. Holwerda, M. Coenders-Gerrits, and two anonymous reviewers. NR 52 TC 4 Z9 4 U1 3 U2 64 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1027-5606 EI 1607-7938 J9 HYDROL EARTH SYST SC JI Hydrol. Earth Syst. Sci. PY 2013 VL 17 IS 11 BP 4659 EP 4670 DI 10.5194/hess-17-4659-2013 PG 12 WC Geosciences, Multidisciplinary; Water Resources SC Geology; Water Resources GA 263IG UT WOS:000327800700025 ER PT J AU Mathis, WN Zatwarnicki, T AF Mathis, Wayne N. Zatwarnicki, Tadeusz TI A revision of the shore-fly genus Hydrochasma Hendel (Diptera, Ephydridae) SO ZOOKEYS LA English DT Article DE Diptera; Ephydridae; Hydrochasma sp n.; New World ID FLIES AB A revision of the shore fly genus Hydrochasma Hendel. The species of the genus Hydrochasma Hendel are revised, including 27 new species (type locality in parenthesis): H. andeum (Ecuador. Guayas: Boliche (02 degrees 07.7' S, 79 degrees 35.5'W)), H. annae (United States. Utah. Grand: Swasey Beach (15.3 km N Green River; 39 degrees 07'N, 110 degrees 06.6'W; Green River; 1255 m)), H. capsum (Ecuador. Orellana: RioTiputini (0 degrees 38.2'S, 76 degrees 8.9'W)), H. castilloi (Ecuador. Loja: Catamayo (03 degrees 59'S, 79 degrees 21'W)), H. crenulum (Peru. Cuzco: Paucartambo, Atalaya (Rio Alto Madre de Dios; 12 degrees 53.3'S, 71 degrees 21.6'W; 600 m)), H. denticum (Ecuador. Orellana: Rio Tiputini (0 degrees 38.2'S, 76 degrees 8.9'W)), H. digitatum (Peru. Madre de Dios: Diamante (Rio Alto Madre de Dios; 12 degrees 19.9'S, 70 degrees 57.5'W; 400 m)), H. distinctum (Costa Rica. Limon: Parque Nacional Barbilla, Sector Casas Negras, (10 degrees 0.8'N, 83 degrees 28.1'W; 300 m)), H. dolabrutum (Dominican Republic. Barahona: Barahona (18 degrees 12'N, 71 degrees 5.3'W)), H. edmistoni (Dominican Republic. Azua: near Pueblo Viejo (18 degrees 24.8'N, 70 degrees 44.7'W)), H. falcatum (Peru. Madre de Dios: Rio Manu, Erika (near Salvacion; 12 degrees 50.7'S, 71 degrees 23.3'W; 550 m)), H. glochium (Dominican Republic. Peravia: San Jose Ocoa (10 km NE; 18 degrees 35'N, 70 degrees 25.6'W)), H. kaieteur (Guyana. Kaieteur Falls (05 degrees 10.5'N, 59 degrees 26.9'W)), H. lineatum (Trinidad and Tobago. Trinidad. St. George: Filette (1 km SE; 10 degrees 47'N, 61 degrees 21'W)), H. miguelito (Honduras. Cortes: San Pedro Sula (8 km S; 15 degrees 25.7'N, 88 degrees 01.4'W)), H. octogonum (Ecuador. Manabi: Pichincha (01 degrees 02.7'S, 79 degrees 49.2'W)), H. parallelum (Trinidad and Tobago. Trinidad. St. Andrew: Lower Manzanilla (16 km S; 10 degrees 22'N, 61 degrees 01'W)), H. peniculum (Dominican Republic. Pedernales: Pedernales (18 degrees 01.8'N, 71 degrees 44.7'W)), H. rictum (Honduras. Cortes: San Pedro Sula (8 km S; 15 degrees 25.7'N, 88 degrees 01.4'W)), H. robustum (Brazil. Sao Paulo. Ubatuba, Praia Puruba (23 degrees 21'S, 44 degrees 55.6'W; beach)), H. sagittarium (Trinidad and Tobago. Tobago: St. John: Parlatuvier (creek; 11 degrees 17.9'N, 60 degrees 35'W)), H. simplicum (Costa Rica. Limon: Parque Nacional Barbilla, Sector Casas Negras, (10 degrees 01.2'N, 83 degrees 26.2'W; 300 m)), H. sinuatum (Belize. Stann Creek: Mullins Creek (17 km N Dangriga; 17 degrees 06.2'N, 88 degrees 17.8'W)), H. spinosum (Costa Rica. Limon: Westfalia (4 km S; 09 degrees 54.5'N, 82 degrees 59'W; beach)), H. urnulum (Dominican Republic. Puerto Plata: Rio Camu (14 km E Puerto Plata; 19 degrees 41.9'N, 70 degrees 37.5'W)), H. viridum (Guyana. Karanambo, Rupununi River (ox bow; 03 degrees 45.1'N, 59 degrees 18.6'W)), H. williamsae (Belize. Stann Creek: Mullins River (17 km N Dangriga; 17 degrees 06.2'N, 88 degrees 17.8'W)). All known species are described with an emphasis on structures of the male terminalia, which are fully illustrated. Detailed locality data and distribution maps for all species are provided. A lectotype is designated for Discocerina incisum Coquillett and Hydrochasma zernyi Hendel. For perspective and to facilitate genus-group and species-group recognition, the tribe Discocerinini is diagnosed and a key to included genera in the New World is provided. C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Zatwarnicki, Tadeusz] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathisw@si.edu OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 FU Caribbean Coral Reef Ecosystems (CCRE); Smithsonian Institution; Exxon Corporation; Smithsonian Institution's Biological Diversity of the Guianas Program; SYNTHESYS [FR-TAF-4729, GB-TAF-1782]; European Community Research Infrastructure Action under the FP7 "Capacities" Program; Sabrosky Fund (Smithsonian Institution); CNPq [401609/2009-0]; National Park Service; Williston Fund (Smithsonian Institution) FX Funding for field work in Belize was provided by the Caribbean Coral Reef Ecosystems (CCRE), Smithsonian Institution (Klaus Rutzler, former director; Scott Jones, Program Coordinator). This is contribution number 945 of the CCRE project, which is partially supported by a grant from the Exxon Corporation. Field work in Guyana (1994, 1995, 1997, 2010) was supported by the Smithsonian Institution's Biological Diversity of the Guianas Program (Vicki A. Funk, Director; Carol Kelloff, Coordinator), and this contribution is number 201 in the Smithsonian's Biological Diversity of the Guiana Shield publication series.; Funding for this research project, especially the field work on islands of the West Indies, in southern California (2003), in Texas (2004), in Idaho, Oregon, and Washington (2006) was funded largely by grants from the Biodiversity Program (Biological Surveys and Inventories, BSI), National Museum of Natural History, Smithsonian Institution (Lynne R. Parenti and George Zug, chairs). Field work on the West Indies was greatly expedited through the able and pleasant assistance of Dianne Mathis, Amnon Freidberg (collector nonpareil of Diptera), Hollis B. Williams, Kelvin Guerrero, Volker Hollmann, Oliver S. Flint, Jr. (whose enthusiasm for collecting was catching), and Daniel Perez G. T. Zatwarnicki received research support from the SYNTHESYS Projects FR-TAF-4729 and GB-TAF-1782, which is financed by the European Community Research Infrastructure Action under the FP7 "Capacities" Program. Visits to museums and production of illustrations and photographs were partially supported by the Sabrosky Fund (Smithsonian Institution), especially the financial contributions to that fund by Ms Hollis B. Williams.; Recent field work in Brazil (December 2009-June 2010) that resulted in the vast majority of Brazilian specimens studied in this paper was supported by a grant from CNPq (Visiting Researcher/Process number 401609/2009-0), which we gratefully acknowledge and thank. We thank Dianne Mathis for helping with all aspects of the production of this paper, especially the field work in Brazil. We also thank A. Bernardo Carvalho and his lab (Elisa, Monica, Susana) for hosting us while conducting field work along the coast of Sao Paulo.; Field work in the George Washington Memorial Parkway was supported by a grant from the National Park Service, and we especially thank Brent W. Steury for his assistance, facilitation, and support. We also acknowledge the financial support of the Williston Fund (Smithsonian Institution), especially for study of specimens in other museums during the summers of 2007, 2008, and 2009. NR 37 TC 4 Z9 5 U1 0 U2 5 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 363 SI SI BP 1 EP 161 DI 10.3897/zookeys.363.6482 PG 161 WC Zoology SC Zoology GA 272YR UT WOS:000328499900001 PM 24363601 ER PT S AU de Forges, BR Chan, TY Corbari, L Lemaitre, R Macpherson, E Ahyong, ST Ng, PKL AF de Forges, Bertrand Richer Chan, Tin-Yam Corbari, Laure Lemaitre, Rafael Macpherson, Enrique Ahyong, Shane T. Ng, Peter K. L. BE Ahyong, ST Chan, TY Corbari, L Ng, PKL TI The MUSORSTOM-TDSB deep-sea benthos exploration programme (1976-2012): An overview of crustacean discoveries and new perspectives on deep-sea zoology and biogeography SO TROPICAL DEEP-SEA BENTHOS, VOL 27 SE Memoires du Museum National d Histoire Naturelle LA English DT Article; Book Chapter ID INDO-WEST PACIFIC; DECAPODA BRACHYURA MAJOIDEA; SPECIES GROUP CRUSTACEA; NEW-CALEDONIA CRUSTACEA; GENERA MUNIDA LEACH; A. MILNE-EDWARDS; PAPUA-NEW-GUINEA; CRABS CRUSTACEA; FRENCH-POLYNESIA; SOLOMON-ISLANDS C1 [de Forges, Bertrand Richer] Kiwa Consulting, Noumea 98800, New Caledonia. [Chan, Tin-Yam] Natl Taiwan Ocean Univ, Inst Marine Biol, Keelung 20224, Taiwan. [Chan, Tin-Yam] Natl Taiwan Ocean Univ, Ctr Excellence Oceans, Keelung 20224, Taiwan. [Corbari, Laure] Museum Natl Hist Nat, Dept Systemat & Evolut, F-75005 Paris, France. [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Macpherson, Enrique] CSIC, CEAB, Blanes 17300, Girona, Spain. [Ahyong, Shane T.] Australian Museum, Sydney, NSW 2010, Australia. [Ng, Peter K. L.] Natl Univ Singapore, Trop Marine Sci Inst, Singapore 119260, Singapore. [Ng, Peter K. L.] Natl Univ Singapore, Dept Biol Sci, Singapore 119260, Singapore. RP de Forges, BR (reprint author), Kiwa Consulting, 5 Rue Felix Franchette, Noumea 98800, New Caledonia. EM b.richerdeforges@gmail.com; corbari@mnhn.fr; lemaitrr@si.edu; macpherson@ceab.csic.es; Shane.Ahyong@austmus.gov.au; peterng@nus.edu.sg NR 208 TC 6 Z9 6 U1 0 U2 1 PU PUBLICATIONS SCIENTIQUES DU MUSEUM PI PARIS PA 57 RUE CUVIER, 75005 PARIS, FRANCE SN 1243-4442 BN 978-2-85653-692-6 J9 MEM MUS NAT HIST NAT JI Mem. Mus. Natl. Hist. Nat. PY 2013 VL 204 BP 13 EP 66 PG 54 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA BIE73 UT WOS:000327902200002 ER PT S AU Lemaitre, R AF Lemaitre, Rafael BE Ahyong, ST Chan, TY Corbari, L Ng, PKL TI The genus Paragiopagurus Lemaitre, 1996 (Crustacea, Decapoda, Anomura, Paguroidea, Parapaguridae): A worldwide review and summary, with descriptions of five new species SO TROPICAL DEEP-SEA BENTHOS, VOL 27 SE Memoires du Museum National d Histoire Naturelle LA English DT Article; Book Chapter ID HERMIT-CRAB; ATLANTIC; PACIFIC; ISLANDS; BIOLOGY; CRUISE; SMITH; BALSS AB A review of the deep-water hermit crab species of the genus Paragiopagurus Lemaitre, 1996 from the world oceans is presented. The core specimen base for this study has come primarily from the abundant collections of species of this genus obtained during French campaigns over the last four decades, and complemented with numerous specimens from many other deep-sea expeditions and deposited in various museum holdings around the world. Paragiopagurus is one of the most speciose genus among the Parapaguridae Smith, 1882, although it is considered a phylogenetically heterogeneous assemblage and does not appear to have an apomorphy of its own. Bathymetrically, the species range in depth from 36 to 2034 m, although they occur most frequently between 200 and 1000 m. The species utilize as housing, gastropod shells (or rarely scaphopod shells, siliceous sponges, or hollow pieces of wood) that may or may not be colonized by actinians or zoanthids. In this review, 24 species are recognized, of which five are new, P laperousei n. sp., P orthotenes n. sp., P. oxychelos n. sp., P. trilineatus n. sp., and P umbonatus n. sp. The new species are fully described and illustrated. All previously known species of the genus are diagnosed or redescribed, and previously published illustrations of important taxonomic characters assembled and complemented, when useful, with new illustrations. The treatment of each species includes a full synonymy, materials examined (type and non-types), colouration, habitat or type of housing used, distribution, and remarks on taxonomy and morphological affinities. Colour photographs are included for 14 of the species. Parapagurus curvispina de Saint Laurent, 1974, a species tentatively moved after its description to Sympagurus Smith, 1883 and then to Paragiopagurus, is herein transferred with certainty to Oncopagurus Lemaitre, 1996. Parapagurus spinimanus Balss, 1911, a species that had been incorrectly placed in Paragiopagurus, is herein moved to Sympagurus. Parapagurus sculptochela Zarenkov, 1990, a taxon previously considered a junior synonym of Paragiopagurus boletifer (de Saint Laurent, 1972), is herein resurrected as a valid species of Paragiopagurus. The bathymetric and geographic distributions of Paragiopagurus species are summarized and briefly discussed, including a summary table, graph, and map with generalized distribution patterns. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu NR 97 TC 1 Z9 1 U1 0 U2 0 PU PUBLICATIONS SCIENTIQUES DU MUSEUM PI PARIS PA 57 RUE CUVIER, 75005 PARIS, FRANCE SN 1243-4442 BN 978-2-85653-692-6 J9 MEM MUS NAT HIST NAT JI Mem. Mus. Natl. Hist. Nat. PY 2013 VL 204 BP 311 EP 421 PG 111 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA BIE73 UT WOS:000327902200011 ER PT J AU Erwin, TL Amundson, LM AF Erwin, Terry L. Amundson, Lauren M. TI Beetles that live with ants (Carabidae, Pseudomorphini, Pseudomorpha Kirby, 1825): A revision of the santarita species group SO ZOOKEYS LA English DT Article DE False-form beetles; new species; new species groups; identification key; distributions; male genitalia; female ovipositor; Hymenoptera: Formicidae ID COLEOPTERA; GENUS AB The Western Hemisphere genus Pseudomorpha Kirby 1825 was last revised by Notman in 1925 based on only a few known species (22) and paltry few specimens (73); other authors have added an additional six species represented by 53 additional specimens since 1925. Baehr (1997) assigned three species from Australia to this genus, albeit in a new subgenus, Austropseudomorpha Baehr 1997. A recent study of collections from throughout the Americas (1757 specimens) has revealed numerous new species that can be arrayed across 19 species groups based on a suite of attributes, some used by Notman and others newly discovered. A taxonomic revision of the species contained in one of these species groups, santarita, is provided herein, as well as a distributional synopsis of the remaining 18 species groups. New species described herein are as follows, each with its type locality: Pseudomorpha huachinera sp. n., Arroyo El Cocono, Sierra Huachinera, Sonora, Mexico; P. patagonia sp. n., Madera Canyon, Santa Rita Mountains, Arizona; P. penablanca sp. n., Pena Blanca Lake, Arizona; P. pima sp. n., Madera Canyon (lower), Santa Rita Mountains, Arizona; P. santacruz sp. n., Madera Canyon, Santa Rita Mountains, Arizona; and P. santarita sp. n., Santa Rita Ranch, Santa Rita Mountains, Arizona. C1 [Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, MRC 187, Hyper Divers Grp,Dept Entomol, Washington, DC 20013 USA. [Amundson, Lauren M.] Smithsonian Inst, Natl Museum Nat Hist, MRC 187, Dept Entomol,Hyper Divers Grp Summer Intern, Washington, DC 20013 USA. RP Erwin, TL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 187, Hyper Divers Grp,Dept Entomol, POB 37012, Washington, DC 20013 USA. EM erwint@si.edu NR 26 TC 0 Z9 0 U1 0 U2 7 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 362 BP 29 EP 54 DI 10.3897/zookeys.362.6300 PG 26 WC Zoology SC Zoology GA 272YN UT WOS:000328499500002 PM 24363599 ER PT J AU Kanzaki, N Giblin-Davis, RM Ye, WM Herre, EA Center, BJ AF Kanzaki, Natsumi Giblin-Davis, Robin M. Ye, Weimin Herre, Edward Allen Center, Barbara J. TI Description of Parasitodiplogaster pharmaconema n. sp and redescription of P-maxinema from Ficus maxima Mill. (Moraceae) SO NEMATOLOGY LA English DT Article DE fig tree; molecular; morphology; morphometrics; new species; Panama; phylogeny; stomatal dimorphism; taxonomy ID BEETLE-ASSOCIATED NEMATODES; FIG WASPS; DIPLOGASTRIDAE; DIVERSITY; AUSTRALIA; AGAONIDAE; PARASITE; SYCONIA AB Parasitodiplogaster species associated with Ficus maxima were surveyed at the Smithsonian Tropical Research Institute, Barro Colorado Island, Panama. Phase B-D syconia were collected from different trees and dissected in distilled water. Because there were different nematode stomatal and male morphotypes observed in a single sycone, nematodes isolated from each fig were observed to determine general morphotype class and stored individually in DNA extraction buffer for accurate morpho/molecular pairing. Additional voucher nematodes were gently heat-treated and fixed in formalin and processed into permanent mounts in dehydrated glycerin for more rigorous morphological examination. The survey yielded two different Parasitodiplogaster species: P. maxinema and P. pharmaconema n. sp. Several morphological characters, e.g., two long and stick-like teeth in the metastegostom, and stomatal dimorphism (presence of eurystomatous form) which were not previously described, were observed in P. maxinema and are ascribed hereto this species. Parasitodiplogaster pharmaconema n. sp. is morphologically similar to P. maxinema and P. yoponema but can be distinguished from these species based upon stomatal morphology, spicule and gubernaculum morphology, and number and arrangement of male genital papillae. C1 [Kanzaki, Natsumi] Forestry & Forest Prod Res Inst, Forest Pathol Lab, Tsukuba, Ibaraki 3058687, Japan. [Kanzaki, Natsumi; Giblin-Davis, Robin M.; Center, Barbara J.] Univ Florida, Ft Lauderdale Res & Educ Ctr, Davie, FL 33314 USA. [Ye, Weimin] North Carolina Dept Agr & Consumer Serv, Div Agron, Nematode Assay Sect, Raleigh, NC 27607 USA. [Herre, Edward Allen] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Kanzaki, N (reprint author), Forestry & Forest Prod Res Inst, Forest Pathol Lab, 1 Matsunosato, Tsukuba, Ibaraki 3058687, Japan. EM nkanzaki@affrc.go.jp FU National Science Foundation (NSF) Biotic Surveys and Inventories projects [DEB-0450537, DEB-0640807]; Ministry of Education, Culture, Sports, Science and Technology, Japan [21770094] FX This study was supported in part by National Science Foundation (NSF) Biotic Surveys and Inventories projects (DEB-0450537; DEB-0640807) and Grant-in-Aid for Young Scientists (B) (No. 21770094) from The Ministry of Education, Culture, Sports, Science and Technology, Japan. Special thanks to Dr Kerrie A. Davies for valuable comments on the earlier version of this manuscript and Dr Annette Aiello for processing specimens for the collections in Panama. NR 30 TC 8 Z9 8 U1 1 U2 5 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1388-5545 J9 NEMATOLOGY JI Nematology PY 2013 VL 15 BP 957 EP 974 DI 10.1163/15685411-00002735 PN 8 PG 18 WC Zoology SC Zoology GA 267YF UT WOS:000328133600007 ER PT S AU Gregory, LT Norconk, MA AF Gregory, L. Tremaine Norconk, Marilyn A. BE Barnett, AA Veiga, LM Ferrari, SF Norconk, MA TI Comparative socioecology of sympatric, free-ranging white-faced and bearded saki monkeys in Suriname: preliminary data SO EVOLUTIONARY BIOLOGY AND CONSERVATION OF TITIS, SAKIS AND UACARIS SE Cambridge Studies in Biological and Evolutionary Anthropology LA English DT Article; Book Chapter ID GENUS PITHECIA CEBIDAE; SPIDER MONKEYS; PRIMATES; PATTERNS; BEHAVIOR; ADAPTATIONS; CHIROPOTES; FRUGIVORY; EVOLUTION; DIETARY C1 [Gregory, L. Tremaine] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20008 USA. [Norconk, Marilyn A.] Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. RP Gregory, LT (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20008 USA. NR 56 TC 2 Z9 2 U1 0 U2 4 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1746-2266 BN 978-0-521-88158-6 J9 CAM S BIO EVOL ANTHR JI CAMBR STUD BIO EVOL ANTHROPOL PY 2013 VL 65 BP 285 EP 294 D2 10.1017/CBO9781139034210 PG 10 WC Evolutionary Biology SC Evolutionary Biology GA BHL11 UT WOS:000325761700033 ER PT J AU Lobo, E Dalling, JW AF Lobo, E. Dalling, J. W. TI Effects of topography, soil type and forest age on the frequency and size distribution of canopy gap disturbances in a tropical forest SO BIOGEOSCIENCES LA English DT Article ID LOWLAND RAIN-FOREST; PHASE REGENERATION; MOIST FOREST; IVORY-COAST; TREE; DYNAMICS; DIVERSITY; MORTALITY; LIANAS; CARBON AB Treefall gaps are the major source of disturbance in most tropical forests. The frequency and size of these gaps have important implications for forest ecosystem processes as they can influence the functional trait distribution of tree communities, stand-level aboveground biomass and productivity. However, we still know little about the relative importance of environmental drivers of gap disturbance regimes because existing studies vary greatly in criteria used for defining gaps, in the spatial extent of the study area, and the spatial resolution of canopy height measurements. Here we use lidar (light detecting and ranging) to explore how forest age, topography and soil type affect canopy disturbance patterns across a 1500 ha tropical forest landscape in central Panama. We characterize disturbance based on the frequency distribution of gap sizes (the "gap size distribution"), and the area of the forest affected by gaps (the "gap area fraction"). We found that slope and forest age had significant effects on the gap size distribution, with a higher frequency of large gaps associated with old-growth forests and more gentle slopes. Slope and forest age had similar effects on the gap area fraction, however gap area fraction was also affected by soil type and by aspect. We conclude that variation in disturbance patterns across the landscape can be linked to factors that act at the fine scale (such as aspect or slope), and factors that show heterogeneity at coarser scales (such as forest age or soil type). Awareness of the role of different environmental factors influencing gap formation can help scale up the impacts of canopy disturbance on forest communities measured at the plot scale to landscape and regional scales. C1 [Lobo, E.; Dalling, J. W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Lobo, E.] DMCii, Guildford GU2 7AG, Surrey, England. [Dalling, J. W.] Ancon, Smithsonian Trop Res Inst, Panama City, Panama. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM dalling@illinois.edu FU NSF [0939907]; Smithsonian Tropical Research Institute; University of Illinois; University of California Los Angeles; Clemson University FX This study was funded by NSF grant 0939907, and with additional support from the Smithsonian Tropical Research Institute, University of Illinois, University of California Los Angeles, and Clemson University. We thank G. Z. Gertner for assistance with data analysis and Joe Wright and Patrick Jansen for providing the 25 ha plot data set. NR 48 TC 4 Z9 4 U1 3 U2 44 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 EI 1726-4189 J9 BIOGEOSCIENCES JI Biogeosciences PY 2013 VL 10 IS 11 BP 6769 EP 6781 DI 10.5194/bg-10-6769-2013 PG 13 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 263NG UT WOS:000327814700001 ER PT J AU Erwin, TL AF Erwin, Terry L. TI Beetles that live with ants (Coleoptera, Carabidae, Pseudomorphini): A remarkable new genus and species from Guyane (French Guiana), Guyanemorpha spectabilis gen. n., sp n. SO ZOOKEYS LA English DT Article DE False-form beetles; identification key; distribution; male genitalia; female ovipositor; Hymenoptera: Formicidae ID CICINDINI AB Among the extensive collections currently being made in Guyane (French Guiana), adults of a large and colorful species of pseudomorphine were encountered. The adults present, for the first time in the Western Hemisphere, elytra with a marked color pattern, and in addition a size considerably beyond that of the rest of the members of all other known genera in the Western Hemisphere. Both of these attributes, however, are well known in the Australian pseudomorphine fauna. This new species is described and illustrated and a revised key to the Western Hemisphere genera is included. The type locality of Guyanemorpha spectabilis gen. n., sp. n. is Guyane, Risquetout, PK20, 4.916 degrees N, 52.516 degrees W, 12m altitude. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Hyperdivers Grp, Washington, DC 20013 USA. RP Erwin, TL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Hyperdivers Grp, MRC 187,POB 37012, Washington, DC 20013 USA. EM erwint@si.edu NR 24 TC 2 Z9 2 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 358 BP 11 EP 23 DI 10.3897/zookeys.358.6298 PG 13 WC Zoology SC Zoology GA 263OO UT WOS:000327818100002 PM 24363582 ER PT J AU Sues, HD Hook, RW Olsen, PE AF Sues, Hans-Dieter Hook, Robert W. Olsen, Paul E. TI Donald Baird and his discoveries of Carboniferous and early Mesozoic vertebrates in Nova Scotia SO ATLANTIC GEOLOGY LA English DT Article ID GREERERPETON-BURKEMORANI ROMER; CRANIAL MORPHOLOGY; TETRAPOD; CANADA; AMPHIBIA AB Donald Baird (1926-2011), an influential and innovative vertebrate paleontologist with a scientific career spanning nearly 50 years, had an exceptional breadth of expertise in the study of late Paleozoic and Mesozoic vertebrates and their life traces. Beginning in 1956, Baird conducted fieldwork in the Carboniferous and Triassic-Jurassic of Nova Scotia, making a total of 21 trips in 30 years. His many scientific contributions include the discoveries of important assemblages of Carboniferous vertebrates as well as an unexpectedly diverse record of early Mesozoic tetrapods and their trackways in the province. Baird also encouraged and supported fieldwork by other vertebrate paleontologists as well as amateurs in Nova Scotia and elsewhere. His career-long commitment to the vertebrate paleontology of the province was instrumental in establishing it as an important source of fossils of Carboniferous and early Mesozoic continental vertebrates. C1 [Sues, Hans-Dieter] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hook, Robert W.] Univ Texas Austin, Vertebrate Paleontol Lab, Austin, TX 78758 USA. [Olsen, Paul E.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Sues, HD (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu NR 65 TC 2 Z9 2 U1 0 U2 5 PU ATLANTIC GEOSCIENCE SOC PI WOLFVILLE PA ACADIA UNIV, DEPT GEOLOGY, PO BOX 116, WOLFVILLE, NS B0P 1X0, CANADA SN 0843-5561 EI 1718-7885 J9 ATL GEOL JI Atl. Geol. PY 2013 VL 49 BP 90 EP 103 DI 10.4138/atlgeol.2013.004 PG 14 WC Geology SC Geology GA 257YI UT WOS:000327423300005 ER PT J AU Liu, G Liu, J Tarasick, DW Fioletov, VE Jin, JJ Moeini, O Liu, X Sioris, CE Osman, M AF Liu, G. Liu, J. Tarasick, D. W. Fioletov, V. E. Jin, J. J. Moeini, O. Liu, X. Sioris, C. E. Osman, M. TI A global tropospheric ozone climatology from trajectory-mapped ozone soundings SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID BREWER-MAST; INTERCOMPARISON CAMPAIGN; ELECTROCHEMICAL SONDES; SATELLITE DATA; WATER-VAPOR; MODEL; TRANSPORT; ACCURACY; CELL; UNCERTAINTIES AB A global three-dimensional (i.e. latitude, longitude, altitude) climatology of tropospheric ozone is derived from the ozone sounding record by trajectory mapping. Approximately 52 000 ozonesonde profiles from more than 100 stations worldwide since 1965 are used. The small number of stations results in a sparse geographical distribution. Here, forward and backward trajectory calculations are performed for each sounding to map ozone measurements to a number of other locations, and so to fill in the spatial domain. This is possible because the lifetime of ozone in the troposphere is of the order of weeks. This physically based interpolation method offers obvious advantages over typical statistical interpolation methods. The trajectory-mapped ozone values show reasonable agreement, where they overlap, to the actual soundings, and the patterns produced separately by forward and backward trajectory calculations are similar. Major regional features of the tropospheric ozone distribution are clearly evident in the global maps. An interpolation algorithm based on spherical functions is further used for smoothing and to fill in remaining data gaps. The resulting three-dimensional global tropospheric ozone climatology facilitates visualization and comparison of different years, decades, and seasons, and offers some intriguing insights into the global variation of tropospheric ozone. It will be useful for climate and air quality model initialization and validation, and as an a priori climatology for satellite data retrievals. Further division of the climatology into decadal and annual averages can provide a global view of tropospheric ozone changes, although uncertainties with regard to the performance of older sonde types, as well as more recent variations in operating procedures, need to be taken into account. C1 [Liu, G.; Tarasick, D. W.; Fioletov, V. E.; Sioris, C. E.; Osman, M.] Environm Canada, Air Qual Res Div, Toronto, ON M3H 5T4, Canada. [Liu, J.] Univ Toronto, Dept Geog, Toronto, ON M5S 3G3, Canada. [Liu, J.] Univ Toronto, Program Planning, Toronto, ON M5S 3G3, Canada. [Jin, J. J.; Moeini, O.] York Univ, Dept Earth & Space Sci & Engn, Toronto, ON M3J 1P3, Canada. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Tarasick, DW (reprint author), Environm Canada, Air Qual Res Div, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. EM david.tarasick@ec.gc.ca RI Jin, Jianjun/G-8357-2012; Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Fioletov, Vitali/0000-0002-2731-5956; Sioris, Christopher/0000-0003-1168-8755; Tarasick, David/0000-0001-9869-0692 FU World Meteorological Organization FX The authors thank the many observers who, over many years, obtained the ozonesonde measurements used in this study. Their careful work is gratefully acknowledged. The global ozone sounding data were obtained from the World Ozone and Ultraviolet Radiation Data Centre (WOUDC, http://www.woudc.org) operated by Environment Canada, Toronto, Ontario, Canada, under the auspices of the World Meteorological Organization. We also gratefully acknowledge the the NOAA Air Resources Laboratory (ARL) for the provision of the trajectory model HYSPLIT (Hybrid Single Particle Lagrangian Integrated Trajectory Model) (http://www.arl.noaa.gov/ready.html), and the NOAA Physical Sciences Division for the NCEP/NCAR reanalysis data (http://www.esrl.noaa.gov/psd/data/reanalysis/reanalysis.shtml). NR 77 TC 7 Z9 7 U1 1 U2 13 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2013 VL 13 IS 21 BP 10659 EP 10675 DI 10.5194/acp-13-10659-2013 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 253PP UT WOS:000327101900007 ER PT B AU Wang, Z AF Wang, Zhong BE Sun, WH Xu, KC Scoville, NZ Sanders, DB TI Connecting the Dots between the Antennae and Arp 220 SO GALAXY MERGERS IN AN EVOLVING UNIVERSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on Galaxy Mergers in an Evolving Universe CY OCT 23-28, 2011 CL Hualien, TAIWAN SP Natl Sci Council Taiwan, Natl Sci Fdn US, Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys ID LUMINOUS INFRARED GALAXIES; DUST; GAS AB The late stages of a merger between two gas-rich galaxies are often characterized by a high concentration of dense gas and active starbursts near the nuclear region. We are continuing a comprehensive study of such systems in the local universe, focusing on the detailed observations of the molecular gas component and its relationship to the on-going star formation. We compare these to active star-forming regions in nearby galaxies in order to better understand the underlying physical processes. C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Wang, Z (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-838-1 J9 ASTR SOC P PY 2013 VL 477 BP 55 EP 58 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BIB57 UT WOS:000327278600009 ER PT B AU Torrey, P Cox, TJ Kewley, L Hernquist, L AF Torrey, Paul Cox, T. J. Kewley, Lisa Hernquist, Lars BE Sun, WH Xu, KC Scoville, NZ Sanders, DB TI The Metallicity Evolution of Interacting Galaxies SO GALAXY MERGERS IN AN EVOLVING UNIVERSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on Galaxy Mergers in an Evolving Universe CY OCT 23-28, 2011 CL Hualien, TAIWAN SP Natl Sci Council Taiwan, Natl Sci Fdn US, Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys AB Nuclear inflows of metal-poor interstellar gas triggered by galaxy interactions can account for the systematically lower central oxygen abundances observed in local interacting galaxies. We investigate the metallicity evolution of a large set of simulations of colliding galaxies with numerical simulations including cooling, star formation, feedback, and mass recycling. We focus on the influence of merger-induced inflows and chemical enrichment in determining the nuclear metallicity evolution. We find an average depression in the nuclear metallicity of similar to 0.07 for gas-poor-disk-disk interactions. The simulations fare reasonably well when compared to the observed mass-metallicity and separation-metallicity relationships. C1 [Torrey, Paul; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, T. J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Kewley, Lisa] Mt Stromlo & Siding Spring Observ, Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Torrey, P (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 6 TC 1 Z9 1 U1 1 U2 3 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-838-1 J9 ASTR SOC P PY 2013 VL 477 BP 237 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BIB57 UT WOS:000327278600042 ER PT B AU Scudder, JM Patton, DR Ellison, SL Torrey, P Mendel, JT AF Scudder, Jillian M. Patton, David R. Ellison, Sara L. Torrey, Paul Mendel, J. Trevor BE Sun, WH Xu, KC Scoville, NZ Sanders, DB TI Star Formation Rates, Metallicities, and Colours as Probes of Merger Timelines SO GALAXY MERGERS IN AN EVOLVING UNIVERSE SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on Galaxy Mergers in an Evolving Universe CY OCT 23-28, 2011 CL Hualien, TAIWAN SP Natl Sci Council Taiwan, Natl Sci Fdn US, Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys AB Pairs of interacting galaxies show significant alterations to their colours, gas-phase metallicities, and SFRs. By investigating the spectroscopic and photometric properties of a sample of interacting galaxies, these changes can be probed. By exploiting the statistical power of the SDSS DR7, we construct a sample of interacting pairs with stringent selection criteria, and develop a methodology that allows us to significantly detect very small deviations for each pair in our sample, relative to a control sample. These deviations can then be interpreted as a function of projected separation. By subdividing the sample based on visual classifications of morphological disturbance, we are able to further investigate these shifts away from control values. We find that galaxies are affected by their encounter out to projected separations of at least 80 kpc h(-1). Metallicities shift to significantly lower values over a broader range of projected separations for the morphologically selected sample. Through a comparison with theoretical models, we interpret the form of these trends as the signature of coalescing galaxies at small separations, and of post-pericentric galaxies blurred by projection effects at wider separations. C1 [Scudder, Jillian M.; Ellison, Sara L.; Mendel, J. Trevor] Univ Victoria, Victoria, BC V8P 1A1, Canada. [Patton, David R.] Trent Univ, Peterborough, ON K9J 7B8, Canada. [Torrey, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Scudder, JM (reprint author), Univ Victoria, Victoria, BC V8P 1A1, Canada. NR 2 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-838-1 J9 ASTR SOC P PY 2013 VL 477 BP 241 EP + PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BIB57 UT WOS:000327278600043 ER PT J AU Woodley, NE AF Woodley, Norman E. TI A revision of the Neotropical genus Paraberismyia Woodley (Diptera, Stratiomyidae, Beridinae) with three new species SO ZOOKEYS LA English DT Article DE Beridinae; Mexico; Neotropical Region; new species; taxonomy AB The Neotropical genus Paraberismyia Woodley, 1995, is revised. Three new species, P. chiapas sp. n., P. mathisi sp. n., and P. triunfo sp. n. are described, all having type localities in Chiapas, Mexico. A key to the four known species is provided. C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, Washington, DC 20013 USA. RP Woodley, NE (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst NHB 168, POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 NR 3 TC 1 Z9 1 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 353 BP 25 EP 45 DI 10.3897/zookeys.353.6301 PG 21 WC Zoology SC Zoology GA 259TH UT WOS:000327548700002 PM 24294096 ER PT J AU Rota, J Miller, SE AF Rota, Jadranka Miller, Scott E. TI A new genus of metalmark moths (Lepidoptera, Choreutidae) with Afrotropical and Australasian distribution SO ZOOKEYS LA English DT Article DE Alpha taxonomy; DNA barcoding; Ficus spp.; Kenya; Niveas agassizi; Niveas kone; Papua New Guinea; Solomon Islands; phylogenetics ID NEW-GUINEA; PHYLOGENETIC INFERENCE; DNA BARCODES; CATERPILLARS; FOREST; WEB AB Niveas Rota, new genus, and its two new species, N. agassizi Rota, new species, and N. kone Rota, new species, are described and illustrated. Niveas is assigned to the subfamily Choreutinae based on morphological and molecular data. Niveas agassizi is currently known only from Kenya and only from female specimens. Niveas kone has been found on the Solomon Islands and in Papua New Guinea (PNG). In PNG, larvae of this species have been reared from several species of Ficus (Moraceae). The two species are superficially quite dissimilar from each other. However, they share features in wing pattern and venation, as well as female genitalia, and the molecular data strongly support the monophyly of Niveas. C1 [Rota, Jadranka] Univ Turku, Genet Lab, FI-20014 Turku, Finland. [Rota, Jadranka] Univ Turku, Zool Museum, Dept Biol, FI-20014 Turku, Finland. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Rota, J (reprint author), Univ Turku, Genet Lab, FI-20014 Turku, Finland. EM jadranka.rota@utu.fi RI Rota, Jadranka/C-6702-2011; OI Rota, Jadranka/0000-0003-0220-3920; Miller, Scott/0000-0002-4138-1378 FU US National Science Foundation [DEB-0211591, 0515678]; Czech Science Foundation [206/09/0115]; Czech Ministry of Education; European Union [CZ.1.-07/2.3.00/20.0064]; Genome Canada; Ontario Genomics Institute; Finnish Kone Foundation FX Papua New Guinea: This paper stems from a rearing campaign led by Vojtech Novotny, George Weiblen, Yves Basset, and Scott Miller, and supported by the US National Science Foundation (grants DEB-0211591, 0515678 and others), Czech Science Foundation grant 206/09/0115 and others, and Czech Ministry of Education & European Union grant CZ.1.-07/2.3.00/20.0064. We thank the staff at the PNG Binatang Research Center for field assistance, PNG land owners for access to field sites and assistance, and PNG agencies for permits. DNA barcoding was provided by Paul Hebert through a grant from Genome Canada and the Ontario Genomics Institute in support of the iBOL project. Karolyn Darrow, Lauren Helgen and Margaret Rosati provided assistance at the Smithsonian. Kenya: We thank David Agassiz for sharing his material of African choreutids and the National Museums of Kenya for facilitating our collaboration. Phylogenetics: We thank Niklas Wahlberg for designing primers used in this project; and Carlos Pena and Eero Vesterinen for laboratory assistance. Phylogenetic analyses were conducted on the freely available Bioportal cluster (http://www.bioportal.uio.no) and RAxML blackbox (http://phylobench.vital-it.ch/raxml-bb/). We thank John Brown and an anonymous reviewer for helpful comments on an earlier version of the manuscript. SEM also thanks the Natural History Museum, London, Bishop Museum, Honolulu, and International Center for Insect Physiology and Ecology, Nairobi, for their continued support of this research program. JR was funded by the Finnish Kone Foundation experienced researcher grant during this project. NR 23 TC 2 Z9 3 U1 0 U2 4 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 355 BP 29 EP 47 DI 10.3897/zookeys.355.6158 PG 19 WC Zoology SC Zoology GA 259TS UT WOS:000327549800003 PM 24363568 ER PT J AU Breedy, O Williams, GC Guzman, HM AF Breedy, Odalisca Williams, Gary C. Guzman, Hector M. TI Two new species of gorgonian octocorals from the Tropical Eastern Pacific Biogeographic Region (Cnidaria, Anthozoa, Gorgoniidae) SO ZOOKEYS LA English DT Article DE Eugorgia; eastern Pacific; gorgonian; soft corals; taxonomy; white species AB The gorgoniid Eugorgia is exclusively an eastern Pacific genus. It has a wide geographic and bathymetric range of distribution, found from California to Per and extends down to 65 m deep. Two new species are herein described. The morphological characters were analyzed and illustrated by light and scanning electron microscopy. Eugorgia beebei sp. n. can be distinguished by its white, ascending, sparse colony growth. Eugorgia mutabilis sp. n. can be distinguished by its white colony that changes color after collection, and the conspicuous sharp-crested disc sclerites. From a morphological point of view the new species are related to the daniana-group, the rubens-group and the siedenburgae-group of Eugorgia; their affiliations, and the proposal of a new group are discussed. These new species increases the number of species in the genus to 15, and contribute to the knowledge of the eastern Pacific octocoral biodiversity. C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, San Jose, Costa Rica. [Williams, Gary C.] Calif Acad Sci, Dept Invertebrate Zool & Geol, San Francisco, CA 94118 USA. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, Ctr Invest Estruct Microscop, POB 11501-2060, San Jose, Costa Rica. EM odaliscab@gmail.com FU Universidad de Costa Rica/ University of Manitoba, Canada; Vicerrectoria de Investigacion, Universidad de Costa Rica; Smithsonian Tropical Research Institute FX We are grateful to anonymous reviewers for critical improvements of the manuscript. We thank Adam Baldinger (MCZ) and Stephen Cairns (USNM) for specimen loans, and Ardis Johnston (former collection manager MCZ) for providing information about the MCZ collection, and Rita Vargas (UCR), and Carlos Guevara (STRI) for laboratory and field work. We thank Rosalinda Abeytia for collecting paratype STRI 1122, and Celeste Sanchez for providing the submarine pictures in Figure 3. We thank Federico Bolanos, director of the Field Biology and Conservation in the Tropics Program (Universidad de Costa Rica/ University of Manitoba, Canada) for funding the 2013 collection trip to Golfo Dulce.; This project was partially funded by the Vicerrectoria de Investigacion, Universidad de Costa Rica, and Smithsonian Tropical Research Institute. NR 17 TC 2 Z9 2 U1 0 U2 7 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 350 BP 75 EP 90 DI 10.3897/zookeys.350.6117 PG 16 WC Zoology SC Zoology GA 259SE UT WOS:000327545800004 PM 24294084 ER PT J AU Zamora, S Zhu, XJ Lefebvre, B AF Zamora, Samuel Zhu, Xuejian Lefebvre, Bertrand TI A new Furongian (Cambrian) Echinoderm-Lagerstatte from the Sandu Formation (South China) SO CAHIERS DE BIOLOGIE MARINE LA English DT Article; Proceedings Paper CT 14th International Echinoderm Conference (IEC) CY AUG 20-24, 2012 CL Royal Acad Sci Belgium, Brussels, BELGIUM SP Natl Fund Sci Res, Univ Libre Bruxelles, Univ Mons, Univ Catholique Louvain, Belgian Sci Policy Off, FEI, Jeol, Titertek Berthold HO Royal Acad Sci Belgium DE China; Echinoderms; Evolutionary Faunas; Furongian; Lagerstatte; Palaeobiogeography ID PALEOZOIC ECHINODERMS; STYLOPHORAN; DIVERSIFICATION; PALEOBIOGEOGRAPHY; PALEOECOLOGY; DIVERSITY; PATTERNS; GUANGXI; ORIGIN AB A new Furongian (Cambrian) Echinoderm-Lagerstatte from South China has yielded one of the most diverse and well preserved echinoderm faunas from this poorly known time interval. Eight different taxa were identified and belong to four major groups of echinoderms: edrioasteroids, rhombiferans, solutans, and stylophorans. This assemblage shows strong palaeobiogeographic affinities with other, previously described, Gondwanan faunas from Australia, France, and Korea. In terms of faunal evolution, it is intermediate between "Cambrian Evolutionary Fauna" and "Palaeozoic Evolutionary Fauna". C1 [Zamora, Samuel] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Zhu, Xuejian] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Nanjing 210008, Jiangsu, Peoples R China. [Zhu, Xuejian] Nanjing Univ, Dept Earth Sci, Nanjing 210093, Jiangsu, Peoples R China. [Lefebvre, Bertrand] Univ Lyon 1, CNRS, UMR 5276, F-69622 Villeurbanne, France. [Lefebvre, Bertrand] ENS Lyon, F-69622 Villeurbanne, France. RP Zamora, S (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. EM samuel@unizar.es NR 27 TC 4 Z9 5 U1 0 U2 3 PU CAHIERS DE BIOLOGIE MARINE PI ROSCOFF PA STATION BIOLOGIQUE PLACE GEORGES TEISSIER, 29680 ROSCOFF, FRANCE SN 0007-9723 EI 2262-3094 J9 CAH BIOL MAR JI Cah. Biol. Mar. PY 2013 VL 54 IS 4 SI SI BP 565 EP 569 PG 5 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 251TS UT WOS:000326954200014 ER PT S AU Chance, K Liu, X Suleiman, RM Flittner, DE Al-Saadi, J Janz, SJ AF Chance, Kelly Liu, Xiong Suleiman, Raid M. Flittner, David E. Al-Saadi, Jassim Janz, Scott J. BE Butler, JJ Xiong, X Gu, X TI Tropospheric emissions: Monitoring of pollution (TEMPO) SO EARTH OBSERVING SYSTEMS XVIII SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Earth Observing Systems XVIII CY AUG 26-29, 2013 CL San Diego, CA SP SPIE DE Urban and regional atmospheric pollution; tropospheric composition and chemistry; tropospheric transport; atmospheric aerosols ID ABSORPTION CROSS-SECTIONS; OZONE PROFILE RETRIEVALS; IN-FLIGHT CALIBRATION; FOURIER-TRANSFORM MEASUREMENTS; ROTATIONAL RAMAN-SCATTERING; AEROSOL OPTICAL DEPTH; SURFACE UV IRRADIANCE; AIR-QUALITY; SATELLITE ESTIMATION; NORTH-AMERICA AB TEMPO was selected in 2012 by NASA as the first Earth Venture Instrument, for launch circa 2018. It will measure atmospheric pollution for greater North America from space using ultraviolet and visible spectroscopy. TEMPO measures from Mexico City to the Canadian tar sands, and from the Atlantic to the Pacific, hourly and at high spatial resolution (similar to 2 km N/Sx4.5 km E/W at 36.5 degrees N, 100 degrees W). TEMPO provides a tropospheric measurement suite that includes the key elements of tropospheric air pollution chemistry. Measurements are from geostationary (GEO) orbit, to capture the inherent high variability in the diurnal cycle of emissions and chemistry. The small product spatial footprint resolves pollution sources at sub-urban scale. Together, this temporal and spatial resolution improves emission inventories, monitors population exposure, and enables effective emission-control strategies. TEMPO takes advantage of a commercial GEO host spacecraft to provide a modest cost mission that measures the spectra required to retrieve O-3, NO2, SO2, H2CO, C2H2O2, H2O, aerosols, cloud parameters, and UVB radiation. TEMPO thus measures the major elements, directly or by proxy, in the tropospheric O-3 chemistry cycle. Multi-spectral observations provide sensitivity to O-3 in the lowermost troposphere, substantially reducing uncertainty in air quality predictions. TEMPO quantifies and tracks the evolution of aerosol loading. It provides near-real-time air quality products that will be made widely, publicly available. TEMPO will launch at a prime time to be the North American component of the global geostationary constellation of pollution monitoring together with European Sentinel-4 and Korean GEMS. C1 [Chance, Kelly; Liu, Xiong; Suleiman, Raid M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 NR 137 TC 17 Z9 17 U1 0 U2 10 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9716-1 J9 PROC SPIE PY 2013 VL 8866 AR 88660D DI 10.1117/12.2024479 PG 16 WC Instruments & Instrumentation; Remote Sensing; Optics SC Instruments & Instrumentation; Remote Sensing; Optics GA BHU75 UT WOS:000326700700011 ER PT S AU Allured, R Donovan, BD McEntaffer, RL AF Allured, Ryan Donovan, Benjamin D. McEntaffer, Randall L. BE ODell, SL Pareschi, G TI Alignment Tolerances for Off-Plane Reflection Grating Spectrometry: Theoretical Calculations and Laboratory Techniques SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 26-29, 2013 CL San Diego, CA SP SPIE AB Off-plane reflection gratings can be used to provide high throughput and spectral resolution in the 0.3-2.0 keV band, allowing for unprecedented diagnostics of energetic astrophysical processes. A grating spectrometer consists of multiple aligned gratings intersecting the converging beam of a Wolter-I telescope. Each grating will be aligned such that the diffracted spectra overlap at the focal plane. Misalignments will degrade both spectral resolution and effective area. In this paper we present a summary of analytical alignment tolerance calculations, including an investigation of diffraction efficiency alignment dependence. Our plan for extending this work to future modeling and simulation is laid out. Finally, we report on the status of laboratory techniques to achieve these tolerances for flight-like optics. C1 [Allured, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Allured, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 12 TC 1 Z9 1 U1 1 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9711-6 J9 PROC SPIE PY 2013 VL 8861 AR 88611C DI 10.1117/12.2022873 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT77 UT WOS:000326645100046 ER PT S AU Gorenstein, P AF Gorenstein, Paul BE ODell, SL Pareschi, G TI On Kirkpatrick-Baez telescopes with adjustable X-ray optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 26-29, 2013 CL San Diego, CA SP SPIE DE X-ray telescopes; TAXRO; AXRO; AXO; Kirkpatrick-Baez telescopes ID ASTRONOMY AB High resolution spectroscopy is the most favored objective of the next X-ray astronomy mission. A longer term goal is the development of a very large area X-ray telescope whose angular resolution and effective area are superior to the Chandra X-Ray Observatory. Adjustable X-ray optics with thin piezoelectric coatings is a methodology that may be capable of accomplishing that goal. It consists of applying piezoelectric coatings to the rear of a mirror substrate, which will be thermally slumped to the approximate figure. The figure is optimized by applying voltages to the piezoelectric coatings. Near term spectroscopy mission can benefit from higher angular resolution and a Kirkpatrick-Baez telescope should be considered as an alternative to the Wolter telescope. Adjustable X-ray optics technology should be very effective in refining the resolution of a KB telescope. When the thermally slumped mirrors of either the front or rear section are assembled and illuminated by a parallel visible light or X-ray beam line, line images formed by individual mirrors can be isolated by a moveable slit. With the piezoelectric controllers acting in only dimension the figure of each mirror can be optimized sequentially completely under computer control. The front and rear sections can be tuned independently and then joined with rather lenient tolerances. Dispersing along the 45 degree direction between the two orthogonal KB axes reduces the effect of scattering and figure errors similar to what is accomplished by using only part of the azimuth of a Wolter mirror. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gorenstein, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 18 TC 0 Z9 0 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9711-6 J9 PROC SPIE PY 2013 VL 8861 AR 88611P DI 10.1117/12.2024905 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT77 UT WOS:000326645100059 ER PT S AU Reid, PB Aldcroft, TL Cotroneo, V Davis, W Johnson-Wilke, RL McMuldroch, S Ramsey, BD Schwartz, DA Trolier-McKinstry, S Vikhlinin, A Wilke, RHT AF Reid, Paul B. Aldcroft, Thomas L. Cotroneo, Vincenzo Davis, William Johnson-Wilke, Reagan L. McMuldroch, Stuart Ramsey, Brian D. Schwartz, Daniel A. Trolier-McKinstry, Susan Vikhlinin, Alexey Wilke, Rudeger H. T. BE ODell, SL Pareschi, G TI Development status of adjustable grazing incidence optics for 0.5 arc second X-ray imaging SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 26-29, 2013 CL San Diego, CA SP SPIE DE x-ray optics; adjustable optics; active optics; piezoelectric; deformable mirrors; Smart-X; high resolution; lightweight optics ID PZT THIN-FILMS AB We describe progress in the development of adjustable grazing incidence X-ray optics for 0.5 arcsec resolution cosmic X-ray imaging. To date, no optics technology is available to blend high resolution imaging like the Chandra X-ray Observatory, with square meter collecting area. Our approach to achieve these goals simultaneously is to directly deposit thin film piezoelectric actuators on the back surface of thin, lightweight Wolter-I or Wolter-Schwarschild mirror segments. The actuators are used to correct mirror figure errors due to fabrication, mounting and alignment, using calibration and a one-time figure adjustment on the ground. If necessary, it will also be possible to correct for residual gravity release and thermal effects on-orbit. In this paper we discuss our most recent results in operating multiple adjusters, and extending the process from flat test mirrors to cylindrical and conical test mirror segments. A comparison of modeled and measured influence functions is shown. We also present simulation results showing the process is consistent with the achievement of half arcsec imaging. C1 [Reid, Paul B.; Aldcroft, Thomas L.; Cotroneo, Vincenzo; Davis, William; McMuldroch, Stuart; Schwartz, Daniel A.; Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, PB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pried@cfa.harvard.edu OI Trolier-McKinstry, Susan/0000-0002-7267-9281 NR 18 TC 2 Z9 2 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9711-6 J9 PROC SPIE PY 2013 VL 8861 AR 88611Q DI 10.1117/12.2026429 PG 8 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT77 UT WOS:000326645100060 ER PT S AU Romaine, S Bruni, R Choi, B Gorenstein, P Jensen, C Ramsey, B Rosati, R Sampath, S AF Romaine, S. Bruni, R. Choi, B. Gorenstein, P. Jensen, C. Ramsey, B. Rosati, R. Sampath, S. BE ODell, SL Pareschi, G TI Development of light weight replicated X-ray optics SO OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY VI SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Optics for EUV, X-Ray, and Gamma-Ray Astronomy VI as part of the SPIE Optics + Photonics International Symposium on Optical Engineering + Applications CY AUG 26-29, 2013 CL San Diego, CA SP SPIE DE X-ray optics; TiN; electroformed optics; release layer; multilayers ID PROGRESS AB Nearly all X-ray astronomy missions of the past 25 years have utilized grazing incidence telescopes which use the principle of nested shells to maximize the collecting area. Most of these missions have had multiple X-ray telescopes, e.g. ASCA(1), Beppo-SAX(2), Suzaku(3), XMM-Newton(4), NuStar(5), and also upcoming missions Astro-H-6 and Spectrum-Roentgen-Gamma(7). Multiple telescopes, which favor replication, may continue to be the appropriate architecture of some future missions. XMM-Newton and the upcoming Spectrum-Roentgen-Gamma mission use an electroformed nickel replication (ENR) process to fabricate their X-ray telescope mirror shells, a process which has achieved the best angular resolution to date for replicated telescopes. We are developing a process to fabricate metal-ceramic replicated optics which will be lighter weight than current nickel replicated technology. They will be stiffer than the XMM mirrors, which we expect will result in better angular resolution. Recent results on fabrication and testing of these optics is presented. C1 [Romaine, S.; Bruni, R.; Gorenstein, P.; Rosati, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romaine, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sromaine@cfa.harvard.edu NR 13 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9711-6 J9 PROC SPIE PY 2013 VL 8861 AR 88610U DI 10.1117/12.2024897 PG 7 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT77 UT WOS:000326645100030 ER PT S AU Bergner, H Caldwell, D Case, AW Daigneau, P Freeman, M Kasper, J AF Bergner, H. Caldwell, D. Case, A. W. Daigneau, P. Freeman, M. Kasper, J. BE Fineschi, S Fennelly, J TI Mechanical Design of the Solar Probe Cup instrument on Solar Probe Plus SO SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solar Physics and Space Weather Instrumentation V CY AUG 25-26, 2013 CL San Diego, CA SP SPIE DE Solar Probe Cup (SPC); high temperature sensors; SAO; Solar Probe Plus AB The Solar Probe Cup (SPC) Instrument is a Sun-facing Faraday Cup instrument slated for launch aboard the Solar Probe Plus (SPP) spacecraft in 2018. SPC is one of two instruments onboard the Solar Wind Electrons Alphas Protons (SWEAP) instrument suite and is the only SPP charged particle instrument that will not be shielded behind the spacecraft's Thermal Protection System (TPS). The 7-year SPP mission will take SPC on 24 solar encounters at perihelia ranging from 35 to 9.86 solar radii (R-S). The SPC components will encounter a large range of temperatures, from in excess of 1500 degrees C at perihelion to -130 degrees C at or near aphelion. This paper details the derived mechanical and structural requirements on the primary SPC mechanical assemblies including its thermal shield, the sensor unit and the strut/adapter assembly. An example of sensor requirements derivation to the component level is provided by the modulator flex ring. Preliminary requirements derivation, definition, and compliance are provided for these assemblies and components. C1 [Bergner, H.; Caldwell, D.; Case, A. W.; Daigneau, P.; Freeman, M.] Smithsonian Astrophys Observ, Cambridge, MA 02140 USA. RP Bergner, H (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02140 USA. EM pdaigneau@cfa.harvard.edu NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9712-3 J9 PROC SPIE PY 2013 VL 8862 AR UNSP 88620L DI 10.1117/12.2022761 PG 9 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT17 UT WOS:000326605000018 ER PT S AU Cheimets, P Bookbinder, J Freeman, M Gates, R Gauron, T Guth, G Kasper, J McCracken, K Podgorski, W AF Cheimets, Peter Bookbinder, Jay Freeman, Mark Gates, Richard Gauron, Thomas Guth, Giora Kasper, Justin McCracken, Kenneth Podgorski, William BE Fineschi, S Fennelly, J TI The design, development, and implementation of a solar environmental simulator (SES) for the SAO Faraday Cup on Solar Probe Plus SO SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solar Physics and Space Weather Instrumentation V CY AUG 25-26, 2013 CL San Diego, CA SP SPIE DE Solar Probe Plus; Simulator; Faraday Cup AB This paper describes the implementation of a solar simulator, know as the Solar Environment Simulator (SES), that can simulate solar flux levels up to those encountered at 9.8 solar radii. The paper outlines the design, and the challenges of realizing the SES. It also describes its initial uses for proving out the design of the Solar Winds Electrons, Alphas, and Protons (SWEAP) Faraday cup. The upcoming Solar Probe Plus (SPP) mission requires that its in-situ plasma instrument (the Faraday Cup) survive and operate over an unprecedented range of temperatures. One of the key risk mitigation activities during Phase B has been to develop and implement a simulator that will enable thermal testing of the Faraday Cup under flight-like conditions. While still in the initial start-up, the SES has proven to be an instrumental component in the process of predicting the in-flight performance of the SWEAP Faraday Cup. With near continuously variable power control above the threshold of 1.6kW/lamp up to approximately 6.5kW/lamp, the SES has been used to determine the system response to a wide range of incoming flux, thereby making it possible to correlate detailed thermal models to a high degree of certainty (see Ref. [1], Figure 1.1). The SES consists of a set of repurposed, and slightly re-designed standard movie projectors. The projectors have proven to be an economical and effective means to safely hold and control the xenon short-arc lamps that are the basis of the SES. This paper outlines the key challenges controlling the extremely high flux levels (similar to 70w/cm<^>2) necessary to make the SES a useful test facility. C1 [Cheimets, Peter; Bookbinder, Jay; Freeman, Mark; Gates, Richard; Gauron, Thomas; Guth, Giora; Kasper, Justin; McCracken, Kenneth; Podgorski, William] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Cheimets, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. NR 2 TC 1 Z9 1 U1 0 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9712-3 J9 PROC SPIE PY 2013 VL 8862 AR UNSP 88620M DI 10.1117/12.2024051 PG 10 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT17 UT WOS:000326605000019 ER PT S AU Freeman, MD Kasper, J Case, AW Daigneau, P Gauron, T Bookbinder, J Brodu, E Balat-Pichelin, M Wright, K AF Freeman, Mark D. Kasper, Justin Case, Anthony W. Daigneau, Peter Gauron, Thomas Bookbinder, Jay Brodu, Etienne Balat-Pichelin, Marianne Wright, Kenneth BE Fineschi, S Fennelly, J TI Technology development for the Solar Probe Plus Faraday Cup SO SOLAR PHYSICS AND SPACE WEATHER INSTRUMENTATION V SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Solar Physics and Space Weather Instrumentation V CY AUG 25-26, 2013 CL San Diego, CA SP SPIE DE Faraday cup; solar wind; ion instrumentation; plasma; solar mission; Solar Probe; heliophysics ID HIGH-TEMPERATURE; VACUUM AB The upcoming Solar Probe Plus (SPP) mission requires novel approaches for in-situ plasma instrument design. SPP's Solar Probe Cup (SPC) instrument will, as part of the Solar Wind Electrons, Alphas, and Protons (SWEAP) instrument suite, operate over an enormous range of temperatures, yet must still accurately measure currents below 1 pico-amp, and with modest power requirements. This paper discusses some of the key technology development aspects of the SPC, a Faraday Cup and one of the few instruments on SPP that is directly exposed to the solar disk, where at closest approach to the Sun (less than 10 solar radii (R-s) from the center of the Sun) the intensity is greater than 475 earth-suns. These challenges range from materials characterization at temperatures in excess of 1400 degrees C to thermal modeling of the behavior of the materials and their interactions at these temperatures. We discuss the trades that have resulted in the material selection for the current design of the Faraday Cup. Specific challenges include the material selection and mechanical design of insulators, particularly for the high-voltage (up to 8 kV) grid and coaxial supply line, and thermo-optical techniques to minimize temperatures in the SPC, with the specific intent of demonstrating Technology Readiness Level 6 by the end of 2013. C1 [Freeman, Mark D.; Kasper, Justin; Case, Anthony W.; Daigneau, Peter; Gauron, Thomas; Bookbinder, Jay; Brodu, Etienne] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Freeman, MD (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mfreeman@cfa.harvard.edu NR 4 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 978-0-8194-9712-3 J9 PROC SPIE PY 2013 VL 8862 AR UNSP 88620K DI 10.1117/12.2024983 PG 12 WC Astronomy & Astrophysics; Optics SC Astronomy & Astrophysics; Optics GA BHT17 UT WOS:000326605000017 ER PT S AU Duchene, G Kraus, A AF Duchene, Gaspard Kraus, Adam BE Faber, SM VanDishoeck, E TI Stellar Multiplicity SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, VOL 51 SE Annual Review of Astronomy and Astrophysics LA English DT Review; Book Chapter DE main-sequence stars; pre-main-sequence stars; protostars; star formation ID LOW-MASS STARS; HUBBLE-SPACE-TELESCOPE; BROWN DWARF DESERT; ORION-NEBULA-CLUSTER; ADAPTIVE OPTICS SURVEY; SOLAR-TYPE STARS; CLOSE BINARY-SYSTEMS; PROPER-MOTION STARS; ANGULAR RESOLUTION MULTIPLICITY; OBSERVED ORBITAL ECCENTRICITIES AB Stellar multiplicity is a ubiquitous outcome of the star-formation process. The frequency and main characteristics of multiple systems, and their dependence on primary mass and environment, are powerful tools to probe this process. Although early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the past two decades now enable robust statistical analyses. In this review, we summarize current empirical knowledge of stellar multiplicity for main sequence stars and brown dwarfs, as well as among populations of pre-main-sequence stars and embedded protostars. Among field objects, the multiplicity rate and breadth of the orbital period distribution are steep functions of the primary mass, whereas the mass ratio distribution is essentially flat for most populations other than the lowest mass objects. The time-variation of the frequency of visual companions follows two parallel, constant tracks corresponding to loose and dense stellar populations, although current observations do not yet distinguish whether initial multiplicity properties are universal or dependent on the physical conditions of the parent cloud. Nonetheless, these quantitative trends provide a rich comparison basis for numerical and analytical models of star formation. C1 [Duchene, Gaspard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Duchene, Gaspard] UJF Grenoble 1, CNRS INSU, UMR 5274, IPAG, F-38041 Grenoble 9, France. [Kraus, Adam] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Duchene, G (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. EM gduchene@berkeley.edu; akraus@cfa.harvard.edu NR 315 TC 204 Z9 204 U1 1 U2 4 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0066-4146 BN 978-0-8243-0951-0 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 2013 VL 51 BP 269 EP 310 DI 10.1146/annurev-astro-081710-102602 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHT29 UT WOS:000326621000008 ER PT J AU Parrella, JP Chance, K Salawitch, RJ Canty, T Dorf, M Pfeilsticker, K AF Parrella, J. P. Chance, K. Salawitch, R. J. Canty, T. Dorf, M. Pfeilsticker, K. TI New retrieval of BrO from SCIAMACHY limb: an estimate of the stratospheric bromine loading during April 2008 SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID ABSORPTION CROSS-SECTIONS; OZONE-MONITORING-EXPERIMENT; GLOBAL OBSERVATIONS; UV SPECTROSCOPY; NO2; TEMPERATURE; SENSITIVITY; PROFILES; O-3; PARAMETERS AB We present a new retrieval of stratospheric BrO (bromine monoxide) from channel 2 SCIAMACHY (SCanning Imaging Absorption spectrometer for Atmospheric CHartographY) limb observations. Retrievals are shown to agree with independent balloon observations to within one standard deviation of the retrieval noise. We retrieve BrO profiles for all of April 2008, and apply simulated [BrO]/[Bry] (bromine monoxide : stratospheric inorganic bromine) ratios to estimate the stratospheric Bry loading. We find 23.5 +/- 6 ppt Br, suggesting 7 ppt Br from short-lived bromocarbons to be at the high end of the current best estimate (3-8 ppt). The 6 ppt Br uncertainty estimate is dominated by the 21% uncertainty in the simulated [BrO] /[Bry] ratio due to propagation of errors from the underlying chemical kinetics. C1 [Parrella, J. P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Salawitch, R. J.; Canty, T.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Salawitch, R. J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Salawitch, R. J.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Dorf, M.; Pfeilsticker, K.] Heidelberg Univ, Inst Umweltphys, Heidelberg, Germany. RP Parrella, JP (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM parrella@post.harvard.edu RI Canty, Timothy/F-2631-2010; Salawitch, Ross/B-4605-2009; OI Canty, Timothy/0000-0003-0618-056X; Salawitch, Ross/0000-0001-8597-5832; Chance, Kelly/0000-0002-7339-7577 FU NASA; Smithsonian Institution FX This research was supported by NASA and the Smithsonian Institution. The authors thank Xiong Liu for discussions and helpful comments on optimal estimation and statistics, Thomas Kurosu for help with spectral fitting, Alexei Rozanov for his helpful comments on SCIAMACHY data and optimal estimation retrievals, and Chris Sioris for help with radiative transfer. NR 56 TC 3 Z9 3 U1 0 U2 6 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2013 VL 6 IS 10 BP 2549 EP 2561 DI 10.5194/amt-6-2549-2013 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 246OB UT WOS:000326547100002 ER PT J AU Wiacek, A Martin, RV Bourassa, AE Lloyd, ND Degenstein, DA AF Wiacek, A. Martin, R. V. Bourassa, A. E. Lloyd, N. D. Degenstein, D. A. TI Absorbing aerosol radiative effects in the limb-scatter viewing geometry SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MINERAL DUST; RETRIEVAL; OSIRIS; ABSORPTION; SUNLIGHT; CLOUDS; ODIN; INSTRUMENT; MODELS; SYSTEM AB The limb-scatter satellite viewing geometry is well suited to detecting low-concentration aerosols in the upper troposphere due to its long observation path length (similar to 200 km), high vertical resolution (similar to 1-2 km) and good geographic coverage. We use the fully three-dimensional radiative transfer code SASKTRAN to simulate the sensitivity of limb-scatter viewing Odin/OSIRIS satellite measurements to absorbing mineral dust and carbonaceous aerosols (smoke and pure soot), as well as to non-absorbing sulfate aerosols and ice in the upper troposphere. At long wavelengths (813 nm) the addition of all aerosols (except soot) to an air only atmosphere produced a radiance increase as compared to air only, on account of the low Rayleigh scattering in air only at 813 nm. The radiance reduction due to soot aerosol was negligible (< 0.1 %) at all heights (0-100 km). At short wavelengths (337, 377, 452 nm), we found that the addition of any aerosol species to an air only atmosphere caused a decrease in single-scattered radiation due to an extinction of Rayleigh scattering in the direction of OSIRIS. The reduction was clearly related to particle size first, with absorption responsible for second-order effects only. Multiple-scattered radiation could either increase or decrease in the presence of an aerosol species, depending both on particle size and absorption. Large scatterers (ice, mineral dust) all increased multiple-scattered radiation within, below and above the aerosol layer. Small, highly absorbing pure soot particles produced a negligible multiple-scattering response (< 0.1 %) at all heights, primarily confined to within and below the soot layer. Medium-sized scatterers produced a multiple-scattering response that depended on their absorbing properties. Increased radiances were simulated as compared to air only at all short wavelengths (337, 377 and 452 nm) for sulfate aerosol particles (non-absorbing) while decreased radiances were simulated for smoke particles (absorbing) at 337 and 377 nm, where multiple scattering involving the medium-sized carbonaceous particles amplified their absorbing properties. At 452 nm, however, this effect was attenuated and albedo-dependent. At short wavelengths, the combined effect of single scattering decreases and multiple scattering increases led to complex total radiance signatures that generally could not unambiguously distinguish absorbing versus non-absorbing aerosols. Smoke aerosols led to a total radiance decrease (as compared to air only) at all altitudes above the aerosol layer (15-100 km). This unique signature was a result of the aerosols' strong absorbing properties, non-negligible scattering efficiency, and number concentrations high enough to make multiple scattering effects due to the aerosol itself significant. Thus, in the limb-scatter viewing geometry scene darkening above the aerosol layer is unambiguously due to absorption whereas scene darkening within and below the aerosol layer can simply be the result of a reduction in single-scattered radiance. Our simulations show a greater scene darkening for decreasing wavelengths, increasing surface albedo, decreasing solar zenith angle, and increasing particle number concentration, however, at 337 nm this effect did not exceed 0.5% of the total radiance due to air only, making the unique identification of medium-sized carbonaceous aerosols, i.e., smoke, difficult. Scene darkening (or brightening) varies linearly with particle number concentration over three orders of magnitude. A fortuitous, unexpected implication of our analysis is that limb-scatter retrievals of aerosol extinction are not sensitive to external information about aerosol absorption. C1 [Wiacek, A.; Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Wiacek, A.] St Marys Univ, Dept Environm Sci, Halifax, NS B3H 3C3, Canada. [Wiacek, A.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Bourassa, A. E.; Lloyd, N. D.; Degenstein, D. A.] Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wiacek, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM aldona.wiacek@smu.ca RI Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU Canadian Foundation for Climate and Atmospheric Science (CFCAS); Canadian Space Agency (CSA) FX This work was supported by the Canadian Foundation for Climate and Atmospheric Science (CFCAS) and by the Canadian Space Agency (CSA). We thank O. Dubovik and T. Lapyonok for providing spheroid mixture scattering phase functions corresponding exactly to our particle size distributions and refractive index. NR 33 TC 0 Z9 0 U1 0 U2 4 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2013 VL 6 IS 10 BP 2761 EP 2776 DI 10.5194/amt-6-2761-2013 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 246OB UT WOS:000326547100016 ER PT J AU Chakrabarty, P Warren, M Page, LM Baldwin, CC AF Chakrabarty, Prosanta Warren, Melanie Page, Lawrence M. Baldwin, Carole C. TI GenSeq: An updated nomenclature and ranking for genetic sequences from type and non-type sources SO ZOOKEYS LA English DT Article DE GenBank; genetics; molecular phylogenetics; systematics; taxonomy ID WESTERN ATLANTIC; RIVER-BASIN; KILLIFISH; TRINDADE; LABRIDAE; GENBANK; ISLAND AB An improved and expanded nomenclature for genetic sequences is introduced that corresponds with a ranking of the reliability of the taxonomic identification of the source specimens. This nomenclature is an advancement of the "Genetypes" naming system, which some have been reluctant to adopt because of the use of the "type" suffix in the terminology. In the new nomenclature, genetic sequences are labeled "genseq," followed by a reliability ranking (e. g., 1 if the sequence is from a primary type), followed by the name of the genes from which the sequences were derived (e. g., genseq-1 16S, COI). The numbered suffix provides an indication of the likely reliability of taxonomic identification of the voucher. Included in this ranking system, in descending order of taxonomic reliability, are the following: sequences from primary types - "genseq-1," secondary types - "genseq-2," collection-vouchered topotypes - "genseq-3," collection-vouchered non-types - "genseq-4," and non-types that lack specimen vouchers but have photo vouchers - "genseq-5." To demonstrate use of the new nomenclature, we review recently published new-species descriptions in the ichthyological literature that include DNA data and apply the GenSeq nomenclature to sequences referenced in those publications. We encourage authors to adopt the GenSeq nomenclature (note capital "G" and "S" when referring to the nomenclatural program) to provide a searchable tag (e. g., "genseq"; note lowercase "g" and "s" when referring to sequences) for genetic sequences from types and other vouchered specimens. Use of the new nomenclature and ranking system will improve integration of molecular phylogenetics and biological taxonomy and enhance the ability of researchers to assess the reliability of sequence data. We further encourage authors to update sequence information on databases such as GenBank whenever nomenclatural changes are made. C1 [Chakrabarty, Prosanta; Warren, Melanie] Louisiana State Univ, Museum Nat Sci, Dept Biol Sci, Ichthyol Sect, Baton Rouge, LA 70803 USA. [Page, Lawrence M.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Chakrabarty, P (reprint author), Louisiana State Univ, Museum Nat Sci, Dept Biol Sci, Ichthyol Sect, 119 Foster Hall, Baton Rouge, LA 70803 USA. EM prosanta@lsu.edu RI Chakrabarty, Prosanta/E-3307-2010 FU National Science Foundation [DEB 0916695] FX We thank all the authors who were contacted and provided additional information about the sequences in Table 3. Two anonymous reviewers provided excellent suggestions that have been incorporated into this final publication. We would like to acknowledge Dr. Tanya Dewey (Animal Diversity Web) and Andy Bentley (University of Kansas) for their comments. We would like to also acknowledge the Louisiana State University Office of Strategic Initiatives 2012 Summer Research Experience for Undergraduates Program and the LSU Initiative for Maximizing Diversity for allowing MW to participate in this project. Financial support for this project was obtained from a National Science Foundation Grant to PC (DEB 0916695). NR 21 TC 26 Z9 29 U1 0 U2 8 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 346 BP 29 EP 41 DI 10.3897/zookeys.346.5753 PG 13 WC Zoology SC Zoology GA 246TX UT WOS:000326563100004 PM 24223486 ER PT J AU Buden, DW Helgen, KM Wiles, GJ AF Buden, Donald W. Helgen, Kristofer M. Wiles, Gary J. TI Taxonomy, distribution, and natural history of flying foxes (Chiroptera, Pteropodidae) in the Mortlock Islands and Chuuk State, Caroline Islands SO ZOOKEYS LA English DT Article DE Pteropus phaeocephalus; P. pelagicus; P. insularis; P. tokudae; Mortlock Islands; Chuuk; Micronesia; atoll; taxonomy; distribution; status; natural history; climate change; sea level rise ID BATS PTEROPUS-MARIANNUS; CLIMATE-CHANGE; FRUIT BATS; PACIFIC; MICRONESIA; TONGANUS; DISASTER; SAMOA; OCEAN; GENUS AB The taxonomy, biology, and population status of flying foxes (Pteropus spp.) remain little investigated in the Caroline Islands, Micronesia, where multiple endemic taxa occur. Our study evaluated the taxonomic relationships between the flying foxes of the Mortlock Islands (a subgroup of the Carolines) and two closely related taxa from elsewhere in the region, and involved the first ever field study of the Mortlock population. Through a review of historical literature, the name Pteropus pelagicus Kittlitz, 1836 is resurrected to replace the prevailing but younger name P. phaeocephalus Thomas, 1882 for the flying fox of the Mortlocks. On the basis of cranial and external morphological comparisons, Pteropus pelagicus is united taxonomically with P. insularis "Hombron and Jacquinot, 1842" (with authority herein emended to Jacquinot and Pucheran, 1853), and the two formerly monotypic species are now treated as subspecies-P. pelagicus pelagicus in the Mortlocks, and P. p. insularis on the islands of Chuuk Lagoon and Namonuito Atoll. The closest relative of P. pelagicus is P. tokudae Tate, 1934, of Guam, which is best regarded as a distinct species. Pteropus p. pelagicus is the only known resident bat in the Mortlock Islands, a chain of more than 100 atoll islands with a total land area of < 12 km(2). Based on field observations in 2004, we estimated a population size of 925-1, 200 bats, most of which occurred on Satawan and Lukunor Atolls, the two largest and southernmost atolls in the chain. Bats were absent on Nama Island and possibly extirpated from Losap Atoll in the northern Mortlocks. Resident Mortlockese indicated bats were more common in the past, but that the population generally has remained stable in recent years. Most P. p. pelagicus roosted alone or in groups of 5-10 bats; a roost of 27 was the largest noted. Diet is comprised of at least eight plant species, with breadfruit (Artocarpus spp.) being a preferred food. Records of females with young (April, July) and pregnant females (July) suggest an extended breeding season. Pteropus p. pelagicus appears most threatened by the prospect of sea level rise associated with global climate change, which has the potential to submerge or reduce the size of atolls in the Mortlocks. Occasional severe typhoons probably temporarily reduce populations on heavily damaged atolls, but hunting and ongoing habitat loss are not current problems for the subspecies. C1 [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Wiles, Gary J.] Washington Dept Fish & Wildlife, Olympia, WA 98501 USA. EM don_buden@comfsm.fm NR 103 TC 2 Z9 2 U1 2 U2 22 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 345 BP 97 EP 135 DI 10.3897/zookeys.345.5840 PG 39 WC Zoology SC Zoology GA 244FJ UT WOS:000326372200005 PM 24194666 ER PT S AU Korzennik, SG Rabello-Soares, MC Schou, J Larson, T AF Korzennik, S. G. Rabello-Soares, M. C. Schou, J. Larson, T. GP IOP TI Accurate characterization of high-degree modes using MDI data SO ECLIPSE ON THE CORAL SEA: CYCLE 24 ASCENDING (GONG 2012, LWS/SDO-5, AND SOHO 27) SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Conference on Eclipse on the Coral Sea - Cycle 24 Ascending (GONG 2012, LWS/SDO-5, and SOHO 27) CY NOV 12-16, 2012 CL AUSTRALIA ID FREQUENCIES AB We present the first accurate characterization of high-degree modes (i.e., l up to 1000), using the best MDI full-disk full-resolution data set available (90-day long time series, acquired in 2001). The Dopplergrams were spatially decomposed using our best estimate of the image scale and the known components of MDI's image distortion. Multi-tapered power spectra were fitted for all degrees and all azimuthal orders, between l = 100 and l = 1000, and for all orders with substantial amplitude. Fitting at high degrees generates ridge characteristics, characteristics that do not correspond to the underlying mode characteristics. We used a sophisticated forward modeling to recover the best possible estimate of the underlying mode characteristics. We have derived a final set of corrected mode characteristics (frequencies, line widths, asymmetries and amplitudes) and their uncertainties. C1 [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rabello-Soares, M. C.; Schou, J.; Larson, T.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA USA. [Rabello-Soares, M. C.] Univ Fed Minas Gerais, Dept Phys, Minas Gerais, Brazil. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skorzennik@cfa.harvard.edu RI Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 FU NASA [NAG5-8878, NAG5-10483, NAG5-9819, NNG05GD58G]; Stanford [PR-6333] FX The Solar Oscillations Investigation - Michelson Doppler Imager project on SOHO is supported by NASA grant NAG5-8878 and NAG5-10483 at Stanford University. SOHO is a project of international cooperation between ESA and NASA. SGK was supported by Stanford contract PR-6333 and NASA grants NAG5-9819 and NNG05GD58G. NR 5 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2013 VL 440 AR UNSP 012016 DI 10.1088/1742-6596/440/1/012016 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHN05 UT WOS:000325951200016 ER PT S AU Korzennik, SG Eff-Darwich, A AF Korzennik, S. G. Eff-Darwich, A. GP IOP TI Mode Frequencies from 17, 15 and 2 Years of GONG, MDI, and HMI Data SO ECLIPSE ON THE CORAL SEA: CYCLE 24 ASCENDING (GONG 2012, LWS/SDO-5, AND SOHO 27) SE Journal of Physics Conference Series LA English DT Proceedings Paper CT Conference on Eclipse on the Coral Sea - Cycle 24 Ascending (GONG 2012, LWS/SDO-5, and SOHO 27) CY NOV 12-16, 2012 CL AUSTRALIA ID SOLAR ROTATION AB We present results from fitting all the available data to date from the three major helioseismic instruments: MDI, GONG and HMI. These data were fitted using an innovative and independent methodology devised a few years ago. The mode fitting was carried out on time series of varying lengths (1x, 2x, 4x, 8x, 16x, 32x, 64 x 72 day-long), using co-eval epochs for all three data sets. By fitting time series of varying lengths, one trades off some temporal resolution for a better precision. We present a comparison of these results, and discuss the potential sources of the residual small discrepancies. We also present inferences from these results on the determination of the solar internal rotation and changes with epoch and thus activity levels. C1 [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Eff-Darwich, A.] Univ La Laguna, Dept Edafol & Geol, Tenerife 38206, Spain. [Eff-Darwich, A.] Inst Astrofis Canarias, Tenerife 38205, Spain. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM skorzennik@cfa.harvard.edu; adarwich@ull.es FU NASA [NAG5-8878, NAG5-10483, NAG5-9819, NNG05GD58G] FX The Solar Oscillations Investigation - Michelson Doppler Imager project on SOHO is supported by NASA grant NAG5-8878 and NAG5-10483 at Stanford University. SOHO is a project of international cooperation between ESA and NASA. This work utilizes data obtained by the Global Oscillation Network Group (GONG) program, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. SGK was supported by NASA grants NAG5-9819 and NNG05GD58G. NR 4 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1742-6588 J9 J PHYS CONF SER PY 2013 VL 440 AR UNSP 012015 DI 10.1088/1742-6596/440/1/012015 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BHN05 UT WOS:000325951200015 ER PT J AU Cuesta, J Eremenko, M Liu, X Dufour, G Cai, Z Hopfner, M von Clarmann, T Sellitto, P Foret, G Gaubert, B Beekmann, M Orphal, J Chance, K Spurr, R Flaud, JM AF Cuesta, J. Eremenko, M. Liu, X. Dufour, G. Cai, Z. Hoepfner, M. von Clarmann, T. Sellitto, P. Foret, G. Gaubert, B. Beekmann, M. Orphal, J. Chance, K. Spurr, R. Flaud, J. -M. TI Satellite observation of lowermost tropospheric ozone by multispectral synergism of IASI thermal infrared and GOME-2 ultraviolet measurements over Europe SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID NM SPECTRAL REGIONS; 10 MU-M; ABSORPTION-COEFFICIENTS; ATMOSPHERIC COMPOSITION; MONITORING INSTRUMENT; PROFILE RETRIEVAL; NEXT-GENERATION; AIR-POLLUTION; MODEL; REGULARIZATION AB We present a new multispectral approach for observing lowermost tropospheric ozone from space by synergism of atmospheric radiances in the thermal infrared (TIR) observed by IASI (Infrared Atmospheric Sounding Interferometer) and earth reflectances in the ultraviolet (UV) measured by GOME-2 (Global Ozone Monitoring Experiment-2). Both instruments are onboard the series of MetOp satellites (in orbit since 2006 and expected until 2022) and their scanning capabilities offer global coverage every day, with a relatively fine ground pixel resolution (12 km-diameter pixels spaced by 25 km for IASI at nadir). Our technique uses altitude-dependent Tikhonov-Phillips-type constraints, which optimize sensitivity to lower tropospheric ozone. It integrates the VLIDORT (Vector Linearized Discrete Ordinate Radiative Transfer) and KOPRA (Karlsruhe Optimized and Precise Radiative transfer Algorithm) radiative transfer codes for simulating UV reflectance and TIR radiance, respectively. We have used our method to analyse real observations over Europe during an ozone pollution episode in the summer of 2009. The results show that the multispectral synergism of IASI (TIR) and GOME-2 (UV) enables the observation of the spatial distribution of ozone plumes in the lowermost troposphere (LMT, from the surface up to 3 km a.s.l., above sea level), in good agreement with the CHIMERE regional chemistry-transport model. In this case study, when high ozone concentrations extend vertically above 3 km a.s.l., they are similarly observed over land by both the multispectral and IASI retrievals. On the other hand, ozone plumes located below 3 km a.s.l. are only clearly depicted by the multispectral retrieval (both over land and over ocean). This is achieved by a clear enhancement of sensitivity to ozone in the lowest atmospheric layers. The multispectral sensitivity in the LMT peaks at 2 to 2.5 km a.s.l. over land, while sensitivity for IASI or GOME-2 only peaks at 3 to 4 km a.s.l. at lowest (above the LMT). The degrees of freedom for the multispectral retrieval increase by 0.1 (40% in relative terms) with respect to IASI only retrievals for the LMT. Validations with ozonesondes (over Europe during summer 2009) show that our synergetic approach for combining IASI (TIR) and GOME-2 (UV) measurements retrieves lowermost tropospheric ozone with a mean bias of 1% and a precision of 16 %, when smoothing by the retrieval vertical sensitivity (1% mean bias and 21% precision for direct comparisons). C1 [Cuesta, J.; Eremenko, M.; Dufour, G.; Sellitto, P.; Foret, G.; Gaubert, B.; Beekmann, M.; Flaud, J. -M.] Univ Paris Diderot, Univ Paris Est Creteil, CNRS UMR7583, LISA, Creteil, France. [Liu, X.; Chance, K.; Spurr, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cai, Z.] Chinese Acad Sci, IAP, Key Lab Middle Atmosphere & Global Environm Obser, Beijing, Peoples R China. [Hoepfner, M.; von Clarmann, T.; Orphal, J.] KIT, Inst Meteorol & Klimaforsch, Karlsruhe, Germany. [Spurr, R.] RT Solut Inc, Cambridge, MA USA. RP Cuesta, J (reprint author), Univ Paris Diderot, Univ Paris Est Creteil, CNRS UMR7583, LISA, Creteil, France. EM cuesta@lisa.u-pec.fr RI Hopfner, Michael/A-7255-2013; Orphal, Johannes/A-8667-2012; 杨, 宇栋/F-6250-2012; Liu, Xiong/P-7186-2014; OI Hopfner, Michael/0000-0002-4174-9531; Orphal, Johannes/0000-0002-1943-4496; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Centre National des Etudes Spatiales (CNES, the French Space Agency); Universite Paris Est Creteil (UPEC); Centre National des Recherches Scientifiques - Institut National des Sciences de l'Univers (CNRS-INSU); project "GEOQAIR-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere); CNES; "Chaire d'Excellence" of UPEC; data centres ETHER; NOAA CLASS FX The authors are grateful for the financial support given by the Centre National des Etudes Spatiales (CNES, the French Space Agency), the Universite Paris Est Creteil (UPEC) and the Centre National des Recherches Scientifiques - Institut National des Sciences de l'Univers (CNRS-INSU) for achieving this research work and its publication. This study was supported by the project "GEOQAIR-TOSCA" (Terre, Ocean, Surfaces continentals, Atmosphere) financed by CNES and by a "Chaire d'Excellence" of UPEC and CNES. IASI is a joint mission of EUMETSAT and CNES. We acknowledge the support by the data centres ETHER (http://www.pole-ether.fr/) and NOAA CLASS (http://www.class.ncdc.noaa.gov) for providing respectively L1 IASI and GOME-2 data sets, which are originally supplied by EUMETSAT through the Eumetcast system distribution (http://www.eumetsat.int). Meteorological analyses are supplied by ECMWF, surface emissivities by the University of Wisconsin, MODIS-derived aerosol optical depth by NASA and radiosounding profiles by the University of Wyoming. The ozonesonde data sets used in this study were provided by WOUDC. We acknowledge groups responsible for the WOUDC measurements and archives for making the ozonesonde data available. We thank the organizers of the POGEQA meetings in Toulouse and Emeric Hache from Meteo-France for collaboration on radiative transfer calculations as well as Benedict Picquet-Varrault, Aline Gratien, Agnes Perrin and Jean-Michel Hartmann from LISA for fruitful discussions on ozone spectroscopy. NR 61 TC 18 Z9 20 U1 1 U2 25 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2013 VL 13 IS 19 BP 9675 EP 9693 DI 10.5194/acp-13-9675-2013 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 234OY UT WOS:000325654900001 ER PT J AU Iceland, H AF Iceland, Harry TI REFINING PALEO-INDIAN LITHIC TECHNOLOGY AT SHAWNEE-MINISINK VIA AN ARTIFACT REFITTING STUDY SO NORTH AMERICAN ARCHAEOLOGIST LA English DT Article AB A collection of lithic artifacts from the Shawnee-Minisink site in Pennsylvania, originally excavated, analyzed, and published by American University in the 1970-80s, was re-studied using primarily the methodology of refitting. The results of this new study strengthen many of the original conclusions, contradict others, and provide a more nuanced interpretation of Clovis-period activities at the site. It confirms the remarkable spatial integrity of the site and supports the extensive refurbishment of scrapers that entered the site as finished products, as well as on-site production exploiting local chert sources and the use of distinctive hafting techniques. Refitting further confirms the predominance of endscrapers in the assemblage, including fragments that have been interpreted otherwise; suggests that many were made on blades and blade-like flakes, rather than flakes; and provides some evidence for core-blade reduction at the site. This re-analysis strengthens the view that the excavated portion of the site represents an area of intensive specialized economic activity. C1 [Iceland, Harry] Smithsonian Inst, Paleoindian Program, Washington, DC 20560 USA. RP Iceland, H (reprint author), 315 King Farm Blvd,Apt 301, Rockville, MD 20850 USA. EM iceland2@comeast.net NR 23 TC 1 Z9 1 U1 0 U2 5 PU BAYWOOD PUBL CO INC PI AMITYVILLE PA 26 AUSTIN AVE, PO BOX 337, AMITYVILLE, NY 11701 USA SN 0197-6931 EI 1541-3543 J9 N AM ARCHAEOL JI N. Am. Archaeol. PY 2013 VL 34 IS 3 BP 237 EP 267 DI 10.2190/NA.34.3.b PG 31 WC Archaeology SC Archaeology GA 238IH UT WOS:000325938500002 ER PT J AU Kim, PS Jacob, DJ Liu, X Warner, JX Yang, K Chance, K Thouret, V Nedelec, P AF Kim, P. S. Jacob, D. J. Liu, X. Warner, J. X. Yang, K. Chance, K. Thouret, V. Nedelec, P. TI Global ozone-CO correlations from OMI and AIRS: constraints on tropospheric ozone sources SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID NORTH-ATLANTIC OCEAN; TROPICAL SOUTH-ATLANTIC; CARBON-MONOXIDE; SATELLITE MEASUREMENTS; MONITORING INSTRUMENT; STRATOSPHERIC OZONE; MODEL DESCRIPTION; AURA SATELLITE; INTEX-B; EMISSIONS AB We present a global data set of free tropospheric ozone-CO correlations with 2 degrees x 2.5 degrees spatial resolution from the Ozone Monitoring Instrument (OMI) and Atmospheric Infrared Sounder (AIRS) satellite instruments for each season of 2008. OMI and AIRS have near-daily global coverage of ozone and CO respectively and observe coincident scenes with similar vertical sensitivities. The resulting ozone-CO correlations are highly statistically significant (positive or negative) in most regions of the world, and are less noisy than previous satellite-based studies that used sparser data. Comparison with ozone-CO correlations and regression slopes (dO(3)/dCO) from MOZAIC (Measurements of OZone, water vapour, carbon monoxide and nitrogen oxides by in-service AIrbus airCraft) aircraft profiles shows good general agreement. We interpret the observed ozone-CO correlations with the GEOS (Goddard Earth Observing System)-Chem chemical transport model to infer constraints on ozone sources. Driving GEOS-Chem with different meteorological fields generally shows consistent ozone-CO correlation patterns, except in some tropical regions where the correlations are strongly sensitive to model transport error associated with deep convection. GEOS-Chem reproduces the general structure of the observed ozone-CO correlations and regression slopes, although there are some large regional discrepancies. We examine the model sensitivity of dO(3)/dCO to different ozone sources (combustion, biosphere, stratosphere, and lightning NOx) by correlating the ozone change from that source to CO from the standard simulation. The model reproduces the observed positive dO(3)/dCO in the extratropical Northern Hemisphere in spring-summer, driven by combustion sources. Stratospheric influence there is also associated with a positive dO(3)/dCO because of the interweaving of stratospheric downwelling with continental outflow. The well-known ozone maximum over the tropical South Atlantic is associated with negative dO(3)/dCO in the observations; this feature is reproduced in GEOS-Chem and supports a dominant contribution from lightning to the ozone maximum. A major model discrepancy is found over the northeastern Pacific in summer-fall where dO(3)/dCO is positive in the observations but negative in the model, for all ozone sources. We suggest that this reflects a model overestimate of lightning at northern midlatitudes combined with an underestimate of the East Asian CO source. C1 [Kim, P. S.; Jacob, D. J.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Jacob, D. J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Warner, J. X.] Univ Maryland, Coll Comp Math & Nat Sci, College Pk, MD 20742 USA. [Yang, K.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Yang, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Thouret, V.; Nedelec, P.] CNRS, Lab Aerol, UMR5560, Toulouse, France. [Thouret, V.; Nedelec, P.] Univ Toulouse, Toulouse, France. RP Kim, PS (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM kim68@fas.harvard.edu RI Chem, GEOS/C-5595-2014; Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU NASA Aura Program; Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF) [DE-AC05-06OR23100]; MOZAIC program by the European Commission; EADS; Airbus; airline (Lufthansa); airline (Austrian); airline (Air France); airline (Air Namibia) FX This work was funded by the NASA Aura Program and in part by the Department of Energy Office of Science Graduate Fellowship Program (DOE SCGF), made possible in part by the American Recovery and Reinvestment Act of 2009, administered by ORISE-ORAU under contract no. DE-AC05-06OR23100. The authors acknowledge the support of the MOZAIC program by the European Commission, EADS, Airbus, and the airlines (Lufthansa, Austrian, Air France, and Air Namibia) who carry the MOZAIC equipment free of charge and who have performed the maintenance since 1994. The MOZAIC database is supported by ETHER (CNES and INSU-CNRS). NR 84 TC 20 Z9 20 U1 1 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2013 VL 13 IS 18 BP 9321 EP 9335 DI 10.5194/acp-13-9321-2013 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229RC UT WOS:000325283800013 ER PT J AU Davis, DR Mendel, H AF Davis, Donald R. Mendel, Howard TI The genus Erechthias Meyrick of Ascension Island, including discovery of a new brachypterous species ( Lepidoptera, Tineidae) SO ZOOKEYS LA English DT Article DE Brachyptery; distribution; genital morphology; larval case AB One previously named and two new species of the tineid genus Erechthias Meyrick are described and illustrated from the small, remote, mid-Atlantic Ascension Island. With these additions the Lepidoptera fauna of Ascension now totals 38 known species. Little is known regarding the biology of the two new species of Erechthias, and none of the species has been reared from larvae from Ascension. Erechthias minuscula (Walsingham) is a widespread, largely pantropical species first described from the West Indies. Larvae of E. minuscula are known to be scavengers on a wide variety of dead plant material. Erechthias ascensionae, new species, is one of two species of Erechthias now known to be endemic to the island. The other endemic species, Erechthias grayi, new species, is further remarkable in having wing reduction occurring in both sexes. It is one of the few species of Lepidoptera known where this extreme of brachyptery involving both sexes has evolved. The larvae of E. grayi are believed to be lichenivorous, and larval cases suspected to represent this species are illustrated. C1 [Davis, Donald R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Mendel, Howard] Nat Hist Museum, Dept Life Sci Entomol, London SW7 5BD, England. RP Davis, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 105, Washington, DC 20013 USA. EM davisd@si.edu FU Overseas Territories Environment Programme (OTEP); DFID (Department for International Development); Foreign and Commonwealth Office; OTEP FX HM had the good fortune to visit Ascension on three occasions, and the new Erechthias was collected each time. The first trip (August 2003) was greatly assisted by Dr Alan Gray, who was commissioned to carry out an environmental impact assessment on a proposed development at the US airbase there. The second trip (December 2005) consisted of a few days in transit en route to St Helena on a project (Mendel et al. 2008) funded under the Overseas Territories Environment Programme (OTEP) run jointly by DFID (Department for International Development) and the Foreign and Commonwealth Office; their support is gratefully acknowledged. The third visit (November 2012), again organised by Dr Alan Gray, was also a project funded by OTEP. The logistical help and goodwill of Ascension Island Government (AIG) Conservation Department personnel (Stedson Stroud, Jolene Sim, Natasha Williams, Liza White, Catherine Supple, Sam Weber and Nicola Weber,) are gratefully acknowledged. Thanks to Liza White and Dr Andrew Wakeham-Dawson for allowing us to study additional material they collected. NR 55 TC 1 Z9 2 U1 0 U2 5 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 341 BP 1 EP 20 DI 10.3897/zookeys.341.6146 PG 20 WC Zoology SC Zoology GA 232UR UT WOS:000325520400001 PM 24146595 ER PT B AU Boyne, WJ AF Boyne, Walter J. BE Rothstein, H Whaley, B TI MiG Sweep-Operation BOLO SO ART AND SCIENCE OF MILITARY DECEPTION SE Artech House Intelligence and Information Operations Series LA English DT Article; Book Chapter C1 [Boyne, Walter J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ARTECH HOUSE PI NORWOOD PA 685 CANTON ST, NORWOOD, MA 02062 USA BN 978-1-60807-551-5 J9 ARTECH HSE INTEL INF PY 2013 BP 425 EP 431 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA BGY19 UT WOS:000324560900057 ER PT J AU Bak, J Liu, X Wei, JC Pan, LL Chance, K Kim, JH AF Bak, J. Liu, X. Wei, J. C. Pan, L. L. Chance, K. Kim, J. H. TI Improvement of OMI ozone profile retrievals in the upper troposphere and lower stratosphere by the use of a tropopause-based ozone profile climatology SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MONITORING INSTRUMENT; VALIDATION; EXCHANGE AB Motivated by the need of obtaining a more accurate global ozone distribution in the upper troposphere and lower stratosphere (UTLS), we have investigated the use of a tropopause-based (TB) ozone climatology in ozone profile retrieval from the Ozone Monitoring Instrument (OMI). Due to the limited vertical ozone information in the UTLS region from OMI backscattered ultraviolet radiances, better climatological a priori information is important for improving ozone profile retrievals. We present the new TB climatology and evaluate the result of retrievals against previous work. The TB climatology is created using ozonesonde profiles from 1983 through 2008 extended with climatological ozone data above sonde burst altitude (similar to 35 km) with the corresponding temperature profiles used to identify the thermal tropopause. The TB climatology consists of the mean states and 1 sigma standard deviations for every month for each 10 degrees latitude band. Compared to the previous TB climatology by Wei et al. (2010), three additional processes are applied in deriving our climatology: (1) using a variable shifting offset to define the TB coordinate, (2) separating ozonesonde profiles into tropical and extratropical regimes based on a threshold of 14 km in the thermal tropopause height, and (3) merging with an existing climatology from 5-10 km above the tropopause. The first process changes the reference of profiles to a variable position between local and mean tropopause heights within +/- 5 km of the tropopause and to the mean tropopause elsewhere. The second helps to preserve characteristics of either tropical or extratropical ozone structures depending on tropopause height, especially in the subtropical region. The third improves the climatology above ozonesonde burst altitudes and in the stratosphere by using climatology derived from many more satellite observations of ozone profiles. With aid from the National Centers for Environmental Prediction (NCEP) Global Forecast System (GFS) tropopause height, the new climatology and retrieval can better represent the dynamical variability of ozone in the tropopause region. The new retrieval result demonstrates significant improvement of UTLS ozone, especially in the extratropical UTLS, when evaluated using ozonesonde measurements and the meteorological data. The use of TB climatology significantly enhances the spatial consistency and the statistical relationship between ozone and potential vorticity/tropopause height in the extratropical UTLS region. Comparisons with ozonesonde measurements show substantial improvements in both mean biases and their standard deviations over the extratropical lowermost stratosphere and upper troposphere. Overall, OMI retrievals with the TB climatology show improved ability in capturing ozone gradients across the tropopause found in tropical/extratropical ozonesonde measurements. C1 [Bak, J.; Kim, J. H.] Pusan Natl Univ, Pusan, South Korea. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wei, J. C.] Adnet Syst Inc, Rockville, MD USA. [Wei, J. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pan, L. L.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Kim, JH (reprint author), Pusan Natl Univ, Pusan, South Korea. EM jaekim@pusan.ac.kr RI Pan, Laura/A-9296-2008; Liu, Xiong/P-7186-2014; OI Pan, Laura/0000-0001-7377-2114; Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU Eco Innovation Program of KEITI, Korea [ARQ201204015] FX Research at Pusan National University by J. Bak and J. H. Kim is funded by the Eco Innovation Program of KEITI (ARQ201204015), Korea. Research at the Smithsonian Astrophysical Observatory (SAO) by X. Liu and K. Chance, as well as by J. Bak during her 6-month visit to the SAO is supported by NASA and the Smithsonian Institution. We acknowledge the WOUDC, SHADOZ and NOAA/ESRL for providing ozonesonde data, OMI science team for providing OMI level 1b data. The NCEP GFS data for this study are from the Research Data Archive (RDA), which is maintained by the Computational and Information Systems Laboratory (CISL) at the National Center for Atmospheric Research (NCAR); the original data are available from the RDA (http://rda.ucar.edu) in dataset number ds083.2. NR 38 TC 5 Z9 6 U1 0 U2 7 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2013 VL 6 IS 9 BP 2239 EP 2254 DI 10.5194/amt-6-2239-2013 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 229SB UT WOS:000325286500001 ER PT J AU Furth, DG AF Furth, David G. TI Diversity of Alticinae in Oaxaca, Mexico: A preliminary study (Coleoptera, Chrysomelidae) SO ZOOKEYS LA English DT Article DE Mexico; Oaxaca; diversity; Coleoptera; Chrysomelidae; Alticinae; endemism; fieldwork; collections ID AMERICA AB This is a preliminary study of the diversity of the Flea Beetles (Alticinae) of the Mexican state of Oaxaca based on fieldwork by the author in 1991, 1997, and 2010, the literature, and specimens in several institutional collections. The number of genera and species for Mexico as well as for Oaxaca increased significantly from previous studies. There are now 625 species in 90 genera recorded from Mexico with 275 species in 68 genera recorded from Oaxaca. There are 113 species known only from the state of Oaxaca and another 38 species known only from Oaxaca and the surrounding states. Oaxaca has a relatively high diversity as well as a high percentage of endemism. This study also demonstrates the effects of how even a small amount of fieldwork together with extracting specimen data from institutional collections can significantly increase the total faunistic and diversity knowledge of an area. A complete list of the genera and species known from Oaxaca is included. C1 Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. RP Furth, DG (reprint author), Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. EM furthd@si.edu FU National Museum of Natural History's (Smithsonian Institution) Small Grants Program FX I would like to thank the following persons for access to specimens: Cheryl Barr (University of California Berkeley); Charles Bellamy (California Department of Food & Agriculture, Sacramento); Shawn Clark (Brigham Young University, Provo); Lee Hermann (American Museum of Natural History, New York); Lynn Kimsey (University of California, Davis); Alexander Konstantinov (National Museum of Natural History, Washington, D.C.); Norman Penny (California Academy of Sciences, San Francisco); Edward Riley (Texas A & M University, College Station); Sharon Shute (Natural History Museum, London); Eva Sprecher-Ubersax (Naturhistorisches Museum Basel). For help with the digital photographs of specimens in Figure 10 I would like to thank Karie Darrow and for help with the other figures, maps, appendix, and other technical advice I am very grateful to Floyd Shockley, both from my department. I am also grateful to Diana X. Munn from my museum for assistance during the field trip of 2010 and for the Resumen. For funding for the 2010 fieldwork in Oaxaca I thank the National Museum of Natural History's (Smithsonian Institution) Small Grants Program. NR 22 TC 4 Z9 5 U1 3 U2 6 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 332 SI SI BP 1 EP 32 DI 10.3897/zookeys.332.4790 PG 32 WC Zoology SC Zoology GA 221AM UT WOS:000324629300001 PM 24163579 ER PT J AU Moser, WE Briggler, JT Richardson, DJ Schuette, CD Hammond, CI Hopkins, WA Lazo-Wasem, EA AF Moser, William E. Briggler, Jeffrey T. Richardson, Dennis J. Schuette, Chawna D. Hammond, Charlotte I. Hopkins, William A. Lazo-Wasem, Eric A. TI Redescription and molecular characterization of Placobdella cryptobranchii (Johnson & Klemm, 1977) (Glossiphoniidae, Hirudinida) SO ZOOKEYS LA English DT Article DE Placobdella cryptobranchii; Batracobdella; Desserobdella; Cryptobranchus bishopi; Cryptobranchus alleganiensis bishopi; Ozark Hellbender; Glossiphoniidae; Hirudinea; Rhychobdellida; Clitellata; leech ID OZARK HELLBENDER; LEECH; OLIGACANTHORHYNCHIDAE; VERRILL; HOST AB Placobdella cryptobranchii (Johnson & Klemm, 1977) was originally described from specimens collected from Ozark Hellbenders (Cryptobranchus alleganiensis bishopi) from the North Fork of the White River in Missouri, U.S.A. Leeches collected during August 2009 to August 2011 from five localities in Missouri (including the type locality) facilitated a redescription and molecular characterization of P. cryptobranchii. Placobdella cryptobranchii has a rusty, reddish-brown dorsum with 2 lateral rows of unpigmented papillae, two unpigmented nuchal bands, unpigmented patches, and pair of four pre-anal papillae. Molecular comparison of CO-I sequence data from P. cryptobranchii revealed a 93-94% similarity to Placobdella ornata and 10-17% difference among other species of Placobdella. C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Briggler, Jeffrey T.] Missouri Dept Conservat, Jefferson City, MO 65109 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Schuette, Chawna D.] St Louis Zoo, Herpetol & Aquat, St Louis, MO 63110 USA. [Hopkins, William A.] Virginia Tech, Dept Fish & Wildlife Conservat, Blacksburg, VA 24061 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu NR 20 TC 3 Z9 3 U1 2 U2 4 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 338 BP 1 EP 10 DI 10.3897/zookeys.338.5995 PG 10 WC Zoology SC Zoology GA 227QY UT WOS:000325129800001 PM 24146580 ER PT J AU Windsor, DM Dury, GJ Frieiro-Costa, FA Lanckowsky, S Pasteels, JM AF Windsor, Donald M. Dury, Guillaume J. Frieiro-Costa, Fernando A. Lanckowsky, Susanne Pasteels, Jacques M. TI Subsocial Neotropical Doryphorini (Chrysomelidae, Chrysomelinae): new observations on behavior, host plants and systematics SO ZOOKEYS LA English DT Article DE Maternal care; Subsociality; Coleoptera; Chrysomelidae; Chrysomelinae; Neotropical ID COLEOPTERA-CHRYSOMELIDAE; LEAF BEETLES; NATURAL-HISTORY; INSECTS; EVOLUTION; PATTERNS; BIOLOGY; CARE; DNA AB A summary of literature, documented observations and field studies finds evidence that mothers actively defend offspring in at least eight species and three genera of Neotropical Chrysomelinae associated with two host plant families. Reports on three Doryphora species reveal that all are oviparous and feed on vines in the Apocyanaceae. Mothers in the two subsocial species defend eggs and larvae by straddling, blocking access at the petiole and greeting potential predators with leaf-shaking and jerky advances. A less aggressive form of maternal care is found in two Platyphora and four Proseicela species associated with Solanaceae, shrubs and small trees. For these and other morphologically similar taxa associated with Solanaceae, genetic distances support morphology-based taxonomy at the species level, reveal one new species, but raise questions regarding boundaries separating genera. We urge continued study of these magnificent insects, their enemies and their defenses, both behavioral and chemical, especially in forests along the eastern versant of the Central and South American cordillera. C1 [Windsor, Donald M.; Dury, Guillaume J.] Smithsonian Trop Res Inst, Balboa 084300153, Panama. [Dury, Guillaume J.] McGill Univ, Dept Plant Sci, Quebec City, PQ H9X 3V9, Canada. [Frieiro-Costa, Fernando A.] Ctr Univ Lavras, Setor Zool, BR-37200000 Lavras, Minas Gerais, Brazil. [Lanckowsky, Susanne] Staatliches Museum Naturkun Karlsruhe, Referat Entomol, D-76133 Karlsruhe, Germany. [Pasteels, Jacques M.] Univ Libre Brussels, B-1050 Brussels, Belgium. RP Windsor, DM (reprint author), Smithsonian Trop Res Inst, Apartado, Balboa 084300153, Panama. EM windsord@si.edu NR 45 TC 3 Z9 3 U1 1 U2 4 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 332 SI SI BP 71 EP 93 DI 10.3897/zookeys.332.5199 PG 23 WC Zoology SC Zoology GA 221AM UT WOS:000324629300004 PM 24163582 ER PT J AU Flack, JC Erwin, D Elliot, T Krakauer, DC AF Flack, Jessica C. Erwin, Doug Elliot, Tanya Krakauer, David C. BE Sterelny, K Joyce, R Calcott, B Fraser, B TI Timescales, Symmetry, and Uncertainty Reduction in the Origins of Hierarchy in Biological Systems SO COOPERATION AND ITS EVOLUTION SE Life and Mind-Philosophical Issues in Biology and Psychology LA English DT Article; Book Chapter ID GENE REGULATORY NETWORKS; NICHE CONSTRUCTION; ECOSYSTEM ENGINEERS; MUTATION-RATE; EVOLUTION; STABILITY; MACROEVOLUTION; CONSEQUENCES; ASSEMBLAGES; PERSPECTIVE C1 [Flack, Jessica C.; Erwin, Doug; Elliot, Tanya; Krakauer, David C.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Erwin, Doug] Smithsonian Inst, Washington, DC 20560 USA. RP Flack, JC (reprint author), Santa Fe Inst, Santa Fe, NM 87501 USA. NR 86 TC 7 Z9 7 U1 2 U2 9 PU MIT PRESS PI CAMBRIDGE PA FIVE CAMBRIDGE CENTER, CAMBRIDGE, MA 02142 USA BN 978-0-262-01853-1 J9 LIFE MIND-PHILOS ISS PY 2013 BP 45 EP 74 PG 30 WC Psychology, Biological; Behavioral Sciences; Evolutionary Biology; Psychology, Social SC Psychology; Behavioral Sciences; Evolutionary Biology GA BGB89 UT WOS:000322219800003 ER PT J AU Quintero, GC AF Quintero, Gabriel C. TI Role of nucleus accumbens glutamatergic plasticity in drug addiction SO NEUROPSYCHIATRIC DISEASE AND TREATMENT LA English DT Review DE glutamate; drug addiction; nucleus accumbens ID COCAINE-SEEKING BEHAVIOR; OBSESSIVE-COMPULSIVE DISORDER; PERMEABLE AMPA RECEPTORS; FAMILY-BASED ASSOCIATION; N-ACETYLCYSTEINE; SYNAPTIC PLASTICITY; NEUROTROPHIC FACTOR; GLUTAMATE-RECEPTOR-6 GENE; STRUCTURAL PLASTICITY; PARKINSONS-DISEASE AB Substance dependence is characterized by a group of symptoms, according to the Diagnostic and Statistical Manual of Mental Disorders, 4th Edition, Text Revision (DSM-IV-TR). These symptoms include tolerance, withdrawal, drug consumption for alleviating withdrawal, exaggerated consumption beyond original intention, failure to reduce drug consumption, expending a considerable amount of time obtaining or recovering from the substance's effects, disregard of basic aspects of life (for example, family), and maintenance of drug consumption, despite facing adverse consequences. The nucleus accumbens (NAc) is a brain structure located in the basal forebrain of vertebrates, and it has been the target of addictive drugs. Different neurotransmitter systems at the level of the NAc circuitry have been linked to the different problems of drug addiction, like compulsive use and relapse. The glutamate system has been linked mainly to relapse after drug-seeking extinction. The dopamine system has been linked mainly to compulsive drug use. The glutamate homeostasis hypothesis centers around the dynamics of synaptic and extrasynaptic levels of glutamate, and their impact on circuitry from the prefrontal cortex (PFC) to the NAc. After repetitive drug use, deregulation of this homeostasis increases the release of glutamate from the PFC to the NAc during drug relapse. Glial cells also play a fundamental role in this hypothesis; glial cells shape the interactions between the PFC and the NAc by means of altering glutamate levels in synaptic and extrasynaptic spaces. On the other hand, cocaine self-administration and withdrawal increases the surface expression of subunit glutamate receptor 1 (GluA1) of alpha-amino-3-hydroxy-5-methyl-4-isoxazolepropionic acid (AMPA) receptors at the level of the NAc. Also, cocaine self-administration and withdrawal induce the formation of subunit glutamate -receptor 2 (GluA2), lacking the Ca2+-permeable AMPA receptors (CP-AMPARs) at the level of the NAc. Antagonism of the CP-AMPARs reduces cravings. It is necessary to pursue further exploration of the AMPA receptor subunit composition and variations at the level of the NAc for a better understanding of glutamatergic plastic changes. It is known that cocaine and morphine are able to induce changes in dendritic spine morphology by modifying actin cycling. These changes include an initial increase in spine head diameter and increases in AMPA receptor expression, followed by a second stage of spine head diameter retraction and reduction of the AMPA receptors' expression in spines. Besides glutamate and dopamine, other factors, like brain-derived neurotrophic factor (BDNF), can influence NAc activity and induce changes in dendritic spine density. BDNF also induces drug-related behaviors like self-administration and relapse. Neither apoptosis nor neurogenesis plays a relevant role in the neurobiological processes subjacent to cocaine addiction in adults (rodent or human). Different therapeutic drugs like N-acetylcysteine (NAC), modafinil, acamprosate, and topiramate have been tested in preclinical and/or clinical models for alleviating drug relapse. Moreover, these therapeutic drugs target the glutamatergic circuitry between the PFC and the NAc. NAC and acamprosate have shown inconsistent results in clinical trials. Modafinil and topiramate have shown some success, but more clinical trials are necessary. Based on the current review findings, it could be recommendable to explore therapeutic approaches that include synergism between different drugs and neurotransmitter systems. The discrepancy in the results of some therapeutic drugs between preclinical versus clinical trials for alleviating relapse or drug dependence could be linked to the scarce exploration of preclinical models that mimic polydrug abuse patterns, for example, cocaine plus alcohol. At the clinical level, the pattern of polydrug consumption is a phenomenon of considerable frequency. Finally, as a complement at the end, an updated summary is included about the role of glutamate in other neuropsychiatric disorders (for example, mood disorders, schizophrenia, and others). C1 [Quintero, Gabriel C.] Florida State Univ Panama, Clayton, Ciudad Del Sabe, Panama. [Quintero, Gabriel C.] Med Univ S Carolina, Charleston, SC 29425 USA. [Quintero, Gabriel C.] Smithsonian Trop Res Inst, Ancon, Panama. RP Quintero, GC (reprint author), Florida State Univ Panama, Bldg 227, Clayton, Ciudad Del Sabe, Panama. EM gquintero@fsu.edu FU SENACYT-IFARHU Fellowship; Programa de Becas de Doctorado y Post-Doctorado; SNI (Sistema Nacional de Investigacion) (SENACYT-Panama) FX Thanks to the SENACYT-IFARHU Fellowship (SENACYT - Secretaria Nacional de Ciencia, Tecnologia e Innovacion; IFARHU: Instituto para la Formacion y Aprovechamiento de Recursos Humanos), the Programa de Becas de Doctorado y Post-Doctorado, and SNI (Sistema Nacional de Investigacion) (SENACYT-Panama) awarded to GCQ. Thanks to Peter W Kalivas (MUSC) for lab facilities and support. NR 125 TC 22 Z9 23 U1 3 U2 23 PU DOVE MEDICAL PRESS LTD PI ALBANY PA PO BOX 300-008, ALBANY, AUCKLAND 0752, NEW ZEALAND SN 1176-6328 J9 NEUROPSYCH DIS TREAT JI Neuropsychiatr. Dis. Treat. PY 2013 VL 9 BP 1499 EP 1512 DI 10.2147/NDT.S45963 PG 14 WC Clinical Neurology; Psychiatry SC Neurosciences & Neurology; Psychiatry GA 224RH UT WOS:000324905300001 PM 24109187 ER PT B AU Van Loo, S Butler, MJ Tan, JC Falle, SAEG AF Van Loo, Sven Butler, Mike J. Tan, Jonathan C. Falle, Sam A. E. G. BE Pogorelov, NV Audit, E Zank, GP TI Kiloparsec-Scale Simulations of Magnetised Molecular Clouds in Disk Galaxies SO NUMERICAL MODELING OF SPACE PLASMA FLOWS ASTRONUM-2012 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 7th Annual International Conference on Numerical Modeling of Space Plasma Flows CY JUN 25-29, 2012 CL Big Isl, HI SP Univ Alabama, Ctr Space Plasma & Aeronom Res, CEA CNRS, Maison Simulat ID STAR-FORMATION; INTERSTELLAR-MEDIUM; NEARBY GALAXIES; INSTABILITY; FIELDS; MODELS AB We present simulations of the evolution of self-gravitating dense gas on kiloparsec-size scales in a galactic disk, designed to study dense clump formation from giant molecular clouds (GMCs). These dense clumps are expected to be the precursors to star clusters and this process may be the rate limiting step controlling star formation rates in galactic systems as described by the Kennicutt-Schmidt relation. The evolution of these simulated GMCs and clumps is determined by self-gravity balanced by turbulent pressure support and the large scale galactic shear. While the cloud structures and densities significantly change during their evolution, they remain roughly in virial equilibrium for time scales exceeding the free-fall time of GMCs, indicating that energy from the galactic shear continuously cascades down. We implement star formation at a slow, inefficient rate of 2% per local free-fall time, but this still yields global star formation rates that are similar to two orders of magnitude larger than the observed Kennicutt-Schmidt relation due to the over-production of dense clump gas. To explain this discrepancy, we anticipate magnetic fields to provide additional support. Low-resolution simulations indeed show that the magnetic field reduces the star formation rate. C1 [Van Loo, Sven] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Van Loo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svanloo@cfa.harvard.edu NR 14 TC 0 Z9 0 U1 1 U2 6 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-832-9 J9 ASTR SOC P PY 2013 VL 474 BP 122 EP 127 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGW86 UT WOS:000324446200019 ER PT J AU Prathapan, KD Konstantinov, AS Shameem, KM Balan, AP AF Prathapan, Kaniyarikkal Divakaran Konstantinov, Alexander S. Shameem, K. M. Balan, A. P. TI First record of leaf-hole shelters used and modified by leaf beetles (Coleoptera, Chrysomelidae), with descriptions of two new Orthaltica Crotch species from southern India SO ZOOKEYS LA English DT Article DE Leaf-hole shelter; faeces; leaf beetles; new species; host plant ID NATURAL-HISTORY; GALERUCINAE AB Behavioural novelties observed in adult leaf beetles of two new Orthaltica Crotch species include: 1) the use of low cost leaf-hole shelters, either in pre-formed holes produced by larger beetles that fed on the same leaf, or artificially created holes as part of an experiment; and 2) the use of faeces to partition the hole. Two new southern Indian species of the genus Orthaltica are described and illustrated: O. syzygium and O. terminalia. Host plants are identified for both species. A key to the Indian species of Orthaltica is provided. C1 [Prathapan, Kaniyarikkal Divakaran; Shameem, K. M.; Balan, A. P.] Kerala Agr Univ, Dept Entomol, Trivandrum 695522, Kerala, India. [Konstantinov, Alexander S.] Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, Washington, DC 20013 USA. RP Konstantinov, AS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, ARS,USDA, POB 37012,MRC-168, Washington, DC 20013 USA. EM alex.konstantinov@ars.usda.gov NR 21 TC 1 Z9 1 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 336 BP 47 EP 59 DI 10.3897/zookeys.336.5435 PG 13 WC Zoology SC Zoology GA 224RS UT WOS:000324906400003 PM 24146572 ER PT J AU Foerder, P Chodorow, M Moore, DE AF Foerder, Preston Chodorow, Martin Moore, Donald E., III TI Behavioural synchrony in two species of communally housed captive penguins SO BEHAVIOUR LA English DT Article DE penguins; behavioural synchrony; captivity ID ASSOCIATION; CHINSTRAP; GENTOO AB Animals in aggregations such as herds, schools, flocks, or colonies tend to synchronize their behaviour with each other for food acquisition and predator detection. Different species of captive penguins, when housed communally, intermingle more than in their natural habitat. Wild penguins typically divide themselves into separate colonies by species. We predicted that penguins would synchronize their behaviour more with conspecifics rather than interspecifically in a mixed-species zoo exhibit. The subjects were 65 penguins of two different species, chinstrap (Pygoscelis antarctica) and gentoo (Pygoscelis papua) in the Central Park Zoo, New York, NY, USA. Using instantaneous scan sampling, 359 video scans were taken over 10 days. Scans were analysed for nine different categories of behaviour for both species. Intra-species synchrony scores were calculated using the Kappa coefficient of agreement, and inter-species synchrony was measured by computing cross-correlations. As predicted, overall synchrony was significantly greater within both species of penguins than for randomly aggregated data representing mixed groups. There was also significantly less synchrony between species than between randomly mixed data for six of the nine behaviour categories. The pattern of results indicates that the penguins had organized by behaviour into separate species-specific colonies within the enclosure. They maintained species separation through behavioural synchrony despite the restrictions imposed by captivity. C1 [Foerder, Preston; Chodorow, Martin] CUNY Hunter Coll, Dept Psychol, New York, NY USA. [Moore, Donald E., III] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. RP Foerder, P (reprint author), CUNY Hunter Coll, Dept Psychol, 611 Hunter North,695 Pk Ave, New York, NY USA. EM preston-foerder@utc.edu NR 39 TC 1 Z9 1 U1 5 U2 56 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PY 2013 VL 150 IS 12 BP 1357 EP 1374 DI 10.1163/1568539X-00003100 PG 18 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 214AF UT WOS:000324101500002 ER PT J AU Frescura, VD Kuhn, AW Laughinghouse, HD Nicoloso, FT Lopes, SJ Tedesco, SB AF Frescura, Viviane Dal-Souto Kuhn, Andrielle Wouters Laughinghouse, Haywood Dail Nicoloso, Fernando Teixeira Lopes, Sidnei Jose Tedesco, Solange Bosio TI Evaluation of the allelopathic, genotoxic, and antiproliferative effect of the medicinal species Psychotria brachypoda and Psychotria birotula (Rubiaceae) on the germination and cell division of Eruca sativa (Brassicaceae) SO CARYOLOGIA LA English DT Article DE biological assays; alellopathy; Psychotria brachypoda; Psychotria birotula; Eruca sativa ID ALLIUM-CEPA; GROWTH; EXTRACTS; PLANTS; BIDENS; CYCLE; L. AB Biological assays are widely used to monitor toxic and allelopathic substances. The present study aimed to evaluate the allelopathic, genotoxic, and antiproliferative potential of aqueous extracts of Psychotria brachypoda (Mull. Arg.) Britton and Psychotria birotula Smith & Downs in two concentrations on the germination and cell division of Eruca sativa Hill. seeds. The biological assay was conducted in a controlled growth chamber. For monitoring the allelopathic effect, the following variables were evaluated: total number of germinated seeds, seedling root length, germination velocity index, and germination percentage. The means were compared using the Tukey test and orthogonal contrasts were undertaken to better compare the variables. To evaluate the antiproliferative and genotoxic effects, seedling roots were collected and the squashing technique was followed for preparation of slides. The results of the present study demonstrated that the medicinal species Psychotria brachypoda and Psychotria birotula inhibited root growth, germination velocity index, and germination percentage in seeds of arugula, in addition to inhibiting cell division and inducing chromosomal alterations in Eruca sativa. We conclude that the studied species have alellopathic, genotoxic, and antiproliferative effects on Eruca sativa in both concentrations studied. C1 [Frescura, Viviane Dal-Souto] Univ Fed Santa Maria, Grad Program Agrobiol, Santa Maria, RS, Brazil. [Kuhn, Andrielle Wouters] Univ Fed Santa Maria, Undergrad Program Biol, Santa Maria, RS, Brazil. [Laughinghouse, Haywood Dail] Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. [Laughinghouse, Haywood Dail] Univ Liege, Inst Chem, Ctr Prot Engn, Liege, Belgium. [Nicoloso, Fernando Teixeira; Lopes, Sidnei Jose; Tedesco, Solange Bosio] Univ Fed Santa Maria, Dept Bot, Santa Maria, RS, Brazil. RP Laughinghouse, HD (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20560 USA. EM hdliv@hotmail.com RI Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) FX The authors thank the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) for financial support, Prof. Jucara Terzinha Paranhos for assistance in fieldwork, R. M. Fischer for comments on the final text. NR 33 TC 5 Z9 5 U1 0 U2 7 PU UNIV FLORENCE BOTANY INST PI FLORENCE PA VIA LAMARMORA 4, 50121 FLORENCE, ITALY SN 0008-7114 J9 CARYOLOGIA JI Caryologia PY 2013 VL 66 IS 2 BP 138 EP 144 DI 10.1080/00087114.2013.821832 PG 7 WC Plant Sciences; Genetics & Heredity SC Plant Sciences; Genetics & Heredity GA 214EF UT WOS:000324113100006 ER PT J AU Yu, XY Wang, JP Kays, R Jansen, PA Wang, TJ Huang, T AF Yu, Xiaoyuan Wang, Jiangping Kays, Roland Jansen, Patrick A. Wang, Tianjiang Huang, Thomas TI Automated identification of animal species in camera trap images SO EURASIP JOURNAL ON IMAGE AND VIDEO PROCESSING LA English DT Article DE Species identification; SIFT; cLBP; Feature learning; Max pooling; Weighted sparse coding ID CLASSIFICATION; RECOGNITION AB Image sensors are increasingly being used in biodiversity monitoring, with each study generating many thousands or millions of pictures. Efficiently identifying the species captured by each image is a critical challenge for the advancement of this field. Here, we present an automated species identification method for wildlife pictures captured by remote camera traps. Our process starts with images that are cropped out of the background. We then use improved sparse coding spatial pyramid matching (ScSPM), which extracts dense SIFT descriptor and cell-structured LBP (cLBP) as the local features, that generates global feature via weighted sparse coding and max pooling using multi-scale pyramid kernel, and classifies the images by a linear support vector machine algorithm. Weighted sparse coding is used to enforce both sparsity and locality of encoding in feature space. We tested the method on a dataset with over 7,000 camera trap images of 18 species from two different field cites, and achieved an average classification accuracy of 82%. Our analysis demonstrates that the combination of SIFT and cLBP can serve as a useful technique for animal species recognition in real, complex scenarios. C1 [Yu, Xiaoyuan; Wang, Tianjiang] Huazhong Univ Sci & Technol, Dept Comp Sci, Wuhan 430074, Hubei, Peoples R China. [Yu, Xiaoyuan; Wang, Jiangping; Huang, Thomas] Univ Illinois, Beckman Inst, Urbana, IL USA. [Kays, Roland; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon Panama, Panama. [Kays, Roland] North Carolina Museum Nat Sci, Raleigh, NC USA. [Kays, Roland] N Carolina State Univ, Fisheries Wildlife & Conservat Program, Raleigh, NC 27695 USA. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AP Wageningen, Netherlands. RP Wang, JP (reprint author), Univ Illinois, Beckman Inst, Urbana, IL USA. EM jwang63@illinois.edu RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU National Science Foundation [DBI 10-62351]; National Natural Science Foundation of China [61073094] FX This work was supported in part by the National Science Foundation Grant DBI 10-62351. Field data were collected with support from the National Science Foundation (NSF-DEB 0717071 to R. W. K.) and the Netherlands Organization for Scientific Research (863-07-008 to P. A. J.). XY and TW would like to acknowledge support by the National Natural Science Foundation of China Grant 61073094. NR 18 TC 15 Z9 15 U1 6 U2 33 PU SPRINGER INTERNATIONAL PUBLISHING AG PI CHAM PA GEWERBESTRASSE 11, CHAM, CH-6330, SWITZERLAND SN 1687-5281 J9 EURASIP J IMAGE VIDE JI EURASIP J. Image Video Process. PY 2013 AR 52 DI 10.1186/1687-5281-2013-52 PG 10 WC Engineering, Electrical & Electronic; Imaging Science & Photographic Technology SC Engineering; Imaging Science & Photographic Technology GA 219XR UT WOS:000324545500001 ER PT J AU Gurdebeke, PR Van Bocxlaer, B AF Gurdebeke, Pieter R. Van Bocxlaer, Bert TI Conch logical differentiation in an ongoing radiation of Lanistes gastropods from ancient Lake Malawi: how adaptive is shell morphology? SO GEOLOGICA BELGICA LA English DT Editorial Material ID AFRICA C1 [Gurdebeke, Pieter R.; Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Gurdebeke, PR (reprint author), Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. EM pieter.gurdebeke@ugent.be RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X NR 10 TC 3 Z9 3 U1 0 U2 10 PU GEOLOGICA BELGICA PI BRUSSELS PA JENNER STREET 13, BRUSSELS, BELGIUM SN 1374-8505 J9 GEOL BELG JI Geol. Belg. PY 2013 VL 16 IS 1-2 BP 118 EP 119 PG 2 WC Geology SC Geology GA 218RK UT WOS:000324449900011 ER PT J AU Gervais, C Languille, MA Reguer, S Gillet, M Pelletier, S Garnier, C Vicenzi, EP Bertrand, L AF Gervais, Claire Languille, Marie-Angelique Reguer, Solenn Gillet, Martine Pelletier, Sebastien Garnier, Chantal Vicenzi, Edward P. Bertrand, Loic TI Why does Prussian blue fade? Understanding the role(s) of the substrate SO JOURNAL OF ANALYTICAL ATOMIC SPECTROMETRY LA English DT Article ID ABSORPTION-SPECTRA; K-EDGE; COMPLEXES; PAPER; CHEMILUMINESCENCE; ELECTROCHEMISTRY; DEGRADATION; DIFFRACTION; CELLULOSE; FILMS AB Prussian blue (PB) and its analogues are widely studied because of their interesting and promising magnetic and optical properties. The pigment Prussian blue, found in different types of artworks (paintings, watercolors and photographs), is also studied in the area of heritage science, where its capricious fading behavior under light or anoxia treatment poses problematic conservation issues. PB fading is due to the reduction of iron(III) to iron(II) and depends significantly on the artefact. This paper focuses on the roles of the substrate in affecting the PB structure and modifying the redox process. In particular, X-ray absorption experiments at the Fe K-edge of unfaded and faded PB-paper samples show that changes in the PB structure can happen by simple contact with the substrate, prior to the fading treatment. Spectrophotometric measurements on a series of model PB-paper samples further demonstrate the multiple influences of the substrate and show that not only its chemical composition but also its role as a dispersion and textured medium significantly alter the fading behavior of PB. A potential roadmap is proposed to rationally investigate the complex fading process of Prussian blue on a substrate. C1 [Gervais, Claire; Vicenzi, Edward P.] Smithsonian Museum, Conservat Inst, Suitland, MD 20746 USA. [Languille, Marie-Angelique; Pelletier, Sebastien; Bertrand, Loic] Synchrotron SOLEIL, MCC, CNRS, IPANEMA,USR 3461, F-91192 Gif Sur Yvette, France. [Reguer, Solenn; Bertrand, Loic] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France. [Gillet, Martine; Garnier, Chantal] CNRS, USR3224, MCC, Museum Natl Hist Nat CRCC, F-75005 Paris, France. RP Gervais, C (reprint author), Bern Univ Arts, Fellerstr 11, CH-3027 Bern, Switzerland. EM claire.gervais@bfh.ch RI Gervais, Claire/E-5505-2012 OI Gervais, Claire/0000-0003-2433-5537 FU Swiss National Science Foundation [138986] FX We deeply thank K. Chaouchi and S. Blanchandin for their help in preparing the samples, Dr E. Elkaim for his help on the CRISTAL beamline and Dr P. Dumas for access to the Raman spectrometer. We thank Dr P. Ropret also for the paint samples and M. Ballard for information about Prussian blue dyeing. C. Gervais would like to acknowledge the Swiss National Science Foundation for partial funding of this project through the grant no. 138986, as well as Dr T. Wust and Prof. P. Laszlo for useful comments. We thank Dr R.J. Koestler for suggesting investigation of Prussian blue fading in cultural artefacts. This work has been developed as part of the IPANEMA/Smithsonian Institution agreement on science cooperation. NR 50 TC 11 Z9 11 U1 2 U2 27 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 0267-9477 EI 1364-5544 J9 J ANAL ATOM SPECTROM JI J. Anal. At. Spectrom. PY 2013 VL 28 IS 10 BP 1600 EP 1609 DI 10.1039/c3ja50025j PG 10 WC Chemistry, Analytical; Spectroscopy SC Chemistry; Spectroscopy GA 218EE UT WOS:000324414800004 ER PT J AU Hershler, R Liu, HP Bradford, C AF Hershler, Robert Liu, Hsiu-Ping Bradford, Corbin TI Systematics of a widely distributed western North American springsnail, Pyrgulopsis micrococcus (Caenogastropoda, Hydrobiidae), with descriptions of three new congeners SO ZOOKEYS LA English DT Article DE Pyrgulopsis; Hydrobiidae; Gastropoda; United States; California; Nevada; freshwater; taxonomy; conservation ID RIVER-BASIN; CALIFORNIA-NEVADA; ASH MEADOWS; GASTROPODA; RISSOOIDEA; SNAILS AB We describe three new species of springsnails (genus Pyrgulopsis) from the Amargosa River basin, California and Nevada (P. licina sp. n., P. perforata sp. n., P. sanchezi sp. n.), each of which was previously considered to be part of P. micrococcus. We also restrict P. micrococcus to its type locality area (Oasis Valley) and redefine a regional congener, P. turbatrix, to include populations from the central Death Valley region and San Bernardino Mountains that had been previously identified as P. micrococcus. The five species treated herein form genetically distinct lineages that differ from each other by 4.2-12.6% for mtCOI and 5.2-13.6% for mtNDI (based on previously published and newly obtained data), and are diagnosable by shell and/or penial characters. The new molecular data presented herein confirm sympatry of P. licina and P. sanchezi in Ash Meadows (consistent with morphological evidence) and delineate an additional lineage of P. micrococcus (in the broad sense) that we do not treat taxonomically owing to the paucity of morphological material. Conservation measures are needed to ensure the long term persistence of populations of P. micrococcus and a genetically differentiated lineage of P. sanchezi which live in disturbed habitats on private lands. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping; Bradford, Corbin] Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM hershlerr@si.edu NR 42 TC 8 Z9 8 U1 0 U2 3 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 330 BP 27 EP 52 DI 10.3897/zookeys.330.5852 PG 26 WC Zoology SC Zoology GA 217XX UT WOS:000324397500002 PM 24146554 ER PT J AU Sun, YW Liu, C Chan, KL Xie, PH Liu, WQ Zeng, Y Wang, SM Huang, SH Chen, J Wang, YP Si, FQ AF Sun, Y. W. Liu, C. Chan, K. L. Xie, P. H. Liu, W. Q. Zeng, Y. Wang, S. M. Huang, S. H. Chen, J. Wang, Y. P. Si, F. Q. TI Stack emission monitoring using non-dispersive infrared spectroscopy with an optimized nonlinear absorption cross interference correction algorithm SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID GAS; POLLUTION; DATABASE; DESIGN AB In this paper, we present an optimized analysis algorithm for non-dispersive infrared (NDIR) to in situ monitor stack emissions. The proposed algorithm simultaneously compensates for nonlinear absorption and cross interference among different gases. We present a mathematical derivation for the measurement error caused by variations in interference coefficients when nonlinear absorption occurs. The proposed algorithm is derived from a classical one and uses interference functions to quantify cross interference. The interference functions vary proportionally with the nonlinear absorption. Thus, interference coefficients among different gases can be modeled by the interference functions whether gases are characterized by linear or nonlinear absorption. In this study, the simultaneous analysis of two components (CO2 and CO) serves as an example for the validation of the proposed algorithm. The interference functions in this case can be obtained by least-squares fitting with third-order polynomials. Experiments show that the results of cross interference correction are improved significantly by utilizing the fitted interference functions when nonlinear absorptions occur. The dynamic measurement ranges of CO2 and CO are improved by about a factor of 1.8 and 3.5, respectively. A commercial analyzer with high accuracy was used to validate the CO and CO2 measurements derived from the NDIR analyzer prototype in which the new algorithm was embedded. The comparison of the two analyzers show that the prototype works well both within the linear and nonlinear ranges. C1 [Sun, Y. W.; Xie, P. H.; Liu, W. Q.; Zeng, Y.; Wang, S. M.; Huang, S. H.; Chen, J.; Wang, Y. P.; Si, F. Q.] Chinese Acad Sci, Anhui Inst Opt & Fine Mech, Key Lab Environm Opt & Technol, Hefei 230031, Peoples R China. [Liu, C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chan, K. L.] City Univ Hong Kong, Sch Energy & Environm, Hong Kong, Hong Kong, Peoples R China. RP Liu, C (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ywsun@aiofm.ac.cn; chliu@cfa.harvard.edu FU Special Scientific Research Fund of Meteorological Public Welfare Profession of China [GYHY201106045-1, 201109007]; Anhui Province Natural Science Foundation of China [1308085QF124]; National Natural Science Foundation of China [41275037, 41105011] FX This work is jointly supported by the Special Scientific Research Fund of Meteorological Public Welfare Profession of China (Grant No. GYHY201106045-1 and No. 201109007), Anhui Province Natural Science Foundation of China (Grant No. 1308085QF124), and the National Natural Science Foundation of China (Grant No. 41275037 and No. 41105011). We thank X. Zhou, manager of the Shangfeng cement plant, for our access to the field site, and C. Liu for his valuable comments on the manuscript. NR 36 TC 7 Z9 7 U1 2 U2 10 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2013 VL 6 IS 8 BP 1993 EP 2005 DI 10.5194/amt-6-1993-2013 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 212JA UT WOS:000323978000008 ER PT J AU Meyer, V Saatchi, SS Chave, J Dalling, JW Bohlman, S Fricker, GA Robinson, C Neumann, M Hubbell, S AF Meyer, V. Saatchi, S. S. Chave, J. Dalling, J. W. Bohlman, S. Fricker, G. A. Robinson, C. Neumann, M. Hubbell, S. TI Detecting tropical forest biomass dynamics from repeated airborne lidar measurements SO BIOGEOSCIENCES LA English DT Article ID BARRO-COLORADO ISLAND; LARGE-FOOTPRINT LIDAR; RAIN-FOREST; CARBON STOCKS; SEVERE DROUGHT; AMAZON FOREST; PANAMA; CANOPY; LIANAS; PLOTS AB Reducing uncertainty of terrestrial carbon cycle depends strongly on the accurate estimation of changes of global forest carbon stock. However, this is a challenging problem from either ground surveys or remote sensing techniques in tropical forests. Here, we examine the feasibility of estimating changes of tropical forest biomass from two airborne lidar measurements of forest height acquired about 10 yr apart over Barro Colorado Island (BCI), Panama. We used the forest inventory data from the 50 ha Center for Tropical Forest Science (CTFS) plot collected every 5 yr during the study period to calibrate the estimation. We compared two approaches for detecting changes in forest aboveground biomass (AGB): (1) relating changes in lidar height metrics from two sensors directly to changes in ground-estimated biomass; and (2) estimating biomass from each lidar sensor and then computing changes in biomass from the difference of two biomass estimates, using two models, namely one model based on five relative height metrics and the other based only on mean canopy height (MCH). We performed the analysis at different spatial scales from 0.04 ha to 10 ha. Method (1) had large uncertainty in directly detecting biomass changes at scales smaller than 10 ha, but provided detailed information about changes of forest structure. The magnitude of error associated with both the mean biomass stock and mean biomass change declined with increasing spatial scales. Method (2) was accurate at the 1 ha scale to estimate AGB stocks (R-2 = 0.7 and RMSEmean = 27.6 Mg ha(-1)). However, to predict biomass changes, errors became comparable to ground estimates only at a spatial scale of about 10 ha or more. Biomass changes were in the same direction at the spatial scale of 1 ha in 60 to 64% of the subplots, corresponding to p values of respectively 0.1 and 0.033. Large errors in estimating biomass changes from lidar data resulted from the uncertainty in detecting changes at 1 ha from ground census data, differences of approximately one year between the ground census and lidar measurements, and differences in sensor characteristics. Our results indicate that the 50 ha BCI plot lost a significant amount of biomass (-0.8Mg ha(-1) yr(-1) +/- 2.2(SD)) over the past decade (2000-2010). Over the entire island and during the same period, mean AGB change was 0.2 +/- 2.4Mg ha(-1) yr(-1) with old growth forests losing -0.7 Mg ha(-1) yr(-1) +/- 2.2 (SD), and secondary forests gaining +1.8Mg ha yr(-1) +/- 3.4 (SD) biomass. Our analysis suggests that repeated lidar surveys, despite taking measurement with different sensors, can estimate biomass changes in old-growth tropical forests at landscape scales (> 10 ha). C1 [Meyer, V.; Saatchi, S. S.; Neumann, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Chave, J.] Univ Toulouse 3, CNRS, UMR5174, Lab Evolut & Divers Biol, F-31062 Toulouse, France. [Dalling, J. W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Bohlman, S.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Fricker, G. A.; Robinson, C.] Univ Calif Los Angeles, Dept Geog, Los Angeles, CA 90095 USA. [Hubbell, S.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, S.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20521 USA. RP Meyer, V (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM victoria.meyer@jpl.nasa.gov FU NSF [0939907]; Smithsonian Tropical Research Institute; University of Illinois; University of California Los Angeles; Clemson University; French "Investissement d'avenir" [CEBA: ANR-10-LABX-0025, TULIP: ANR-10-LABX-0041]; TOSCA funds (CNES, France) FX The research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We would like to thank the reviewers for their constructive comments and recommendations. We are grateful for insightful comments from Helene Muller-Landau. We thank Richard Condit for providing the field data (2010). The BCI forest dynamics research project was made possible by National Science Foundation grants to Stephen P. Hubbell, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund, and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past two decades. The DRL dataset was obtained with funding from NSF grant 0939907, and with additional support from the Smithsonian Tropical Research Institute, University of Illinois, University of California Los Angeles, and Clemson University to S.J. DeWalt. This work has benefited from French "Investissement d'avenir" grants (CEBA: ANR-10-LABX-0025; TULIP: ANR-10-LABX-0041) and from TOSCA funds (CNES, France). NR 58 TC 21 Z9 21 U1 5 U2 57 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2013 VL 10 IS 8 BP 5421 EP 5438 DI 10.5194/bg-10-5421-2013 PG 18 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 212JW UT WOS:000323980300012 ER PT J AU Polizzi, E Bergstrom, M Crofoot, M Fedigan, L Izar, P Perry, S Petite, O Thierry, B Tiddi, B Tokuda, M Verderane, M Wheeler, B Sueur, C AF Polizzi, Eugenia Bergstrom, Mackenzie Crofoot, Margareth Fedigan, Linda Izar, Patricia Perry, Susan Petite, Odile Thierry, Bernard Tiddi, Barbara Tokuda, Marcos Verderane, Michele Wheeler, Brandon Sueur, Cedric TI Comparing Affiliative Relationships of Cebus and Sapajus Species: A Social Networking Approach SO FOLIA PRIMATOLOGICA LA English DT Meeting Abstract DE Cebus; Sapajus; Grooming; Social network; Clustering coefficient C1 [Polizzi, Eugenia] ISTC CNR, Unit Cognit Primatol, Rome, Italy. [Polizzi, Eugenia] ISTC CNR, Ctr Primate, Rome, Italy. [Bergstrom, Mackenzie; Fedigan, Linda] Univ Calgary, Dept Anthropol, Calgary, AB, Canada. [Crofoot, Margareth] Smithsonian Trop Res Inst, Panama City, Panama. [Izar, Patricia; Tokuda, Marcos; Verderane, Michele] Univ Sao Paulo, Inst Psychol, Dept Expt Psychol, Sao Paulo, Brazil. [Perry, Susan] Univ Calif Los Angeles, Dept Anthropol, Los Angeles, CA 90024 USA. [Petite, Odile; Thierry, Bernard; Sueur, Cedric] CNRS, Dept Ecol Physiol & Ethol, Strasbourg, France. [Tiddi, Barbara; Wheeler, Brandon] German Primate Ctr, Cognit Ethol Lab, Gottingen, Germany. EM eugenia.polizzi@gmail.com RI Verderane, Michele/E-3078-2013; Sueur, Cedric/A-4020-2011 OI Sueur, Cedric/0000-0001-8206-2739 NR 0 TC 0 Z9 0 U1 0 U2 2 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0015-5713 J9 FOLIA PRIMATOL JI Folia Primatol. PY 2013 VL 84 IS 3-5 BP 313 EP 313 PG 1 WC Zoology SC Zoology GA 210CR UT WOS:000323807400136 ER PT J AU Reinhardt, JF Whitlatch, RB Osman, RW AF Reinhardt, James F. Whitlatch, Robert B. Osman, Richard W. TI Effects of temperature on the recruitment phenology and niche overlap of shallow epifaunal assemblages in southern New England SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Recruitment; Temperature; Long Island Sound; Niche overlap; Invasive species; Phenology; Fouling community ID CLIMATE-CHANGE; INVASION SUCCESS; SPECIES INTERACTIONS; COMMUNITY; COMPETITION; COEXISTENCE; DISTURBANCE; RESPONSES; SETTLEMENT; DIVERSITY AB Recruitment phenology, or the timing of recruitment, can have a large influence on individuals and populations by affecting their exposure to adverse environmental conditions and interspecific competition. In this study, we examined whether temperature parameters could predict the timing of recruitment, the duration of recruitment and total recruitment in 18 benthic epifaunal species using partial least squares regression (PLSR) and ordinary least squares regression. Additionally, we used a null model to test whether temperature parameters and inter-annual variation in those parameters affect the temporal niche overlap of these benthic species. We specifically examined the recruitment patterns of non-native species to help illustrate how shifts in phenology may help drive changes in the community composition. Results from the PLSR helped determine the most instructive regressors for univariate least-squares models. For many (14 of 18) of the species examined, recruitment patterns could be predicted by seasonal growing degree days. Additionally, communities at cooler sites exhibited greater temporal niche overlap than assemblages found at warmer sites. Finally, we observed a unique pattern among invasive species, with more recent invaders recruiting later in the season, which may be a result of shifts in niche overlap. The findings of this study illustrate potential mechanisms for species coexistence and increased rates of invasion resulting from climate change. C1 [Reinhardt, James F.] NOAA Restorat Ctr, Silver Spring, MD 20910 USA. [Whitlatch, Robert B.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Osman, Richard W.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reinhardt, JF (reprint author), NOAA Restorat Ctr, 1315 East West Hwy, Silver Spring, MD 20910 USA. EM jamesfreinhardt@hotmail.com OI Reinhardt, James/0000-0003-4707-4026 FU U.S. EPA STAR; NSF; Long Island Sound Study FX This research was partially supported by U.S. EPA STAR and NSF grants awarded to R.B.W. and R.W.O. J.F.R. was supported by a fellowship from the Long Island Sound Study for a portion of this work. Thanks to J. Carlton, R. Colwell, D. Avery and M. Whitney for helpful information and suggestions. Many thanks to the individuals who helped collect recruitment data and the anonymous reviewer. NR 39 TC 2 Z9 2 U1 1 U2 23 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2013 VL 489 BP 61 EP 74 DI 10.3354/meps10423 PG 14 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 211WA UT WOS:000323941000005 ER PT J AU Deck, J Barker, K Beaman, R Buttigieg, PL Droge, G Guralnick, R Miller, C Tuama, EO Murrell, Z Parr, C Robbins, B Schigel, D Stucky, B Walls, R Wieczorek, J Morrison, N Wooley, J AF Deck, John Barker, Katharine Beaman, Reed Buttigieg, Pier Luigi Droege, Gabriele Guralnick, Robert Miller, Chuck Tuama, Eamonn O. Murrell, Zack Parr, Cynthia Robbins, Bob Schigel, Dmitry Stucky, Brian Walls, Ramona Wieczorek, John Morrison, Norman Wooley, John TI Clarifying Concepts and Terms in Biodiversity Informatics SO STANDARDS IN GENOMIC SCIENCES LA English DT Article C1 [Deck, John; Wieczorek, John] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Barker, Katharine; Parr, Cynthia] Smithsonian Inst, Washington, DC 20560 USA. [Beaman, Reed] Univ Florida, Gainesville, FL USA. [Buttigieg, Pier Luigi] Alfred Wegener Inst, Helmholtz Ctr Polar & Marine Res, Bremen, Germany. [Droege, Gabriele] Free Univ Berlin, Berlin, Germany. [Guralnick, Robert; Stucky, Brian] Univ Colorado, Boulder, CO 80309 USA. [Miller, Chuck] Missouri Bot Garden, St Louis, MO 63166 USA. [Tuama, Eamonn O.] GBIF Secretariat, Global Biodivers Informat Facil, Copenhagen, Denmark. [Murrell, Zack] Appalachian State Univ, Boone, NC 28608 USA. [Robbins, Bob; Wooley, John] Univ Calif San Diego, La Jolla, CA 92093 USA. [Schigel, Dmitry] Univ Helsinki, Metapopulat Res Grp, FIN-00014 Helsinki, Finland. [Schigel, Dmitry] Univ Helsinki, Finnish Museum Nat Hist, FIN-00014 Helsinki, Finland. [Walls, Ramona] Univ Arizona, Iplant Collaborat, Tucson, AZ USA. [Morrison, Norman] Univ Manchester, Sch Comp Sci, Manchester, Lancs, England. RP Deck, J (reprint author), Univ Calif Berkeley, Berkeley, CA 94720 USA. OI Schigel, Dmitry/0000-0002-2919-1168; Buttigieg, Pier Luigi/0000-0002-4366-3088 NR 6 TC 4 Z9 4 U1 2 U2 8 PU GENOMIC STAND CONSORT PI EAST LANSING PA MICHIGAN STATE UNIV, GEEO GARRITY, DEPT MICROBIOL, 6162 BIOMED & PHYS SCI BLDG, EAST LANSING, MI 48824 USA SN 1944-3277 J9 STAND GENOMIC SCI JI Stand. Genomic Sci. PY 2013 VL 8 IS 2 BP 352 EP 359 DI 10.4056/sigs.3907833 PG 8 WC Genetics & Heredity; Microbiology SC Genetics & Heredity; Microbiology GA 203XC UT WOS:000323326900016 PM 23991264 ER PT J AU Stoev, P Penev, L Akkari, N Cheung, DKB Enghoff, H Brunke, A de Souza, CM Pape, T Mietchen, D Erwin, T AF Stoev, Pavel Penev, Lyubomir Akkari, Nesrine Cheung, David Koon-Bong Enghoff, Henrik Brunke, Adam de Souza, Carina Mara Pape, Thomas Mietchen, Daniel Erwin, Terry TI Revolving images and multi-image keys open new horizons in descriptive taxonomy: ZooKeys working examples SO ZOOKEYS LA English DT Editorial Material ID INTERACTIVE KEY C1 [Stoev, Pavel] Bulgarian Acad Sci, Natl Museum Nat Hist, Sofia 1700, Bulgaria. [Stoev, Pavel; Penev, Lyubomir; Mietchen, Daniel] Pensoft Publishers, Sofia 1700, Bulgaria. [Penev, Lyubomir] Bulgarian Acad Sci, Inst Biodivers & Ecosyst Res, Sofia 1700, Bulgaria. [Akkari, Nesrine; Cheung, David Koon-Bong; Enghoff, Henrik; Brunke, Adam; Pape, Thomas] Univ Copenhagen, Zool Museum, Nat Hist Museum Denmark, DK-2100 Copenhagen, Denmark. [de Souza, Carina Mara] Univ Estadual Campinas, UNICAMP, Inst Biol, Dept Anim Biol, BR-13083970 Campinas, SP, Brazil. [Mietchen, Daniel] Leibniz Inst Evolut & Biodiversitatsforsch, Museum Naturkunde, D-10115 Berlin, Germany. [Erwin, Terry] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Stoev, P (reprint author), Bulgarian Acad Sci, Natl Museum Nat Hist, 12 Prof Georgi Zlatarski St, Sofia 1700, Bulgaria. EM pavel.e.stoev@gmail.com RI Pape, Thomas/E-7520-2011; Enghoff, Henrik/A-5796-2013; OI Pape, Thomas/0000-0001-6609-0609; Stoev, Pavel/0000-0002-5702-5677; Mietchen, Daniel/0000-0001-9488-1870 NR 10 TC 1 Z9 1 U1 0 U2 7 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 328 BP 1 EP 3 DI 10.3897/zookeys.328.6171 PG 3 WC Zoology SC Zoology GA 211EG UT WOS:000323887100001 PM 24146545 ER PT B AU Asgari-Targhi, M van Ballegooijen, AA AF Asgari-Targhi, M. van Ballegooijen, A. A. BE Pugliese, G DeKoter, A Wijburg, M TI Alfven Waves and the Heating of Solar Coronal Loops SO 370 YEARS OF ASTRONOMY IN UTRECHT SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT International Conference on 370 Years of Astronomy in Utrecht CY APR 02-05, 2012 CL Noordwijkerhout, NETHERLANDS SP Netherlands Res Sch Astron, Space Res Org Netherlands, Leidsch Kerkhoven Bosscha Fdn, Utrecht Univ, Dept Phys ID WIND; TURBULENCE AB We construct a 3D magnetic model for the dissipation and propagation of Alfven waves in a coronal loop. The waves are assumed to be generated by foot-point motions inside the kilogauss magnetic flux elements at the two ends of the loop. Counter propagating waves are subject to non-linear interactions that lead to turbulent decay of the waves and heating of the chromospheric and coronal plasma. We find that hot coronal loops typically found in active region and the underlying chromosphere can be explained by Alfven wave turbulence. C1 [Asgari-Targhi, M.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS-15, Cambridge, MA 02138 USA. EM asgari@head.cfa.harvard.edu; vanballe@cfa.harvard.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-824-4 J9 ASTR SOC P PY 2013 VL 470 BP 77 EP 82 PG 6 WC Astronomy & Astrophysics; History & Philosophy Of Science SC Astronomy & Astrophysics; History & Philosophy of Science GA BGL97 UT WOS:000323460400008 ER PT J AU Vilhelmsen, L Blank, SM Costa, VA Alvarenga, TM Smith, DR AF Vilhelmsen, Lars Blank, Stephan M. Costa, Valmir A. Alvarenga, Thiago M. Smith, David R. TI Phylogeny of the ophrynopine clade revisited: review of the parasitoid sawfly genera Ophrella Middlekauff, Ophrynopus Konow and Stirocorsia Konow (Hymenoptera:Orussidae) SO INVERTEBRATE SYSTEMATICS LA English DT Article ID ORUSSIDAE INSECTA; SYMPHYTA; XIPHYDRIIDAE; GENUS; WASP AB The rare family Orussidae comprises the only parasitoid sawflies and are sister to the Apocrita, the latter comprising most of Hymenoptera. Because of this, their morphology and relationships have been particularly important for interpreting the morphology of and biological transitions within the order as a whole. Within the Orussidae the ophrynopines are a comparatively diverse clade with a predominantly southern hemisphere distribution. Here, a revised and expanded morphological dataset incorporating several new taxa is used to test ophrynopine relationships and provide further insights into their evolutionary history. The analyses largely corroborate previous results. The distribution pattern and the fossil record indicate that the ophrynopines radiated in the early Cenozoic in the Australasian-Oceanian and the Neotropic regions and later dispersed into the Nearctic, Eastern Palaearctic and Indomalayan regions. The South American genus Ophrella Middlekauff, 1985 is well supported as a monophyletic genus, whereas Ophrynopus Konow, 1897 is paraphyletic with respect to Stirocorsia Konow, 1897. Three new species, Ophrella eldorado Vilhelmsen, sp. nov., Ophrynopus guarani Blank, D. R. Smith & Vilhelmsen, sp. nov., and Ophrynopus rupestris Vilhelmsen, Costa & Alvarenga, sp. nov. are described. Ophrella lingulata Middlekauff, 1985 is treated as a junior synonym of Ophrella amazonica (Westwood, 1874). Stirocorsia is treated as a junior synonym of Ophrynopus. The species Ophrynopus apicalis (Togashi, 2000), Ophrynopus kohli (Konow, 1897), Ophrynopus maculipennis (F. Smith, 1859) and Ophrynopus tosensis (Tosawa & Sugihara, 1934), formerly in Stirocorsia, are transferred to Ophrynopus. Revised keys to the species of Ophrella, Ophrynopus and the genera in the ophrynopine clade are provided. In addition, Orussidae are recorded from Bolivia and French Guiana for the first time. C1 [Vilhelmsen, Lars] Nat Hist Museum Denmark, DK-2100 Copenhagen, Denmark. [Blank, Stephan M.] Senckenberg Deutsch Entomol Inst, D-15374 Muncheberg, Germany. [Costa, Valmir A.] Inst Biol, Lab Controle Biol, BR-13012970 Campinas, SP, Brazil. [Alvarenga, Thiago M.] Univ Estadual Campinas, Programa Posgrad Biol Anim Inst Biol, BR-13083970 Campinas, SP, Brazil. [Smith, David R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Vilhelmsen, L (reprint author), Nat Hist Museum Denmark, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM lbvilhelmsen@snm.ku.dk RI Vilhelmsen, Lars/A-3396-2013; Costa, Valmir/N-6371-2013 OI Vilhelmsen, Lars/0000-0002-5593-5722; Costa, Valmir/0000-0003-0122-3567 NR 28 TC 5 Z9 5 U1 1 U2 9 PU CSIRO PUBLISHING PI CLAYTON PA UNIPARK, BLDG 1, LEVEL 1, 195 WELLINGTON RD, LOCKED BAG 10, CLAYTON, VIC 3168, AUSTRALIA SN 1445-5226 EI 1447-2600 J9 INVERTEBR SYST JI Invertebr. Syst. PY 2013 VL 27 IS 4 BP 450 EP 483 DI 10.1071/IS13006 PG 34 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA 208ZK UT WOS:000323721900006 ER PT J AU Talamas, EJ Masner, L Johnson, NF AF Talamas, Elijah J. Masner, Lubomir Johnson, Norman F. TI Systematics of Trichoteleia Kieffer and Paridris Kieffer (Hymenoptera, Platygastroidea, Platygastridae) SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Egg-parasitoid; Platygastroidea; key; Paridris; Trichoteleia; revision; phylogeny ID SEQUENCE ALIGNMENT; RIBOSOMAL-RNA; GENUS; SCELIONIDAE; PHYLOGENY; REVISION; 28S AB Paridris Kieffer and Trichoteleia Kieffer are morphologically similar genera of solitary egg parasitoids with little overlap between their distributions: Paridris is found commonly worldwide with the exceptions of Madagascar, from which a single specimen is known, and New Zealand, from which no records are known; Trichoteleia is endemic to the Malagasy islands. Here we present the first phylogenetic analysis of platygastroid wasps that combines and compares morphological and molecular data. We find the results of the phylogenetic analyses of the two data sources to be largely congruent for the species treated here. Paridris and Trichoteleia are found to be monophyletic, as are two morphologically well-defined species groups within Paridris. Neoparidris Galloway is found to belong within Paridris and is treated as a junior synonym, syn. n. The faunas of Paridris from Africa, Melanesia and the Indo-Malay islands are revised. Fifteen species are described of which 9 are new: Paridris anikulapo Talamas, sp. n. (sub-Saharan Africa); Paridris densiclava (Kieffer), (Seychelles); Paridris bispinosa (Masner), (Gabon); Paridris nigriclava (Kieffer), (Seychelles); Paridris nitidiceps (Kieffer), (Seychelles); Paridris tenuis (Nixon), (sub-Saharan Africa); Paridris trispinosa Talamas & Masner, sp. n., (Cameroon, Democratic Republic of the Congo); Paridris bifurcata (Dodd), comb. n., (Australia, Papua New Guinea); Paridris mnestros Talamas & Masner, sp. n., (Indonesia, Malaysia); Paridris pantex Talamas, sp. n., (Fiji); Paridris phrikos Talamas & Masner, sp. n., (Fiji); Paridris skolops Talamas & Masner, sp. n., (Fiji); Paridris sulcata Talamas, sp. n., (Vanuatu); Paridris taekuli Talamas & Masner, sp. n., (Australia, Bangladesh, Fiji, India, Indonesia, Ivory Coast, Madagascar, New Caledonia, Thailand, Vietnam); Paridris xestos Talamas & Masner, sp. n., (Fiji). Paridris flaviclava (Kieffer), syn. n., and P. nigraticeps (Kieffer), syn. n., are treated as junior synonyms of P. nigriclava. C1 [Talamas, Elijah J.] Smithsonian Inst, USNM, USDA ARS, Systemat Entomol Lab, Washington, DC 20560 USA. [Masner, Lubomir] Agr & Agri Food Canada, Ottawa, ON K1A 0C6, Canada. [Johnson, Norman F.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43212 USA. RP Talamas, EJ (reprint author), Smithsonian Inst, USNM, USDA ARS, Systemat Entomol Lab, Washington, DC 20560 USA. EM elijah.talamas@ars.usda.gov FU NSF [DEB-0542864]; National Science Foundation [DEB-0614764] FX Thanks to K. van Achterberg, M. Buffington, R. Danielsson, T. Nuhn, S. van Noort, and M. Sharkey (Thai specimens collected under NSF grant No. DEB-0542864) for the loans of material for this study, to A. Polaszek and V. Blagoderov for help with imaging type material at BMNH, and to L. Musetti, J. Cora, and S. Hemly for critical assistance with specimen handling, software and databasing. This material is based upon work supported in part by the National Science Foundation under grant No. DEB-0614764 to N.F. Johnson and A.D.Austin. NR 35 TC 3 Z9 4 U1 0 U2 3 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2013 VL 34 BP 1 EP 79 DI 10.3897/JHR.33.4714 PG 79 WC Entomology SC Entomology GA 209ZQ UT WOS:000323799500001 ER PT J AU Kula, RR AF Kula, Robert R. TI A new brachypterous species of Heterospilus Haliday (Braconidae, Doryctinae) from the Neotropical Region SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Apterous; aptery; brachyptery; Neotropical; parasitoid; taxonomy AB A new species, Heterospilus michaeli Kula, from the Neotropical Region is described and differentiated from all other New World species of Doryctinae with brachypterous or apterous individuals. It is the first species of Heterospilus Haliday in the Neotropical Region known to exhibit brachyptery and the fourth described brachypterous species of Heterospilus worldwide. Errors and omissions in a recently published article on brachypterous and apterous doryctines in the New World are corrected. C1 ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Kula, RR (reprint author), ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov NR 7 TC 1 Z9 1 U1 0 U2 1 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2013 VL 33 BP 83 EP 90 DI 10.3897/JHR.33.4009 PG 8 WC Entomology SC Entomology GA 207GQ UT WOS:000323587300004 ER PT J AU Talamas, EJ Buffington, M Hoelmer, K AF Talamas, Elijah J. Buffington, Matthew Hoelmer, Kim TI New synonymy of Trissolcus halyomorphae Yang SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Halyomorpha halys; Trissolcus japonicus; Trissolcus halyomorphae; brown marmorated stink bug ID SCELIONIDAE; HYMENOPTERA; PENTATOMIDAE; HETEROPTERA AB Trissolcus halyomorphae Yang syn. n. is treated as a junior synonym following examination of the holotype of T japonicus (Ashmead). C1 [Talamas, Elijah J.; Buffington, Matthew] ARS, Systemat Entomol Lab, USDA, NMNH,Smithsonian Inst, Washington, DC USA. [Hoelmer, Kim] ARS, Beneficial Insects Intro Res Unit, USDA, Newark, DE USA. RP Talamas, EJ (reprint author), ARS, Systemat Entomol Lab, USDA, NMNH,Smithsonian Inst, Washington, DC USA. EM talamas.1@osu.edu NR 18 TC 12 Z9 14 U1 0 U2 19 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1070-9428 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2013 VL 33 BP 113 EP 117 DI 10.3897/JHR.33.5627 PG 5 WC Entomology SC Entomology GA 207GQ UT WOS:000323587300007 ER PT B AU Latham, DW Buchhave, LA AF Latham, David W. Buchhave, Lars A. CA Kepler Team BE Chavez, M Bertone, E Vega, O DeLaLuz, V TI Small Planets Do Not Require a Metal-Rich Environment SO NEW QUESTS IN STELLAR ASTROPHYSICS III: A PANCHROMATIC VIEW OF SOLAR-LIKE STARS, WITH AND WITHOUT PLANETS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 3rd International Conference on New Quests in Stellar Astrophysics: A Panchromatic View of Solar-like Stars With and Without Planets CY MAR 12-16, 2012 CL Puerto Vallarta, MEXICO SP INAOE, Univ Guadalajara AB The abundance of heavy elements in the photospheres of planet-hosting stars similar to the Sun may provide a record of the chemical composition of their initial protoplanetary discs. Several studies have shown that metal-rich stars are much more likely to harbor gas giant planets, thereby supporting the core accretion scenario for giant planet formation. The large sample of transiting planets smaller than Neptune identified by the Kepler mission provides a first opportunity to probe the metallicities of a statistically significant number of stars with small planets. We have derived spectroscopic metallicities for 152 stars hosting 226 planet candidates discovered by Kepler and find that, in contrast to the preference for gas giants to be found around metal-rich stars, the detection of planets smaller than Neptune does not depend as strongly on the metallicity of the host star. Planets smaller than 4 Earth radii are found around host stars with a wide range of metallicities. C1 [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dlatham@cfa.harvard.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-828-2 J9 ASTR SOC P PY 2013 VL 472 BP 91 EP 96 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BGO40 UT WOS:000323627300014 ER PT J AU Sekerka, L Windsor, D Staines, CL AF Sekerka, Lukas Windsor, Donald Staines, Charles L. TI A new species of Cephaloleia from Panama with description of larva and first record of orchid-feeding in Cephaloleiini (Coleoptera: Chrysomelidae: Cassidinae) SO ACTA ENTOMOLOGICA MUSEI NATIONALIS PRAGAE LA English DT Article DE Coleoptera; Chrysomelidae; entomology; taxonomy; new species; host plant; Orchideaceae; Panama; Neotropical Region AB Cephaloleia orchideivora sp. nov. is described and figured from Panama including larva, host plants and biology. This is the first Cephaloleia species known to be associated with Orchideaceae. C1 [Sekerka, Lukas] Univ South Bohemia, Fac Sci, Dept Zool, CZ-37005 Ceske Budejovice, Czech Republic. [Windsor, Donald] Smithsonian Trop Res Inst, Panama City, Panama. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Sekerka, L (reprint author), Univ South Bohemia, Fac Sci, Dept Zool, Branisovska 31, CZ-37005 Ceske Budejovice, Czech Republic. EM sagrinae@seznam.cz; windsord@si.edu; stainesc@si.edu FU University of South Bohemia [04-135/2010/P] FX We thank Panama's ministry of the environment (ANAM) for collecting (SE/AP-7-10) and export (SEX/AP-2-09) permission; to STRI for support in conducting field research. We also thank K. Silvera (STRI, Panama) for identification of the host plants; Duane McKenna (University of Memphis, USA) for photos of the C. irregularis holotype; and reviewers Lech Borowiec and Carlos Garcia-Robledo for valuable comments improving the manuscript. The paper was supported by the grant no. 04-135/2010/P of the University of South Bohemia. NR 13 TC 4 Z9 4 U1 2 U2 4 PU NARODNI MUZEUM - PRIRODOVEDECKE MUZEUM PI PRAHA PA KUNRATICE, PRAHA, CZ-148 00, CZECH REPUBLIC SN 0374-1036 EI 1804-6487 J9 ACTA ENT MUS NAT PRA JI Acta Entomol. Mus. Natl. Pragae PY 2013 VL 53 IS 1 BP 303 EP 314 PG 12 WC Entomology SC Entomology GA 202RV UT WOS:000323238200019 ER PT J AU Azar, D Engel, MS Jarzembowski, E Krogmann, L Nel, A Santiago-Blay, J AF Azar, Dany Engel, Michael S. Jarzembowski, Edmund Krogmann, Lars Nel, Andre Santiago-Blay, Jorge TI Insect Evolution in an Amberiferous and Stone Alphabet Introduction SO INSECT SYSTEMATICS & EVOLUTION LA English DT Editorial Material C1 [Azar, Dany] Lebanese Univ, Fac Sci 2, Dept Nat Sci, Fanar Matn, Lebanon. [Engel, Michael S.] Univ Kansas, Nat Hist Museum, Div Entomol, Lawrence, KS 66045 USA. [Engel, Michael S.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Jarzembowski, Edmund] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, Key State Lab Palaeobiol & Stratig, Nanjing 210008, Jiangsu, Peoples R China. [Krogmann, Lars] State Museum Nat Hist Stuttgart, D-70191 Stuttgart, Germany. [Nel, Andre] Museum Natl Hist Nat, CNRS, UMR 7205, F-75231 Paris, France. [Santiago-Blay, Jorge] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Azar, D (reprint author), Lebanese Univ, Fac Sci 2, Dept Nat Sci, POB 26110217, Fanar Matn, Lebanon. EM azar@mann.fr; lars.krogmann@smns-bw.de RI Engel, Michael/C-5461-2012 OI Engel, Michael/0000-0003-3067-077X NR 0 TC 3 Z9 3 U1 0 U2 3 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 1399-560X J9 INSECT SYST EVOL JI Insect Syst. Evol. PY 2013 VL 44 IS 2 BP 111 EP 115 DI 10.1163/1876312X-44022102 PG 5 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 204VB UT WOS:000323398300001 ER PT J AU Morrow, KM Liles, MR Paul, VJ Moss, AG Chadwick, NE AF Morrow, Kathleen M. Liles, Mark R. Paul, Valerie J. Moss, Anthony G. Chadwick, Nanette E. TI Bacterial shifts associated with coral-macroalgal competition in the Caribbean Sea SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Montastraea faveolata; Porites astreoides; Macroalgae; Microbial community; Allelopathy; Benthic survey; Halimeda; Dictyota ID REEF-BUILDING CORAL; 16S RIBOSOMAL-RNA; MICROBIAL ASSOCIATIONS; METAGENOMIC ANALYSIS; OCEAN ACIDIFICATION; PORITES-ASTREOIDES; ORGANIC-CARBON; DICTYOTA SPP.; FLORIDA-KEYS; DIVERSITY AB Present-day coral reefs are impacted by frequent disturbance and increasing global stressors, which provide an environment that supports the growth of alternative dominants, such as macroalgae, sponges, and tunicates, rather than stony corals. Competitively damaging inter actions arise between macroalgae and reef-building corals that can involve chemical, physical, and microbial mechanisms. Using 16S rRNA denaturing gradient gel electrophoresis (DGGE), amplicon sequencing, and multivariate analyses, we examined coral-and algae-associated bacterial assemblages along interaction gradients between the common Caribbean stony corals Montastraea faveolata and Porites astreoides and the benthic macroalgae Halimeda opuntia and Dictyota menstrualis. Benthic surveys were conducted in 3 Caribbean locations, and interactions were sampled for bacterial analyses. Both macroalgae were capable of inducing shifts in coral-associated bacteria to an assemblage that more closely resembled macroalgal-associated bacteria. Overall, M. faveolata-associated bacteria were more significantly affected by macroalgal competitors than were P. astreoides-associated bacteria at all sites. Bacteria associated with M. faveolata corals changed during >83% of interactions, even when samples were taken 5 cm away from competing macroalgae. Detectable shifts in coral-associated bacteria at all sampling sites suggest that macroalgae play a large role in coral holobiont health. The degree to which coral species maintain stable microbial assemblages in the face of environmental fluctuations and competitive stress may indicate specific species and coral reefs that have the capacity to resist perturbations and those that may need additional protection in the future. C1 [Morrow, Kathleen M.; Liles, Mark R.; Moss, Anthony G.; Chadwick, Nanette E.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Morrow, Kathleen M.] Australian Inst Marine Sci, Townsville MC, Townsville, Qld 4810, Australia. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Morrow, KM (reprint author), Auburn Univ, Dept Biol Sci, 101 Rouse Life Sci Bldg, Auburn, AL 36849 USA. EM morrow.kathleen@gmail.com FU National Oceanic and Atmospheric Administration National Marine Sanctuary Program Nancy Foster Scholarship; Puerto Rico Sea Grant [R-101-1-08]; NSF-EPSCoR [EPS0447675]; Smithsonian Caribbean Coral Reef Ecosystems Program; Hunterdon Oceanographic Fund; [NSF-MCB034827] FX We thank the Florida Keys National Marine Sanctuary for granting collection and research permits (FKNMS- 2008-019) and the Belize Fisheries Department for permits to collect coral mucus samples. The Mote Marine Laboratory, University of the Virgin Islands MacLean Marine Science Center, the Smithsonian Marine Station at Fort Pierce, and the Smithsonian's Carrie Bow Cay Field Station all provided invaluable logistical support. We are grateful to G. Cook, N. Fogarty, L. Huebner, A. Isbell, M. Nelsen, M. Newman, R. Ritson-Williams, J. Voss, and A. Wilson for editorial, field, and laboratory assistance. Particular thanks go to S. Donahue and Dr. B. Keller for their support during survey data collection aboard the NOAA RV 'Nancy Foster'. This work was supported by a National Oceanic and Atmospheric Administration National Marine Sanctuary Program Nancy Foster Scholarship (K. M. M.), a Puerto Rico Sea Grant R-101-1-08 (N.E.C.), NSF-MCB034827 (A. G. M.), NSF-EPSCoR EPS0447675 (Auburn University CECST Program - Cell and Environmental Signaling and Transduction Program), and the Smithsonian Caribbean Coral Reef Ecosystems Program and Hunterdon Oceanographic Fund. This research was completed in partial fulfillment of requirements for the PhD degree in Biological Sciences by K. M. M. and is contribution 108 of the Marine Biology Program at Auburn University, Auburn, AL, and 920 of the Smithsonian Caribbean Coral Reef Ecosystems Program. NR 91 TC 8 Z9 8 U1 7 U2 44 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2013 VL 488 BP 103 EP 117 DI 10.3354/meps10394 PG 15 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 202US UT WOS:000323245800009 ER PT J AU Helgen, KM Pinto, CM Kays, R Helgen, LE Tsuchiya, MTN Quinn, A Wilson, DE Maldonado, JE AF Helgen, Kristofer M. Pinto, C. Miguel Kays, Roland Helgen, Lauren E. Tsuchiya, Mirian T. N. Quinn, Aleta Wilson, Don E. Maldonado, Jesus E. TI Taxonomic revision of the olingos (Bassaricyon), with description of a new species, the Olinguito SO ZOOKEYS LA English DT Article DE Andes; Bassaricyon; biogeography; Neotropics; new species; olingo; Olinguito ID COMPLETE MITOCHONDRIAL GENOME; CENTRAL AMERICAN HERPETOFAUNA; CYTOCHROME-B GENE; ORDER CARNIVORA; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; BRAZILIAN AMAZON; NORTHERN ANDES; SOUTH-AMERICA; GEOGRAPHIC DISTRIBUTIONS AB We present the first comprehensive taxonomic revision and review the biology of the olingos, the endemic Neotropical procyonid genus Bassaricyon, based on most specimens available in museums, and with data derived from anatomy, morphometrics, mitochondrial and nuclear DNA, field observations, and geographic range modeling. Species of Bassaricyon are primarily forest-living, arboreal, nocturnal, frugivorous, and solitary, and have one young at a time. We demonstrate that four olingo species can be recognized, including a Central American species (B. gabbii), lowland species with eastern, cis-Andean (B. alleni) and western, trans-Andean (B. medius) distributions, and a species endemic to cloud forests in the Andes. The oldest evolutionary divergence in the genus is between this last species, endemic to the Andes of Colombia and Ecuador, and all other species, which occur in lower elevation habitats. Surprisingly, this Andean endemic species, which we call the Olinguito, has never been previously described; it represents a new species in the order Carnivora and is the smallest living member of the family Procyonidae. We report on the biology of this new species based on information from museum specimens, niche modeling, and fieldwork in western Ecuador, and describe four Olinguito subspecies based on morphological distinctions across different regions of the Northern Andes. C1 [Helgen, Kristofer M.; Helgen, Lauren E.; Tsuchiya, Mirian T. N.; Quinn, Aleta; Wilson, Don E.; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Pinto, C. Miguel] Pontifica Univ Catol Ecuador, Escuela Ciencias Biol, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. [Pinto, C. Miguel] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Pinto, C. Miguel] Amer Museum Nat Hist, Sackler Inst Comparat Gen, New York, NY 10024 USA. [Pinto, C. Miguel] CUNY, Grad Ctr, New York, NY 10016 USA. [Pinto, C. Miguel] Texas Tech Univ, Dept Biol Sci & Museum, Lubbock, TX 79409 USA. [Kays, Roland] North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. [Kays, Roland] N Carolina State Univ, Fisheries Wildlife & Conservat Program, Raleigh, NC 27695 USA. [Kays, Roland] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Tsuchiya, Mirian T. N.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Tsuchiya, Mirian T. N.; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Quinn, Aleta; Maldonado, Jesus E.] Univ Pittsburgh, Dept Hist & Philosophy Sci, Pittsburgh, PA 15260 USA. RP Helgen, KM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, NHB 390,MRC 108,POB 37012, Washington, DC 20013 USA. EM helgenk@si.edu FU Smithsonian Institution; Texas Tech University Association of Biologists FX For assistance in Ecuador we thank E. Tapia, C. Tapia, G. Onore, P. Asimbaya, L. Velasquez, P. Rosero, M. Grijalva, G. Acosta, P. Pinto, M. Gallo, A. Padilla, M. Vargas, P. Vargas, I. Rodriguez, C. Byrne, and Fundacion Otonga. For access to specimens under their care, loan of tissues, and other assistance during museum visits we are grateful to D. Lunde, E. Westwig, R. Voss, W. Stanley, B. Patterson, L. Heaney, R. Banasiak, S. Burneo, R. Timm, J. Patton, C. Conroy, M. Engstrom, B. Lim, J. Eger, P. Jenkins, R. Portela Miguez, D. Hills, J. Chupasko, N. Gilmore, J. Dines, J. Light, W. Murphy, R. Asher, I. Thomas, L. Albuja-V., O. Groenwall, R. Anderson, E. Sargis, K. Zyskowski, P. Myers, S. Jansa, R. Baker, K. Koepfli, R. Fleischer, R. Arcos, C. Handley, Jr., L. Gordon, and H. Kafka. For assistance in the registrar's office at the National Zoo, we thank L. Morse. For helpful reviews, helpful discussion, and other assistance, we thank W. Bogdanowicz, B. Patterson, R. Sampaio, E. Gutierrez, G. Slater, K. Koepfli, R. Anderson, I. Poglayen-Neuwall, J. Gibbons, P. Engelbrektsson, F. Reid, J. Pino, R. Samudio, M. Bass, T. Flannery, E. Eizirik, R. Baker, H. Mantilla, R. Ree, R. Voss, and L. Emmons. This work was partially funded by the Smithsonian Institution. M. P. was supported in part by a grant from the Texas Tech University Association of Biologists. We thank Nancy Halliday for original artwork. For photographic contributions we thank P. Asimbaya and L. Velasquez of Finding Species, and M. Gurney, I. Poglayen-Neuwall, T. Gregory (Smithsonian Conservation Biology Institute), C. Aguilar, G. Basco, M. Guerra, R. Banasiak, R. Bornholdt, and S. Burke. NR 297 TC 25 Z9 31 U1 7 U2 82 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 324 SI SI BP 1 EP 83 DI 10.3897/zookeys.324.5827 PG 83 WC Zoology SC Zoology GA 203RB UT WOS:000323309500001 PM 24003317 ER PT S AU Trifonov, AS Jaskula, JC Teulon, C Glenn, DR Bar-Gill, N Walsworth, RL AF Trifonov, Alexei S. Jaskula, Jean-Christophe Teulon, Claire Glenn, David R. Bar-Gill, Nir Walsworth, Ronald L. BE Arimondo, E Berman, PR Lin, CC TI Limits to Resolution of CW STED Microscopy SO ADVANCES IN ATOMIC, MOLECULAR, AND OPTICAL PHYSICS, VOL 62 SE Advances In Atomic Molecular and Optical Physics LA English DT Review; Book Chapter ID NITROGEN-VACANCY CENTERS; FLUORESCENCE MICROSCOPY; DEPLETION MICROSCOPY; NANOSCALE RESOLUTION; STIMULATED-EMISSION; DIAMOND AB We report a systematic theoretical and experimental study of the limits to spatial resolution for stimulated emission depletion (STED) superresolution fluorescence microscopy using continuous wave (CVV) laser beams. We develop a theoretical framework for CW STED imaging from point fluorescent emitters and calculate the dependence of 2D spatial resolution on the power of the CW excitation (pump) beam, as well as the power, contrast, and polarization of the CW STED "doughnut" beam. We perform CW STED experiments on (non-bleaching) nitrogen vacancy (NV) color centers in diamond and find good agreement with the theoretical expressions for CW STED spatial resolution. Our results will aid the optimization and application of CW STED microscopy in both the physical and life sciences. C1 [Trifonov, Alexei S.; Teulon, Claire; Bar-Gill, Nir; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Trifonov, Alexei S.; Jaskula, Jean-Christophe; Glenn, David R.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Trifonov, Alexei S.] RAS, Ioffe Phys Tech Inst, St Petersburg, Russia. RP Trifonov, AS (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. NR 18 TC 2 Z9 2 U1 4 U2 39 PU ELSEVIER ACADEMIC PRESS INC PI SAN DIEGO PA 525 B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-250X BN 978-0-12-408090-4 J9 ADV ATOM MOL OPT PHY JI Adv. Atom. Mol. Opt. Phys. PY 2013 VL 62 BP 279 EP 302 DI 10.1016/B978-0-12-408090-4.00005-0 PG 24 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA BGI23 UT WOS:000323088400006 ER PT J AU Ballentine, B Gkoo, KW Greenberg, R AF Ballentine, Barbara Gkoo, Kun Woo Greenberg, Russell TI Mechanisms of song divergence between swamp sparrow subspecies SO BEHAVIOUR LA English DT Article DE song; birds; speciation; vocal performance; swamp sparrow ID MALE BIRD SONG; DARWINS FINCHES; MELOSPIZA-GEORGIANA; MORPHOLOGICAL ADAPTATION; INTRASPECIFIC VARIATION; REPRODUCTIVE ISOLATION; VOCAL PERFORMANCE; SEXUAL SELECTION; FEMALE RESPONSE; TIDAL MARSHES AB Speciation is promoted when traits under divergent selection also contribute to non-random mating. For example, divergent selection on bill morphology in birds can influence song because of the role of bills in song production (ecomorphological constraints). Since song is used by females to find appropriate mates, divergent selection on bills through its impact on song can promote non-random mating. However, because song in songbirds is learned, divergence in song between populations could be the result of cultural influences (cultural evolution). In this study, we use an experimental approach to address the relative influence of ecomorphological constraints and culture on song divergence in swamp sparrow subspecies (Melospiza georgiana). As with other songbirds, swamp sparrows are subject to cultural influences that may explain differences in song between subspecies (cultural evolution). However, ecological conditions promote larger bill size in the coastal subspecies of swamp sparrows rendering males unable to perform the broad-band, rapid songs that inland females prefer potentially contributing to non-random mating between subspecies. To determine the impact of ecomorphological constraints on song learning, we trained hand-raised swamp sparrows from divergent populations with an identical set of tutor songs from a foreign inland population. Males from both populations learned species typical songs. We found that inland males produced learned songs with better vocal performance than coastal males suggesting that observed differences in specific features of song are influenced more by morphological constraints than cultural drift. Further, we found that inland males reproduced tutor songs more accurately than coastal males suggesting that coastal males tried but were less able to accurately reproduce physically challenging songs. These results support the current model for how motor constraints influence song production and may demonstrate a mechanism by which natural selection can influence signal evolution and population divergence through divergent selection on bills. C1 [Ballentine, Barbara; Gkoo, Kun Woo] Univ West Georgia, Dept Biol, Carrollton, GA USA. [Ballentine, Barbara; Greenberg, Russell] Smithsonian Migratory Bird Ctr, Washington, DC USA. RP Ballentine, B (reprint author), Univ West Georgia, Dept Biol, Carrollton, GA USA. EM bballent@westga.edu FU Smithsonian National Zoo; University of West Georgia FX We thank the Smithsonian National Zoo and the University of West Georgia for providing funding and logistical support during this project. We thank Susan Peters and the Smithsonian National Zoo nutritional staff and veterinarians for advice on hand rearing techniques. We thank the National Zoo volunteer program for coordinating volunteers to help with swamp sparrow hand rearing. We especially thank all the volunteers who so generously donated their time, energy and commitment to care for the captive population of swamp sparrows. We thank two anonymous reviewers for helpful comments that improved the quality of this manuscript. We thank Marc Naguib and Jordan Price for inviting us to contribute our work to the symposium and special issue honoring R. Haven Wiley. Finally we gratefully acknowledge the influential work of R. Haven Wiley, a valued mentor, colleague and friend. NR 53 TC 2 Z9 2 U1 1 U2 33 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0005-7959 J9 BEHAVIOUR JI Behaviour PY 2013 VL 150 IS 9-10 SI SI BP 1165 EP 1181 DI 10.1163/1568539X-00003093 PG 17 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 195DD UT WOS:000322681600011 ER PT S AU Jaramillo, C Cardenas, A AF Jaramillo, Carlos Cardenas, Andres BE Jeanloz, R TI Global Warming and Neotropical Rainforests: A Historical Perspective SO ANNUAL REVIEW OF EARTH AND PLANETARY SCIENCES, VOL 41 SE Annual Review of Earth and Planetary Sciences LA English DT Review; Book Chapter DE evolution; tropic; temperature; speciation; climate change; biome ID SEA-SURFACE-TEMPERATURE; EOCENE THERMAL MAXIMUM; LATITUDINAL DIVERSITY GRADIENTS; GLASSY FORAMINIFERAL CALCITE; NORTHERN SOUTH-AMERICA; OCEANIC HEAT-TRANSPORT; PLANT DIVERSITY; LATE PALEOCENE; TROPICAL TREE; CERREJON FORMATION AB There is concern over the future of the tropical rainforest (TRF) in the face of global warming. Will TRFs collapse? The fossil record can inform us about that. Our compilation of 5,998 empirical estimates of temperature over the past 120 Ma indicates that tropics have warmed as much as 7 degrees C during both the mid-Cretaceous and the Paleogene. We analyzed the paleobotanical record of South America during the Paleogene and found that the TRF did not expand toward temperate latitudes during global warm events, even though temperatures were appropriate for doing so, suggesting that solar insolation can be a constraint on the distribution of the tropical biome. Rather, a novel biome, adapted to temperate latitudes with warm winters, developed south of the tropical zone. The TRF did not collapse during past warmings; on the contrary, its diversity increased. The increase in temperature seems to be a major driver in promoting diversity. C1 [Jaramillo, Carlos; Cardenas, Andres] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM jaramilloc@si.edu; alc1006@gmail.com NR 188 TC 11 Z9 11 U1 6 U2 45 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0897 USA SN 0084-6597 BN 978-0-8243-2041-6 J9 ANNU REV EARTH PL SC JI Annu. Rev. Earth Planet. Sci. PY 2013 VL 41 BP 741 EP + DI 10.1146/annurev-earth-042711-105403 PG 37 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BFX18 UT WOS:000321742600028 ER PT J AU Mannise, N Gonzalez, S Maldonado, JE Izquierdo, G Francescoli, G Cosse, M AF Mannise, N. Gonzalez, S. Maldonado, J. E. Izquierdo, G. Francescoli, G. Cosse, M. TI High levels of polymorphism found through cross-amplification of microsatellite loci in a Ctenomys pearsoni (Rodentia, Ctenomyidae) population SO GENETICS AND MOLECULAR RESEARCH LA English DT Article DE Subterranean rodents; Rodentia: Ctenomyidae; Caviomorpha; Nuclear short tandem repeats ID DEER OZOTOCEROS-BEZOARTICUS; GENUS CTENOMYS; TUCO-TUCOS; OCTODONTIDAE; URUGUAY; DIFFERENTIATION; SOLITARY; TALARUM AB Ctenomys pearsoni (Pearson's tuco-tuco) is a subterranean rodent native to Uruguay. We tested the amplification pattern of 12 microsatellite loci, designed for C. sociabilis and C. haigi in a C. pearsoni population. DNA extractions were made from hair samples, and PCR amplification products were run on an ABI 3100 microcapillary gel. Eight loci were selected to form a highly polymorphic panel that could be used to efficiently screen populations of this species. InDNA from 35 tuco-tucos, the mean polymorphic information content value was 0.6536 and the mean expected heterozygosity was 0.7166. Paternity non-exclusion probabilities for seven independent loci were NE-1P = 0.0766 and NE-2P = 0.0108, and combined non-exclusion P(ID) was 6.2 x 10(-7). This panel of microsatellite loci has sufficient power to make inferences regarding group structure, mating strategies and evolutionary relationships among populations. C1 [Mannise, N.; Gonzalez, S.; Cosse, M.] Univ Republica, Unidad Asociada Fac Ciencias, Inst Invest Biol Clemente Estable, Dept Genet, Montevideo, Uruguay. [Maldonado, J. E.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Maldonado, J. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Izquierdo, G.; Francescoli, G.] Univ Republica, Fac Ciencias, Inst Biol, Secc Etol, Montevideo, Uruguay. RP Cosse, M (reprint author), Univ Republica, Unidad Asociada Fac Ciencias, Inst Invest Biol Clemente Estable, Dept Genet, Montevideo, Uruguay. EM mcosse@iibce.edu.uy FU Comision Sectorial de Investigacion Cientifica (Universidad de la Republica, Uruguay) FX We thank Monica Rumbo, Noelia Zambra, Erika Grke, Yennifer Hernandez, Noelia Kandratavicius, Martin Petrella, Micaela Trimble, and Lorena Coelho for field support; Guillermo Maccio and workers at El Relincho, who kindly provided logistic assistance and housing during fieldwork; Ivanna Tomasco and the Laboratorio de Evolucion (Facultad de Ciencias, Universidad de la Republica, Uruguay) for help in obtaining primers, and Guillermo D'Elia and Matias Mora for their suggestions. Research supported by Comision Sectorial de Investigacion Cientifica (Universidad de la Republica, Uruguay). NR 23 TC 0 Z9 0 U1 1 U2 8 PU FUNPEC-EDITORA PI RIBEIRAO PRETO PA RUA FLORIANO PEIXOTO 2444, ALTO DA BOA VISTA, RIBEIRAO PRETO, SP 00000, BRAZIL SN 1676-5680 J9 GENET MOL RES JI Genet. Mol. Res. PY 2013 VL 12 IS 2 BP 887 EP 891 DI 10.4238/2013.April.2.5 PG 5 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA 159FI UT WOS:000320030100003 PM 23613235 ER PT S AU Launius, RD AF Launius, Roger D. BE Harlow, J TI An Unintended Consequence of the ICY: Eisenhower, Sputnik, and the Founding of NASA SO HISTORY OF ROCKETRY AND ASTRONAUTICS SE AAS History Series LA English DT Proceedings Paper CT 42nd History Symposium of the International-Academy-of-Astronautics CY SEP 29-OCT 03, 2008 CL Glasgow, SCOTLAND AB On 4 October 1957, the Soviet Union launched the first Earth-circling artificial satellite and the United States responded by taking numerous actions aimed at "remediating" a Cold War crisis. This included the establishment of a separate civilian space agency charged with the conduct of an official program of scientific and technological space exploration, consolidation of Department of Defense space activities, the passage of the National Defense Education Act, the creation of a Presidential Science Advisor, and a host of lesser actions. The politics of these changes is fascinating, and has been interpreted as an appropriate political response to a unique crisis situation. Interest groups, all for differing reasons, prodded national leaders to undertake large-scale efforts, something the president thought unnecessarily expensive and once set in place impossible to dismantle. But was the Sputnik crisis truly a crisis in any real sense? Was it made into one by interest groups who used it for their own ends? This chapter will trace briefly some of the major themes associated with the International Geophysical Year (IGY) and Sputnik and describe the political construction of the crisis as it emerged in 1957-1958. It will also discuss something about the transformation of federal science and technology that took place in response to this "crisis" and how it set in train a series of processes and policies that did not unravel until the end of the Cold War. C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. NR 80 TC 0 Z9 0 U1 0 U2 3 PU AMER ASTRONAUTICAL SOC PI SAN DIEGO PA PUBLICATIONS OFFICE PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0730-3564 BN 978-0-87703-590-9 J9 AAS HIST SER PY 2013 VL 39 BP 3 EP 24 PG 22 WC Engineering, Aerospace SC Engineering GA BFR69 UT WOS:000321076100001 ER PT S AU Launius, RD AF Launius, Roger D. BE Harlow, J TI Managing the Unmanageable: Apollo, Space Age Management, and American Social Problems SO HISTORY OF ROCKETRY AND ASTRONAUTICS SE AAS History Series LA English DT Proceedings Paper CT 42nd History Symposium of the International-Academy-of-Astronautics CY SEP 29-OCT 03, 2008 CL Glasgow, SCOTLAND AB There are numerous beliefs about the ability of the federal government to accomplish positive results in social transformations that have become a part of American culture using space program management practices. The most obvious of these is the now trite question, "If we can put a man on the Moon, why can't we ... ?" But in the middle part of the 1960s NASA Administrator James E. Webb asked this same question in a more concrete manner; if we can accomplish Apollo "why can't we do something for grandma with Medicare?" This perception led to efforts by Webb and others at NASA to export the management practices that enabled the successful lunar landing program toward solving the myriad of social problems taken up by the Lyndon B. Johnson presidential administration and its successors in the United States. The application of these ideas to city administration, public health, entitlement programs such as Social Security and Medicare, energy, and veteran's affairs offers a case study in seeking to control what ultimately proved uncontrollable. Webb's 1969 book, Space Age Management: The Large-Scale Approach, was based on a set of lectures at the McKinsey Foundation that for a time became the darling of the management community. It emphasized the authority of unelected experts to implement well-executed plans for managing any difficult task. It outlined a strategy for the application of systems management techniques to tackle virtually any challenge imaginable. The linkage of space policy and social policy may seem tenuous at first, but both celebrate the power of the federal government and the state system to affect in fundamental ways the lives of citizens. This chapter explores those linkages, the relationship among the authority of experts and political leaders, and the manner in which management practices successful at NASA may have been applied with varying success to other governmental organizations. C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. NR 39 TC 0 Z9 0 U1 0 U2 1 PU AMER ASTRONAUTICAL SOC PI SAN DIEGO PA PUBLICATIONS OFFICE PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0730-3564 BN 978-0-87703-590-9 J9 AAS HIST SER PY 2013 VL 39 BP 53 EP 69 PG 17 WC Engineering, Aerospace SC Engineering GA BFR69 UT WOS:000321076100004 ER PT J AU Richmond, CE Rose, KA Breitburg, DL AF Richmond, Courtney E. Rose, Kenneth A. Breitburg, Denise L. TI Individual variability and environmental conditions: effects on zooplankton cohort dynamics SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Variability among individuals; Fitness; Cohort dynamics; Individual-based model; Acartia tonsa; Environmental conditions; Size-dependent mortality ID COPEPOD ACARTIA-TONSA; CTENOPHORE MNEMIOPSIS-LEIDYI; NARRAGANSETT BAY; EGG-PRODUCTION; CHESAPEAKE-BAY; BODY-SIZE; RHODE-ISLAND; SEED BANK; CHRYSAORA-QUINQUECIRRHA; POPULATION-DYNAMICS AB We use an individual-based cohort model of the planktonic calanoid copepod Acartia tonsa to examine how variability among individuals in bioenergetic traits affects cohort dynamics. The model follows a cohort of individual zooplankton through the hourly processes of feeding and energy distribution among growth, development, and reproduction, under high and low rates of size-dependent mortality. The degree of variability in traits among individuals was quantified by the coefficient of variation (CV). In our first simulation experiment (Expt 1), population growth rate (lambda) increased with increasing variability among individuals (increasing CV) when overall mortality was high; egg production increased with CV under high and low mortality rates, and survival was unaffected by the degree of trait variability. Expt 2 tested the effect of genetic makeup on cohort dynamics; when mortality rate was high, increasing CV resulted in individuals with correlated traits having higher egg production and lambda than individuals with randomly assigned traits. Expt 3 tested how environmental conditions altered the effect of CV on survival, egg production, and lambda. Population growth rate increased with increasing CV under high mortality rate and suboptimal conditions. Our analyses demonstrate how small differences in the values of individual-level traits can influence growth and reproduction which can in turn translate into ecologically important effects on cohort dynamics. The effect of increased variability among individuals on cohort dynamics was particularly important when environmental conditions were poor, when the mortality rate was high, and under certain types of size-dependent mortality. These results may have important implications for understanding the dynamics of populations experiencing stress. C1 [Richmond, Courtney E.] Rowan Univ, Dept Biol Sci, Glassboro, NJ 08028 USA. [Rose, Kenneth A.] Louisiana State Univ, Dept Oceanog & Coastal Sci Energy Coast & Environ, Baton Rouge, LA 70803 USA. [Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Richmond, CE (reprint author), Rowan Univ, Dept Biol Sci, Glassboro, NJ 08028 USA. EM richmond@rowan.edu OI Richmond, Courtney/0000-0002-8699-3589 FU National Oceanic and Atmospheric Administration (NOAA); Center for Sponsored Coastal Ocean Research (CSCOR); National Research Council Research Associateship Award; EPA-Atlantic Ecology Division laboratory in Narragansett, Rhode Island, USA; NOAA; CSCOR; NGOMEX06 grant [NA06 NOS4780131, NA09NOS4780179] FX This work was supported by the National Oceanic and Atmospheric Administration (NOAA), Center for Sponsored Coastal Ocean Research (CSCOR) to the COASTES project, and by a National Research Council Research Associateship Award to C.E.R. C.E.R thanks the EPA-Atlantic Ecology Division laboratory in Narragansett, Rhode Island, USA for support and resources during the initial stages of this work. K.A.R was partially supported by the NOAA, CSCOR, NGOMEX06 grant number NA06 NOS4780131 awarded to the University of Texas. K.A.R was partially supported by the NOAA, CSCOR, NGOMEX grant number NA09NOS4780179 awarded to the University of Texas. This is publication number 181 of NOAA's CSCOR NGOMEX Program. NR 108 TC 0 Z9 0 U1 1 U2 14 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2013 VL 486 BP 59 EP 78 DI 10.3354/meps10418 PG 20 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 182WX UT WOS:000321776600006 ER PT J AU Soledade, GO Baeza, JA Boehs, G Simoes, SM Santos, PS da Costa, RC Almeida, AO AF Soledade, Guidomar Oliveira Antonio Baeza, Juan Boehs, Guisla Simoes, Sabrina Morilhas Santos, Patricia Souza da Costa, Rogerio Caetano Almeida, Alexandre Oliveira TI A PRECAUTIONARY TALE WHEN DESCRIBING SPECIES IN A WORLD OF INVADERS: MORPHOLOGY, COLORATION AND GENETICS DEMONSTRATE THAT LYSMATA RAULI IS NOT A NEW SPECIES ENDEMIC TO BRAZIL BUT A JUNIOR SYNONYM OF THE INDO-PACIFIC L. VITTATA SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE alien species; hermaphroditism; Lysmata; morphology; population structure ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; EXHIPPOLYSMATA-OPLOPHOROIDES; PEPPERMINT SHRIMP; SOUTHWESTERN ATLANTIC; DECAPOD CRUSTACEA; WESTERN ATLANTIC; CARIDEAN SHRIMPS; SEXUAL SYSTEM; CARIBBEAN SEA; HIPPOLYTIDAE AB The objective of this study was to investigate morphological variation in traits of systematic relevance and the phylogenetic position, ecology, and reproductive biology of the shrimp Lysmata rauli Laubenheimer and Rhyne, 2010 (Caridea: Hippolytidae), described based only on a single specimen collected in Salvador, Bahia, Brazil. We analyzed a total of 89 specimens from Camamu Bay, Bahia (n = 88) and from Sao Vicente estuary, Sao Paulo (n = 1). Considerable morphological variation was detected in the rostral spine series, number of segments on the carpus and merus of pereiopod 2, number of spiniform setae on the ventrolateral margin of merus and on the ventral margin of propodus of pereiopods 3-5. Importantly, L. rauli can be distinguished neither using morphology, nor coloration from the Indo-Pacific L. vittata (Stimpson, 1860). Furthermore, molecular phylogenetic analyses (using the 16S mt DNA fragment) did not reveal any considerable genetic dissimilarities between L. rauli and L. vittata. Thus, our results clearly indicate that L. rauli is not a new species but a junior synonym of L. vittata. The high density observed within the structures of oyster farming indicates that the invasive L. vittata lives in "crowds" in Brazil. The studied population was composed of males, hermaphrodites, and transitional individuals (having characteristics of males and hermaphrodites). The above information suggests that L. rauli is a protandric simultaneous hermaphrodite, as it has been observed in all species of Lysmata that have been investigated. Lysmata vittata has invaded the southwestern Atlantic and is present in Bahia, Rio de Janeiro and Sao Paulo, Brazil. C1 [Soledade, Guidomar Oliveira; Boehs, Guisla; Santos, Patricia Souza; Almeida, Alexandre Oliveira] Univ Estadual Santa Cruz, Dept Ciencias Biol, BR-45662900 Ilheus, BA, Brazil. [Antonio Baeza, Juan] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, Juan] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. [Simoes, Sabrina Morilhas; da Costa, Rogerio Caetano] Univ Estadual Paulista, Fac Ciencias, Dept Ciencias Biol, BR-17033360 Bauru, SP, Brazil. RP Almeida, AO (reprint author), Univ Estadual Santa Cruz, Dept Ciencias Biol, Rod Jorge Amado,Km 16, BR-45662900 Ilheus, BA, Brazil. EM aalmeida@uesc.br RI Boehs, Guisla/K-7377-2012; Costa, Rogerio/A-5402-2008; OI Oliveira Almeida, Alexandre/0000-0003-0470-8658; Baeza, Juan Antonio/0000-0002-2573-6773 FU Financiadora de Estudos e Projetos (FINEP, MCT-Brazil) [PPP0073/2010, 04/07309-8, 08/53999-7, 09/546724, 10/50188-8]; Universidade Estadual de Santa Cruz [00220.1100.573, 00220.1100.590, 00220.1100.821]; CNPq (Conselho Nacional de Desenvolvimento Cientffico e Tecnologico, MCT-Brazil); Universidade Estadual de Santa Cruz (UESC); FAPESB FX The authors are indebted to Financiadora de Estudos e Projetos (FINEP, MCT-Brazil), to FAPESB (Fundacao de Amparo a Pesquisa do Egtado da Bahia) (PPP0073/2010), to FAPESP (04/07309-8; 08/53999-7, 09/546724 and 10/50188-8), and to Universidade Estadual de Santa Cruz (Projects 00220.1100.573;" 00220.1100.590 and 00220.1100.821) and CNPq (Conselho Nacional de Desenvolvimento Cientffico e Tecnologico, MCT-Brazil) for providing financial support. GOS thanks Universidade Estadual de Santa Cruz (UESC) and FAPESB, for the provision of scholarships. To Organizacao Pro-Defesa e Estudos dos Manguezais da Bahia (ORDEM), especially to Elias Veloso, for the support in the field trips. The authors are also indebted to Anna Gabrielle Pedra, Helen Affe, Thailla Ourives, Gabriel Barros and Roberto Almeida for their help in the field and to Anna Gabrielle Pedra for taking some photographs used in this paper. Many thanks to Sammy De Grave for examining specimens of L. vittata deposited in the Oxford University Museum of Natural History. The authors are also indebted to two anonymous referees and the associate editor whose comments improved the manuscript. This is SMSFP contribution number 898. NR 64 TC 6 Z9 9 U1 2 U2 13 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD JAN PY 2013 VL 33 IS 1 BP 66 EP 77 DI 10.1163/1937240X-00002122 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 168BO UT WOS:000320680900010 ER PT S AU Case, AW Kasper, JC Daigneau, PS Caldwell, D Freeman, M Gauron, T Maruca, BA Bookbinder, J Korreck, KE Cirtain, JW Effinger, ME Halekas, JS Larson, DE Lazarus, AJ Stevens, ML Taylor, ER Wright, JKH AF Case, A. W. Kasper, J. C. Daigneau, P. S. Caldwell, D. Freeman, M. Gauron, T. Maruca, B. A. Bookbinder, J. Korreck, K. E. Cirtain, J. W. Effinger, M. E. Halekas, J. S. Larson, D. E. Lazarus, A. J. Stevens, M. L. Taylor, E. R. Wright, Jr K. H. BE Zank, GP Borovsky, J Bruno, R Cirtain, J Cranmer, S Elliott, H Giacalone, J Gonzalez, W Li, G Marsch, E Moebius, E Pogorelov, N Spann, J Verkhoglyadova, O TI Designing a Sun-pointing Faraday Cup for Solar Probe Plus SO PROCEEDINGS OF THE THIRTEENTH INTERNATIONAL SOLAR WIND CONFERENCE (SOLAR WIND 13) SE AIP Conference Proceedings LA English DT Proceedings Paper CT 13th International Solar Wind Conference (Solar Wind) CY JUN 17-22, 2012 CL HI SP Natl Sci Fdn (NSF), Int Conf & Networking Solut (ICNS) DE Solar Wind; Space Plasma; Instrumentation ID PLASMA; INSTRUMENT AB The NASA Solar Probe Plus (SPP) mission will be the first spacecraft to pass through the sub-Alfvenic solar corona. The objectives of the mission are to trace the flow of energy that heats and accelerates the solar corona and solar wind, to determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind, and to explore mechanisms that accelerate and transport energetic particles. The Solar Wind Electrons, Alphas, and Protons (SWEAP) Investigation instrument suite on SPP will measure the bulk solar wind conditions in the inner heliosphere. SWEAP consists of the Solar Probe Cup (SPC), a sun-pointing Faraday Cup, and the Solar Probe ANalyzers (SPAN), a set of 3 electrostatic analyzers that will reside in the penumbra of SPP's thermal protection system and measure solar wind ions and electrons. SPP is scheduled to launch in 2018 into an equatorial solar orbit where a sequence of Venus gravity assists will gradually lower its closest solar approach to within 9.5 solar radii (R-S) of the center of the Sun. The photon flux at 9.5 R-S is more than 500 times greater than at 1 AU and therefore presents a design challenge for SPC, which will point directly at the Sun. SPC is derived from the Faraday cup instruments successfully flown on spacecraft from the beginning of the space age, but updated with high temperature materials to operate through the solar encounters. Current work includes both instrument design and the development of a testing approach capable of demonstrating adequate performance in encounter conditions. This paper will briefly discuss the suite as a whole, and then focus on the design and capabilities of SPC. We will also present the planned calibration and characterization of the instrument and the testing required to demonstrate the technological readiness of the design. C1 [Case, A. W.; Kasper, J. C.; Daigneau, P. S.; Caldwell, D.; Freeman, M.; Gauron, T.; Bookbinder, J.; Korreck, K. E.; Stevens, M. L.] Harvard Smithsonian Ctr Astrophys, Boston, MA 02115 USA. RP Case, AW (reprint author), Harvard Smithsonian Ctr Astrophys, Boston, MA 02115 USA. OI Halekas, Jasper/0000-0001-5258-6128 NR 4 TC 6 Z9 6 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-1163-0 J9 AIP CONF PROC PY 2013 VL 1539 BP 458 EP 461 DI 10.1063/1.4811083 PG 4 WC Energy & Fuels; Physics, Applied SC Energy & Fuels; Physics GA BFQ76 UT WOS:000320997100108 ER PT J AU Mirabello, MJ Yavitt, JB Garcia, M Harms, KE Turner, BL Wright, SJ AF Mirabello, M. J. Yavitt, J. B. Garcia, M. Harms, K. E. Turner, B. L. Wright, S. J. TI Soil phosphorus responses to chronic nutrient fertilisation and seasonal drought in a humid lowland forest, Panama SO SOIL RESEARCH LA English DT Article DE extractable phosphorus; Hedley fractionation; organic bound P; strongly weathered soil ID TROPICAL MOIST FOREST; ORGANIC PHOSPHORUS; MICROBIAL BIOMASS; P-FRACTIONS; NEW-ZEALAND; PEDOGENESIS; PHOSPHATE; DYNAMICS; NITROGEN; GROWTH AB We used the Hedley sequential fractionation scheme to assess phosphorus (P) chemistry of a strongly weathered soil from a humid lowland forest in Panama. Our analyses were part of a factorial experiment of nitrogen, P, and potassium addition, with nutrients added annually, i.e. a chronic input. The aim was to examine changes in soil P chemistry with 7 years of nutrient addition for soils collected in the wet season and the dry season. The majority of P occurred in fractions extracted by NaOH (24% of the total soil P) and hot concentrated HCl (58% of the total). Organic P (P-o) was similar to 54% of extractable P. Labile P, defined as P-o plus inorganic P (P-i) extracted by NaHCO3, was largely P-o (84% of the NaHCO3-extractable P). Chronic P addition increased NaHCO3-extractable P-o several-fold and NaOH-extractable P-i two-fold. Seasonal variation occurred for labile P and NaOH-extractable P, whereas occluded P did not vary throughout the study period. Extractable P was similar to 15% higher in surface than subsurface soil. We added 350 kg P ha(-1) during the 7-year period and recovered similar to 55% by sequential extraction. According to biogeochemical theory, added P should show up in fractions with the shortest residence times, e. g. labile P. Our finding that added P accumulated in fractions with presumably long residence times, i.e. extracted by NaOH (bound) and hot concentrated HCl (occluded), suggests that greater attention be paid to the short-term dynamics of bound and occluded P in strongly weathered tropical forest soils. C1 [Mirabello, M. J.; Yavitt, J. B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Garcia, M.; Harms, K. E.; Turner, B. L.; Wright, S. J.] Smithsonian Trop Res Inst, Panama City, Panama. [Harms, K. E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Yavitt, JB (reprint author), Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. EM jby1@cornell.edu RI Turner, Benjamin/E-5940-2011; Wright, Stuart/M-3311-2013 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676 FU Scholarly Studies program of the Smithsonian Institution; Andrew W. Mellon Foundation FX Rufino Gonzalez and Omar Hernandez have added nutrients since 1998. Funding was provided by grants from the Scholarly Studies program of the Smithsonian Institution and the Andrew W. Mellon Foundation to S. J. Wright. NR 49 TC 2 Z9 3 U1 1 U2 45 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1838-675X J9 SOIL RES JI Soil Res. PY 2013 VL 51 IS 3 BP 215 EP 221 DI 10.1071/SR12188 PG 7 WC Soil Science SC Agriculture GA 168NG UT WOS:000320712200005 ER PT J AU Cernusak, LA Winter, K Dalling, JW Holtum, JAM Jaramillo, C Korner, C Leakey, ADB Norby, RJ Poulter, B Turner, BL Wright, SJ AF Cernusak, Lucas A. Winter, Klaus Dalling, James W. Holtum, Joseph A. M. Jaramillo, Carlos Koerner, Christian Leakey, Andrew D. B. Norby, Richard J. Poulter, Benjamin Turner, Benjamin L. Wright, S. Joseph TI Tropical forest responses to increasing atmospheric CO2: current knowledge and opportunities for future research SO FUNCTIONAL PLANT BIOLOGY LA English DT Review DE carbon storage; CO2 enrichment; liana; phosphorus; succession; water use efficiency ID WATER-USE EFFICIENCY; ELEVATED CARBON-DIOXIDE; AMAZON RAIN-FOREST; SOIL ORGANIC PHOSPHORUS; GLOBAL VEGETATION MODEL; BARRO-COLORADO ISLAND; BASIN-WIDE VARIATIONS; FICUS-INSIPIDA WILLD; STOMATAL CONDUCTANCE; LONG-TERM AB Elevated atmospheric CO2 concentrations (ca) will undoubtedly affect the metabolism of tropical forests worldwide; however, critical aspects of how tropical forests will respond remain largely unknown. Here, we review the current state of knowledge about physiological and ecological responses, with the aim of providing a framework that can help to guide future experimental research. Modelling studies have indicated that elevated ca can potentially stimulate photosynthesis more in the tropics than at higher latitudes, because suppression of photorespiration by elevated ca increases with temperature. However, canopy leaves in tropical forests could also potentially reach a high temperature threshold under elevated ca that will moderate the rise in photosynthesis. Belowground responses, including fine root production, nutrient foraging and soil organic matter processing, will be especially important to the integrated ecosystem response to elevated ca. Water use efficiency will increase as ca rises, potentially impacting upon soil moisture status and nutrient availability. Recruitment may be differentially altered for some functional groups, potentially decreasing ecosystem carbon storage. Whole-forest CO2 enrichment experiments are urgently needed to test predictions of tropical forest functioning under elevated ca. Smaller scale experiments in the understorey and in gaps would also be informative, and could provide stepping stones towards stand-scale manipulations. C1 [Cernusak, Lucas A.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Winter, Klaus; Holtum, Joseph A. M.; Jaramillo, Carlos; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dalling, James W.; Leakey, Andrew D. B.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Holtum, Joseph A. M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Koerner, Christian] Univ Basel, Inst Bot, CH-4056 Basel, Switzerland. [Norby, Richard J.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Norby, Richard J.] Oak Ridge Natl Lab, Climate Change Sci Inst, Oak Ridge, TN 37831 USA. [Poulter, Benjamin] Univ Versailles St Quentin, F-91191 Versailles, France. RP Cernusak, LA (reprint author), James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. EM lcernusak@gmail.com RI Cernusak, Lucas/A-6859-2011; Turner, Benjamin/E-5940-2011; Korner, Christian/B-6592-2014; James Cook University, TESS/B-8171-2012; Wright, Stuart/M-3311-2013; Research ID, CTBCC /O-3564-2014; Norby, Richard/C-1773-2012; Leakey, Andrew/Q-9889-2016 OI Cernusak, Lucas/0000-0002-7575-5526; Turner, Benjamin/0000-0002-6585-0722; Poulter, Benjamin/0000-0002-9493-8600; Wright, Stuart/0000-0003-4260-5676; Norby, Richard/0000-0002-0238-9828; Leakey, Andrew/0000-0001-6251-024X FU Smithsonian Tropical Research Institute; Australian Research Council [FT100100329] FX This review resulted from a symposium held at the Smithsonian Tropical Research Institute on 31 March and 1 April 2011. Funding for the symposium was provided by the Smithsonian Tropical Research Institute. LAC was supported by a Future Fellowship from the Australian Research Council (FT100100329). NR 243 TC 31 Z9 32 U1 9 U2 142 PU CSIRO PUBLISHING PI COLLINGWOOD PA 150 OXFORD ST, PO BOX 1139, COLLINGWOOD, VICTORIA 3066, AUSTRALIA SN 1445-4408 J9 FUNCT PLANT BIOL JI Funct. Plant Biol. PY 2013 VL 40 IS 6 BP 531 EP 551 DI 10.1071/FP12309 PG 21 WC Plant Sciences SC Plant Sciences GA 162NH UT WOS:000320271400001 ER PT S AU Birnstiel, T Pinilla, P Andrews, SM Benisty, M Ercolano, B AF Birnstiel, T. Pinilla, P. Andrews, S. M. Benisty, M. Ercolano, B. BE Barge, P Jorda, L TI Transition Disks - Grain Growth, Planets, or Photoevaporation? SO INSTABILITIES AND STRUCTURES IN PROTO-PLANETARY DISKS SE EPJ Web of Conferences LA English DT Proceedings Paper CT Workshop on Instabilities and Structures in Proto-Planetary Disks CY SEP 17-20, 2012 CL Marseille, FRANCE SP AMU, Lab Astrophysique Marseille (LAM) ID SOLAR-TYPE STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; X-RAY; HYDRODYNAMIC MODELS; GM-AURIGAE; INNER HOLE; DUST; COAGULATION; DISCS AB In the past years, many transition disks have been detected via SED modeling or imaging. The disks feature dust cavities in their inner regions with sizes ranging from a few to more than 70 AU. The origin of those structures, however, remains mysterious. We will present how our recent simulation results, which include gap opening by a giant planet and effects of dust evolution, could explain these structures. C1 [Birnstiel, T.; Ercolano, B.] Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. [Birnstiel, T.; Ercolano, B.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany. [Pinilla, P.] Heidelberg Univ, Inst Theoret Astrophys, Heidelberg, Germany. [Andrews, S. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benisty, M.] Inst Planetol & Astrophys Grenoble, UMR 5274, F-38041 Grenoble, France. RP Birnstiel, T (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM til.birnstiel@lmu.de OI Birnstiel, Tilman/0000-0002-1899-8783 NR 44 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 2100-014X BN 978-2-7598-0983-7 J9 EPJ WEB CONF PY 2013 VL 46 AR UNSP 02001 DI 10.1051/epjconf/20134602001 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFH95 UT WOS:000319936900003 ER PT J AU Goots, A Bruwelheide, K Owsley, D AF Goots, Alexis Bruwelheide, Kari Owsley, Doug TI Post-traumatic bone loss in Civil War soldiers. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Goots, Alexis] Ohio State Univ, Dept Anthropol, Columbus, OH 43210 USA. [Goots, Alexis; Bruwelheide, Kari; Owsley, Doug] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 134 EP 134 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043201299 ER PT J AU Hatala, KG Lieberman, DE Dingwall, HL Castillo, ER Wunderlich, RE Okutoyi, P Sigei, T Anjila, A Pitsiladis, Y Richmond, BG AF Hatala, Kevin G. Lieberman, Daniel E. Dingwall, Heather L. Castillo, Eric R. Wunderlich, Roshna E. Okutoyi, Paul Sigei, Timothy Anjila, Adwin Pitsiladis, Yannis Richmond, Brian G. TI Variation in running foot strike patterns in two habitually unshod Kenyan populations. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Hatala, Kevin G.; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Lieberman, Daniel E.; Dingwall, Heather L.; Castillo, Eric R.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Wunderlich, Roshna E.] James Madison Univ, Dept Biol, Harrisonburg, VA USA. [Okutoyi, Paul; Sigei, Timothy; Anjila, Adwin; Pitsiladis, Yannis] Moi Univ, Sch Med, Eldoret, Kenya. [Pitsiladis, Yannis] Univ Glasgow, Coll Med Vet & Life Sci, Glasgow G12 8QQ, Lanark, Scotland. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 144 EP 145 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043201345 ER PT J AU Hunt, DR Ousley, SD AF Hunt, David R. Ousley, Stephen D. TI The Biological Anthropology Database legacy of Richard L. Jantz. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Hunt, David R.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Ousley, Stephen D.] Mercyhurst Univ, Dept Anthropol Archaeol, Erie, PA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 154 EP 155 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043201387 ER PT J AU Knigge, RP Tocheri, MW Orr, CM Mcnulty, KP AF Knigge, Ryan P. Tocheri, Matthew W. Orr, Caley M. Mcnulty, Kieran P. TI The relationship between talar morphology and habitual substrate use among living gorilla taxa assessed using 3D geometric morphometrics SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Knigge, Ryan P.; Mcnulty, Kieran P.] Univ Minnesota, Evolutionary Anthropol Lab, Minneapolis, MN 55455 USA. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. [Orr, Caley M.] Midwestern Univ, Dept Anat, Downers Grove, IL USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 170 EP 170 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043201455 ER PT J AU Lague, MR Richmond, BG Green, DJ Braun, DR Harris, JWK Mbua, E Chirchir, H AF Lague, Michael R. Richmond, Brian G. Green, David J. Braun, David R. Harris, John W. K. Mbua, Emma Chirchir, Habiba TI A new similar to 1.5 Ma hominin distal humerus from Ileret, Kenya. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Lague, Michael R.] Richard Stockton Coll New Jersey, Sch Nat Sci & Math, Pomona, NJ USA. [Richmond, Brian G.; Braun, David R.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Green, David J.] Midwestern Univ, Dept Anat, Downers Grove, IL USA. [Harris, John W. K.] Rutgers State Univ, Dept Anthropol, Piscataway, NJ 08855 USA. [Chirchir, Habiba] George Washington Univ, Dept Anthropol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. NR 0 TC 0 Z9 0 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 176 EP 176 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043201481 ER PT J AU Milligan, LA Bernstein, R Wright, L Drought, H Lewis, C Murtough, K Power, M AF Milligan, Lauren A. Bernstein, Robin Wright, Lewis Drought, Heather Lewis, Cari Murtough, Katie Power, Michael TI Longitudinal changes in macronutrient and hormone concentration in orangutan milk during peak lactation. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Milligan, Lauren A.; Murtough, Katie; Power, Michael] Natl Zool Pk, Smithsonian Conservat Biol Inst, Nutr Lab, Front Royal, VA USA. [Bernstein, Robin; Drought, Heather] George Washington Univ, Washington, DC 20052 USA. [Wright, Lewis] Fresno Chaffee Zoo, Vet Care, Fresno, CA USA. [Lewis, Cari] Indiana Univ, Bloomington, IN 47405 USA. [Power, Michael] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC USA. NR 0 TC 0 Z9 0 U1 2 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 199 EP 199 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202078 ER PT J AU O'Mara, T AF O'Mara, Teague TI The ontogeny of sex differences in ring-tailed lemur feeding ecology: costs of reproduction and niche partitioning SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [O'Mara, Teague] Arizona State Univ, Smithsonian Inst, Smithsonian Trop Res Inst, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. NR 0 TC 0 Z9 0 U1 1 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 210 EP 210 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202123 ER PT J AU Power, ML Schulkin, J Drought, H Hinde, K Bernstein, RM AF Power, Michael L. Schulkin, Jay Drought, Heather Hinde, Katie Bernstein, Robin M. TI Bioactive factors in milk: Comparisons across nonhuman primates and humans. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Power, Michael L.] Georgetown Univ, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC 20057 USA. [Power, Michael L.; Schulkin, Jay] Georgetown Univ, Res Dept, Amer Coll Obstetricians & Gynecologists, Washington, DC 20057 USA. Georgetown Univ, Dept Neurosci, Washington, DC 20057 USA. [Drought, Heather; Bernstein, Robin M.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Hinde, Katie] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. NR 0 TC 1 Z9 1 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 224 EP 224 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202182 ER PT J AU Prang, C Tocheri, MW AF Prang, Cody Tocheri, Matthew W. TI Locomotor diversity and midfoot mobility in gorillas. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Prang, Cody] NYU, Dept Anthropol, New York, NY 10003 USA. [Prang, Cody] Smithsonian Inst, New York Consortium Evolutionary Primatol, Washington, DC 20560 USA. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 1 Z9 1 U1 2 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 224 EP 225 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202185 ER PT J AU Rabey, KN Green, DJ Begun, DR Richmond, BG Mcfarlin, SC AF Rabey, Karyne N. Green, David J. Begun, David R. Richmond, Brian G. Mcfarlin, Shannon C. TI Activity type and level influence growth rate, remodeling, and diaphyseal geometry of cortical bone. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Rabey, Karyne N.] Duke Univ, Durham, NC 27706 USA. [Rabey, Karyne N.; Begun, David R.] Univ Toronto, Dept Anthropol, Toronto, ON M5S 1A1, Canada. [Green, David J.] Midwestern Univ, Dept Anat, Downers Grove, IL USA. [Richmond, Brian G.; Mcfarlin, Shannon C.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 228 EP 228 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202200 ER PT J AU Schroer, K Ramirez, K Wood, B AF Schroer, Kes Ramirez, Kristen Wood, Bernard TI Mandibular premolar morphology is correlated with mechanically challenging diets in sympatric primates. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Schroer, Kes; Ramirez, Kristen; Wood, Bernard] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Wood, Bernard] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 246 EP 246 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202276 ER PT J AU Sobolewski, ME Brown, J Mitani, JC AF Sobolewski, Marissa E. Brown, Janine Mitani, John C. TI Anticipatory stress, territoriality and hunting in wild chimpanzees. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Sobolewski, Marissa E.; Mitani, John C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Brown, Janine] Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 259 EP 259 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202332 ER PT J AU Ward, CV Tocheri, MW Plavcan, JM Brown, FH Manthi, FK AF Ward, Carol V. Tocheri, Matthew W. Plavcan, J. Michael Brown, Frank H. Manthi, Fredrick K. TI Earliest evidence of distinctive modern human-like hand morphology from West Turkana, Kenya SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Ward, Carol V.] Univ Missouri, Columbia, MO 65211 USA. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Plavcan, J. Michael] Univ Arkansas, Fayetteville, AR 72701 USA. [Brown, Frank H.] Univ Utah, Coll Mines & Earth Sci, Salt Lake City, UT 84112 USA. NR 0 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 284 EP 284 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202441 ER PT J AU Williams, L Norris, AL Dupras, T Wheeler, S Tocheri, M AF Williams, Lana Norris, Annie Laurie Dupras, Tosha Wheeler, Sandra Tocheri, Matthew TI Isotopic measures of intra-individual variation in fetal bone collagen and apatite. SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Meeting Abstract CT 82nd Annual Meeting of the American-Association-of-Physical-Anthropologists CY APR 09-13, 2013 CL Knoxville, TN SP Amer Assoc Phys Anthropologists C1 [Williams, Lana; Dupras, Tosha; Wheeler, Sandra] Univ Cent Florida, Dept Anthropol, Orlando, FL 32816 USA. [Norris, Annie Laurie] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Dupras, Tosha] NYU, Inst Study Ancient World, New York, NY 10003 USA. [Tocheri, Matthew] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PY 2013 VL 150 SU 56 SI SI BP 292 EP 292 PG 1 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 132BR UT WOS:000318043202476 ER PT J AU Manera, M Scoccimarro, R Percival, WJ Samushia, L McBride, CK Ross, AJ Sheth, RK White, M Reid, BA Sanchez, AG de Putter, R Xu, XY Berlind, AA Brinkmann, J Maraston, C Nichol, B Montesano, F Padmanabhan, N Skibba, RA Tojeiro, R Weaver, BA AF Manera, Marc Scoccimarro, Roman Percival, Will J. Samushia, Lado McBride, Cameron K. Ross, Ashley J. Sheth, Ravi K. White, Martin Reid, Beth A. Sanchez, Ariel G. de Putter, Roland Xu, Xiaoying Berlind, Andreas A. Brinkmann, Jonathan Maraston, Claudia Nichol, Bob Montesano, Francesco Padmanabhan, Nikhil Skibba, Ramin A. Tojeiro, Rita Weaver, Benjamin A. TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: a large sample of mock galaxy catalogues SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: haloes; large-scale structure of Universe ID DIGITAL SKY SURVEY; COLD DARK-MATTER; HALO OCCUPATION DISTRIBUTION; POWER-SPECTRUM ANALYSIS; LARGE-SCALE STRUCTURE; GRAVITATIONAL-INSTABILITY; REDSHIFT-SPACE; COSMOLOGICAL IMPLICATIONS; ACOUSTIC-OSCILLATIONS; LAGRANGIAN APPROACH AB We present a fast method for producing mock galaxy catalogues that can be used to compute the covariance of large-scale clustering measurements and test analysis techniques. Our method populates a second-order Lagrangian perturbation theory (2LPT) matter field, where we calibrate masses of dark matter haloes by detailed comparisons with N-body simulations. We demonstrate that the clustering of haloes is recovered at similar to 10 per cent accuracy. We populate haloes with mock galaxies using a halo occupation distribution (HOD) prescription, which has been calibrated to reproduce the clustering measurements on scales between 30 and 80 h(-1) Mpc. We compare the sample covariance matrix from our mocks with analytic estimates, and discuss differences. We have used this method to make catalogues corresponding to Data Release 9 of the Baryon Oscillation Spectroscopic Survey (BOSS), producing 600 mock catalogues of the 'CMASS' galaxy sample. These mocks have enabled detailed tests of methods and errors, and have formed an integral part of companion analyses of these galaxy data. C1 [Manera, Marc; Percival, Will J.; Samushia, Lado; Ross, Ashley J.; Maraston, Claudia; Nichol, Bob; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Scoccimarro, Roman; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sheth, Ravi K.] Abdus Salam Int Ctr Theoret Phys, I-34151 Trieste, Italy. [Sheth, Ravi K.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [White, Martin] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. [White, Martin; Reid, Beth A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Sanchez, Ariel G.; Montesano, Francesco] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [de Putter, Roland] Univ Valencia, CSIC, Inst Fis Corpuscular, E-46071 Valencia, Spain. [de Putter, Roland] Univ Barcelona IEEC UB, Inst Cincies Cosmos, E-08028 Barcelona, Spain. [Xu, Xiaoying; Skibba, Ramin A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Berlind, Andreas A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Brinkmann, Jonathan] Apache Point Observ, Sunspot, NM 88349 USA. [Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Manera, M (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. EM marc.manera@port.ac.uk RI White, Martin/I-3880-2015 OI White, Martin/0000-0001-9912-5070 FU European Research Council; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; ICG; SEPNet; University of Portsmouth; STFC; HEFCE; SGI; NSF [AST-0607747]; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge,; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX MM acknowledges support from European Research Council. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. The analysis made use of the computing resources of the National Energy Research Scientific Computing Center, the Shared Research Computing Services Pilot of the University of California and the Laboratory Research Computing project at Lawrence Berkeley National Laboratory.; Part of the numerical computations and analyses were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth. MM thanks Gary Burton and David Bacon for designing the system and for their help when running the mocks. Parts of the process were performed on the COSMOS supercomputer which is funded by STFC, HEFCE and SGI. This research was partially supported by grant NSF AST-0607747 NR 79 TC 96 Z9 96 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1036 EP 1054 DI 10.1093/mnras/sts084 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000007 ER PT J AU Steffen, JH Fabrycky, DC Agol, E Ford, EB Morehead, RC Cochran, WD Lissauer, JJ Adams, ER Borucki, WJ Bryson, S Caldwell, DA Dupree, A Jenkins, JM Robertson, P Rowe, JF Seader, S Thompson, S Twicken, JD AF Steffen, Jason H. Fabrycky, Daniel C. Agol, Eric Ford, Eric B. Morehead, Robert C. Cochran, William D. Lissauer, Jack J. Adams, Elisabeth R. Borucki, William J. Bryson, Steve Caldwell, Douglas A. Dupree, Andrea Jenkins, Jon M. Robertson, Paul Rowe, Jason F. Seader, Shawn Thompson, Susan Twicken, Joseph D. TI Transit timing observations from Kepler - VII. Confirmation of 27 planets in 13 multiplanet systems via transit timing variations and orbital stability SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: photometric; celestial mechanics ID 1ST 4 MONTHS; GIANT PLANET; SUPER-EARTH; CANDIDATES; STARS; VALIDATION; MIGRATION; DYNAMICS; MODELS; MASS AB We confirm 27 planets in 13 planetary systems by showing the existence of statistically significant anticorrelated transit timing variations, which demonstrates that the planet candidates are in the same system, and long-term dynamical stability, which places limits on the masses of the candidates - showing that they are planetary. All of these newly confirmed planetary systems have orbital periods that place them near first-order mean motion resonances (MMRs), including six systems near the 2: 1 MMR, five near 3: 2, and one each near 4: 3, 5: 4 and 6:5. In addition, several unconfirmed planet candidates exist in some systems (that cannot be confirmed with this method at this time). A few of these candidates would also be near first-order MMRs with either the confirmed planets or other candidates. One system of particular interest, Kepler-56 (KOI-1241), is a pair of planets orbiting a twelfth magnitude, giant star with radius over three times that of the Sun and effective temperature of 4900 K - among the largest stars known to host a transiting exoplanetary system. C1 [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 90195 USA. [Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. [Cochran, William D.; Robertson, Paul] Univ Texas Austin, McDonald Observ, Austin, TX 78730 USA. [Lissauer, Jack J.; Borucki, William J.; Bryson, Steve; Jenkins, Jon M.; Rowe, Jason F.; Seader, Shawn; Thompson, Susan; Twicken, Joseph D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Adams, Elisabeth R.; Dupree, Andrea] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caldwell, Douglas A.] SETI Inst, Mountain View, CA 94043 USA. RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500,MS 127, Batavia, IL 60510 USA. EM jsteffen@fnal.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; /0000-0002-0802-9145; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX08AR04G, NAS 5-26555]; NASA through Hubble Fellowship [HF-51272.01-A, HF-51267.01-A]; Space Telescope Science Institute; National Science Foundation Graduate Research Fellowship [DGE-0802270] FX We thank Yoram Lithwick, Roberto Sanchis-Ojeda, Bill Chaplin and Daniel Huber for their useful input and discussions. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is proving so successful. JHS acknowledges support by NASA under grant NNX08AR04G issued through the Kepler Participating Scientist Program. DCF and JAC acknowledge that support for this work was provided by NASA through Hubble Fellowship grants #HF-51272.01-A and #HF-51267.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. RCM is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0802270. NR 38 TC 74 Z9 74 U1 1 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1077 EP 1087 DI 10.1093/mnras/sts090 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000009 ER PT J AU Ross, AJ Percival, WJ Carnero, A Zhao, GB Manera, M Raccanelli, A Aubourg, E Bizyaev, D Brewington, H Brinkmann, J Brownstein, JR Cuesta, AJ da Costa, LAN Eisenstein, DJ Ebelke, G Guo, H Hamilton, JC Magana, MV Malanushenko, E Malanushenko, V Maraston, C Montesano, F Nichol, RC Oravetz, D Pan, KK Prada, F Sanchez, AG Samushia, L Schlegel, DJ Schneider, DP Seo, HJ Sheldon, A Simmons, A Snedden, S Swanson, MEC Thomas, D Tinker, JL Tojeiro, R Zehavi, I AF Ross, Ashley J. Percival, Will J. Carnero, Aurelio Zhao, Gong-bo Manera, Marc Raccanelli, Alvise Aubourg, Eric Bizyaev, Dmitry Brewington, Howard Brinkmann, J. Brownstein, Joel R. Cuesta, Antonio J. da Costa, Luiz A. N. Eisenstein, Daniel J. Ebelke, Garrett Guo, Hong Hamilton, Jean-Christophe Magana, Mariana Vargas Malanushenko, Elena Malanushenko, Viktor Maraston, Claudia Montesano, Francesco Nichol, Robert C. Oravetz, Daniel Pan, Kaike Prada, Francisco Sanchez, Ariel G. Samushia, Lado Schlegel, David J. Schneider, Donald P. Seo, Hee-Jong Sheldon, Alaina Simmons, Audrey Snedden, Stephanie Swanson, Molly E. C. Thomas, Daniel Tinker, Jeremy L. Tojeiro, Rita Zehavi, Idit TI The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmology: observations; (cosmology:) inflation; (cosmology:) large-scale structure of Universe ID DIGITAL-SKY-SURVEY; LUMINOUS RED GALAXIES; SURVEY IMAGING DATA; DATA RELEASE; ACOUSTIC-OSCILLATIONS; REDSHIFT SURVEYS; BIAS; EVOLUTION; QUASARS; PROBE AB We analyse the density field of 264 283 galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) and included in the SDSS Data Release 9 (DR9). In total, the SDSS DR9 BOSS data include spectroscopic redshifts for over 400 000 galaxies spread over a footprint of more than 3000 deg(2). We measure the power spectrum of these galaxies with redshifts 0.43 < z < 0.7 in order to constrain the amount of local non-Gaussianity, f(NL)(local), in the primordial density field, paying particular attention to the impact of systematic uncertainties. The BOSS galaxy density field is systematically affected by the local stellar density and this influences the ability to accurately measure f(NL)(local). In the absence of any correction, we find (erroneously) that the probability that f(NL)(local) is greater than zero, P(f(NL)(local) > 0), is 99.5 per cent. After quantifying and correcting for the systematic bias and including the added uncertainty, we find -45 < f(NL)(local) < 195 at 95 per cent confidence and P(f(NL)(local) > 0) = 91.0 per cent. A more conservative approach assumes that we have only learnt the k dependence of the systematic bias and allows any amplitude for the systematic correction; we find that the systematic effect is not fully degenerate with that of f(NL)(local), and we determine that - 82 < f(NL)(local) < 178 (at 95 per cent confidence) and P(f(NL)(local) > 0) = 68 per cent. This analysis demonstrates the importance of accounting for the impact of Galactic foregrounds on f(NL)(local) measurements. We outline the methods that account for these systematic biases and uncertainties. We expect our methods to yield robust constraints on f(NL)(local) for both our own and future large-scale structure investigations. C1 [Ross, Ashley J.; Percival, Will J.; Zhao, Gong-bo; Manera, Marc; Raccanelli, Alvise; Maraston, Claudia; Nichol, Robert C.; Samushia, Lado; Thomas, Daniel; Tojeiro, Rita] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Carnero, Aurelio; da Costa, Luiz A. N.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero, Aurelio; da Costa, Luiz A. N.] Lab Interinst E Astron LineA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Raccanelli, Alvise] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Raccanelli, Alvise] CALTECH, Pasadena, CA 91125 USA. [Aubourg, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France. [Bizyaev, Dmitry; Brewington, Howard; Brinkmann, J.; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Sheldon, Alaina; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Cuesta, Antonio J.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Eisenstein, Daniel J.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guo, Hong; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Hamilton, Jean-Christophe; Magana, Mariana Vargas] Univ Paris 07, APC, CNRS IN2P3, CEA,Observ Paris, Paris, France. [Montesano, Francesco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Tinker, Jeremy L.] NYU, Ctr Cosmol & Particle Phys, York, NY 10003 USA. RP Ross, AJ (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. EM ashley.ross@port.ac.uk RI Guo, Hong/J-5797-2015; OI Guo, Hong/0000-0003-4936-8247; Raccanelli, Alvise/0000-0001-6726-0438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU UK Science and Technology Facilities Council [ST/I001204/1]; UK Science and Technology Facilities Research Council; European Research Council; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Cambridge University; Carnegie Mellon University; Case Western University; University of Florida; Fermilab; French Participation Group; German Participation Group; Harvard University; UC Irvine; Instituto de Astrofisica de Andalucia; Instituto de Astrofisica de Canarias; Institucio Catalana de Recerca y Estudis Avancat, Barcelona; Instituto de Fisica Corpuscular; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Korean Institute for Advanced Study; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Pittburgh; University of Portsmouth; Princeton University; UC Santa Cruz; Spanish Participation Group; Texas Christian University; Trieste Astrophysical Observatory; University of Tokyo/IPMU; University of Utah; Vanderbilt University; University of Virginia; University of Washington; University of Wisconson; Yale University FX We thank the anonymous referee for comments that helped improve this paper. AJR is grateful to the UK Science and Technology Facilities Council for financial support through the grant ST/I001204/1. WJP is grateful for support from the UK Science and Technology Facilities Research Council and the European Research Council.; Part of the research described in this paper was carried out at the JetPropulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Cambridge University, Carnegie Mellon University, Case Western University, University of Florida, Fermilab, the French Participation Group, the German Participation Group, Harvard University, UC Irvine, Instituto de Astrofisica de Andalucia, Instituto de Astrofisica de Canarias, Institucio Catalana de Recerca y Estudis Avancat, Barcelona, Instituto de Fisica Corpuscular, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Korean Institute for Advanced Study, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Pittburgh, University of Portsmouth, Princeton University, UC Santa Cruz, the Spanish Participation Group, Texas Christian University, Trieste Astrophysical Observatory, University of Tokyo/IPMU, University of Utah, Vanderbilt University, University of Virginia, University of Washington, University of Wisconson and Yale University. NR 64 TC 46 Z9 46 U1 1 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1116 EP 1127 DI 10.1093/mnras/sts094 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000012 ER PT J AU Blecha, L Civano, F Elvis, M Loeb, A AF Blecha, Laura Civano, Francesca Elvis, Martin Loeb, Abraham TI Constraints on the nature of CID-42: recoil kick or supermassive black hole pair? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; gravitational waves; galaxies: active; galaxies: interactions; galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; GRAVITATIONAL-WAVE RECOIL; LINE REGION KINEMATICS; DIGITAL SKY SURVEY; GALAXY MERGERS; COSMOS FIELD; DISK GALAXIES; BINARY; QUASAR; GAS AB The galaxy CXOC J100043.1+020637, also known as CID-42, is a highly unusual object. As an apparent galaxy merger remnant, it displays signatures of both an inspiraling, kiloparsec-scale active galactic nucleus (AGN) pair and of a recoiling AGN with a kick velocity of greater than or similar to 1300 km s(-1). Among recoiling AGN candidates, CID-42 alone has both spatial offsets (in optical and X-ray bands) and spectroscopic offsets. In order to constrain the relative likelihood of both scenarios, we develop models using hydrodynamic galaxy merger simulations coupled with radiative transfer calculations. Our gas-rich, major merger models are generally well matched to the galactic morphology and to the inferred stellar mass and star formation rate. We show that a recoiling supermassive black hole (SMBH) in CID-42 should be observable as an AGN at the time of observation. However, in order for the recoiling AGN to produce narrow-line emission, it must be observed shortly after the kick while it still inhabits a dense gaseous region, implying a large total kick velocity (v(k) greater than or similar to 2000 km s(-1)). For the dual AGN scenario, an unusually large broad-line offset is required, and the best match to the observed morphology requires a galaxy that is less luminous than CID-42. Further, the lack of X-ray emission from one of the two optical nuclei is not easily attributed to an intrinsically quiescent SMBH or to a Compton thick galactic environment. While the current data do not allow either the recoiling or the dual AGN scenario for CID-42 to be excluded, our models highlight the most relevant parameters for distinguishing these possibilities with future observations. In particular, high-quality, spatially resolved spectra that can pinpoint the origin of the broad-line and narrow-line features will be critical for determining the nature of this unique source. C1 [Blecha, Laura; Civano, Francesca; Elvis, Martin; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Blecha, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lblecha@cfa.harvard.edu FU NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We would like to thank Julie Comerford for useful discussions and Chris Hayward, Patrik Jonsson and Greg Snyder for helpful guidance with using SUNRISE. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 72 TC 13 Z9 13 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1341 EP 1350 DI 10.1093/mnras/sts114 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000032 ER PT J AU Foster, JB Mandel, KS Pineda, JE Covey, KR Arce, HG Goodman, AA AF Foster, Jonathan B. Mandel, Kaisey S. Pineda, Jaime E. Covey, Kevin R. Arce, Hector G. Goodman, Alyssa A. TI Evidence for grain growth in molecular clouds: a Bayesian examination of the extinction law in Perseus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; ISM: clouds; dust, extinction ID NEAR-INFRARED EXTINCTION; DIGITAL SKY SURVEY; STAR-FORMING REGIONS; INTERSTELLAR EXTINCTION; BARNARD 5; OPTICAL-PROPERTIES; DATA RELEASE; DARK CLOUD; DUST; 2MASS AB We investigate the shape of the extinction law in two 1 degrees square fields of the Perseus molecular cloud complex. We combine deep red-optical (r, i and z band) observations obtained using Megacam on the MMT with UKIRT (United Kingdom Infrared Telescope) Infrared Deep Sky Survey near-infrared (J, H and K band) data to measure the colours of background stars. We develop a new hierarchical Bayesian statistical model, including measurement error, intrinsic colour variation, spectral type and dust reddening, to simultaneously infer parameters for individual stars and characteristics of the population. We implement an efficient Markov chain Monte Carlo algorithm utilizing generalized Gibbs sampling to compute coherent probabilistic inferences. We find a strong correlation between the extinction (A(V)) and the slope of the extinction law (parametrized by R-V). Because the majority of the extinction towards our stars comes from the Perseus molecular cloud, we interpret this correlation as evidence of grain growth at moderate optical depths. The extinction law changes from the ` diffuse' value of R-V similar to 3 to the 'dense cloud' value of R-V similar to 5 as the column density rises from A(V) = 2 to 10 mag. This relationship is similar for the two regions in our study, despite their different physical conditions, suggesting that dust grain growth is a fairly universal process. C1 [Foster, Jonathan B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Mandel, Kaisey S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Pineda, Jaime E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Covey, Kevin R.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Foster, JB (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM jonathan.b.foster@yale.edu RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010; OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477; Covey, Kevin/0000-0001-6914-7797 FU National Science Foundation [AST-0908159, AST-0407172, AST-0907903]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; National Aeronautics and Space Administration FX This material is based upon work supported by the National Science Foundation under Grant No. AST-0908159, AST-0407172 and AST-0907903. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 69 TC 14 Z9 14 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1606 EP 1622 DI 10.1093/mnras/sts144 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000052 ER PT J AU Ciardi, B Labropoulos, P Maselli, A Thomas, R Zaroubi, S Graziani, L Bolton, JS Bernardi, G Brentjens, M de Bruyn, AG Daiboo, S Harker, GJA Jelic, V Kazemi, S Koopmans, LVE Martinez, O Mellema, G Offringa, AR Pandey, VN Schaye, J Veligatla, V Vedantham, H Yatawatta, S AF Ciardi, B. Labropoulos, P. Maselli, A. Thomas, R. Zaroubi, S. Graziani, L. Bolton, J. S. Bernardi, G. Brentjens, M. de Bruyn, A. G. Daiboo, S. Harker, G. J. A. Jelic, V. Kazemi, S. Koopmans, L. V. E. Martinez, O. Mellema, G. Offringa, A. R. Pandey, V. N. Schaye, J. Veligatla, V. Vedantham, H. Yatawatta, S. TI Prospects for detecting the 21 cm forest from the diffuse intergalactic medium with LOFAR SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; dark ages, reionization, first stars; radio astronomy; radio continuum: general; radio lines: general ID HIGH-REDSHIFT; RADIATIVE-TRANSFER; CENTIMETER TOMOGRAPHY; COSMIC REIONIZATION; 21-CM EMISSION; LY-ALPHA; EPOCH; ABSORPTION; FLUCTUATIONS; FOREGROUNDS AB We discuss the feasibility of the detection of the 21 cm forest in the diffuse intergalactic medium (IGM) with the radio telescope LOFAR. The optical depth to the 21 cm line has been derived using simulations of reionization which include detailed radiative transfer of ionizing photons. We find that the spectra from reionization models with similar total comoving hydrogen ionizing emissivity but different frequency distribution look remarkably similar. Thus, unless the reionization histories are very different from each other (e.g. a predominance of UV versus X-ray heating) we do not expect to distinguish them by means of observations of the 21 cm forest. Because the presence of a strong X-ray background would make the detection of the 21 cm line absorption impossible, the lack of absorption could be used as a probe of the presence/intensity of the X-ray background and the thermal history of the Universe. Along a random line of sight LOFAR could detect a global suppression of the spectrum from z greater than or similar to 12, when the IGM is still mostly neutral and cold, in contrast with the more well-defined, albeit broad, absorption features visible at lower redshift. Sharp, strong absorption features associated with rare, high-density pockets of gas could also be detected at z similar to 7 along preferential lines of sight. C1 [Ciardi, B.; Graziani, L.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Labropoulos, P.; Brentjens, M.; de Bruyn, A. G.; Jelic, V.; Pandey, V. N.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Maselli, A.] Autonomous Univ Barcelona, EVENT Lab Neurosci & Technol, E-08035 Barcelona, Spain. [Thomas, R.; Yatawatta, S.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Zaroubi, S.; de Bruyn, A. G.; Daiboo, S.; Kazemi, S.; Koopmans, L. V. E.; Martinez, O.; Offringa, A. R.; Pandey, V. N.; Veligatla, V.; Vedantham, H.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bolton, J. S.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harker, G. J. A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Mellema, G.] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Mellema, G.] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Schaye, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Ciardi, B (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM saleem@astro.rug.nl RI Jelic, Vibor/B-2938-2014; Mellema, Garrelt/K-4962-2014; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Yatawatta, Sarod/E-6037-2013; OI Schaye, Joop/0000-0002-0668-5560; Jelic, Vibor/0000-0002-6034-8610; Mellema, Garrelt/0000-0002-2512-6748; Harker, Geraint/0000-0002-7894-4082; Graziani, Luca/0000-0002-9231-1505; Yatawatta, Sarod/0000-0001-5619-4017; Bolton, James/0000-0003-2764-8248 FU DFG [1177, 1573]; NASA Lunar Science Institute [NNA09DB30A]; European Research Council under ERC [FIRSTLIGHT 258942] FX The authors would like to thank an anonymous referee for his/her comments. This work was supported by DFG Priority Programs 1177 and 1573. GH is a member of the LUNAR consortium, which is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. LVEK, HV and SD acknowledge the financial support from the European Research Council under ERC-Starting Grant FIRSTLIGHT 258942. NR 48 TC 9 Z9 9 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 2 BP 1755 EP 1765 DI 10.1093/mnras/sts156 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QO UT WOS:000318229000063 ER PT B AU Gingerich, O AF Gingerich, Owen BA Way, MJ Hunter, D BF Way, MJ Hunter, D TI The Critical Importance of Russell's Diagram SO ORIGINS OF THE EXPANDING UNIVERSE: 1912-1932 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Origins of the Expanding Universe 1912-1932 CY SEP 13-15, 2012 CL Flagstaff, AZ ID CEPHEID VARIATION; MAGNITUDES; CLUSTERS; COLORS AB The idea of dwarf and giants stars, but not the nomenclature, was first established by Eijnar Hertzsprung in 1905; his first diagrams in support appeared in 1911. In 1913 Henry Norris Russell could demonstrate the effect far more strikingly because he measured the parallaxes of many stars at Cambridge, and could plot absolute magnitude against spectral type for many points. The general concept of dwarf and giant stars was essential in the galactic structure work of Harlow Shapley, Russell's first graduate student. In order to calibrate the period-luminosity relation of Cepheid variables, he was obliged to fall back on statistical parallax using only 11 Cepheids, a very sparse sample. Here the insight provided by the Russell diagram became critical. The presence of yellow K giant stars in globular clusters credentialed his calibration of the period-luminosity relation by showing that the calibrated luminosity of the Cepheids was comparable to the luminosity of the K giants. It is well known that in 1920 Shapley did not believe in the cosmological distances of Heber Curtis' spiral nebulae. It is not so well known that in 1920 Curtis' plot of the period-luminosity relation suggests that he didn't believe it was a physical relation and also he failed to appreciate the significance of the Russell diagram for understanding the large size of the Milky Way. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 27 TC 0 Z9 0 U1 1 U2 2 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-826-8 J9 ASTR SOC P PY 2013 VL 471 BP 205 EP 215 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ27 UT WOS:000320095400013 ER PT B AU DeVorkin, D AF DeVorkin, David BA Way, MJ Hunter, D BF Way, MJ Hunter, D TI Henry Norris Russell and the Expanding Universe SO ORIGINS OF THE EXPANDING UNIVERSE: 1912-1932 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Conference on Origins of the Expanding Universe 1912-1932 CY SEP 13-15, 2012 CL Flagstaff, AZ ID SCIENCE AB Henry Norris Russell, one of the most influential American astronomers of the first half of the 20th Century, had a special place in his heart for the Lowell Observatory. Although privately critical of the founder for his pronouncements about life on Mars and the superiority of the Mars Hill observing site, he always supported the Observatory in public and professional circles. He staunchly supported Tombaugh's detection of a planet as leading from Lowell's prediction, and always promoted V. M. Slipher's spectroscopic investigations of planetary and stellar phenomena. But how did he react to Slipher's puzzling detection of the extreme radial velocities of spiral nebulae starting in 1912, and how did he regard the extension and interpretation of those observations by Hubble and others in following decades? Here we describe the arc of Russell's reactions, dating from Slipher's first detection, as an indicator of how mainstream stellar astronomers reacted to the concept of an expanding universe. C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP DeVorkin, D (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 54 TC 0 Z9 0 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-826-8 J9 ASTR SOC P PY 2013 VL 471 BP 217 EP 233 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ27 UT WOS:000320095400014 ER PT J AU Robbins, RK Glassberg, J AF Robbins, Robert K. Glassberg, Jeffrey TI A butterfly with olive green eyes discovered in the United States and the Neotropics (Lepidoptera, Lycaenidae, Eumaeini) SO ZOOKEYS LA English DT Article DE Butterfly Eye Color; Curacao; Isla Margarita; Ministrymon azia; Ministrymon janevicroy; Vicroy's Ministreak ID SEXUAL SELECTION; THECLINAE; EVOLUTION AB We describe Ministrymon janevicroy Glassberg, sp. n., from the United States (Texas). Its wing pattern closely resembles that of the widespread and well-known lycaenid, Ministrymon azia (Hewitson). The new species is distinguished by the structure of its male and female genitalia, by the patterning of the ground color on the basal half of the ventral hindwing surface, and by the color of its eyes. Adults of Ministrymon janevicroy in nature have olive green eyes in contrast to the dark brown/black eyes of M. azia. Ministrymon janevicroy occurs in dry deciduous forest and scrub from the United States (Texas) to Costa Rica (Guanacaste) with disjunct populations on Curacao and Isla Margarita (Venezuela). In contrast, M. azia occurs from the United States to southern Brazil and Chile in both dry and wet lowland habitats. Nomenclaturally, we remove the name Electrostrymon grumus K. Johnson & Kroenlein, 1993, from the synonymy of M. azia (where it had been listed as a synonym of Ministrymon hernandezi Schwartz & K. Johnson, 1992). We accord priority to Angulopis hernandezi K. Johnson & Kroenlein, 1993 over Electrostrymon grumus K. Johnson & Kroenlein, 1993, syn. n., which currently is placed in Ziegleria K. Johnson, 1993. The English name Vicroy's Ministreak is proposed for M. janevicroy. We update biological records of dispersal and caterpillar food plants, previously attributed to M. azia, in light of the new taxonomy. C1 [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Glassberg, Jeffrey] North Amer Butterfly Assoc, Morristown, NJ 07960 USA. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 105,E-514, Washington, DC 20013 USA. EM RobbinsR@SI.edu NR 51 TC 3 Z9 3 U1 0 U2 7 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 305 BP 1 EP 20 DI 10.3897/zookeys.305.5081 PG 20 WC Zoology SC Zoology GA 155HZ UT WOS:000319739900001 PM 23794910 ER PT J AU Baldwin, CC Robertson, DR AF Baldwin, Carole C. Ross Robertson, D. TI A new Haptoclinus blenny (Teleostei, Labrisomidae) from deep reefs off Curacao, southern Caribbean, with comments on relationships of the genus SO ZOOKEYS LA English DT Article DE Blenniiformes; submersible; Substation Curacao; Haptoclinus apectolophus; Deep Reef Observation Project (DROP) ID CLINID FISH; PERCIFORMES; FAMILIES AB A second species of the blenniiform genus Haptoclinus is described from deep reefs off Curacao, southern Caribbean. Haptoclinus dropi sp. n. differs from the northwestern Caribbean H. apectolophus Bohlke and Robins, 1974, in having 29 total dorsal-fin elements-III-I-XIII, 12 (vs. 31-III-I-XIV, 13 or III-I-XIII, 14); 19 anal-fin soft rays (vs. 20-21); 12 pectoral-fin rays (vs. 13); 12 precaudal vertebrae (vs. 13); and the first dorsal-fin spine longer than the second (vs. the second longer than the first). It further differs from H. apectolophus in lacking scales (vs. three-quarters of body densely scaled), in having a distinctive pattern of spotting on the trunk and fins in preservative (vs. no spotting), and in lacking a fleshy flap on the anterior rim of the posterior nostril (vs. flap present). Color in life is unknown for H. apectolophus, and the color description presented for the new species constitutes the first color information for the genus. Familial placement of Haptoclinus remains questionable, but the limited relevant information obtained from morphological examination of the new species provides additional support for a close relationship with the Chaenopsidae. Haptoclinus dropi represents one of numerous new teleost species emerging from sampling to 300 m off Curacao as part of the Smithsonian Institution's Deep Reef Observation Project (DROP). C1 [Baldwin, Carole C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Ross Robertson, D.] Smithsonian Trop Res Inst, Balboa, Panama. RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM baldwinc@si.edu FU Consortium for Understanding and Sustaining a Biodiverse Planet; National Geographic Society's Committee for Research and Exploration [9102-12] FX We thank Adriaan (Dutch) Schrier, Cristina Castillo, Bruce Brandt, Barbara van Bebber, Laureen Schenk, Lee Weigt, and Amy Driskell for assistance in the field; Sandra Raredon and Ian Silver-Gorges for providing the radiograph and images of the preserved holotype; and Mark Sabaj Perez for sending the type material of H. apectolophus on loan to the first author. Funding for the Smithsonian Institution's Deep Reef Observation Project is provided internally by the Consortium for Understanding and Sustaining a Biodiverse Planet and by National Geographic Society's Committee for Research and Exploration (Grant #9102-12). Victor Springer, Philip Hastings, and Jeffrey Williams provided helpful comments on drafts of this manuscript. NR 13 TC 13 Z9 13 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 306 BP 71 EP 81 DI 10.3897/zookeys.306.5198 PG 11 WC Zoology SC Zoology GA 157LT UT WOS:000319898300005 PM 23794919 ER PT J AU Tereszchuk, KA Abad, GG Clerbaux, C Hadji-Lazaro, J Hurtmans, D Coheur, PF Bernath, PF AF Tereszchuk, K. A. Abad, G. Gonzalez Clerbaux, C. Hadji-Lazaro, J. Hurtmans, D. Coheur, P. -F. Bernath, P. F. TI ACE-FTS observations of pyrogenic trace species in boreal biomass burning plumes during BORTAS SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID FOREST-FIRE EMISSIONS; ATMOSPHERIC CHEMISTRY; ORGANIC-COMPOUNDS; AIRCRAFT; GASES; HCN; CO; POLLUTION; ARCTAS; OZONE AB To further our understanding of the effects of biomass burning emissions on atmospheric composition, the BORTAS campaign (BOReal forest fires on Tropospheric oxidants over the Atlantic using Aircraft and Satellites) was conducted on 12 July to 3 August 2011 during the boreal forest fire season in Canada. The simultaneous aerial, ground and satellite measurement campaign sought to record instances of boreal biomass burning to measure the tropospheric volume mixing ratios (VMRs) of short- and long-lived trace molecular species from biomass burning emissions. The goal was to investigate the connection between the composition and the distribution of these pyrogenic outflows and their resulting perturbation to atmospheric chemistry, with particular focus on oxidant species to determine the overall impact on the oxidizing capacity of the free troposphere. Measurements of pyrogenic trace species in boreal biomass burning plumes were made by the Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE-FTS) onboard the Canadian Space Agency (CSA) SCISAT-1 satellite during the BORTAS campaign. Even though biomass burning emissions are typically confined to the boundary layer, outflows are often injected into the upper troposphere by isolated convection and fire-related convective processes, thus allowing space-borne instruments to measure these pyrogenic outflows. An extensive set of 14 molecules - CH3OH, C2H2, C2H6, C3H6O, CO, HCN, HCOOH, HNO3, H2CO, NO, NO2, OCS, O-3, and PAN - have been analysed. Included in this analysis is the calculation of age-dependent sets of enhancement ratios for each of the species originating from fires in North America (Canada, Alaska) and Siberia for a period of up to 7 days. Ratio values for the shorter lived primary pyrogenic species decrease over time primarily due to oxidation by the OH radical as the plume ages and values for longer lived species such as HCN and C2H6 remain relatively unchanged. Increasing negative values are observed for the oxidant species, including O-3, indicating a destruction process in the plume as it ages such that concentrations of the oxidant species have dropped below their off-plume values. Results from previous campaigns have indicated that values for the molar ratios of Delta O-3/Delta CO obtained from the measurements of the pyrogenic outflow from boreal fires are highly variable and range from negative to positive, irrespective of plume age. This variability has been attributed to pollution effects where the pyrogenic outflows have mixed with either local urban NOx emissions or pyrogenic emissions from the long-range transport of older plumes, thus affecting the production of O-3 within the plumes. The results from this study have identified another potential cause of the variability in O-3 concentrations observed in the measurements of biomass burning emissions, where evidence of stratosphere-troposphere exchange due to the pyroconvective updrafts from fires has been identified. Perturbations caused by the lofted emissions in these fire-aided convective processes may result in the intrusion of stratospheric air masses into the free troposphere and subsequent mixing of stratospheric O-3 into the pyrogenic outflows causing fluctuations in observed Delta O-3/Delta CO molar ratios. C1 [Tereszchuk, K. A.; Abad, G. Gonzalez; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Clerbaux, C.] Univ Paris 06, Univ Versailles St Quentin, CNRS INSU, LATMOS IPSL, Paris, France. [Clerbaux, C.; Hadji-Lazaro, J.; Hurtmans, D.; Coheur, P. -F.] ULB, Serv Chim Quant & Photophys, Brussels, Belgium. [Abad, G. Gonzalez] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Bernath, P. F.] Old Dominion Univ, Dept Chem & Biochem, Norfolk, VA 23529 USA. RP Tereszchuk, KA (reprint author), Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. EM keith.tereszchuk@york.ac.uk RI Bernath, Peter/B-6567-2012; clerbaux, cathy/I-5478-2013; OI Bernath, Peter/0000-0002-1255-396X; Gonzalez Abad, Gonzalo/0000-0002-8090-6480 FU Canadian Space Agency; Natural Environment Research Council of the United Kingdom [NE/F017391/1]; Wild Fund FX The ACE mission is funded primarily by the Canadian Space Agency. The authors would like to thank the Natural Environment Research Council of the United Kingdom for funding K. A. Tereszchuk through grant NE/F017391/1 and the Wild Fund for their support of G. Gonzalez Abad. The authors would like to further acknowledge the LATMOS research group for providing the Level 2 IASI CO data. IASI has been developed and built under the responsibility of the Centre National d'Etudes Spatiales (CNES, France). It is flown onboard the MetOp satellites as part of the Eumetsat Polar System. NR 35 TC 9 Z9 9 U1 2 U2 11 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2013 VL 13 IS 9 BP 4529 EP 4541 DI 10.5194/acp-13-4529-2013 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 144LR UT WOS:000318941300004 ER PT J AU Hastings, AK Bloch, JI Jaramillo, CA Rincon, AF Macfadden, BJ AF Hastings, Alexander K. Bloch, Jonathan I. Jaramillo, Carlos A. Rincon, Aldo F. Macfadden, Bruce J. TI SYSTEMATICS AND BIOGEOGRAPHY OF CROCODYLIANS FROM THE MIOCENE OF PANAMA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID SOUTH-AMERICA; ALLIGATOR-MISSISSIPPIENSIS; CAIMAN-CROCODILUS; DISPERSAL; EOCENE; PERSPECTIVE; ARCHOSAURS; COLLISION; PLIOCENE; ISTHMUS AB Despite the fact that fossil crocodylians have been recovered from the Panama Canal Zone starting with initial excavations in 1912, detailed studies have been lacking. Recent excavations of the canal have resulted in new discoveries of many vertebrate fossils, including the first known Miocene crocodylian skulls from Central America. These fossil skulls from the early-middle Miocene represent two new taxa with distinct morphology that is shared with extinct and extant caimans (Caimaninae). A cladistic analysis of 32 alligatorid and three outgroup taxa, scored for 75 characters, resulted in 1210 equally most parsimonious cladograms, all of which suggest that Culebrasuchus mesoamericanus, gen. et sp. nov., is the sister taxon to all previously known Caimaninae. Additionally, the analysis suggests that Centenariosuchus gilmorei, gen. et sp. nov., is the sister taxon to a caimanine clade that includes Purussaurus from the Miocene of South America. In fact, teeth very similar to those of Purussaurus have also been recovered from the Panama Canal. Given these South American affinities, we suggest that these early caimanines dispersed across saltwater. This is a potentially surprising result, because all extant alligatorids lack the salt glands that would have been necessary for the marine dispersal required to reach Central America during the Miocene. Unlike Miocene mammals that all have North American affinities, the Miocene crocodylians of Panama represent a 'melting pot' with taxa of disparate origins living together at the southern extreme of Central America. C1 [Hastings, Alexander K.; Bloch, Jonathan I.; Rincon, Aldo F.; Macfadden, Bruce J.] Univ Florida, Dept Geol Sci, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Jaramillo, Carlos A.; Rincon, Aldo F.] Smithsonian Trop Res Inst, Ancon 084303092, Panama. RP Hastings, AK (reprint author), Univ Florida, Dept Geol Sci, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM akh@ufl.edu OI Bloch, Jonathan/0000-0003-1484-6931 FU Smithsonian Tropical Research Institute (STRI); Florida Museum of Natural History (FLMNH); U.S. National Science Foundation Partnerships in International Research and Education grant [0966884, EAR 0824299, EAR 0418042]; Autoridad del Canal de Panama; Mark Tupper Fellowship; Ricardo Perez SA; Smithsonian Institute FX We would like to thank the Smithsonian Tropical Research Institute (STRI) and Florida Museum of Natural History (FLMNH) for support and assistance with the research project and for collection of the fossil described here. The accomplishment of this project was possible thanks to the support of the U.S. National Science Foundation Partnerships in International Research and Education grant 0966884 (OISE, EAR, DRL), EAR 0824299, and EAR 0418042; the Autoridad del Canal de Panama; the Mark Tupper Fellowship; Ricardo Perez SA; and the Smithsonian Institute. Thanks to U. Denetclaw for collection of the holotype of Centenariosuchus gilmorei and L. Grawe-Desantis for collection of one of the longirostrine dentary sections (UF 259873). Thanks to J. Bourque for excellent preparation of the holotype and paratype specimens and to K. Rowe and J. Nestler for research assistance. Thanks to M. Brett-Surman (USNM), R. Hulbert (FLMNH), and D. Winkler (SMU) for access to, and assistance with, collections. NR 88 TC 19 Z9 21 U1 2 U2 15 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2013 VL 33 IS 2 BP 239 EP 263 DI 10.1080/02724634.2012.713814 PG 25 WC Paleontology SC Paleontology GA 152XD UT WOS:000319564300001 ER PT J AU Oreska, MPJ Carrano, MT Dzikiewicz, KM AF Oreska, Matthew P. J. Carrano, Matthew T. Dzikiewicz, Katherine M. TI VERTEBRATE PALEONTOLOGY OF THE CLOVERLY FORMATION (LOWER CRETACEOUS), I: FAUNAL COMPOSITION, BIOGEOGRAPHIC RELATIONSHIPS, AND SAMPLING SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID CEDAR-MOUNTAIN FORMATION; NORTH-AMERICA; MULTITUBERCULATE MAMMALS; AMPHIBIAN ALBANERPETON; TRICONODONT MAMMALS; WILLWOOD FORMATION; CENTRAL MONTANA; RIVER FORMATION; LOWER EOCENE; LOCAL FAUNA AB The vertebrate fauna of the Cloverly Formation has been studied for more than 75 years, but remains poorly sampled and incompletely understood. We undertook an extensive survey of the formation that resulted in the discovery of several new, highly productive vertebrate microfossil bonebeds (VMBs). Comprehensive sampling of these and other sites has nearly doubled the known vertebrate diversity of the Cloverly Formation. In addition to the comparatively well-known dinosaurs, this augmented faunal list includes hybodontoid sharks, numerous bony fishes, three lissamphibian lineages, lizards, multiple crocodylians, and several new mammal occurrences. The known Cloverly vertebrate fauna now more closely resembles those of other late Early Cretaceous formations in North America, indicating broad similarities across wide geographic areas at this time. In addition, this work underscores the important role VMBs can play in areas previously studied primarily through surface prospecting and quarrying, especially for assessing paleoecology and species diversity. C1 [Oreska, Matthew P. J.; Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Dzikiewicz, Katherine M.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. RP Carrano, MT (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM mpo4zx@virginia.edu; carranom@si.edu; kmdzikie@ncsu.edu RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 FU Smithsonian Institution through a Walcott Grant; NMNH Equipment Fund FX We are very grateful for the extensive efforts of S. Jabo and P. Kroehler (Smithsonian Institution) during several years of fieldwork and fossil preparation for this project. R. Lockwood and J. Swaddle provided important guidance to M.P.J.O. during an earlier phase of this project. F. Grady picked most of the fossil materials from the matrix; M. Brett-Surman and M. Florence helped with specimen cataloguing and databasing; S. Whittaker supervised SEM work; M. Fox and C. Norris provided access to the YPM collections. Numerous others provided important assistance, including E. Duneman, C. Gruet, M. Gruet, J. Guibord, R. Hill, A. Massagli, S. McIntyre, J. Mitchell, S. Moran, C. Peredo, and J. Velez-Juarbe as well as M. Coffey, P. Lopez, and R. Horace-Middleton under the collaborative supervision of G. Wesley-Hunt (Montgomery College). We thank C. Manuel, R. Manuel, and E. Kvale for their invaluable advice, support, and hospitality. This work was supported by the Smithsonian Institution through a Walcott Grant and two Small Grants to M.T.C., as well as the NMNH Equipment Fund. Finally, we thank D. Brinkman and S. Sweetman for their detailed, insightful reviews that led to several significant improvements in this paper. NR 155 TC 12 Z9 13 U1 0 U2 2 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2013 VL 33 IS 2 BP 264 EP 292 DI 10.1080/02724634.2012.717567 PG 29 WC Paleontology SC Paleontology GA 152XD UT WOS:000319564300002 ER PT J AU Rincon, AF Bloch, JI Macfadden, BJ Jaramillo, CA AF Rincon, Aldo F. Bloch, Jonathan I. Macfadden, Bruce J. Jaramillo, Carlos A. TI FIRST CENTRAL AMERICAN RECORD OF ANTHRACOTHERIIDAE (MAMMALIA, BOTHRIODONTINAE) FROM THE EARLY MIOCENE OF PANAMA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID HELOHYIDAE ARTIODACTYLA; NORTH-AMERICA; LAND; HIPPOPOTAMIDAE; EMERGENCE; EVOLUTION; EOCENE; CETARTIODACTYLA; BIOSTRATIGRAPHY; HYPSODONTY AB A new species of bothriodontine anthracothere, Arretotherium meridionale, is described from the early Miocene (Arikareean North America Land Mammal Age) Las Cascadas fossil assemblage in Panama, Central America. Fossils of A. meridionale are the first record of an anthracothere from the New World Tropics. Among anthracotheres, A. meridionale is most similar to A. acridens from the middle Arikareean from Texas in having a relatively deep and robust jaw, high and sharp cusps on the lower molars, short c-p1 diastema, and absence of a mesiolingual metacristid. A. meridionale differs from other species in being generally larger, two lower incisors (rather than three), prehypocristid never reaching the postprotocristid, more apical junction between postprotocristid and postmetacristid, mesiolingual entocristid transversely notching preentocrisitid, and transverse valley tapered lingually by prehypocristid. Although cladistic analysis of 28 anthracotheriids coded for 51 characters supports a relationship between A. meridionale and A. acridens, some presumably convergent dental characteristics are also similar to certain Oligocene-Miocene Eurasian bothriodontines. The presence of Arretotherium in the Las Cascadas Formation in Panama, and absence in the later Centenario Fauna, shows that primitive bothriodontines entered into Central America by the early Miocene before disappearing from the New World during the late early-middle Miocene. C1 [Rincon, Aldo F.; Bloch, Jonathan I.; Macfadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Rincon, AF (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM arincon@ufl.edu; jbloch@flmnh.ufl.edu; bmacfadd@flmnh.ufl.edu; jaramilloc@si.edu OI Bloch, Jonathan/0000-0003-1484-6931 FU University of Florida Research Opportunity Grant; U.S. National Science Foundation Partnerships in International Research and Education [0966884, EAR 0824299, EAR 0418042]; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; Ricardo Perez Toyota, Panama FX We thank J. Bourque at FLMNH, who prepared the specimens in the laboratory; J. Schiebout and S. Ting at the Louisiana State University Department of Geology for access to relevant research collections; M. Warren at C.A. Pound Human Identification Laboratory (University of Florida) for access to the X-ray equipment; C. Montes, S. Suarez, M. Vallejo, and F. Moreno (STRI) who helped in the collection of the specimens; R. Hulbert Jr. for help with anatomical terminology and taxonomic nomenclature; F. Lihoreau and B. Shockey for help with the phylogenetic character matrix; and C. Manz, L. Oviedo, K. Cummings, E. Woodruff, F. Herrera, A. Hastings, and J. Pardo, who edited an earlier version of the manuscript and made helpful comments for its improvement. We thank the Panama Canal Authority (ACP) and the Ministerio de Comercio e Industria (MICI) for assess to relevant fossil sites. This research was supported by University of Florida Research Opportunity Grant; the U.S. National Science Foundation Partnerships in International Research and Education grant 0966884 (OISE, EAR, DRL), EAR 0824299, and EAR 0418042; STRI-Tupper Paleontological Fund; STRI-Panama Canal Authority Fund; and Ricardo Perez Toyota, Panama. This is a University of Florida Contribution to Paleobiology number 643. NR 62 TC 7 Z9 8 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0272-4634 EI 1937-2809 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PY 2013 VL 33 IS 2 BP 421 EP 433 DI 10.1080/02724634.2013.722573 PG 13 WC Paleontology SC Paleontology GA 152XD UT WOS:000319564300012 ER PT J AU van Noort, S Buffington, ML AF van Noort, Simon Buffington, Matthew L. TI Revision of the Afrotropical Mayrellinae (Cynipoidea, Liopteridae), with the first record of Paramblynotus from Madagascar SO JOURNAL OF HYMENOPTERA RESEARCH LA English DT Article DE Africa; Afrotropical region; Cynipoidea; Hymenoptera; identification key; Liopteridae; Madagascar; Mayrellinae; systematics ID FIG WASPS; HYMENOPTERA; HISTORY AB The liopterid subfamily Mayrellinae is revised for the Afrotropical region including the description of the following nine new species of Paramblynotus Cameron: Paramblynotus alexandriensis Buffington & van Noort sp. n.; Paramblynotus bayangensis van Noort & Buffington sp. n.; Paramblynotus behara van Noort & Buffington sp. n.; Paramblynotus dzangasangha van Noort & Buffington sp. n.; Paramblynotus matele van Noort & Buffington sp. n.; Paramblynotus parinari Buffington & van Noort sp. n.; Paramblynotus ruvubuensis van Noort & Buffington sp. n..; Paramblynotus seyrigi van Noort & Buffington sp. n.; Paramblynotus zohy van Noort & Buffington sp. n. The genus Paramblynotus is recorded from Madagascar for the first time, with representatives of two species-groups being present on the island: the Paramblynotus yangambicolous species-group and the new Paramblynotus seyrigi species-group, which we erect here to accommodate a single, but highly distinctive new species possessing apomorphic character states. The latter species-group is possibly endemic to Madagascar. We provide identification keys to the species-groups and species occurring in the Afrotropical region. Online dichotomous and interactive Lucid keys are available at http://www.waspweb.org/Cynipoidea/Keys/index.htm C1 [van Noort, Simon] Iziko South African Museum, Nat Hist Dept, ZA-8000 Cape Town, South Africa. [van Noort, Simon] Univ Cape Town, Dept Zool, ZA-7701 Rondebosch, South Africa. [Buffington, Matthew L.] USDA, Systemat Entomol Lab, Smithsonian NMNH, Washington, DC 20013 USA. RP van Noort, S (reprint author), Iziko South African Museum, Nat Hist Dept, POB 61, ZA-8000 Cape Town, South Africa. EM svannoort@iziko.org.za RI van Noort, Simon/C-4006-2017 OI van Noort, Simon/0000-0001-6930-9741 FU South African National Research Foundation [GUN 2068865, GUN 61497, GUN 79004, GUN 79211, GUN 81139]; Systematic Entomology Lab, USDA/ARS; World Wildlife Fund (US) FX SVN was funded by South African National Research Foundation grants: GUN 2068865; GUN 61497; GUN 79004; GUN 79211; GUN 81139. MLB was funded by the Systematic Entomology Lab, USDA/ARS. The expedition to the Central African Republic was supported by funds from the World Wildlife Fund (US). The Ugandan Wildlife Authority and UNCST provided permits to conduct research in Uganda. We thank Dr. Richard Bagine, Director of Research, Kenya Wildlife Service for granting R. S. Copeland permission to sample in Kenyan National Parks and Reserves. Dr. Helida Oyieke, Head of Collections and Research, National Museums of Kenya, was instrumental in granting permission to loan insects for study. We thank Mattias Forshage (Swedish Museum of Natural History) for his careful review of the manuscript including numerous helpful suggestions and Istvan Miko (Pennsylvania State University) for formulating the URI table. We also acknowledge MorphBank (http://www.morphbank.net), Florida State University, School of Computational Science, Tallahassee, FL 32306-4026, USA. The USDA is an equal provider and employer. NR 42 TC 3 Z9 3 U1 0 U2 2 PU PENSOFT PUBL PI SOFIA PA 12 PROF GEORGI ZLATARSKI ST, SOFIA, 1700, BULGARIA SN 1070-9428 EI 1314-2607 J9 J HYMENOPT RES JI J. Hymenopt. Res. PY 2013 VL 31 BP 1 EP 64 DI 10.3897/JHR.31.4072 PG 64 WC Entomology SC Entomology GA 140OU UT WOS:000318665600001 ER PT J AU Villepastour, A AF Villepastour, Amanda BE Hellier, R TI Amelia Pedroso The Voice of a Cuban Priestess Leading from the Inside SO WOMEN SINGERS IN GLOBAL CONTEXTS: MUSIC, BIOGRAPHY, IDENTITY LA English DT Article; Book Chapter C1 [Villepastour, Amanda] Univ London Goldsmiths Coll, London SE14 6NW, England. [Villepastour, Amanda] Univ London, London WC1E 7HU, England. [Villepastour, Amanda] Smithsonian Inst, Washington, DC 20560 USA. [Villepastour, Amanda] Bowling Green State Univ, Bowling Green, OH 43403 USA. RP Villepastour, A (reprint author), Cardiff Univ, Cardiff CF10 3AX, S Glam, Wales. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV ILLINOIS PRESS PI URBANA PA URBANA, IL 61801 USA BN 978-0-252-09436-1 PY 2013 BP 54 EP 72 PG 19 WC Music; Women's Studies SC Music; Women's Studies GA BET30 UT WOS:000318013900003 ER PT J AU Muscarella, R Uriarte, M Forero-Montana, J Comita, LS Swenson, NG Thompson, J Nytch, CJ Jonckheere, I Zimmerman, JK AF Muscarella, Robert Uriarte, Maria Forero-Montana, Jimena Comita, Liza S. Swenson, Nathan G. Thompson, Jill Nytch, Christopher J. Jonckheere, Inge Zimmerman, Jess K. TI Life-history trade-offs during the seed-to-seedling transition in a subtropical wet forest community SO JOURNAL OF ECOLOGY LA English DT Article DE life-history trade-offs; Luquillo; plant population and community dynamics; Puerto Rico; regeneration niche; seed and seedling establishment limitation; successional niche ID LAND-USE HISTORY; TROPICAL FOREST; PUERTO-RICO; HURRICANE HUGO; NEOTROPICAL PIONEERS; NATURAL DISTURBANCE; REGENERATION NICHE; LIANA ABUNDANCE; RAIN-FORESTS; LEAF-LITTER AB 1. The transition from seed to established seedling (STS) represents a major bottleneck in plant demography with implications for community dynamics and the maintenance of species diversity. The relative strength of seed limitation versus seedling establishment limitation can reveal life-history trade-offs that contribute to the maintenance of community diversity. If seed limitation dominates, chance arrival to open sites may play a key role in maintaining diversity. If seedling establishment limitation dominates, however, species relative abundances may depend more on tolerance to environmental and biotic conditions during seedling establishment (i.e. species-specific regeneration niche). 2. We used three years of seed rain and seedling recruitment data for 19 species of tropical woody plants collected in the Luquillo Forest Dynamics Plot in Puerto Rico to (i) examine a trade-off between seed and seedling establishment limitation and (ii) quantify the biotic and abiotic factors that mediate the STS transition. 3. We did not find evidence of a life-history trade-off in the form of a negative correlation between seed and seedling establishment limitation. However, species varied considerably in the relative levels of seed and seedling establishment limitation they displayed. Seed mass correlated negatively with seedling establishment limitation but not with seed limitation. We found striking differences in STS transition between life-forms categorized as trees (including two palms) and lianas; lianas exhibited significantly higher STS transition rates than trees. 4. The biotic and abiotic variables most strongly associated with successful STS transition differed between life-forms. For trees, conspecific seed density and temporal fruiting concentration had negative effects on seedling establishment, while seed mass had a positive effect. A significant interaction between leaf litter input at a plot and seed size suggested that large-seeded species had higher STS transition probability in plots with more leaf litter biomass. This effect was reversed for small-seeded species. For lianas, leaf litter had a negative effect on STS transition and temporal fruiting concentration had a positive effect. 5. Synthesis. Our analyses demonstrate the multidimensional axes of regeneration niches and how they can be related to seed size. Long-term data sets are critical for understanding these relationships because the relevant factors vary along large spatial and temporal scales. C1 [Muscarella, Robert; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Forero-Montana, Jimena; Thompson, Jill; Nytch, Christopher J.; Zimmerman, Jess K.] Univ Puerto Rico, Dept Environm Sci, San Juan, PR 00936 USA. [Comita, Liza S.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Thompson, Jill] Ctr Ecol & Hydrol Edinburgh, Penicuik EH26 0QB, Midlothian, Scotland. [Jonckheere, Inge] FAO United Nations, Forestry Dept FOMR, UN REDD, Rome, Italy. RP Muscarella, R (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. EM bob.muscarella@gmail.com RI Uriarte, Maria/L-8944-2013; Thompson, Jill/K-2200-2012; OI Thompson, Jill/0000-0002-4370-2593; Comita, Liza/0000-0002-9169-1331 FU NSF [DEB-0516066, DEB-0614659, DEB-0620910, DEB-0218039]; US Forest Service; University of Puerto Rico FX This work was supported by NSF grants DEB-0516066 and DEB-0614659, which supported tree and seed/seedling censuses, respectively, and grants DEB-0620910 and DEB-0218039 from NSF to the Institute for Tropical Ecosystem Studies, University of Puerto Rico, working with the International Institute of Tropical Forestry (USDA Forest Service), for the Luquillo Long-Term Ecological Research Program. The US Forest Service and the University of Puerto Rico provided additional support. Many thanks to the numerous members of seedling survey field crews and the El Verde field station technicians Maroa Aponte, John Bithorn, Samuel Matta, Jose Rivera, Nereida Ramirez, Rebecca de Jesus and Paola Olaya for their data collection efforts. This manuscript was improved by comments of the editors and several referees. The authors have no conflict of interest to declare. NR 67 TC 10 Z9 11 U1 6 U2 71 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD JAN PY 2013 VL 101 IS 1 BP 171 EP 182 DI 10.1111/1365-2745.12027 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 130MQ UT WOS:000317922200019 ER PT J AU Penna, RF Sadowski, A Kulkarni, AK Narayan, R AF Penna, Robert F. Sadowski, Aleksander Kulkarni, Akshay K. Narayan, Ramesh TI The Shakura-Sunyaev viscosity prescription with variable alpha(r) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; gravitation; hydrodynamics; MHD ID ANGULAR-MOMENTUM TRANSPORT; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; BLACK-HOLE SPIN; ADVECTION-DOMINATED ACCRETION; WEAKLY MAGNETIZED DISKS; MARGINALLY STABLE ORBIT; LOCAL SHEAR INSTABILITY; MAGNETOROTATIONAL INSTABILITY; HYDROMAGNETIC TURBULENCE; GLOBAL SIMULATIONS AB Almost all hydrodynamic accretion disc models parametrize viscosity with the dimensionless parameter alpha. There is no detailed model for alpha, so it is usually taken to be a constant. However, global simulations of magnetohydrodynamic discs find that alpha varies with distance from the central object. Also, Newtonian simulations tend to find smaller alpha's than general relativistic simulations. We seek a one-dimensional model for alpha that can reproduce these two observations. We are guided by data from six general relativistic magnetohydrodynamic accretion disc simulations. The variation of a in the inner, laminar regions of the flow results from stretching of mean magnetic field lines by the flow. The variation of alpha in the outer, turbulent regions results from the dependence of the magnetorotational instability on the dimensionless shear rate. We give a one-dimensional prescription for alpha(r) that captures these two effects and reproduces the radial variation of alpha observed in the simulations. For thin discs, the prescription simplifies to the formula alpha( r) = 0.025[q(r)/1.5](6), where the shear parameter, q(r), is an analytical function of radius in the Kerr metric. The coefficient and exponent are inferred from our simulations and will change as better simulation data becomes available. We conclude that the alpha-viscosity prescription can be extended to the radially varying alpha's observed in simulations. It is possible that Newtonian simulations find smaller alpha's than general relativistic simulations because the shear parameter is lower in Newtonian flows. C1 [Penna, Robert F.; Sadowski, Aleksander; Kulkarni, Akshay K.; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Penna, RF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rpenna@cfa.harvard.edu FU NASA [NNX11AE16G]; NSF [AST-0805832] FX We thank Eric Blackman for discussions. This work was supported in part by NASA grant NNX11AE16G and NSF grant AST-0805832. The simulations presented in this work were performed in part on the Pleiades supercomputer, using resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. We also acknowledge NSF support via XSEDE resources at NICS Kraken and LoneStar. NR 68 TC 26 Z9 26 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2255 EP 2274 DI 10.1093/mnras/sts185 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700031 ER PT J AU Besla, G Hernquist, L Loeb, A AF Besla, Gurtina Hernquist, Lars Loeb, Abraham TI The origin of the microlensing events observed towards the LMC and the stellar counterpart of the Magellanic stream SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: micro; Magellanic Clouds; Galaxy: halo; galaxies: interactions; dark matter; galaxies: irregular ID GRAVITATIONAL LENSING EXPERIMENT.; SPACE-TELESCOPE OBSERVATIONS; DOMINATED GALACTIC HALO; STAR-FORMATION HISTORY; HIGH-VELOCITY CLOUDS; N-BODY SIMULATIONS; RR LYR STARS; MILKY-WAY; DARK-MATTER; PROPER-MOTION AB We introduce a novel theoretical model to explain the longstanding puzzle of the nature of the microlensing events reported towards the Large Magellanic Cloud (LMC) by the massive compact halo object (MACHO) and Optical Gravitational Lensing Experiment (OGLE) collaborations. We propose that a population of tidally stripped stars from the Small Magellanic Cloud (SMC) located similar to 4-10 kpc behind a lensing population of LMC disc stars can naturally explain the observed event durations (17-71 d), event frequencies and spatial distribution of the reported events. Differences in the event frequencies reported by the OGLE (similar to 0.33 yr(-1)) and MACHO (similar to 1.75 yr(-1)) surveys appear to be naturally accounted for by their different detection efficiencies and sensitivity to faint sources. The presented models of the Magellanic System were constructed without prior consideration of the microlensing implications. These results favour a scenario for the interaction history of the Magellanic Clouds, wherein the Clouds are on their first infall towards the Milky Way and the SMC has recently collided with the LMC 100-300 Myr ago, leading to a large number of faint sources distributed non-uniformly behind the LMC disc. In contrast to self-lensing models, microlensing events are also expected to occur in fields off the LMC's stellar bar since the stellar debris is not expected to be concentrated in the bar region. This scenario leads to a number of observational tests: the sources are low-metallicity SMC stars; they exhibit high velocities relative to LMC disc stars that may be detectable via proper motion studies and, most notably, there should exist a stellar counterpart to the gaseous Magellanic Stream and Bridge with a V-band surface brightness of >34 mag arcsec(-2). In particular, the stellar Bridge should contain enough RR Lyrae stars to be detected by the ongoing OGLE survey of this region. C1 [Besla, Gurtina] Columbia Univ, Dept Astron & Astrophys, New York, NY 10027 USA. [Hernquist, Lars; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Besla, G (reprint author), Columbia Univ, Dept Astron & Astrophys, 550 West 120th St, New York, NY 10027 USA. EM gbesla@astro.columbia.edu FU FAS Science Division Research Computing Group at Harvard University; NASA [HST-HF-51284.01-A, NNX08AL43G, NNA09DB30A]; NSF [AST-0907890] FX We thank Dave Bennett, Charles Alcock, Roeland P. van der Marel, Nitya Kallivayalil, Knut Olsen, Ed Olszewski, Tim Axelrod, Abi Saha, Kailash Sahu, Raja Guhathakurta, David Nidever, Dusan Keres, Kathryn Johnston, Ruben Sanchez-Janssen, Renyue Cen, Jenny Green and Martin Weinberg for useful discussions that have contributed to this paper. The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. GB acknowledges support from NASA through Hubble Fellowship grant HST-HF-51284.01-A. This work was also supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 134 TC 14 Z9 14 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2342 EP 2365 DI 10.1093/mnras/sts192 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700038 ER PT J AU Lundman, C Pe'er, A Ryde, F AF Lundman, C. Pe'er, A. Ryde, F. TI A theory of photospheric emission from relativistic, collimated outflows SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE plasmas; radiation mechanisms: thermal; radiative transfer; scattering; gamma-ray burst: general ID GAMMA-RAY-BURSTS; SPECTRAL CATALOG; PEAK ENERGY; NONTHERMAL EMISSION; FERMI OBSERVATIONS; THERMAL EMISSION; JETS; COMPONENT; MODEL; COLLAPSARS AB Relativistic outflows in the form of jets are common in many astrophysical objects. By their very nature, jets have angle-dependent velocity profiles, Gamma = Gamma(r,theta, phi), where Gamma is the outflow Lorentz factor. In this work we consider photospheric emission from non-dissipative jets with various Lorentz factor profiles, of the approximate form Gamma approximate to Gamma(0)/[(theta/theta(j))(p) + 1], where theta(j) is the characteristic jet opening angle. In collimated jets, the observed spectrum depends on the viewing angle, theta(v). We show that for narrow jets (theta(j)Gamma(0) less than or similar to few), the obtained low-energy photon index is alpha approximate to -1 (dN/dE alpha E-alpha), independent of viewing angle, and weakly dependent on the Lorentz factor gradient (p). A similar result is obtained for wider jets observed at theta(v) approximate to theta(j). This result is surprisingly similar to the average low-energy photon index seen in gamma-ray bursts. For wide jets (theta(j)Gamma(0) greater than or similar to few) observed at theta(v) << theta(j), a multicolour blackbody spectrum is obtained. We discuss the consequences of this theory on our understanding of the prompt emission in gamma-ray bursts. C1 [Lundman, C.; Ryde, F.] AlbaNova, Dept Phys, Royal Inst Technol KTH, SE-10691 Stockholm, Sweden. [Lundman, C.; Ryde, F.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Pe'er, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lundman, C (reprint author), AlbaNova, Dept Phys, Royal Inst Technol KTH, SE-10691 Stockholm, Sweden. EM clundman@particle.kth.se FU Fermi GI [41162] FX We would like to thank Peter Meszaros, Martin Rees and Bing Zhang for useful discussions. The Swedish National Space Board is acknowledged for financial support. AP wishes to acknowledge support from Fermi GI programme #41162. NR 50 TC 41 Z9 41 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2430 EP 2442 DI 10.1093/mnras/sts219 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700043 ER PT J AU Braito, V Ballo, L Reeves, JN Risaliti, G Ptak, A Turner, TJ AF Braito, V. Ballo, L. Reeves, J. N. Risaliti, G. Ptak, A. Turner, T. J. TI Decoupling absorption and continuum variability in the Seyfert 2 NGC 4507 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: NGC 4507; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; XMM-NEWTON; GALAXY NGC-4507; K-LINES; PDS 456; AGN; SUZAKU; ABSORBER; EMISSION AB We present the results of the Suzaku observation of the Seyfert 2 galaxy NGC 4507. This source is one of the X-ray brightest Compton-thin Seyfert 2s and a candidate for a variable absorber. Suzaku caught NGC 4507 in a highly absorbed state characterized by a high column density (N-H similar to 8 x 10(23) cm(-2)), a strong reflected component (R similar to 1.9) and a high equivalent width FeK alpha emission line (EW similar to 500 eV). The FeK alpha emission line is unresolved at the resolution of the Suzaku CCDs [sigma < 30 eV or full width at half-maximum (FWHM) < 3000 km s(-1)] and most likely originates in a distant absorber. The Fe K beta emission line is also clearly detected and its intensity is marginally higher than the theoretical value for low ionization Fe. A comparison with previous observations performed with XMM-Newton and BeppoSAX reveals that the X-ray spectral curvature changes on a time-scale of a few months. We analysed all these historical observations, with standard models as well as with a most recent model for a toroidal reprocessor and found that the main driver of the observed 2-10 keV spectral variability is a change of the line-of-sight obscuration, varying from similar to 4 x 10(23) to similar to 9 x 10(23) cm(-2). The primary continuum is also variable, although its photon index does not appear to vary, while the FeK alpha line and reflection component are consistent with being constant across the observations. This suggests the presence of a rather constant reprocessor and that the observed line-of-sight N-H variability is either due to a certain degree of clumpiness of the putative torus or due to the presence of a second clumpy absorber. C1 [Braito, V.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Ballo, L.] CSIC UC, Inst Fs Cantabria, E-39005 Santander, Spain. [Reeves, J. N.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Reeves, J. N.; Turner, T. J.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Ptak, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Braito, V (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, LC, Italy. EM valentina.braito@brera.inaf.it RI XRAY, SUZAKU/A-1808-2009; OI Braito, Valentina/0000-0002-2629-4989; Ballo, Lucia/0000-0002-5036-3497; Risaliti, Guido/0000-0002-3556-977X NR 77 TC 11 Z9 11 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2516 EP 2528 DI 10.1093/mnras/sts226 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700051 ER PT J AU Hayward, CC Narayanan, D Keres, D Jonsson, P Hopkins, PF Cox, TJ Hernquist, L AF Hayward, Christopher C. Narayanan, Desika Keres, Dusan Jonsson, Patrik Hopkins, Philip F. Cox, T. J. Hernquist, Lars TI Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution and implications for the IMF SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; stars: luminosity function, mass function; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID INITIAL MASS FUNCTION; STAR-FORMING GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; DEGREE EXTRAGALACTIC SURVEY; FAR-INFRARED PROPERTIES; MOVING-MESH COSMOLOGY; DEEP FIELD-SOUTH; SIMILAR-TO 2; SUPERMASSIVE BLACK-HOLES; AZTEC MILLIMETER SURVEY AB High-redshift submillimetre galaxies (SMGs) are some of the most rapidly star-forming galaxies in the Universe. Historically, galaxy formation models have had difficulty explaining the observed number counts of SMGs. We combine a semi-empirical model with 3D hydrodynamical simulations and 3D dust radiative transfer to predict the number counts of unlensed SMGs. Because the stellar mass functions, gas and dust masses, and sizes of our galaxies are constrained to match observations, we can isolate uncertainties related to the dynamical evolution of galaxy mergers and the dust radiative transfer. The number counts and redshift distributions predicted by our model agree well with observations. Isolated disc galaxies dominate the faint (S-1.1 less than or similar to 1 or S-850 less than or similar to 2 mJy) population. The brighter sources are a mix of merger-induced starbursts and galaxy-pair SMGs; the latter subpopulation accounts for similar to 30-50 per cent of all SMGs at all S-1.1 greater than or similar to 0.5mJy (S-850 greater than or similar to 1 mJy). The mean redshifts are similar to 3.0-3.5, depending on the flux cut, and the brightest sources tend to be at higher redshifts. Because the galaxy-pair SMGs will be resolved into multiple fainter sources by the Atacama Large Millimeter/submillimeter Array (ALMA), the bright ALMA counts should be as much as two times less than those observed using single-dish telescopes. The agreement between our model, which uses a Kroupa initial mass function (IMF), and observations suggests that the IMF in high-redshift starbursts need not be top heavy; if the IMF were top heavy, our model would overpredict the number counts. We conclude that the difficulty some models have reproducing the observed SMG counts is likely indicative of more general problems - such as an underprediction of the abundance of massive galaxies or a star formation rate and stellar mass relation normalization lower than that observed - rather than a problem specific to the SMG population. C1 [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Hayward, Christopher C.; Jonsson, Patrik; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayanan, Desika] Univ Arizona, Dept Astron, Steward Observ, Tucson, AZ 85721 USA. [Keres, Dusan] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. RP Hayward, CC (reprint author), Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. EM christopher.hayward@h-its.org RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU National Science Foundation [AST-1009452]; NASA [HST-HF-51276.01-A]; W. M. Keck Foundation FX We thank Andrew Benson, Romeel Dave, Mark Swinbank and Naoki Yoshida for comments on the manuscript; Scott Chapman, Michal Michalowski, Pierluigi Monaco, Alex Pope, Isaac Roseboom and Josh Younger for useful discussion; Carlton Baugh, Cedric Lacey, Fabio Fontanot, Gian-Luigi Granato, Vernesa Smolcic, Axel Weiss and Min Yun for providing data with which we have compared and for useful discussion and Volker Springel for providing the non-public version of GADGET-2 used for this work. DN acknowledges support from a National Science Foundation Grant (AST-1009452). DK was supported by NASA through Hubble Fellowship grant HST-HF-51276.01-A. PJ acknowledges support by a grant from the W. M. Keck Foundation. The simulations in this paper were performed on the Odyssey cluster supported by the FAS Research Computing Group at Harvard University. NR 205 TC 69 Z9 69 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2529 EP 2547 DI 10.1093/mnras/sts222 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700052 ER PT J AU Casey, MP Zwintz, K Guenther, DB Weiss, WW Amado, PJ Diaz-Fraile, D Rodriguez, E Kuschnig, R Matthews, JM Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D AF Casey, M. P. Zwintz, K. Guenther, D. B. Weiss, W. W. Amado, P. J. Diaz-Fraile, D. Rodriguez, E. Kuschnig, R. Matthews, J. M. Moffat, A. F. J. Rowe, J. F. Rucinski, S. M. Sasselov, D. TI MOST observations of the Herbig Ae delta-Scuti star HD 34282 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; techniques: photometric; stars: individual: HD 34282; stars: pre-main sequence; stars: variables: delta Scuti ID MAIN-SEQUENCE STARS; SPECTRAL CLASSIFICATION; FREQUENCY; PHOTOMETRY; SATELLITE; CATALOG; SPACE; MODES; SUN AB Microvariability and Oscillations of STars (MOST) observations and model analysis of the Herbig Ae star HD 34282 (V1366 Ori) reveal delta Scuti pulsations. 22 frequencies are observed, 10 of which confirm those previously identified by Amado et al. and 12 of which are newly discovered in this work. We show that the weighted-average frequency in each group fits the radial p-mode frequencies of viable models. We argue that the observed pulsation spectrum extends just to the edge to the acoustic cut-off frequency and shows that this is also consistent with our best-fitting models. C1 [Casey, M. P.; Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Zwintz, K.; Weiss, W. W.; Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Amado, P. J.; Diaz-Fraile, D.; Rodriguez, E.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Casey, MP (reprint author), St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. EM mcasey@ap.smu.ca RI Amado, Pedro Jose/G-3450-2011; OI Amado, Pedro Jose/0000-0002-8388-6040; Rodriguez, Eloy/0000-0001-6827-9077 FU Austrian Academy of Sciences at the Institute of Astronomy of the University Vienna; Natural Sciences and Engineering Research Council of Canada; FQRNT; Austrian Science Fund [P22691-N16]; Austrian Research Promotion Agency-ALR; Ministry of Economy and Competitiveness [AYA2010-14840]; Junta de Andalucia; Direccion General de Investigacion (DGI) [AYA2009-10394] FX KZ is a recipient of an APART fellowship of the Austrian Academy of Sciences at the Institute of Astronomy of the University Vienna. DBG, MPC, SMR and AFJM acknowledge the funding support of the Natural Sciences and Engineering Research Council of Canada. AFJM also acknowledges the funding support of FQRNT. RK and WWW are supported by the Austrian Science Fund (P22691-N16) and by the Austrian Research Promotion Agency-ALR. PJA acknowledges financial support of the previous Spanish Ministry of Science and Innovation (MICINN), currently Ministry of Economy and Competitiveness, grant AYA2010-14840. DD and ER acknowledge the support by the Junta de Andalucia and the Direccion General de Investigacion (DGI), project AYA2009-10394. NR 38 TC 5 Z9 5 U1 0 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 3 BP 2596 EP 2604 DI 10.1093/mnras/sts241 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134RA UT WOS:000318230700056 ER PT J AU Branstetter, MG AF Branstetter, Michael G. TI Revision of the Middle American clade of the ant genus Stenamma Westwood (Hymenoptera, Formicidae, Myrmicinae) SO ZOOKEYS LA English DT Article DE Stenammini; systematics; taxonomy; cryptic ants; Neotropics; Central America; cloud forest ID DIVERSIFICATION AB Stenamma is a cryptic "leaf-litter" ant genus that occurs in mesic forest habitats throughout the Holarctic region, Central America, and part of northwestern South America (Colombia and Ecuador). The genus was thought to be restricted primarily to the temperate zone, but recent collecting efforts have uncovered a large radiation of Neotropical forms, which rival the Holarctic species in terms of morphological and behavioral diversity. By inferring a broad-scale molecular phylogeny of Stenamma, Branstetter (2012) showed that all Neotropical species belong to a diverse Middle American clade (MAC), and that this clade is sister to an almost completely geographically separated Holarctic clade (HOC). Here, the Middle American clade of Stenamma is revised to recognize 40 species, of which 33 are described as new. Included in the revision are a key to species based on the worker caste, and for each species where possible, descriptions and images of workers and queens, images of males, information on geographic distribution, descriptions of intraspecific variation, and notes on natural history. Several species groups are defined, but the majority of species remain unassigned due to a lack of diagnostic morphological character states for most molecular clades. The following species are redescribed: S. alas Longino, S. diversum Mann, S. expolitum Smith, S. felixi Mann, S. huachucanum Smith, S. manni Wheeler, and S. schmidti Menozzi. The following are described as new: S. andersoni sp. n., S. atribellum sp. n., S. brujita sp. n., S. callipygium sp. n., S. catracho sp. n., S. connectum sp. n., S. crypticum sp. n., S. cusuco sp. n., S. excisum sp. n., S. expolitico sp. n., S. hojarasca sp. n., S. ignotum sp. n., S. lagunum sp. n., S. llama sp. n., S. leptospinum sp. n., S. lobinodus sp. n., S. longinoi sp. n., S. maximon sp. n., S. megamanni sp. n., S. monstrosum sp. n., S. muralla sp. n., S. nanozoi sp. n., S. nonotch sp. n., S. ochrocnemis sp. n., S. pelophilum sp. n., S. picopicucha sp. n., S. saenzae sp. n., S. sandinista sp. n., S. stictosomum sp. n., S. tiburon sp. n., S. tico sp. n., S. vexator sp. n., and S. zelum sp. n. Although many of the newly defined species consist of challenging species complexes, this study establishes a robust baseline that will guide future work on the systematics of MAC Stenamma. The total global diversity of Stenamma now includes 84 extant species. C1 [Branstetter, Michael G.] Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. [Branstetter, Michael G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Branstetter, MG (reprint author), Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. EM mgbranstetter@gmail.com RI sebastianovitsch, stepan/G-8507-2013 FU National Science Foundation (Project LLAMA) [DEB-0640015, EF0431330]; National Geographic Society [8408-08]; Conservation International; UC MEXUS; Organization for Tropical Studies; Center for Population Biology and Department of Entomology at UC Davis; Harvard Museum of Comparative Zoology (Ernst Mayr Travel Grant); Smithsonian Institution FX I owe a great debt of gratitude to many people, institutions, and funding agencies for helping me complete this project. For providing specimens for morphological and molecular work I thank Jack Longino (JTLC), Phil Ward (PSWC, UCDC), Roy Snelling (LACM), Fernando Fernandez (ICN), Bill MacKay, Stefan Cover (MCZ), Laura Saenz, Manuel Solis (INBio), Corrie Moreau (FMNH), James Boone (FMNH), Ted Schultz (USNM), Sean Brady (USNM), David Donoso and Bob Anderson. I am especially grateful to everyone who participated in the Leaf Litter Arthropods of MesoAmerica (LLAMA) project, which provided specimens, field assistance, and financial support for several seasons of fieldwork (Figure 172). The senior personnel and main collaborators in project LLAMA were Jack Longino, Bob Anderson, Laura Saenz, Jorge Leon (ECOSCE), Jack Schuster (UVGC), Jose Mora (EAPZ), Oliver Schlein (EAPZ), Jean-Michel Maes, Eric Van Den Berghe, and Jose Monzon. I also thank all of the student participants in LLAMA, who carried out most of the hard labor. By country these are: CHIAPAS (Brittany Broyles, D. J. Cox, Jesse McAlpine, Duke Brady, Dina Estrada, Yensy Recinos, Ubaldo Caballero, Irma Miss, Obed Reyes, Jesus Luna); GUATEMALA (Steven Bylsma, Jennie Russ, Theo Sumnicht, Crystal Vincent, Samanta Orellana, Diego Pons, Manuel Barrios, Cristian Beza); HONDURAS (Tammy Andrews, Ali Stefancich, Brendon Boudinot, Kyle Phillips, Shefik Handal, Katherine Gonzalez, Luis Orellana, Alicia Bustillos); and NICARAGUA (Matt Prebus, Jane Allison, Corwin Parker, Elizabeth Foster, Januar Lopez, Aquiles Reyes, Blas Hernandez). Additional field assistance was provided by Miguel Vasquez-Bolaos, Santiago Nino, Manuel Solis, Enio Cano, Carlos Viquez, Luis Cervantes, Ana Samayoa, Calixto Ordoes, and Fidel. I thank Phil Ward, Marek Borowiec, and Jack Longino for testing early versions of the key. Phil Ward, Penny Gulan, and Jack Longino provided helpful comments on the manuscript. I thank Brian Fisher, Michele Esposito and the rest of the team at CAS for creating and maintaining AntWeb. This work was funded by the National Science Foundation (Project LLAMA, DEB-0640015; Ant AToL, EF0431330), the National Geographic Society (CRE grant 8408-08), Conservation International, UC MEXUS, the Organization for Tropical Studies, the Center for Population Biology and Department of Entomology at UC Davis, the Harvard Museum of Comparative Zoology (Ernst Mayr Travel Grant), and the Smithsonian Institution (Peter Buck postdoctoral fellowship). NR 19 TC 7 Z9 7 U1 0 U2 9 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 295 SI SI BP 1 EP 277 DI 10.3897/zookeys.295.4905 PG 277 WC Zoology SC Zoology GA 131SE UT WOS:000318015300001 PM 23794874 ER PT J AU Fu, D Worden, JR Liu, X Kulawik, SS Bowman, KW Natraj, V AF Fu, D. Worden, J. R. Liu, X. Kulawik, S. S. Bowman, K. W. Natraj, V. TI Characterization of ozone profiles derived from Aura TES and OMI radiances SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID TROPOSPHERIC EMISSION SPECTROMETER; MOLECULAR SPECTROSCOPIC DATABASE; ROTATIONAL RAMAN-SCATTERING; MONITORING INSTRUMENT; ATMOSPHERIC COMPOSITION; SATELLITE MEASUREMENTS; NADIR RETRIEVALS; SPECTRAL REGIONS; ERROR ANALYSIS; AIR-QUALITY AB We present satellite based ozone profile estimates derived by combining radiances measured at thermal infrared (TIR) wavelengths from the Aura Tropospheric Emission Spectrometer (TES) and ultraviolet (UV) wavelengths measured by the Aura Ozone Monitoring Instrument (OMI). The advantage of using these combined wavelengths and instruments for sounding ozone over either instrument alone is improved sensitivity near the surface as well as the capability to consistently resolve the lower troposphere, upper troposphere, and lower stratosphere for scenes with varying geophysical states. For example, the vertical resolution of ozone estimates from either TES or OMI varies strongly by surface albedo and temperature. Typically, TES provides 1.6 degrees of freedom for signal (DOFS) and OMI provides less than 1 DOFS in the troposphere. The combination provides 2 DOFS in the troposphere with approximately 0.4 DOFS for near surface ozone (surface to 700 hPa). We evaluated these new ozone profile estimates with ozonesonde measurements and found that calculated errors for the joint TES and OMI ozone profile estimates are in reasonable agreement with actual errors as derived by the root-mean-square (RMS) difference between the ozonesondes and the joint TES/OMI ozone estimates. We also used a common a priori profile in the retrievals in order to evaluate the capability of different retrieval approaches on capturing near-surface ozone variability. We found that the vertical resolution of the joint TES/OMI ozone profile estimates shows significant improvements on quantifying variations in near-surface ozone with RMS differences of 49.9% and correlation coefficient of R = 0.58 for the TES/OMI near-surface estimates as compared to 67.2% RMS difference and R = 0.33 for TES and 115.8% RMS difference and R = 0.09 for OMI. This comparison removes the impacts of using the climatological a priori in the retrievals. However, it results in artificially large sonde/retrieval differences. The TES/OMI ozone profiles from the production code of joint retrievals will use climatological a priori and therefore will have more realistic ozone estimates than those from using a common a priori volume mixing ratio profile. C1 [Fu, D.; Worden, J. R.; Kulawik, S. S.; Bowman, K. W.; Natraj, V.] CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. [Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fu, D (reprint author), CALTECH, Jet Prop Lab, Div Earth & Space Sci, Pasadena, CA 91109 USA. EM dejian.fu@jpl.nasa.gov RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU National Aeronautics and Space Administration; Smithsonian Institution FX We are grateful to Ruud Dirksen, Robert Voors, and Marcel Dobbers for providing OMI spectral slit function data and Braak Remco at Royal Netherlands Meteorological Institute for providing information on OMI L1b data. We thank Annmarie Eldering, Stanley Sander, Robert Herman, and Alyn Lambert for helpful discussions. We thank the World Ozone Data Centre for making the routine sonde data accessible. We thank the editor and reviewers for helpful suggestions. The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Research at the Smithsonian Astrophysical Observatory was supported by the National Aeronautics and Space Administration and by the Smithsonian Institution. The JPL authors' copyright for this publication is held by the California Institute of Technology. Government Sponsorship acknowledged. NR 91 TC 20 Z9 20 U1 2 U2 23 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PY 2013 VL 13 IS 6 BP 3445 EP 3462 DI 10.5194/acp-13-3445-2013 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 117NU UT WOS:000316961000032 ER PT J AU Rafferty, DA Birzan, L Nulsen, PEJ McNamara, BR Brandt, WN Wise, MW Rottgering, HJA AF Rafferty, D. A. Birzan, L. Nulsen, P. E. J. McNamara, B. R. Brandt, W. N. Wise, M. W. Rottgering, H. J. A. TI A deep Chandra observation of the active galactic nucleus outburst and merger in Hickson compact group 62 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays: galaxies: clusters; galaxies: clusters: individual: HCG 62 ID X-RAY CAVITIES; FLOW CLUSTER ABELL-2052; ELLIPTIC GALAXIES; PERSEUS CLUSTER; STAR-FORMATION; AGN FEEDBACK; RADIO-SOURCE; BLACK-HOLES; COSMIC-RAYS; XMM-NEWTON AB We report on an analysis of new Chandra data of the galaxy group HCG 62, well known for possessing cavities in its intragroup medium (IGM) that were inflated by the radio lobes of its central active galactic nucleus (AGN). With the new data, a factor of 3 deeper than previous Chandra data, we re-examine the energetics of the cavities and determine new constraints on their contents. We confirm that the ratio of radiative to mechanical power of the AGN outburst that created the cavities is less than 10(-4), among the lowest of any known cavity system, implying that the relativistic electrons in the lobes can supply only a tiny fraction of the pressure required to support the cavities. This finding implies additional pressure support in the lobes from heavy particles (e. g. protons) or thermal gas. Using spectral fits to emission in the cavities, we constrain any such volume-filling thermal gas to have a temperature kT greater than or similar to 4.3 keV. For the first time, we detect X-ray emission from the central AGN, with a luminosity of L2-10 keV = (1.1 +/- 0.4) x 10(39) erg s(-1) and properties typical of a low-luminosity AGN. Finally, we report evidence for a recent merger from the surface brightness, temperature and metallicity structure of the IGM. C1 [Rafferty, D. A.; Birzan, L.; Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Nulsen, P. E. J.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2YS, Canada. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wise, M. W.] ASTRON Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. RP Rafferty, DA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM rafferty@strw.leidenuniv.nl RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Nulsen, Paul/0000-0003-0297-4493 FU NASA [NNX10AC99G, GO9-0136a] FX We thank the referee for helpful comments that improved the paper considerably. DAR was supported in part by the NASA ADP grant NNX10AC99G and CXC grant GO9-0136a. NR 55 TC 8 Z9 8 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 1 BP 58 EP 70 DI 10.1093/mnras/sts007 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QH UT WOS:000318227900016 ER PT J AU Munoz, DJ Springel, V Marcus, R Vogelsberger, M Hernquist, L AF Munoz, D. J. Springel, V. Marcus, R. Vogelsberger, M. Hernquist, L. TI Multidimensional, compressible viscous flow on a moving Voronoi mesh SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; methods: numerical ID TAYLOR-COUETTE FLOW; SMOOTHED PARTICLE HYDRODYNAMICS; NAVIER-STOKES EQUATIONS; FINITE-VOLUME METHODS; MAGNETOROTATIONAL INSTABILITY; NUMERICAL-SIMULATION; INCOMPRESSIBLE-FLOW; SUBSONIC TURBULENCE; PLANET INTERACTION; ACCRETION DISKS AB Numerous formulations of finite-volume schemes for the Euler and Navier-Stokes equations exist, but in the majority of cases they have been developed for structured and stationary meshes. In many applications, more flexible mesh geometries that can dynamically adjust to the problem at hand and move with the flow in a (quasi-)Lagrangian fashion would, however, be highly desirable, as this can allow a significant reduction of advection errors and an accurate realization of curved and moving boundary conditions. Here we describe a novel formulation of viscous continuum hydrodynamics that solves the equations of motion on a Voronoi mesh created by a set of mesh-generating points. The points can move in an arbitrary manner, but the most natural motion is that given by the fluid velocity itself, such that the mesh dynamically adjusts to the flow. Owing to the mathematical properties of the Voronoi tessellation, pathological mesh-twisting effects are avoided. Our implementation considers the full Navier-Stokes equations and has been realized in the AREPO code both in two and three dimensions. We propose a new approach to compute accurate viscous fluxes for a dynamic Voronoi mesh, and use this to formulate a finite-volume solver of the Navier-Stokes equations. Through a number of test problems, including circular Couette flow and flow past a cylindrical obstacle, we show that our new scheme combines good accuracy with geometric flexibility, and hence promises to be competitive with other highly refined Eulerian methods. This will in particular allow astrophysical applications of the AREPO code where physical viscosity is important, such as in the hot plasma in galaxy clusters, or for viscous accretion disc models. C1 [Munoz, D. J.; Marcus, R.; Vogelsberger, M.; Hernquist, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, V.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, V.] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. RP Munoz, DJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmunoz@cfa.harvard.edu NR 71 TC 9 Z9 9 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 1 BP 254 EP 279 DI 10.1093/mnras/sts015 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QH UT WOS:000318227900033 ER PT J AU Van Loo, S Ashmore, I Caselli, P Falle, SAEG Hartquist, TW AF Van Loo, S. Ashmore, I. Caselli, P. Falle, S. A. E. G. Hartquist, T. W. TI Sputtering in oblique C-type shocks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE MHD; shock waves; ISM: jets and outflows ID WEAKLY IONIZED CLOUDS; SIO LINE EMISSION; MOLECULAR CLOUDS; INTERSTELLAR SHOCKS; UMIST DATABASE; GRAIN DYNAMICS; DENSE CLOUDS; DUST GRAINS; WAVES; EVOLUTION AB We present the first results for the sputtering of grain mantles and cores obtained with self-consistent multifluid hydromagnetic models of oblique C-type shocks propagating through dusty media. The threshold shock speed for mantle sputtering is about 10 km s(-1) and is independent of density. The mantles are completely vapourized in shocks with speeds of 20-25 km s(-1). At such shock speeds, core sputtering commences and gas-phase SiO forms. Core destruction is not total in any C-type shock because grains are not completely destroyed in shocks with speeds near the minimum speeds at which J-type shocks appear. Due to the density dependence of the critical shock speed for this transition, higher gas-phase SiO fractional abundances are produced behind shocks propagating in lower density gas. For shock speeds near the threshold speeds for both core and mantle sputtering, sputtering is much greater for shock velocities at smaller angles relative to the upstream magnetic field. At higher shock speeds, the angular variation is still present but less pronounced. C1 [Van Loo, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ashmore, I.; Caselli, P.; Hartquist, T. W.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Falle, S. A. E. G.] Univ Leeds, Dept Appl Math, Leeds LS2 9JT, W Yorkshire, England. RP Van Loo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM svanloo@cfa.harvard.edu OI Van Loo, Sven/0000-0003-4746-8500 FU UK Science and Technology Funding Council; SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory FX We thank the anonymous referee for his/her constructive comments. We are grateful for the support provided by a studentship and successive rolling grants awarded by the UK Science and Technology Funding Council and from the SMA Postdoctoral Fellowship of the Smithsonian Astrophysical Observatory held by SVL. NR 36 TC 9 Z9 9 U1 4 U2 8 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 1 BP 381 EP 388 DI 10.1093/mnras/sts030 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QH UT WOS:000318227900042 ER PT J AU Margutti, R Zaninoni, E Bernardini, MG Chincarini, G Pasotti, F Guidorzi, C Angelini, L Burrows, DN Capalbi, M Evans, PA Gehrels, N Kennea, J Mangano, V Moretti, A Nousek, J Osborne, JP Page, KL Perri, M Racusin, J Romano, P Sbarufatti, B Stafford, S Stamatikos, M AF Margutti, R. Zaninoni, E. Bernardini, M. G. Chincarini, G. Pasotti, F. Guidorzi, C. Angelini, L. Burrows, D. N. Capalbi, M. Evans, P. A. Gehrels, N. Kennea, J. Mangano, V. Moretti, A. Nousek, J. Osborne, J. P. Page, K. L. Perri, M. Racusin, J. Romano, P. Sbarufatti, B. Stafford, S. Stamatikos, M. TI The prompt-afterglow connection in gamma-ray bursts: a comprehensive statistical analysis of Swift X-ray light curves SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanism: non-thermal; gamma-ray burst: general ID FLARING ACTIVITY; COMPLETE SAMPLE; COLUMN DENSITY; CENTRAL ENGINE; JET BREAKS; 1ST SURVEY; XRT DATA; EMISSION; LONG; FLARES AB We present a comprehensive statistical analysis of Swift X-ray light curves of gamma-ray bursts (GRBs) collecting data from more than 650 GRBs discovered by Swift and other facilities. The unprecedented sample size allows us to constrain the rest-frame X-ray properties of GRBs from a statistical perspective, with particular reference to intrinsic time-scales and the energetics of the different light-curve phases in a common rest-frame 0.3-30 keV energy band. Temporal variability episodes are also studied and their properties constrained. Two fundamental questions drive this effort: (i) Does the X-ray emission retain any kind of 'memory' of the prompt gamma-ray phase? (ii) Where is the dividing line between long and short GRB X-ray properties? We show that short GRBs decay faster, are less luminous and less energetic than long GRBs in the X-rays, but are interestingly characterized by similar intrinsic absorption. We furthermore reveal the existence of a number of statistically significant relations that link the X-ray to prompt gamma-ray parameters in long GRBs; short GRBs are outliers of the majority of these two-parameter relations. However and more importantly, we report on the existence of a universal three-parameter scaling that links the X-ray and the gamma-ray energy to the prompt spectral peak energy of both long and short GRBs: E-X,E-iso proportional to E-gamma,iso(1.00 +/- 0.06)//E-pk(0.60 +/- 0.10). C1 [Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Margutti, R.; Zaninoni, E.; Bernardini, M. G.; Chincarini, G.; Pasotti, F.; Moretti, A.; Sbarufatti, B.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Zaninoni, E.] Univ Padua, Phys & Astron Dept Galileo Galilei, I-35131 Padua, Italy. [Chincarini, G.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy. [Guidorzi, C.] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy. [Angelini, L.; Gehrels, N.; Racusin, J.; Stamatikos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Capalbi, M.; Perri, M.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Evans, P. A.; Osborne, J. P.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England. [Mangano, V.; Romano, P.] INAF IASF Palermo, Palermo, Italy. [Stafford, S.; Stamatikos, M.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Stafford, S.; Stamatikos, M.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rmargutti@cfa.harvard.edu OI Perri, Matteo/0000-0003-3613-4409; moretti, alberto/0000-0002-9770-0315; Sbarufatti, Boris/0000-0001-6620-8347 FU ASI [SWIFT I/004/11/0]; UK Space Agency; ASI-INAF [I/009/10/0] FX RM thanks Lorenzo Amati and Lara Nava for sharing their data before publication. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. MGB thanks ASI grant SWIFT I/004/11/0. PAE, KLP and JPO acknowledge financial support from the UK Space Agency. PR acknowledges financial contribution from the agreement ASI-INAF I/009/10/0. NR 55 TC 65 Z9 65 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 1 BP 729 EP 742 DI 10.1093/mnras/sts066 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QH UT WOS:000318227900068 ER PT J AU Leigh, N Knigge, C Sills, A Perets, HB Sarajedini, A Glebbeek, E AF Leigh, Nathan Knigge, Christian Sills, Alison Perets, Hagai B. Sarajedini, Ata Glebbeek, Evert TI The origins of blue stragglers and binarity in globular clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; binaries: close; blue stragglers; globular clusters: general; stars: kinematics and dynamics; binaries: general ID COLOR-MAGNITUDE DIAGRAM; STELLAR COLLISIONS; RADIAL-DISTRIBUTION; STAR-CLUSTERS; MAIN-SEQUENCE; ACS SURVEY; MILKY-WAY; NGC 188; CATALOG; POPULATION AB Two basic formation channels have been proposed for blue straggler stars in globular clusters: binary star evolution and stellar collisions. We recently showed that the number of blue stragglers found in the core of a globular cluster is strongly correlated with the total stellar mass of the core, but not with the collision rate in the core. This result strongly favoured binary evolution as the dominant channel for blue straggler formation. Here, we use newly available empirical binary fractions for globular clusters to carry out a more direct test of the binary evolution hypothesis, and also of collisional channels that involve binary stars. More specifically, using the correlation between blue straggler numbers and core mass as a benchmark, we test for correlations with the number of binary stars, as well as with the rates of single-single, single-binary and binary-binary encounters. We also consider joint models, in which blue straggler numbers are allowed to depend on star/binary numbers and collision rates simultaneously. Surprisingly, we find that the simple correlation with core mass remains by far the strongest predictor of blue straggler population size, even in our joint models. This is despite the fact that the binary fractions themselves strongly anticorrelate with core mass, just as expected in the binary evolution model. At first sight, these results do not fit neatly with either binary evolution or collisional models in their simplest forms. Arguably, the simplest and most intriguing possibility to explain this unexpected result is that observational errors on the core binary fractions are larger than the true intrinsic dispersion associated with their dependence on core mass. In the context of the binary evolution model, this would explain why the combination of binary fraction and core mass is a poorer predictor of blue straggler numbers than core mass alone. It would also imply that core mass is a remarkably clean predictor of core binary fractions. This would be of considerable importance for the dynamical evolution of globular clusters and provides an important benchmark for models attempting to understand their present-day properties. C1 [Leigh, Nathan; Sills, Alison; Glebbeek, Evert] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Leigh, Nathan] European Space Agcy, Dept Space Sci, NL-2200 AG Noordwijk, Netherlands. [Knigge, Christian] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. [Sarajedini, Ata] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Glebbeek, Evert] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Leigh, N (reprint author), McMaster Univ, Dept Phys & Astron, 1280 Main St W, Hamilton, ON L8S 4M1, Canada. EM naynaysnebula@hotmail.com FU ESA; NSERC; Ontario Graduate Scholarship programme FX We would like to thank Craig Heinke for useful comments, Frank Verbunt, Tom Maccarone and Dave Zurek for helpful suggestions for improvement, as well as an anonymous referee for many suggestions that resulted in significant improvements to our manuscript. This research has been supported by ESA, NSERC and the Ontario Graduate Scholarship programme. NR 39 TC 17 Z9 17 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JAN PY 2013 VL 428 IS 1 BP 897 EP 905 DI 10.1093/mnras/sts085 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 134QH UT WOS:000318227900081 ER PT J AU Carvalho, LN Fidelis, L Arruda, R Galuch, A Zuanon, J AF Carvalho, Lucelia Nobre Fidelis, Luana Arruda, Rafael Galuch, Andre Zuanon, Jansen TI Second floor, please: the fish fauna of floating litter banks in Amazonian streams and rivers SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Ephemeral habitats; Fish assemblages; Insectivores; Lotic systems; Trophic structure AB Floating litter banks are an ephemeral habitat consisting of branches, twigs, flowers, seeds, and fruits that are trapped on the stream water surface by a variety of retention mechanisms. These heterogeneous materials form a deep layer of dead plant matter that is colonized by a variety of organisms, including fish that forage on the aquatic macroinvertebrates found in this unique habitat. In this study, we aimed to characterize which fish species occupy the floating litter banks and their trophic characteristics, as well as determine if fish assemblage composition and species richness can be predicted by the size of the floating litter banks. Fish sampling was conducted in five rivers located in the Amazon basin. Of the 31 floating litter banks sampled that contained fish, 455 individuals were recorded and were distributed within 40 species, 15 families and five orders. Siluriformes were the most representative order among the samples and contained the largest number of families and species. The fish fauna sampled was mainly composed of carnivorous species that are typically found in submerged litter banks of Amazonian streams. The fish assemblage composition in the kinon can be predicted by the volume of the floating litter banks using both presence/absence and abundance data, but not its species richness. In conclusion, kinon banks harbor a rich fish assemblage that utilizes this habitat for shelter and feeding, and may function as a refuge for the fishes during the peak of the flooding season. C1 [Carvalho, Lucelia Nobre; Arruda, Rafael] Univ Fed Mato Grosso, Inst Ciencias Nat Humanas & Sociais, Sinop, MT, Brazil. [Carvalho, Lucelia Nobre; Fidelis, Luana; Galuch, Andre; Zuanon, Jansen] Coordenacao Biodiversidade, Biol Dynam Forest Fragments Priject, BR-69060001 Manaus, AM, Brazil. [Carvalho, Lucelia Nobre; Fidelis, Luana; Galuch, Andre; Zuanon, Jansen] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, BR-69060001 Manaus, AM, Brazil. RP Carvalho, LN (reprint author), Univ Fed Mato Grosso, Inst Ciencias Nat Humanas & Sociais, Campus Univ Sinop, Sinop, MT, Brazil. EM carvalholn@yahoo.com.br RI Nobre Carvalho, Lucelia/D-5986-2013; Arruda, Rafael/D-4362-2012 OI Nobre Carvalho, Lucelia/0000-0002-0673-0165; Arruda, Rafael/0000-0003-2869-5134 FU CNPq [307464/2009-1]; FAPEAM; Fundacao "O Boticario" de Protecao a Natureza; IIEB (BECA program) [B/2006/01/BDP/05] FX We thank Alberto Akama and Ocirio Pereira for their help with fieldwork. Fabiola Artemis Souza do Valle helped with the identification of food items. Oscar Shibatta checked the identification of the Pseudopimelodidae species. The Fundacao Nacional da Saude (FUNASA), the Instituto de Pesquisas Ecologicas (IPE) and the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis (IBAMA/Programa ARPA) provided logistical support. Fernando P. Mendonca by photos of Figs. 1(b) and 2 (a, b), and Leandro M. Sousa by photos of Fig. 2 (c, d). CNPq, FAPEAM, and the Fundacao "O Boticario" de Protecao a Natureza provided essential financial support. This study was supported by fellowships from CNPq to JZ (process 307464/2009-1); graduate fellowships from CNPq and IIEB (BECA program, B/2006/01/BDP/05, the Gordon and Betty Moore Foundation) to LNC. This is contribution number 612 in the BDFFP Technical Series and contribution 28 of Projeto Igarapes. NR 30 TC 2 Z9 2 U1 0 U2 9 PU SOC BRASILEIRA ICTIOLOGIA PI SAO PAULO PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO PAULO, SP 05508-900, BRAZIL SN 1679-6225 J9 NEOTROP ICHTHYOL JI Neotrop. Ichthyol. PD JAN-MAR PY 2013 VL 11 IS 1 BP 85 EP 94 PG 10 WC Zoology SC Zoology GA 130SJ UT WOS:000317939200010 ER PT B AU Kilic, M Brown, WR Hermes, JJ AF Kilic, Mukremin Brown, Warren R. Hermes, J. J. BE Auger, G Binetruy, P Plagnol, E TI Ultra-Compact Binaries: eLISA Verification Sources SO 9TH LISA SYMPOSIUM SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 9th LISA Symposium CY MAY, 2012 CL Paris, FRANCE ID AM CVN STARS; MINUTE ORBITAL PERIOD; DWARF MERGER SYSTEMS; MASS WHITE-DWARFS; DOUBLE-DEGENERATE; DOUBLE-PULSAR; DISCOVERY; TESTS; I. AB There are numerous ultra-compact binary systems containing white dwarfs and neutron stars in the Galaxy. Many of these systems are weak gravitational wave emitters. However, there are eight known systems where the gravitational wave strain is strong enough to be detected by the proposed eLISA mission. These verification binaries are the strongest gravitational wave sources currently known, and eLISA will detect the gravitational waves from them within a few weeks to months. We review the properties of these eight sources including the observed rate of orbital decay. In addition, we present the recent results from the ELM Survey, which discovered the second best verification binary currently known. We also discuss the future prospects for increasing the number of verification binaries. C1 [Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hermes, J. J.] Univ Texas, Dept Astron, Austin, TX USA. RP Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. NR 36 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-58381-816-9 J9 ASTR SOC P PY 2013 VL 467 BP 47 EP + PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI60 UT WOS:000316716900006 ER PT S AU Kielkopf, JF Allard, NF Babb, J AF Kielkopf, J. F. Allard, N. F. Babb, J. BE Stehle, C Joblin, C DHendecourt, L TI A COMPARISON OF LABORATORY SPECTRA WITH A NEW THEORETICAL STUDY OF POTASSIUM RESONANCE LINES PERTURBED BY HELIUM SO ECLA: EUROPEAN CONFERENCE ON LABORATORY ASTROPHYSICS SE EAS Publications Series LA English DT Proceedings Paper CT ECLA: European Conference on Laboratory Astrophysics CY SEP 26-30, 2011 CL Paris, FRANCE SP Minist Enseignement Super Rech, CNRS, Programme Natl Phys & Chim, Observ Paris, Univ Pierre & Marie Curie, Univ Cergy Pontolse, Univ Paris Sud, Ctr Natl Etudes Spatiales, Commissariat Energie Atom, Inst Astrophys Paris, Inst Rech Astrophys & Plantetol, Lab Etude Matiere & Env Astrophys, Soc Bruker, Ville Paris AB The optical spectra of L- and T-type dwarfs exhibit a continuum dominated by the far wings of the absorption profiles of the Na 3s-3p and K 4s-4p doublets perturbed by molecular hydrogen and helium. We examine the K resonance line wing and core with a unified line profile theory and compare to laboratory experiments and observations of the cool brown dwarf epsilon Indi Ba, b. C1 [Kielkopf, J. F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Allard, N. F.] Observatoire Paris, GEPI, F-75014 Paris, France. [Allard, N. F.] Univ Paris VI, CNRS, Inst dAstrophys Paris, UMR 7095, F-75014 Paris, France. [Babb, J.] Harvard Smithsonian Ctr Astrophys, TAMP, Cambridge, MA 02138 USA. RP Kielkopf, JF (reprint author), Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-0941-7 J9 EAS PUBLICATIONS PY 2013 VL 58 BP 75 EP + DI 10.1051/eas/1258011 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEP63 UT WOS:000317632700011 ER PT S AU Fayolle, EC Oberg, KI Cuppen, HM Visser, R Linnartz, H AF Fayolle, E. C. Oeberg, K. I. Cuppen, H. M. Visser, R. Linnartz, H. BE Stehle, C Joblin, C DHendecourt, L TI LABORATORY H2O:CO2 ICE DESORPTION: ENTRAPMENT AND ITS PARAMETERIZATION WITH AN EXTENDED THREE-PHASE MODEL SO ECLA: EUROPEAN CONFERENCE ON LABORATORY ASTROPHYSICS SE EAS Publications Series LA English DT Proceedings Paper CT ECLA: European Conference on Laboratory Astrophysics CY SEP 26-30, 2011 CL Paris, FRANCE SP Minist Enseignement Super Rech, CNRS, Programme Natl Phys & Chim, Observ Paris, Univ Pierre & Marie Curie, Univ Cergy Pontolse, Univ Paris Sud, Ctr Natl Etudes Spatiales, Commissariat Energie Atom, Inst Astrophys Paris, Inst Rech Astrophys & Plantetol, Lab Etude Matiere & Env Astrophys, Soc Bruker, Ville Paris AB Ice desorption affects the evolution of the gas-phase chemistry during the protostellar stage, and also determines the ice composition of comets forming in circumstellar disks. From observations, most volatile species, including CO2, are found in H2O-dominated ices. In this study, the desorption of CO2 mixed in H2O ice and the impact of ice thickness, mixture ratio and heating rate are experimentally determined. The results are used to parametrize an extended three-phase model (gas, ice surface and ice mantle) which describes ice mixture desorption using rate equations and a minimum number of free parameters. The model can be used to predict the evolution in thickness and concentration of volatile-rich H2O ice during infall of icy grains around protostars. C1 [Fayolle, E. C.; Linnartz, H.] Leiden Univ, Leiden Observ, Sackler Lab Astrophys, POB 9513, NL-2300 RA Leiden, Netherlands. [Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cuppen, H. M.] Radboud Univ Nijmegen, Inst Mol & Mat, NL-6500 GL Nijmegen, Netherlands. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Fayolle, EC (reprint author), Leiden Univ, Leiden Observ, Sackler Lab Astrophys, POB 9513, NL-2300 RA Leiden, Netherlands. OI Fayolle, Edith/0000-0001-8109-5256 NR 7 TC 1 Z9 1 U1 0 U2 3 PU E D P SCIENCES PI CEDEX A PA 17 AVE DU HOGGAR PARC D ACTIVITES COUTABOEUF BP 112, F-91944 CEDEX A, FRANCE SN 1633-4760 BN 978-2-7598-0941-7 J9 EAS PUBLICATIONS PY 2013 VL 58 BP 327 EP + DI 10.1051/eas/1258053 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEP63 UT WOS:000317632700053 ER PT J AU Sosdian, SM Lear, CH Tao, K Grossman, EL O'Dea, A Rosenthal, Y AF Sosdian, S. M. Lear, C. H. Tao, K. Grossman, E. L. O'Dea, A. Rosenthal, Y. TI Cenozoic Seawater Sr/Ca Evolution (vol 14, pg 263, 2013) SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Correction ID CARBON-DIOXIDE CONCENTRATIONS; OCEAN ACIDIFICATION; DEGREES C; ARAGONITE; CLIMATE; RECORD C1 [Sosdian, S. M.; Lear, C. H.] Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AX, S Glam, Wales. [Tao, K.; Grossman, E. L.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX USA. [O'Dea, A.] Smithsonian Trop Res Inst, Washington, DC USA. [Rosenthal, Y.] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08903 USA. [Rosenthal, Y.] Rutgers State Univ, Dept Geol, New Brunswick, NJ 08903 USA. RP Sosdian, SM (reprint author), Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AX, S Glam, Wales. EM SosdianS@cardiff.ac.uk RI O'Dea, Aaron/D-4114-2011 NR 14 TC 2 Z9 2 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD JAN PY 2013 VL 14 IS 1 BP 263 EP 264 DI 10.1029/2012GC004540 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 129EV UT WOS:000317822600016 ER PT J AU Wilson, LB Koval, A Szabo, A Breneman, A Cattell, CA Goetz, K Kellogg, PJ Kersten, K Kasper, JC Maruca, BA Pulupa, M AF Wilson, L. B., III Koval, A. Szabo, A. Breneman, A. Cattell, C. A. Goetz, K. Kellogg, P. J. Kersten, K. Kasper, J. C. Maruca, B. A. Pulupa, M. TI Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; WHISTLER-MODE TURBULENCE; MAGNETIC NOISE BURSTS; LOWER-HYBRID WAVES; HIGH MACH NUMBER; SOLAR-WIND; GEOTAIL OBSERVATIONS; LION ROARS; ISEE-2 OBSERVATIONS; FREQUENCY AB We present waveform observations of electromagnetic lower hybrid and whistler waves with f(ci) << f < f(ce) downstream of four supercritical interplanetary shocks using the Wind search coil magnetometer. The whistler waves were observed to have a weak positive correlation between dB and normalized heat flux magnitude and an inverse correlation with T-eh/T-ec. All were observed simultaneous with electron distributions satisfying the whistler heat flux instability threshold and most with T-perpendicular to h/T-parallel to h>1.01. Thus, the whistler mode waves appear to be driven by a heat flux instability and cause perpendicular heating of the halo electrons. The lower hybrid waves show a much weaker correlation between delta B and normalized heat flux magnitude and are often observed near magnetic field gradients. A third type of event shows fluctuations consistent with a mixture of both lower hybrid and whistler mode waves. These results suggest that whistler waves may indeed be regulating the electron heat flux and the halo temperature anisotropy, which is important for theories and simulations of electron distribution evolution from the Sun to the Earth. Citation: Wilson III, L. B., et al. (2013), Electromagnetic waves and electron anisotropies downstream of supercritical interplanetary shocks, J. Geophys. Res. Space Physics, 118, 5-16, doi:10.1029/2012JA018167. C1 [Wilson, L. B., III; Koval, A.; Szabo, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Breneman, A.; Cattell, C. A.; Goetz, K.; Kellogg, P. J.; Kersten, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Kasper, J. C.; Maruca, B. A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pulupa, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Koval, A.] Univ Maryland Baltimore Cty, Goddard Planetary Heliophys Inst, Baltimore, MD 21228 USA. RP Wilson, LB (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lynn.b.wilsoniii@gmail.com RI Kasper, Justin/D-1152-2010; Wilson III, Lynn/D-4425-2012; OI Kasper, Justin/0000-0002-7077-930X; Wilson III, Lynn/0000-0002-4313-1970; Cattell, Cynthia/0000-0002-3805-320X; Pulupa, Marc/0000-0002-1573-7457 FU NESSF [NNX07AU72H, NNX07AI05G]; Dr. Leonard Burlaga/Arctowski Medal Fellowship; NASA [NNX10AT09G] FX We thank S. D. Bale, J.R. Wygant, and R. Lysak for useful discussions of the physics involved in our study. All Wind spacecraft data were produced under Wind MO&DA grants. This research was partially supported by NESSF grant NNX07AU72H and grant NNX07AI05G, the Dr. Leonard Burlaga/Arctowski Medal Fellowship, and UCB work sponsored by NASA grant NNX10AT09G. NR 65 TC 9 Z9 9 U1 0 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JAN PY 2013 VL 118 IS 1 BP 5 EP 16 DI 10.1029/2012JA018167 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 129RC UT WOS:000317858600002 ER PT J AU Kawashima, T Thorington, RW Sato, F AF Kawashima, Tomokazu Thorington, Richard W., Jr. Sato, Fumi TI Systematic and comparative morphologies of the extrinsic cardiac nervous system in lemurs (Primates: Strepsirrhini: Infraorder Lemuriformes, Gray, 1821) with evolutionary morphological implications SO ZOOLOGISCHER ANZEIGER LA English DT Article DE Lemurs; Comparative anatomy; Primate evolution; Cardiac nerve; Cardiac branch ID HUMAN HEART; ARTERIAL DIFFERENTIATION; ATRIAL-FIBRILLATION; COMPARATIVE ANATOMY; RHESUS-MONKEY; WORLD MONKEYS; NEURAL CREST; RABBIT HEART; CHICK HEART; VAGUS NERVE AB The detailed systematic morphology of the extrinsic cardiac nervous system (ECNS) and its surrounding structures in lemurs, Lemuriformes, were examined using 18 sides of nine lemurs including all four families: Lemuridae, Indriidae, Lepilemuridae, and Cheirogaleidae. Although the general morphology of ECNS in lemurs is similar to that in Lorisiformes, several anatomical differences, such as the structural variation of the cervicothoracic ganglion, the positional variation of the middle cervical ganglion, and the unusual appearance of the superior cardiac nerve originating from the superior cervical ganglion, demonstrate the diversity within Lemuriformes. In other words, the comparative anatomical findings of the wide variations in ECNS in the four families of Lemuriformes compared with the lower variations in the two families of Lorisiformes possibly reflect their evolutionary history and diversity, as is shown in the recent molecular phylogeny. On the other hand, the shared common morphology of ECNS in Lorisiformes and Lemuriformes is considered to be the morphology of the common ancestor of strepsirrhines and demonstrates the gradual evolutionary changes in the primate lineage. Our present and previous results also suggest that ECNS is preserved in the primate lineage without modification and specialization because of its functional adaptation, as is seen in the somatic system. (C) 2012 Elsevier GmbH. All rights reserved. C1 [Kawashima, Tomokazu; Thorington, Richard W., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Washington, DC 20013 USA. [Kawashima, Tomokazu; Sato, Fumi] Toho Univ, Sch Med, Dept Anat, Ota Ku, Tokyo 1438540, Japan. RP Kawashima, T (reprint author), Toho Univ, Sch Med, Dept Anat, Ota Ku, Omori Nishi 5-21-16, Tokyo 1438540, Japan. EM tomokazu.kawashima@med.toho-u.ac.jp FU Ministry of Education, Culture, Sports, Science and Technology (MEXT) [16790804, 19790985, 23791579]; International Research Program from the MEXT; Toho University Medical School [H23-29] FX This study,was supported by grants for the Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) (Nos. 16790804 (2004-2006), 19790985 (2007-2009), and 23791579(2011-2014)), from the International Research Program from the MEXT (2008-2009), and for the Project Research from Toho University Medical School (No. H23-29 (2011)). NR 86 TC 2 Z9 2 U1 2 U2 9 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0044-5231 J9 ZOOL ANZ JI Zool. Anz. PY 2013 VL 252 IS 1 BP 101 EP 117 DI 10.1016/j.jcz.2012.04.001 PG 17 WC Zoology SC Zoology GA 130AE UT WOS:000317884300008 ER PT S AU Kirshner, RP AF Kirshner, Robert P. BE Di Stefano, R Orio, M Moe, M TI Better Understanding of SN Ia from Near Infrared Observations SO BINARY PATHS TO TYPE IA SUPERNOVAE EXPLOSIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 281st Symposium of the International-Astronomical-Union CY JUL 04-08, 2011 CL Padova, ITALY SP INAF, City Padova, Univ Padova, Dept Astronomy, INAF Padova Observ, ANEMOS DE supernovae: general; cosmology: distance scale, cosmological parameters ID LIGHT CURVES; SUPERNOVAE; UNIVERSE; SPECTRA; DUST; CONSTRAINTS; DIVERSITY; REDSHIFT; MODELS; SAMPLE AB Type Ia supernovae (SN Ia) are explosions of white dwarfs whose distances can be measured to a precision of similar to 5% using luminosity information that is encoded in the light curve shape. This property has been very successfully exploited to measure the history of cosmic expansion and to infer the presence of dark energy. But to learn the properties of dark energy and determine whether it is different from the cosmological constant demands higher precision and better accuracy than optical light curves alone can provide. The largest systematic uncertainties come from light curve fitters, photometric calibration errors, and from poor knowledge of the scattering properties of dust along the line of sight. Efforts to use SN Ia spectra as luminosity indicators have had some success, but have not produced a big step forward. Fortunately, observations of SN Ia in the near infrared (NIR), from 1 to 2 microns, offer a very promising path to better knowledge of the Hubble constant, improved constraints on dark energy, and, possibly, a route to discriminating the progenitor paths for SN Ia explosions. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kirshner, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM Kirshner@cfa.harvard.edu NR 53 TC 1 Z9 1 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01981-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2013 VL 281 BP 1 EP 8 DI 10.1017/S1743921312014573 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI40 UT WOS:000316706100003 ER PT S AU Di Stefano, R AF Di Stefano, Rosanne BE Di Stefano, R Orio, M Moe, M TI Studying the Progenitors of Type Ia Supernovae via Lensing with the Kepler Survey SO BINARY PATHS TO TYPE IA SUPERNOVAE EXPLOSIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 281st Symposium of the International-Astronomical-Union CY JUL 04-08, 2011 CL Padova, ITALY SP INAF, City Padova, Univ Padova, Dept Astronomy, INAF Padova Observ, ANEMOS DE supernovae; gravitational lensing ID COMPACT OBJECTS AB Every model for the progenitors of Type Ia supernovae (SNe Ia) requires that binaries pass through an epoch during which a white dwarf (WD) orbits a non-degenerate star. Depending on the mass of the WD, the radius of its companion, and the orbital separation, the WD may lens its companion. The lensing event would be an antitransit, an increase in light from the companion that can rise to the level of a percent or more, during an interval of hours. Antitransits are periodic. By studying them we can determine the properties of both the WD and its companion, as well as the characteristics of the orbit. Lensing events of this type are almost certain to be observed by the Kepler mission, while some can even be detected by ground-based surveys. Antitransits and transits will both provide valuable insight into the end states of common envelope evolution and of stable mass transfer, resolving issues that must be understood before we can fully unravel the progenitor puzzle. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rd@cfa.harvard.edu NR 8 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01981-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2013 VL 281 BP 34 EP 35 DI 10.1017/S1743921312014652 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI40 UT WOS:000316706100011 ER PT S AU Di Stefano, R Voss, R Claeys, J AF Di Stefano, R. Voss, R. Claeys, J. BE Di Stefano, R Orio, M Moe, M TI Spin-Up/Spin-Down Models SO BINARY PATHS TO TYPE IA SUPERNOVAE EXPLOSIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 281st Symposium of the International-Astronomical-Union CY JUL 04-08, 2011 CL Padova, ITALY SP INAF, City Padova, Univ Padova, Dept Astronomy, INAF Padova Observ, ANEMOS DE stars: white dwarfs; supernovae - accretion; accretion disks ID RAPIDLY ROTATING STARS; MASSIVE WHITE-DWARFS; IA SUPERNOVAE; BINARY-SYSTEM; AE-AQUARII; EVOLUTION AB Angular momentum transport plays an important role in mass transfer systems, and can significantly spin up an accreting star. When the accretor is a white dwarf (WD) on its way to becoming a Type Ia supernova (SN Ia), the spin up of the WD can have significant consequences for the appearance of the progenitor, the characteristics of the explosion and its aftermath, the geometry of the supernova remnant, and for single-degenerate models, the appearance of the donor star post-explosion. These consequences can be "game changers", altering results that have long been taken for granted. We discuss key features of our spin-up/spin-down models and their implications. We relate our models to work still needed to address the difficult physical issues related to angular momentum transport and its effects on the properties and appearance of Type la supernova progenitors. C1 [Di Stefano, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Voss, R.; Claeys, J.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rd@cfa.harvard.edu; R.Voss@astro.ru.nl; J.Claeys@astro.ru.nl NR 16 TC 0 Z9 0 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01981-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2013 VL 281 BP 64 EP + DI 10.1017/S1743921312014706 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI40 UT WOS:000316706100016 ER PT S AU Di Stefano, R AF Di Stefano, Rosanne BE Di Stefano, R Orio, M Moe, M TI The Appearance of Type Ia Supernova Progenitors: If Not SSSs, then What Do They Look Like? SO BINARY PATHS TO TYPE IA SUPERNOVAE EXPLOSIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 281st Symposium of the International-Astronomical-Union CY JUL 04-08, 2011 CL Padova, ITALY SP INAF, City Padova, Univ Padova, Dept Astronomy, INAF Padova Observ, ANEMOS DE stars: white dwarfs, binaries, supernovae; X-rays: binaries; cosmological parameters ID X-RAY SOURCES; SUPERSOFT SOURCES; IONIZATION; BINARIES; STATES; II. AB "What do the progenitors of Type Ia supernovae (SNe Ia) look like? How can we hope to find them?" We focus on the epoch during which mass is incident on a white dwarf (WD) at high rates (>10(-7)M(circle dot) yr(-1)). Such epochs are expected in single-degenerate (SD) progenitors, double-degenerate (DD) progenitors, and in a wide range of binaries with WDs that will not achieve the Chandrasekhar mass, M-Ch. High-rate accretion onto a WD produces high luminosities through accretion alone; in addition, most calculations show that quasisteady or episodic nuclear burning can occur, increasing the luminosity by more than an order of magnitude. If the photosphere is not much larger than the WD, the emission will have values of kT in the range of tens of eV, and the source will appear as a luminous supersoft x-ray source (SSS). Studies of local SSSs that are good candidates for nuclear-burning WDs (NBWDs) suggest that many have low duty cycles of SSS activity. This is consistent with the fact that binary WD models predict about 100 times as many SSSs in external galaxies of all types as are actually detected. Interstellar absorption does not appear to be the problem. Instead, it is likely that the similar to 10(37) - 10(38) erg s(-1) emitted by NBWDs emerges in other wavebands. The challenge we face is to search for highly luminous systems within the Milky Way and nearby galaxies that have unusual properties consistent with NBWDs, and inconsistent with other physical models. Model tests can then be conducted for individual candidates, allowing us to identify large numbers of progenitors years before explosion. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rd@cfa.harvard.edu NR 15 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01981-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2013 VL 281 BP 132 EP 135 DI 10.1017/S174392131201486X PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI40 UT WOS:000316706100032 ER PT S AU Moe, M Di Stefano, R AF Moe, Maxwell Di Stefano, Rosanne BE Di Stefano, R Orio, M Moe, M TI Population Synthesis of Type Ia SNe: Constraining Free Parameters from Observations SO BINARY PATHS TO TYPE IA SUPERNOVAE EXPLOSIONS SE IAU Symposium Proceedings Series LA English DT Proceedings Paper CT 281st Symposium of the International-Astronomical-Union CY JUL 04-08, 2011 CL Padova, ITALY SP INAF, City Padova, Univ Padova, Dept Astronomy, INAF Padova Observ, ANEMOS DE stars: AGB and post-AGB, white dwarfs, supernovae; binaries: close, symbiotic ID BINARIES; STARS AB Computing the rate of Type Ia supernovae (SNe Ia) from first principles is difficult because there are large uncertainties regarding several key binary processes such as common envelope evolution, tidal interactions, and the efficiency of mass transfer. Fortunately, a range of observational parameters of binaries in intermediate stages of evolution can help us model these processes in a way that is likely to mirror the true binary evolution. We discuss how this observationally-motivated approach may have the effect of increasing the predicted rate of single degenerate progenitors of SNe Ia, while simultaneously decreasing the number of double degenerate progenitors. C1 [Moe, Maxwell; Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moe, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmoe@cfa.harvard.edu; rd@cfa.harvard.edu NR 15 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA THE PITT BUILDING, TRUMPINGTON ST, CAMBRIDGE CB2 1RP, CAMBS, ENGLAND SN 1743-9213 BN 978-1-107-01981-2 J9 IAU SYMP P SERIES JI IAU Symposium Proc. Series PY 2013 VL 281 BP 240 EP 243 DI 10.1017/S1743921312015128 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BEI40 UT WOS:000316706100058 ER PT J AU Kirwan, ML Langley, JA Guntenspergen, GR Megonigal, JP AF Kirwan, M. L. Langley, J. A. Guntenspergen, G. R. Megonigal, J. P. TI The impact of sea-level rise on organic matter decay rates in Chesapeake Bay brackish tidal marshes SO BIOGEOSCIENCES LA English DT Article ID SALT-MARSH; LITTER DECOMPOSITION; VERTICAL ACCRETION; PEAT DECOMPOSITION; COASTAL MARSHES; WETLAND; ACCUMULATION; RESPONSES; TRENDS; FRESH AB The balance between organic matter production and decay determines how fast coastal wetlands accumulate soil organic matter. Despite the importance of soil organic matter accumulation rates in influencing marsh elevation and resistance to sea-level rise, relatively little is known about how decomposition rates will respond to sea-level rise. Here, we estimate the sensitivity of decomposition to flooding by measuring rates of decay in 87 bags filled with milled sedge peat, including soil organic matter, roots and rhizomes. Experiments were located in field-based mesocosms along 3 mesohaline tributaries of the Chesapeake Bay. Mesocosm elevations were manipulated to influence the duration of tidal inundation. Although we found no significant influence of inundation on decay rate when bags from all study sites were analyzed together, decay rates at two of the sites increased with greater flooding. These findings suggest that flooding may enhance organic matter decay rates even in water-logged soils, but that the overall influence of flooding is minor. Our experiments suggest that sea-level rise will not accelerate rates of peat accumulation by slowing the rate of soil organic matter decay. Consequently, marshes will require enhanced organic matter productivity or mineral sediment deposition to survive accelerating sea-level rise. C1 [Kirwan, M. L.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. [Langley, J. A.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Guntenspergen, G. R.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD USA. [Megonigal, J. P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kirwan, ML (reprint author), Univ Virginia, Dept Environm Sci, Clark Hall, Charlottesville, VA 22903 USA. EM mlk4n@virginia.edu FU USGS Global Change Research Program FX This work was supported by the USGS Global Change Research Program. We appreciate the efforts of R. Kyle Derby and Patrick Brennand in conducting field work. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the US Government. NR 46 TC 13 Z9 13 U1 10 U2 92 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 J9 BIOGEOSCIENCES JI Biogeosciences PY 2013 VL 10 IS 3 BP 1869 EP 1876 DI 10.5194/bg-10-1869-2013 PG 8 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 118FV UT WOS:000317010600041 ER PT J AU Wolski, A Henry, TJ AF Wolski, Andrzej Henry, Thomas J. TI Revision of the New World species of Peritropis Uhler (Hemiptera: Miridae: Cylapinae) (vol 43, pg 213, 2012) SO INSECT SYSTEMATICS & EVOLUTION LA English DT Correction C1 [Wolski, Andrzej] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. RP Wolski, A (reprint author), Opole Univ, Dept Biosystemat, Oleska 22, PL-45052 Opole, Poland. EM andrzej.wolski@uni.opole.pl NR 1 TC 2 Z9 2 U1 1 U2 2 PU APOLLO BOOKS PI STENSTRUP PA KIRKEBY SAND, 19, DK-5771 STENSTRUP, DENMARK SN 1399-560X J9 INSECT SYST EVOL JI Insect Syst. Evol. PY 2013 VL 44 IS 1 BP 107 EP 109 DI 10.1163/1876312X-04401005 PG 3 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 127LF UT WOS:000317699800004 ER PT J AU McNeill, DF Klaus, JS O'Connell, LG Coates, AG Morgan, WA AF McNeill, Donald F. Klaus, James S. O'Connell, Laura G. Coates, Anthony G. Morgan, William A. TI DEPOSITIONAL SEQUENCES AND STRATIGRAPHY OF THE COLON CARBONATE PLATFORM: BOCAS DEL TORO ARCHIPELAGO, PANAMA SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID ACROPORA-PALMATA; COSTA-RICA; NEOGENE; ISTHMUS; RECORD; SEAWAY; CIRCULATION; GEOLOGY; CLOSURE; RISE AB The Colon platform, located in the Bocas del Toro region of Panama, was studied as a near-modern analog for buried reefal platforms. The platform has an areal extent of similar to 90 km(2) and formed in a convergent tectonic setting (backarc) under a tropical climatic regime. The attached platform formed as part of a discontinuously rimmed shelf along the Caribbean side of the Isthmus of Panama and consisted of mixed carbonates and siliciclastics. Based on field relations and strontium-isotope stratigraphy, three depositional sequences were identified in the near-surface deposits of the uplifted platform. A Miocene to late Pliocene lithic sandstone unit (sequence 1, Old Bank Formation) forms the foundation of the platform. Coral-rich limestone and coral-rich siliciclastic units were deposited during both the late Pliocene (sequence 2, Isla Colon Formation) and early Pleistocene (sequence 3, Urraca Formation). In sequences 2 and 3 the sediment composition and fauna show distinct differences between the windward and leeward sides of the platform, with the main lithologic variable being the amount of siliciclastic sediment that was admixed with the biogenic carbonate sediments. The siliciclastic deposits (mud rich) in sequences 2 and 3 exhibit lower permeability and relatively minor diagenetic modification, and they lack major karst features. Conversely, the more carbonate-rich deposits are well cemented and strongly affected by meteoric dissolution and karstification. This facies-selective dissolution occurred when middle Pleistocene regional uplift exposed the platform to a tropical climate with high rainfall. Earthquakes and associated uplift of the platform over the past similar to 1 Myr intensely fractured the limestone. Fracture porosity has contributed to rapid infiltration of meteoric water and pervasive dissolution that resulted in numerous vertical sinks as well as an extensive network of horizontal conduits. A large, incised channel feature connects several of the pre-existing caves and conduits. The Colon platform limestone is a product of an equatorial humid carbonate system and is of size similar to platforms of Oligo-Miocene age near Malaysia (Sarawak), Indonesia, and farther north in the South China Sea. C1 [McNeill, Donald F.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Geol & Geophys, Miami, FL 33149 USA. [Klaus, James S.; O'Connell, Laura G.] Univ Miami, Dept Geol Sci, Coral Gables, FL 33124 USA. [Coates, Anthony G.] Smithsonian Trop Res Inst, Panama City, Panama. [Morgan, William A.] Conoco Phillips, Houston, TX 77252 USA. RP McNeill, DF (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Geol & Geophys, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM dmcneill@rsmas.miami.edu FU Smithsonian Tropical Research Institute; Bocas del Toro field station; ConocoPhillips; Industrial Associates of the CSL-Center for Carbonate Research FX This project was made possible through the financial and logistical support of the Smithsonian Tropical Research Institute, especially the Bocas del Toro field station. ConocoPhillips and the Industrial Associates of the CSL-Center for Carbonate Research provided support for fieldwork. We thank Peter Swart and the staff of the University of Miami Stable Isotope Laboratory for analyses related to Sr-isotope dating. We thank Bill Berggren for foraminifer identifications of Swan Cay material. ConocoPhillips allowed release of information collected during 2008 and 2009. We gratefully acknowledge collection and export permits from the Government of Panama. This manuscript benefited from comments by reviewers Steve Bachtel, Bob Loucks, Art Saller, Stacy Atchley, Lynn Soreghan, and editor Gene Rankey. NR 49 TC 4 Z9 4 U1 3 U2 29 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 EI 1938-3681 J9 J SEDIMENT RES JI J. Sediment. Res. PD JAN-FEB PY 2013 VL 83 IS 1-2 BP 155 EP 167 DI 10.2110/jsr.2013.13 PG 13 WC Geology SC Geology GA 127MN UT WOS:000317703200012 ER PT J AU Baker, AC McClanahan, TR Starger, CJ Boonstra, RK AF Baker, Andrew C. McClanahan, Tim R. Starger, Craig J. Boonstra, Roxane K. TI Long-term monitoring of algal symbiont communities in corals reveals stability is taxon dependent and driven by site-specific thermal regime SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Acclimatization; Adaptation; Adaptive bleaching hypothesis; Community change; Indian Ocean; Symbiosis ID CLIMATE-CHANGE; GENUS SYMBIODINIUM; TEMPERATURE-VARIATION; CARIBBEAN CORALS; BLEACHING EVENT; REEF CORALS; CLADE-D; DIVERSITY; ZOOXANTHELLAE; ENDOSYMBIONTS AB Survival trajectories for coral reefs under climate change may depend in part on shifts in the composition of their algal symbiont communities (Symbiodinium spp.). Shifts favoring thermotolerant symbionts have been recorded in response to mass bleaching events but rarely tracked through time. A 10 yr monitoring study of Symbiodinium in a variety of Kenyan corals assessed their variability through time, across coral taxa and between sites, and their relationship to environmental conditions. Coral genera varied significantly in their propensity to host thermotolerant symbionts of Symbiodinium clade D, with some genera becoming dominated by clade D at annual maximum temperatures of 32 degrees C but others showing clade D only rarely at 35 degrees C. High annual maximum temperatures, high standard deviation, positive skewness and positive kurtosis characterized sites where clade D was common. In corals whose symbiont communities were thermally labile (e. g. Pocillopora) an increase in maximum annual temperature from 30 to 35 degrees C resulted in 3- to 4-fold increases in dominance by clade D. There was no directional change in symbiont communities over the study period, but there was evidence for a similar to 6 yr decline in the incidence of mixed (C + D) communities following the 1998 bleaching event. These data illustrate how acute and chronic thermal stress caused by oceanographic and tidal oscillations interact to produce highly dynamic symbiotic communities. The clade D niche is a function of the environment and host taxon and, through a variety of mechanisms, is expected to expand with climate warming. Corals from warm and variable conditions represent conservation priorities because they establish a niche for these symbionts in contemporary reef environments. C1 [Baker, Andrew C.; Boonstra, Roxane K.] Univ Miami, Div Marine Biol & Fisheries, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA. [Baker, Andrew C.; McClanahan, Tim R.] Wildlife Conservat Soc, Marine Program, Bronx, NY 10460 USA. [Starger, Craig J.] Smithsonian Inst, Div Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20530 USA. [Starger, Craig J.] Amer Assoc Advancement Sci, Ctr Sci Policy & Soc Programs, Washington, DC 20005 USA. RP Baker, AC (reprint author), Univ Miami, Div Marine Biol & Fisheries, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Cswy, Miami, FL 33149 USA. EM abaker@rsmas.miami.edu OI McClanahan, Timothy/0000-0001-5821-3584 FU Wildlife Conservation Society through Western Indian Ocean Marine Science Association MASMA program; Tiffany Co. Foundation; Lenfest Ocean Program FX The Wildlife Conservation Society supported the research through grants from the Western Indian Ocean Marine Science Association MASMA program, and the Tiffany & Co. Foundation. A. C. B. and R. K. B. were also supported by the Lenfest Ocean Program. H. Wirshing and P. Jones provided laboratory assistance, and J. Maina assisted with obtaining the NOAA temperature data. The Kenyan Ministry of Science and Technology provided research clearance, and Kenya Wildlife Services provided the CITES permit. NR 51 TC 9 Z9 9 U1 1 U2 29 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PY 2013 VL 479 BP 85 EP + DI 10.3354/meps10102 PG 39 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA 122ZB UT WOS:000317356300007 ER PT J AU Bak, J Kim, JH Liu, X Chance, K Kim, J AF Bak, J. Kim, J. H. Liu, X. Chance, K. Kim, J. TI Evaluation of ozone profile and tropospheric ozone retrievals from GEMS and OMI spectra SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MONITORING INSTRUMENT; SATELLITE MEASUREMENTS; STRATOSPHERIC OZONE; RAMAN-SCATTERING; SENSITIVITY; ULTRAVIOLET; ALGORITHM; SCIAMACHY; CLIMATE; MISSION AB South Korea is planning to launch the GEMS (Geostationary Environment Monitoring Spectrometer) instrument into the GeoKOMPSAT (Geostationary Korea Multi-Purpose SATellite) platform in 2018 to monitor tropospheric air pollutants on an hourly basis over East Asia. GEMS will measure backscattered UV radiances covering the 300-500 nm wavelength range with a spectral resolution of 0.6 nm. The main objective of this study is to evaluate ozone profiles and stratospheric column ozone amounts retrieved from simulated GEMS measurements. Ozone Monitoring Instrument (OMI) Level 1B radiances, which have the spectral range 270-500 nm at spectral resolution of 0.42-0.63 nm, are used to simulate the GEMS radiances. An optimal estimation-based ozone profile algorithm is used to retrieve ozone profiles from simulated GEMS radiances. Firstly, we compare the retrieval characteristics (including averaging kernels, degrees of freedom for signal, and retrieval error) derived from the 270-330 nm (OMI) and 300330 nm (GEMS) wavelength ranges. This comparison shows that the effect of not using measurements below 300 nm on retrieval characteristics in the troposphere is insignificant. However, the stratospheric ozone information in terms of DFS decreases greatly from OMI to GEMS, by a factor of similar to 2. The number of the independent pieces of information available from GEMS measurements is estimated to 3 on average in the stratosphere, with associated retrieval errors of similar to 1% in stratospheric column ozone. The difference between OMI and GEMS retrieval characteristics is apparent for retrieving ozone layers above similar to 20 km, with a reduction in the sensitivity and an increase in the retrieval errors for GEMS. We further investigate whether GEMS can resolve the stratospheric ozone variation observed from high vertical resolution Earth Observing System (EOS) Microwave Limb Sounder (MLS). The differences in stratospheric ozone profiles between GEMS and MLS are comparable to those between OMI and MLS below similar to 3 hPa (similar to 40 km), except with slightly larger biases and larger standard deviations by up to 5 %. At pressure altitudes above similar to 3 hPa, GEMS retrievals show strong influence of a priori and large differences with MLS, which, however, can be sufficiently improved by using better a priori information. The GEMS-MLS differences show negative biases of less than 4% for stratospheric column ozone, with standard deviations of 1-3 %, while OMI retrievals show similar agreements with MLS except for 1% smaller biases at middle and high latitudes. Based on the comparisons, we conclude that GEMS will measure tropospheric ozone and stratospheric ozone columns with accuracy comparable to that of OMI and ozone profiles with slightly worse performance than that of OMI below 3 hPa. C1 [Bak, J.; Kim, J. H.] Pusan Natl Univ, Pusan, South Korea. [Liu, X.; Chance, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, J.] Yonsei Univ, Seoul 120749, South Korea. RP Kim, JH (reprint author), Pusan Natl Univ, Pusan, South Korea. EM jaekim@pusan.ac.kr RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU EcoInnovation Program of KEITI, Korea [ARQ201204015]; NASA; Smithsonian Institution FX This research was supported by the EcoInnovation Program of KEITI (ARQ201204015), Korea. Research at the Smithsonian Astrophysical Observatory was funded by NASA and the Smithsonian Institution. We acknowledge OMI and MLS science teams for providing the satellite data used in this study. NR 46 TC 9 Z9 9 U1 0 U2 20 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PY 2013 VL 6 IS 2 BP 239 EP 249 DI 10.5194/amt-6-239-2013 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 118FY UT WOS:000317011000007 ER PT J AU Debey, LB Pyenson, ND AF Debey, Lauren B. Pyenson, Nicholas D. TI Osteological correlates and phylogenetic analysis of deep diving in living and extinct pinnipeds: What good are big eyes? SO MARINE MAMMAL SCIENCE LA English DT Article DE allometry; diving depth; evolution; morphology; phylogenetic independent contrasts; Pinnipedia; skull; vision ID ANTARCTIC FUR SEALS; MARINE MAMMALS; NEW-ZEALAND; BODY-SIZE; INDEPENDENT CONTRASTS; CARNIVORA MAMMALIA; STATE RECONSTRUCTION; MOLECULAR PHYLOGENY; RESPONSE MECHANISM; FORAGING BEHAVIOR AB Marine tetrapods have evolved different sensory solutions to meet the ecological challenges of foraging at depth. It has been proposed that pinipeds, like ichthyosaurs, evolved large eyeballs for such demands. Here, we test this hypothesis using morphological and diving data from a comprehensive data set (n = 54 species; 435 individual specimens), including living and extinct pinnipeds and other select carnivorans as outgroup taxa. We used bony orbit size as a proxy for eyeball size, and recorded associated skull measurements to control for relative changes in orbit size; for diving depth, we used the deepest dive depth reported in the literature. Our analyses included both standard regressions and those corrected for phylogeny (i.e., independent contrasts). Standard regression statistics showed orbit size was a significantly good predictor of diving depth for phocids and for pinnipeds overall, although there was no correlation for otariids. In contrast, independent contrasts showed little support for a relationship between orbit size and diving depth for any group broader than family level, although this approach did demonstrate deep diving has evolved multiple times in crown Pinnipedia. Lastly, using select fossil taxa, we highlight the need to test adaptive hypotheses using comparative data in an evolutionary context. C1 [Debey, Lauren B.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Debey, Lauren B.; Pyenson, Nicholas D.] Univ Washington, Dept Paleontol, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Univ Washington, Dept Mammal, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA. RP Debey, LB (reprint author), Univ Washington, Dept Biol, Box 351800, Seattle, WA 98195 USA. EM lbdebey@uw.edu FU Biodiversity Synthesis Center at the Field Museum, Chicago; National Science Foundation; Natural Sciences and Engineering Research Council of Canada; Smithsonian Institution FX We thank S. Ingleby (AM), I. Westwig (AMNH), M. Flannery (CAS), N. Rybczynski (CMN), L. G. Barnes (LACM), C. Conroy (MVZ), T. A. Demere (SDNHM), P. A. Holroyd (UCMP), E. B. Davis (UOMNH), D. J. Bohaska, C. W. Potter and J. G. Mead (USNM), and J. Bradley and C. A. Sidor (UWBM) for their time and access to collections. We also especially thank A. Berta, E. B. Davis, T. A. Demere, E. M. G. Fitzgerald, J. Flynn, J. A. Goldbogen, A. Goswami, K. E. Jones, C. Kirk, I. Koretsky, D. R. Lindberg, J. F. Parham, L. Schmitz, C. A. Sidor, and G. P. Wilson for advice and discussion during the course of this study. For assistance with statistical analyses, we thank K. Ayres, M. Bryan, J. Hille Ris Lambers, D. Vilhena, and S. Yang. We thank M. Chen, G. P. Wilson, Editor D. Boness, Associate Editor D. P. Domning, and three anonymous reviewers for insightful comments on drafts of this paper. This study also benefited from valuable discussion at an Encyclopedia of Life synthesis meeting on the evolution and diversity of marine tetrapods funded by the Biodiversity Synthesis Center at the Field Museum, Chicago. This research was supported by National Science Foundation Graduate Research Fellowships to L. M. B. and N. D. P., and by funding from the Natural Sciences and Engineering Research Council of Canada and the Smithsonian Institution to N. D. P. NR 147 TC 9 Z9 9 U1 9 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JAN PY 2013 VL 29 IS 1 BP 48 EP 83 DI 10.1111/j.1748-7692.2011.00545.x PG 36 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 122AW UT WOS:000317288200004 ER PT J AU Reeder, DM Helgen, KM Vodzak, ME Lunde, DP Ejotre, I AF Reeder, DeeAnn M. Helgen, Kristofer M. Vodzak, Megan E. Lunde, Darrin P. Ejotre, Imran TI A new genus for a rare African vespertilionid bat: insights from South Sudan SO ZOOKEYS LA English DT Article DE Glauconycteris superba; Glauconycteris poensis; Glauconycteris curryae; Niumbaha gen. nov.; Badger Bat; South Sudan; Description ID CHIROPTERA AB A new genus is proposed for the strikingly patterned African vespertilionid "Glauconycteris" superba Hayman, 1939 on the basis of cranial and external morphological comparisons. A review of the attributes of a newly collected specimen from South Sudan (a new country record) and other museum specimens of "G." superba suggests that "G." superba is markedly distinct ecomorphologically from other species classified in Glauconycteris and is likely the sister taxon to Glauconycteris sensu stricto. The recent capture of this rarely collected but widespread bat highlights the need for continued research in tropical sub-Saharan Africa and in particular, for more work in western South Sudan, which has received very little scientific attention. New country records for G. cf. poensis (South Sudan) and G. curryae (Gabon) are also reported. C1 [Reeder, DeeAnn M.; Vodzak, Megan E.] Bucknell Univ, Dept Biol, Lewisburg, PA 17837 USA. [Helgen, Kristofer M.; Lunde, Darrin P.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Ejotre, Imran] Islamic Univ Uganda, Dept Biol Sci, Mbale, Uganda. RP Reeder, DM (reprint author), Bucknell Univ, Dept Biol, Lewisburg, PA 17837 USA. EM dreeder@bucknell.edu OI Reeder, DeeAnn/0000-0001-8651-2012 FU Woodtiger Fund FX We are indebted to Matthew Rice and Adrian Garside of Fauna & Flora International (FFI), who provided significant assistance with field logistics in South Sudan and who provided figure 1. Our thanks go to Lauren Helgen of the National Museum of Natural History (NMNH, Smithsonian Institution) for help with photographing specimens, Melissa Meierhofer of Bucknell University for illustrations, Aniko Toth and Paige Engelbrektsson for the distribution map, and to the Woodtiger Fund who graciously provided the funding for the 2012 expedition to South Sudan. NR 25 TC 4 Z9 4 U1 0 U2 9 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 285 BP 89 EP 115 DI 10.3897/zookeys.285.4892 PG 27 WC Zoology SC Zoology GA 119KO UT WOS:000317096400004 PM 23805046 ER PT J AU Bohm, M Collen, B Baillie, JEM Bowles, P Chanson, J Cox, N Hammerson, G Hoffmann, M Livingstone, SR Ram, M Rhodin, AGJ Stuart, SN van Dijk, PP Young, BE Afuang, LE Aghasyan, A Garcia, A Aguilar, C Ajtic, R Akarsu, F Alencar, LRV Allison, A Ananjeva, N Anderson, S Andren, C Ariano-Sanchez, D Arredondo, JC Auliya, M Austin, CC Avci, A Baker, PJ Barreto-Lima, AF Barrio-Amoros, CL Basu, D Bates, MF Batistella, A Bauer, A Bennett, D Bohme, W Broadley, D Brown, R Burgess, J Captain, A Carreira, S Castaneda, MD Castro, F Catenazzi, A Cedeno-Vazquez, JR Chapple, DG Cheylan, M Cisneros-Heredia, DF Cogalniceanu, D Cogger, H Corti, C Costa, GC Couper, PJ Courtney, T Crnobrnja-Isailovic, J Crochet, PA Crother, B Cruz, F Daltry, JC Daniels, RIR Das, I de Silva, A Diesmos, AC Dirksen, L Doan, TM Dodd, CK Doody, JS Dorcas, ME de Barros, JD Egan, VT El Mouden, E Embert, D Espinoza, RE Fallabrino, A Feng, X Feng, ZJ Fitzgerald, L Flores-Villela, O Franca, FGR Frost, D Gadsden, H Gamble, T Ganesh, SR Garcia, MA Garcia-Perez, JE Gatus, J Gaulke, M Geniez, P Georges, A Gerlach, J Goldberg, S Gonzalez, JCT Gower, DJ Grant, T Greenbaum, E Grieco, C Guo, P Hamilton, AM Hare, K Hedges, SB Heideman, N Hilton-Taylor, C Hitchmough, R Hollingsworth, B Hutchinson, M Ineich, I Iverson, J Jaksic, FM Jenkins, R Joger, U Jose, R Kaska, Y Kaya, U Keogh, JS Kohler, G Kuchling, G Kumlutas, Y Kwet, A La Marca, E Lamar, W Lane, A Lardner, B Latta, C Latta, G Lau, M Lavin, P Lawson, D LeBreton, M Lehr, E Limpus, D Lipczynski, N Lobo, AS Lopez-Luna, MA Luiselli, L Lukoschek, V Lundberg, M Lymberakis, P Macey, R Magnusson, WE Mahler, DL Malhotra, A Mariaux, J Maritz, B Marques, OAV Marquez, R Martins, M Masterson, G Mateo, JA Mathew, R Mathews, N Mayer, G McCranie, JR Measey, GJ Mendoza-Quijano, F Menegon, M Metrailler, S Milton, DA Montgomery, C Morato, SAA Mott, T Munoz-Alonso, A Murphy, J Nguyen, TQ Nilson, G Nogueira, C Nunez, H Orlov, N Ota, H Ottenwalder, J Papenfuss, T Pasachnik, S Passos, P Pauwels, OSG Perez-Buitrago, N Perez-Mellado, V Pianka, ER Pleguezuelos, J Pollock, C Ponce-Campos, P Powell, R Pupin, F Diaz, GEQ Radder, R Ramer, J Rasmussen, AR Raxworthy, C Reynolds, R Richman, N Rico, EL Riservato, E Rivas, G da Rocha, PLB Rodel, MO Schettino, LR Roosenburg, WM Ross, JP Sadek, R Sanders, K Santos-Barrera, G Schleich, HH Schmidt, BR Schmitz, A Sharifi, M Shea, G Shi, HT Shine, R Sindaco, R Slimani, T Somaweera, R Spawls, S Stafford, P Stuebing, R Sweet, S Sy, E Temple, HJ Tognelli, MF Tolley, K Tolson, PJ Tuniyev, B Tuniyev, S Uzum, N van Buurt, G Van Sluys, M Velasco, A Vences, M Vesely, M Vinke, S Vinke, T Vogel, G Vogrin, M Vogt, RC Wearn, OR Werner, YL Whiting, MJ Wiewandt, T Wilkinson, J Wilson, B Wren, S Zamin, T Zhou, K Zug, G AF Boehm, Monika Collen, Ben Baillie, Jonathan E. M. Bowles, Philip Chanson, Janice Cox, Neil Hammerson, Geoffrey Hoffmann, Michael Livingstone, Suzanne R. Ram, Mala Rhodin, Anders G. J. Stuart, Simon N. van Dijk, Peter Paul Young, Bruce E. Afuang, Leticia E. Aghasyan, Aram Garcia, Andres Aguilar, Cesar Ajtic, Rastko Akarsu, Ferdi Alencar, Laura R. V. Allison, Allen Ananjeva, Natalia Anderson, Steve Andren, Claes Ariano-Sanchez, Daniel Arredondo, Juan Camilo Auliya, Mark Austin, Christopher C. Avci, Aziz Baker, Patrick J. Barreto-Lima, Andre F. Barrio-Amoros, Cesar L. Basu, Dhruvayothi Bates, Michael F. Batistella, Alexandre Bauer, Aaron Bennett, Daniel Boehme, Wolfgang Broadley, Don Brown, Rafe Burgess, Joseph Captain, Ashok Carreira, Santiago Castaneda, Maria del Rosario Castro, Fernando Catenazzi, Alessandro Cedeno-Vazquez, Jose R. Chapple, David G. Cheylan, Marc Cisneros-Heredia, Diego F. Cogalniceanu, Dan Cogger, Hal Corti, Claudia Costa, Gabriel C. Couper, Patrick J. Courtney, Tony Crnobrnja-Isailovic, Jelka Crochet, Pierre-Andre Crother, Brian Cruz, Felix Daltry, Jennifer C. Daniels, R. I. Ranjit Das, Indraneil de Silva, Anslem Diesmos, Arvin C. Dirksen, Lutz Doan, Tiffany M. Dodd, C. Kenneth, Jr. Doody, J. Sean Dorcas, Michael E. de Barros Filho, Jose Duarte Egan, Vincent T. El Mouden, El Hassan Embert, Dirk Espinoza, Robert E. Fallabrino, Alejandro Feng, Xie Feng, Zhao-Jun Fitzgerald, Lee Flores-Villela, Oscar Franca, Frederico G. R. Frost, Darrell Gadsden, Hector Gamble, Tony Ganesh, S. R. Garcia, Miguel A. Garcia-Perez, Juan E. Gatus, Joey Gaulke, Maren Geniez, Philippe Georges, Arthur Gerlach, Justin Goldberg, Stephen Gonzalez, Juan-Carlos T. Gower, David J. Grant, Tandora Greenbaum, Eli Grieco, Cristina Guo, Peng Hamilton, Alison M. Hare, Kelly Hedges, S. Blair Heideman, Neil Hilton-Taylor, Craig Hitchmough, Rod Hollingsworth, Bradford Hutchinson, Mark Ineich, Ivan Iverson, John Jaksic, Fabian M. Jenkins, Richard Joger, Ulrich Jose, Reizl Kaska, Yakup Kaya, Ugur Keogh, J. Scott Koehler, Gunther Kuchling, Gerald Kumlutas, Yusuf Kwet, Axel La Marca, Enrique Lamar, William Lane, Amanda Lardner, Bjorn Latta, Craig Latta, Gabrielle Lau, Michael Lavin, Pablo Lawson, Dwight LeBreton, Matthew Lehr, Edgar Limpus, Duncan Lipczynski, Nicola Lobo, Aaron S. Lopez-Luna, Marco A. Luiselli, Luca Lukoschek, Vimoksalehi Lundberg, Mikael Lymberakis, Petros Macey, Robert Magnusson, William E. Mahler, D. Luke Malhotra, Anita Mariaux, Jean Maritz, Bryan Marques, Otavio A. V. Marquez, Rafael Martins, Marcio Masterson, Gavin Mateo, Jose A. Mathew, Rosamma Mathews, Nixon Mayer, Gregory McCranie, James R. Measey, G. John Mendoza-Quijano, Fernando Menegon, Michele Metrailler, Sebastien Milton, David A. Montgomery, Chad Morato, Sergio A. A. Mott, Tami Munoz-Alonso, Antonio Murphy, John Nguyen, Truong Q. Nilson, Goeran Nogueira, Cristiano Nunez, Herman Orlov, Nikolai Ota, Hidetoshi Ottenwalder, Jose Papenfuss, Theodore Pasachnik, Stesha Passos, Paulo Pauwels, Olivier S. G. Perez-Buitrago, Nestor Perez-Mellado, Valentin Pianka, Eric R. Pleguezuelos, Juan Pollock, Caroline Ponce-Campos, Paulino Powell, Robert Pupin, Fabio Quintero Diaz, Gustavo E. Radder, Raju Ramer, Jan Rasmussen, Arne R. Raxworthy, Chris Reynolds, Robert Richman, Nadia Rico, Edmund L. Riservato, Elisa Rivas, Gilson da Rocha, Pedro L. B. Roedel, Mark-Oliver Rodriguez Schettino, Lourdes Roosenburg, Willem M. Ross, James P. Sadek, Riyad Sanders, Kate Santos-Barrera, Georgina Schleich, Hermann H. Schmidt, Benedikt R. Schmitz, Andreas Sharifi, Mozafar Shea, Glenn Shi, Hai-Tao Shine, Richard Sindaco, Roberto Slimani, Tahar Somaweera, Ruchira Spawls, Steve Stafford, Peter Stuebing, Rob Sweet, Sam Sy, Emerson Temple, Helen J. Tognelli, Marcelo F. Tolley, Krystal Tolson, Peter J. Tuniyev, Boris Tuniyev, Sako Uzum, Nazan van Buurt, Gerard Van Sluys, Monique Velasco, Alvaro Vences, Miguel Vesely, Milan Vinke, Sabine Vinke, Thomas Vogel, Gernot Vogrin, Milan Vogt, Richard C. Wearn, Oliver R. Werner, Yehudah L. Whiting, Martin J. Wiewandt, Thomas Wilkinson, John Wilson, Byron Wren, Sally Zamin, Tara Zhou, Kaiya Zug, George TI The conservation status of the world's reptiles SO BIOLOGICAL CONSERVATION LA English DT Article DE IUCN Red List; Extinction risk; Threatened species; Lizards; Snakes; Turtles; Distribution maps ID BIODIVERSITY CONSERVATION; MOLECULAR PHYLOGENY; GLOBAL BIODIVERSITY; SPECIES-DIVERSITY; VERTEBRATES; AMPHIBIANS; CLIMATE; CLASSIFICATION; DISTRIBUTIONS; RADIATION AB Effective and targeted conservation action requires detailed information about species, their distribution, systematics and ecology as well as the distribution of threat processes which affect them. Knowledge of reptilian diversity remains surprisingly disparate, and innovative means of gaining rapid insight into the status of reptiles are needed in order to highlight urgent conservation cases and inform environmental policy with appropriate biodiversity information in a timely manner. We present the first ever global analysis of extinction risk in reptiles, based on a random representative sample of 1500 species (16% of all currently known species). To our knowledge, our results provide the first analysis of the global conservation status and distribution patterns of reptiles and the threats affecting them, highlighting conservation priorities and knowledge gaps which need to be addressed urgently to ensure the continued survival of the world's reptiles. Nearly one in five reptilian species are threatened with extinction, with another one in five species classed as Data Deficient. The proportion of threatened reptile species is highest in freshwater environments, tropical regions and on oceanic islands, while data deficiency was highest in tropical areas, such as Central Africa and Southeast Asia, and among fossorial reptiles. Our results emphasise the need for research attention to be focussed on tropical areas which are experiencing the most dramatic rates of habitat loss, on fossorial reptiles for which there is a chronic lack of data, and on certain taxa such as snakes for which extinction risk may currently be underestimated due to lack of population information. Conservation actions specifically need to mitigate the effects of human-induced habitat loss and harvesting, which are the predominant threats to reptiles. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Boehm, Monika; Collen, Ben; Ram, Mala; Richman, Nadia; Wearn, Oliver R.] Zool Soc London, Inst Zool, London NW1 4RY, England. [Baillie, Jonathan E. 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[Malhotra, Anita] Bangor Univ, Coll Nat Sci, Sch Biol Sci, Bangor LL57 2UW, Gwynedd, Wales. [Mariaux, Jean] Museum Nat Hist, CH-1208 Geneva, Switzerland. [Maritz, Bryan; Masterson, Gavin] Univ Witwatersrand, Sch Anim Plant & Environm Sci, ZA-2050 Johannesburg, South Africa. [Marques, Otavio A. V.] Inst Butantan, Lab Ecol & Evolucao, BR-05503900 Sao Paulo, Brazil. [Marquez, Rafael] CSIC, Museo Nacl Ciencias Nat, Dept Biodiversidad & Biol Evolut, E-28006 Madrid, Spain. [Mateo, Jose A.] Univ Las Palmas, BIOGES, Las Palmas Gran Canaria 35001, Canary Islands, Spain. [Mathew, Rosamma] Zool Survey India, North Eastern Reg Ctr, Shillong 793003, Meghalaya, India. [Mayer, Gregory] Univ Wisconsin Parkside, Dept Biol Sci, Kenosha, WI 53141 USA. [Measey, G. John] North West Univ, Sch Environm Sci & Dev, ZA-2520 Potchefstroom, South Africa. [Mendoza-Quijano, Fernando] Inst Tecnol Huejutla, Huejutla De Reyes 43000, Hidalgo, Mexico. [Menegon, Michele; Pupin, Fabio] Museo Tridentino Sci Nat, I-38122 Trento, Italy. [Milton, David A.] CSIRO Marine & Atmospher Res, Cleveland, Qld 4163, Australia. [Montgomery, Chad] Truman State Univ, Kirksville, MO 63501 USA. [Morato, Sergio A. A.] Univ Tuiuti Parana, Curitiba, Parana, Brazil. [Mott, Tami] Univ Fed Mato Grosso, Inst Biociencias, Dept Biol & Zool, Cuiaba, Brazil. [Munoz-Alonso, Antonio] El Colegio Frontera Sur, Chiapas, Mexico. [Murphy, John; Stuebing, Rob] Field Museum Nat Hist, Chicago, IL 60605 USA. [Nguyen, Truong Q.] Inst Ecol & Biol Resources, Hanoi, Vietnam. [Nilson, Goeran] Goteborg Nat Hist Museum, SE-40235 Gothenburg, Sweden. [Nogueira, Cristiano] Univ Brasilia, Dept Zool, BR-70910900 Brasilia, DF, Brazil. [Nunez, Herman] Museo Nacl Hist Nat, Santiago, Chile. [Ota, Hidetoshi] Univ Hyogo, Inst Nat & Environm Sci, Sanda, Hyogo 6691546, Japan. [Papenfuss, Theodore] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Pasachnik, Stesha] Univ Tennessee, Knoxville, TN 37996 USA. [Passos, Paulo] Univ Fed Rio de Janeiro, Museu Nacl, Dept Vertebrados, BR-20940040 Rio De Janeiro, RJ, Brazil. [Pauwels, Olivier S. G.] Inst Royal Sci Nat Belg, B-1000 Brussels, Belgium. [Perez-Buitrago, Nestor] Univ Puerto Rico, San Juan, PR 00936 USA. [Perez-Mellado, Valentin] Univ Salamanca, Fac Biol, E-37008 Salamanca, Spain. [Pianka, Eric R.] Univ Texas Austin, Austin, TX 78712 USA. [Pleguezuelos, Juan] Univ Granada, Dep Anim Biol, Fac Sci, E-18071 Granada, Spain. [Ponce-Campos, Paulino] Basque Trop AC, Jocotepec 45800, Jalisco, Mexico. [Powell, Robert] Avila Univ, Dept Biol, Kansas City, MO 64145 USA. [Quintero Diaz, Gustavo E.] Univ Autonoma Aguascalientes, Aguascalientes, Mexico. [Radder, Raju; Shine, Richard; Somaweera, Ruchira] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia. [Ramer, Jan] Indianapolis Zoo, Indianapolis, IN 46222 USA. [Rasmussen, Arne R.] Royal Danish Acad Fine Arts, Sch Conservat, DK-1263 Copenhagen K, Denmark. [Reynolds, Robert] Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. [Rico, Edmund L.] Int Inst Rural Reconstruct YC James Yen Ctr Silan, Cavite 4118, Philippines. [Rivas, Gilson] Univ Zulia, Fac Ciencias Expt, Museo Biol, Maracaibo 4011, Zulia, Venezuela. [da Rocha, Pedro L. B.] Univ Fed Bahia, Inst Biol, BR-40170290 Salvador, BA, Brazil. [Roedel, Mark-Oliver] Humboldt Univ, Museum Naturkunde, D-10115 Berlin, Germany. [Rodriguez Schettino, Lourdes] Inst Ecol & Systemat, Havana, Cuba. [Roosenburg, Willem M.] Ohio Univ, Dept Biol Sci, Ohio Ctr Ecol & Evolutionary Studies, Athens, OH 45701 USA. [Sadek, Riyad] Amer Univ Beirut, Dept Biol, Beirut, Lebanon. [Sanders, Kate] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Santos-Barrera, Georgina] Univ Nacl Autonoma Mexico, Fac Ciencias, Mexico City 04510, DF, Mexico. [Schleich, Hermann H.] Inst & Nucl Zool ARCO, E-04200 Tabernas, Spain. [Schmidt, Benedikt R.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland. [Schmidt, Benedikt R.] Karch, CH-2000 Neuchatel, Switzerland. [Schmitz, Andreas] Museum Hist Nat, Dept Herpetol & Ichthyol, CH-1208 Geneva, Switzerland. [Sharifi, Mozafar] Razi Univ, Dept Biol, Kermanshah, Iran. [Shi, Hai-Tao] Hainan Normal Univ, Coll Life Sci, Haikou 571158, Peoples R China. [Spawls, Steve] City Coll, Dept Hlth & Sci, Norwich NR2 2LJ, Norfolk, England. [Sweet, Sam] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Temple, Helen J.] Biodivers Consultancy, Cambridge, England. [Tognelli, Marcelo F.] Inst Argentina Invest Zonas Aridas IADIZA CONICET, RA-5500 Mendoza, Argentina. [Tolley, Krystal] South African Natl Biodivers Inst, ZA-7735 Cape Town, South Africa. [Tolson, Peter J.] Toledo Zoo, Toledo, OH 43614 USA. [Van Sluys, Monique] Univ Estado Rio de Janeiro, IBRAG, Dept Ecol, BR-20550013 Rio De Janeiro, Brazil. [Velasco, Alvaro] IUCN SSC Crocodile Specialist Grp, Caracas, Venezuela. [Vences, Miguel] Tech Univ Carolo Wilhelmina Braunschweig, D-38092 Braunschweig, Germany. [Vesely, Milan] Palacky Univ, CR-77147 Olomouc, Czech Republic. [Vogel, Gernot] Soc Southeast Asian Herpetol, D-69115 Heidelberg, Germany. [Vogrin, Milan] DPPVN, Race, Slovenia. [Werner, Yehudah L.] Hebrew Univ Jerusalem, Inst Life Sci EEB, IL-91904 Jerusalem, Israel. [Werner, Yehudah L.] Senckenberg Dresden, Museum Tierkunde, D-01109 Dresden, Germany. [Whiting, Martin J.] Macquarie Univ, Sydney, NSW 2109, Australia. [Wiewandt, Thomas] Wild Horizons Inc, Tucson, AZ 85703 USA. [Wilkinson, John] Amphibian & Reptile Conservat, Bournemouth BH1 4AP, Dorset, England. [Wilson, Byron] Univ W Indies, Mona, Jamaica. [Zamin, Tara] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Zhou, Kaiya] Nanjing Normal Univ, Coll Life Sci, Nanjing, Jiangsu, Peoples R China. RP Bohm, M (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM monika.bohm@ioz.ac.uk RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016; Fachbereich14, Dekanat/C-8553-2015; Lukoschek, Vimoksalehi/C-6126-2013; Georges, Arthur/D-2153-2009; Perez-Mellado, Valentin/G-3476-2015; Martins, Marcio/C-1150-2011; Nogueira, Cristiano/I-5100-2012; Keogh, Scott/C-8441-2009; Somaweera, Ruchira/G-7531-2014; Rocha, Pedro Luis/A-3325-2008; Collen, Ben/F-2543-2016; Courtney, Anthony/C-7867-2009; Cisneros-Heredia, Diego/D-1744-2011; Alencar, Laura/E-2030-2013; Lehr, Edgar/K-1210-2016; Barreto-Lima, A/E-3383-2015; Schmidt, Benedikt/B-8491-2008; Catenazzi, Alessandro/C-8615-2009; Gadsden, Hector/A-2066-2015; Marquez, Rafael/E-4454-2013; Costa, Gabriel/A-4147-2008; Measey, G John/F-2028-2010; Cogalniceanu, Dan/B-7065-2011; Chapple, David/B-9073-2008; Franca, Frederico/M-6718-2013; Nguyen, Truong/F-3730-2012; jaksic, Fabian/G-1705-2014; Hoffmann, Michael/E-6419-2010; Magnusson, William/J-9408-2014 OI Malhotra, Anita/0000-0002-1738-9046; Hare, Kelly/0000-0002-9473-5256; Tognelli, Marcelo/0000-0002-9761-4505; Whiting, Martin/0000-0002-4662-0227; Mariaux, Jean/0000-0002-9601-855X; Zamin, Tara/0000-0002-0991-6651; Lukoschek, Vimoksalehi/0000-0002-0268-3808; Gerlach, Justin/0000-0002-0157-0449; Marquez, Rafael/0000-0002-2070-860X; Rocha, Pedro Luis Bernardo da/0000-0002-8330-483X; Vences, Miguel/0000-0003-0747-0817; Georges, Arthur/0000-0003-2428-0361; Perez-Mellado, Valentin/0000-0002-7137-4945; Martins, Marcio/0000-0001-8108-6309; Keogh, Scott/0000-0002-1373-6186; Collen, Ben/0000-0003-2564-4243; Cisneros-Heredia, Diego/0000-0002-6132-2738; Lehr, Edgar/0000-0002-0517-390X; Barreto-Lima, A/0000-0002-3686-6573; Schmidt, Benedikt/0000-0002-4023-1001; Catenazzi, Alessandro/0000-0002-3650-4783; Costa, Gabriel/0000-0002-6777-6706; Measey, G John/0000-0001-9939-7615; Cogalniceanu, Dan/0000-0003-2959-014X; Chapple, David/0000-0002-7720-6280; Franca, Frederico/0000-0001-6989-2455; Hoffmann, Michael/0000-0003-4785-2254; FU Esmee Fairbairn Foundation; Rufford Foundation; Regina Bauer Frankenberg Foundation for Animal Welfare; Moore Family Foundation; Gordon and Betty Moore Foundation; Conservation International, Critical Ecosystem Partnership Fund (CEPF); European Commission; Zayed Species Conservation Fund; Conservation International Madagascar; Darwin Initiative FX MB and MR were funded by a grant from the Esmee Fairbairn Foundation, BC by the Rufford Foundation. North American and Mexican species assessments were funded by the Regina Bauer Frankenberg Foundation for Animal Welfare. Species assessments under the Global Reptile Assessment (GRA) initiative are supported by: Moore Family Foundation, Gordon and Betty Moore Foundation, Conservation International, Critical Ecosystem Partnership Fund (CEPF), and European Commission. Additional acknowledgements are included in the online supplementary material.; The assessment workshop for Mexican reptiles was kindly hosted by Ricardo Ayala and the station personnel of the Estacion de Biologia Chamela, Institut de Biologia, Universidad Nacional Autonoma de Mexico. Workshop and logistical organisation of the Philippines assessments was provided by the Conservation International Philippines Office, in particular Ruth Grace Rose Ambal, Melizar V. Duya and Oliver Coroza. Workshop and logistical organisation for the European Reptile and Amphibian Assessments was provided by Doga Dernegi, in particular Ozge Balkiz and Ozgur Koc. Workshop and logistical organisation for assessments of sea snakes and homalopsids was provided by the International Sea Turtle Symposium and Dr. Colin Limpus (Australian Government Environmental Protection Agency). Special thanks to Jenny Chapman (EPA) and Chloe Schaub le (ISTS). Thank you also to Dr. Gordon Guymer (Chief Botanist Director of Herbarium) for accommodating us at the Herbarium in the Brisbane Botanical Gardens, and Mark Read and Kirsten Dobbs (Great Barrier Reef Marine Parks Association) and Dave Pollard and Brad Warren (Ocean Watch Australia) for institutional support. Mohamed Bin Zayed Species Conservation Fund, Conservation International Madagascar and the Darwin Initiative contributed to funding the costs of the Madagascar reptile workshop. NR 48 TC 190 Z9 196 U1 58 U2 396 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD JAN PY 2013 VL 157 BP 372 EP 385 DI 10.1016/j.biocon.2012.07.015 PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 113FF UT WOS:000316651200043 ER PT J AU Gowaty, PA Kim, YK Anderson, WW AF Gowaty, Patricia Adair Kim, Yong-Kyu Anderson, Wyatt W. TI Mendel's law reveals fatal flaws in Bateman's 1948 study of mating and fitness SO FLY LA English DT Article DE fitness variances; number of mates; number of offspring; reproductive success; Mendel's rules; Drosophila melanogaster; AJ Bateman; genetic parentage tests ID SEXUAL SELECTION; EASTERN BLUEBIRDS; MATE CHOICE; PRINCIPLES; EVOLUTION; SUCCESS; FERTILIZATIONS; CONSTRAINTS; VALIDATION; REPETITION C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolut Biol, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Washington, DC USA. [Kim, Yong-Kyu; Anderson, Wyatt W.] Univ Georgia, Dept Genet, Athens, GA 30602 USA. [Kim, Yong-Kyu] Emory Univ, Dept Biol, Atlanta, GA 30322 USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolut Biol, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu; yongkyu@uga.edu; wyatt@uga.edu FU NSF [IBN-9631801, IBN-0911606, IOS-1121797] FX We thank Stephen P. Hubbell for comments on the manuscript and Margaret Anderson for technical support and advice. We gratefully acknowledge funding from NSF grants IBN-9631801, IBN-0911606, IOS-1121797 to P.A.G. and W.W.A., which provided support for various aspects of the work reported here. Attributions: P.A.G., W.W.A. and Y.K.K. designed the original research; technicians blind to the purpose of our study, under the supervision of W.W.A. and Y.K.K., performed the experiments; P.A.G. performed analyses, made figures and wrote the papers. NR 39 TC 2 Z9 2 U1 2 U2 39 PU LANDES BIOSCIENCE PI AUSTIN PA 1806 RIO GRANDE ST, AUSTIN, TX 78702 USA SN 1933-6934 J9 FLY JI Fly PD JAN-MAR PY 2013 VL 7 IS 1 DI 10.4161/fly.23505 PG 11 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 115BO UT WOS:000316787500006 PM 23360967 ER PT J AU Kamble, A Kaplan, DLA AF Kamble, Atish Kaplan, David L. A. TI ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES: MERGERS OF COMPACT OBJECTS SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article DE Gravitational waves ID GAMMA-RAY BURST; SUPERMASSIVE BLACK-HOLES; NEUTRON-STAR MERGERS; PERTURBATIONS; EXPLOSIONS; SUPERNOVA; SPECTRA; ENERGY; JETS AB Mergers of compact objects are considered prime sources of gravitational waves (GW) and will soon be targets of GW observatories such as the Advanced-LIGO and VIRGO. Finding electromagnetic counterparts of these GW sources will be important to understand their nature. We discuss possible electromagnetic signatures of the mergers. We show that the BH-BH mergers could have luminosities which exceed Eddington luminosity from unity to several orders of magnitude depending on the masses of the merging BHs. As a result these mergers could be explosive, release up to 10(51) erg of energy and shine as radio transients. At any given time we expect about a few such transients in the sky at GHz frequencies, which could be detected to be about 300 Mpc. It has also been argued that these radio transients would look alike radio supernovae with comparable detection rates. Multi-band follow-up could, however, distinguish between the mergers and supernovae. C1 [Kamble, Atish] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaplan, David L. A.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53211 USA. RP Kamble, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM akamble@cfa.harvard.edu; kaplan@uwm.edu FU NSF [AST-1008353] FX A. Kamble gratefully acknowledges the organizers of the ASTROD-5 meeting and Raman Research Institute for invitation, support and hospitality. The authors thank the anonymous referee for a prompt and helpful review which improved this paper. A. Kamble and D. L. A. Kaplan were partially supported by NSF award AST-1008353. NR 37 TC 8 Z9 8 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD JAN PY 2013 VL 22 IS 1 SI SI AR 1341011 DI 10.1142/S0218271813410113 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 116UA UT WOS:000316907300012 ER PT J AU Rick, TC Fitzpatrick, SM AF Rick, Torben C. Fitzpatrick, Scott M. TI Eight and Counting SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Editorial Material C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Fitzpatrick, Scott M.] 1218 Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, POB 37012, Washington, DC 20013 USA. EM rickt@si.edu; smfitzpa@uoregon.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PD JAN 1 PY 2013 VL 8 IS 1 BP 1 EP 2 DI 10.1080/15564894.2013.767103 PG 2 WC Archaeology SC Archaeology GA 117CJ UT WOS:000316929400001 ER PT J AU Fitzhugh, WW AF Fitzhugh, William W. TI Archaeology and the Sea in Scandinavia and Britain. A Personal Account SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Book Review C1 [Fitzhugh, William W.] Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Dept Anthropol, POB 37012,MRC 112, Washington, DC 20013 USA. EM fitzhugh@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PD JAN 1 PY 2013 VL 8 IS 1 BP 144 EP 146 DI 10.1080/15564894.2012.736918 PG 3 WC Archaeology SC Archaeology GA 117CJ UT WOS:000316929400010 ER PT J AU Restrepo, JC Franco, D Escobar, J Correa, ID Otero, L Gutierrez, J AF Restrepo, Juan C. Franco, Diana Escobar, Jaime Dario Correa, Ivan Otero, Luis Gutierrez, Julio TI Cartagena Bay (Colombia): superficial sediments distribution and sedimentary environments SO LATIN AMERICAN JOURNAL OF AQUATIC RESEARCH LA Spanish DT Article DE surface sediment; textural analysis; sedimentary environments; Cartagena Bay; Dike Channel; Colombia ID GRAIN-SIZE DISTRIBUTION; DISTRIBUTION PATTERNS AB We studied the spatial distribution and textural characteristics of 234 surface sediment samples from the Bay of Cartagena, Colombia, to understand sedimentation processes over the last few decades. We used three discriminant functions to characterize depositional environments and to differentiate among: (i) beach deposits and sediments of high-energy, shallow marine environments, (ii) fluvial deposits and sediments of shallow marine environments, and (iii) fluvial deposits influenced by turbidity currents. The predominant sediment type is a medium-size (5.35 +/- 1.2 phi), poorly sorted (sigma = 1.63 +/- 0.8) mud, with a noticeable asymmetry (S-k = -0.052 +/- 0.2) and kurtosis (k) of 0.84 +/- 0.4. There were two main superficial sediments types in the Bay of Cartagena: (1) sediments of high-energy, shallow marine environments with high fluvial influence, and (2) turbidity current deposits with high fluvial influence. Sediments with the lowest sand content (<5%) are located along a latitudinal axis running from the Dike Channel prodelta to the western end of Tierrabomba Island. The CaCO3 content of the sediments is <10%. Autogenous calcareous sediments are covered by fine terrigenous sediment transported through the Dike Canal, which has a more active and dominant role in the Bay's sediment deposition than previously reported. C1 [Franco, Diana] Univ Ind Santander, Inst Colombiano Petr, Grp Invest Estratig, Bucaramanga, Colombia. [Escobar, Jaime] Univ Norte UNINORTE, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst STRI, Ctr Trop Paleoecol & Archeol CTPA, Panama City, Panama. [Dario Correa, Ivan] Univ Eafit, Dept Geol, Grp Ciencias Mar, Medellin, Colombia. [Gutierrez, Julio] Ctr Invest Oceanog & Hidrog, Area Manejo Integral Zonas Costeras, Direcc Gen Maritima, Cartagena, Colombia. EM restrepocj@uninorte.edu.co OI Restrepo, Juan Camilo/0000-0001-5696-8625 NR 40 TC 1 Z9 1 U1 0 U2 10 PU UNIV CATOLICA DE VALPARAISO PI VALPARAISO PA AV BRASIL 2950, PO BOX 4059, VALPARAISO, CHILE SN 0718-560X J9 LAT AM J AQUAT RES JI Lat. Am. J. Aquat. Res. PY 2013 VL 41 IS 1 BP 99 EP 112 DI 10.3856/vol41-issue1-fulltext-8 PG 14 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 115YO UT WOS:000316848000008 ER PT J AU Weatherford, E Niro, S AF Weatherford, Elizabeth Niro, Shelley BE Marubbio, ME Buffalohead, EL TI The Journey's Discovery An Interview with Shelley Niro SO NATIVE AMERICANS ON FILM: CONVERSATIONS, TEACHING, AND THEORY LA English DT Editorial Material; Book Chapter C1 [Weatherford, Elizabeth] NMAI, Smithsonian Natl Museum Amer Indian, Film & Video Ctr, New York, NY USA. [Weatherford, Elizabeth] NYU, Program Media & Culture, New York, NY 10003 USA. [Weatherford, Elizabeth] NYU, Sch Visual Arts, New York, NY 10003 USA. [Weatherford, Elizabeth] NYU, New Sch, New York, NY 10003 USA. RP Weatherford, E (reprint author), NYU, Dept Anthropol, New York, NY 10003 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV PRESS KENTUCKY PI LEXINGTON PA 102 LAFFERTY HALL, UNIVERSITY OF KENTUCKY, LEXINGTON, KY 40506 USA BN 978-0-8131-3681-3 PY 2013 BP 337 EP 358 PG 22 WC Ethnic Studies; Film, Radio, Television SC Ethnic Studies; Film, Radio & Television GA BEE15 UT WOS:000316260900018 ER PT J AU Loss, SR Will, T Marra, PP AF Loss, Scott R. Will, Tom Marra, Peter P. TI The impact of free-ranging domestic cats on wildlife of the United States SO NATURE COMMUNICATIONS LA English DT Article ID TRAP-NEUTER-RETURN; HOUSE CATS; PREDATION; ISLAND; CONSERVATION; MANAGEMENT; AUSTRALIA; CANBERRA AB Anthropogenic threats, such as collisions with man-made structures, vehicles, poisoning and predation by domestic pets, combine to kill billions of wildlife annually. Free-ranging domestic cats have been introduced globally and have contributed to multiple wildlife extinctions on islands. The magnitude of mortality they cause in mainland areas remains speculative, with large-scale estimates based on non-systematic analyses and little consideration of scientific data. Here we conduct a systematic review and quantitatively estimate mortality caused by cats in the United States. We estimate that free-ranging domestic cats kill 1.4-3.7 billion birds and 6.9-20.7 billion mammals annually. Un-owned cats, as opposed to owned pets, cause the majority of this mortality. Our findings suggest that free-ranging cats cause substantially greater wildlife mortality than previously thought and are likely the single greatest source of anthropogenic mortality for US birds and mammals. Scientifically sound conservation and policy intervention is needed to reduce this impact. C1 [Loss, Scott R.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Will, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN USA. RP Loss, SR (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,POB 37012 MRC 5503, Washington, DC 20013 USA. EM LossS@si.edu RI Loss, Scott/B-1504-2014 FU US Fish and Wildlife Service through the Smithsonian Conservation Biology Institute's Postdoctoral Fellowship programme FX S.R.L. was supported by a postdoctoral fellowship funded by the US Fish and Wildlife Service through the Smithsonian Conservation Biology Institute's Postdoctoral Fellowship programme. P. Blancher provided insight for development of the model of cat predation magnitude, and R. Kays, C. Lepczyk and Y. van Heezik provided raw data from their publications. C. Machtans facilitated data sharing, and participants in the 2011 Society of Canadian Ornithologists' anthropogenic mortality of birds symposium provided context and perspectives. C. Lepczyk and P. Blancher provided comments on the manuscript. The findings and conclusions in this article are those of the authors and do not necessarily represent the views of the Smithsonian or US Fish and Wildlife Service. All data used for this analysis is available in the Supplementary Materials. NR 41 TC 100 Z9 102 U1 30 U2 336 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JAN PY 2013 VL 4 AR 1396 DI 10.1038/ncomms2380 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 112SV UT WOS:000316614600066 PM 23360987 ER PT J AU Cognato, AI Rabaglia, RJ Vandenberg, NJ AF Cognato, Anthony I. Rabaglia, Robert J. Vandenberg, Natalia J. TI Another Asian ambrosia beetle, Xyleborinus artestriatus (Eichhoff 1878) (Coleoptera: Curculionidae: Scolytinae: Xyleborini), newly detected in North America SO PAN-PACIFIC ENTOMOLOGIST LA English DT Article DE Coleoptera; Curculionidae; Scolytidae; Xyleborini; Xyleborinus artestriatus; new North American record; exotic species AB Xyleborinus artestriatus (Eichhoff 1878), an ambrosia beetle native to Asia, is reported for the first time in North America based on specimens from Georgia and Texas. This is the twenty-fourth species of exotic Xyleborini documented in North America. North American distributional records, key identification characteristics, morphological variability, and a brief history of the systematics are presented. C1 [Cognato, Anthony I.] Michigan State Univ, Dept Entomol, E Lansing, MI 48824 USA. [Rabaglia, Robert J.] USDA, Forest Serv, Arlington, VA 22209 USA. [Vandenberg, Natalia J.] Agr Res Serv, SEL, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Cognato, AI (reprint author), Michigan State Univ, Dept Entomol, 288 Farm Lane, E Lansing, MI 48824 USA. EM cognato@msu.edu; brabaglia@fs.fed.us; Natalia.Vandenberg@ars.usda.gov FU USDA-FS EDRR program [07-DG-11420004-257] FX We thank Kayla Brownell (University of Georgia) for maintaining the traps and screening out the original specimens from Port Wentworth, Georgia, and Bobby Brown, USDA-APHIS, for recognizing the specimens as different from known U.S. species. We also thank Terry Price for maintaining traps in Port Wentworth in 2011 and Rick Hoebeke (University of Georgia) for identifying the additional specimens from those traps. Thanks also to the Master Naturalists of Texas who maintained the FS EDRR traps around Houston. We appreciate Harald Schillhammer's help to access Schedl's collection in the Vienna Natural History Museum. The USDA-FS EDRR program funded this study, in part (# 07-DG-11420004-257 to AIC). USDA is an equal opportunity provider and employer. NR 15 TC 2 Z9 2 U1 1 U2 2 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 EI 2162-0237 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD JAN PY 2013 VL 89 IS 1 BP 27 EP 31 PG 5 WC Entomology SC Entomology GA 118KC UT WOS:000317023400004 ER PT J AU Venegas, PJ Torres-Carvajal, O Duran, V de Queiroz, K AF Venegas, Pablo J. Torres-Carvajal, Omar Duran, Vilma de Queiroz, Kevin TI Two sympatric new species of woodlizards (Hoplocercinae, Enyalioides) from Cordillera Azul National Park in northeastern Peru SO ZOOKEYS LA English DT Article DE Cordillera Azul; Enyalioides; Hoplocercinae; new species; Peru; systematics AB We report the discovery of two sympatric new species of Enyalioides from a montane rainforest of the Rio Huallaga basin in northeastern Peru. Among other characters, the first new species is distinguishable from other Enyalioides by the combination of the following characters: strongly keeled ventral scales, more than 37 longitudinal rows of dorsals in a transverse line between the dorsolateral crests at midbody, low vertebral crest on the neck with vertebrals on neck similar in size to those between hind limbs, projecting scales on body or limbs absent, 96 mm maximum SVL in both sexes, and caudals increasing in size posteriorly within each autotomic segment. The second new species differs from other species of Enyalioides in having strongly keeled ventral scales, scales posterior to the superciliaries forming a longitudinal row of strongly projecting scales across the lateral edge of the skull roof in adults of both sexes, 31 or fewer longitudinal rows of strongly keeled dorsals in a transverse line between the dorsolateral crests at midbody, vertebrals on neck more than five times the size of vertebrals between hind limbs in adult males, projecting scales on body or limbs absent, and caudals increasing in size posteriorly within each autotomic segment. We also present an updated molecular phylogenetic tree of hoplocercines including new samples of E. rudolfarndti, E. rubrigularis, both species described in this paper, as well as an updated identification key for species of Hoplocercinae. C1 [Venegas, Pablo J.; Duran, Vilma; de Queiroz, Kevin] Ctr Ornitol & Biodiversidad CORBIDI, Div Herpetol, Lima, Peru. [Torres-Carvajal, Omar] Pontificia Univ Catolica Ecuador, Escuela Biol, Quito, Ecuador. [Torres-Carvajal, Omar; de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Venegas, PJ (reprint author), Ctr Ornitol & Biodiversidad CORBIDI, Div Herpetol, Santa Rita 105 Of 202, Lima, Peru. EM sancarranca@yahoo.es FU Mohamed bin Zayed Species Conservation Fund [0925417]; Smithsonian Institution; Secretaria Nacional de Educacion Superior, Ciencia y Tecnologia [PIC-08-0000470] FX For allowing access to the MUSM herpetological collections we are grateful to J. Cordova and C. Torres. We thank the staff of Centro de Conservacion, Investigacion y Manejo de Areas Naturales (CIMA), and the Servicio Nacional de Areas Naturales Protegidas por el Estado (SERNANP), especially the rangers and volunteers. We are indebted to J. Martinez and T. Pequeno of CIMA for their logistic support and help with the permits and to P. Saldana and C. Savedra of SERNANP for his logistic support and company in the field. We are grateful to L. Lujan for arranging the plates. Fieldwork was supported by a grant from the Mohamed bin Zayed Species Conservation Fund (project number 0925417). K. de Queiroz and O. Torres-Carvajal had support from a Restricted Endowment Award from the Smithsonian Institution; O. Torres-Carvajal also had support from the Secretaria Nacional de Educacion Superior, Ciencia y Tecnologia (PIC-08-0000470). NR 12 TC 3 Z9 3 U1 0 U2 3 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 EI 1313-2970 J9 ZOOKEYS JI ZooKeys PY 2013 IS 277 BP 69 EP 90 DI 10.3897/zookeys.277.3594 PG 22 WC Zoology SC Zoology GA 106WW UT WOS:000316176600005 PM 23794824 ER PT J AU Dmitriev, DA McKamey, SH AF Dmitriev, Dmitry A. McKamey, Stuart H. TI Nomenclatural changes in Cicadellidae: Typhlocybinae and Delphacidae (Homoptera) SO ZOOKEYS LA English DT Article DE Typhlocybinae; Delphacidae; leafhopper; planthopper; systematics; homonym; synonym AB New replacement names are proposed for seven species of the subfamily Typhlocybinae; one new synonym is recognized in the family Delphacidae. The following changes are proposed: Empoasca (Empoasca) angustata nom. nov. for Empoasca angusta Linnavuori & DeLong (not Dworakowska); Empoasca (Empoasca) chilensis nom. nov. for Empoasca diversa Linnavuori & DeLong (not Vilbaste); Austroasca verdensis nom. nov. for Empoasca artemisiae Lindberg (not Lethierry); Kropka vidanoi Dworakowska for Erythroneura unipunctata Dlabola (not Cerutti); Zyginella vietnamica nom. nov. for Zyginella melichari Dworakowska (not Kirkaldy); Eupteryx (Eupteryx) dlabolai nom. nov. for Eupteryx octonotata Dlabola (not Hardy); Baaora ahmedi nom. nov. for Baaora spinosa (Ahmed) (not Beamer); Paradelphacodes insolitus Dmitriev is synonymized with Paradelphacodes gvosdevi (Mitjaev), syn. nov. C1 [Dmitriev, Dmitry A.] Univ Illinois, Prairie Res Inst, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [McKamey, Stuart H.] ARS, USDA, Systemat Entomol Lab, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Dmitriev, DA (reprint author), Univ Illinois, Prairie Res Inst, Illinois Nat Hist Survey, 1816 S Oak St, Champaign, IL 61820 USA. EM dmitriev@inhs.uiuc.edu FU National Science Foundation [DEB 0315373, DEB-050529679, DEB-0715499] FX This work was partially supported by the National Science Foundation grants (DEB 0315373, DEB-050529679, and DEB-0715499). NR 27 TC 2 Z9 2 U1 2 U2 12 PU PENSOFT PUBL PI SOFIA PA GEO MILEV STR 13A, SOFIA, 1111, BULGARIA SN 1313-2989 J9 ZOOKEYS JI ZooKeys PY 2013 IS 277 BP 109 EP 113 DI 10.3897/zookeys.277.4273 PG 5 WC Zoology SC Zoology GA 106WW UT WOS:000316176600007 PM 23794826 ER EF