FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Reid, MJ Menten, KM Zheng, XW Brunthaler, A Moscadelli, L Xu, Y Zhang, B Sato, M Honma, M Hirota, T Hachisuka, K Choi, YK Moellenbrock, GA Bartkiewicz, A AF Reid, M. J. Menten, K. M. Zheng, X. W. Brunthaler, A. Moscadelli, L. Xu, Y. Zhang, B. Sato, M. Honma, M. Hirota, T. Hachisuka, K. Choi, Y. K. Moellenbrock, G. A. Bartkiewicz, A. TI TRIGONOMETRIC PARALLAXES OF MASSIVE STAR-FORMING REGIONS. VI. GALACTIC STRUCTURE, FUNDAMENTAL PARAMETERS, AND NONCIRCULAR MOTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; stars: formation ID HIPPARCOS PROPER MOTIONS; MILKY-WAY GALAXY; ROTATION CURVE; SPIRAL STRUCTURE; BLACK-HOLE; STELLAR ORBITS; OB STARS; DISTANCE; DISK; KINEMATICS AB We are using the Very Long Baseline Array and the Japanese VLBI Exploration of Radio Astronomy project to measure trigonometric parallaxes and proper motions of masers found in high-mass star-forming regions across the Milky Way. Early results from 18 sources locate several spiral arms. The Perseus spiral arm has a pitch angle of 16 degrees +/- 3 degrees, which favors four rather than two spiral arms for the Galaxy. Combining positions, distances, proper motions, and radial velocities yields complete three-dimensional kinematic information. We find that star-forming regions on average are orbiting the Galaxy approximate to 15 km s(-1) slower than expected for circular orbits. By fitting the measurements to a model of the Galaxy, we estimate the distance to the Galactic center R(0) = 8.4 +/- 0.6 kpc and a circular rotation speed Theta(0) = 254 +/- 16 km s(-1). The ratio Theta(0)/R(0) can be determined to higher accuracy than either parameter individually, and we find it to be 30.3 +/- 0.9 km s(-1) kpc(-1), in good agreement with the angular rotation rate determined from the proper motion of Sgr A*. The data favor a rotation curve for the Galaxy that is nearly flat or slightly rising with Galactocentric distance. Kinematic distances are generally too large, sometimes by factors greater than 2; they can be brought into better agreement with the trigonometric parallaxes by increasing Theta(0)/R(0) from the IAU recommended value of 25.9 km s(-1) kpc(-1) to a value near 30 km s(-1) kpc(-1). We offer a "revised" prescription for calculating kinematic distances and their uncertainties, as well as a new approach for defining Galactic coordinates. Finally, our estimates of Theta(0) and Theta(0)/R(0), when coupled with direct estimates of R(0), provide evidence that the rotation curve of the Milky Way is similar to that of the Andromeda galaxy, suggesting that the dark matter halos of these two dominant Local Group galaxy are comparably massive. C1 [Reid, M. J.; Sato, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Brunthaler, A.; Xu, Y.; Choi, Y. K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zheng, X. W.; Zhang, B.] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China. [Moscadelli, L.] Arcetri Observ, Florence, Italy. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Sato, M.; Honma, M.; Hirota, T.] Natl Astron Observ, VERA Project, Tokyo 1818588, Japan. [Hachisuka, K.] Shanghai Astron Observ, Shanghai, Peoples R China. [Moellenbrock, G. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Bartkiewicz, A.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Bartkiewicz, Anna/D-6212-2014; OI Moscadelli, Luca/0000-0002-8517-8881 NR 64 TC 559 Z9 562 U1 1 U2 20 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 137 EP 148 DI 10.1088/0004-637X/700/1/137 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900012 ER PT J AU Salim, S Dickinson, M Rich, RM Charlot, S Lee, JC Schiminovich, D Perez-Gonzalez, PG Ashby, MLN Papovich, C Faber, SM Ivison, RJ Frayer, DT Walton, JM Weiner, BJ Chary, RR Bundy, K Noeske, K Koekemoer, AM AF Salim, Samir Dickinson, Mark Rich, R. Michael Charlot, Stephane Lee, Janice C. Schiminovich, David Perez-Gonzalez, Pablo G. Ashby, Matthew L. N. Papovich, Casey Faber, S. M. Ivison, Rob J. Frayer, David T. Walton, Josiah M. Weiner, Benjamin J. Chary, Ranga-Ram Bundy, Kevin Noeske, Kai Koekemoer, Anton M. TI MID-IR LUMINOSITIES AND UV/OPTICAL STAR FORMATION RATES AT z < 1.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: fundamental parameters; infrared: galaxies; surveys; ultraviolet: galaxies ID ACTIVE GALACTIC NUCLEI; LUMINOUS INFRARED GALAXIES; COLOR-MAGNITUDE DIAGRAM; EXTENDED GROTH STRIP; HIGH-REDSHIFT GALAXIES; FORMING GALAXIES; PHYSICAL-PROPERTIES; SPITZER OBSERVATIONS; STELLAR POPULATIONS; STARBURST GALAXIES AB Ultraviolet (UV) nonionizing continuum and mid-infrared (IR) emission constitute the basis of two widely used star formation (SF) indicators at intermediate and high redshifts. We study 2430 galaxies with z < 1.4 in the Extended Groth Strip with deep MIPS 24 mu m observations from FIDEL, spectroscopy from DEEP2, and UV, optical, and near-IR photometry from the AEGIS. The data are coupled with dust-reddened stellar population models and Bayesian spectral energy distribution (SED) fitting to estimate dust-corrected star formation rates (SFRs). In order to probe the dust heating from stellar populations of various ages, the derived SFRs were averaged over various timescales-from 100 Myr for "current" SFR (corresponding to young stars) to 1-3 Gyr for long-timescale SFRs (corresponding to the light-weighted age of the dominant stellar populations). These SED-based UV/optical SFRs are compared to total IR luminosities extrapolated from 24 mu m observations, corresponding to 10-18 mu m rest frame. The total IR luminosities are in the range of normal star-forming galaxies and luminous IR galaxies (10(10)-10(12)L(circle dot)). We show that the IR luminosity can be estimated from the UV and optical photometry to within a factor of 2, implying that most z < 1.4 galaxies are not optically thick. We find that for the blue, actively star-forming galaxies the correlation between the IR luminosity and the UV/optical SFR shows a decrease in scatter when going from shorter to longer SFR-averaging timescales. We interpret this as the greater role of intermediate age stellar populations in heating the dust than what is typically assumed. Equivalently, we observe that the IR luminosity is better correlated with dust-corrected optical luminosity than with dust-corrected UV light. We find that this holds over the entire redshift range. Many so-called green valley galaxies are simply dust-obscured actively star-forming galaxies. However, there exist 24 mu m detected galaxies, some with L(IR) > 10(11) L(circle dot), yet with little current SF. For them a reasonable amount of dust absorption of stellar light (but presumably higher than in nearby early-type galaxies) is sufficient to produce the observed levels of IR, which includes a large contribution from intermediate and old stellar populations. In our sample, which contains very few ultraluminous IR galaxies, optical and X-ray active galactic nuclei do not contribute on average more than similar to 50% to the mid-IR luminosity, and we see no evidence for a large population of "IR excess" galaxies. C1 [Salim, Samir; Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85724 USA. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Charlot, Stephane] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Lee, Janice C.] Carnegie Observ, Pasadena, CA 91101 USA. [Schiminovich, David] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Perez-Gonzalez, Pablo G.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Perez-Gonzalez, Pablo G.; Papovich, Casey; Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Ashby, Matthew L. N.; Noeske, Kai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Faber, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Ivison, Rob J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Frayer, David T.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Walton, Josiah M.] Univ Arkansas, Fayetteville, AR 72701 USA. [Chary, Ranga-Ram] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Bundy, Kevin] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Salim, S (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85724 USA. EM samir@noao.edu RI Perez-Gonzalez, Pablo/J-2871-2016; Ivison, R./G-4450-2011; OI Perez-Gonzalez, Pablo/0000-0003-4528-5639; Ivison, R./0000-0001-5118-1313; Weiner, Benjamin/0000-0001-6065-7483; Salim, Samir/0000-0003-2342-7501; Koekemoer, Anton/0000-0002-6610-2048 NR 81 TC 92 Z9 92 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 161 EP 182 DI 10.1088/0004-637X/700/1/161 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900015 ER PT J AU Huang, JS Faber, SM Daddi, E Laird, ES Lai, K Omont, A Wu, Y Younger, JD Bundy, K Cattaneo, A Chapman, SC Conselice, CJ Dickinson, M Egami, E Fazio, GG Im, M Koo, D Le Floc'h, E Papovich, C Rigopoulou, D Smail, I Song, M Van de Werf, PP Webb, TMA Willmer, CNA Willner, SP Yan, L AF Huang, J. -S. Faber, S. M. Daddi, E. Laird, E. S. Lai, K. Omont, A. Wu, Y. Younger, J. D. Bundy, K. Cattaneo, A. Chapman, S. C. Conselice, C. J. Dickinson, M. Egami, E. Fazio, G. G. Im, M. Koo, D. Le Floc'h, E. Papovich, C. Rigopoulou, D. Smail, I. Song, M. Van de Werf, P. P. Webb, T. M. A. Willmer, C. N. A. Willner, S. P. Yan, L. TI INFRARED SPECTROGRAPH SPECTROSCOPY AND MULTI-WAVELENGTH STUDY OF LUMINOUS STAR-FORMING GALAXIES AT z similar or equal to 1.9 SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; galaxies: starburst; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; DEEP-FIELD-SOUTH; SUBMILLIMETER-SELECTED GALAXIES; ACTIVE GALACTIC NUCLEI; EXTENDED GROTH STRIP; HIGH-REDSHIFT; MIDINFRARED SPECTROSCOPY; MASSIVE GALAXIES; RED GALAXIES; OPTICAL SPECTROSCOPY AB We analyze a sample of galaxies chosen to have F(24) (mu m) > 0.5 mJy and satisfy a certain IRAC color criterion. Infrared Spectrograph (IRS) spectra yield redshifts, spectral types, and polycyclic aromatic hydrocarbons (PAH) luminosities, to which we add broadband photometry from optical through IRAC wavelengths, MIPS from 24-160 mu m, 1.1 mm, and radio at 1.4 GHz. Stellar population modeling and IRS spectra together demonstrate that the double criteria used to select this sample have efficiently isolated massive star-forming galaxies at z similar to 1.9. This is the first starburst (SB)-dominated ultraluminous infrared galaxies (ULIRG) sample at high redshift with total infrared luminosity measured directly from FIR and millimeter photometry, and as such gives us the first accurate view of broadband spectral energy distributions for SB galaxies at extremely high luminosity and at all wavelengths. Similar broadband data are assembled for three other galaxy samples-local SB galaxies, local active galactic nucleus (AGN)/ULIRGs, and a second 24 mu m-luminous z similar to 2 sample dominated by AGN. L(PAH)/L(IR) for the new z similar to 2 SB sample is the highest ever seen, some three times higher than in local SBs, whereas in AGNs this ratio is depressed below the SB trend, often severely. Several pieces of evidence imply that AGNs exist in this SB-dominated sample, except two of which even host very strong AGN, while they still have very strong PAH emission. The Advanced Camera for Surveys images show that most objects have very extended morphologies in the rest-frame ultraviolet band, thus extended distribution of PAH molecules. Such an extended distribution prevents further destruction PAH molecules by central AGNs. We conclude that objects in this sample are ULIRGs powered mainly by SB; and the total infrared luminosity density contributed by this type of objects is 0.9-2.6 x 10(7) L(circle dot) Mpc(-3). C1 [Huang, J. -S.; Lai, K.; Younger, J. D.; Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Faber, S. M.; Koo, D.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Daddi, E.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA DSM CNRS,DAPNIA, F-91191 Gif Sur Yvette, France. [Laird, E. S.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Omont, A.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. [Wu, Y.; Yan, L.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Younger, J. D.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Bundy, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Cattaneo, A.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Chapman, S. C.] Univ Victoria, Victoria, BC V8P 1A1, Canada. [Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Egami, E.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Im, M.; Song, M.] Seoul Natl Univ, Dept Phys & Astron, FPRD, Seoul 151747, South Korea. [Le Floc'h, E.] Univ Hawaii, IfA, Honolulu, HI 96822 USA. [Papovich, C.] Texas A&M Univ, Dept Phys, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Smail, I.] Univ Durham, Inst Computat Cosmol, Durham, England. [Van de Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Webb, T. M. A.] McGill Univ, Dept Phys, Montreal, PQ, Canada. RP Huang, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Wu, Yanling/A-1261-2010; Daddi, Emanuele/D-1649-2012; Im, Myungshin/B-3436-2013; Conselice, Christopher/B-4348-2013; Smail, Ian/M-5161-2013 OI Daddi, Emanuele/0000-0002-3331-9590; Im, Myungshin/0000-0002-8537-6714; Smail, Ian/0000-0003-3037-257X FU NASA 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. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 116 TC 49 Z9 50 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 183 EP 198 DI 10.1088/0004-637X/700/1/183 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900016 ER PT J AU Tang, YW Ho, PTP Koch, PM Girart, JM Lai, SP Rao, R AF Tang, Ya-Wen Ho, Paul T. P. Koch, Patrick M. Girart, Josep M. Lai, Shih-Ping Rao, Ramprasad TI EVOLUTION OF MAGNETIC FIELDS IN HIGH-MASS STAR FORMATION: LINKING FIELD GEOMETRY AND COLLAPSE FOR THE W51 e2/e8 CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (W51 e2/e8); ISM: magnetic fields; polarization; stars: formation ID MOLECULAR CLOUD CORES; FORMING REGIONS; INFRARED POLARIMETRY; SUBMILLIMETER ARRAY; LINEAR-POLARIZATION; AMBIPOLAR DIFFUSION; DYNAMICAL COLLAPSE; RADIATIVE TORQUES; WATER MASERS; EMISSION AB We report our observational results of 870 mu m continuum emission and its linear polarization in the massive star formation site W51 e2/e8. Inferred from the linear polarization maps, the magnetic field in the plane of sky (B(perpendicular to)) is traced with an angular resolution of 0 ''.7 with the Submillimeter Array. Whereas previous BIMA observations with an angular resolution of 3 '' (0.1 pc) showed a uniform B field, our revealed B(perpendicular to) morphology is hourglass-like in the collapsing core near the ultracompact H II region e2 and also possibly in e8. The decrease in polarization near the continuum peak seen at lower angular resolution is apparently due to the more complex structures at smaller scales. In e2, the pinched direction of the hourglass-like B-field morphology is parallel to the plane of the ionized accretion flow traced by H53 alpha, suggesting that the massive stars are formed via processes similar to the low-mass stars, i.e., accretion through a disk, except that the mass involved is much larger. Furthermore, our finding that the resolved collapsing cores in e2 and e8 lie within one subcritical 0.5 pc envelope supports the scenario of magnetic fragmentation via ambipolar diffusion. We therefore suggest that magnetic fields control the dynamical evolution of the envelope and cores in W51 e2 and e8. C1 [Tang, Ya-Wen] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Tang, Ya-Wen; Ho, Paul T. P.; Koch, Patrick M.; Lai, Shih-Ping] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Girart, Josep M.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, Bellaterra 08193, Catalunya, Spain. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 300, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 300, Taiwan. RP Tang, YW (reprint author), Natl Taiwan Univ, Dept Phys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Tang, Ya-Wen/0000-0002-0675-276X FU National Science Council of Taiwan [NSC 97-2112-M-001-007-MY3] FX The authors are grateful for the anonymous referee's comments, which helped to improve the manuscript. Y.-W.T. and P. T. P. H. thank the National Science Council of Taiwan for supporting this project through grants NSC 97-2112-M-001-007-MY3. NR 52 TC 54 Z9 54 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 251 EP 261 DI 10.1088/0004-637X/700/1/251 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900022 ER PT J AU Winn, JN Johnson, JA Fabrycky, D Howard, AW Marcy, GW Narita, N Crossfield, IJ Suto, Y Turner, EL Esquerdo, G Holman, MJ AF Winn, Joshua N. Johnson, John Asher Fabrycky, Daniel Howard, Andrew W. Marcy, Geoffrey W. Narita, Norio Crossfield, Ian J. Suto, Yasushi Turner, Edwin L. Esquerdo, Gil Holman, Matthew J. TI ON THE SPIN-ORBIT MISALIGNMENT OF THE XO-3 EXOPLANETARY SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planetary systems: formation; stars: individual (XO-3, GSC 03727-01064); stars: rotation ID LIGHT-CURVE PROJECT; EXTRASOLAR PLANETARY SYSTEMS; SPECTROSCOPIC TRANSIT; TIDAL EVOLUTION; MASSIVE PLANET; GIANT PLANETS; HOT JUPITERS; HD 147506B; ALIGNMENT; SCATTERING AB We present photometric and spectroscopic observations of the 2009 February 2 transit of the exoplanet XO-3b. The new data show that the planetary orbital axis and stellar rotation axis are misaligned, as reported earlier by Hebrard and coworkers. We find the angle between the sky projections of the two axes to be 37.3 +/- 3.7 deg, as compared to the previously reported value of 70 +/- 15 deg. The significance of this discrepancy is unclear because there are indications of systematic effects. XO-3b is the first exoplanet known to have a highly inclined orbit relative to the equatorial plane of its parent star, and as such it may fulfill the predictions of some scenarios for the migration of massive planets into close-in orbits. We revisit the statistical analysis of spin orbit alignment in hot-Jupiter systems. Assuming the stellar obliquities to be drawn from a single Rayleigh distribution, we find the mode of the distribution to be 13(-2)(+5) deg. However, it remains the case that a model representing two different migration channels-in which some planets are drawn from a perfectly aligned distribution and the rest are drawn from an isotropic distribution-is favored over a single Rayleigh distribution. C1 [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fabrycky, Daniel; Esquerdo, Gil; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Narita, Norio] Natl Astron Observ Japan, Tokyo 1818588, Japan. [Crossfield, Ian J.] Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90024 USA. [Suto, Yasushi] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Turner, Edwin L.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Turner, Edwin L.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Turner, Edwin/A-4295-2011; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX09AD36G, NNX09AB33G] FX We thank Peter McCullough for reminding us about the near-coincidence of the orbital and rotational periods of XO-3b. We are grateful to Gaspar Bakos for trading telescope time at FLWO on short notice, and to Breann Sitarski and Tracy Ly for helping with the observations at Lick Observatory. We are indebted to Lara Winn for enabling this work to be completed in a timely fashion. This work was partly supported by the NASA Origins program through awards NNX09AD36G and NNX09AB33G. J.A.J. acknowledges support from an NSF Astronomy and NR 43 TC 66 Z9 66 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 302 EP 308 DI 10.1088/0004-637X/700/1/302 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900027 ER PT J AU Hicken, M Challis, P Jha, S Kirshner, RP Matheson, T Modjaz, M Rest, A Wood-Vasey, WM Bakos, G Barton, EJ Berlind, P Bragg, A Briceno, C Brown, WR Caldwell, N Calkins, M Cho, R Ciupik, L Contreras, M Dendy, KC Dosaj, A Durham, N Eriksen, K Esquerdo, G Everett, M Falco, E Fernandez, J Gaba, A Garnavich, P Graves, G Green, P Groner, T Hergenrother, C Holman, MJ Hradecky, V Huchra, J Hutchison, B Jerius, D Jordan, A Kilgard, R Krauss, M Luhman, K Macri, L Marrone, D McDowell, J McIntosh, D McNamara, B Megeath, T Mochejska, B Munoz, D Muzerolle, J Naranjo, O Narayan, G Pahre, M Peters, W Peterson, D Rines, K Ripman, B Roussanova, A Schild, R Sicilia-Aguilar, A Sokoloski, J Smalley, K Smith, A Spahr, T Stanek, KZ Barmby, P Blondin, S Stubbs, CW Szentgyorgyi, A Torres, MAP Vaz, A Vikhlinin, A Wang, Z Westover, M Woods, D Zhao, P AF Hicken, Malcolm Challis, Peter Jha, Saurabh Kirshner, Robert P. Matheson, Tom Modjaz, Maryam Rest, Armin Wood-Vasey, W. Michael Bakos, Gaspar Barton, Elizabeth J. Berlind, Perry Bragg, Ann Briceno, Cesar Brown, Warren R. Caldwell, Nelson Calkins, Mike Cho, Richard Ciupik, Larry Contreras, Maria Dendy, Kristi-Concannon Dosaj, Anil Durham, Nick Eriksen, Kris Esquerdo, Gil Everett, Mark Falco, Emilio Fernandez, Jose Gaba, Alejandro Garnavich, Peter Graves, Genevieve Green, Paul Groner, Ted Hergenrother, Carl Holman, Matthew J. Hradecky, Vit Huchra, John Hutchison, Bob Jerius, Diab Jordan, Andres Kilgard, Roy Krauss, Miriam Luhman, Kevin Macri, Lucas Marrone, Daniel McDowell, Jonathan McIntosh, Daniel McNamara, Brian Megeath, Tom Mochejska, Barbara Munoz, Diego Muzerolle, James Naranjo, Orlando Narayan, Gautham Pahre, Michael Peters, Wayne Peterson, Dawn Rines, Ken Ripman, Ben Roussanova, Anna Schild, Rudolph Sicilia-Aguilar, Aurora Sokoloski, Jennifer Smalley, Kyle Smith, Andy Spahr, Tim Stanek, K. Z. Barmby, Pauline Blondin, Stephane Stubbs, Christopher W. Szentgyorgyi, Andrew Torres, Manuel A. P. Vaz, Amili Vikhlinin, Alexey Wang, Zhong Westover, Mike Woods, Deborah Zhao, Ping TI CfA3: 185 TYPE Ia SUPERNOVA LIGHT CURVES FROM THE CfA SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID INFRARED PHOTOMETRY; ABSOLUTE MAGNITUDES; IMAGE SUBTRACTION; REDSHIFT; SHAPES; TIMESCALE; GALAXIES; UNIVERSE; CATALOG; MOTION AB We present multiband photometry of 185 type-Ia supernovae (SNe Ia), with over 11,500 observations. These were acquired between 2001 and 2008 at the F. L. Whipple Observatory of the Harvard-Smithsonian Center for Astrophysics (CfA). This sample contains the largest number of homogeneously observed and reduced nearby SNe Ia (z less than or similar to 0.08) published to date. It more than doubles the nearby sample, bringing SN Ia cosmology to the point where systematic uncertainties dominate. Our natural system photometry has a precision of less than or similar to 0.02 mag in BV RIr'i' and less than or similar to 0.04 mag in U for points brighter than 17.5 mag. We also estimate a systematic uncertainty of 0.03 mag in our SN Ia standard system BV RIr'i' photometry and 0.07 mag for U. Comparisons of our standard system photometry with published SN Ia light curves and comparison stars, where available for the same SN, reveal agreement at the level of a few hundredths mag in most cases. We find that 1991bg-like SNe Ia are sufficiently distinct from other SNe Ia in their color and light-curve-shape/luminosity relation that they should be treated separately in light-curve/distance fitter training samples. The CfA3 sample will contribute to the development of better light-curve/distance fitters, particularly in the few dozen cases where near-infrared photometry has been obtained and, together, can help disentangle host-galaxy reddening from intrinsic supernova color, reducing the systematic uncertainty in SN Ia distances due to dust. C1 [Hicken, Malcolm; Challis, Peter; Kirshner, Robert P.; Bakos, Gaspar; Berlind, Perry; Brown, Warren R.; Caldwell, Nelson; Calkins, Mike; Cho, Richard; Contreras, Maria; Dosaj, Anil; Durham, Nick; Falco, Emilio; Fernandez, Jose; Green, Paul; Groner, Ted; Holman, Matthew J.; Hradecky, Vit; Huchra, John; Hutchison, Bob; Jerius, Diab; Jordan, Andres; Kilgard, Roy; Marrone, Daniel; McDowell, Jonathan; Megeath, Tom; Munoz, Diego; Naranjo, Orlando; Narayan, Gautham; Pahre, Michael; Peters, Wayne; Peterson, Dawn; Rines, Ken; Ripman, Ben; Schild, Rudolph; Sicilia-Aguilar, Aurora; Sokoloski, Jennifer; Smalley, Kyle; Smith, Andy; Spahr, Tim; Stubbs, Christopher W.; Szentgyorgyi, Andrew; Torres, Manuel A. P.; Vikhlinin, Alexey; Wang, Zhong; Westover, Mike; Woods, Deborah; Zhao, Ping] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hicken, Malcolm; Rest, Armin; Stubbs, Christopher W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Matheson, Tom] NOAO Gemini Sci Ctr, Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Modjaz, Maryam] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wood-Vasey, W. Michael] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Barton, Elizabeth J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bragg, Ann] Marietta Coll, Dept Phys, Marietta, OH 45750 USA. [Briceno, Cesar] Ctr Invest Astron CIDA, Merida 5101A, Venezuela. [Ciupik, Larry] Adler Planetarium & Astron Museum, Chicago, IL 60605 USA. [Dendy, Kristi-Concannon; Gaba, Alejandro] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Eriksen, Kris; Hergenrother, Carl; Muzerolle, James] Univ Arizona, Tucson, AZ 85721 USA. [Esquerdo, Gil; Everett, Mark] Planetary Sci Inst, Tucson, AZ 85719 USA. [Garnavich, Peter] Univ Notre Dame, Notre Dame, IN 46556 USA. [Graves, Genevieve] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Krauss, Miriam; Roussanova, Anna; Vaz, Amili] MIT, Cambridge, MA 02139 USA. [Luhman, Kevin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Macri, Lucas] Texas A&M Univ, Dept Phys, George P & Cynthia W Mitchell Inst Fundamental Ph, College Stn, TX 77843 USA. [McIntosh, Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [McNamara, Brian] Univ Waterloo, Dept Phys & Astron, W Waterloo, ON N2L 3G1, Canada. [Mochejska, Barbara] Copernicus Astron Ctr Warsaw, PL-00716 Warsaw, Poland. [Stanek, K. Z.] Ohio State Univ, Dept Astron, McPherson Lab, Columbus, OH 43210 USA. [Barmby, Pauline] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Blondin, Stephane] European So Observ, D-85748 Garching, Germany. RP Hicken, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhicken@cfa.harvard.edu; kirshner@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; Barmby, Pauline/I-7194-2016; OI Stubbs, Christopher/0000-0003-0347-1724; Barmby, Pauline/0000-0003-2767-0090; Marrone, Daniel/0000-0002-2367-1080; Jordan, Andres/0000-0002-5389-3944; Narayan, Gautham/0000-0001-6022-0484; Macri, Lucas/0000-0002-1775-4859 FU NSF [AST0606772] FX We thank the staff at FLWO for their dedicated work in maintaining the 1.2 m telescope and instruments. This work has been supported, in part, by NSF grant AST0606772 to Harvard University. A. R. thanks the Goldberg Fellowship Program for its support. NR 67 TC 219 Z9 220 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 331 EP 357 DI 10.1088/0004-637X/700/1/331 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900029 ER PT J AU Teixeira, PS Lada, CJ Wood, K Robitaille, TP Luhman, KL AF Teixeira, Paula S. Lada, Charles J. Wood, Kenneth Robitaille, Thomas P. Luhman, Kevin L. TI INFRARED SPECTROGRAPH CHARACTERIZATION OF A DEBRIS DISK AROUND AN M-TYPE STAR IN NGC 2547 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; open clusters and associations: individual (NGC 2547); stars: individual (2MASS 08093547-4913033) ID SPITZER-SPACE-TELESCOPE; TERRESTRIAL PLANET FORMATION; LOW-MASS STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; BROWN DWARF DISKS; PROTOSTELLAR ENVELOPES; INTERSTELLAR DUST; SIZE DISTRIBUTION; ACCRETION; EVOLUTION AB We present 5 to 15 mu m Spitzer Infrared Spectrograph (IRS) low-resolution spectral data of a candidate debris disk around an M4.5 star identified as a likely member of the similar to 40 Myr old cluster NGC 2547. The IRS spectrum shows a silicate emission feature, indicating the presence of warm, small, (sub) micron-sized dust grains in the disk. Of the 15 previously known candidate debris disks around M-type stars, the one we discuss in this paper is the first to have an observed mid-infrared spectrum and is also the first to have measured silicate emission. We combined the IRS data with ancillary data (optical, JHK(s), and Spitzer InfraRed Array Camera and 24 mu m data) to build the spectral energy distribution (SED) of the source. Monte Carlo radiation transfer modeling of the SED characterized the dust disk as being very flat (h(100) = 2 AU) and extending inward within at least 0.13 AU of the central star. Our analysis shows that the disk is collisionally dominated and is likely a debris disk. C1 [Teixeira, Paula S.; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teixeira, Paula S.] Univ Lisbon, Fac Ciencias, Dept Fis, P-1749016 Lisbon, Portugal. [Teixeira, Paula S.] Univ Lisbon, Lab Associado Inst D Luiz SIM, P-1749016 Lisbon, Portugal. [Wood, Kenneth; Robitaille, Thomas P.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Luhman, Kevin L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Teixeira, PS (reprint author), European Org Astron Res So Hemisphere, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM pteixeir@eso.org; clada@cfa.harvard.edu; kw25@st-andrews.ac.uk; tr9@st-andrews.ac.uk; kluhman@astro.psu.edu RI Teixeira, Paula Stella/O-2289-2013; OI Teixeira, Paula Stella/0000-0002-3665-5784; Robitaille, Thomas/0000-0002-8642-1329 NR 53 TC 0 Z9 0 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 454 EP 459 DI 10.1088/0004-637X/700/1/454 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900038 ER PT J AU Rho, J Reach, WT Tappe, A Hwang, U Slavin, JD Kozasa, T Dunne, L AF Rho, J. Reach, W. T. Tappe, A. Hwang, U. Slavin, J. D. Kozasa, T. Dunne, L. TI SPITZER OBSERVATIONS OF THE YOUNG CORE-COLLAPSE SUPERNOVA REMNANT 1E0102-72.3: INFRARED EJECTA EMISSION AND DUST FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: general; supernova remnants; supernovae: general ID SMALL-MAGELLANIC-CLOUD; POLYCYCLIC AROMATIC-HYDROCARBONS; X-RAY OBSERVATIONS; CASSIOPEIA-A; INTERSTELLAR-MEDIUM; 1E 0102.2-7219; SPACE-TELESCOPE; GRAIN DESTRUCTION; DISTANT QUASARS; II SUPERNOVAE AB We present Spitzer Infrared Spectrograph and Infrared Array Camera observations of the young supernova remnant E0102 (SNR 1E0102-7219) in the Small Magellanic Cloud. The infrared spectra show strong lines of Ne and O, with the [Ne II] line at 12.8 mu m having a large velocity dispersion of 2000-4500 km s(-1) indicative of fast-moving ejecta. Unlike the young Galactic SNR Cas A, E0102 lacks emission from Ar and Fe. Diagnostics of the observed [Ne III] line pairs imply that [Ne III] emitting ejecta have a low temperature of 650 K, while [Ne v] line pairs imply that the infrared [Ne v] emitting ejecta have a high density of similar to 104 cm(-3). We have calculated radiative shock models for various velocity ranges including the effects of photoionization. The shock model indicates that the [Ne v] lines come mainly from the cooling zone, which is hot and dense, whereas [Ne II] and [Ne III] come mainly from the photoionization zone, which has a low temperature of 400-1000 K. We estimate an infrared-emitting Ne ejecta mass of 0.04 M-circle dot from the infrared observations, and discuss implications for the progenitor mass. The spectra also have a dust continuum feature peaking at 18 mu m that coincides spatially with the ejecta, providing evidence that dust formed in the expanding ejecta. The 18 mu m peak dust feature is fitted by a mixture of MgSiO3 and Si dust grains, while the rest of the continuum requires either carbon or Al2O3 grains. We measure the total dust mass formed within the ejecta of E0102 to be similar to 0.014 M-circle dot. The dust mass in E0102 is thus a factor of a few smaller than that in Cas A. The composition of the dust is also different, showing relatively less silicate and likely no Fe-bearing dust, as is suggested by the absence of Fe-emitting ejecta. C1 [Rho, J.; Reach, W. T.; Tappe, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Tappe, A.; Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hwang, U.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kozasa, T.] Hokkaido Univ, Grad Sch Sci, Dept Cosmosci, Sapporo, Hokkaido 0600810, Japan. [Dunne, L.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. RP Rho, J (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. EM rho@ipac.caltech.edu RI Kozasa, Takashi/A-5213-2012; OI Reach, William/0000-0001-8362-4094 FU NASA [1407] FX We thank Haley Gomez for insightful, helpful comments on the manuscript. J.R. thanks Pierre-Olivier Lagage, Sacha Hony, and Anne Decourchelle for fruitful discussion on dust and SN ejecta during her visit to Saclay. We thank Lee Armus and David Shupe for sharing the results of the IRS wavelength calibration on the IRS instrumental line widths, and Steven Finkelstein and William Blair for sharing their digitalized formats of HST and the optical images, and Shaun Amy for a radio image. 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 NASA contract 1407. Partial support for this work was provided by NASA through an GO award issued by JPL/Caltech. NR 78 TC 37 Z9 37 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 JUL 20 PY 2009 VL 700 IS 1 BP 579 EP 596 DI 10.1088/0004-637X/700/1/579 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900048 ER PT J AU Smith, RK Chen, GX Kirby, K Brickhouse, NS AF Smith, Randall K. Chen, Guo-Xin Kirby, Kate Brickhouse, Nancy S. TI A NEW CALCULATION OF Ne IX LINE DIAGNOSTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; line: formation; X-rays: stars ID HELIUM-LIKE IONS; PHOTOIONIZATION CROSS-SECTIONS; X-RAY SPECTROSCOPY; HE-LIKE IONS; ELECTRON-IMPACT EXCITATION; FINITE-DENSITY PLASMAS; XMM-NEWTON; ISOELECTRONIC SEQUENCE; GRATING SPECTROMETER; EXTREME-ULTRAVIOLET AB We describe the effect that new atomic calculations, including fully relativistic R-matrix calculations of collisional excitation rates and level-specific dielectronic and radiative recombination rates, have on line ratios from the astrophysically significant ion Ne IX. The new excitation rates systematically change some predicted Ne IX line ratios by 25% at temperatures at or below the temperature of maximum emissivity (4 x 10(6) K), while the new recombination rates lead to systematic changes at higher temperatures. The new line ratios are shown to agree with observations of Capella and sigma(2) CrB significantly better than older line ratios, showing that 25% 30% accuracy in atomic rates is inadequate for high-resolution X-ray observations from existing spectrometers. C1 [Smith, Randall K.; Chen, Guo-Xin; Kirby, Kate; Brickhouse, Nancy S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rsmith@cfa.harvard.edu OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [NAS8-03060] FX We acknowledge support from the Chandra GO Theory Program. Support for N. S. B. was provided by NASA contract NAS8-03060 to the Smithsonian Astrophysical Observatory for the CXC. NR 51 TC 13 Z9 13 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 679 EP 683 DI 10.1088/0004-637X/700/1/679 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900054 ER PT J AU Chan, CK Psaltis, D Ozel, F AF Chan, Chi-Kwan Psaltis, Dimitrios Oezel, Feryal TI SPECTRAL METHODS FOR TIME-DEPENDENT STUDIES OF ACCRETION FLOWS. III. THREE-DIMENSIONAL, SELF-GRAVITATING, MAGNETOHYDRODYNAMIC DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; hydrodynamics; MHD ID NONLINEAR CONSERVATION-LAWS; 2 SPACE DIMENSIONS; MAGNETOROTATIONAL INSTABILITY; VISCOSITY METHOD; ASTROPHYSICAL FLOWS; HYDRODYNAMIC DISKS; NUMERICAL SCHEME; BLACK-HOLES; SIMULATIONS; TRANSPORT AB Accretion disks are three-dimensional, turbulent, often self-gravitating, magnetohydrodynamic (MHD) flows, which can be modeled with numerical simulations. In this paper, we present a new algorithm that is based on a spectral decomposition method to simulate such flows. Because of the high order of the method, we can solve the induction equation in terms of the magnetic vector potential and, therefore, ensure trivially that the magnetic fields in the numerical solution are divergence free. The spectral method also suffers minimally from numerical dissipation and allows for an easy implementation of models for subgrid physics. Both properties make our method ideal for studying MHD turbulent flows such as those found in accretion disks around compact objects. We verify our algorithm with a series of standard tests and use it to show the development of MHD turbulence in a simulation of an accretion disk. Finally, we study the evolution and saturation of the power spectrum of MHD turbulence driven by the magnetorotational instability. C1 [Chan, Chi-Kwan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chan, Chi-Kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. RP Chan, CK (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. NR 49 TC 4 Z9 4 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 741 EP 751 DI 10.1088/0004-637X/700/1/741 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900060 ER PT J AU Pal, A Bakos, GA Fernandez, J Sipocz, B Torres, G Latham, DW Kovacs, G Noyes, RW Marcy, GW Fischer, DA Butler, RP Sasselov, DD Esquerdo, GA Shporer, A Mazeh, T Stefanik, RP Isaacson, H AF Pal, A. Bakos, G. A. Fernandez, J. Sipocz, B. Torres, G. Latham, D. W. Kovacs, Geza Noyes, R. W. Marcy, G. W. Fischer, D. A. Butler, R. P. Sasselov, D. D. Esquerdo, G. A. Shporer, A. Mazeh, T. Stefanik, R. P. Isaacson, H. TI INDEPENDENT CONFIRMATION AND REFINED PARAMETERS OF THE HOT JUPITER XO-5b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (XO-5, GSC 02959-00729); techniques: spectroscopic ID TRANSITING PLANET CANDIDATES; TESTING BLEND SCENARIOS; Y-2 ISOCHRONES; LIGHT CURVES; BRIGHT STAR; LOW-DENSITY; K-DWARF; SEARCH; STELLAR; FIELD AB We present HATNet observations of XO-5b, confirming its planetary nature based on evidence beyond that described in the announcement of Burke et al., namely, the lack of significant correlation between spectral bisector variations and orbital phase. In addition, using extensive spectroscopic measurements spanning multiple seasons, we investigate the relatively large scatter in the spectral line bisectors. We also examine possible blended stellar configurations (hierarchical triples, chance alignments) that can mimic the planet signals, and we are able to show that none are consistent with the sum of all the data. The analysis of the S activity index shows no significant stellar activity. Our results for the planet parameters are consistent with values in Burke et al., and we refine both the stellar and the planetary parameters using our data. XO-5b orbits a slightly evolved, late G type star with mass M(star) = 0.88 +/- 0.03 M(circle dot), radius R(star) = 1.08 +/- 0.04 R(circle dot), and metallicity close to solar. The planetary mass and radius are 1.059 +/- 0.028 M(J) and 1.109 +/- 0.050 R(J), respectively, corresponding to a mean density of 0.96(-0.11)(+ 0.14) g cm(-3). The ephemeris for the orbit is P = 4.187757 +/- 0.000011 days, E = 2454552.67168 +/- 0.00029 (BJD) with transit duration of 0.1307 +/- 0.0013 days. By measuring four individual transit centers, we found no signs for transit timing variations. The planet XO-5b is notable for its anomalously high Safronov number and has a high surface gravity when compared to other transiting exoplanets with similar period. C1 [Pal, A.; Bakos, G. A.; Fernandez, J.; Sipocz, B.; Torres, G.; Latham, D. W.; Noyes, R. W.; Sasselov, D. D.; Esquerdo, G. A.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pal, A.; Sipocz, B.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Pal, A.; Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary. [Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fischer, D. A.; Isaacson, H.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Butler, R. P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20005 USA. [Shporer, A.; Mazeh, T.] Tel Aviv Univ, Wise Observ, IL-69978 Tel Aviv, Israel. RP Pal, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apal@szofi.net RI Butler, Robert/B-1125-2009; OI Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G]; SAO; NSF Astronomy and Astrophysics Program [AST-0702843]; Kepler Mission [NCC2-1390]; Hungarian Scientific Research Foundation [K-60750]; NASA and NOAO [N162Hr, N128Hr, A264Hr] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G and SAO IR& D grants. Work of G.A.B. was supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843). We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D. W. L., P. I.). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-60750. A. P. is grateful for the SAO Visiting Student Fellowship that supported his work. This research has made use of Keck telescope time granted through NASA and NOAO (programs N162Hr, N128Hr, and A264Hr). NR 51 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 783 EP 790 DI 10.1088/0004-637X/700/1/783 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900064 ER PT J AU Wuyts, S Franx, M Cox, TJ Schreiber, NMF Hayward, CC Hernquist, L Hopkins, PF Labbe, I Marchesini, D Robertson, BE Toft, S van Dokkum, PG AF Wuyts, Stijn Franx, Marijn Cox, Thomas J. Schreiber, Natascha M. Foerster Hayward, Christopher C. Hernquist, Lars Hopkins, Philip F. Labbe, Ivo Marchesini, Danilo Robertson, Brant E. Toft, Sune van Dokkum, Pieter G. TI COLOR DISTRIBUTIONS, NUMBER, AND MASS DENSITIES OF MASSIVE GALAXIES AT 1.5 < z < 3: COMPARING OBSERVATIONS WITH MERGER SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: stellar content ID STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; QUASAR LUMINOSITY FUNCTION; ULTRALUMINOUS INFRARED GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; SPECTRAL ENERGY-DISTRIBUTION; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES AB We present a comparison between the observed color distribution, number, and mass density of massive galaxies at 1.5 < z < 3 and a model by Hopkins et al. that relates the quasar and galaxy population on the basis of gas-rich mergers. In order to test the hypothesis that quiescent red galaxies are formed after a gas-rich merger involving quasar activity, we confront photometry of massive (M > 4 x 10(10) M(circle dot)) galaxies extracted from the FIRES, GOODS-South, and MUSYC surveys, together spanning an area of 496 arcmin(2), with synthetic photometry from hydrodynamical merger simulations. As in the Hopkins et al. model, we use the observed quasar luminosity function to estimate the merger rate. We find that the synthetic U-V and V-J colors of galaxies that had a quasar phase in their past match the colors of observed galaxies that are best characterized by a quiescent stellar population. At z similar to 2.6, the observed number and mass density of quiescent red galaxies with M > 4 x 1010 M(circle dot) is consistent with the model in which every quiescent massive galaxy underwent a quasar phase in the past. At z similar to 1.9, 2.8 times less quiescent galaxies are observed than predicted by the model as descendants of higher redshift quasars. The merger model also predicts a large number and mass density of galaxies undergoing star formation driven by the merger. We find that the predicted number and mass density accounts for 30%-50% of the observed massive star-forming galaxies. However, their colors do not match those of observed star-forming galaxies. In particular, the colors of dusty red galaxies (accounting for 30%-40% of the massive galaxy population) are not reproduced by the simulations. Several possible origins of this discrepancy are discussed. The observational constraints on the validity of the model are currently limited by cosmic variance and uncertainties in stellar population synthesis and radiative transfer. C1 [Wuyts, Stijn; Cox, Thomas J.; Hayward, Christopher C.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schreiber, Natascha M. Foerster] MPE, D-85748 Garching, Germany. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Labbe, Ivo] Carnegie Observ, Pasadena, CA 91101 USA. [Marchesini, Danilo; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Robertson, Brant E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Robertson, Brant E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Robertson, Brant E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Toft, Sune] European So Observ, D-85748 Garching, Germany. [Toft, Sune] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. RP Wuyts, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU W. M. Keck Foundation; NASA FX S. Wuyts and T. J. Cox gratefully acknowledge support from the W. M. Keck Foundation. B. E. Robertson gratefully acknowledges support from a Spitzer Fellowship through a NASA grant administrated by the Spitzer Science Center. NR 103 TC 38 Z9 38 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 799 EP 819 DI 10.1088/0004-637X/700/1/799 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900066 ER PT J AU Bruderer, S Benz, AO Doty, SD van Dishoeck, EF Bourke, TL AF Bruderer, S. Benz, A. O. Doty, S. D. van Dishoeck, E. F. Bourke, T. L. TI MULTIDIMENSIONAL CHEMICAL MODELING OF YOUNG STELLAR OBJECTS. II. IRRADIATED OUTFLOW WALLS IN A HIGH-MASS STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; methods: data analysis; molecular processes; stars: formation; stars: individual (AFGL 2591) ID PHOTODISSOCIATION REGIONS; PROTOSTELLAR ENVELOPES; MOLECULAR-HYDROGEN; RADIATIVE-TRANSFER; MIXING LAYERS; HOT CORES; EMISSION; CHEMISTRY; SUBMILLIMETER; GAS AB Observations of the high-mass star-forming region AFGL 2591 reveal a large abundance of CO+, a molecule known to be enhanced by far-ultraviolet (FUV) and X-ray irradiation. In chemical models assuming a spherically symmetric envelope, the volume of gas irradiated by protostellar FUV radiation is very small due to the high extinction by dust. The abundance of CO+ is thus underpredicted by orders of magnitude. In a more realistic model, FUV photons can escape through an outflow region and irradiate gas at the border to the envelope. Thus, we introduce the first two-dimensional axisymmetric chemical model of the envelope of a high-mass star-forming region to explain the CO+ observations as a prototypical FUV tracer. The model assumes an axisymmetric power-law density structure with a cavity due to the outflow. The local FUV flux is calculated by a Monte Carlo radiative transfer code taking scattering on dust into account. A grid of precalculated chemical abundances, introduced in the first part of this series of papers, is used to quickly interpolate chemical abundances. This approach allows us to calculate the temperature structure of the FUV-heated outflow walls self-consistently with the chemistry. Synthetic maps of the line flux are calculated using a raytracer code. Single-dish and interferometric observations are simulated and the model results are compared to published and new JCMT and Submillimeter Array (SMA) observations. The two-dimensional model of AFGL 2591 is able to reproduce the JCMT single-dish observations and also explains the nondetection by the SMA. We conclude that the observed CO+ line flux and its narrow width can be interpreted by emission from the warm and dense outflow walls irradiated by protostellar FUV radiation. C1 [Bruderer, S.; Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bruderer, S (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM simonbr@astro.phys.ethz.ch NR 58 TC 33 Z9 33 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 JUL 20 PY 2009 VL 700 IS 1 BP 872 EP 886 DI 10.1088/0004-637X/700/1/872 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900071 ER PT J AU Lee, CF Mao, YY Reipurth, B AF Lee, Chin-Fei Mao, Yao-Yuan Reipurth, Bo TI INFALL AND ROTATION MOTIONS IN THE HH 111 PROTOSTELLAR SYSTEM: A FLATTENED ENVELOPE IN TRANSITION TO A DISK (vol 694, pg 1895, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Lee, Chin-Fei] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lee, Chin-Fei] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Mao, Yao-Yuan] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Reipurth, Bo] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw NR 1 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2009 VL 700 IS 1 BP 898 EP 898 DI 10.1088/0004-637X/700/1/898 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467UP UT WOS:000267768900073 ER PT J AU Keres, D Hernquist, L AF Keres, Dusan Hernquist, Lars TI SEEDING THE FORMATION OF COLD GASEOUS CLOUDS IN MILKY WAY-SIZE HALOS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: formation; Galaxy: halo; Galaxy: formation; instabilities; methods: numerical ID HIGH-VELOCITY CLOUDS; GALAXY FORMATION; GAS ACCRETION; SIMULATIONS; UNIVERSE; SYSTEMS; ORIGIN; STREAM; FLOWS AB We use one of the highest resolution cosmological smoothed particle hydrodynamic simulations to date to demonstrate that cold gaseous clouds form around Milky Way-size galaxies. We further explore mechanisms responsible for their formation and show that a large fraction of clouds originate as a consequence of late-time filamentary "cold mode" accretion. Here, filaments that are still colder and denser than the surrounding halo gas are not able to connect directly to galaxies, as they do at high redshift, but are instead susceptible to the combined action of cooling and Rayleigh-Taylor instabilities at intermediate radii within the halo leading to the production of cold, dense pressure-confined clouds, without an associated dark matter component. This process is aided through the compression of the incoming filaments by the hot halo gas and expanding shocks during the halo buildup. Our mechanism directly seeds clouds from gas with substantial local overdensity, unlike in previous models, and provides a channel for the origin of cloud complexes. These clouds can later "rain" onto galaxies, delivering fuel for star formation. Owing to the relatively large cross-section of filaments and the net angular momentum carried by the gas, the clouds will be distributed in a modestly flattened region around a galaxy. C1 [Keres, Dusan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keres, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 41 TC 89 Z9 89 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2009 VL 700 IS 1 BP L1 EP L5 DI 10.1088/0004-637X/700/1/L1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 469FG UT WOS:000267880600001 ER PT J AU Risaliti, G Young, M Elvis, M AF Risaliti, G. Young, M. Elvis, M. TI THE SLOAN DIGITAL SKY SURVEY/XMM-NEWTON QUASAR SURVEY: CORRELATION BETWEEN X-RAY SPECTRAL SLOPE AND EDDINGTON RATIO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; ACCRETION RATE; EMISSION; REDSHIFT; SAMPLE; BROAD; GALAXIES; GROWTH AB We present a correlation between the 2-10 keV spectral slope Gamma(X) and the Eddington ratio L/L(EDD) in a sample of similar to 400 Sloan Digital Sky Survey (SDSS) quasars with available hard X-ray spectra from XMM-Newton serendipitous observations. We find that the Gamma(X)-L/L(EDD) correlation is strongest in objects with black hole (BH) masses determined from the H beta line, and weaker (but still present) for those based on Mg II. An empirical nonlinear correction of the Mg II-based masses, obtained by comparing the mass estimates in SDSS quasars having both H beta and Mg II measurements, significantly increases the strength of the correlation. No correlation is found among objects with BH masses derived from C IV, confirming that this line is not a reliable indicator of the BH mass. No significant correlation is found with the bolometric luminosity, while a Gamma(X)-M(BH) relation is present, though with a lower statistical significance than between Gamma(X) and L/L(EDD). Our results imply a physical link between the accretion efficiency in the (cold) accretion disk of active galactic nuclei and the physical status of the (hot) corona responsible for the X-ray emission. C1 [Risaliti, G.; Young, M.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Young, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Risaliti, Guido/0000-0002-3556-977X FU ASI-INAF [I/088/06/0]; NASA [NNX07AI22G]; [2006025203] FX We are grateful to the referee for his/her constructive comments. This work has been partly supported by grants prin-miur 2006025203, ASI-INAF I/088/06/0, and NASA NNX07AI22G. NR 21 TC 52 Z9 52 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2009 VL 700 IS 1 BP L6 EP L10 DI 10.1088/0004-637X/700/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 469FG UT WOS:000267880600002 ER PT J AU Soyler, SG Capogrosso-Sansone, B Prokof'ev, NV Svistunov, BV AF Soeyler, S. G. Capogrosso-Sansone, B. Prokof'ev, N. V. Svistunov, B. V. TI Sign-alternating interaction mediated by strongly correlated lattice bosons SO NEW JOURNAL OF PHYSICS LA English DT Article ID OPTICAL LATTICES; GASES; PHYSICS; ATOMS AB We reveal a generic mechanism of generating sign-alternating intersite interactions mediated by strongly correlated lattice bosons. The ground-state phase diagram of the two-component hard-core Bose-Hubbard model on a square lattice at half-integer filling factor for each component, obtained by worm algorithm Monte Carlo simulations, is strongly modified by these interactions and features the solid + superfluid (SF) phase for strong asymmetry between the hopping amplitudes. The new phase is a direct consequence of the effective nearest-neighbor repulsion between 'heavy' atoms mediated by the 'light' SF component. Due to their sign-alternating character, mediated interactions lead to a rich variety of yet to be discovered quantum phases. C1 [Soeyler, S. G.; Capogrosso-Sansone, B.; Prokof'ev, N. V.; Svistunov, B. V.] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Prokof'ev, N. V.; Svistunov, B. V.] Russian Res Ctr, Kurchatov Inst, Moscow 123182, Russia. RP Soyler, SG (reprint author), Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. EM soyler@physics.umass.edu RI PROKOFIEV, NIKOLAY/F-6865-2010 FU ITAMP; DARPA OLE program; NSF [PHY-0653183] FX We thank L Pollet, E Demler and M Lukin for fruitful discussions. This work was supported by ITAMP, DARPA OLE program and NSF grant PHY-0653183. NR 30 TC 45 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUL 17 PY 2009 VL 11 AR 073036 DI 10.1088/1367-2630/11/7/073036 PG 8 WC Physics, Multidisciplinary SC Physics GA 474ZT UT WOS:000268324500004 ER PT J AU Evans, NM Lindner, A Raikova, EV Collins, AG Cartwright, P AF Evans, Nathaniel M. Lindner, Alberto Raikova, Ekaterina V. Collins, Allen G. Cartwright, Paulyn TI Phylogenetic placement of the enigmatic parasite, Polypodium hydriforme, within the Phylum Cnidaria (vol 8, pg 139, 2008) SO BMC EVOLUTIONARY BIOLOGY LA English DT Correction AB Correction to Evans, N. M., Lindner, A., Raikova, E. V., Collins, A. G. and Cartwright, P. Phylogenetic placement of the enigmatic parasite, Polypodium hydriforme, within the phylum Cnidaria. BMC Evol Biol, 2008, 8:139. C1 [Evans, Nathaniel M.; Cartwright, Paulyn] Univ Kansas, Dept Ecol & Evolut Biol, Lawrence, KS 66045 USA. [Lindner, Alberto] Univ Sao Paulo, CEBIMar, Sao Sebastiao, Brazil. [Raikova, Ekaterina V.] Russian Acad Sci, Inst Cytol, St Petersburg 194064, Russia. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, NOAA Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. RP Cartwright, P (reprint author), Univ Kansas, Dept Ecol & Evolut Biol, Lawrence, KS 66045 USA. EM evansnat@ku.edu; alindner@usp.br; raikova@swipnet.se; COLLINSA@si.edu; pcart@ku.edu RI Lindner, Alberto/E-1946-2013; OI Evans, Nathaniel/0000-0003-4524-372X NR 1 TC 1 Z9 1 U1 2 U2 10 PU BIOMED CENTRAL LTD PI LONDON PA CURRENT SCIENCE GROUP, MIDDLESEX HOUSE, 34-42 CLEVELAND ST, LONDON W1T 4LB, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD JUL 15 PY 2009 VL 9 AR 165 DI 10.1186/1471-2148-9-165 PG 2 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 479QD UT WOS:000268675100001 PM 19604374 ER PT J AU Ren, ZM Zhu, B Ma, EB Wen, J Tu, TY Cao, Y Hasegawa, M Zhong, Y AF Ren, Zhumei Zhu, Bin Ma, Enbo Wen, Jun Tu, Tieyao Cao, Ying Hasegawa, Masami Zhong, Yang TI Complete nucleotide sequence and gene arrangement of the mitochondrial genome of the crab-eating frog Fejervarya cancrivora and evolutionary implications SO GENE LA English DT Article DE Crab-eating frog; Fejervarya cancrivora; Mitochondrial genome; Rearrangement; Phylogeny ID RIBOSOMAL-RNA GENES; PHYLOGENETIC-RELATIONSHIPS; DNA-SEQUENCES; RANA-CANCRIVORA; NUCLEAR GENES; RICE FROG; FAMILY RHACOPHORIDAE; CROSSING EXPERIMENTS; STRUCTURAL FEATURES; MOLECULAR PHYLOGENY AB The complete nucleotide sequence of the mitochondrial (mt) genome of the crab-eating frog, Fejervarya cancrivora Gravenhorst (Amphibia: Anura: Ranidae), was determined. The mt genome is 17,843 bp long and contains 13 protein-coding (ATP6, ATP8, COI-III, ND1-6 and 4L, and Cyt b) and two ribosomal RNA (12S and 16SrRNA) genes. Although metazoan mt genomes typically encode 22 transfer RNA genes (tRNAs), the E cancrivora mtDNA contains 23 tRNAs due to the presence of an extra copy of tRNA(Met). A major noncoding region and a prominent intergenic spacer corresponding to the control region and light-strand replication origin were also found. To confirm the phylogenetic position of F cancrivora, we compared the gene arrangement with that of other anurans and performed phylogenetic analyses based on mt genomic data. The genome organization of E cancrivora mtDNA differs from that of typical vertebrates and neobatrachian frogs but is identical with that of F limnocharis, suggesting that the unique gene arrangement occurred in the common ancestor of the genus. Phylogenetic analyses supported the monophyly of the Fejervarya species used here as well as the dicroglossini clade. Although the family Ranidae as previously recognized (=Ranidae, Discoglossidae, and some other natatanuran families; sensu Frost et al., 2006) is shown as a clade in the maximum parsimony analysis, the maximum likelihood and the Bayesian analyses suggest the paraphyly of the Ranidae with respect to the families, Mantellidae and Rhacophoridae. Three-tandem duplications of gene regions followed by subsequent deletions of supernumerary genes were proposed to explain the evolution of the extra tRNA(Met) and translocation of ND5 from the original neobatrachian gene order. (C) 2008 Published by Elsevier B.V. C1 [Zhu, Bin; Hasegawa, Masami; Zhong, Yang] Fudan Univ, Sch Life Sci, Shanghai 200433, Peoples R China. [Ren, Zhumei; Ma, Enbo] Shanxi Univ, Coll Life Sci & Technol, Taiyuan 030006, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Tu, Tieyao] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. [Tu, Tieyao] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Cao, Ying] Inst Stat Math, Minato Ku, Tokyo 106, Japan. [Cao, Ying] Grad Univ Adv Studies, Dept Biosyst Sci, Kanagawa 2400193, Japan. [Zhong, Yang] Shanghai Ctr Bioinformat Technol, Shanghai 200433, Peoples R China. RP Zhong, Y (reprint author), Fudan Univ, Sch Life Sci, Shanghai 200433, Peoples R China. EM yangzhong@fudan.edu.cn FU National Natural Science Foundation [30670361]; Natural Science Foundation Shanxi Province [2007011078]; National infrastructure of Natural Resources for Science and Technology [2005DKA21403]; Shanghai Leading Academic Discipline Project [B111]; Shanghai Science and Technology Committee [07XD14025] FX This project was partially supported by National Natural Science Foundation (30670361), Natural Science Foundation Shanxi Province (2007011078), National infrastructure of Natural Resources for Science and Technology (2005DKA21403), Shanghai Leading Academic Discipline Project (B111), and Shanghai Science and Technology Committee (07XD14025). We would like to thank Lee Weigt and Edward Staples as well as the two anonymous reviewers for critical reading on the manuscript, Dr. Lei Xie for data analyses, Dr. Qingbiao Wang and Mr. Dangwei Zhou for technical assistance, and two anonymous reviewers for their critical comments and suggestions. NR 71 TC 16 Z9 19 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1119 J9 GENE JI Gene PD JUL 15 PY 2009 VL 441 IS 1-2 BP 148 EP 155 DI 10.1016/j.gene.2008.09.010 PG 8 WC Genetics & Heredity SC Genetics & Heredity GA 460YP UT WOS:000267229600019 PM 18848608 ER PT J AU Ritson-Williams, R Shjegstad, SM Paul, VJ AF Ritson-Williams, Raphael Shjegstad, Sonia M. Paul, Valerie J. TI Larval metamorphosis of Phestilla spp. in response to waterborne cues from corals SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Coral predators; Larval ecology; Metamorphosis; Phestilla ID URCHIN HOLOPNEUSTES-PURPURASCENS; ADALARIA-PROXIMA GASTROPODA; SPECIALIST MARINE HERBIVORE; SUPPLY-SIDE ECOLOGY; BEHAVIORAL-RESPONSES; SETTLEMENT CUES; ALDERIA-MODESTA; SIBOGAE BERGH; NUDIBRANCH; OPISTHOBRANCHIA AB Many marine invertebrates depend on their larvae for dispersal and to settle and metamorphose in the appropriate habitat for adult survival, yet the mechanisms of habitat selection remain poorly understood. In Hawaii, the nudibranch Phestilla sibogae only feeds on Porites compressa and requires a water-soluble cue from this coral for metamorphosis. On Guam, we tested three different species of Phestilla to determine if their larvae require water-soluble compounds from corals to induce metamorphosis. Larvae of P sibogae metamorphosed at high rates to waterborne cues from multiple species of corals in the genus Porites. Larvae of Phestilla minor could distinguish among waterborne compounds from different species of Porites, but also had high rates of metamorphosis in filtered seawater and in response to corals that adults did not eat. Larvae of Phestilla sp. 2 could distinguish among water-soluble cues from different species of Goniopora and consistently had the highest rates of metamorphosis in response to waterborne cues released from Goniopora fruticosa. P. minor was the only species studied that did not require waterborne cues for larval metamorphosis. Published by Elsevier B.V. C1 [Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM williams@si.edu FU NSF [OCE-9911867, OCE-0317707] FX Special thanks to the staff and students of the University of Guam Marine Laboratory for their help collecting coral and nudibranchs. Clay Carlson and Michael Hadfield provided invaluable advice on the taxonomy of Phestilla and the larval experiments. Thanks to the anonymous reviewers whose suggestions greatly improved this manuscript. All animals were collected according to the Guam Department of Agriculture Division of Aquatic and Wildlife Resources regulations. This work was supported by NSF grant OCE-9911867 and OCE-0317707 to V. J. Paul. This manuscript is the University of Guam Marine Laboratory contribution # 624 and the Smithsonian Marine Station at Fort Pierce contribution # 784. [SS] NR 39 TC 5 Z9 6 U1 3 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD JUL 15 PY 2009 VL 375 IS 1-2 BP 84 EP 88 DI 10.1016/j.jembe.2009.05.010 PG 5 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 475YI UT WOS:000268403200012 ER PT J AU Glaze, LS Baloga, SM Garry, WB Fagents, SA Parcheta, C AF Glaze, Lori S. Baloga, Stephen M. Garry, W. Brent Fagents, Sarah A. Parcheta, Carolyn TI A hybrid model for leveed lava flows: Implications for eruption styles on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VOLCANO; EMPLACEMENT; MORPHOLOGY; HAWAII; ROCKS; QUANTIFICATION; RHEOLOGY; PAHOEHOE; CHANNELS; ICELAND AB Many channelized lava flows on the plains of Mars have substantial embanking margins and levees inferred to have been stationary while the central channel was active. Levee formation can be attributed to two end-member processes during emplacement: construction during passage of the flow front and growth along the entire length of the flow while it is active. It is shown here that the amount of lava that can be deposited by the flow front alone is limited. Estimates of the levee volume for many Mars plains flows exceed this limit and must have formed by processes that continued after the passage of the front. Experimental studies of analogous laboratory flows also indicate a combination of both modes of emplacement. A model that combines both modes of levee formation is presented, including a method for estimating volumetric flow rate, eruption duration, and viscosity. Six lava flows on the plains of the Tharsis volcanic province are used as illustrative examples. Crustal thicknesses for the six flows examined range from 9 to 23 m. Estimated emplacement times required to cool crusts of these thicknesses range from 1 year to 10 years. Corresponding viscosities are on the order of 10(5)-10(6) Pa s. Effusion rates range from 25 to 840 m(3) s(-1) and are all within the range of terrestrial observations. Therefore, the large leveed plains flows on Mars are not dramatically different in eruption rate or lava viscosity from large terrestrial analogs. C1 [Glaze, Lori S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Baloga, Stephen M.] Proxemy Res, Gaithersburg, MD 20882 USA. [Fagents, Sarah A.; Parcheta, Carolyn] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Garry, W. Brent] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Glaze, LS (reprint author), NASA, Goddard Space Flight Ctr, Code 698, Greenbelt, MD 20771 USA. EM Lori.S.Glaze@nasa.gov; Steve@proxemy.com; GarryW@si.edu; fagents@higp.hawaii.edu; parcheta@hawaii.edu RI Glaze, Lori/D-1314-2012; Garry, Brent/I-5920-2013; Fagents, Sarah/B-3983-2014 FU NASA Mars Data Analysis Program [NAG5-13348, NNX06AD98G] FX The authors would like to thank Laszlo Keszthelyi and an anonymous reviewer for helpful suggestions for improving this manuscript. Support for this work was provided by the NASA Mars Data Analysis Program through grants NAG5-13348 (S. A. F. and C. P.) and NNX06AD98G (S. M. B.) and RTOP support for L. Glaze. NR 46 TC 11 Z9 11 U1 0 U2 4 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 JUL 14 PY 2009 VL 114 AR E07001 DI 10.1029/2008JE003278 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 512OF UT WOS:000271258800001 ER PT J AU Hardcastle, MJ Evans, DA Croston, JH AF Hardcastle, M. J. Evans, D. A. Croston, J. H. TI The active nuclei of z < 1.0 3CRR radio sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; X-rays: galaxies ID BL-LACERTAE OBJECTS; XMM-NEWTON OBSERVATIONS; ACCRETING BLACK-HOLES; X-RAY OBSERVATIONS; 7C REDSHIFT SURVEY; GALACTIC NUCLEI; COMPLETE SAMPLE; UNIFIED MODELS; EMISSION-LINE; INFRARED PROPERTIES AB We combine Chandra and XMM-Newton X-ray data from our previous papers with new X-ray observations and with Spitzer mid-infrared (mid-IR) data in order to study the nature of the nuclei of radio galaxies and radio-loud quasars with z < 1.0 from the 3CRR sample. The significant increase in sample size over our previous work, the reduction of bias in the sample as a result of new observations and the availability of more mid-IR data allow us to show conclusively that almost all objects classed as low-excitation radio galaxies in optical spectroscopic studies lack a radiatively efficient active nucleus. We show that the distribution of absorbing columns in the narrow-line radio galaxies differs from the population of X-ray-selected radio-quiet type 2 quasars and from that in local Seyfert 2s. We comment on the current evidence for the nature of the soft X-ray component in radio-galaxy nuclear spectra, concluding that a jet origin for this component is very hard to evade. Finally, we discuss the recently discovered 'fundamental plane' of black hole activity, showing that care must be taken when placing radio-loud active galactic nucleus (AGN) on such diagnostic diagrams. C1 [Hardcastle, M. J.; Croston, J. H.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Evans, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM mjh@star.herts.ac.uk RI Hardcastle, Martin/E-2264-2012 OI Hardcastle, Martin/0000-0003-4223-1117 FU Royal Society for a research; NASA XMM-Newton GO program [NNX07AQ52G, NNX08AX30G] FX MJH thanks the Royal Society for a research fellowship. DAE acknowledges partial financial support from the NASA XMM-Newton GO program, through grants NNX07AQ52G and NNX08AX30G. We are very grateful to Vincenzo Mainieri for providing data on the COSMOS sample of X-ray-selected type 2 quasars in advance of publication, to Elmar Kording for discussion of the fundamental plane relation, to Matt Jarvis for discussion of the expectations from receding-torus models, and to Chiranjib Konar for allowing us to use XMM-Newton data on 3C 457 obtained for another purpose in this paper. We thank an anonymous referee for helpful comments on the paper. This work is partly based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). NR 82 TC 88 Z9 88 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 11 PY 2009 VL 396 IS 4 BP 1929 EP 1952 DI 10.1111/j.1365-2966.2009.14887.x PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467BG UT WOS:000267710400009 ER PT J AU Keres, D Katz, N Dave, R Fardal, M Weinberg, DH AF Keres, Dusan Katz, Neal Dave, Romeel Fardal, Mark Weinberg, David H. TI Galaxies in a simulated Lambda CDM universe - II. Observable properties and constraints on feedback SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical - cooling flows; galaxies: evolution; galaxies: formation; galaxies: luminosity function; mass function ID SMOOTHED PARTICLE HYDRODYNAMICS; STAR-FORMING GALAXIES; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; DWARF GALAXIES; COSMOLOGICAL SIMULATIONS; LOCAL UNIVERSE; MASS FUNCTION; STELLAR MASS AB We compare the properties of galaxies that form in a cosmological simulation without strong feedback to observations of the z = 0 galaxy population. We confirm previous findings that models without strong feedback overproduce the observed galaxy baryonic mass function, especially at the low- and high-mass extremes. Through post-processing we investigate what kinds of feedback would be required to reproduce the statistics of observed galaxy masses and star formation rates. To mimic an extreme form of 'preventive' feedback, such as a highly efficient active galactic nucleus 'radio mode', we remove all baryonic mass that was originally accreted from shock-heated gas ('hot-mode' accretion). This removal does not bring the high-mass end of the galaxy mass function into agreement with observations because much of the stellar mass in these systems formed at high redshift from baryons that originally accreted via 'cold mode' on to lower mass progenitors. An efficient 'ejective' feedback mechanism, such as supernova-driven galactic winds, must reduce the masses of these progenitors before they merge to form today's massive galaxies. Feedback must also reduce the masses of lower mass z = 0 galaxies, which assemble at lower redshifts and have much lower star formation rates. If we monotonically remap galaxy masses to reproduce the observed mass function, but retain the simulation-predicted star formation rates, we obtain fairly good agreement with the observed sequence of star-forming galaxies. However, we fail to recover the observed population of passive, low star formation rate galaxies, especially at the high-mass end. Suppressing all hot-mode accretion improves the agreement for high-mass galaxies, but it worsens the agreement at intermediate masses. Reproducing these z = 0 observations requires a feedback mechanism that dramatically suppresses star formation in a fraction of galaxies, increasing with mass, while leaving star formation rates of other galaxies essentially unchanged. C1 [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Katz, Neal; Fardal, Mark] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Dave, Romeel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Keres, D (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM dkeres@cfa.harvard.edu; nsk@astro.umass.edu; rad@astro.as.arizona.edu; fardal@astro.umass.edu; dhw@astronomy.ohio-state.edu FU NSF [AST-0205969]; NASA [NAGS-13308, NNG04GK68G] FX We are grateful to Samir Salim for sharing with us stellar masses and SSFRs from his paper and for useful comments. DK acknowledges the support of the ITC fellowship at the Harvard College Observatory. We also acknowledge support from NSF grant AST-0205969 and from NASA grants NAGS-13308 and NNG04GK68G. NR 86 TC 90 Z9 90 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 JUL 11 PY 2009 VL 396 IS 4 BP 2332 EP 2344 DI 10.1111/j.1365-2966.2009.14924.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 467BG UT WOS:000267710400040 ER PT J AU Yeates, AR Mackay, DH AF Yeates, A. R. Mackay, D. H. TI INITIATION OF CORONAL MASS EJECTIONS IN A GLOBAL EVOLUTION MODEL SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections; Sun: evolution; Sun: magnetic fields ID SOLAR ACTIVE REGIONS; LARGE-SCALE CORONA; OPEN MAGNETIC-FLUX; HEMISPHERIC PATTERN; ERUPTIVE PROMINENCE; FILAMENT CHANNELS; CURRENT HELICITY; FIELDS; SUN; FORCE AB Loss of equilibrium of magnetic flux ropes is a leading candidate for the origin of solar coronal mass ejections (CMEs). The aim of this paper is to explore to what extent this mechanism can account for the initiation of CMEs in the global context. A simplified MHD model for the global coronal magnetic field evolution in response to flux emergence and shearing by large-scale surface motions is described and motivated. Using automated algorithms for detecting flux ropes and ejections in the global magnetic model, the effects of key simulation parameters on the formation of flux ropes and the number of ejections are considered, over a 177 day period in 1999. These key parameters include the magnitude and sign of magnetic helicity emerging in active regions, and coronal diffusion. The number of flux ropes found in the simulation at any one time fluctuates between about 28 and 48, sustained by the emergence of new bipolar regions, but with no systematic dependence on the helicity of these regions. However, the emerging helicity does affect the rate of flux rope ejections, which doubles from 0.67 per day if the bipoles emerge untwisted to 1.28 per day in the run with greatest emerging twist. The number of ejections in the simulation is also increased by 20%-30% by choosing the majority sign of emerging bipole helicity in each hemisphere, or by halving the turbulent diffusivity in the corona. For reasonable parameter choices, the model produces approximately 50% of the observed CME rate. This indicates that the formation and loss of equilibrium of flux ropes may be a key element in explaining a significant fraction of observed CMEs. C1 [Yeates, A. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yeates, A. R.; Mackay, D. H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RP Yeates, AR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ayeates@cfa.harvard.edu; duncan@mcs.st-and.ac.uk RI Yeates, Anthony/D-1338-2014 OI Yeates, Anthony/0000-0002-2728-4053 FU SRIF/STFC; NASA/LWS [NNG05GK32G]; NASA [NNM07AB07C]; UK STFC; Royal Society FX We thank A. A. van Ballegooijen, P. C. H. Martens, and the anonymous referee for useful suggestions that have led to significant improvements in the paper's presentation. The simulations were performed on the UKMHD parallel computer in St Andrews, funded jointly by SRIF/STFC. A.R.Y. acknowledges financial support from NASA/LWS grant NNG05GK32G, from NASA contract NNM07AB07C, from the UK STFC, and from the Solar Physics NSF-REU program at Montana State University, during which this work was initiated. D. H. M. thanks the STFC for financial support, and the Royal Society for support through their research grant scheme. Synoptic magnetogram data from NSO/Kitt Peak were produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL, and made publicly accessible on the World Wide Web. NR 80 TC 32 Z9 32 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 JUL 10 PY 2009 VL 699 IS 2 BP 1024 EP 1037 DI 10.1088/0004-637X/699/2/1024 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500013 ER PT J AU Hong, J Van den Berg, M Laycock, S Grindlay, JE Zhao, P AF Hong, JaeSub Van den Berg, Maureen Laycock, Silas Grindlay, Jonathan E. Zhao, Ping TI CHANDRA DISCOVERY OF AN INTERMEDIATE POLAR IN BAADE'S WINDOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; Galaxy: bulge; X-rays: binaries ID X-RAY SOURCES; GALACTIC-CENTER; CATACLYSMIC VARIABLES; CATALOG; VARIABILITY; EMISSION; FIELDS; BULGE; MAPS AB We have discovered an intermediate polar (IP) in the 100 ks Chandra observation of Baade's window (BW), a low extinction region at about 4 degrees south of the Galactic center. The source exhibits large X-ray modulations at a period of 1028.4 s in the 0.3-8 keV band. The X-ray spectral fit with a power-law model shows that the integrated spectrum is intrinsically hard (photon index Gamma = 0.44 +/- 0.05) and moderately absorbed (N(H) = 1.5 +/- 1.0 x 10(21) cm(-2)). The relatively poor statistics only allow for a mild constraint on the presence of an iron emission line (equivalent width = 0.5 +/- 0.3 keV at 6.7 keV). Quantile analysis reveals that the modulations in the X-ray flux strongly correlate with spectral changes that are dominated by varying internal absorption. The X-ray spectrum of the source is heavily absorbed (NH > 10(22) cm(-2)) during the faint phases, while the absorption is consistent with the field value (similar to 10(21) cm(-2)) during the bright phases. These X-ray properties are typical signatures of IPs. Images taken with the IMACS camera on the Magellan 6.5 m telescope show a faint (V similar to 22), relatively blue object (B(0) - V(0) greater than or similar to 0.05) within the 2 sigma error circle of the Chandra source, which is a good candidate for being the optical counterpart. If we assume a nominal range of absolute V magnitude for a cataclysmic variable (M(V) similar to 5.5-10.5) and the known reddening in the region (A(V) = 1.4 at > 3 kpc), the source would likely be at a distance of 2-10 kpc and not in the local solar neighborhood. The corresponding average X-ray luminosity would be 6 x 10(31) - 10(33) erg s(-1) in the 2-8 keV band. Assuming the space density of IPs follows the stellar distribution, which is highly concentrated in the Galactic bulge, the source is probably a relatively bright IP (similar to 10(33) erg s(-1) if it is at 8 kpc) belonging to the Galactic bulge X-ray population, the majority of which is now believed to be magnetic cataclysmic variables. C1 [Hong, JaeSub; Van den Berg, Maureen; Grindlay, Jonathan E.; Zhao, Ping] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Laycock, Silas] Gemini Observ, Hilo, HI 96720 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu FU NASA/Chandra [GO6-7088X, GO7-8090X, GO8-9093X] FX We thank A. Ruiter for providing the X-ray-luminosity distribution of IPs. This work is supported in part by NASA/Chandra grants GO6-7088X, GO7-8090X, and GO8-9093X. NR 31 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1053 EP 1058 DI 10.1088/0004-637X/699/2/1053 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500015 ER PT J AU Morales, FY Werner, MW Bryden, G Plavchan, P Stapelfeldt, KR Rieke, GH Su, KYL Beichman, CA Chen, CH Grogan, K Kenyon, SJ Moro-Martin, A Wolf, S AF Morales, Farisa Y. Werner, M. W. Bryden, G. Plavchan, P. Stapelfeldt, K. R. Rieke, G. H. Su, K. Y. L. Beichman, C. A. Chen, C. H. Grogan, K. Kenyon, S. J. Moro-Martin, A. Wolf, S. TI SPITZER MID-IR SPECTRA OF DUST DEBRIS AROUND A AND LATE B TYPE STARS: ASTEROID BELT ANALOGS AND POWER-LAW DUST DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; planetary systems: formation; stars: individual (HD 1404, HD 10939, HD 23267, HD 23642, HD 23763, HD 24141, HD 24817, HD 28355, HD 30422, HD 32977, HD 37286, HD 38056, HD 38206, HD 70313, HD 71722, HD 74873, HD 79108, HD 80950, HD 87696, HD 92536, HD 93738, HD 98673, HD 110411, HD 115892, HD 125283, HD 126135, HD 128207, HD 132238, HD 135379, HD 135454, HD 136246, HD 136347, HD 136482, HD 137015, HD 138923, HD 138965, HD 141378, HD 142139, HD 145964, HD 153053, HD 159170, HD 159492, HD 166046, HD 182919, HD 183324, HD 191174, HD 192425, HD 196544, HD 215766, HD 220825, HD 223352, HD 225200) ID SUN-LIKE STARS; MULTIBAND IMAGING PHOTOMETER; SOLAR-TYPE STARS; SPACE-TELESCOPE; BETA-PICTORIS; CIRCUMSTELLAR DISK; KUIPER-BELT; HR 4796A; ABSOLUTE CALIBRATION; INFRARED-EMISSION AB Using the Spitzer/Infrared Spectrograph (IRS) low-resolution modules covering wavelengths from 5 to 35 mu m, we observed 52 main-sequence A and late B type stars previously seen using Spitzer/Multiband Imaging Photometer (MIPS) to have excess infrared emission at 24 mu m above that expected from the stellar photosphere. The mid-IR excess is confirmed in all cases but two. While prominent spectral features are not evident in any of the spectra, we observed a striking diversity in the overall shape of the spectral energy distributions. Most of the IRS excess spectra are consistent with single-temperature blackbody emission, suggestive of dust located at a single orbital radius-a narrow ring. Assuming the excess emission originates from a population of large blackbody grains, dust temperatures range from 70 to 324 K, with a median of 190 K corresponding to a distance of 10 AU. Thirteen stars however, have dust emission that follows a power-law distribution, F(nu) = F(0)lambda(alpha), with exponent alpha ranging from 1.0 to 2.9. The warm dust in these systems must span a greater range of orbital locations-an extended disk. All of the stars have also been observed with Spitzer/MIPS at 70 mu m, with 27 of the 50 excess sources detected (signal-to-noise ratio > 3). Most 70 mu m fluxes are suggestive of a cooler, Kuiper Belt-like component that may be completely independent of the asteroid belt-like warm emission detected at the IRS wavelengths. Fourteen of 37 sources with blackbody-like fits are detected at 70 mu m. The 13 objects with IRS excess emission fit by a power-law disk model, however, are all detected at 70 mu m (four above, three on, and six below the extrapolated power law), suggesting that the mid-IR IRS emission and far-IR 70 mu m emission may be related for these sources. Overall, the observed blackbody and power-law thermal profiles reveal debris distributed in a wide variety of radial structures that do not appear to be correlated with spectral type or stellar age. An additional 43 fainter A and late B type stars without 70 mu m photometry were also observed with Spitzer/IRS; results are summarized in Appendix B. C1 [Morales, Farisa Y.; Werner, M. W.; Bryden, G.; Stapelfeldt, K. R.; Beichman, C. A.; Grogan, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Morales, Farisa Y.] Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA. [Plavchan, P.; Beichman, C. A.] CALTECH, NExScI, Pasadena, CA 91125 USA. [Rieke, G. H.; Su, K. Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chen, C. H.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kenyon, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Moro-Martin, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. [Wolf, S.] Univ Kiel, Inst Theor Phys & Astrophys, D-24118 Kiel, Germany. RP Morales, FY (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Farisa@jpl.nasa.gov RI Stapelfeldt, Karl/D-2721-2012; OI Kenyon, Scott/0000-0003-0214-609X; Su, Kate/0000-0002-3532-5580 NR 55 TC 48 Z9 48 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1067 EP 1086 DI 10.1088/0004-637X/699/2/1067 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500017 ER PT J AU Roman-Duval, J Jackson, JM Heyer, M Johnson, A Rathborne, J Shah, R Simon, R AF Roman-Duval, Julia Jackson, James M. Heyer, Mark Johnson, Alexis Rathborne, Jill Shah, Ronak Simon, Robert TI KINEMATIC DISTANCES TO MOLECULAR CLOUDS IDENTIFIED IN THE GALACTIC RING SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: structure; H II regions; ISM: clouds; molecular data ID INFRARED DARK CLOUDS; H-II REGIONS; STAR-FORMATION; MILKY-WAY; TRIGONOMETRIC PARALLAXES; ATOMIC-HYDROGEN; BOSTON-UNIVERSITY; SELF-ABSORPTION; CARBON-MONOXIDE; SPIRAL-ARM AB Kinematic distances to 750 molecular clouds identified in the (13)CO J = 1 -> 0 Boston University-Five College Radio Astronomy Observatory Galactic Ring Survey (GRS) are derived assuming the Clemens rotation curve of the Galaxy. The kinematic distance ambiguity is resolved by examining the presence of Hi self-absorption toward the 13CO emission peak of each cloud using the Very Large Array Galactic Plane Survey. We also identify 21 cm continuum sources embedded in the GRS clouds in order to use absorption features in the Hi 21 cm continuum to distinguish between near and far kinematic distances. The Galactic distribution of GRS clouds is consistent with a four-arm model of the Milky Way. The locations of the Scutum-Crux and Perseus arms traced by GRS clouds match star-count data from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire star-count data. We conclude that molecular clouds must form in spiral arms and be short-lived (lifetimes < 10(7) yr) in order to explain the absence of massive, (13)CO bright molecular clouds in the interarm space. C1 [Roman-Duval, Julia; Jackson, James M.; Johnson, Alexis] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Heyer, Mark] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Rathborne, Jill] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Simon, Robert] MIT, Lincoln Lab, Lexington, MA 02134 USA. [Simon, Robert] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. RP Roman-Duval, J (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. EM jduval@bu.edu; jackson@bu.edu OI Shah, Ronak/0000-0002-2801-6317 FU NSF [AST-0507657]; National Science Foundation [AST 98-00334, AST 00-98562, AST 01-00793, AST 02-28993, AST 05-07657] FX This work was supported by NSF grant AST-0507657. The molecular line data used in this paper are from the BU-FCRAO GRS, a joint project of Boston University and the Five College Radio Astronomy Observatory funded by the National Science Foundation under grants AST 98-00334, AST 00-98562, AST 01-00793, AST 02-28993, and AST 05-07657. The authors also gratefully acknowledge the contribution of Robert Benjamin, who provided the two-arm model of the Milky Way, and the referee, whose careful reading resulted in a much improved presentation. NR 57 TC 100 Z9 101 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1153 EP 1170 DI 10.1088/0004-637X/699/2/1153 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500025 ER PT J AU Dallacasa, D Brunetti, G Giacintucci, S Cassano, R Venturi, T Macario, G Kassim, NE Lane, W Setti, G AF Dallacasa, D. Brunetti, G. Giacintucci, S. Cassano, R. Venturi, T. Macario, G. Kassim, N. E. Lane, W. Setti, G. TI DEEP 1.4 GHz FOLLOW-UP OF THE STEEP SPECTRUM RADIO HALO IN A521 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; galaxies: clusters: individual (A521); radiation mechanisms: non-thermal; radio continuum: general ID COSMIC-RAY PROTONS; GALAXY CLUSTERS; ALFVENIC REACCELERATION; PARTICLE REACCELERATION; RELATIVISTIC-PARTICLES; COMA CLUSTER; GAMMA-RAY; EMISSION; ELECTRONS; ORIGIN AB In a recent paper, we reported on the discovery of a radio halo with very steep spectrum in the merging galaxy cluster A521 through observations with the Giant Metrewave Radio Telescope. We showed that the steep spectrum of the halo is inconsistent with a secondary origin of the relativistic electrons and supports a turbulent acceleration scenario. At that time, due to the steep spectrum, the available observations at 1.4 GHz (archival NRAO-Very Large Array-VLA-CnB-configuration data) were not adequate to accurately determine the flux density associated with the radio halo. In this paper, we report the detection at 1.4 GHz of the radio halo in A521 using deep VLA observations in the D configuration. We use these new data to confirm the steep spectrum of the object. We consider A521 the prototype of a population of very steep spectrum halos. This population is predicted assuming that turbulence plays an important role in the acceleration of relativistic particles in galaxy clusters, and we expect it will be unveiled by future surveys at low frequencies with the LOFAR and LWA radio telescopes. C1 [Dallacasa, D.; Macario, G.; Setti, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Brunetti, G.; Cassano, R.; Venturi, T.; Macario, G.; Setti, G.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kassim, N. E.; Lane, W.] USN, Res Lab, Washington, DC 20375 USA. RP Dallacasa, D (reprint author), Univ Bologna, Dipartimento Astron, Via Ranzani 1, I-40127 Bologna, Italy. OI Cassano, Rossella/0000-0003-4046-0637; Venturi, Tiziana/0000-0002-8476-6307; Brunetti, Gianfranco/0000-0003-4195-8613 FU INAF [PRIN-INAF2007]; ASI [ASI-INAF I/088/06/0] FX This work is partially supported by INAF under grant PRIN-INAF2007 and by ASI under grant ASI-INAF I/088/06/0. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 base funds. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. NR 36 TC 34 Z9 34 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1288 EP 1292 DI 10.1088/0004-637X/699/2/1288 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500037 ER PT J AU Williams, JP Mann, RK Beaumont, CN Swift, JJ Adams, JD Hora, J Kassis, M Lada, EA Roman-Zuniga, CG AF Williams, Jonathan P. Mann, Rita K. Beaumont, Christopher N. Swift, Jonathan J. Adams, Joseph D. Hora, Joe Kassis, Marc Lada, Elizabeth A. Roman-Zuniga, Carlos G. TI DIVERSE PROTOSTELLAR EVOLUTIONARY STATES IN THE YOUNG CLUSTER AFGL961 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: structure; stars: formation; stars: pre-main sequence ID SPECTRAL ENERGY-DISTRIBUTIONS; ROSETTE MOLECULAR CLOUD; SUBMILLIMETER CONTINUUM OBSERVATIONS; MASS STAR-FORMATION; STELLAR OBJECTS; NGC 2244; COMPLEX; EMISSION; NEBULA; MODELS AB We present arcsecond resolution mid-infrared and millimeter observations of the center of the young stellar cluster AFGL961 in the Rosette molecular cloud. Within 0.2 pc of each other, we find an early B star embedded in a dense core, a neighboring star of similar luminosity with no millimeter counterpart, a protostar that has cleared out a cavity in the circumcluster envelope, and two massive, dense cores with no infrared counterparts. An outflow emanates from one of these cores, indicating a deeply embedded protostar, but the other is starless, bound, and appears to be collapsing. The diversity of states implies either that protostellar evolution is faster in clusters than in isolation or that clusters form via quasi-static rather than dynamic collapse. The existence of a pre-stellar core at the cluster center shows that some star formation continues after and in close proximity to massive, ionizing stars. C1 [Williams, Jonathan P.; Mann, Rita K.; Beaumont, Christopher N.; Swift, Jonathan J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Adams, Joseph D.] Cornell Univ, Dept Radiophys Space Res, Ithaca, NY 14853 USA. [Hora, Joe] CfA, Harvard Smithsonian, Cambridge, MA 02138 USA. [Kassis, Marc] Keck Observ, Kamuela, HI 96743 USA. [Lada, Elizabeth A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Roman-Zuniga, Carlos G.] Ctr Astron Hispano Aleman, Granada 18008, Spain. RP Williams, JP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jpw@ifa.hawaii.edu RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Williams, Jonathan/0000-0001-5058-695X; Hora, Joseph/0000-0002-5599-4650 FU NSF [AST-0324328, AST-0607710]; National Aeronautics and Space Administration; National Science Foundation FX We thank Matthew Bate and Ian Bonnell for comments. 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 the National Aeronautics and Space Administration and the National Science Foundation, and the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 43 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1300 EP 1306 DI 10.1088/0004-637X/699/2/1300 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500039 ER PT J AU Dobler, G Draine, B Finkbeiner, DP AF Dobler, Gregory Draine, Bruce Finkbeiner, Douglas P. TI CONSTRAINING SPINNING DUST PARAMETERS WITH THE WMAP FIVE-YEAR DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; dust, extinction; ISM: clouds; radiation mechanisms: non-thermal; radio continuum: ISM ID MICROWAVE-ANISOTROPY-PROBE; INTERSTELLAR-MEDIUM EMISSION; FOREGROUND EMISSION; INFRARED-EMISSION; GALACTIC PLANE; RADIATION; SKY; POLARIZATION; GRAINS; RESOLUTION AB We characterize spinning dust emission in the warm ionized medium (WIM) by comparing templates of Galactic dust and H alpha with the five-year maps from the Wilkinson Microwave Anisotropy Probe (WMAP). The H alpha-correlated microwave emission deviates from the thermal bremsstrahlung (free-free) spectrum expected for ionized gas, exhibiting an additional broad bump peaked at similar to 40 GHz which provides similar to 20% of the peak intensity. We confirm that the bump is consistent with a modified Draine and Lazarian spinning dust model, though the peak frequency of the emission is somewhat lower than the 50 GHz previously claimed. This frequency shift results from systematic errors in the large-scale modes of the three-year WMAP data which have been corrected in the five-year data release. We show that the bump is not the result of errors in the H alpha template by analyzing regions of high free-free intensity, where the WMAP K-band map may be used as the free-free template. We rule out a pure free-free spectrum for the H alpha-correlated emission at high confidence: similar to 27 sigma for the nearly full-sky fit, even after marginalizing over the cosmic microwave background cross-correlation bias. We also extend the previous analysis by searching the parameter space of the Draine and Lazarian model but letting the amplitude float. The best fit for reasonable values of the characteristic electric dipole moment and density requires an amplitude factor of similar to 0.3. This suggests that small polycyclic aromatic hydrocarbons in the WIM are depleted by a factor of similar to 3. C1 [Dobler, Gregory; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Draine, Bruce] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Dobler, G (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM gdobler@cfa.harvard.edu OI Draine, Bruce/0000-0002-0846-936X NR 42 TC 31 Z9 31 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1374 EP 1388 DI 10.1088/0004-637X/699/2/1374 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500045 ER PT J AU Schuster, MT Marengo, M Hora, JL Fazio, GG Humphreys, RM Gehrz, RD Hinz, PM Kenworthy, MA Hoffmann, WF AF Schuster, M. T. Marengo, M. Hora, J. L. Fazio, G. G. Humphreys, R. M. Gehrz, R. D. Hinz, P. M. Kenworthy, M. A. Hoffmann, W. F. TI IMAGING THE COOL HYPERGIANT NML CYGNI'S DUSTY CIRCUMSTELLAR ENVELOPE WITH ADAPTIVE OPTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; open clusters and associations: individual (Cyg OB2); stars: imaging; stars: individual (NML Cyg); stars: mass loss ID VY-CANIS-MAJORIS; SPITZER-SPACE-TELESCOPE; LATE-TYPE STARS; 3-DIMENSIONAL MORPHOLOGY; INFRARED OBSERVATIONS; NEARBY GALAXIES; HIGH-RESOLUTION; LUMINOUS STARS; PROPER MOTIONS; ARRAY CAMERA AB We present subarcsecond angular resolution, high-Strehl ratio mid-IR adaptive optics images of the powerful OH/IR source and cool hypergiant NML Cyg at 8.8, 9.8, and 11.7 mu m. These images reveal once more the complexity in the dusty envelope surrounding this star. We spatially resolve the physical structures ( radius similar to 0 ''.14, similar to 240 AU adopting a distance of 1.74 kpc) responsible for NML Cyg's deep 10 mu m silicate dust absorption feature. We also detect an asymmetric excess, at separations of similar to 0 ''.3-0 ''.5 (similar to 520-870 AU), northwest from the star. The colors of this excess are consistent with thermal emission of hot, optically thin dust. This excess is oriented in the direction of the Cyg OB2 stellar association, and is likely due to the disruption of NML Cyg's dusty wind with the near-UV radiation flux from the massive hot stars within Cyg OB2. This interaction was predicted in our previous paper to explain the geometry of an inverted photodissociation region observed at optical wavelengths. C1 [Schuster, M. T.; Marengo, M.; Hora, J. L.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Humphreys, R. M.; Gehrz, R. D.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Hinz, P. M.; Kenworthy, M. A.; Hoffmann, W. F.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Schuster, MT (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mschuster@cfa.harvard.edu; mmarengo@cfa.harvard.edu OI Hora, Joseph/0000-0002-5599-4650 FU NASA [1215746, 1256406] FX We are pleased to acknowledge interesting conversations with David Boboltz regarding his VLA observations. NASA provided support for this work. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work is based in part on observations made with Spitzer, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for R. D. G. was provided by NASA through grants 1215746 and 1256406 issued by JPL-Caltech to the University of Minnesota. This work is based in part on observations made with the NASA/ESA HST, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 59 TC 9 Z9 9 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 JUL 10 PY 2009 VL 699 IS 2 BP 1423 EP 1432 DI 10.1088/0004-637X/699/2/1423 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500050 ER PT J AU Getman, KV Feigelson, ED Luhman, KL Sicilia-Aguilar, A Wang, JF Garmire, GP AF Getman, Konstantin V. Feigelson, Eric D. Luhman, Kevin L. Sicilia-Aguilar, Aurora Wang, Junfeng Garmire, Gordon P. TI PROTOPLANETARY DISK EVOLUTION AROUND THE TRIGGERED STAR-FORMING REGION CEPHEUS B SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Cepheus B cloud); open clusters and associations: individual (Cepheus OB3) planetary systems: protoplanetary disks; stars: formation; stars: pre-main sequence; X-rays: stars ID BRIGHT-RIMMED CLOUDS; SPITZER-SPACE-TELESCOPE; RADIATION-DRIVEN IMPLOSION; INFRARED ARRAY CAMERA; X-RAY-EMISSION; T-TAURI STARS; ORION ULTRADEEP PROJECT; INTERMEDIATE-MASS STARS; NEWTON EXTENDED SURVEY; YOUNG STELLAR OBJECTS AB The Cepheus B (Cep B) molecular cloud and a portion of the nearby Cep OB3b OB association, one of the most active regions of star formation within 1 kpc, have been observed with the Infrared Array Camera detector on board the Spitzer Space Telescope. The goals are to study protoplanetary disk evolution and processes of sequential triggered star formation in the region. Out of similar to 400 pre-main-sequence (PMS) stars selected with an earlier Chandra X-ray Observatory observation, similar to 95% are identified with mid-infrared sources and most of these are classified as diskless or disk-bearing stars. The discovery of the additional > 200 IR-excess low-mass members gives a combined Chandra+Spitzer PMS sample that is almost complete down to 0.5 M(circle dot) outside of the cloud, and somewhat above 1 M(circle dot) in the cloud. Analyses of the nearly disk-ubiased combined Chandra and Spitzer-selected stellar sample give several results. Our major finding is a spatio-temporal gradient of young stars from the hot molecular core toward the primary ionizing O star HD 217086. This strongly supports the radiation-driven implosion (RDI) model of triggered star formation in the region. The empirical estimate for the shock velocity of similar to 1 km s(-1) is very similar to theoretical models of RDI in shocked molecular clouds. The initial mass function (IMF) of the lightly obscured triggered population exhibits a standard Galactic field IMF shape. The unusually high apparent value of greater than or similar to 70% star formation efficiency inferred from the ratio of star mass to current molecular gas mass indicates that most of the Cep B molecular cloud has been already ablated or transformed to stars. Contrary to the current RDI simulations, our findings indicate that star formation triggering by H II region shocks is not restricted to a single episode but can continue for millions of years. Other results include: (1) agreement of the disk fractions, their mass dependency, and fractions of transition disks with other clusters; (2) confirmation of the youthfulness of the embedded Cep B cluster; (3) confirmation of the effect of suppression of time-integrated X-ray emission in disk-bearing versus diskless systems. C1 [Getman, Konstantin V.; Feigelson, Eric D.; Luhman, Kevin L.; Garmire, Gordon P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Feigelson, Eric D.; Luhman, Kevin L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Sicilia-Aguilar, Aurora] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wang, Junfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Getman, KV (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM gkosta@astro.psu.edu RI Wang, Junfeng/A-1476-2011 NR 83 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1454 EP 1472 DI 10.1088/0004-637X/699/2/1454 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500052 ER PT J AU Cohen, O Drake, JJ Kashyap, VL Gombosi, TI AF Cohen, O. Drake, J. J. Kashyap, V. L. Gombosi, T. I. TI THE EFFECT OF MAGNETIC SPOTS ON STELLAR WINDS AND ANGULAR MOMENTUM LOSS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: numerical; MHD; stars: coronae; stars: mass loss; stars: spots ID LOW-MASS STARS; SOLAR-WIND; POLAR SPOTS; AB-DORADUS; DIFFERENTIAL ROTATION; FIELDS; PROMINENCES; EVOLUTION; BRAKING; CORONA AB We simulate the effect of latitudinal variations in the location of star spots, as well as their magnetic field strength, on stellar angular momentum loss (AML) to the stellar wind. We use the Michigan solar corona global magnetohydrodynamic model, which incorporates realistic relation between the magnetic field topology and the wind distribution. We find that the spots' location significantly affects the stellar wind structure, and as a result, the total mass loss rate and AML rate. In particular, we find that the AML rate is controlled by the mass flux when spots are located at low latitudes but is controlled by an increased plasma density between the stellar surface and the Alfven surface when spots are located at high latitudes. Our results suggest that there might be a feedback mechanism between the magnetic field distribution, wind distribution, AML through the wind, and the motions at the convection zone that generate the magnetic field. This feedback might explain the role of coronal magnetic fields in stellar dynamos. C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU NSF-SHINE [ATM-0823592]; NASA-LWSTRT [NNG05GM44G]; NASA [NAS8-39073] FX We thank the anonymous referee for useful comments and suggestions. This work has been supported by NSF-SHINE ATM-0823592 grant, NASA-LWSTRT Grant NNG05GM44G. 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. J.J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) during the course of this research. NR 53 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1501 EP 1510 DI 10.1088/0004-637X/699/2/1501 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500056 ER PT J AU Lee, CF Hirano, N Palau, A Ho, PTP Bourke, TL Zhang, QZ Shang, H AF Lee, Chin-Fei Hirano, Naomi Palau, Aina Ho, Paul T. P. Bourke, Tyler L. Zhang, Qizhou Shang, Hsien TI ROTATION AND OUTFLOW MOTIONS IN THE VERY LOW-MASS CLASS 0 PROTOSTELLAR SYSTEM HH 211 AT SUBARCSECOND RESOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; ISM: individual (HH 211); ISM: jets and outflows ID YOUNG STELLAR OBJECTS; SIO LINE EMISSION; SUBMILLIMETER ARRAY; INTERSTELLAR JETS; MOLECULAR OUTFLOW; STAR-FORMATION; HIGH-VELOCITY; SHOCK-WAVES; CO OUTFLOWS; BROWN DWARF AB HH 211 is a nearby young protostellar system with a highly collimated jet. We have mapped it in 352 GHz continuum, SiO (J = 8 - 7), and HCO(+) (J = 4 - 3) emission at up to similar to 0 ''.2 resolution with the Submillimeter Array (SMA). The continuum source is now resolved into two sources, SMM1 and SMM2, with a separation of similar to 84 AU. SMM1 is seen at the center of the jet, probably tracing a (inner) dusty disk around the protostar driving the jet. SMM2 is seen to the southwest of SMM1 and may trace an envelope-disk around a small binary companion. A flattened envelope-disk is seen in HCO(+) around SMM1 with a radius of similar to 80 AU perpendicular to the jet axis. Its velocity structure is consistent with a rotation motion and can be fitted with a Keplerian law that yields a mass of similar to 50 +/- 15 M(Jup) (a mass of a brown dwarf) for the protostar. Thus, the protostar could be the lowest mass source known to have a collimated jet and a rotating flattened envelope-disk. A small-scale (similar to 200 AU) low-speed (similar to 2 km s(-1)) outflow is seen in HCO(+) around the jet axis extending from the envelope-disk. It seems to rotate in the same direction as the envelope-disk and may carry away part of the angular momentum from the envelope-disk. The jet is seen in SiO close to similar to 100 AU from SMM1. It is seen with a "C-shaped" bending. It has a transverse width of less than or similar to 40 AU and a velocity of similar to 170 +/- 60 km s(-1). A possible velocity gradient is seen consistently across its innermost pair of knots, similar to 0.5 km s(-1) at similar to 10 AU, consistent with the sense of rotation of the envelope-disk. If this gradient is an upper limit of the true rotational gradient of the jet, then the jet carries away a very small amount of angular momentum of less than or similar to 5 AU km s(-1) and thus must be launched from the very inner edge of the disk near the corotation radius. C1 [Lee, Chin-Fei; Hirano, Naomi; Ho, Paul T. P.; Shang, Hsien] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Palau, Aina] INTA CSIC, Ctr Astrobiol, Lab Astrofis Estelar & Exoplanets, E-28691 Villanueva De La Canada, Madrid, Spain. [Ho, Paul T. P.; Bourke, Tyler L.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 NR 48 TC 46 Z9 46 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1584 EP 1594 DI 10.1088/0004-637X/699/2/1584 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500065 ER PT J AU Ercolano, B Clarke, CJ Drake, JJ AF Ercolano, Barbara Clarke, Cathie J. Drake, Jeremy J. TI X-RAY IRRADIATED PROTOPLANETARY DISK ATMOSPHERES. II. PREDICTIONS FROM MODELS IN HYDROSTATIC EQUILIBRIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: stars; planetary systems: protoplanetary disks; stars: formation; stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; ORION ULTRADEEP PROJECT; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; ACCRETION DISKS; MASSIVE STARS; EXTREME-ULTRAVIOLET; FAR-ULTRAVIOLET; NEBULA CLUSTER; LINE EMISSION AB We present new models for the X-ray photoevaporation of circumstellar disks which suggest that the resulting mass loss (occurring mainly over the radial range 10-40 AU) may be the dominant dispersal mechanism for gas around low-mass pre-main-sequence stars, contrary to the conclusions of previous workers. Our models combine use of the MOCASSIN Monte Carlo radiative transfer code and a self-consistent solution of the hydrostatic structure of the irradiated disk. We estimate the resulting photoevaporation rates assuming sonic outflow at the surface where the gas temperature equals the local escape temperature and derive mass-loss rates of similar to 10(-9) M(circle dot) yr(-1), typically a factor of 2-10 times lower than the corresponding rates in our previous work where we did not adjust the density structure of the irradiated disk. The somewhat lower rates, and the fact that mass loss is concentrated toward slightly smaller radii, result from the puffing up of the heated disk at a few AU which partially screens the disk at tens of AU. Our mass-loss fluxes agree with those of Alexander et al. but we differ from Alexander et al. in our assessment of the overall significance of X-ray photoevaporation, given the large disk radii (and hence emitting area) associated with X-ray-driven winds. Gorti & Hollenbach, on the other hand, predict considerably lower mass-loss fluxes than either Alexander et al. or ourselves and we discuss possible reasons for this difference. We highlight the fact that X-ray photoevaporation has two generic advantages for disk dispersal compared with photoevaporation by extreme ultraviolet (EUV) photons that are only modestly beyond the Lyman limit: the demonstrably large X-ray fluxes of young stars even after they have lost their disks and the fact that X-rays are effective at penetrating much larger columns of material close to the star. We however stress that our X-ray-driven mass-loss rates are considerably more uncertain than the corresponding rates for EUV photoevaporation (around 10(-10) M(circle dot) yr(-1)) and that this situation will need to be remedied through future radiation hydrodynamical simulations. C1 [Ercolano, Barbara; Clarke, Cathie J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Drake, Jeremy J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ercolano, B (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. FU NASA [NAS8-39073] FX We thank Uma Gorti and David Hollenbach for useful discussion. We thank Al Glassgold for providing the data grids for their model. We thank John Raymond for helpful discussions and a critical assessment of this work. We also thank Paola D'Alessio for providing us with the electronic data for the gas density distribution in the disk. J.J.D. was supported by the Chandra X-ray Center NASA contract NAS8-39073 during the course of this research. This work was performed using the Darwin Supercomputer of the University of Cambridge High Performance Computing Service ( http://www.hpc.cam.ac.uk/), provided by Dell Inc., using Strategic Research Infrastructure Funding from the Higher Education Funding Council for England. NR 59 TC 92 Z9 92 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1639 EP 1649 DI 10.1088/0004-637X/699/2/1639 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500069 ER PT J AU Tchekhovskoy, A McKinney, JC Narayan, R AF Tchekhovskoy, Alexander McKinney, Jonathan C. Narayan, Ramesh TI EFFICIENCY OF MAGNETIC TO KINETIC ENERGY CONVERSION IN A MONOPOLE MAGNETOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; black hole physics; galaxies: jets; gamma rays: bursts; methods: analytical; methods: numerical; MHD; relativity; X-rays: bursts ID GAMMA-RAY BURSTS; RELATIVISTIC MAGNETOHYDRODYNAMIC FLOWS; ROTATING COMPACT OBJECTS; HOLE ACCRETION SYSTEMS; AFTERGLOW LIGHT CURVES; DOUBLE RADIO-SOURCES; STRIPED PULSAR WIND; FREE 2D EQUILIBRIUM; FORCE-FREE; CRAB-NEBULA AB Unconfined relativistic outflows from rotating, magnetized compact objects are often well modeled by assuming that the field geometry is approximately a split-monopole at large radii. Earlier work has indicated that such an unconfined flow has an inefficient conversion of magnetic energy to kinetic energy. This has led to the conclusion that ideal magnetohydrodynamical (MHD) processes fail to explain observations of, e. g., the Crab pulsar wind at large radii where energy conversion appears efficient. In addition, as a model for astrophysical jets, the monopole field geometry has been abandoned in favor of externally confined jets since the latter appeared to be generically more efficient jet accelerators. We perform time-dependent axisymmetric relativistic MHD simulations in order to find steady-state solutions for a wind from a compact object endowed with a monopole field geometry. Our simulations follow the outflow for 10 orders of magnitude in distance from the compact object, which is large enough to study both the initial "acceleration zone" of the magnetized wind as well as the asymptotic "coasting zone." We obtain the surprising result that acceleration is actually efficient in the polar region, which develops a jet despite not being confined by an external medium. Our models contain jets that have sufficient energy to account for moderately energetic long and short gamma-ray burst (GRB) events (similar to 10(51)-10(52) erg), collimate into narrow opening angles (opening half-angle theta(j) approximate to 0.03 rad), become matter-dominated at large radii (electromagnetic energy flux per unit matter energy flux sigma < 1), and move at ultrarelativistic Lorentz factors (gamma(j) similar to 200 for our fiducial model). The simulated jets have gamma(j)theta(j) similar to 5-15, so they are in principle capable of generating "achromatic jet breaks" in GRB afterglow light curves. By defining a "causality surface" beyond which the jet cannot communicate with a generalized "magnetic nozzle" near the axis of rotation, we obtain approximate analytical solutions for the Lorentz factor that fit the numerical solutions well. This allows us to extend our results to monopole wind models with arbitrary magnetization. Overall, our results demonstrate that the production of ultrarelativistic jets is a more robust process than previously thought. C1 [Tchekhovskoy, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McKinney, Jonathan C.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Tchekhovskoy, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. EM atchekho@cfa.harvard.edu; jmckinne@stanford.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 126 TC 81 Z9 81 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1789 EP 1808 DI 10.1088/0004-637X/699/2/1789 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500080 ER PT J AU Grady, CA Schneider, G Sitko, ML Williger, GM Hamaguchi, K Brittain, SD Ablordeppey, K Apai, D Beerman, L Carpenter, WJ Collins, KA Fukagawa, M Hammel, HB Henning, T Hines, D Kimes, R Lynch, DK Menard, F Pearson, R Russell, RW Silverstone, M Smith, PS Troutman, M Wilner, D Woodgate, B Clampin, M AF Grady, C. A. Schneider, G. Sitko, M. L. Williger, G. M. Hamaguchi, K. Brittain, S. D. Ablordeppey, K. Apai, D. Beerman, L. Carpenter, W. J. Collins, K. A. Fukagawa, M. Hammel, H. B. Henning, Th. Hines, D. Kimes, R. Lynch, D. K. Menard, F. Pearson, R. Russell, R. W. Silverstone, M. Smith, P. S. Troutman, M. Wilner, D. Woodgate, B. Clampin, M. TI REVEALING THE STRUCTURE OF A PRE-TRANSITIONAL DISK: THE CASE OF THE HERBIG F STAR SAO 206462 (HD 135344B) SO ASTROPHYSICAL JOURNAL LA English DT Review DE planetary systems: protoplanetary disks; stars: individual (SAO 206462) ID T-TAURI STARS; MAIN-SEQUENCE STARS; VEGA-LIKE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; INTERMEDIATE-MASS STARS; X-RAY-EMISSION; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; HIGH-RESOLUTION SPECTROSCOPY AB SAO 206462 (HD 135344B) has previously been identified as a Herbig F star with a circumstellar disk with a dip in its infrared excess near 10 mu m. In combination with a low accretion rate estimated from Br gamma, it may represent a gapped, but otherwise primordial or "pre-transitional" disk. We test this hypothesis with Hubble Space Telescope coronagraphic imagery, FUV spectroscopy and imagery and archival X-ray data, and spectral energy distribution (SED) modeling constrained by the observed system inclination, disk outer radius, and outer disk radial surface brightness (SB) profile using the Whitney Monte Carlo Radiative Transfer Code. The essentially face-on (i less than or similar to 20 degrees) disk is detected in scattered light from 0 ''.4 to 1 ''.15 (56-160 AU), with a steep (r(-9.6)) radial SB profile from 0.'' 6 to 0.'' 93. Fitting the SB data requires a concave upward or anti-flared outer disk, indicating substantial dust grain growth and settling by 8 +/- 4 Myr. The warm dust component is significantly variable in near to mid-IR excess and in temperature. At its warmest, it appears confined to a narrow belt from 0.08 to 0.2 AU. The steep SED for this dust component is consistent with grains with a <= 2.5 mu m. For cosmic carbon to silicate dust composition, conspicuous 10 mu m silicate emission would be expected and is not observed. This may indicate an elevated carbon to silicate ratio for the warm dust, which is not required to fit the outer disk. At its coolest, the warm dust can be fit with a disk from 0.14 to 0.31 AU, but with a higher inclination than either the outer disk or the gaseous disk, providing confirmation of the high inclination inferred from mid-IR interferometry. In tandem, the compositional and inclination difference between the warm dust and the outer dust disk suggests that the warm dust may be of second-generation origin, rather than a remnant of a primordial disk component. With its near face-on inclination, SAO 206462's disk is a prime location for planet searches. C1 [Grady, C. A.; Silverstone, M.] Eureka Sci, Oakland, CA 96002 USA. [Grady, C. A.; Woodgate, B.; Clampin, M.] NASA, Goddard Space Flight Ctr, ExoPlanets & Stellar Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, K.; Woodgate, B.] NASA, Goddard Space Flight Ctr, Goddard Ctr Astrobiol, Greenbelt, MD 20771 USA. [Schneider, G.; Apai, D.; Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sitko, M. L.; Hammel, H. B.; Hines, D.] Space Sci Inst, Boulder, CO 80301 USA. [Sitko, M. L.; Ablordeppey, K.; Beerman, L.; Carpenter, W. J.; Kimes, R.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Williger, G. M.; Collins, K. A.] Univ Louisville, Dept Phys, Louisville, KY 40292 USA. [Williger, G. M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Williger, G. M.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Hamaguchi, K.] NASA, Goddard Space Flight Ctr, CRESST, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Hamaguchi, K.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Brittain, S. D.; Troutman, M.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Fukagawa, M.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lynch, D. K.; Pearson, R.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Menard, F.] CNRS UJF, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grady, CA (reprint author), Eureka Sci, 2452 Delmer,Suite 100, Oakland, CA 96002 USA. RI Woodgate, Bruce/D-2970-2012; Clampin, mark/D-2738-2012; Brittain, Sean/K-9001-2012 OI Brittain, Sean/0000-0001-5638-1330 NR 126 TC 41 Z9 41 U1 1 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 JUL 10 PY 2009 VL 699 IS 2 BP 1822 EP 1842 DI 10.1088/0004-637X/699/2/1822 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500082 ER PT J AU Berger, E Soderberg, AM Chevalier, RA Fransson, C Foley, RJ Leonard, DC Debes, JH Diamond-Stanic, AM Dupree, AK Ivans, II Simmerer, J Thompson, IB Tremonti, CA AF Berger, E. Soderberg, A. M. Chevalier, R. A. Fransson, C. Foley, R. J. Leonard, D. C. Debes, J. H. Diamond-Stanic, A. M. Dupree, A. K. Ivans, I. I. Simmerer, J. Thompson, I. B. Tremonti, C. A. TI AN INTERMEDIATE LUMINOSITY TRANSIENT IN NGC 300: THE ERUPTION OF A DUST-ENSHROUDED MASSIVE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: evolution; stars: mass loss; stars: winds, outflows ID RED SUPERGIANT IRC+10420; ETA-CARINAE ANALOG; OPTICAL TRANSIENT; V838 MONOCEROTIS; II SUPERNOVAE; EMISSION; SPECTROSCOPY; EVOLUTION; RADIO; PROGENITOR AB We present multi-epoch high-resolution optical spectroscopy, UV/radio/X-ray imaging, and archival Hubble and Spitzer observations of an intermediate luminosity optical transient recently discovered in the nearby galaxy NGC 300. We find that the transient (NGC 300 OT2008-1) has a peak absolute magnitude of M(bol) approximate to -11.8 mag, intermediate between novae and supernovae, and similar to the recent events M85 OT2006-1 and SN 2008S. Our high-resolution spectra, the first for this event, are dominated by intermediate velocity (similar to 200-1000 km s(-1)) hydrogen Balmer lines and Ca II emission and absorption lines that point to a complex circumstellar environment, reminiscent of the yellow hypergiant IRC+10420. In particular, we detect asymmetric Ca II H&K absorption with a broad red wing extending to similar to 10(3) km s(-1), indicative of gas inflow at high velocity (possibly the wind of a massive binary companion). The low luminosity, intermediate velocities, and overall similarity to a known eruptive star indicate that the event did not result in a complete disruption of the progenitor. We identify the progenitor in archival Spitzer observations, with deep upper limits from Hubble data. The spectral energy distribution points to a dust-enshrouded star with a luminosity of about 6 x 10(4) L(circle dot), indicative of a similar to 10-20 M(circle dot) progenitor (or binary system). This conclusion is in good agreement with our interpretation of the outburst and circumstellar properties. The lack of significant extinction in the transient spectrum indicates that the dust surrounding the progenitor was cleared by the outburst. We thus predict that the progenitor should be eventually visible with Hubble if the transient event marks an evolutionary transition to a dust-free state, or with Spitzer if the event marks a cyclical process of dust formation. C1 [Berger, E.; Soderberg, A. M.; Foley, R. J.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Fransson, C.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Debes, J. H.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Diamond-Stanic, A. M.; Tremonti, C. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Ivans, I. I.; Thompson, I. B.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Simmerer, J.] Lund Observ, SE-22100 Lund, Sweden. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA; NSF [AST0807727] FX This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. We thank David Sand for obtaining the LDSS-3 spectrum on 2008 June 5, Bruce Draine for insightful discussions about the spectral properties of NGC 300 OT2008-1, Ranga Chary for assistance with the Spitzer data, and the referee for helpful comments which have improved the quality of the manuscript. A. M. S. acknowledges support by NASA through a Hubble Fellowship grant. R. A. C. acknowledges support from an NSF grant AST0807727. NR 35 TC 63 Z9 65 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 1850 EP 1865 DI 10.1088/0004-637X/699/2/1850 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500084 ER PT J AU Ruiter, AJ Belczynski, K Fryer, C AF Ruiter, Ashley J. Belczynski, Krzysztof Fryer, Chris TI RATES AND DELAY TIMES OF TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; supernovae: general ID MASS ACCUMULATION EFFICIENCY; GRAVITATIONAL-WAVE SOURCES; SINGLE-DEGENERATE MODEL; HELIUM SHELL FLASHES; DOUBLE WHITE-DWARFS; AM CVN SYSTEMS; POPULATION SYNTHESIS; COMMON-ENVELOPE; STAR-FORMATION; SPECTROSCOPIC BINARIES AB We analyze the evolution of binary stars to calculate synthetic rates and delay times of the most promising Type Ia Supernovae (SNe Ia) progenitors. We present and discuss evolutionary scenarios in which a white dwarf (WD) reaches the Chandrasekhar mass and potentially explodes in a SNe Ia. We consider Double Degenerate (DDS; merger of two WDs), Single Degenerate (SDS; WD accreting from H-rich companion), and AM Canum Venaticorum (AM CVn; WD accreting from He-rich companion) scenarios. The results are presented for two different star formation histories: burst (elliptical-like galaxies) and continuous (spiral-like galaxies). It is found that delay times for the DDS in our standard model (with common envelope efficiency alpha(CE) = 1) follow a power-law distribution. For the SDS we note a wide range of delay times, while AM CVn progenitors produce a short burst of SNe Ia at early times. The DDS median delay time falls between similar to 0.5 and 1 Gyr; the SDS between similar to 2 and 3 Gyr; and the AM CVn between similar to 0.8 and 0.6 Gyr depending on the assumed alpha(CE). For a Milky-Way-like (MW-like) galaxy, we estimate the rates of SNe Ia arising from different progenitors as: similar to 10(-4) yr(-1) for the SDS and AM CVn, and similar to 10(-3) yr(-1) for the DDS. We point out that only the rates for two merging carbon-oxygen WDs, the only systems found in the DDS, are consistent with the observed rates for typical MW-like spirals. We also note that DDS progenitors are the dominant population in elliptical galaxies. The fact that the delay time distribution for the DDS follows a power law implies more SNe Ia (per unit mass) in young rather than in aged populations. Our results do not exclude other scenarios, but strongly indicate that the DDS is the dominant channel generating SNe Ia in spiral galaxies, at least in the framework of our adopted evolutionary models. Since it is believed that WD mergers cannot produce a thermonuclear explosion given the current understanding of accreting WDs, either the evolutionary calculations along with accretion physics are incorrect, or the explosion calculations are inaccurate and need to be revisited. C1 [Ruiter, Ashley J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Ruiter, Ashley J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belczynski, Krzysztof; Fryer, Chris] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. RP Ruiter, AJ (reprint author), New Mexico State Univ, Dept Astron, 1320 Frenger Mall, Las Cruces, NM 88003 USA. EM aruiter@nmsu.edu; kbelczyn@nmsu.edu; clfreyer@lanl.gov NR 92 TC 154 Z9 154 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2009 VL 699 IS 2 BP 2026 EP 2036 DI 10.1088/0004-637X/699/2/2026 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 463AU UT WOS:000267401500098 ER PT J AU Pineda, JE Rosolowsky, EW Goodman, AA AF Pineda, Jaime E. Rosolowsky, Erik W. Goodman, Alyssa A. TI THE PERILS OF CLUMPFIND: THE MASS SPECTRUM OF SUBSTRUCTURES IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: clouds; ISM: individual (Perseus molecular complex); ISM: molecules; stars: formation ID STAR-FORMATION; SUBMILLIMETER CLUMPS; DENSE CORES; LARGE-SCALE; PERSEUS; DUST; EXTINCTION; EVOLUTION; CLUSTERS; ORION AB We study the mass spectrum of substructures in the Perseus Molecular Cloud Complex traced by (13)CO(1-0), finding that dN/dM proportional to M(-2.4) for the standard Clumpfind parameters. This result does not agree with the classical dN/dM proportional to M(-1.6). To understand this discrepancy, we study the robustness of the mass spectrum derived using the Clumpfind algorithm. Both two- and three-dimensional Clumpfind versions are tested, using 850 mu m dust emission and (13)CO spectral-line observations of Perseus, respectively. The effect of varying threshold is not important, but varying stepsize produces a different effect for two- and three-dimensional cases. In the two- dimensional case, where emission is relatively isolated (associated with only the densest peaks in the cloud), the mass spectrum variability is negligible compared to the mass function fit uncertainties. In the three-dimensional case, however, where the (13)CO emission traces the bulk of the molecular cloud (MC), the number of clumps and the derived mass spectrum are highly correlated with the stepsize used. The distinction between "two dimension" and "three dimension" here is more importantly also a distinction between "sparse" and "crowded" emission. In any "crowded" case, Clumpfind should not be used blindly to derive mass functions. Clumpfind's output in the "crowded" case can still offer a statistical description of emission useful in intercomparisons, but the clump-list should not be treated as a robust region decomposition suitable to generate a physically meaningful mass function. We conclude that the (13)CO mass spectrum depends on the observations resolution, due to the hierarchical structure of the MC. C1 [Pineda, Jaime E.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosolowsky, Erik W.] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada. RP Pineda, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jpineda@cfa.harvard.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 FU National Science Foundation [AF002, AST-9613615, AST0407172, AST0502605]; Association of Universities for Research in Astronomy, Inc.; Fundacion Andes [C-13442]; NSERC of Canada. FX We thank Jonathan B. Foster and Jens Kauffmann for helpful discussions. We thank the referee for useful comments that helped to improve the Letter. J. E. P. is supported by the National Science Foundation through grant AF002 from the Association of Universities for Research in Astronomy, Inc., under NSF cooperative agreement AST-9613615 and by Fundacion Andes under project C-13442. This material is based upon work supported by the National Science Foundation under grant AST0407172 to A. A. G. E. W. R.' s work is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST0502605) and a Discovery Grant from NSERC of Canada. NR 35 TC 67 Z9 67 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2009 VL 699 IS 2 BP L134 EP L138 DI 10.1088/0004-637X/699/2/L134 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 462RG UT WOS:000267372800017 ER PT J AU Wang, X Filippenko, AV Ganeshalingam, M Li, W Silverman, JM Wang, L Chornock, R Foley, RJ Gates, EL Macomber, B Serduke, FJD Steele, TN Wong, DS AF Wang, X. Filippenko, A. V. Ganeshalingam, M. Li, W. Silverman, J. M. Wang, L. Chornock, R. Foley, R. J. Gates, E. L. Macomber, B. Serduke, F. J. D. Steele, T. N. Wong, D. S. TI IMPROVED DISTANCES TO TYPE Ia SUPERNOVAE WITH TWO SPECTROSCOPIC SUBCLASSES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; distance scale; dust, extinction; supernovae: general ID INFRARED OBSERVATIONS; OPTICAL SPECTROSCOPY; DECLINE RATE; DUST; LUMINOSITY; SPECTRA; LIGHT; DIVERSITY; PARAMETER; CONSTANT AB We study the observables of 158 relatively normal Type Ia supernovae (SNe Ia) by dividing them into two groups in terms of the expansion velocity inferred from the absorption minimum of the Si II lambda 6355 line in their spectra near B-band maximum brightness. One group ("Normal") consists of normal SNe Ia populating a narrow strip in the Si II velocity distribution, with an average expansion velocity < v > = 10,600 +/- 400 km s(-1) near B maximum; the other group ("HV") consists of objects with higher velocities, v greater than or similar to 11,800 km s(-1). Compared with the Normal group, the HV one shows a narrower distribution in both the peak luminosity and the luminosity decline rate Delta m(15). In particular, their B-V colors at maximum brightness are found to be on average redder by similar to 0.1 mag, suggesting that they either are associated with dusty environments or have intrinsically red B-V colors. The HV SNe Ia are also found to prefer a lower extinction ratio R(V) approximate to 1.6 (versus similar to 2.4 for the Normal ones). Applying such an absorption-correction dichotomy to SNe Ia of these two groups remarkably reduces the dispersion in their peak luminosity from 0.178 mag to only 0.125 mag. C1 [Wang, X.; Filippenko, A. V.; Ganeshalingam, M.; Li, W.; Silverman, J. M.; Chornock, R.; Foley, R. J.; Macomber, B.; Serduke, F. J. D.; Steele, T. N.; Wong, D. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wang, X.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, X.] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Wang, L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gates, E. L.] Univ Calif Santa Cruz, Lick Observ, Mt Hamilton, CA 95140 USA. RP Wang, X (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wangxf@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015 FU NSF [AST-0607485, AST-0708873]; TABASGO Foundation; US Department of Energy [DE-FC0206ER41453, DE-FG0208ER41563]; National Natural Science Foundation of China [10673007]; China-973 Program [2009CB824800] FX We thank M. M. Phillips for allowing us to use the photometric parameters of SN2005A before publication, and D. C. Leonard for useful discussion, and the Lick Observatory staff for their assistance with the observations. C. V. Griffith, J. J. Kong, N. Lee, and E. Miller helped maintain and improve the SN Database of A. V. F.' s supernova group at UC Berkeley. We are grateful to many students, postdocs, and other collaborators who have contributed to observations and reductions of our SN spectra and images over the past two decades, especially C. Anderson, A. J. Barth, L.-B. Desroches, G. Foster, B. Grigsby, N. Joubert, D. C. Leonard, T. Matheson, M. Moore, M. Papenkova, S. Park, B. Swift, T. Pritchard, and D. Winslow. This group is supported by NSF grant AST-0607485, the TABASGO Foundation, US Department of Energy SciDACgrant DE-FC0206ER41453, and US Department of Energy grant DE-FG0208ER41563. We are also grateful to the National Natural Science Foundation of China (10673007), and the China-973 Program 2009CB824800. The work of L. Wang is supported by NSF grant AST-0708873 KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the HP Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. We 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. NR 50 TC 123 Z9 126 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2009 VL 699 IS 2 BP L139 EP L143 DI 10.1088/0004-637X/699/2/L139 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 462RG UT WOS:000267372800018 ER PT J AU Zhang, P Kharchenko, V Jamieson, MJ Dalgarno, A AF Zhang, P. Kharchenko, V. Jamieson, M. J. Dalgarno, A. TI Energy relaxation in collisions of hydrogen and deuterium with oxygen atoms SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORRELATED MOLECULAR CALCULATIONS; FAST NITROGEN-ATOMS; GAUSSIAN-BASIS SETS; VENUS; THERMALIZATION; ESCAPE; GASES; SCATTERING; ENTHALPY; MARS AB Collision energy transfer processes between hydrogen, deuterium, and oxygen atoms in the upper atmospheres of the terrestrial planets are studied. A new set of interaction potentials has been constructed using an accurate ab initio method. Full orientation-dependent scattering cross sections have been obtained quantum mechanically and have been incorporated into the construction of the linear Boltzmann kinetic equation describing the energy relaxation process. The isotope and temperature dependence of the energy relaxation parameters have been analyzed. Distributions of the secondary energetic recoil atoms have been computed and the fractions of hot atoms capable of escaping from the atmospheres of the terrestrial planets have been determined. For applications to atmospheric physics and astrophysics, we have computed effective hard sphere cross sections for O + H and O + D collisions that closely reproduce the energy relaxation kinetics obtained from the linear Boltzmann equation. These effective cross sections, which are functions of the laboratory frame collisional energy and the temperature of the bath gas, may be used in simulations of the thermalization of hot O, H, and D atoms and their escape from planets. C1 [Zhang, P.; Kharchenko, V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Jamieson, M. J.] Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. [Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT USA. RP Zhang, P (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St,Mail Stop 14, Cambridge, MA 02138 USA. EM pezhang@cfa.harvard.edu FU National Science Foundation [ATM-0430506]; NASA [NNX07AR03G, NNG06GD40G]; National Center for Atmospheric Research (NCAR) FX Wolfgang Baumjohann thanks James Duff and another reviewer for their assistance in evaluating this paper. NR 33 TC 12 Z9 12 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD JUL 9 PY 2009 VL 114 AR A07101 DI 10.1029/2009JA014055 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 469YJ UT WOS:000267937600006 ER PT J AU Anker, A Hurt, C Knowlton, N AF Anker, Arthur Hurt, Carla Knowlton, Nancy TI Description of cryptic taxa within the Alpheus bouvieri A. Milne-Edwards, 1878 and A. hebes Kim and Abele, 1988 species complexes (Crustacea: Decapoda: Alpheidae) SO ZOOTAXA LA English DT Article DE Alpheus; snapping shrimp; Alpheidae; eastern Pacific; western Atlantic; color pattern; transisthmian species; new species; extinction; Caribbean; molecular phylogeny; barcode; COI ID SHRIMP GENUS ALPHEUS; SNAPPING SHRIMP; CARIBBEAN SEA; CARIDEA; PACIFIC; MARINE; PANAMA; DIVERGENCE; ISTHMUS; DNA AB Alpheus bouvieri A. Milne-Edwards, 1878 and A. hebes Kim and Abele, 1988 are reviewed based on morphological and genetic data. Alpheus bouvieri, previously believed to be distributed in the eastern Pacific and Atlantic, is restricted to the Atlantic populations; the eastern Pacific populations (A. bouvieri sensu Kim and Abele 1988) are assigned to A. javieri n. sp. A second new species, A. agilis n. sp., closely related to the eastern Pacific A. hebes, is described based on recently collected specimens from the eastern Atlantic (Sao Tome, Cape Verde) and western Atlantic (Atol das Rocas off northeastern Brazil). The absence of A. agilis n. sp. (or any other representative of the A. hebes clade) in the Caribbean Sea is likely due to a relatively recent (similar to 1-2 my) extinction. Genetic data (COI sequences) indicates that A. bouvieri and A. javieri n. sp., and A. hebes and A. agilis n. sp. diverged approximately 6 and 7.5 mya, respectively, i.e., around 3 my before the final closure of the Isthmus of Panama. C1 [Anker, Arthur; Hurt, Carla; Knowlton, Nancy] Inst Smithsonian Invest Trop, Panama City, Panama. [Anker, Arthur; Hurt, Carla; Knowlton, Nancy] Smithsonian Trop Res Inst, Naos Unit 0948, APO, AA 34002 USA. [Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. RP Anker, A (reprint author), Univ Florida, Florida Museum Nat Hist, 250A Dickinson Hall, Gainesville, FL 32611 USA. EM aanker@flmnh.ufl.edu RI Hurt, Carla/A-3284-2011 FU John Dove Isaacs Professorship of Natural Philosophy; Scripps Institution of Oceanography, La Jolla, USA; Smithsonian Tropical Research Institute (STRI); Panama City, Panama; Census of Marine Life/CReefs Project FX This study was supported by the John Dove Isaacs Professorship of Natural Philosophy and the Scripps Institution of Oceanography, La Jolla, USA, and the Smithsonian Tropical Research Institute (STRI), Panama City, Panama, and is part of the Census of Marine Life/CReefs Project. We are grateful to the Autoridad National del Ambiente (ANAM) of the Republic of Panama, and the Direccao das Pescas of the Democratic Republic of Sao Tome for collection permits for material collected in Panama and Sao Tome in 2005-2007. Javier Jara, Eyda Gomez, Eva Toth (Naos, STRI), Jonathan Vera Caripe (Universidad de Oriente, Boca del Rio, Isla Margarita, Venezuela) and Ivan Marin (Laboratory of Ecology and Morphology of Marine Invertebrates, A. N. Severtzov Institute of Ecology and Evolution, RAS, Moscow, Russia) assisted in the field. Additional specimens were collected by Dominique Roche (STRI and McGill University, Montreal, Canada), Thomas Lamy (STRI and Ecole Nationale Superieure, Paris, France) and Nuno Simoes (UMDI-Sisal, Facultad de Ciencias, UNAM, Sisal, Mexico). Paulo Young (late of MNRJ) arranged the loan of Atol das Rocas specimens. NR 100 TC 11 Z9 14 U1 4 U2 4 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 JUL 9 PY 2009 IS 2153 BP 1 EP 23 PG 23 WC Zoology SC Zoology GA 468FV UT WOS:000267803300001 ER PT J AU Ranere, AJ Piperno, DR AF Ranere, Anthony J. Piperno, Dolores R. TI Reply to Perttula: Identifying an early Holocene projectile point type from central Mexico SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [Ranere, Anthony J.] Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. [Piperno, Dolores R.] Smithsonian Natl Museum Nat Hist, Archaeobiol Program, Dept Anthropol, Washington, DC 20560 USA. [Piperno, Dolores R.] Smithsonian Trop Res Inst, Balboa, Panama. RP Ranere, AJ (reprint author), Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. EM ranere@temple.edu NR 4 TC 0 Z9 0 U1 1 U2 1 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 JUL 7 PY 2009 VL 106 IS 27 BP E74 EP E74 DI 10.1073/pnas.0905971106 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 468DX UT WOS:000267796100106 ER PT J AU Ryder, TB Parker, PG Blake, JG Loiselle, BA AF Ryder, Thomas B. Parker, Patricia G. Blake, John G. Loiselle, Bette A. TI It takes two to tango: reproductive skew and social correlates of male mating success in a lek-breeding bird SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE coordinated display; manakins; Pipra filicauda; reproductive skew; social networks ID MICROSATELLITE DNA MARKERS; ANIMAL SOCIETIES; COMPLEX NETWORKS; EASTERN ECUADOR; TAILED MANAKIN; LEKKING BIRD; MATE CHOICE; PATERNITY; ORGANIZATION; SELECTION AB Variance in reproductive success among individuals is a defining characteristic of many social vertebrates. Yet, our understanding of which male attributes contribute to reproductive success is still fragmentary in most cases. Male-male reproductive coalitions, where males jointly display to attract females, are of particular interest to evolutionary biologists because one male appears to forego reproduction to assist the social partner. By examining the relationship between social behaviour and reproductive success, we can elucidate the proximate function of coalitions in the context of mate choice. Here, we use data from a 4-year study of wire-tailed manakins (Pipra filicauda) to provide molecular estimates of reproductive skew and to test the hypothesis that male-male social interactions, in the context of coordinated displays, positively influence a male's reproductive success. More specifically, we quantify male-male social interactions using network metrics and predict that greater connectivity will result in higher relative reproductive success. Our data show that four out of six leks studied had significant reproductive skew, with success apportioned to very few individuals in each lek. Metrics of male social affiliations derived from our network analysis, especially male connectivity, measured as the number of males with whom the focal male has extended interactions, were strong predictors of the number of offspring sired. Thus, network connectivity is associated with male fitness in wire-tailed manakins. This pattern may be the result of shared cues used by both sexes to assess male quality, or the result of strict female choice for coordinated display behaviour. C1 [Ryder, Thomas B.; Parker, Patricia G.; Blake, John G.; Loiselle, Bette A.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Ryder, Thomas B.; Parker, Patricia G.; Blake, John G.; Loiselle, Bette A.] Univ Missouri, Whitney R Harris World Ecol Ctr, St Louis, MO 63121 USA. RP Ryder, TB (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,POB 37012,MRC 5503, Washington, DC 20013 USA. EM rydert@si.edu RI Loiselle, Bette/O-7106-2016 OI Loiselle, Bette/0000-0003-1434-4173 FU International Center for Tropical Ecology; Association of Field Ornithologists' Alexander Bergstrom Award; National Geographic Society [7113-01]; National Science Foundation [IBN 0235141, IOB 0508189] FX Funding was provided by the International Center for Tropical Ecology, the Association of Field Ornithologists' Alexander Bergstrom Award, National Geographic Society (7113-01) and National Science Foundation (IBN 0235141, IOB 0508189). NR 55 TC 32 Z9 32 U1 4 U2 29 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 JUL 7 PY 2009 VL 276 IS 1666 BP 2377 EP 2384 DI 10.1098/rspb.2009.0208 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 458CK UT WOS:000266990700007 PM 19324732 ER PT J AU Van Bael, SA Fernandez-Marin, H Valencia, MC Rojas, EI Wcislo, WT Herre, EA AF Van Bael, Sunshine A. Fernandez-Marin, Hermogenes Valencia, Mariana C. Rojas, Enith I. Wcislo, William T. Herre, Edward A. TI Two fungal symbioses collide: endophytic fungi are not welcome in leaf-cutting ant gardens SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Atta colombica; endophyte; Glomerella cingulata; inhibition; microbial interactions; microfungi ID GROWING ANTS; PATHOGENS; EVOLUTION; INFECTION; PLANTS; AGRICULTURE; HYMENOPTERA; FORMICIDAE; PREFERENCE; PARASITISM AB Interactions among the component members of different symbioses are not well studied. For example, leaf-cutting ants maintain an obligate symbiosis with their fungal garden, while the leaf material they provide to their garden is usually filled with endophytic fungi. The ants and their cultivar may interact with hundreds of endophytic fungal species, yet little is known about these interactions. Experimental manipulations showed that (i) ants spend more time cutting leaves from a tropical vine, Merremia umbellata, with high versus low endophyte densities, (ii) ants reduce the amount of endophytic fungi in leaves before planting them in their gardens, (iii) the ants' fungal cultivar inhibits the growth of most endophytes tested. Moreover, the inhibition by the ants' cultivar was relatively greater for more rapidly growing endophyte strains that could potentially out-compete or overtake the garden. Our results suggest that endophytes are not welcome in the garden, and that the ants and their cultivar combine ant hygiene behaviour with fungal inhibition to reduce endophyte activity in the nest. C1 [Van Bael, Sunshine A.; Fernandez-Marin, Hermogenes; Valencia, Mariana C.; Rojas, Enith I.; Wcislo, William T.; Herre, Edward A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Fernandez-Marin, Hermogenes] Univ Copenhagen, Dept Biol, Inst Biol, DK-2100 Copenhagen, Denmark. RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM vanbaels@si.edu FU NSF IRFP award [OISE-0401957]; American Association of University Women post-doctoral fellowship; World Cacao Foundation FX We thank G. Gilbert, P. Hebbar, M. Seid, L. Ramirez, Z. Maynard and L. Mejia for their advice, comments and help with endophyte collections; for help in the greenhouse and field, we thank E. Gomez, A. Portugal, B. Perez and L. Sosa. This research was funded by an NSF IRFP award (no. OISE-0401957) to S.A.V., an American Association of University Women post-doctoral fellowship to S.A.V, Smithsonian postdoctoral fellowships to S.A.V. and H.F.M. and a grant from the World Cacao Foundation to E.A.H. We thank the ANAM of Panama for permission to do research. NR 47 TC 35 Z9 36 U1 2 U2 21 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD JUL 7 PY 2009 VL 276 IS 1666 BP 2419 EP 2426 DI 10.1098/rspb.2009.0196 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 458CK UT WOS:000266990700012 PM 19364739 ER PT J AU Breedy, O Guzman, HM Vargas, S AF Breedy, Odalisca Guzman, Hector M. Vargas, Sergio TI A revision of the genus Eugorgia Verrill, 1868 (Coelenterata: Octocorallia: Gorgoniidae) SO ZOOTAXA LA English DT Article DE Cnidaria; Coelenterata; octocorals; eastern Pacific; Mexico; Costa Rica; Panama; Ecuador; Eugorgia; phylogenetic analysis ID EASTERN PACIFIC AB The species of the gorgoniid genus Eugorgia that occur along the eastern Pacific are taxonomically revised based on original type material of all species described until now, and reference specimens from recent surveys and expeditions. The genus Eugorgia is characterised by having a dominance of double disc sclerites in the coenenchyme which separate this taxon from the other gorgonians with similar external morphology such as Leptogorgia. In this revision, 12 species are recognized as valid and one is synonymised, E. forreri. Lectotypes were assigned for two species in order to establish their taxonomic status, and three varieties were established as species, E. alba, E. excelsa and E. purpurascens. All the species are described and illustrated. Based on the morphology of colonies and sclerites and supported by a phylogenetic analysis, we recognised three species groups within the genus Eugorgia: the "ampla-group" consisting of eight species, with slightly raised polyp-mounds and dichotomous branching or irregular variations of it; the "daniana group", consisting of three species, with prominent polyp-mounds and pinnate-like branching; and the "rubens-group" consisting of a single species, E. rubens, which is closely related to species within the second group. The fauna herein reported does not represent the diversity or geographical range of the species because more surveys are needed and more material stored in museums needs attention to complete the regional assessment. C1 [Breedy, Odalisca; Vargas, Sergio] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca; Vargas, Sergio] Univ Costa Rica, Escuela Biol, Museo Zool, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, MRC 0580 08, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. EM odalisca.breedy@ucr.ac.cr RI Vargas, Sergio/A-5678-2011 OI Vargas, Sergio/0000-0001-8704-1339 NR 45 TC 14 Z9 14 U1 0 U2 4 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 JUL 7 PY 2009 IS 2151 BP 1 EP 46 PG 46 WC Zoology SC Zoology GA 468FS UT WOS:000267802900001 ER PT J AU Taori, K Liu, YX Paul, VJ Luesch, H AF Taori, Kanchan Liu, Yanxia Paul, Valerie J. Luesch, Hendrik TI Combinatorial Strategies by Marine Cyanobacteria: Symplostatin 4, an Antimitotic Natural Dolastatin 10/15 Hybrid that Synergizes with the Coproduced HDAC Inhibitor Largazole SO CHEMBIOCHEM LA English DT Article DE dolastatins; marine cyanobacteria; natural products; structure elucidation; structure-activity relationships ID HISTONE DEACETYLASE INHIBITOR; ANTINEOPLASTIC AGENTS; SYMPLOCA-HYDNOIDES; ANTICANCER DRUGS; CANCER-CELLS; ANALOG; PEPTIDES; PRODUCTS; TUBULIN; CYTOTOXICITY C1 [Taori, Kanchan; Liu, Yanxia; Luesch, Hendrik] Univ Florida, Dept Med Chem, 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, 1600 SW Archer Rd, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU NOAA [NA060AR4170014]; University of Florida College of Pharmacy; NSF FX Financial support was provided by the Florida Sea Grant College Program with support from NOAA, Office of Sea Grant, U.S. Deportment of Commerce (Grant No. NA060AR4170014) and the University of Florida College of Pharmacy. We acknowledge NSF for funding through the External User Program of the National High Magnetic Field Laboratory (NHMFL), which supported our NMR studies at the Advanced Magnetic Resonance Imaging and Spectroscopy (AMRIS) facility in the McKnight Brain Institute of the University of Florida (UF). The 600 MHz I mm triple-resononce HTS cryogenic probe was developed through collaboration between UF NHMFL, and Bruker Biospin. We thank M. Becerro for extracting the cyanobacterium, J. Rocco for assistance in NMR data acquisition, S. McClellan for flow cytometry, Dr. J. Johnson for the MSIMS analysis and Professors W. H. Gerwick and R. G. Linington for providing NMR spectra of gallinamide A in CDCi3. This is contribution 779 from the Smithsonian Marine Station at Fort Pierce. NR 36 TC 32 Z9 33 U1 3 U2 26 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1439-4227 J9 CHEMBIOCHEM JI ChemBioChem PD JUL 6 PY 2009 VL 10 IS 10 BP 1634 EP 1639 DI 10.1002/cbic.200900192 PG 6 WC Biochemistry & Molecular Biology; Chemistry, Medicinal SC Biochemistry & Molecular Biology; Pharmacology & Pharmacy GA 469JI UT WOS:000267893200010 PM 19514039 ER PT J AU Carroll, SM Mantry, S Ramsey-Musolf, MJ Stubbs, CW AF Carroll, Sean M. Mantry, Sonny Ramsey-Musolf, Michael J. Stubbs, Christoper W. TI Dark-Matter-Induced Violation of the Weak Equivalence Principle SO PHYSICAL REVIEW LETTERS LA English DT Article AB A long-range fifth force coupled to dark matter can induce a coupling to ordinary matter if the dark matter interacts with standard model fields. We consider constraints on such a scenario from both astrophysical observations and laboratory experiments. We also examine the case where the dark matter is a weakly interacting massive particle, and derive relations between the coupling to dark matter and the coupling to ordinary matter for different models. Currently, this scenario is most tightly constrained by galactic dynamics, but improvements in Eoumltvoumls experiments can probe unconstrained regions of parameter space. C1 [Carroll, Sean M.; Mantry, Sonny; Ramsey-Musolf, Michael J.] CALTECH, Pasadena, CA 91125 USA. [Ramsey-Musolf, Michael J.] Univ Wisconsin, Madison, WI 53706 USA. [Stubbs, Christoper W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Carroll, SM (reprint author), CALTECH, Pasadena, CA 91125 USA. RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 FU Department of Energy [DE-FG03-92-ER40701, DE-FG0208ER41531]; Wisconsin Alumni Research Foundation; Gordon and Betty Moore Foundation FX We thank J. Distler, M. Kamionkowski, T. Tait, M. Wise, and K. Zurek for helpful conversations. This research was supported in part by Department of Energy Contracts No. DE-FG03-92-ER40701 and No. DE-FG0208ER41531, the Wisconsin Alumni Research Foundation, and the Gordon and Betty Moore Foundation. NR 26 TC 14 Z9 14 U1 0 U2 0 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 JUL 3 PY 2009 VL 103 IS 1 AR 011301 DI 10.1103/PhysRevLett.103.011301 PG 4 WC Physics, Multidisciplinary SC Physics GA 466XH UT WOS:000267697900011 PM 19659134 ER PT J AU Hardy, CR Sloat, LL Faden, RB AF Hardy, Christopher R. Sloat, Lindsey L. Faden, Robert B. TI FLORAL ORGANOGENESIS AND THE DEVELOPMENTAL BASIS FOR POLLINATOR DECEPTION IN THE ASIATIC DAYFLOWER, COMMELINA COMMUNIS (COMMELINACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Commelina; Commelinaceae; congenital fusion of sepals; dayflower; floral development; floral monosymmetry; pollinator deception; staminode development; staminodization; TCP gene family ID FLOWER SYMMETRY; GAMETOPHYTES; VASCULATURE; EVOLUTION AB The upper half of flowers in Commelina communis deceptively lures potential pollinators with its showy petals and staminodes on the false promise of abundant pollen. This paper presents evidence that staminodization in the upper half is associated with a severe retardation of the entire upper floral hemisphere early in development. Possible consequences of this developmental retardation are seen also in the gynoecium, where the upper carpel of the three-carpel late ovary is underdeveloped and sterile at maturity. Only late in development do the upper petals and staminodes expand and acquire pigments necessary for their attractive function. We surmise that retardations of this severity are unlikely to be found for functionally fertile organs such as stamens and ovule-producing carpels, because key preparatory events preceding sporogenesis might otherwise be disrupted. Such differential growth about the floral apex resembles that known in some eudicots to be regulated by the TCP gene family;, thus, future molecular developmental studies in Commelina may help to extend our understanding of the evolutionary genetics of floral monosymmetry to monocots. C1 [Hardy, Christopher R.; Sloat, Lindsey L.] Millersville Univ Pennsylvania, Dept Biol, James C Pk Herbarium, Millersville, PA 17551 USA. [Hardy, Christopher R.; Faden, Robert B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Hardy, CR (reprint author), Millersville Univ Pennsylvania, Dept Biol, James C Pk Herbarium, POB 1002, Millersville, PA 17551 USA. EM christopher.hardy@millersville.edu NR 25 TC 6 Z9 8 U1 2 U2 7 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JUL PY 2009 VL 96 IS 7 BP 1236 EP 1244 DI 10.3732/ajb.0800344 PG 9 WC Plant Sciences SC Plant Sciences GA 469BT UT WOS:000267870800003 PM 21628272 ER PT J AU Gomez-Navarro, C Jaramillo, C Herrera, F Wing, SL Callejas, R AF Gomez-Navarro, Carolina Jaramillo, Carlos Herrera, Fabiany Wing, Scott L. Callejas, Ricardo TI PALMS (ARECACEAE) FROM A PALEOCENE RAINFOREST OF NORTHERN COLOMBIA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Arecaceae; Arecoideae; Attaleinae; Cerrejon; Cocos; Colombia; neotropics; Nypa; Paleocene ID MONOCOT RELATIONSHIPS; TERTIARY SEDIMENTS; CERREJON FORMATION; COCOS-NUCIFERA; NEW-ZEALAND; FOSSIL; CLASSIFICATION; RECORDS; PALYNOLOGY; PHYLOGENY AB Palms are a monophyletic group with a dominantly tropical distribution; however, their fossil record in low latitudes is strikingly scarce. In this paper, we describe fossil leaves, inflorescences, and fruits of palms from the middle to late Paleocene Cerrejon Formation, outcropping in the Rancheria River Valley, northern Colombia. The fossils demonstrate the presence of at least five palm morphospecies in the basin ca. 60 Ma. We compare the morphology of the fossils with extant palms and conclude that they belong to at least three palm lineages: the pantropical Cocoseae of the subfamily Arecoideae, the monotypic genus Nypa, and either Calamoideae or Coryphoideae. The fossil fruits and inflorescences are among the oldest megafossil records of these groups and demonstrate that the divergence of the Cocoseae was more than 60 Ma, earlier than has previously been thought. These fossils are useful in tracing the range expansion or contraction of historical or current neotropical elements and also have profound implications for the understanding of the evolution of neotropical rainforests. C1 [Gomez-Navarro, Carolina; Jaramillo, Carlos; Herrera, Fabiany] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. [Gomez-Navarro, Carolina] Univ Calif Berkeley, Dept Plant & Microbial Biol, Berkeley, CA 94720 USA. [Herrera, Fabiany] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Wing, Scott L.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Callejas, Ricardo] Univ Antioquia, Inst Biol, Medellin 1226, Colombia. RP Jaramillo, C (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM jaramilloc@si.edu OI Wing, Scott/0000-0002-2954-8905 NR 62 TC 30 Z9 34 U1 0 U2 3 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD JUL PY 2009 VL 96 IS 7 BP 1300 EP 1312 DI 10.3732/ajb.0800378 PG 13 WC Plant Sciences SC Plant Sciences GA 469BT UT WOS:000267870800010 PM 21628279 ER PT J AU Hinde, K AF Hinde, Katherine TI Richer Milk for Sons but More Milk for Daughters: Sex-Biased Investment during Lactation Varies with Maternal Life History in Rhesus Macaques SO AMERICAN JOURNAL OF HUMAN BIOLOGY LA English DT Review ID LOCAL RESOURCE COMPETITION; FATTY-ACID-COMPOSITION; MACACA-MULATTA; SUCKLING BEHAVIOR; NIPPLE PREFERENCE; FACULTATIVE ADJUSTMENT; REPRODUCTIVE SUCCESS; INTERBIRTH INTERVALS; CALLITHRIX-JACCHUS; JAPANESE MACAQUES AB Lactation represents the greatest postnatal energetic expenditure for human and non-human primate females, and the ability to sustain the costs of lactation is influenced by a mother's physical condition. This is especially true for young mothers that initiate reproduction shortly after adolescence. These mothers have fewer bodily reserves available for lactation and face tradeoffs between reproduction and their own growth. Milk synthesis among captive rhesus macaques (Macaca mulatta) was investigated at the California National Primate Research Center from 2005 to 2007 (N = 114). Rhesus macaques produced low energy density milk typical of the primate order, but there was substantial individual variation among mothers in both milk energy density and yield. As a consequence, the available milk energy (AME), the product of milk energy density and milk yield, to support infant growth, development, and activity, varied tenfold among mothers. Primiparous mothers (N = 40) had fewer bodily resources, as measured by mass and body mass index, available for lactation than did multiparous mothers (N = 74) and showed poorer lactational performance. Mothers of sons produced milk of higher energy density, especially primiparous mothers, but lower milk yield, such that AME was the same for sons and daughters. Although AME from the mother was the same for sons and daughters, there was significant sexual dimorphism in infant mass. These data indicate that selection has likely favored sex-specific regulation of growth and development that is not necessarily contingent on greater maternal investment. Am. J. Hum. Biol. 21:512-519, 2009. (C) 2009 Wiley-Liss, Inc. C1 [Hinde, Katherine] UC Santa Barbara, Dept Anthropol, Santa Barbara, CA 93106 USA. [Hinde, Katherine] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Hinde, Katherine] Calif Natl Primate Res Ctr, Davis, CA USA. RP Hinde, K (reprint author), UC Santa Barbara, Dept Anthropol, Santa Barbara, CA 93106 USA. EM kjhinde@anth.ucsb.edu OI Hinde, Katie/0000-0002-0528-866X FU NCRR NIH HHS [RR019970, RR000169]; NIDDK NIH HHS [DK77639] NR 102 TC 53 Z9 54 U1 3 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1042-0533 EI 1520-6300 J9 AM J HUM BIOL JI Am. J. Hum. Biol. PD JUL-AUG PY 2009 VL 21 IS 4 SI SI BP 512 EP 519 DI 10.1002/ajhb.20917 PG 8 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA 460QR UT WOS:000267202700012 PM 19384860 ER PT J AU Loaiza, J Scott, M Bermingham, E Rovira, J Sanjur, O Conn, JE AF Loaiza, Jose Scott, Marilyn Bermingham, Eldredge Rovira, Jose Sanjur, Oris Conn, Jan E. TI Short Report: Anopheles darlingi (Diptera: Culicidae) in Panama SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Article ID MALARIA VECTOR; POPULATION-GROWTH; SOUTH-AMERICA; DNA; NEUTRALITY; TESTS AB We report Anopheles darlingi in Darien Province in eastern Panama. Polymerase chain reaction-restriction fragment length polymorphism profiles of the single copy nuclear white gene and sequence comparisons confirmed the presence of 66 specimens of the northern lineage of An. darlingi. The parsimony network depicted 5 CO1 haplotypes in 40 specimens of An. darlingi, which connected through 7-8 mutational steps with sequences from Central and South America. Furthermore, the presence of haplotypes in Biroquera, Darien Province identical to those previously published from northern Colombia suggests that Panamanian samples originated in Colombia. Results of neutrality tests (R(2) and Fu's F(s)) were not significant and the mismatch distribution was multimodal and did not fit the model of sudden population growth. These findings may indicate a long and stable presence of An. darlingi in eastern Panama. C1 [Conn, Jan E.] New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY 12159 USA. [Loaiza, Jose] McGill Univ, Dept Nat Resource Sci, Quebec City, PQ H9X 3V9, Canada. [Scott, Marilyn] McGill Univ, Inst Parasitol, Quebec City, PQ H9X 3V9, Canada. [Bermingham, Eldredge; Sanjur, Oris] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Rovira, Jose] Inst Conmemorat Gorgas Estudios Salud, Panama City, Panama. RP Conn, JE (reprint author), New York State Dept Hlth, Wadsworth Ctr, Griffin Lab, Slingerlands, NY 12159 USA. EM jose.loaiza@mail.mcgill.ca; marilyn.scott@mcgill.ca; bermingham@si.edu; jconn@wadsworth.org OI Conn, Jan/0000-0002-5301-7020 FU Secretariat for Science, Technology and Innovation of Panama [COL08-066]; Smithsonian Tropical Research Institute; Institute of Parasitology of McGill University; National Institutes of Health [AI R0154139] FX This study was supported by the Secretariat for Science, Technology and Innovation of Panama through research grant COL08-066 to Jose Loaiza, the Smithsonian Tropical Research Institute, the Institute of Parasitology of McGill University through its Centre for Host-Parasite Interactions travel fellowship awards program, and National Institutes of Health grant AI R0154139 to Jan E. Conn. NR 24 TC 14 Z9 14 U1 0 U2 1 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD JUL PY 2009 VL 81 IS 1 BP 23 EP 26 PG 4 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA 464SI UT WOS:000267526500006 PM 19556561 ER PT J AU Mercer, EP Miller, JM Calvet, N Hartmann, L Hernandez, J Sicilia-Aguilar, A Gutermuth, R AF Mercer, E. P. Miller, J. M. Calvet, N. Hartmann, L. Hernandez, J. Sicilia-Aguilar, A. Gutermuth, R. TI CHANDRA AND SPITZER OBSERVATIONS REVEAL NEW YSOs IN THE HEART OF TRUMPLER 37 SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations: individual (Trumpler 37); stars: formation; stars: pre-main sequence; X-rays: stars ID T-TAURI STARS; X-RAY-EMISSION; ORION ULTRADEEP PROJECT; INTERMEDIATE-MASS STARS; NEWTON EXTENDED SURVEY; YOUNG STELLAR OBJECTS; MOLECULAR CLOUD; SPACE-TELESCOPE; HYDRAE ASSOCIATION; NEBULA CLUSTER AB We have discovered 22 new low-mass members in the center of the 4 Myr old open cluster Trumpler 37 (Tr 37) using archival Chandra and Spitzer data. Our use of the Chandra ACIS data and an improved reduction of Spitzer Infrared Array Camera data of the central region in Tr 37 led to the discovery of three new disk-bearing members, 19 new diskless members, and potentially 10 more infrared excess sources. Combining these new members with previous known members, we measured a disk frequency of similar to 39%, which is lower than the previously reported disk frequency of similar to 48%. Most of the new members are diskless stars that lie within 0.65 pc of the central massive O6.5V star HD 206267. The proximity of these sources to HD 206267 suggests photoevaporation may be accelerating disk evolution in the center of Tr 37. The new members have solar-type masses ranging from similar to 0.6 M(circle dot) to 1.8 M(circle dot), spectral types ranging from late to early K, and X-ray luminosities in the range 29.3 erg s(-1) <= log L(X) <= 31.9 erg s(-1). The median X-ray luminosity (L(X) similar to 3 x 10(30) erg s(-1)) of the new members in this intermediate-aged cluster is on the same level as younger (1-3 Myr) and slightly older (5 Myr) populations in the same mass range, which suggests the age activity relation for pre-main-sequence solar-mass stars is constant up to similar to 5 Myr and decays sometime thereafter. C1 [Mercer, E. P.; Miller, J. M.; Calvet, N.; Hartmann, L.; Hernandez, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hernandez, J.] Ctr Invest Astron CIDA, Merida 5101A, Venezuela. [Sicilia-Aguilar, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Gutermuth, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mercer, EP (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. FU National Aeronautics and Space Administration; National Science Foundation FX 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 60 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 7 EP 18 DI 10.1088/0004-6256/138/1/7 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300002 ER PT J AU DeRose, KL Bourke, TL Gutermuth, RA Wolk, SJ Megeath, ST Alves, J Nurnberger, D AF DeRose, K. L. Bourke, T. L. Gutermuth, R. A. Wolk, S. J. Megeath, S. T. Alves, J. Nuernberger, D. TI A VERY LARGE TELESCOPE/NACO STUDY OF STAR FORMATION IN THE MASSIVE EMBEDDED CLUSTER RCW 38 SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; ISM: individual (RCW 38); stars: formation ID H-II REGIONS; RECOMBINATION LINE EMISSION; ORION NEBULA; CIRCUMSTELLAR DISKS; X-RAY; TRAPEZIUM CLUSTER; MOLECULAR CLOUDS; FORMING REGIONS; STELLAR GROUPS; O-STARS AB We present the results of high angular resolution adaptive optics (AO) near-infrared (JHK(s)) observations of the deeply embedded massive cluster RCW 38 using NACO on the Very Large Telescope. Narrowband AO observations centered at wavelengths of 1.28 mu m, 2.12 mu m, and 2.17 mu m were also obtained. The area covered by these observations is about 0.5 pc(2), centered on the O-star RCW 38 IRS 2. We use the JHK(s) colors to identify young stars with infrared (IR) excess in this region. Through a detailed comparison to a nearby control field, we find that most of the 337 stars detected in all three IR bands are cluster members (similar to 317), with essentially no contamination due to background (likely due to the high cluster extinction of A(V) similar to 15) or foreground sources. Five sources with three band detections have colors suggestive of deeply embedded protostars, while 53 sources are detected at K(s) only; their spatial distribution with respect to the extinction suggests they are highly reddened cluster members but their evolutionary status is unclear. Detectable K(s)-band excess is found toward 29% +/- 3% of the stars. For comparison to a similar area of Orion Nebula Cluster observed in the near-IR, mass and extinction cuts are applied, and the excess fractions redetermined. The resulting excesses are then 25% +/- 5% for RCW 38, and 42% +/- 8% for Orion. RCW 38 IRS 2 is shown to be a massive star binary with a projected separation of similar to 500 AU. Two regions of molecular hydrogen emission are revealed through the 2.12 mu m imaging. One of these shows a morphology suggestive of a protostellar jet, and is clearly associated with a star only detected at H and K(s), and previously identified as a highly obscured X-ray source. Three spatially extended cometary-like objects, suggestive of photoevaporating disks, are identified, but only one is clearly directly influenced by RCW 38 IRS 2. The structure of the inner core of RCW 38 is also characterized and compared to Orion and other clusters. A King profile provides a reasonable fit to the cluster radial density profile and a nearest-neighbor distance analysis shows essentially no subclustering. C1 [DeRose, K. L.; Bourke, T. L.; Gutermuth, R. A.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Alves, J.] Ctr Astron Hispano Aleman, E-04004 Almeria, Spain. [Nuernberger, D.] European So Observ, Santiago 19001, Chile. RP DeRose, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261; Alves, Joao/0000-0002-4355-0921 FU NASA [1279160, NAS8-03060] FX We thank Joana Ascenso for providing the SOFI data in advance of publication, and for sharing her ISAAC results in advance of publication. We thank the VLT Science Operations team for successfully executing our NACO observations in service mode. Partial support for this work was provided by NASA through contract 1279160 issued by JPL/Caltech, and by NASA contract NAS8-03060. This research has made use of NASA's Astrophysics Data System. NR 59 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 33 EP 45 DI 10.1088/0004-6256/138/1/33 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300005 ER PT J AU Marengo, M Sanchez, MC AF Marengo, Massimo Sanchez, Mayly C. TI A k-NN METHOD TO CLASSIFY RARE ASTRONOMICAL SOURCES: PHOTOMETRIC SEARCH OF BROWN DWARFS WITH SPITZER/IRAC SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; methods: statistical; stars: low-mass, brown dwarfs ID DIGITAL SKY SURVEY; T-DWARFS; SPACE-TELESCOPE; SPECTRAL CLASSIFICATION; INFRARED PHOTOMETRY; ULTRACOOL DWARFS; COOL NEIGHBORS; FIELD; 2MASS; SPECTROSCOPY AB We present a statistical method for the photometric search of rare astronomical sources based on the weighted k-Nearest Neighbors method. A metric is defined in a multidimensional color-magnitude space based only on the photometric properties of template sources and the photometric uncertainties of both templates and data, without the need to define ad hoc color and magnitude cuts which could bias the search. The metric is defined as a function of two parameters, the number of neighbors k and a threshold distance D(th) that can be optimized for maximum selection efficiency and completeness. We apply the method to the search of L and T dwarfs in the Spitzer Extragalactic First Look Survey and the Bootes field of the Spitzer Shallow Survey, as well as to the search of substellar mass companions around nearby stars. With high level of completeness, we confirm the absence of late-T dwarfs detected in at least two bands in the First Look Survey, and only one in the Shallow Survey (previously discovered by Stern et al.). This result is in agreement with the expected statistics for late-T dwarfs. One L/early-T candidate is found in the First Look Survey, and three in the Shallow Surveys, currently undergoing follow-up spectroscopic verification. Finally, we discuss the potential for brown dwarf searches with this method in the Spitzer warm mission Exploration Science programs. C1 [Marengo, Massimo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanchez, Mayly C.] Argonne Natl Lab, Argonne, IL 60439 USA. [Sanchez, Mayly C.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmarengo@cfa.harvard.edu; mayly.sanchez@anl.gov FU NASA; National Aeronautics and Space Administration; National Science Foundation 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. 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 the National Aeronautics and Space Administration and the National Science Foundation. It also used data from the Sloan Digital Sky Survey (see full acknowledgment at http://www.sdss.org/collaboration/credits.html), and software provided by the U. S. National Virtual Observatory, which is sponsored by the National Science Foundation. We thank the Spitzer Shallow Survey and FLAMINGO Extragalactic Survey (FLAMEX) teams for permission to use data from their surveys. We also thank the National Optical Astronomy Observatory (NOAO) Deep Wide-Field Survey Team for providing the optical and near-IR imaging data used in the Bootes field. NOAO is operated by the Association of Universities for research in Astronomy (AURA), Inc., under a cooperative agreement with the National Science Foundation. The authors finally thank Peter Eisenhardt, Daniel Stern, Mark Brodwin, and Buell Jannuzi for useful discussions and suggestions, and the anonymous referee for insightful comments that helped improving this manuscript. NR 46 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 63 EP 75 DI 10.1088/0004-6256/138/1/63 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300008 ER PT J AU Kilic, M Kowalski, PM von Hippel, T AF Kilic, Mukremin Kowalski, Piotr M. von Hippel, Ted TI A NEAR-INFRARED SPECTROSCOPIC SURVEY OF COOL WHITE DWARFS IN THE SLOAN DIGITAL SKY SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: atmospheres; stars: evolution; white dwarfs ID PHOTOMETRIC ANALYSIS; HELIUM-ATMOSPHERE; GALACTIC HALO; SPECTROGRAPH; EVOLUTION; CATALOG; OPACITY; MODELS; STARS; SPEX AB We present near-infrared photometric observations of 15 and spectroscopic observations of 38 cool white dwarfs (WDs). This is the largest near-infrared spectroscopic survey of cool WDs to date. Combining the Sloan Digital Sky Survey photometry and our near-infrared data, we perform a detailed model atmosphere analysis. The spectral energy distributions of our objects are explained fairly well by model atmospheres with temperatures ranging from 6300 K down to 4200 K. Two WDs show significant absorption in the infrared, and are best explained with mixed H/He atmosphere models. Based on the up-to-date model atmosphere calculations by Kowalski & Saumon, we find that the majority of the stars in our sample have hydrogen-rich atmospheres. We do not find any pure helium atmosphere WDs below 5000 K, and we find a trend of increasing hydrogen to helium ratio with decreasing temperature. These findings present an important challenge to understanding the spectral evolution of WDs. C1 [Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kowalski, Piotr M.] Ruhr Univ Bochum, Lehrstuhl Theoret Chem, D-44780 Bochum, Germany. [von Hippel, Ted] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Kowalski, Piotr/L-7411-2013 OI Kowalski, Piotr/0000-0001-6604-3458 FU NASA; National Science Foundation [AST 06-07480]; National Aeronautics and Space Administration FX We thank S. K. Leggett and P. Dufour for extensive discussions, and D. Saumon and the anonymous referee for useful comments. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. P. M. K. thanks D. Marx as well as the theoretical chemistry group at Ruhr-Universitat Bochum for their hospitality and support. T. v. H. acknowledges support from the National Science Foundation under grant AST 06-07480. 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 40 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 102 EP 109 DI 10.1088/0004-6256/138/1/102 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300012 ER PT J AU High, FW Stubbs, CW Rest, A Stalder, B Challis, P AF High, F. William Stubbs, Christopher W. Rest, Armin Stalder, Brian Challis, Peter TI STELLAR LOCUS REGRESSION: ACCURATE COLOR CALIBRATION AND THE REAL-TIME DETERMINATION OF GALAXY CLUSTER PHOTOMETRIC REDSHIFTS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: fundamental parameters; methods: data analysis; stars: fundamental parameters; stars: statistics; techniques: photometric ID DIGITAL SKY SURVEY; HIGH-GALACTIC LATITUDE; MILKY-WAY TOMOGRAPHY; STANDARD STARS; CATALOG; SDSS; EXTINCTION; ATMOSPHERE; EMISSION; DWARFS AB We present stellar locus regression (SLR), a method of directly adjusting the instrumental broadband optical colors of stars to bring them into accord with a universal stellar color-color locus, producing accurately calibrated colors for both stars and galaxies. This is achieved without first establishing individual zero points for each passband, and can be performed in real-time at the telescope. We demonstrate how SLR naturally makes one wholesale correction for differences in instrumental response, for atmospheric transparency, for atmospheric extinction, and for Galactic extinction. We perform an example SLR treatment of Sloan Digital Sky Survey data over a wide range of Galactic dust values and independently recover the direction and magnitude of the canonical Galactic reddening vector with 14-18 mmag rms uncertainties. We then isolate the effect of atmospheric extinction, showing that SLR accounts for this and returns precise colors over a wide range of air mass, with 5-14 mmag rms residuals. We demonstrate that SLR-corrected colors are sufficiently accurate to allow photometric redshift estimates for galaxy clusters (using red sequence galaxies) with an uncertainty sigma(z)/(1 + z) = 0.6% per cluster for redshifts 0.09 < z < 0.25. Finally, we identify our objects in the 2MASS all-sky catalog, and produce i-band zero points typically accurate to 18 mmag using only SLR. We offer open-source access to our IDL routines, validated and verified for the implementation of this technique, at http://stellar-locus-regression.googlecode.com. C1 [High, F. William] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP High, FW (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM high@physics.harvard.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 NR 43 TC 56 Z9 56 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 110 EP 129 DI 10.1088/0004-6256/138/1/110 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300013 ER PT J AU Hole, KT Geller, AM Mathieu, RD Platais, I Meibom, S Latham, DW AF Hole, K. Tabetha Geller, Aaron M. Mathieu, Robert D. Platais, Imants Meibom, Soren Latham, David W. TI WIYN OPEN CLUSTER STUDY. XXIV. STELLAR RADIAL-VELOCITY MEASUREMENTS IN NGC 6819 SO ASTRONOMICAL JOURNAL LA English DT Article DE open clusters and associations: individual (NGC 6819); techniques: radial velocities ID OLD OPEN CLUSTERS; BLUE STRAGGLERS; VARIABLE-STARS; M67; NGC-6819; FIELD; PHOTOMETRY; MODELS; TRIPLE AB We present the current results from our ongoing radial-velocity (RV) survey of the intermediate-age (2.4 Gyr) open cluster NGC 6819. Using both newly observed and other available photometry and astrometry, we define a primary target sample of 1454 stars that includes main-sequence, subgiant, giant, and blue straggler stars, spanning a magnitude range of 11 <= V <= 16.5 and an approximate mass range of 1.1-1.6 M(circle dot). Our sample covers a 23 arcminute (13 pc) square field of view centered on the cluster. We have measured 6571 radial velocities for an unbiased sample of 1207 stars in the direction of the open cluster NGC 6819, with a single-measurement precision of 0.4 km s(-1) for most narrow-lined stars. We use our RV data to calculate membership probabilities for stars with >= 3 measurements, providing the first comprehensive membership study of the cluster core that includes stars from the giant branch through the upper main sequence. We identify 480 cluster members. Additionally, we identify velocity-variable systems, all of which are likely hard binaries that dynamically power the cluster. Using our single cluster members, we find a cluster average RV of 2.34 +/- 0.05 km s(-1). We use our kinematic cluster members to construct a cleaned color-magnitude diagram from which we identify rich giant, subgiant, and blue straggler populations and a well defined red clump. The cluster displays a morphology near the cluster turnoff clearly indicative of core convective overshoot. Finally, we discuss a few stars of note, one of which is a short-period red-clump binary that we suggest may be the product of a dynamical encounter. C1 [Platais, Imants] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Meibom, Soren; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hole, K. Tabetha; Geller, Aaron M.; Mathieu, Robert D.; Meibom, Soren] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. EM kth@astro.wisc.edu; geller@astro.wisc.edu; mathieu@astro.wisc.edu; imants@pha.jhu.edu; smeibom@cfa.harvard.edu; dlatham@cfa.harvard.edu FU NSF [AST-0406615, AST-0406689]; Wisconsin Space Grant Consortium; Oberlin College FX The authors are grateful to the following individuals for invaluable contributions to this work: Joanne Rosvick and Jason Kalirai for providing their photometry data for our comparisons; Bob Davis, Jim Peters, Perry Berlind, Ed Horine, Joe Zajac, and Ale Milone for their work on the CfA RV observations; Nigel Sharp for taking our original cluster photometry; Chris Dolan for initial setup work for the survey; and undergraduate and REU students Nick Stroud, Sylvana Yelda, Meagan Morscher, Michael DiPompeo, and Natalie Gosnell. This research was funded in part by NSF grants AST-0406615 (R.D.M.) and AST-0406689 (I.P.). K. T. H. gratefully acknowledges support from the Wisconsin Space Grant Consortium and Oberlin College. NR 42 TC 48 Z9 48 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 159 EP 168 DI 10.1088/0004-6256/138/1/159 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300016 ER PT J AU Paradis, D Reach, WT Bernard, JP Block, M Engelbracht, CW Gordon, K Hora, JL Indebetouw, R Kawamura, A Meade, M Meixner, M Sewilo, M Vijh, UP Volk, K AF Paradis, Deborah Reach, William T. Bernard, Jean-Philippe Block, Miwa Engelbracht, Chad W. Gordon, Karl Hora, Joseph L. Indebetouw, Remy Kawamura, Akiko Meade, Marilyn Meixner, Margaret Sewilo, Marta Vijh, Uma P. Volk, Kevin TI SPATIAL VARIATIONS OF DUST ABUNDANCES ACROSS THE LARGE MAGELLANIC CLOUD SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; ISM: abundances; infrared: ISM; Magellanic Clouds ID SPITZER-SPACE-TELESCOPE; POLYCYCLIC AROMATIC-HYDROCARBONS; SPECTRAL ENERGY-DISTRIBUTION; GALAXY EVOLUTION SAGE; INTERSTELLAR DUST; SMALL GRAINS; MIDINFRARED COLORS; INFRARED-EMISSION; STAR-FORMATION; PAH EMISSION AB Using the data obtained with the Spitzer Space Telescope as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) legacy survey, we have studied the variations of the dust composition and abundance across the Large Magellanic Cloud (LMC). Such variations are expected, as the explosive events which have lead to the formation of the many H I shells observed should have affected the dust properties. Using a model and comparing with a reference spectral energy distribution from our Galaxy, we deduce the relative abundance variations of small dust grains across the LMC. We examined the infrared color ratios as well as the relative abundances of very small grains (VSGs) and polycyclic aromatic hydrocarbons (PAHs) relative to the big grain abundance. Results show that each dust component could have different origins or evolution in the interstellar medium (ISM). The VSG abundance traces the star formation activity and could result from shattering of larger grains, whereas the PAH abundance increases around molecular clouds as well as in the stellar bar, where they could have been injected into the ISM during mass loss from old stars. C1 [Paradis, Deborah; Reach, William T.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Bernard, Jean-Philippe] Univ Toulouse, UPS, CESR, F-31028 Toulouse 9, France. [Bernard, Jean-Philippe] CNRS, UMR5187, F-31028 Toulouse, France. [Block, Miwa; Engelbracht, Chad W.; Gordon, Karl] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, Remy] Univ Virginia, Natl Radio Astron Observ 7, Charlottesville, VA 22903 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Kawamura, Akiko] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 46401, Japan. [Meade, Marilyn] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Meixner, Margaret; Sewilo, Marta] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Vijh, Uma P.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. [Volk, Kevin] No Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. RP Paradis, D (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. OI Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094 NR 46 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 196 EP 209 DI 10.1088/0004-6256/138/1/196 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300019 ER PT J AU Hall, JC Henry, GW Lockwood, GW Skiff, BA Saar, SH AF Hall, Jeffrey C. Henry, Gregory W. Lockwood, G. Wesley Skiff, Brian A. Saar, Steven H. TI THE ACTIVITY AND VARIABILITY OF THE SUN AND SUN-LIKE STARS. II. CONTEMPORANEOUS PHOTOMETRY AND SPECTROSCOPY OF BRIGHT SOLAR ANALOGS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: activity; Sun: activity ID MAUNDER MINIMUM; UVBY PHOTOMETRY; COOL STARS; IRRADIANCE; PERSPECTIVE; PATTERNS; PROJECT; SEARCH; SAMPLE; TWIN AB We present 14 years of contemporaneous photometric and spectroscopic observations of 28 solar analog stars, taken with the Tennessee State University Automatic Photometric Telescopes at Fairborn Observatory and the Solar-Stellar Spectrograph at Lowell Observatory. These are the best observed and most nearly Sun-like of the targets in our magnitude-limited (V <= 7.5) sample. The correlations between luminosity and activity reveal the expected inverse activity-brightness correlations for active stars. Strong direct correlations between activity and brightness are not prevalent for the less active solar age stars, but are precision limited. The Sun does not appear to have unusually low photometric variability when compared with the most Sun-like inactive solar analogs. We present evidence that the activity index R(HK)' is not a good discriminant of Maunder Minimum candidate stars. On the basis of a star that appears to have transitioned from a low-variability state to a cycling state, we investigate the regime in which stars might switch from faculae-dominated to spot-dominated variations. C1 [Hall, Jeffrey C.; Lockwood, G. Wesley; Skiff, Brian A.] Lowell Observ, Flagstaff, AZ 86001 USA. [Henry, Gregory W.] Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hall, JC (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. EM jch@lowell.edu NR 37 TC 64 Z9 64 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2009 VL 138 IS 1 BP 312 EP 322 DI 10.1088/0004-6256/138/1/312 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 457GK UT WOS:000266916300030 ER PT J AU Zwintz, K Hareter, M Kuschnig, R Amado, PJ Nesvacil, N Rodriguez, E Diaz-Fraile, D Weiss, WW Pribulla, T Guenther, DB Matthews, JM Moffat, AFJ Rucinski, SM Sasselov, D Walker, GAH AF Zwintz, K. Hareter, M. Kuschnig, R. Amado, P. J. Nesvacil, N. Rodriguez, E. Diaz-Fraile, D. Weiss, W. W. Pribulla, T. Guenther, D. B. Matthews, J. M. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Walker, G. A. H. TI MOST observations of the young open cluster NGC 2264 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: pre-main sequence; open clusters and associations: individual: NGC 2264; delta Sct; techniques: photometric ID PRE-MAIN-SEQUENCE; INITIAL MASS FUNCTION; LINE-DATA-BASE; DELTA-SCUTI STARS; INSTABILITY STRIP; PHOTOMETRY; NGC-2264; SPACE; PULSATION; SEISMOLOGY AB Context. Photometric time series obtained from space are one of the best ways to study pulsations in pre-main sequence (PMS) stars, especially as the corresponding amplitudes are at the millimagnitude level or below. We present high-precision time-series photometry of stars in the field of NGC2264 obtained with the MOST (Microvariability & Oscillations of STars) satellite. Aims. A search for pulsating A and F type members of NGC 2264 with ultra-precise MOST photometry was conducted. Methods. 68 stars in the field of NGC2264 were observed simultaneously with the MOST satellite, 34 of which were previously identified as potential targets to search for PMS pulsation. The routines SigSpec and Period04 were used for the frequency analysis. Results. We discovered pulsation in 4 potential A and F type PMS members of NGC2264 with frequencies between 2.7 h and 23 min. For one of the PMS pulsators identified with MOST after the first days of observation, simultaneous ground-based Stromgren photometry was obtained with the OSN 0.9 m telescope and confirms the highest frequency identified in the MOST photometry. 26 stars with other (i.e., hotter and cooler) spectral types show clear variability: SPB and gamma Doradus pulsation, red giant oscillations, eclipsing binaries and variability caused by rotational modulation. C1 [Zwintz, K.; Hareter, M.; Kuschnig, R.; Nesvacil, N.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kuschnig, R.; Matthews, J. M.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Amado, P. J.; Rodriguez, E.; Diaz-Fraile, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Pribulla, T.] Inst Astrophys, D-07740 Jena, Germany. [Pribulla, T.] Univ Sternwarte, D-07740 Jena, Germany. [Pribulla, T.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Richmond Hill, ON L4C 4Y6, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zwintz, K (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria. EM zwintz@astro.univie.ac.at; kuschnig@astro.ubc.ca; pja@iaa.es; eloy@iaa.es; dario@iaa.es; pribulla@ta3.sk; guenther@ap.smu.ca; matthews@astro.ubc.ca; moffat@astro.umontreal.ca; rucinski@astro.utoronto.ca; sasselov@cfa.harvard.edu; gordonwa@uvic.ca RI Amado, Pedro Jose/G-3450-2011; OI Amado, Pedro Jose/0000-0002-8388-6040; Rodriguez, Eloy/0000-0001-6827-9077; Zwintz, Konstanze/0000-0001-9229-8315; Nesvacil, Nicole/0000-0002-7920-7754 FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung [T335-N16, P17890]; Spanish Ministry of Education and Science; Natural Sciences and Engineering Research Council of Canada; FQRT (Quebec); Canadian Space Agency; EU [MTKD-CT-2006-042514] FX K. Z., M. H., N. N. and W. W. W. acknowledge support by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung (K. Z.: project T335-N16; M. H., N. N. and W. W. W.: project P17890). P. J. A. acknowledges financial support from a "Ramon y Cajal" contract of the Spanish Ministry of Education and Science. The Natural Sciences and Engineering Research Council of Canada supports the research of D. B. G., J. M. M., A. F. J. M. and S. M. R.; A. F. J. M. is also supported by FQRT (Quebec), and R. K. is also supported by the Canadian Space Agency. T. P. has beed funded by the Canadian Space Agency Enhancement Program (SSEP) holding a post-doctoral fellowship position at the University of Toronto and also acknowledges support from the EU in the FP6 MC ToK project MTKD-CT-2006-042514. Frequency analysis was performed using SigSpec (Reegen 2007) and Period04 (Lenz & Breger 2005). This research has made use of the WEBDA database, developed by J.-C. Mermilliod (Laboratory of Astrophysics of the EPFL, Switzerland) and operated by E. Paunzen at the Institute for Astronomy of the University of Vienna. Spectroscopic observations were obtained at the David Dunlap Observatory, University of Toronto. NR 54 TC 18 Z9 18 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 JUL PY 2009 VL 502 IS 1 BP 239 EP 252 DI 10.1051/0004-6361/200911863 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 477RI UT WOS:000268535800022 ER PT J AU Tengstrand, O Guainazzi, M Siemiginowska, A Bonilla, NF Labiano, A Worrall, DM Grandi, P Piconcelli, E AF Tengstrand, O. Guainazzi, M. Siemiginowska, A. Fonseca Bonilla, N. Labiano, A. Worrall, D. M. Grandi, P. Piconcelli, E. TI The X-ray view of giga-hertz peaked spectrum radio galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: jets; galaxies: active; X-rays: galaxies ID COMPACT STEEP-SPECTRUM; ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; DIGITAL SKY SURVEY; COMPTON-THICK AGN; HI ABSORBING GAS; XMM-NEWTON; SYMMETRIC OBJECTS; FR-I; ENERGY-DISTRIBUTIONS AB Context. This paper presents the X-ray properties of a flux- and volume-limited complete sample of 16 giga-hertz peaked spectrum (GPS) galaxies. Aims. This study addresses three basic questions in our understanding of the nature and evolution of GPS sources: a) What is the physical origin of the X-ray emission in GPS galaxies? b) Which physical system is associated with the X-ray obscuration? c) What is the "endpoint" of the evolution of compact radio sources? Methods. We discuss in this paper the results of the X-ray spectral analysis, and compare the X-ray properties of the sample sources with radio observables. Results. We obtain a 100% (94%) detection fraction in the 0.5-2 keV (0.5-10 keV) energy band. GPS galaxy X-ray spectra are typically highly obscured (< N(H)(GPS)> = 3 x 10(22) cm(-2); sigma(NH) similar or equal to 0.5 dex). The X-ray column density is larger than the HI column density measured in the radio by a factor 10 to 100. GPS galaxies lie well on the extrapolation to high radio powers of the correlation between radio and X-ray luminosity known in low-luminosity FR I radio galaxies. On the other hand, GPS galaxies exhibit a comparable X-ray luminosity to FR II radio galaxies, notwithstanding their much larger radio luminosity. Conclusions. The X-ray to radio luminosity ratio distribution in our sample is consistent with the bulk of the high-energy emission being produced by the accretion disk, as well as with dynamical models of GPS evolution where X-rays are produced by Compton upscattering of ambient photons. Further support to the former scenario comes from the location of GPS galaxies in the X-ray to O[III] luminosity ratio versus N(H) plane. We propose that GPS galaxies are young radio sources, which would reach their full maturity as classical FR II radio galaxies. However, column densities greater than or similar to 10(22) cm(-2) could lead to a significant underestimate of dynamical age determinations based on the hotspot recession velocity measurements. C1 [Tengstrand, O.; Guainazzi, M.; Fonseca Bonilla, N.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Tengstrand, O.] Linkoping Univ, Inst Technol, S-58183 Linkoping, Sweden. [Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Labiano, A.] CSIC, Inst Estruct Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. [Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Grandi, P.] INAF, Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Piconcelli, E.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. RP Tengstrand, O (reprint author), ESA, European Space Astron Ctr, POB 78, Madrid 28691, Spain. EM Matteo.Guainazzi@sciops.esa.int OI piconcelli, enrico/0000-0001-9095-2782; Grandi, Paola/0000-0003-1848-6013 FU NASA [NNX07AQ55G, NAS8-39073]; ESA Internal Fellowship Trainee FX 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 made use of data obtained through the High Energy Astrophysics Science Archive Research Centre Online Service, provided by the NASA/Goddard Space Flight Centre and 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. O.T. thanks the whole ESA administration, and in particular Nienke de Boer, Marcus Kirsch and Fernando Maura, for their support during a six-month traineeship at ESAC, where most of the data analysis included in this paper was performed. This research is funded in part by NASA grant NNX07AQ55G. O.T. gratefully acknowledge an ESA Internal Fellowship Trainee grant. A. S. is partly supported by NASA contract NAS8-39073. The authors thank C. Stanghellini for a critical revision of an early version of this manuscript. Last, but not least, the authors gratefully acknowledge a careful and accurate referee report by Dr. D.J. Saikia, which greatly improved the overall presentation of the paper, while allowing us to better clarify some aspects of the radio measurements discussed in this paper. NR 84 TC 25 Z9 25 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 JUL PY 2009 VL 501 IS 1 BP 89 EP 102 DI 10.1051/0004-6361/200811284 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 470HF UT WOS:000267965100010 ER PT J AU Panic, O Hogerheijde, MR Wilner, D Qi, C AF Panic, O. Hogerheijde, M. R. Wilner, D. Qi, C. TI A break in the gas and dust surface density of the disc around the T Tauri star IM Lupi SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems: protoplanetary disks; stars: individual: IM Lup; stars: pre-main sequence; circumstellar matter ID MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; CIRCUMSTELLAR DISKS; RADIATIVE-TRANSFER; ACCRETION DISKS; DM-TAU; MODELS; TEMPERATURE; OPACITIES AB Aims. We study the distribution and physical properties of molecular gas in the disc around the T Tauri star IM Lup on scales close to 200 AU. We investigate how well the gas and dust distributions compare and work towards a unified disc model that can explain both gas and dust emission. Methods. (12)CO, (13)CO, and C(18)O J = 2-1 line emission, as well as the dust continuum at 1.3 mm, is observed at 1 ''.8 resolution towards IM Lup using the Submillimeter Array. A detailed disc model based on the dust emission is tested against these observations with the aid of a molecular excitation and radiative transfer code. Apparent discrepancies between the gas and dust distribution are investigated by adopting simple modifications to the existing model. Results. The disc is seen at an inclination of 54 degrees +/- 3 degrees and is in Keplerian rotation around a 0.8-1.6 M(circle dot) star. The outer disc radius traced by molecular gas emission is 900 AU, while the dust continuum emission and scattered light images limit the amount of dust present beyond 400 AU and are consistent with the existing model that assumes a 400 AU radius. Our observations require a drastic density decrease close to 400 AU with the vertical gas column density at 900 AU in the range of 5 x 10(20)-10(22) cm(-2). We derive a gas-to-dust mass ratio of 100 or higher in disc regions beyond 400 AU. Within 400 AU from the star our observations are consistent with a gas-to-dust ratio of 100 but other values are not ruled out. C1 [Panic, O.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Wilner, D.; Qi, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Panic, O (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM olja@strw.leidenuniv.nl FU Netherlands Organisation for Scientific Research FX The research of O.P. and M. R. H. is supported through a VIDI grant from the Netherlands Organisation for Scientific Research. We would like to thank our Leiden colleagues Anders Johansen and Richard D. Alexander for valuable insights and discussions, as well as C. P. Dullemond, A. Juhasz and others at the Star and Planet Formation Department of MPIA Heidelberg for their help and advice during the stay of O. P. in March 2008. Finally, we are grateful to E. F. van Dishoeck for her support and guidance throughout the writing of this paper. NR 35 TC 43 Z9 43 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 JUL PY 2009 VL 501 IS 1 BP 269 EP 278 DI 10.1051/0004-6361/200911883 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 470HF UT WOS:000267965100021 ER PT J AU Santangelo, G Testi, L Gregorini, L Leurini, S Vanzi, L Walmsley, CM Wilner, DJ AF Santangelo, G. Testi, L. Gregorini, L. Leurini, S. Vanzi, L. Walmsley, C. M. Wilner, D. J. TI Resolving the molecular environment of super star clusters in Henize 2-10 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: dwarf; galaxies: individual: Henize 2-10; galaxies: starburst ID STARBURST GALAXY HENIZE-2-10; CO-TO-H-2 CONVERSION FACTOR; IRREGULAR GALAXIES; SPIRAL GALAXIES; CLOUDS; GAS; MASS; GLOBULES AB Context. The rate of star formation both in the Galaxy and in external galaxies should be related to the physical properties of the molecular clouds from which stars form. This is expected for the starbursts found both in irregular galaxies and in some mergers. The dwarf galaxy Henize 2-10 is particularly interesting in this context as it shows a number of newly formed super star clusters (SSCs) associated with a very rich molecular environment. Aims. We present a high angular resolution study of the molecular gas associated with the SSCs with the aim of deriving the physical properties of the parent molecular clouds. The final goal is to test the expectation that the formation of SSCs requires exceptionally dense and massive clouds. Methods. We have used the Submillimeter Array with an angular resolution of 1 ''.9 x 1 ''.3 to map the J = 2-1 transition of CO in Henize 2-10. Supplementary measurements of HCN(J = 1-0), (CO)-C-13(J = 2-1) and millimeter continuum were obtained with the APEX, IRAM 30 m and SEST single dish telescopes. Results. Our single dish observations confirm the association of the newly formed SSCs in Henize 2-10 with dense molecular gas. Our interferometric observations resolve the CO(2-1) emission in several giant molecular clouds. Overall the molecular gas accounts for approximately half of the mass in the central regions of Henize 2-10. Although we find indications that the molecular clouds associated with the formation of SSCs in Henize 2-10 are massive and dense, the tracer we used (CO) and the linear resolution of our observations (60 x 80 pc) are still not adequate to test the expectation that exceptionally dense and massive cores are required for SSCs formation. C1 [Santangelo, G.; Testi, L.; Leurini, S.] European So Observ, D-85748 Garching, Germany. [Santangelo, G.; Gregorini, L.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Santangelo, G.; Gregorini, L.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Testi, L.; Walmsley, C. M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Vanzi, L.] Pontificia Univ Catolica Chile, Dept Ingn Elect, Santiago, Chile. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Santangelo, G (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM gsantang@eso.org; ltesti@eso.org RI Vanzi, Leonardo/D-1381-2014 NR 47 TC 9 Z9 9 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2009 VL 501 IS 2 BP 495 EP 503 DI 10.1051/0004-6361/200911688 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472JA UT WOS:000268125300011 ER PT J AU Vilhu, O Hakala, P Hannikainen, DC McCollough, M Koljonen, K AF Vilhu, O. Hakala, P. Hannikainen, D. C. McCollough, M. Koljonen, K. TI Orbital modulation of X-ray emission lines in Cygnus X-3 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; accretion, accretion disks; stars: binaries: spectroscopic; stars: winds, outflows; stars: individual: Cygnus X-3; stars: neutron ID CYG X-3; BINARIES; STARS; SPECTROSCOPY; MODEL; WIND AB Aims. We address the problem where the X-ray emission lines are formed and investigate orbital dynamics using Chandra HETG observations, photoionizing calculations and numerical wind-particle simulations. The aims were to set constraints on the masses of the components of this close binary system consisting of a Wolf-Rayet (WR) star and a compact component and to investigate the nature of the latter (neutron star or black hole). The goal was also to investigate P Cygni signatures in line profiles. Methods. The observed Si XIV (6.185 angstrom) and S XVI (4.733 angstrom) line profiles at four orbital phases were fitted with P Cygni-type profiles consisting of an emission and a blue-shifted absorption component. Numerical models were constructed using photoionizing calculations and particle simulations. In the models, the emission originates in the photoionized wind of the WR companion illuminated by a hybrid source: the X-ray radiation of the compact star and the photospheric EUV-radiation from the WR star. Results. Spectral lines with moderate excitation (such as Si XIV and S XVI) arise in the photoionized wind. The emission component exhibits maximum blue-shift at phase 0.5 (when the compact star is in front), while the velocity of the absorption component is constant (around -900 km s(-1)). Both components, like the continuum flux, have intensity maxima around phase 0.5. The simulated Fe XXVI Lya line (1.78 angstrom, H-like) from the wind is weak compared to the observed one. We suggest that it originates in the vicinity of the compact star, with a maximum blue shift at phase 0.25 (compact star approaching). By combining the mass function derived with that from the infrared He I absorption (arising from the WR companion), we constrain the masses and the inclination of the system. Conclusions. The Si XIV and S XVI lines and their radial velocity curves can be understood in the framework of a photoionized wind involving a hybrid ionizer. Constraints on the compact star mass and orbital inclination (i) are given using the mass functions derived from the Fe XXVI line and He I 2.06 mu m absorption. Both a neutron star at large inclination (i >= 60 degrees) and a black hole at small inclination are possible solutions. The radial velocity amplitude of the He II 2.09 mu m emission (formed in the X-ray shadow behind the WR star) suggests i = 30 degrees, implying a possible compact star mass between 2.8-8.0 M(circle dot). For i = 60 degrees the same range is 1.0-3.2 M(circle dot). C1 [Vilhu, O.; Hannikainen, D. C.; Koljonen, K.] Univ Helsinki, Observ Tahtitorninmaki, FIN-00014 Helsinki, Finland. [Hakala, P.] Univ Turku, Tuorla Observ, Piikkio 21500, Finland. [McCollough, M.; Koljonen, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hannikainen, D. C.] Metsahovi Radio Observ TKK, Kylmala 02540, Finland. RP Vilhu, O (reprint author), Univ Helsinki, Observ Tahtitorninmaki, POB 14, FIN-00014 Helsinki, Finland. EM osmi.vilhu@astro.helsinki.fi; pahakala@astro.utu.fi; diana@kurp.hut.fi; mccolml@head-cfa.harvard.edu OI Koljonen, Karri/0000-0002-9677-1533 FU Academy of Finland for a Fellowship FX We thank Dr. Tim Kallman for advice in using the XSTAR code and providing additional IR line atomic data. D. C. H. is grateful to the Academy of Finland for a Fellowship. We thank the anonymous referee for pushing us to improve the presentation. 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 packages CIAO, ChIPS, and Sherpa. NR 30 TC 21 Z9 21 U1 0 U2 1 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 JUL PY 2009 VL 501 IS 2 BP 679 EP 686 DI 10.1051/0004-6361/200811293 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472JA UT WOS:000268125300025 ER PT J AU Olah, K Kollath, Z Granzer, T Strassmeier, KG Lanza, AF Jarvinen, S Korhonen, H Baliunas, SL Soon, W Messina, S Cutispoto, G AF Olah, K. Kollath, Z. Granzer, T. Strassmeier, K. G. Lanza, A. F. Jarvinen, S. Korhonen, H. Baliunas, S. L. Soon, W. Messina, S. Cutispoto, G. TI Multiple and changing cycles of active stars II. Results SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: atmospheres; stars: late-type; starspots ID LONG-TERM PHOTOMETRY; MAIN-SEQUENCE STARS; STELLAR ACTIVITY CYCLES; SUN-LIKE STARS; MAGNETIC ACTIVITY; CHROMOSPHERIC VARIATIONS; DIFFERENTIAL ROTATION; FLUX MEASUREMENTS; WAVELET ANALYSIS; HK LACERTAE AB Aims. We study the time variations in the cycles of 20 active stars based on decade-long photometric or spectroscopic observations. Methods. A method of time-frequency analysis, as discussed in a companion paper, is applied to the data. Results. Fifteen stars definitely show multiple cycles, but the records of the rest are too short to verify a timescale for a second cycle. The cycles typically show systematic changes. For three stars, we found two cycles in each of them that are not harmonics and vary in parallel, indicating a common physical mechanism arising from a dynamo construct. The positive relation between the rotational and cycle periods is confirmed for the inhomogeneous set of active stars. Conclusions. Stellar activity cycles are generally multiple and variable. C1 [Olah, K.; Kollath, Z.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Granzer, T.; Strassmeier, K. G.; Jarvinen, S.] AIP, D-14482 Potsdam, Germany. [Korhonen, H.] ESO, D-85748 Garching, Germany. [Baliunas, S. L.; Soon, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lanza, A. F.; Messina, S.; Cutispoto, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Jarvinen, S.] Univ Turku, Tuorla Observ, Piikkio 21500, Finland. [Jarvinen, S.] Univ Oulu, Astron Div, Oulu 90014, Finland. RP Olah, K (reprint author), Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. EM olah@konkoly.hu RI Korhonen, Heidi/E-3065-2016; OI Korhonen, Heidi/0000-0003-0529-1161; Lanza, Antonino Francesco/0000-0001-5928-7251; Messina, Sergio/0000-0002-2851-2468 FU Hungarian Research Grants OTKA [T-048961, T-068626]; JPL [12700064]; Smithsonian Institution Restricted Endowment funds; NASA [NNX07AI356]; Vienna-AIP APTs in southern Arizona; State of Brandenburg MWFK FX We are grateful for the useful discussion with L. van Driel-Gesztelyi. K. O. acknowledges support from the Hungarian Research Grants OTKA T-048961 and T-068626. S. B. acknowledges support from JPL 12700064, Smithsonian Institution Restricted Endowment funds and NASA NNX07AI356. K. G. S. appreciates the continuous support of the Vienna-AIP APTs in southern Arizona through the State of Brandenburg MWFK. NR 52 TC 74 Z9 75 U1 0 U2 1 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 JUL PY 2009 VL 501 IS 2 BP 703 EP 713 DI 10.1051/0004-6361/200811304 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 472JA UT WOS:000268125300028 ER PT J AU Zhang, WM Soria, R Zhang, SN Swartz, DA Liu, JF AF Zhang, Wei Ming Soria, Roberto Zhang, Shuang Nan Swartz, Douglas A. Liu, JiFeng TI A CENSUS OF X-RAY NUCLEAR ACTIVITY IN NEARBY GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: nuclei; galaxies: statistics; X-rays: galaxies ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; XMM-NEWTON OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; DWARF SEYFERT NUCLEI; DIGITAL SKY SURVEY; H-II REGIONS; GALACTIC NUCLEI; STAR-FORMATION; SOURCE POPULATION AB We have studied the X-ray nuclear activity of 187 nearby (distance less than 15 Mpc) galaxies observed with Chandra/ACIS. We found that 86 of them have a pointlike X-ray core, consistent with an accreting black hole (BH). We argue that the majority of them are nuclear BHs, rather than X-ray binaries. The fraction of galaxies with an X-ray-detected nuclear BH is higher (approximate to 60%) for ellipticals and early type spirals (E to Sb), and lower (approximate to 30%) for late-type spirals (Sc to Sm). There is no preferential association of X-ray cores with the presence of a large-scale bar; in fact, strongly barred galaxies appear to have slightly lower detection fraction and luminosity for their nuclear Xray sources, compared with nonbarred orweakly barred galaxies of similar Hubble types. The cumulative luminosity distribution of the nuclear sources in the 0.3-8 keV band is a power law with slope approximate to -0.5, from approximate to 2 x 10(38) erg s(-1) to approximate to 10(42) erg s(-1). The Eddington ratio is lower for ellipticals (L-X/L-Edd similar to 10(-8)) and higher for late-type spirals (up to L-X/L-Edd similar to 10(-4)), but in all cases, the accretion rate is low enough to be in the radiatively inefficient regime. The intrinsic absorbing column density is generally low, especially for the less luminous sources: there appear to be no Type 2 nuclear BHs at luminosities less than or similar to 10(39) erg s(-1). The lack of a dusty torus or of other sources of intrinsic absorption (e.g., an optically thick disk wind) may be directly related to the lack of a standard accretion disk around those faint nuclear BHs. The fraction of obscured sources increases with the nuclear BH luminosity: two-thirds of the sources with L-X > 10(40) erg s(-1) have a fitted column density greater than 1022 cm(-2). This is in contrast to the declining trend of the obscured fraction with increasing luminosities, observed in more luminous active galactic nuclei and quasars. C1 [Zhang, Wei Ming; Zhang, Shuang Nan] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Zhang, Wei Ming; Zhang, Shuang Nan] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. [Soria, Roberto] Univ Coll London, MSSL, Dorking RH5 6NT, Surrey, England. [Swartz, Douglas A.] NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Huntsville, AL 35812 USA. [Liu, JiFeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, WM (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM zhangweiming@mails.thu.edu.cn NR 133 TC 51 Z9 51 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 JUL 1 PY 2009 VL 699 IS 1 BP 281 EP 297 DI 10.1088/0004-637X/699/1/281 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458WC UT WOS:000267056300022 ER PT J AU Harris, DE Cheung, CC Stawarz, L Biretta, JA Perlman, ES AF Harris, D. E. Cheung, C. C. Stawarz, Lukasz Biretta, J. A. Perlman, E. S. TI VARIABILITY TIMESCALES IN THE M87 JET: SIGNATURES OF E-2 LOSSES, DISCOVERY OF A QUASI PERIOD IN HST-1, AND THE SITE OF TeV FLARING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M87); galaxies: jets; radiation mechanisms: non-thermal; radio continuum: galaxies; X-rays: general ID GAMMA-RAY EMISSION; GALAXY M87 AB We investigate the variability timescales in the jet of M87 with two goals. The first is to use the rise times and decay times in the radio, ultraviolet, and X-ray light curves of HST-1 to constrain the source size and the energy loss mechanisms affecting the relativistic electron distributions. HST-1 is the first jet knot clearly resolved from the nuclear emission by Chandra and is the site of the huge flare of 2005. We find clear evidence for a frequency-dependent decrease in the synchrotron flux being consistent with E-2 energy losses. Assuming that this behavior is predominantly caused by synchrotron cooling, we estimate a value of 0.6 mG for the average magnetic field strength of the HST-1 emission region, a value consistent with previous estimates of the equipartition field. In the process of analyzing the first derivative of the X-ray light curve of HST-1, we discovered a quasi-periodic oscillation which was most obvious in 2003 and 2004 prior to the major flare in 2005. The four cycles observed have a period of order six months. The second goal is to search for evidence of differences between the X-ray variability timescales of HST-1 and the unresolved nuclear region (diameter <0 ''.6). These features, separated by more than 60 pc, are the two chief contenders for the origin of the TeV variable emissions observed by H. E. S. S. in 2005 and by MAGIC and VERITAS in 2008. The X-ray variability of the nucleus appears to be at least twice as rapid as that of the HST-1 knot. However, the shortest nuclear variability timescale we can measure from the Chandra data (<= 20 days) is still significantly longer than the shortest TeV variability of M87 reported by the H. E. S. S. and MAGIC telescopes (1-2 days). C1 [Harris, D. E.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cheung, C. C.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Stawarz, Lukasz] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Biretta, J. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Perlman, E. S.] Florida Inst Technol, Phys & Space Sci Dept, Melbourne, FL 32901 USA. [Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. RP Harris, DE (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM harris@cfa.harvard.edu NR 21 TC 61 Z9 61 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 JUL 1 PY 2009 VL 699 IS 1 BP 305 EP 314 DI 10.1088/0004-637X/699/1/305 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458WC UT WOS:000267056300024 ER PT J AU Showman, AP Fortney, JJ Lian, Y Marley, MS Freedman, RS Knutson, HA Charbonneau, D AF Showman, Adam P. Fortney, Jonathan J. Lian, Yuan Marley, Mark S. Freedman, Richard S. Knutson, Heather A. Charbonneau, David TI ATMOSPHERIC CIRCULATION OF HOT JUPITERS: COUPLED RADIATIVE-DYNAMICAL GENERAL CIRCULATION MODEL SIMULATIONS OF HD 189733b and HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: numerical; planets and satellites: general; planets and satellites: individual (HD 209458b, HD 189733b) ID EXTRASOLAR GIANT PLANETS; SHALLOW-WATER TURBULENCE; MASS DWARF STARS; TRANSMISSION SPECTRUM; INFRARED-EMISSION; THERMAL STRUCTURE; BROWN DWARFS; LIGHT CURVES; T DWARFS; CHEMISTRY AB We present global, three-dimensional numerical simulations of HD 189733b and HD 209458b that couple the atmospheric dynamics to a realistic representation of nongray cloud-free radiative transfer. The model, which we call the Substellar and Planetary Atmospheric Radiation and Circulation model, adopts the MITgcm for the dynamics and uses the radiative model of McKay, Marley, Fortney, and collaborators for the radiation. Like earlier work with simplified forcing, our simulations develop a broad eastward equatorial jet, mean westward flow at higher latitudes, and substantial flow over the poles at low pressure. For HD189733b, our simulations without TiO and VO opacity can explain the broad features of the observed 8 and 24 mu m light curves, including the modest day-night flux variation and the fact that the planet/star flux ratio peaks before the secondary eclipse. Our simulations also provide reasonable matches to the Spitzer secondary-eclipse depths at 4.5, 5.8, 8, 16, and 24 mu m and the ground-based upper limit at 2.2 mu m. However, we substantially underpredict the 3.6 mu m secondary-eclipse depth, suggesting that our simulations are too cold in the 0.1-1 bar region. Predicted temporal variability in secondary-eclipse depths is similar to 1% at Spitzer bandpasses, consistent with recent observational upper limits at 8 mu m. We also show that nonsynchronous rotation can significantly alter the jet structure. For HD 209458b, we include TiO and VO opacity; these simulations develop a hot (> 2000 K) dayside stratosphere whose horizontal dimensions are small at depth but widen with altitude. Despite this stratosphere, we do not reproduce current Spitzer photometry of this planet. Light curves in Spitzer bandpasses show modest phase variation and satisfy the observational upper limit on day-night phase variation at 8 mu m. C1 [Showman, Adam P.; Lian, Yuan] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Showman, Adam P.; Lian, Yuan] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marley, Mark S.; Freedman, Richard S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Freedman, Richard S.] SETI Inst, Mountain View, CA 94043 USA. [Knutson, Heather A.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Showman, AP (reprint author), Univ Arizona, Dept Planetary Sci, 1629 Univ Blvd, Tucson, AZ 85721 USA. EM showman@lpl.arizona.edu RI Marley, Mark/I-4704-2013; OI Fortney, Jonathan/0000-0002-9843-4354; Charbonneau, David/0000-0002-9003-484X FU NASA [NNX08AF27G]; Planetary Atmospheres [NNX07AF35G, NNG06GF28G] FX This research was supported by NASA Origins grant NNX08AF27G and Planetary Atmospheres grants NNX07AF35G and NNG06GF28G to A.P.S. NR 81 TC 204 Z9 207 U1 1 U2 9 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 JUL 1 PY 2009 VL 699 IS 1 BP 564 EP 584 DI 10.1088/0004-637X/699/1/564 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458WC UT WOS:000267056300044 ER PT J AU Rathborne, JM Lada, CJ Muench, AA Alves, JF Kainulainen, J Lombardi, M AF Rathborne, J. M. Lada, C. J. Muench, A. A. Alves, J. F. Kainulainen, J. Lombardi, M. TI DENSE CORES IN THE PIPE NEBULA: AN IMPROVED CORE MASS FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: globules; ISM: molecules; stars: formation; stars: luminosity function, mass function ID OPHIUCHI MOLECULAR CLOUD; 850 MU-M; STAR-FORMATION; CLUMP DISTRIBUTION; INITIAL CONDITIONS; SCUBA SURVEY; ORION; POPULATION; DUST; EMISSION AB In this paper, we derive an improved core mass function (CMF) for the Pipe Nebula from a detailed comparison between measurements of visual extinction and molecular-line emission. We have compiled a refined sample of 201 dense cores toward the Pipe Nebula using a two-dimensional threshold identification algorithm informed by recent simulations of dense core populations. Measurements of radial velocities using complimentary C(18)O (1-0) observations enable us to cull out from this sample those 43 extinction peaks that are either not associated with dense gas or are not physically associated with the Pipe Nebula. Moreover, we use the derived C18O central velocities to differentiate between single cores with internal structure and blends of two or more physically distinct cores, superposed along the same line of sight. We then are able to produce a more robust dense core sample for future follow-up studies and a more reliable CMF than was possible previously. We confirm earlier indications that the CMF for the Pipe Nebula departs from a single power-law-like form with a break or knee at M similar to 2.7 +/- 1.3 M(circle dot). Moreover, we also confirm that the CMF exhibits a similar shape to the stellar initial mass function (IMF), but is scaled to higher masses by a factor of similar to 4.5. We interpret this difference in scaling to be a measure of the star formation efficiency (22% +/- 8%). This supports earlier suggestions that the stellar IMF may originate more or less directly from the CMF. C1 [Rathborne, J. M.; Lada, C. J.; Muench, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alves, J. F.] Ctr Astron Hispano Aleman, Calar Alto Observ, Almeria 04004, Spain. [Kainulainen, J.] TKK Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Kainulainen, J.] Univ Helsinki, FIN-00014 Helsinki, Finland. [Lombardi, M.] European So Observ, D-85748 Garching, Germany. RP Rathborne, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jrathborne@cfa.harvard.edu; clada@cfa.harvard.edu; gmuench@cfa.harvard.edu; jalves@caha.es; jouni.kainulainen@helsinki.fi; mlombard@eso.org OI Muench, August/0000-0003-0666-6367; LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU NASA Origins [NAG-13041]; NASA Spitzer [PID 20119]; JPL [1279166] FX We thank the referee for a thorough reading of the paper and the useful suggestions which have improved the paper. These observations were supported through NASA Origins grant NAG-13041 and the NASA Spitzer GO program (PID 20119) and supported by JPL contract 1279166. NR 29 TC 56 Z9 57 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2009 VL 699 IS 1 BP 742 EP 753 DI 10.1088/0004-637X/699/1/742 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458WC UT WOS:000267056300056 ER PT J AU Nichols, J Slavin, JD AF Nichols, Joy Slavin, Jonathan D. TI FUSE OBSERVATIONS REVEAL THE NATURE OF THE STELLAR JETS IN R Aqr SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: symbiotic; ISM: jets and outflows; line: profiles; ultraviolet: ISM ID SYMBIOTIC STAR MWC-560; X-RAY; HYDRODYNAMICAL SIMULATIONS; AQUARII JET; BOW SHOCK; SYMMETRICAL JET; ULTRAVIOLET; EMISSION; RADIO; SYSTEM AB R Aquarii is a symbiotic system consisting of a Mira variable and a white dwarf companion. Its jet-like structures have been observed in the X-rays through the radio and extend up to 2500 AU from the central object. We report Far Ultraviolet Spectroscopic Explorer observations of O VI emission from these stellar jets that reveal signature line profiles of bow shocks. We have calculated bow shock models for a fully radiative shock, fully non-radiative shock, and a new hybrid set of models. We found that fully non-radiative shocks do not produce good fits to the data. While a fully radiative bow shock model cannot be excluded, the high densities required led us to develop hybrid bow shock models in which the shock is non-radiative near the apex of the bow shock, but becomes radiative at some distance from the apex. The model that best fits the data is the hybrid bow shock with a shock speed of approximately 235-285 km s(-1) and an inclination angle of similar to + 10 degrees and + 35 degrees with the plane of the sky for the northeast and the southwest jets, respectively. A turbulent velocity of about 60 km s(-1) was required to obtain good fits. Surprisingly, both of the opposing jets have similar model parameters in spite of their very different O VI flux and distance from the central object. This analysis confirms the ejecta bow shock scenario as opposed to the cloudlet bow shock, constraining the mechanism of jet production to characteristics of the central object. The striking similarities in the physical parameters of the jets indicate a common origin and support the precessing accretion disk scenario for the white dwarf in the R Aqr system. For both jets we find pre-shock densities in the range of 10(3)-10(4) cm(-3) at positions of the brightest X-ray emission from the jets, which are also the positions of the apparent outer terminal points of the jets, providing strong support for the theory that the emission and shock structures we are seeing are produced when the jet material interacts with an external nebular wall. C1 [Nichols, Joy; Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nichols, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jnichols@cfa.harvard.edu OI Slavin, Jonathan/0000-0002-7597-6935 NR 32 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2009 VL 699 IS 1 BP 902 EP 910 DI 10.1088/0004-637X/699/1/902 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458WC UT WOS:000267056300069 ER PT J AU Drake, JJ Ercolano, B Flaccomio, E Micela, G AF Drake, Jeremy J. Ercolano, Barbara Flaccomio, Ettore Micela, Giusi TI X-RAY PHOTOEVAPORATION-STARVED T TAURI ACCRETION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems: protoplanetary disks; stars: coronae; stars: formation; stars: pre-main sequence; stars: winds, outflows; X-rays: stars ID ORION NEBULA CLUSTER; INFRARED TRIPLET LINES; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISKS; ULTRADEEP PROJECT; FORMING REGION; MASS STARS; EMISSION; PHOTOIONIZATION; POPULATION AB X-ray luminosities of accreting T Tauri stars are observed to be systematically lower than those of nonaccretors. There is as yet no widely accepted physical explanation for this effect, though it has been suggested that accretion somehow suppresses, disrupts or obscures coronal X-ray activity. Here, we suggest that the opposite might be the case: coronal X-rays modulate the accretion flow. We re-examine the X-ray luminosities of T Tauri stars in the Orion Nebula Cluster and find that not only are accreting stars systematically fainter, but that there is a correlation between mass accretion rate and stellar X-ray luminosity. We use the X-ray heated accretion disk models of Ercolano et al. to show that protoplanetary disk photoevaporative mass-loss rates are strongly dependent on stellar X-ray luminosity and sufficiently high to be competitive with accretion rates. X-ray disk heating appears to offer a viable mechanism for modulating the gas accretion flow and could be at least partially responsible for the observed correlation between accretion rates and X-ray luminosities of T Tauri stars. C1 [Drake, Jeremy J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ercolano, Barbara] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Flaccomio, Ettore; Micela, Giusi] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. EM jdrake@cfa.harvard.edu OI Flaccomio, Ettore/0000-0002-3638-5788; Micela, Giuseppina/0000-0002-9900-4751 FU NASA [NAS8-39073]; EU; Ministero dell'Universita' e della Ricerca; ASI/INAF [I/023/05/0] FX J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) during the course of this research and thanks the CXC director, Harvey Tananbaum, and the CXC science team for advice and support. J. J. D. also thanks the EU ISHERPA program for financial support during his visit to the Osservatorio Astronomico di Palermo, and the Osservatorio director, Prof. S. Sciortino, and staff for their help and warm hospitality. E. F. and G. M. acknowledge financial support from the Ministero dell'Universita' e della Ricerca and ASI/INAF Contract I/023/05/0 NR 38 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2009 VL 699 IS 1 BP L35 EP L38 DI 10.1088/0004-637X/699/1/L35 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458KU UT WOS:000267019800009 ER PT J AU Young, M Elvis, M Risaliti, G AF Young, M. Elvis, M. Risaliti, G. TI THE FIFTH DATA RELEASE SLOAN DIGITAL SKY SURVEY/XMM-NEWTON QUASAR SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; quasars: general ID ACTIVE GALACTIC NUCLEI; X-RAY-PROPERTIES; BROAD ABSORPTION-LINE; HIGH-REDSHIFT QUASARS; SEYFERT 1 GALAXIES; CHANDRA MULTIWAVELENGTH PROJECT; PHOTON IMAGING CAMERA; RADIO-QUIET QUASARS; BLACK-HOLE MASS; XMM-NEWTON AB We present a catalog of 792 Fifth Data Release Sloan Digital Sky Survey quasars with optical spectra that have been observed serendipitously in the X-rays with the XMM-Newton. These quasars cover a redshift range of z = 0.11-5.41 and a magnitude range of i = 15.3-20.7. Substantial numbers of radio-loud (70) and broad absorption line (51) quasars exist within this sample. Significant X-ray detections at >= 2 sigma account for 87% of the sample (685 quasars), and 473 quasars are detected at >= 6 sigma, sufficient to allow X-ray spectral fits. For detected sources, similar to 60% have X-ray fluxes between F(2-10) keV = (1-10) x 10(-14) erg cm(-2) s(-1). We fit a single power law, a fixed power law with intrinsic absorption left free to vary, and an absorbed power-law model to all quasars with X-ray signal-to-noise ratio >= 6, resulting in a weighted mean photon index Gamma = 1.91 +/- 0.08, with an intrinsic dispersion sigma(Gamma) = 0.38. For the 55 sources (11.6%) that prefer intrinsic absorption, we find a weighted mean N(H) = 1.5 +/- 0.3 x 10(21) cm(-2). We find that Gamma correlates significantly with optical color, Delta(g - i), the optical-to-X-ray spectral index (alpha(ox)), and the X-ray luminosity. While the first two correlations can be explained as artifacts of undetected intrinsic absorption, the correlation between Gamma and X-ray luminosity appears to be a real physical correlation, indicating a pivot in the X-ray slope. C1 [Young, M.; Elvis, M.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Young, M.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Risaliti, G.] INAF Osservatorio Arcetri, Florence, Italy. RP Young, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM myoung@cfa.harvard.edu OI Risaliti, Guido/0000-0002-3556-977X FU Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U. S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; NASA [NNX07AI22G, NASA GO6-7102X] FX The authors thank the anonymous referee for insightful comments that improved this paper. The authors also thank Gordon Richards for his excellent assistance in navigating the SDSS database. This paper is based on observations obtained with XMM- Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and the Sloan Digital Sky Survey ( SDSS). 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. This research also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has been partially funded by NASA grants NASA NNX07AI22G and NASA GO6-7102X. NR 100 TC 49 Z9 49 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2009 VL 183 IS 1 BP 17 EP 32 DI 10.1088/0067-0049/183/1/17 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 466IY UT WOS:000267656000002 ER PT J AU Dalcanton, JJ Williams, BF Seth, AC Dolphin, A Holtzman, J Rosema, K Skillman, ED Cole, A Girardi, L Gogarten, SM Karachentsev, ID Olsen, K Weisz, D Christensen, C Freeman, K Gilbert, K Gallart, C Harris, J Hodge, P de Jong, RS Karachentseva, V Mateo, M Stetson, PB Tavarez, M Zaritsky, D Governato, F Quinn, T AF Dalcanton, Julianne J. Williams, Benjamin F. Seth, Anil C. Dolphin, Andrew Holtzman, Jon Rosema, Keith Skillman, Evan D. Cole, Andrew Girardi, Leo Gogarten, Stephanie M. Karachentsev, Igor D. Olsen, Knut Weisz, Daniel Christensen, Charlotte Freeman, Ken Gilbert, Karoline Gallart, Carme Harris, Jason Hodge, Paul de Jong, Roelof S. Karachentseva, Valentina Mateo, Mario Stetson, Peter B. Tavarez, Maritza Zaritsky, Dennis Governato, Fabio Quinn, Thomas TI THE ACS NEARBY GALAXY SURVEY TREASURY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: formation; galaxies: stellar content; surveys ID HUBBLE-SPACE-TELESCOPE; RED-GIANT-BRANCH; STAR-FORMATION HISTORY; DWARF IRREGULAR GALAXIES; EDGE-ON GALAXIES; M81 OUTER DISK; STELLAR POPULATIONS; ADVANCED CAMERA; LOCAL GROUP; ARAUCARIA-PROJECT AB The ACS Nearby Galaxy Survey Treasury (ANGST) is a systematic survey to establish a legacy of uniform multi-color photometry of resolved stars for a volume-limited sample of nearby galaxies (D < 4Mpc). The survey volume encompasses 69 galaxies in diverse environments, including close pairs, small and large groups, filaments, and truly isolated regions. The galaxies include a nearly complete range of morphological types spanning a factor of similar to 10(4) in luminosity and star formation rate. The survey data consist of images taken with the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST), supplemented with archival data and new Wide Field Planetary Camera 2 (WFPC2) imaging taken after the failure of ACS. Survey images include wide field tilings covering the full radial extent of each galaxy, and single deep pointings in uncrowded regions of the most massive galaxies in the volume. The new wide field imaging in ANGST reaches median 50% completenesses of m(F475W) = 28.0 mag, m(F606W)= 27.3 mag, and m(F814W) = 27.3 mag, several magnitudes below the tip of the red giant branch (TRGB). The deep fields reach magnitudes sufficient to fully resolve the structure in the red clump. The resulting photometric catalogs are publicly accessible and contain over 34 million photometric measurements of > 14 million stars. In this paper we present the details of the sample selection, imaging, data reduction, and the resulting photometric catalogs, along with an analysis of the photometric uncertainties (systematic and random), for both ACS and WFPC2 imaging. We also present uniformly derived relative distances measured from the apparent magnitude of the TRGB. C1 [Dalcanton, Julianne J.; Williams, Benjamin F.; Rosema, Keith; Gogarten, Stephanie M.; Christensen, Charlotte; Gilbert, Karoline; Hodge, Paul; Governato, Fabio; Quinn, Thomas] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85756 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Skillman, Evan D.; Weisz, Daniel] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Girardi, Leo] Osservatorio Astron Padova INAF, I-35122 Padua, Italy. [Karachentsev, Igor D.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Circes, Russia. [Olsen, Knut] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [de Jong, Roelof S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Freeman, Ken] Australian Natl Univ, Mt Stromlo Observ, Sch Astron & Astrophys, Canberra, ACT 0200, Australia. [Gallart, Carme] Inst Astrofis Canarias, Tenerife 38200, Spain. [Harris, Jason; Zaritsky, Dennis] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Karachentseva, Valentina] Univ Kiel, Astron Observ, UA-254053 Kiev, Ukraine. [Mateo, Mario] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Stetson, Peter B.] Natl Res Council Canada, Herzberg Inst Astrophys, Dominion Astrophys Observ, Victoria, BC V9E 2E7, Canada. [Tavarez, Maritza] Forest Ridge Sch Sacred Heart, Bellevue, WA 98006 USA. RP Dalcanton, JJ (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM jd@astro.washington.edu; ben@astro.washington.edu; aseth@cfa.harvard.edu; adolphin@raytheon.com; holtz@nmsu.edu; krosema@astro.washington.edu; skillman@astro.umn.edu; andrew.cole@utas.edu.au; leo.girardi@oapd.inaf.it; stephanie@astro.washington.edu; ikar@luna.sao.ru; kolsen@noao.edu; dweisz@astro.umn.edu; christensen@astro.washington.edu; kcf@mso.anu.edu.au; carme@iac.es; jharris@as.arizona.edu; dejong@stsci.edu; vkarach@observ.univ.kiev.ua; mmateo@umich.edu; Peter.Stetson@nrc-cnrc.gc.ca; martavbrown@yahoo.com; dennis@fishingholes.as.arizona.edu; fabio@astro.washington.edu; trq@astro.washington.edu OI Cole, Andrew/0000-0003-0303-3855; Gogarten, Stephanie/0000-0002-7231-9745 NR 67 TC 257 Z9 258 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2009 VL 183 IS 1 BP 67 EP 108 DI 10.1088/0067-0049/183/1/67 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 466IY UT WOS:000267656000005 ER PT J AU Riess, AG Macri, L Li, WD Lampeitl, H Casertano, S Ferguson, HC Filippenko, AV Jha, SW Chornock, R Greenhill, L Mutchler, M Ganeshalingham, M Hicken, M AF Riess, Adam G. Macri, Lucas Li, Weidong Lampeitl, Hubert Casertano, Stefano Ferguson, Henry C. Filippenko, Alexei V. Jha, Saurabh W. Chornock, Ryan Greenhill, Lincoln Mutchler, Max Ganeshalingham, Mohan Hicken, Malcolm TI CEPHEID CALIBRATIONS OF MODERN TYPE Ia SUPERNOVAE: IMPLICATIONS FOR THE HUBBLE CONSTANT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; distance scale; galaxies: distances and redshifts; supernovae: general ID LARGE-MAGELLANIC-CLOUD; EXTRAGALACTIC DISTANCE SCALE; PERIOD-LUMINOSITY RELATION; TELESCOPE KEY PROJECT; LIGHT-CURVE SHAPES; GRAVITATIONAL LENSING EXPERIMENT; GALACTIC ABUNDANCE GRADIENT; PHOTOMETRIC STANDARD STARS; AMPLITUDE-COLOR RELATIONS; SPACE-TELESCOPE AB This is the first of two papers reporting measurements from a program to determine the Hubble constant to similar to 5% precision from a refurbished distance ladder. We present new observations of 110 Cepheid variables in the host galaxies of two recent Type Ia supernovae (SNe Ia), NGC 1309 and NGC 3021, using the Advanced Camera for Surveys on the Hubble Space Telescope (HST). We also present new observations of the hosts previously observed with HST whose SNe Ia provide the most precise luminosity calibrations: SN 1994ae in NGC 3370, SN 1998aq in NGC 3982, SN 1990N in NGC 4639, and SN 1981B in NGC 4536, as well as the maser host, NGC 4258. Increasing the interval between observations enabled the discovery of new, longer-period Cepheids, including 57 with P > 60 days, which extend these period-luminosity (P-L) relations. We present 93 measurements of the metallicity parameter, 12 + log[O/H], measured from H II regions in the vicinity of the Cepheids and show these are consistent with solar metallicity. We find the slope of the seven dereddened P-L relations to be consistent with that of the Large Magellanic Cloud Cepheids and with parallax measurements of Galactic Cepheids, and we address the implications for the Hubble constant. We also present multi-band light curves of SN 2002fk (in NGC 1309) and SN 1995al (in NGC 3021) which may be used to calibrate their luminosities. In the second paper, we present observations of the Cepheids in the H band obtained with the Near-Infrared Camera and Multi-Object Spectrometer on HST, further mitigating systematic errors along the distance ladder resulting from dust and chemical variations. The quality and homogeneity of these SN and Cepheid data provide the basis for a more precise determination of the Hubble constant. C1 [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.; Lampeitl, Hubert; Casertano, Stefano; Ferguson, Henry C.; Mutchler, Max] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Macri, Lucas] Texas A&M Univ, George P & Cynthia W Mitchell Inst Fundamental Ph, Dept Phys, College Stn, TX 77843 USA. [Li, Weidong; Filippenko, Alexei V.; Chornock, Ryan; Ganeshalingham, Mohan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lampeitl, Hubert] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Greenhill, Lincoln] Smithsonian Astrophys Observ, Cambridge, MA USA. [Hicken, Malcolm] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Riess, AG (reprint author), Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. EM ariess@stsci.edu OI Macri, Lucas/0000-0002-1775-4859 FU NASA [GO-9352, GO-9728, GO-10189, GO-10339, GO-10497, GO-10802, NAS 5-26555]; NSF [AST-0607485]; TABASGO Foundation; Sun Microsystems, Inc.,; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; US National Science Foundation (NSF); University of California; Sylvia& Jim Katzman Foundation; W. M. Keck Foundation FX We are grateful to Peter Stetson for making his DAOPHOT/ALLFRAME software available. Financial support for this work was provided by NASA through programs GO-9352, GO-9728, GO-10189, GO-10339, GO-10497, and GO-10802 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. A.V.F.'s supernova group at U. C. Berkeley is also supported by NSF grant AST-0607485 and by the TABASGO Foundation. KAIT was constructed and supported by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the US National Science Foundation (NSF), the University of California, the Sylvia& Jim Katzman Foundation, and the TABASGOFoundation. Some of the data presented herein were obtained with 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. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. NR 77 TC 60 Z9 60 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2009 VL 183 IS 1 BP 109 EP 141 DI 10.1088/0067-0049/183/1/109 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 466IY UT WOS:000267656000006 ER PT J AU Peele, AM Burtt, EH Schroeder, MR Greenberg, RS AF Peele, Ashley M. Burtt, Edward H., Jr. Schroeder, Max R. Greenberg, Russell S. TI DARK COLOR OF THE COASTAL PLAIN SWAMP SPARROW (MELOSPIZA GEORGIANA NIGRESCENS) MAY BE AN EVOLUTIONARY RESPONSE TO OCCURRENCE AND ABUNDANCE OF SALT-TOLERANT FEATHER-DEGRADING BACILLI IN ITS PLUMAGE SO AUK LA English DT Article DE bacilli; color; feather-degrading bacteria; Melospiza georgiana; Swamp Sparrow ID BLACK-AND-WHITE; BACTERIAL-DEGRADATION; DIFFERENTIATION; BIRDS AB The Southern Swamp Sparrow (Melospiza georgiana geoigiana) breeds in northeastern North America in montane, freshwater marshes and fens. Its close relative, the Coastal Plain Swamp Sparrow (M. g nigrescens), breeds in northeastern North America, but in coastal salt marshes. Coastal Plain Swamp Sparrows are darker than Southern Swamp Sparrows. Darkly colored feathers are more resistant to bacterial degradation by bacilli, which are unusually salt-tolerant. We tested whether the difference in feather color of the pale montane Southern Swamp Sparrow and the dark Coastal Plain Swamp Sparrow could be an adaptive response to differences in the occurrence and activity of bacilli in habitats that differ in salinity. Southern Swamp Sparrows were Caught and sampled in cranberry fens in western Maryland, whereas Coastal Plain Swamp Sparrows were sampled in salt marshes on the western shore of the Delaware River, just where it broadens into Delaware Bay. The number of birds with feather-degrading bacteria in their plumage was significantly greater among Swamp Sparrows in salt marshes than among those in freshwater fens. The number of colonies of feather-degrading bacilli per bird was also higher for salt-marsh Swamp Sparrows than for those from freshwater fens. We conclude that the dark plumage of Coastal Plain Swamp Sparrows evolved to resist feather-degradation by salt-tolerant bacilli that occur more frequently and abundantly in their plumage than in the pale plumage of the Southern Swamp Sparrow. Received 25 July 2008, accepted 16 January 2009. C1 [Peele, Ashley M.; Burtt, Edward H., Jr.] Ohio Wesleyan Univ, Dept Zool, Delaware, OH 43015 USA. [Schroeder, Max R.] Ohio Wesleyan Univ, Dept Bot Microbiol, Delaware, OH 43015 USA. [Greenberg, Russell S.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Burtt, EH (reprint author), Ohio Wesleyan Univ, Dept Zool, Delaware, OH 43015 USA. EM ehburtt@owu.edu FU Smithsonian Institution; National Science Foundation [BIR-998805, DEB-0543360] FX Our work was supported by a grant from the Smithsonian Institution to A.M.P., by grants from the National Science Foundation (BIR-998805 and DEB-0543360) to E.H.B., and by an REU (Research Experiences for Undergraduates) fellowship to M.R.S. Pacific Coast Feather donated Domestic Goose feathers for Our laboratory experiments. We thank A. L. Downing for her advice on the calculation of species diversity and S. Lender and A. J. Gatz for their advice on our statistical analysis. We also thank J. Goldstein, S. Rohwer, and two anonymous reviewers for suggesting improvements in our final draft. NR 20 TC 17 Z9 17 U1 0 U2 13 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JUL PY 2009 VL 126 IS 3 BP 531 EP 535 DI 10.1525/auk.2009.08142 PG 5 WC Ornithology SC Zoology GA 484BY UT WOS:000269019500007 ER PT J AU Jehl, JR AF Jehl, Joseph R., Jr. TI IN MEMORIAM: ROBERT WINTHROP STORER, 1914-2008 SO AUK LA English DT Biographical-Item C1 Smithsonian Inst, US Museum Nat Hist, Div Birds, Washington, DC 20013 USA. RP Jehl, JR (reprint author), Smithsonian Inst, US Museum Nat Hist, Div Birds, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD JUL PY 2009 VL 126 IS 3 BP 694 EP 696 DI 10.1525/auk.2009.3709 PG 3 WC Ornithology SC Zoology GA 484BY UT WOS:000269019500024 ER PT J AU Bernal, XE Akre, KL Baugh, AT Rand, AS Ryan, MJ AF Bernal, Ximena E. Akre, Karin L. Baugh, Alexander T. Rand, A. Stanley Ryan, Michael J. TI Female and male behavioral response to advertisement calls of graded complexity in tungara frogs, Physalaemus pustulosus SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Call repertoire; Physalaemus pustulosus; Evoked vocal response; Female choice ID SEXUAL SELECTION; NEOTROPICAL FROG; VOCAL BEHAVIOR; BAT PREDATION; PREFERENCES; FREQUENCY; SIGNALS; BIASES; REPERTOIRE; EVOLUTION AB We investigated the natural dynamics in a sexual signal that combines different call components and explored the role of call complexity in sexual selection using a neotropical frog. Male tA(0)ngara frogs, Physalaemus pustulosus, facultatively add up to seven short, multi-harmonic components (chucks) to the simple form of their calls (whines). Female tA(0)ngara frogs are preferentially attracted to whines with chucks over whines without chucks, and males also call more in response to calls containing chucks. Because acoustic predators prefer complex calls, in the context of simple (no chucks) versus complex (any number of chucks) calls, the variably complex call appears to have evolved in response to the opposing selective forces of natural and sexual selection. There is no evidence, however, for the function of increasing the number of chucks within complex calls. We tested two aspects of increasing call complexity: natural patterns of use of call types in males and how both sexes respond to variation in multi-chuck calls. Males incrementally change call complexity by the addition or subtraction of a single chuck and usually do not produce more than two chucks. Variation in call complexity, for calls with at least one chuck, does not influence response calling in males or phonotaxis in females. Our results suggest that one reason for not increasing call complexity beyond a single chuck is the diminishing effectiveness on the responses of both sexes. C1 [Bernal, Ximena E.; Akre, Karin L.; Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol C0930, Austin, TX 78712 USA. [Rand, A. Stanley; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Bernal, XE (reprint author), Texas Tech Univ, Dept Biol Sci, Box 43131, Lubbock, TX 79409 USA. EM ximena.bernal@ttu.edu RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X FU National Science Foundation [IBN 0078150] FX We are grateful to the assistants that helped us record the calls, analyze the recordings, and perform female choice experiments. We are also thankful to J. Christensen- Dalsgaard and two anonymous reviewers whose comments greatly improved this work. The Smithsonian Tropical Research Institute provided critical logistic support. The Autoridad Nacional del Ambiente de Panama provided the permits to perform this research. The frogs were marked following the Guidelines for the Use of Live Amphibians and Reptiles in Field Research compiled by the American Society of Ichthyologists and Herpetologists (ASIH), the Herpetologists' League (HL), and the Society for the Study of Amphibians and Reptiles (SSAR), available at http://www. asih. org/pubs/herpcoll. html. This work was funded by grant IBN 0078150 from the National Science Foundation. The research presented complies with the current laws of the countries in which it was performed. NR 45 TC 27 Z9 27 U1 2 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD JUL PY 2009 VL 63 IS 9 BP 1269 EP 1279 DI 10.1007/s00265-009-0795-5 PG 11 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA 460TZ UT WOS:000267214900003 ER PT J AU Tierney, SM Schwarz, MP AF Tierney, Simon M. Schwarz, Michael P. TI Reproductive hierarchies in the African allodapine bee Allodapula dichroa (Apidae; Xylocopinae) and ancestral forms of sociality SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Allodapini; alloparental care; benefits to group living; body size; caste evolution; developmental ground plan; facultative social behaviour; reproductive queuing; sex allocation ID GENUS MACROGALEA; HYMENOPTERA; EVOLUTION; PHYLOGENETICS; ALLOCATION; PARASITISM; INSIGHTS; INSECT; AGE AB The social organization of allodapine bees has been described in detail for most genera, although there remains a notable gap for one major lineage, the genus Allodapula. Here, we provide the first detailed study of social organization in Allodapula dichroa. Colony sizes are small and the frequency of cooperative nesting is low compared with other allodapine taxa, but there is very clear evidence for reproductive differentiation among adult nestmates. Reproductively dominant females tend to be larger than their nestmates and have much higher levels of wing wear, suggesting that they perform most foraging activities. Multi-female colonies have: (1) lower rates of complete brood absence, suggesting a substantial benefit to cooperative nesting; and (2) larger numbers of brood, suggesting that the presence of a second adult female leads to a greater reproductive output. These data suggest a major phylogenetic split in the form of social organization within the allodapines. In the genus Macrogalea (sister clade to all other allodapines), body size does not preclude young females from laying eggs, and there appears to be, at most, weak reproductive queues. However, in most other allodapines, reproductive hierarchies are prominent and younger and/or smaller females queue for reproductive opportunities, adopt permanently subordinate roles, or disperse. Interestingly, the most common forms of reproductive hierarchies in allodapines do not involve subordinates undertaking foraging roles before reproduction, but instead involve the delaying of both reproduction and foraging. This has implications for the understanding of suggested developmental ground plans in the early stages of social evolution. (C) 2009 The Linnean Society of London, Biological Journal of the Linnean Society, 2009, 97, 520-530. C1 [Tierney, Simon M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Schwarz, Michael P.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. RP Tierney, SM (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM tierneys@si.edu RI Tierney, Simon/H-2410-2015 OI Tierney, Simon/0000-0002-8812-6753 FU Australian Research Council [A19942062] FX We would like to thank Tania Neville and Meg Schwarz for field assistance and the von Buddenbrock family of Ceres for their warm hospitality. Sandra Rehan provided constructive comments on an earlier version of the manuscript and also made her unpublished data available to us. We are also indebted to three anonymous referees, who raised valid queries and provided advice. We are also grateful to Shirley Hanrahan and Robin Crewe for technical support in South Africa. This work was made possible by Australian Research Council funding to M. P. Schwarz and R. Crewe (A19942062). NR 34 TC 8 Z9 8 U1 2 U2 12 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JUL PY 2009 VL 97 IS 3 BP 520 EP 530 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 461ZY UT WOS:000267315700004 ER PT J AU Luther, DA Greenberg, R AF Luther, David A. Greenberg, Russell TI Mangroves: A Global Perspective on the Evolution and Conservation of Their Terrestrial Vertebrates SO BIOSCIENCE LA English DT Article DE mangrove; endemism; vertebrate; coastal ecosystem; biogeography ID TIDAL MARSHES; BIRDS; AUSTRALIA; FOREST; SWAMPS; ORIGIN AB Mangrove ecosystems are found globally along tropical and subtropical coastlines. They exhibit a steep environmental gradient between inland and marine systems, providing a unique, selective environment that shapes local morphological, physiological, and behavioral adaptations. In the first global assessment of terrestrial vertebrate species that are restricted to mangrove ecosystems, we found 48 bird, 14 reptile, I amphibian, and 6 mammal species endemic to mangroves, the majority of which are found in Asia and Australia. We also found that more than 40% Of assessed mangrove-endemic vertebrates are globally threatened. Clearly, additional research is needed to better understand mangrove-endemic vertebrates in order to conserve them. Future research should focus on global inventories, intercontinental comparative work, and the ecology of mangrove-endemic vertebrates. C1 [Luther, David A.] Univ Puerto Rico, San Juan, PR 00936 USA. [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Luther, DA (reprint author), Univ Maryland, Dept Plant Sci & Landscape Architecture, College Pk, MD 20742 USA. EM lutherd@si.edu; greenbergr@si.edu NR 49 TC 33 Z9 37 U1 3 U2 19 PU AMER INST BIOLOGICAL SCI PI WASHINGTON PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA SN 0006-3568 J9 BIOSCIENCE JI Bioscience PD JUL-AUG PY 2009 VL 59 IS 7 BP 602 EP 612 DI 10.1525/bio.2009.59.7.11 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 470ZZ UT WOS:000268022600013 ER PT J AU Dent, DH Burslem, DFRP AF Dent, Daisy H. Burslem, David F. R. P. TI Performance Trade-offs Driven by Morphological Plasticity Contribute to Habitat Specialization of Bornean Tree Species SO BIOTROPICA LA English DT Article DE Biomass allocation; Dipterocarpaceae; edaphic variation; niche partitioning; Southeast Asia ID TROPICAL RAIN-FOREST; CARBOHYDRATE STORAGE; RELATIVE IMPORTANCE; NEOTROPICAL FOREST; NUTRIENT ADDITION; ROOT COMPETITION; SEEDLING GROWTH; HIGH IRRADIANCE; SOIL NUTRIENTS; LIGHT GRADIENT AB Growth-survival trade-offs play an important role in niche differentiation of tropical tree species in relation to light-gradient partitioning. However, the mechanisms that determine differential species performance in response to light and soil resource availability are poorly understood. To examine responses to light and soil nutrient availability, we grew seedlings of five tropical tree species for 12 mo at < 2 and 18 percent full sunlight and in two soil types representing natural contrasts in nutrient availability within a lowland dipterocarp forest in North Borneo. We chose two specialists of nutrient-rich and nutrient-poor soils, respectively, and one habitat generalist. Across all species, growth was higher in high than low light and on more nutrient rich soil. Although species differed in growth rates, the ranking of species, in terms of growth, was consistent across the four treatments. Nutrient-rich soils improved seedling survival and increased growth of three species even under low light. Slower-growing species increased root allocation and reduced specific leaf area (SLA) and leaf area ratio (LAR) in response to decreased nutrient supply. All species increased LAR in response to low light. Maximum growth rates were negatively correlated with survival in the most resource-limited environment. Nutrient-poor soil specialists had low maximum growth rates but high survival at low resource availability. Specialists of nutrient-rich soils, plus the habitat generalist, had the opposite suite of traits. Fitness component trade-offs may be driven by both light and belowground resource availability. These trade-offs contribute to differentiation of tropical tree species among habitats defined by edaphic variation. C1 [Dent, Daisy H.; Burslem, David F. R. P.] Univ Aberdeen, Dept Plant & Soil Sci, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. RP Dent, DH (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. EM daisy.h.dent@gmail.com RI Dent, Daisy/L-3549-2016; OI Dent, Daisy/0000-0002-1219-7344; Burslem, David/0000-0001-6033-0990 FU British Ecological Society FX We thank the Natural Environment Research Council (studentship to DHD) and the British Ecological Society's Overseas Research Programme for financial support. The Economic Planning Unit of the Federal Government of Malaysia kindly granted permission to conduct research in Malaysia. We also thank R. Nilus and C. Maycock for advice and O. Johnny, R. Yudot, and B. Seligi for their contribution to the field and laboratory work in Sepilok. NR 65 TC 31 Z9 31 U1 1 U2 18 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUL PY 2009 VL 41 IS 4 BP 424 EP 434 DI 10.1111/j.1744-7429.2009.00505.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 464VY UT WOS:000267538200005 ER PT J AU Emmons, LH AF Emmons, Louise H. TI Long-Term Variation in Small Mammal Abundance in Forest and Savanna of Bolivian Cerrado SO BIOTROPICA LA English DT Article DE dew; fire; population variation; rodent declines; smoke; species diversity ID BOLOMYS-LASIURUS RODENTIA; NORTHERN-TERRITORY; AMAZONIAN SAVANNA; DECLINING POPULATION; CONSERVATION STATUS; PLAINS VIZCACHA; DYNAMICS; AUSTRALIA; AEROSOLS; CLIMATE AB Small mammals were trapped annually in two savanna and two forest plots in cerrado habitats of Noel Kempff Mercado National Park, Santa Cruz, Bolivia, for 5-10 yr. Eighteen species were captured in forest and seven species in savanna. Species numbers and total number of individuals captured were tightly correlated. In forest, species and abundance varied interannually by up to fourfold in one plot and to 100-fold in the other, and showed alternating highs and lows as is typical for small mammals. The largest faunal differences were due not to site differences, but to year differences, with markedly different patterns in forests and savannas. Abundance was not correlated with rainfall overall, but showed correlation in exceptional years of rainfall and ENSO drought. In savanna, species and overall abundance declined without recovery during 3 yr after reaching minimum numbers in 2004. One species, Cavia aperea, became extinct on both plots, and subsequently, apparently on the entire savanna. Both herbivorous and insectivorous species declined together. Rainfall, fire, and flooding do not seem to account for savanna rodent declines. I propose the novel hypothesis that smoke from anthropogenic burning raises nocturnal temperatures and prevents dew formation, and that a decrease in nightly dry season dewfall has been instrumental in rodent declines. Anecdotal and climatic data are consistent with this hypothesis, but it cannot yet be tested. C1 Smithsonian Inst, Div Mammals NHB390 MRC108, Washington, DC 20013 USA. RP Emmons, LH (reprint author), Smithsonian Inst, Div Mammals NHB390 MRC108, POB 37012, Washington, DC 20013 USA. EM emmonsl@si.edu FU Universidad Autonoma Gabriel Rene Moreno, of Santa Cruz, Bolivia (MNK) FX This project was undertaken in collaboration with the Museo de Historia Natural Noel Kempff Mercado, Universidad Autonoma Gabriel Rene Moreno, of Santa Cruz, Bolivia (MNK). Its staff, students, and associates helped us in innumerable ways, but I especially thank M. Suarez Riglos and I. P. Herrera for encouraging our collaborative studies, and D. Rumiz, K. Rivero, P. Rebolledo, and M. Vargas for expediting our logistics and permits. This project was supported by A. Weedon and the Weedon Foundation, The Douroucouli Foundation, The National Geographic Society, The Wildlife Conservation Society (WCS), and the W. Alton Jones Foundation through Amazon Conservation Association. Part of the study was conducted under a research agreement between WCS and MNK. Permits to conduct studies in PNK were kindly granted by the Servicio Nacional de Areas Protegidas and the Direccion General de Biodiversidad de Bolivia. For their extraordinary efforts under frequently difficult conditions, I thank field assistants F. del Aguila, S. Angulo, S. Cabrera, A. Cespedes, V. Chavez, P. Cuellar, S. Coppeto, N. Rocha, R. Pena, and M. Swarner. I. Phillips and B. Phillips helped with food, fieldwork and logistics, and L.-A. Hayek gave helpful advice on statistics. L. Luna Wong kindly translated the abstract. K. Helgen and two anonymous reviewers made helpful suggestions on the manuscript. NR 43 TC 6 Z9 11 U1 6 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD JUL PY 2009 VL 41 IS 4 BP 493 EP 502 DI 10.1111/j.1744-7429.2009.00500.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 464VY UT WOS:000267538200013 ER PT J AU Braje, TJ Erlandson, JM Rick, TC Dayton, PK Hatch, MBA AF Braje, Todd J. Erlandson, Jon M. Rick, Torben C. Dayton, Paul K. Hatch, Marco B. A. TI Fishing from past to present: continuity and resilience of red abalone fisheries on the Channel Islands, California SO ECOLOGICAL APPLICATIONS LA English DT Article DE archaeology; Channel Islands, California, USA; coastal ecosystem; fishing; Haliotis rufescens; Holocene; kelp forests; marine ecology; middens; red abalone ID SAN-MIGUEL ISLAND; SOUTHERN-CALIFORNIA; SEA OTTERS; HUMAN IMPACTS; KELP FORESTS; ROSA ISLAND; DAISY CAVE; COMMUNITY; COAST; SUSTAINABILITY AB Archaeological data from coastal shell middens provide a window into the structure of ancient marine ecosystems and the nature of human impacts on fisheries that often span millennia. For decades Channel Island archaeologists have studied Middle Holocene shell middens visually dominated by large and often whole shells of the red abalone (Haliotis rufescens). Here we use modern ecological data, historical accounts, commercial red abalone catch records, and zooarchaeological data to examine long-term spatial and temporal variation in the productivity of red abalone fisheries on the Northern Channel Islands, California (USA). Historical patterns of abundance, in which red abalone densities increase from east to west through the islands, extend deep into the Holocene. The correlation of historical and archaeological data argue for long-term spatial continuity in productive red abalone fisheries and a resilience of abalone populations despite dramatic ecological changes and intensive human predation spanning more than 8000 years. Archaeological, historical, and ecological data suggest that California kelp forests and red abalone populations are structured by a complex combination of top-down and bottom-up controls. C1 [Braje, Todd J.] Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. [Dayton, Paul K.; Hatch, Marco B. A.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. RP Braje, TJ (reprint author), Humboldt State Univ, Dept Anthropol, Arcata, CA 95521 USA. EM tjb50@humboldt.edu OI Erlandson, Jon/0000-0002-4705-4319 FU National Science Foundation [BCS-0613982]; Channel Islands National Park (CINP); Marine Conservation Biology Institute; Western National Parks Association FX Our research was supported by the National Science Foundation (BCS-0613982 to T. J. Braje and J. M. Erlandson), Channel Islands National Park (CINP), the Marine Conservation Biology Institute, Western National Parks Association, and our home institutions. At CINP, we thank Ann Huston, Kelly Minas, and Ian Williams for their support. We compiled data from the research of several Channel Island archaeologists; we are grateful to Doug Kennett, Mike Glassow, John Sharp, Pandora Snethkamp, Rene Vellanoweth, Phil Walker, and Lauren Willis. Finally, we thank the anonymous reviewers for comments and assistance in the revision and production of this paper. NR 82 TC 23 Z9 23 U1 7 U2 36 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD JUL PY 2009 VL 19 IS 4 BP 906 EP 919 DI 10.1890/08-0135.1 PG 14 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 448SD UT WOS:000266281400008 PM 19544733 ER PT J AU Graves, GR Romanek, CS AF Graves, Gary R. Romanek, Christopher S. TI Mesoscale patterns of altitudinal tenancy in migratory wood warblers inferred from stable carbon isotopes SO ECOLOGICAL APPLICATIONS LA English DT Article DE altitudinal tenancy; Appalachian Mountains, North Carolina, USA; Black-throated Blue Warbler; Dendroica caerulescens; isotope turnover rates; migratory birds; stable carbon isotopes ID THROATED BLUE WARBLERS; LONG-DISTANCE DISPERSAL; DENDROICA-CAERULESCENS; NEOTROPICAL MIGRANT; SATELLITE TRACKING; BREEDING ORIGINS; WINTER HABITAT; BARN SWALLOWS; HYDROGEN; RATIOS AB We analyzed carbon isotope ratios (delta C-13) of liver and pectoral muscle of Black-throated Blue Warblers (Dendroica caerulescens) to provide a mesoscale perspective on altitudinal tenancy in the Appalachian Mountains, North Carolina, USA. Movements of males are poorly understood, particularly the degree to which yearlings (first breeding season) and older males (second or later breeding season) wander altitudinally during the breeding season. Liver and muscle delta C-13 values of warblers exhibited significant year and altitude effects, but yearling and older males were isotopically indistinguishable. Liver delta C-13 values increased with altitude at the rate of similar to 0.5 parts per thousand per 1000 m. The altitudinal lapse rate of muscle delta C-13 (similar to 1.1 parts per thousand per 1000 m) was nearly identical to the average rate of increase reported in several groups of C-3 plants (similar to 1.1 parts per thousand per 1000 m). This suggests that the majority of males foraged within relatively narrow altitudinal zones during the breeding season. We caution, however, that the discrimination of altitudinal trends in carbon isotope ratios depends on relatively large multiyear samples. Given the scatter in data, it is unlikely that individuals can be accurately assigned to a particular altitude from carbon isotope values. Rapid adjustment of liver and muscle delta C-13 values to local altitudinal environments is consistent with the results of experimental dietary studies that show carbon turnover rates are relatively rapid in small migratory passerines. In a broader context, carbon isotope data have been increasingly used as proxies for wintering habitat use of Nearctic-Neotropical migratory passerines. However, tissues with high metabolic rates are unlikely to retain much isotopic signal of wintering habitat use by the time migrants reach their breeding territories. C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Romanek, Christopher S.] Univ Georgia, Athens, GA 30602 USA. [Romanek, Christopher S.] Savannah River Ecol Lab, Aiken, SC 29802 USA. [Romanek, Christopher S.] Dept Geol, Aiken, SC 29802 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu FU Alexander Wetmore Fund; Biodiversity Surveys and Inventory Program of the National Museum of Natural History, Smithsonian Institution; Department of Energy [DE-FC09-07SR22506] FX We thank Lindy Paddock and Kenneth Cole for laboratory assistance. Seth Newsome, Mike Wunder, and an anonymous reviewer provided cogent reviews. Brian Schmidt, Chris Milensky, Phil Angle, Jim Dean, and Carla Dove prepared specimens, and Joe Bonnette, John Gerwin, Chuck Hunter, Glen McConnell, and Mark Robison helped with permits. Gary R. Graves was supported by the Alexander Wetmore Fund and the Biodiversity Surveys and Inventory Program of the National Museum of Natural History, Smithsonian Institution. Christopher S. Romanek was supported by the Department of Energy under Award Number DE-FC09-07SR22506 to the University of Georgia Research Foundation. Specimens were collected under the auspices of the Animal Care and Use Committee, National Museum of Natural History. Research permits were issued by the U. S. Fish and Wildlife Service, U. S. Forest Service ( Department of Agriculture), and North Carolina Wildlife Resources Commission. NR 85 TC 3 Z9 4 U1 1 U2 15 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD JUL PY 2009 VL 19 IS 5 BP 1264 EP 1273 DI 10.1890/08-0934.1 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 458KW UT WOS:000267020200017 PM 19688933 ER PT J AU Brenes-Arguedas, T Coley, PD Kursar, TA AF Brenes-Arguedas, Tania Coley, Phyllis D. Kursar, Thomas A. TI Pests vs. drought as determinants of plant distribution along a tropical rainfall gradient SO ECOLOGY LA English DT Article DE drought tolerance; herbivory; Panama; pathogen attack; rainfall gradient; tree distribution; tropical forests ID FOREST TREES; HABITAT ASSOCIATIONS; BETA-DIVERSITY; SPECIES DISTRIBUTIONS; FLORISTIC COMPOSITION; GEOGRAPHICAL RANGE; CLIMATIC GRADIENT; NEOTROPICAL TREE; MOIST FOREST; SOIL AB Understanding the mechanisms that shape the distribution of organisms can help explain patterns of local and regional biodiversity and predict the susceptibility of communities to environmental change. In the species-rich tropics, a gradient in rainfall between wet evergreen and dry seasonal forests correlates with turnover of plant species. The strength of the dry season has previously been shown to correlate with species composition. Herbivores and pathogens (pests) have also been hypothesized to be important drivers of plant distribution, although empirical evidence is lacking. In this study we experimentally tested the existence of a gradient in pest pressure across a rainfall gradient in the Isthmus of Panama and measured the influence of pests relative to drought on species turnover. We established two common gardens on the dry and wet sides of the Isthmus using seedlings from 24 plant species with contrasting distributions along the Isthmus. By experimentally manipulating water availability and insect herbivore access, we showed that pests are not as strong a determinant of plant distributions as is seasonal drought. Seasonal drought in the dry site excluded wet-distribution species by significantly increasing their seedling mortality. Pathogen mortality and insect herbivore damage were both higher in the wet site, supporting the existence of a gradient in pest pressure. However, contrary to predictions, we found little evidence that dry-distribution species suffered significantly more pest attack than wet-distribution species. Instead, we hypothesize that dry-distribution species are limited from colonizing wetter forests by their inherently slower growth rates imposed by drought adaptations. We conclude that mechanisms limiting the recruitment of dry-distribution species in wet forests are not nearly as strong as those limiting wet-distribution species from dry forests. C1 [Coley, Phyllis D.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Brenes-Arguedas, Tania; Coley, Phyllis D.; Kursar, Thomas A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Kursar, TA (reprint author), Univ Utah, Dept Biol, 257 S 1400 E, Salt Lake City, UT 84112 USA. EM kursar@biology.utah.edu FU National Science Foundation [DEB-0444590] FX Funding was provided by the National Science Foundation grant DEB-0444590 to T. A. Kursar and P. D. Coley. We thank Cecilia Blundo, Marcos Rios, Gonzalo Rivas, and Natalia Anaya, who conducted the fieldwork. Salomon Aguilar and Rolando Perez helped with species identification. J. Baltzer provided helpful comments on the manuscript. We thank the Smithsonian Tropical Research Institute's Environmental Monitoring Program and the Autoridad del Canal de Panama for making climate data publicly available; similarly the Center for Tropical Forest Science, the Missouri Botanical Gardens, and InBio made species information, herbarium, and distribution maps available. The Peregrine Fund kindly allowed us access to Gunn Hill. The Smithsonian Tropical Research Institute provided logistical support and research facilities. All work was done in compliance with the laws of Panama and the Autoridad Nacional del Ambiente. We dedicate this paper to Elizabeth Leigh who, sharing our appreciation of nature, showed us our first Lafoensia punicifolia. NR 48 TC 24 Z9 25 U1 4 U2 51 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUL PY 2009 VL 90 IS 7 BP 1751 EP 1761 DI 10.1890/08-1271.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 467NO UT WOS:000267745800006 PM 19694125 ER PT J AU Thompson, TW Campbell, BA Ghent, RR Hawke, BR AF Thompson, Thomas W. Campbell, Bruce A. Ghent, Rebecca R. Hawke, B. Ray TI Rugged crater ejecta as a guide to megaregolith thickness in the southern nearside of the Moon SO GEOLOGY LA English DT Article AB The southern highlands of the Moon comprise superposed ejecta layers, individually as thick as a few kilometers, from the major basins. Smaller (1-16-km-diameter) impact craters that penetrate this layered megaregolith and excavate material from depth have radar properties that provide insight into the variability of megaregolith thickness above a postulated basement of large crustal blocks. We observe a significant difference in the population of radar-bright craters, 1-16 km and larger in diameter, between regions of the southeastern nearside highlands north and south of similar to lat 48 degrees S. There are about one-third more radar-bright craters north of this line than to the south, broadly coincident with the mapped boundary between southern deposits mapped as pre-Nectarian age and those of Nectarian-Imbrian age to the north. The radar-bright crater population is consistent with a megaregolith thickness of similar to 1.5 km in the north and similar to 2.5 km in the south, a difference we attribute to South Pole-Aitken basin ejecta. C1 [Thompson, Thomas W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campbell, Bruce A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Ghent, Rebecca R.] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada. [Hawke, B. Ray] Univ Hawaii, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. RP Thompson, TW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 300-227, Pasadena, CA 91109 USA. EM Thomas.W.Thompson@jpl.nasa.gov FU National Science Foundation (NSF); National Aeronautics and Space Administration (NASA) FX We thank the staff at Cornell University, the Arecibo Observatory, and the Robert C. Byrd Green Bank Telescope for invaluable assistance in collecting the new 70 cm lunar radar data. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation (NSF) and with support from the National Aeronautics and Space Administration (NASA). The Green Bank Telescope is part of the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. We thank James W. (Jim) Head and Noah E. Petro for their insightful review comments. This work was supported in part by grants from the NASA Planetary Geology and Geophysics Program. Research by Thompson was carried out at the Jet Propulsion Laboratory, California Institute of Technology, and was sponsored by NASA. NR 18 TC 7 Z9 7 U1 0 U2 3 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD JUL PY 2009 VL 37 IS 7 BP 655 EP 658 DI 10.1130/G25565A.1 PG 4 WC Geology SC Geology GA 462WY UT WOS:000267390100019 ER PT J AU Ewers, RM Scharlemann, JPW Balmford, A Green, RE AF Ewers, Robert M. Scharlemann, Joern P. W. Balmford, Andrew Green, Rhys E. TI Do increases in agricultural yield spare land for nature? SO GLOBAL CHANGE BIOLOGY LA English DT Article DE agricultural intensification; deforestation; food availability; global analysis; land use change ID TROPICAL FOREST; ECONOMIC-DEVELOPMENT; DEFORESTATION RATES; FOOD-PRODUCTION; INTENSIFICATION; BIODIVERSITY; ENVIRONMENT; POLICY; SUSTAINABILITY; CONSERVATION AB Feeding a rapidly expanding human population will require a large increase in the supply of agricultural products during the coming decades. This may lead to the transformation of many landscapes from natural vegetation cover to agricultural land use, unless increases in crop yields reduce the need for new farmland. Here, we assess the evidence that past increases in agricultural yield have spared land for wild nature. We investigated the relationship between the change in the combined energy yield of the 23 most energetically important food crops over the period 1979-1999 and the change in per capita cropland area for 124 countries over the same period. Per capita area of the 23 staple crops tended to decrease in developing countries where large yield increases occurred. However, this was counteracted by a tendency for the area used to grow crops other than staples to increase in the countries where staple crop yields increased. There remained a weak tendency in developing countries for the per capita area of all cropland to decline as staple crop yield increased, a pattern that was most evident in developing countries with the highest per capita food supplies. In developed countries, there was no evidence that higher staple crop yields were associated with decreases in per capita cropland area. This may be because high agricultural subsidies in developed countries override any land-sparing pattern that might otherwise occur. Declines in the area of natural forest were smaller in countries where the yield of staple crops increased most, when the negative effects of human population increases on forest area were controlled for. Our results show that land-sparing is a weak process that occurs under a limited set of circumstances, but that it can have positive outcomes for the conservation of wild nature. C1 [Ewers, Robert M.] Zool Soc London, Inst Zool, London NW1 4RY, England. [Ewers, Robert M.; Balmford, Andrew] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 3EJ, England. [Scharlemann, Joern P. W.] Smithsonian Trop Res Inst, Balboa, Panama. [Green, Rhys E.] Royal Soc Protect Birds, Sandy SG19 2DL, Beds, England. RP Ewers, RM (reprint author), Univ London Imperial Coll Sci Technol & Med, Silwood Pk Campus, Ascot SL5 7PY, Berks, England. EM r.ewers@imperial.ac.uk RI Scharlemann, Jorn/A-4737-2008 OI Scharlemann, Jorn/0000-0002-2834-6367 NR 67 TC 132 Z9 133 U1 17 U2 113 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1354-1013 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JUL PY 2009 VL 15 IS 7 BP 1716 EP 1726 DI 10.1111/j.1365-2486.2009.01849.x PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 454RK UT WOS:000266700000011 ER PT J AU Gladman, BJ Davis, DR Neese, C Jedicke, R Williams, G Kavelaars, JJ Petit, JM Scholl, H Holman, M Warrington, B Esquerdo, G Tricarico, P AF Gladman, Brett J. Davis, Donald R. Neese, Carol Jedicke, Robert Williams, Gareth Kavelaars, J. J. Petit, Jean-Marc Scholl, Hans Holman, Matthew Warrington, Ben Esquerdo, Gil Tricarico, Pasquale TI On the asteroid belt's orbital and size distribution SO ICARUS LA English DT Article DE Asteroids; Collisional physics; Orbit determination ID DIGITAL SKY SURVEY; SURVEY COMMISSIONING DATA; MAIN-BELT; SOLAR-SYSTEM; POPULATION; EVOLUTION; FAMILIES; OBJECTS; MODEL AB For absolute magnitudes greater than the current completeness limit of H-magnitude similar to 15 the main asteroid belt's size distribution is imperfectly known. We have acquired good-quality orbital and absolute H-magnitude determinations for a sample of small main-belt asteroids in order to study the orbital and size distribution beyond H = 15, down to sub-kilometer sizes (H > 18). Based on six observing nights over a 11-night baseline we have detected, measured photometry for, and linked observations of 1087 asteroids which have one-week time baselines or more. The linkages allow the computation of full heliocentric orbits (as opposed to statistical distances determined by some past surveys). judged by known asteroids in the field the typical uncertainty in the (a/e/i) orbital elements is less than 0.03 AU/0.03/0.5 degrees. The distances to the objects are sufficiently well known that photometric uncertainties (of 0.3 magnitudes or better) dominate the error budget of their derived H-magnitudes. The detected asteroids range from H(R) = 12-22 and provide a set of objects down to sizes below 1 km in diameter. We find an on-sky surface density of 210 asteroids per square degree in the ecliptic with opposition magnitudes brighter than m(R) = 23, with the cumulative number of asteroids increasing by a factor of 10(0.27)/mag from m(R) = 18 down to the m(R) similar or equal to 23.5 limit of our survey. In terms of absolute H magnitudes, we find that beyond H = 15 the belt exhibits a constant power-law slope with the number increasing proportional to 10(0.30H) from H similar or equal to 15 to 18, after which incompleteness begins in the survey. Examining only the subset of detections inside 2.5 AU, we find weak evidence for a mildly shallower slope for H = 15-19.5. We provide the information necessary such that anyone wishing to model the main asteroid belt can compare a detailed model to our detected sample. (C) 2009 Elsevier Inc. All rights reserved. C1 [Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Davis, Donald R.; Neese, Carol; Esquerdo, Gil; Tricarico, Pasquale] Planetary Sci Inst, Tucson, AZ 85719 USA. [Jedicke, Robert] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Williams, Gareth] Harvard Smithsonian Ctr Astrophys, IAU Minor Planet Ctr, Cambridge, MA 02138 USA. [Kavelaars, J. J.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Petit, Jean-Marc] Observ Besancon, F-25010 Besancon, France. [Scholl, Hans] Observ Cote Azur, F-06304 Nice 4, France. [Holman, Matthew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Warrington, Ben] Joint Astron Ctr, Hilo, HI 96720 USA. RP Gladman, BJ (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM gladman@astro.ubc.ca FU NSERC; CFI; Canada Research Chairs program for support FX We acknowledge the role of Paolo Farinella in the conception of this research program, and dedicate this paper to his memory. Great thanks are extended to Zeljko Ivezi for his cooperation in diagnosing systematic effects when weak magnitude-dependent efficiencies are present. This work was carried out with support from NASA's Planetary Astronomy program and a time allocation at Kitt Peak National Observatories. BG and BW acknowledge NSERC, CFI, and the Canada Research Chairs program for support. NR 35 TC 38 Z9 38 U1 0 U2 2 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 JUL PY 2009 VL 202 IS 1 BP 104 EP 118 DI 10.1016/j.icarus.2009.02.012 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460ZD UT WOS:000267231000010 ER PT J AU Farmer, AJ AF Farmer, Alison J. TI Saturn in hot water: Viscous evolution of the Enceladus torus SO ICARUS LA English DT Article DE Saturn, magnetospheres; Enceladus; Disks ID VAPOR; MAGNETOSPHERE; MODEL; SPECTRUM; NEPTUNE; COMETS; TRITON; PLUME; ION; OH AB The detection of outgassing water vapor from Enceladus is one of the great breakthroughs of the Cassini mission. The fate of this water once ionized has been widely studied; here we investigate the effects of purely neutral-neutral interactions within the Enceladus torus. We find that, thanks in part to the polar nature of the water molecule, a cold (similar to 180 K) neutral torus would undergo rapid viscous heating and spread to the extent of the observed hydroxyl cloud, before plasma effects become important. We investigate the physics behind the spreading of the torus, paying particular attention to the competition between heating and rotational line cooling. A steady-state torus model is constructed, and it is demonstrated that the torus will be observable in the millimeter band with the upcoming Herschel satellite. The relative strength of rotational lines could be used to distinguish between physical models for the neutral cloud. (C) 2009 Elsevier Inc. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Farmer, AJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM afarmer@cfa.harvard.edu NR 34 TC 19 Z9 19 U1 0 U2 3 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 JUL PY 2009 VL 202 IS 1 BP 280 EP 286 DI 10.1016/j.icarus.2009.02.031 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 460ZD UT WOS:000267231000022 ER PT J AU Horn, JW AF Horn, James W. TI PHYLOGENETICS OF DILLENIACEAE USING SEQUENCE DATA FROM FOUR PLASTID LOCI (rbcL, infA, rps4, rpl16 INTRON) SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Review DE Dilleniaceae; character evolution; molecular systematics; floral morphology ID MOLECULAR-DATA SETS; ANGIOSPERM PHYLOGENY; HIBBERTIA DILLENIACEAE; DNA-SEQUENCES; WOOD ANATOMY; FLOWERING PLANTS; CHLOROPLAST DNA; BASAL EUDICOTS; XYLEM ANATOMY; 18S RDNA AB Dilleniaceae are an angiosperm family consisting of 10-14 genera and; 500 described species, with a pantropical distribution extending into temperate Australia. This study addresses the infrafamilial relationships of Dilleniaceae with nucleotide sequence data from the plastid loci rbcL, infA, rps4, and the rpl16 intron. Analyses of these data using maximum parsimony and Bayesian methods resolve Tetracera, the only pantropical genus in the family, as sister to all other Dilleniaceae. Within the clade of Dilleniaceae exclusive of Tetracera, the New World endemic genera form a clade that is sister to a clade composed of the Old World endemic genera. The latter contains two major subclades: (1) a clade containing Acrotrema, Dillenia, and Schumacheria and (2) a clade containing Hibbertia and its satellite genera, Adrastaea and Pachynema, which are embedded within Hibbertia. Ancestral-state reconstructions of six morphological characters of both biological and taxonomic significance within Dilleniaceae suggest hypotheses of polarity or lability for each that differ substantially from those based on evolutionary trends. Perforation plate-type evolution within Dilleniaceae is equivocal, but the large majority of most parsimonious reconstructions suggest that simple perforation plates are plesiomorphic. Poorly organized leaf venation architecture is synapomorphic for Hibbertia s.l. Floral morphological features classically regarded as primitive, such as exceptionally large numbers of stamens (200+) and numerous carpels (more than isomerous with the corolla), are clearly derived within Dilleniaceae and are features of uncommon occurrence within the family as a whole. Both multicarpellate, synorganized gynoecia and monosymmetric androecia have multiple origins within the family. A new classification of Dilleniaceae is outlined, and nomenclatural changes necessitated by the phylogenetic results are provided. C1 [Horn, James W.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Horn, James W.] Fairchild Trop Bot Garden, Coral Gables, FL 33156 USA. RP Horn, JW (reprint author), Smithsonian Inst, Dept Bot, POB 37012,NMNH MRC 0166, Washington, DC 20013 USA. EM hornj@si.edu FU NSF [DEB 0105089]; A.W. Mellon Foundation; Graduate School of Duke University; Sigma Xi FX I extend my gratitude to Paul S. Manos, who advised this study, in addition to A. Jonathan Shaw, Kathleen Pryer, Bruce Kirchoff, and V. Louise Roth, to whom I am grateful for guidance. W. C. Dickison provided early encouragement. Staff of the Western Australian Herbarium, the Royal Botanic Gardens Sydney, the Queensland Herbarium, the Northern Territory Herbarium, and the IRD Centre in Noumea, New Caledonia, graciously enabled fieldwork. My thanks to the curatorial staff at NY, MO, and US for generously permitting sampling of material critical to this study. W. Burk and K. Wurdack assisted with locating obscure literature. Members of the Manos Lab provided moral support, helpful discussion, and advice. Funding for this research was provided in part by NSF award DEB 0105089 to P. S. Manos, in addition to support from the A.W. Mellon Foundation, the Graduate School of Duke University, and Sigma Xi. NR 116 TC 10 Z9 17 U1 0 U2 15 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD JUL-AUG PY 2009 VL 170 IS 6 BP 794 EP 813 DI 10.1086/599239 PG 20 WC Plant Sciences SC Plant Sciences GA 461QY UT WOS:000267285200009 ER PT J AU Jewgenow, K Neubauer, K Blottner, S Schon, J Wildt, DE Pukazhenthi, BS AF Jewgenow, Katarina Neubauer, Katrin Blottner, Steffen Schoen, Jennifer Wildt, David E. Pukazhenthi, Budhan S. TI Reduced Germ Cell Apoptosis During Spermatogenesis in the Teratospermic Domestic Cat SO JOURNAL OF ANDROLOGY LA English DT Article DE Teratozoospermia; felids; terminal deoxynucleotidyl transferase dUTP nick-end labeling; Caspase-3; antiapoptosis repressor with caspase recruitment domain ID DNA STRAND BREAKS; FELIS-CATUS; SEMINIFEROUS EPITHELIUM; SWIM-UP; TESTIS; SPERM; DEATH; QUALITY; QUANTIFICATION; FRAGMENTATION AB Teratospermia (>60% morphologically abnormal sperm/ejaculate) is associated with increased sperm output in the domestic cat. The objective of this study was to determine whether increased sperm production in teratospermic donors was associated with disturbances in germ cell apoptosis, the usual mechanism for sperm cell elimination. Apoptosis was measured by evaluating DNA fragmentation, expression of Caspase-3, and anti-apoptosis repressor with caspase recruitment domain (ARC) in the testes of normospermic compared with teratospermic cats. Testes (n = 6 males/group) were obtained by bilateral castration and immediately fixed in Bouin solution. Results revealed that greater than 97% of cells labeled as DNA fragmented were tubular regardless of male type. Fewer (P < .05) apoptotic spermatogenic cells per tubule (0.52 +/- 0.11 cells/tubule, <(x)over bar> +/- SEM) and per 100 Sertoli cells (3.79 cells/ 100 Sertoli cells) were observed in teratospermic compared with normospermic (1.25 +/- 0.36 cells/tubule and 6.44 cells/100 Sertoli cells) cats. Among the spermatogenic cells, fewer (P < .03) spermatocytes were positively labeled in teratospermic (0.3 +/- 0.07/tubule) compared with normospermic (0.83 +/- 0.28/tubule) counterparts. Neither donor type differed in Caspase-3 or ARC expression activity. However, each factor was both cell- and stage-specific in expression. Specifically, Caspase-3 was located in Sertoli cells, Aspermatogonia, and round spermatids at stage V. The ARC was found in primary spermatocytes at each stage of the spermatogenic cycle. These results demonstrate that the high incidence of morphologically abnormal sperm in teratospermic male cats is accompanied by a reduced elimination of defective spermatogenic cells via apoptosis. C1 [Jewgenow, Katarina; Neubauer, Katrin; Blottner, Steffen] Leibniz Inst Zoo & Wildlife Res IZW, Dept Reprod Biol, D-10252 Berlin, Germany. [Schoen, Jennifer] Free Univ Berlin, Inst Vet Biochem, D-1000 Berlin, Germany. [Wildt, David E.; Pukazhenthi, Budhan S.] Smithsonians Natl Zool Pk Conservat & Res Ctr, Dept Reprod Sci, Ctr Species Survival, Front Royal, VA USA. RP Jewgenow, K (reprint author), Leibniz Inst Zoo & Wildlife Res IZW, Dept Reprod Biol, PF 601103, D-10252 Berlin, Germany. EM Jewgenow@izw-berlin.de FU Deutsche Forschungsgemeinschaft [DFG Je 163/9-1] FX Supported by Deutsche Forschungsgemeinschaft DFG Je 163/9-1 and Scho 1231/2-1 and the Friends of the National Zoo. NR 39 TC 10 Z9 10 U1 0 U2 2 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 EI 1939-4640 J9 J ANDROL JI J. Androl. PD JUL-AUG PY 2009 VL 30 IS 4 BP 460 EP 468 DI 10.2164/jandrol.108.006726 PG 9 WC Andrology SC Endocrinology & Metabolism GA 469NG UT WOS:000267905700017 PM 19201698 ER PT J AU Powers, JS Montgomery, RA Adair, EC Brearley, FQ DeWalt, SJ Castanho, CT Chave, J Deinert, E Ganzhorn, JU Gilbert, ME Gonzalez-Iturbe, JA Bunyavejchewin, S Grau, HR Harms, KE Hiremath, A Iriarte-Vivar, S Manzane, E de Oliveira, AA Poorter, L Ramanamanjato, JB Salk, C Varela, A Weiblen, GD Lerdau, MT AF Powers, Jennifer S. Montgomery, Rebecca A. Adair, E. Carol Brearley, Francis Q. DeWalt, Saara J. Castanho, Camila T. Chave, Jerome Deinert, Erika Ganzhorn, Joerg U. Gilbert, Matthew E. Antonio Gonzalez-Iturbe, Jose Bunyavejchewin, Sarayudh Grau, H. Ricardo Harms, Kyle E. Hiremath, Ankila Iriarte-Vivar, Silvia Manzane, Eric de Oliveira, Alexandre A. Poorter, Lourens Ramanamanjato, Jean-Baptiste Salk, Carl Varela, Amanda Weiblen, George D. Lerdau, Manuel T. TI Decomposition in tropical forests: a pan-tropical study of the effects of litter type, litter placement and mesofaunal exclusion across a precipitation gradient SO JOURNAL OF ECOLOGY LA English DT Article DE above ground; below ground; climate decomposition index; decomposition; decomposer fauna; litter type; precipitation; tropical forests ID HAWAIIAN MONTANE FORESTS; TERRESTRIAL ECOSYSTEMS; LEAF DECOMPOSITION; RAIN-FOREST; ROOT DECOMPOSITION; PLANT LITTER; SOIL; CLIMATE; RATES; QUALITY AB 1. Litter decomposition recycles nutrients and causes large fluxes of carbon dioxide into the atmosphere. It is typically assumed that climate, litter quality and decomposer communities determine litter decay rates, yet few comparative studies have examined their relative contributions in tropical forests. 2. We used a short-term litterbag experiment to quantify the effects of litter quality, placement and mesofaunal exclusion on decomposition in 23 tropical forests in 14 countries. Annual precipitation varied among sites (760-5797 mm). At each site, two standard substrates (Raphia farinifera and Laurus nobilis) were decomposed in fine- and coarse-mesh litterbags both above and below ground for approximately 1 year. 3. Decomposition was rapid, with >95% mass loss within a year at most sites. Litter quality, placement and mesofaunal exclusion all independently affected decomposition, but the magnitude depended upon site. Both the average decomposition rate at each site and the ratio of above- to below-ground decay increased linearly with annual precipitation, explaining 60-65% of among-site variation. Excluding mesofauna had the largest impact on decomposition, reducing decomposition rates by half on average, but the magnitude of decrease was largely independent of climate. This suggests that the decomposer community might play an important role in explaining patterns of decomposition among sites. Which litter type decomposed fastest varied by site, but was not related to climate. 4. Synthesis. A key goal of ecology is to identify general patterns across ecological communities, as well as relevant site-specific details to understand local dynamics. Our pan-tropical study shows that certain aspects of decomposition, including average decomposition rates and the ratio of above- to below-ground decomposition are highly correlated with a simple climatic index: mean annual precipitation. However, we found no relationship between precipitation and effects of mesofaunal exclusion or litter type, suggesting that site-specific details may also be required to understand how these factors affect decomposition at local scales. C1 [Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav & Plant Biol, St Paul, MN 55108 USA. [Brearley, Francis Q.] Manchester Metropolitan Univ, Dept Geog & Environm Sci, Manchester M1 5GD, Lancs, England. [DeWalt, Saara J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Castanho, Camila T.; de Oliveira, Alexandre A.] Univ Sao Paulo, Inst Biociencias, Sao Paulo, Brazil. [Chave, Jerome] CNRS UPS, Lab Evolut & Divers Biol, UMR5174, F-31062 Toulouse, France. [Deinert, Erika] Org Trop Studies, San Jose, Costa Rica. [Ganzhorn, Joerg U.] Univ Hamburg, Dept Anim Ecol & Conservat, D-20146 Hamburg, Germany. [Gilbert, Matthew E.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Antonio Gonzalez-Iturbe, Jose] Biocenosis AC, Merida 97134, Yucatan, Mexico. [Bunyavejchewin, Sarayudh] Natl Pk, Wildlife & Plant Conservat Dept, Res Off, Bangkok 10900, Thailand. [Grau, H. Ricardo] Univ Nacl Tucuman, Fac Ciencias Nat, Conicet Liey, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hiremath, Ankila] ATREE, New Delhi 110014, India. [Iriarte-Vivar, Silvia] Ctr Invest Cient Yucatan AC, Unidad Recursos Nat, Merida, Yucatan, Mexico. [Manzane, Eric] Univ Miami, Dept Biol, Coral Gables, FL 33146 USA. [Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Resource Ecol Grp, NL-6700 AA Wageningen, Netherlands. [Poorter, Lourens] Inst Boliviano Invest Forestal, Casilla 6204, Santa Cruz, Bolivia. [Ramanamanjato, Jean-Baptiste] QIT Madagascar Minerals, Tolagnaro 614, Madagascar. [Salk, Carl] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Varela, Amanda] Pontificia Univ Javeriana, Lab Ecol Suelos & Hongos Trop, Unidad Ecol & Sistemat, Dept Biol,Fac Ciencias, Bogota, Colombia. [Weiblen, George D.] Univ Minnesota, Plant Biol & Bell Museum Nat Hist, St Paul, MN 55108 USA. [Lerdau, Manuel T.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Lerdau, Manuel T.] Univ Virginia, Dept Biol, Charlottesville, VA 22904 USA. RP Powers, JS (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav & Plant Biol, St Paul, MN 55108 USA. EM powers@umn.edu RI Castanho, Camila/D-4583-2012; Oliveira, Alexandre/G-8830-2012; Montgomery, Rebecca/J-5774-2013; Lerdau, Manuel/E-7320-2011; OI Oliveira, Alexandre/0000-0001-5526-8109; Montgomery, Rebecca/0000-0002-4131-1847; Lerdau, Manuel/0000-0003-1864-0834; Salk, Carl/0000-0003-2833-8292 FU Comparative Tropical Biology Fellowship; Mellon Foundation; NSF [DBI-0338143] FX This study was funded by a Comparative Tropical Biology Fellowship to J.S.P. and R.A.M. from the Organization for Tropical Studies funds from the Mellon Foundation to M.T.L. and an Fellowship NSF ADVANCE (DBI-0338143) to J.S.P. We thank Marie Tiffin and Tom Savre for helping to fill litter bags and Janneke HilleRisLambers and Kit Bingham for statistical advice. Many thanks go to Justin Becknell for preparing the map of the sites. Many people from all over the world helped with data collection, and we thank them all: Brus Isua of New Guinea Binatang Research Center, Ana Horta in Argentina, Rebecca Ostertag at University of Hawaii at Hilo, Rivo A. Rajoharison of QMM (Madagascar), G. Vanaraj at ATREE (Bangalore, India), Kursani of Project Barito Ulu (Indonesia), Marco Vinisio Martinez at Pontificia Universidad Javeriana (Bogotu, Colombia), and Gerardo Polanco Hernundez in CICY, Yucatun (Mexico). We thank the Karnataka and Tamil Nadu Forest Departments for permission to work in BIL and KAL, and MINAE for permission to work in LAS, STR, PAL and SIR. We especially thank two anonymous referees, Peter Tiffin and Hans Cornelissen for comments that improved this manuscript. NR 57 TC 86 Z9 93 U1 9 U2 116 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD JUL PY 2009 VL 97 IS 4 BP 801 EP 811 DI 10.1111/j.1365-2745.2009.01515.x PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 459AG UT WOS:000267071500021 ER PT J AU Briceno, RD Eberhard, WG AF Briceno, R. D. Eberhard, W. G. TI Experimental modifications imply a stimulatory function for male tsetse fly genitalia, supporting cryptic female choice theory SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE tsetse fly; cryptic female choice; genital function; sexual selection ID MALE FERTILIZATION SUCCESS; GLOSSINA-MORSITANS; MATING-BEHAVIOR; MORPHOLOGY; OVULATION; FLIES; SELECTS; BEETLE AB One of the most sweeping of all patterns in morphological evolution is that animal genitalia tend to diverge more rapidly than do other structures. Abundant indirect evidence supports the cryptic female choice (CFC) explanation of this pattern, which supposes that male genitalia often function to court females during copulation; but direct experimental demonstrations of a stimulatory function have been lacking. In this study, we altered the form of two male genital structures that squeeze the female's abdomen rhythmically in Glossina pallidipes flies. As predicted by theory, this induced CFC against the male: ovulation and sperm storage decreased, while female remating increased. Further experiments showed that these effects were due to changes in tactile stimuli received by the female from the male's altered genitalia, and were not due to other possible changes in the males due to alteration of their genital form. Stimulation from male genital structures also induces females to permit copulation to occur. Together with previous studies of tsetse reproductive physiology, these data constitute the most complete experimental confirmation that sexual selection (probably by CFC) acts on the stimulatory properties of male genitalia. C1 [Briceno, R. D.; Eberhard, W. G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. [Eberhard, W. G.] Smithsonian Trop Res Inst, Balboa, Panama. RP Eberhard, WG (reprint author), Univ Costa Rica, Escuela Biol, Ciudad Univ, San Jose, Costa Rica. EM william.eberhard@gmail.com FU IAEA; STRI; Univ. de Costa Rica FX We thank the International Atomic Energy Agency for the use of flies and facilities, John Christy, David Shuker, and Mary Jane West-Eberhard for comments on the ms, and Andrew Parker, Rudolf Boigner and Mark Vreysen for other help; the IAEA, STRI, and the Univ. de Costa Rica provided financial support. NR 28 TC 25 Z9 26 U1 1 U2 21 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUL PY 2009 VL 22 IS 7 BP 1516 EP 1525 DI 10.1111/j.1420-9101.2009.01761.x PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 459SM UT WOS:000267129500014 PM 19467130 ER PT J AU Winter, K Garcia, M Holtum, JAM AF Winter, Klaus Garcia, Milton Holtum, Joseph A. M. TI Canopy CO2 exchange of two neotropical tree species exhibiting constitutive and facultative CAM photosynthesis, Clusia rosea and Clusia cylindrica SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE Clusia cylindrica; Clusia rosea; CO2 exchange; constitutive CAM; crassulacean acid metabolism; facultative CAM; photosynthetic pathway; tree canopy; whole-plant physiology ID CRASSULACEAN-ACID-METABOLISM; PLANT KALANCHOE-DAIGREMONTIANA; CARBON-DIOXIDE ASSIMILATION; COMOSUS L MERR; MESEMBRYANTHEMUM-CRYSTALLINUM; ISOTOPE COMPOSITION; GAS-EXCHANGE; DELTA-C-13 VALUES; PINEAPPLE PLANTS; WATER AB Photon flux density (PFD) and water availability, the daily and seasonal factors that vary most in tropical environments, were examined to see how they influenced expression of crassulacean acid metabolism (CAM) in 3-year-old Clusia shrubs native to Panama. Instead of the commonly used single-leaf approach, diel CO2 exchange was measured for whole individual canopies of plants in large soil containers inside a naturally illuminated 8.8 m(3) chamber. In well-watered C. rosea, a mainly constitutive CAM species, nocturnally fixed CO2 contributed about 50% to 24 h carbon gain on sunny days but the contribution decreased to zero following overcast days. Nonetheless, CO2 fixation in the light responded in such a way that 24 h carbon gain was largely conserved across the range of daily PFDs. The response of C. rosea to drought was similarly buffered. A facultative component of CAM expression led to reversible increases in nocturnal carbon gain that offset drought-induced reductions of CO2 fixation in the light. Clusia cylindrica was a C-3 plant when well-watered but exhibited CAM when subjected to water stress. The induction of CAM was fully reversible upon rewatering. C. cylindrica joins C. pratensis as the most unambiguous facultative CAM species reported in the genus Clusia. C1 [Winter, Klaus; Garcia, Milton] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Holtum, Joseph A. M.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. RP Winter, K (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM winterk@si.edu RI Holtum, Joseph/B-3063-2012 OI Holtum, Joseph/0000-0001-6568-8019 FU Smithsonian Tropical Research Institute; JCU Special Studies Programme grant FX We thank Jorge Aranda and Aurelio Virgo for technical assistance. We acknowledge assistance from Li-Cor in deriving the equations used to calculate CO2 fluxes inside a closed chamber using the LI-7500 open-path analyser. The research was funded by the Smithsonian Tropical Research Institute. JAMH was supported by a JCU Special Studies Programme grant. NR 48 TC 11 Z9 12 U1 1 U2 21 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 J9 J EXP BOT JI J. Exp. Bot. PD JUL PY 2009 VL 60 IS 11 BP 3167 EP 3177 DI 10.1093/jxb/erp149 PG 11 WC Plant Sciences SC Plant Sciences GA 478KX UT WOS:000268588300020 PM 19487388 ER PT J AU Misner, LM Halvorson, AC Dreier, JL Ubelaker, DH Foran, DR AF Misner, Lisa M. Halvorson, Andrea C. Dreier, Jennifer L. Ubelaker, Douglas H. Foran, David R. TI The Correlation Between Skeletal Weathering and DNA Quality and Quantity SO JOURNAL OF FORENSIC SCIENCES LA English DT Article; Proceedings Paper CT 57th Annual Meeting of the American-Academy-of-Forensic-Sciences CY FEB 21-26, 2005 CL New Orleans, LA SP Amer Acad Forens Sci DE forensic science; mitochondrial DNA; bone; DNA degradation; human skeletal remains; Voegtly Cemetery; skeletal weathering ID ANCIENT DNA; MITOCHONDRIAL-DNA; MASS GRAVES; IDENTIFICATION; REMAINS; VICTIMS AB Mitochondrial DNA analysis of skeletal material is invaluable in forensic identification, although results can vary widely among remains. Previous studies have included bones of different ages, burial conditions, and even species. In the research presented, a collection of human remains that lacked major confounders such as burial age, interment style, and gross environmental conditions, while displaying a very broad range of skeletal degradation, were examined for both mitochondrial DNA (mtDNA) quality and quantity. Overall skeletal weathering, individual bone weathering, and bone variety were considered. Neither skeletal nor bone weathering influenced DNA quality or quantity, indicating that factors that degrade bone do not have the same effect on DNA. In contrast, bone variety, regardless of weathering level, was a significant element in DNA amplification success. Taken together, the results indicate that neither skeletal nor individual bone appearance are reliable indicators of subsequent mtDNA typing outcomes, while the type of bone assayed is. C1 [Misner, Lisa M.; Halvorson, Andrea C.; Foran, David R.] Michigan State Univ, Sch Criminal Justice, Forens Sci Program, E Lansing, MI 48824 USA. [Foran, David R.] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. [Ubelaker, Douglas H.] NMNH, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Dreier, Jennifer L.] George Washington Univ, Dept Forens Sci, Washington, DC 20052 USA. RP Foran, DR (reprint author), Michigan State Univ, Sch Criminal Justice, Forens Sci Program, 560 Baker Hall, E Lansing, MI 48824 USA. EM foran@msu.edu NR 25 TC 21 Z9 21 U1 0 U2 5 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD JUL PY 2009 VL 54 IS 4 BP 822 EP 828 DI 10.1111/j.1556-4029.2009.01043.x PG 7 WC Medicine, Legal SC Legal Medicine GA 462BU UT WOS:000267321100011 PM 19368622 ER PT J AU Renner, SC Rasmussen, PC Rappole, JH Aung, T Aung, M AF Renner, Swen C. Rasmussen, Pamela C. Rappole, John H. Aung, Thein Aung, Myint TI Discovery of the Large Blue Flycatcher Cyornis [banyumas] magnirostris breeding in northern Kachin State (Burma/Myanmar) and taxonomic implications for the Cyornis-group SO JOURNAL OF ORNITHOLOGY LA English DT Article DE Cyornis banyumas; Cyornis magnirostris; Burma; Biogeography; Flycatcher; Myanmar; SE Aisa; Taxonomy AB The little-known taxon Cyornis [banyumas] magnirostris has long been treated as a race of the widespread Hill Blue Flycatcher C. banyumas, with which it was thought to be allopatric during the breeding season. On the basis of morphology, magnirostris has lately been considered a full species, endemic as a breeder to northeastern India. Our recent field work during migration and the breeding season (September 2005 and June-July 2006) has, however, resulted in the first records of magnirostris from northern Burma/Myanmar, establishing that its breeding range broadly overlaps the range of C. banyumas whitei. We demonstrate how historical factors, sources of error, including fraud, errors of omission and commission, and inferences based on lack of data have all negatively affected assessment of species limits and conservation status in this speciose group of flycatchers. We also provide evidence that the taxon C. [banyumas] lemprieri is highly distinct and should be treated as a full species. C1 [Renner, Swen C.; Rappole, John H.] Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Rasmussen, Pamela C.] Michigan State Univ Museum, Dept Zool, E Lansing, MI 48824 USA. [Aung, Thein; Aung, Myint] W Gyogone Insein, Nat & Wildlife Conservat Div, Dept Forestry, Yangon, Myanmar. RP Renner, SC (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM renners@si.edu; rasmus39@msu.edu RI Renner, Swen/J-3502-2014 OI Renner, Swen/0000-0002-6893-4219 NR 29 TC 1 Z9 3 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 J9 J ORNITHOL JI J. Ornithol. PD JUL PY 2009 VL 150 IS 3 BP 671 EP 683 DI 10.1007/s10336-009-0395-1 PG 13 WC Ornithology SC Zoology GA 462YH UT WOS:000267394400016 ER PT J AU Barrows, EM Flint, OS AF Barrows, Edward M. Flint, Oliver S., Jr. TI Mecopteran (Mecoptera: Bittacidae, Meropeidae, Panorpidae) Flight Periods, Sex Ratios, and Habitat Frequencies in a United States Mid-Atlantic Freshwater Tidal Marsh, Low Forest, and Their Ecotone SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article DE Bittacidae; deciduous forest; earwigflies; hangingflies; Meropeidae; Panorpidae; phenology; scorpionflies; sex ratios; tidal freshwater marsh ID BIOLOGY AB As part of a long-term arthropod biodiversity study, we operated six Malaise traps in Dyke Marsh Wildlife Preserve (DMWP), Virginia from April 1998 through December 1999 and obtained 104 adult mecopterans in five species. They were present in samples from late May through early November. Samples indicate that as a group, the mecopterans were more abundant in the forest than in the marsh and the forest-marsh ecotone, and the mecopterans had a female-biased sex ratio. Two of the trapped species are uncommon or of limited distribution in North America. Malaise traps can be used efficiently to survey and monitor certain mecopteran species in DMWP and similar places. To understand the mecopteran biodiversity and phenology in the Preserve more completely, it would be worthwhile to survey the entire Preserve for at least 10 yr with all appropriate sampling methods. C1 [Barrows, Edward M.] Georgetown Univ, Dept Biol, Lab Entomol & Biodivers, Washington, DC 20057 USA. [Flint, Oliver S., Jr.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Barrows, EM (reprint author), Georgetown Univ, Dept Biol, Lab Entomol & Biodivers, Reiss Bldg Suite 406,Box 571229, Washington, DC 20057 USA. EM barrowse@georgetown.edu; flinto@si.edu NR 17 TC 5 Z9 5 U1 0 U2 1 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2009 VL 82 IS 3 BP 223 EP 230 PG 8 WC Entomology SC Entomology GA 536YN UT WOS:000273079900002 ER PT J AU Sanchez, E Gallery, R Dalling, JW AF Sanchez, Evelyn Gallery, Rachel Dalling, James W. TI Importance of nurse logs as a substrate for the regeneration of pioneer tree species on Barro Colorado Island, Panama SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE seed germination; seedling establishment; seedling growth; species coexistence; treefall gap; wood ID GAP-PHASE REGENERATION; COARSE WOODY DEBRIS; PICEA-ABIES FOREST; TROPICAL FOREST; RAIN-FOREST; SEEDLING ESTABLISHMENT; RECRUITMENT LIMITATION; TSUGA-HETEROPHYLLA; NEOTROPICAL FOREST; CLOUD FOREST AB Fallen tree trunks ('nurse logs') are important recruitment sites for trees in temperate forest, however nurse log use is seldom reported in tropical forests. We predicted that logs should be important for the regeneration of small-seeded tropical pioneer species because surface leaf litter and competition with established vegetation reduces the establishment success of these species from soil seed banks. In a survey oil Barre, Colorado Island, Panama, we found that pioneer seedlings were present oil logs in 40 of 95 recent treefall gaps. In gaps where seedlings were present oil logs, seedling density was not significantly different from adjacent areas of soil. However, species composition was significantly different: logs were disproportionately colonized by smaller-seeded and wind-dispersed species. In growing-house experiments using 1.2 species. we found that wood substrate had little effect: oil seed germination. In contrast, seedling growth was 50%, lower on decayed wood than soil. Furthermore, species growth rates on wood were not significantly correlated with growth rates in soil (df = 10, r = 0.48). If establishment on logs eventually leads to recruitment to the forest canopy, then logs may promote the maintenance of diversity by favouring a different group of species from those that recruit in Soil. C1 [Sanchez, Evelyn; Dalling, James W.] Smithsonian Trop Res Inst, Balboa, Panama. [Gallery, Rachel; Dalling, James W.] Univ Illinois, Program Ecol & Evolutionary Biol, Urbana, IL 61801 USA. [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Dalling, JW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM dallingj@life.uiuc.edu FU Smithsonian Tropical Research Institute (STRI); National Science Foundation [0342925] FX f This research was funded by a Short-Term Fellowship from the Smithsonian Tropical Research Institute (STRI) to ES and a National Science Foundation Grant DEB 034292 5 to JWD. We thank Guadalupe Alvarado, Dora Alvarez, Osvaldo Calderon, Carlos Sanchez, Luis Ramirez, Rodolfo Rojas and Salomon Aguilar for assistance in the field and lab, Chris Peterson for comments on the manuscript. and STRI and Oris Acevedo for logistic support. NR 52 TC 7 Z9 7 U1 0 U2 15 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 JUL PY 2009 VL 25 BP 429 EP 437 DI 10.1017/S0266467409006130 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 461CR UT WOS:000267242600008 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Oxford Dictionary of Contemporary World History: From 1900 to Present Day, 3rd edition SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400267 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The History of Japan SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400268 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI A Brief History of Ireland SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400269 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The History of Peru SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400266 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Guide to Guinness Collectables SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400265 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Kings and Queens of Britain, 2nd edition SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400263 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Tracing Your Irish Family History SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400262 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI What the Slaves Ate: Recollections of African American Foods and Foodways from the Slave Narratives SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 1 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 JUL PY 2009 VL 134 IS 12 BP 124 EP 124 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 469AG UT WOS:000267866400264 ER PT J AU Brownell, RL Ralls, K Baumann-Pickering, S Poole, MM AF Brownell, Robert L., Jr. Ralls, Katherine Baumann-Pickering, Simone Poole, M. Michael TI Behavior of melon-headed whales, Peponocephala electra, near oceanic islands SO MARINE MAMMAL SCIENCE LA English DT Article DE melon-headed whales; Peponocephala electra; mass-stranding; mid-frequency sonar; behavior; lunar cycles; Hanalei Bay; Hatihue Bay; Sasanhaya Bay ID SPINNER DOLPHIN; CETACEANS; PACIFIC; ECOLOGY AB Southall et al. (2006) concluded that a near mass stranding (MS) of melon-headed whales (MHWs), Peponocephala electra, in Hanalei Bay, Kauai, Hawaii, on 3-4 July 2004, was likely related to the operation of mid-frequency sonars (MFS). However, subsequent authors argued that the nearly simultaneous entry of MHWs into Sasanhaya Bay, Rota (similar to 5,740 km away) made this conclusion untenable. They suggested that both sightings, and other MSs of MHWs, could be related to lunar cycles. To resolve this question, we reviewed information on the biology and behavior of MHWs and compared the two sightings to observations of MHWs around Palmyra Atoll and Nuku Hiva, French Polynesia. We also tested for a relationship between observations and MSs of MHWs with lunar cycles. MHWs near many oceanic islands rest nearshore during the day and feed offshore in deeper water at night. The MHWs at Rota exhibited normal diurnal resting behavior as seen at Palmyra and Nuku Hiva, while those at Kauai showed milling behavior typically seen prior to MS events. Thus, these events were not similar. Neither observations nor MSs of MHWs were related to lunar cycles. Our review of MHW behavior strengthens the case that MFS use played a major role in the near MS in Hanalei Bay. C1 [Brownell, Robert L., Jr.] NOAA Fisheries, SW Fisheries Sci Ctr, Pacific Grove, CA 93959 USA. [Ralls, Katherine] Smithsonian Inst, Natl Zool Pk, Washington, DC 20013 USA. [Baumann-Pickering, Simone] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Poole, M. Michael] Marine Mammal Res Program, Moorea 98728, Fr Polynesia. RP Brownell, RL (reprint author), NOAA Fisheries, SW Fisheries Sci Ctr, 1352 Lighthouse Ave, Pacific Grove, CA 93959 USA. EM robert.brownell@noaa.gov FU Vista Press; National Oceanic Society; Engelhard Foundation FX We thank Robert Braun for many helpful discussions about the Hanalei Bay, Kauai, sighting; Mark Michael and Monty Keel for providing details and photographs of the Rota sighting, Nicole Richardot for photos and video of the Nuku Hiva event, Xavier Curvat of the Centre de Plongee Marquises, for his records of killer whale sightings at Nuku Hiva from 1998 to 2005, Patrick Guennou of the Ouvrage Carte Instrument of the Fench Navy base in Papeete for providing charts of Nuku Hiva, and Chloe and Robin Meadows for help with translations from French. Robin Baird, Douglas DeMaster, John Hildebrand, Mark McDonald, William F. Perrin, and an anonymous reviewer made useful comments on the manuscript. SB's work at Palmyra was funded by the University of California San Diego and NOAA's Pacific Islands Fisheries Science Center. MMP's work in French Polynesia was conducted under permit from French Polynesia's Ministry of the Environment and was funded by Vista Press, the National Oceanic Society, and the Engelhard Foundation. NR 44 TC 18 Z9 20 U1 4 U2 12 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JUL PY 2009 VL 25 IS 3 BP 639 EP 658 DI 10.1111/j.1748-7692.2009.00281.x PG 20 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 471CE UT WOS:000268031000009 ER PT J AU Apeti, DA Lauenstein, GG Riedel, GF AF Apeti, Dennis A. Lauenstein, Gunnar G. Riedel, Gerhardt F. TI Cadmium distribution in coastal sediments and mollusks of the US SO MARINE POLLUTION BULLETIN LA English DT Article DE Cadmium; Salinity; Diagenesis; Upwelling; Estuary; Mussel Watch ID OYSTERS CRASSOSTREA-VIRGINICA; TRACE-METALS; CHEMICAL CONCENTRATIONS; ESTUARINE SEDIMENTS; CONTINENTAL-MARGIN; LITTORINA-LITTOREA; MYTILUS-EDULIS; UNITED-STATES; ACCUMULATION; SALINITY AB Cadmium (Cd) concentrations in the coastal United States were assessed using the National Status and Trends (NS&T) Mussel Watch dataset, which is based on the analysis of sediments and bivalves collected from 280 sites since 1986. Using the 1997 sediment data, Pearson correlation (r = 0.44, p < 0.0001) suggested that Cd distributions in sediment can, be to some extent, explained by the proximity of sites to population centers. The 2003 tissue data indicated that "high" Cd concentrations (greater than 5.6 mu g/g dry weights [dw] for mussel and 5.4 mu g/g dw for oysters) were related to salinity along the East and Gulf coasts. Along the West coast, however, these "high" sites appeared to be related to upwelling phenomenon. Additionally, sedimentary diagenesis was found to be the most likely explanation of why sediment and mollusk Cd content were not well correlated. Published by Elsevier Ltd. C1 [Apeti, Dennis A.; Lauenstein, Gunnar G.] NOAA, Natl Ctr Coastal & Ocean Sci, Ctr Coastal Monitoring & Assessment, Silver Spring, MD 20910 USA. [Riedel, Gerhardt F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Apeti, DA (reprint author), NOAA, Natl Ctr Coastal & Ocean Sci, Ctr Coastal Monitoring & Assessment, 1305 East West Highway, Silver Spring, MD 20910 USA. EM dennis.apeti@noaa.gov NR 54 TC 14 Z9 15 U1 1 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD JUL PY 2009 VL 58 IS 7 BP 1016 EP 1024 DI 10.1016/j.marpolbul.2009.02.013 PG 9 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 476EY UT WOS:000268422500019 PM 19342067 ER PT J AU Corrigan, CM Dombard, AJ Spudis, PD Bussey, DBJ McCoy, TJ AF Corrigan, C. M. Dombard, A. J. Spudis, P. D. Bussey, D. B. J. McCoy, T. J. TI CANDIDATE SOURCE REGIONS FOR THE LUNAR METEORITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Corrigan, C. M.; McCoy, T. J.] Smithsonian Inst, Washington, DC 20013 USA. [Dombard, A. J.] Univ Illinois, Chicago, IL 60607 USA. [Spudis, P. D.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Bussey, D. B. J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM corriganc@si.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 BP A54 EP A54 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500084 ER PT J AU MacPherson, GJ Kita, NT Bullock, ES Ushikubo, T Davis, AM AF MacPherson, G. J. Kita, N. T. Bullock, E. S. Ushikubo, T. Davis, A. M. TI THE VIGARANO CAI REFERENCE SUITE, II. HIGH-PRECISION AL-MG ISOTOPIC STUDIES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID SYSTEMATICS C1 [MacPherson, G. J.] US Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Kita, N. T.; Ushikubo, T.] Univ Wisconsin, Wisc SIMS, Madison, WI 53706 USA. [Bullock, E. S.; Davis, A. M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Davis, A. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. EM macphers@si.edu NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500236 ER PT J AU MacPherson, GJ Davis, AM Zinner, E AF MacPherson, G. J. Davis, A. M. Zinner, E. TI WHAT'S IN A HISTOGRAM? DECONSTRUCTING AND RECONSTRUCTING INITIAL (26)AL/(27)AL SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID SOLAR; AL-26/AL-27; AL-26 C1 [MacPherson, G. J.] US Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Davis, A. M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Davis, A. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zinner, E.] Washington Univ, Space Sci Lab, St Louis, MO USA. [Zinner, E.] Washington Univ, Dept Phys, St Louis, MO USA. EM macphers@si.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500235 ER PT J AU Matzel, J Ishii, HA Joswiak, D Hutcheon, I Bradley, J Brownlee, D Weber, P Ramon, E Simon, JI Teslich, N Matrajt, G McKeegan, KD MacPherson, G AF Matzel, J. Ishii, H. A. Joswiak, D. Hutcheon, I. Bradley, J. Brownlee, D. Weber, P. Ramon, E. Simon, J. I. Teslich, N. Matrajt, G. McKeegan, K. D. MacPherson, G. TI MG ISOTOPE MEASUREMENTS OF A STARDUST CAI: NO EVIDENCE OF (26)AL SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl Rec Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Matzel, J.; Ishii, H. A.; Hutcheon, I.; Bradley, J.; Weber, P.; Ramon, E.; Teslich, N.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Joswiak, D.; Brownlee, D.; Matrajt, G.] Univ Washington, Seattle, WA 98195 USA. [Simon, J. I.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [McKeegan, K. D.] Univ Calif Los Angeles, Los Angeles, CA USA. [MacPherson, G.] Smithsonian Inst, Washington, DC 20560 USA. EM matzel2@llnl.gov NR 5 TC 1 Z9 1 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 SU S BP A136 EP A136 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500247 ER PT J AU Mayne, RG McCoy, TJ AF Mayne, R. G. McCoy, T. J. TI DO REDOX REACTIONS PLAY A ROLE IN THE FORMATION HISTORY OF THE MESOSIDERITES? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID IRON-METEORITES; ORIGIN; IIIAB C1 [Mayne, R. G.; McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 BP A137 EP A137 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500249 ER PT J AU McCoy, TJ Schmidt, ME AF McCoy, T. J. Schmidt, M. E. TI WHY AREN'T SHERGOTTITES VESICULAR? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID MARS C1 [McCoy, T. J.; Schmidt, M. E.] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 BP A137 EP A137 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500250 ER PT J AU Welzenbach, LC Mccoy, TJ Welten, KC Nishiizumi, K AF Welzenbach, L. C. McCoy, T. J. Welten, K. C. Nishiizumi, K. TI PETROLOGY AND TERRESTRIAL AGE OF MACALPINE HILLS L4 BRECCIAS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine C1 [Welzenbach, L. C.; McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA. [Welten, K. C.; Nishiizumi, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM welzenbl@si.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 BP A217 EP A217 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500409 ER PT J AU Zega, TJ Cosarinsky, M MacPherson, GJ McKeegan, KD AF Zega, T. J. Cosarinsky, M. MacPherson, G. J. McKeegan, K. D. TI FIB-TEM ANALYIS ON A WARK-LOVERING RIM FROM THE VIGARANO CV3 CHONDRITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 72nd Annual Meeting of the Meteoritical-Society CY JUL 13-18, 2009 CL Nancy, FRANCE SP Meteorit Soc, Barringer Crateer Co, Ctr Natl Etudes Spatiales, Ctr Natl rech Sci, Ctr Rech Petrog & Geochim, Communaute Urbaine Grand Nancy, Conseil Gen Meurthe & Moselle, Inst Natl Sci Univ, Lunar & Planetary Inst, Minist Enseignement Superieur & Rech, Nancy Univ, NASA Cosmochem Program, Planetary Studies Fdn, Reg Lorraine ID CAI C1 [Zega, T. J.] USN, Res Lab, Div Mat Sci & Technol, Washington, DC 20375 USA. [Cosarinsky, M.] Univ Bern, Bern, Switzerland. [MacPherson, G. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. EM tzega@nrl.navy.mil NR 6 TC 2 Z9 2 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2009 VL 44 BP A226 EP A226 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 461ZO UT WOS:000267314500427 ER PT J AU Bisson, IA Marra, PP Burtt, EH Sikaroodi, M Gillevet, PM AF Bisson, Isabelle-A. Marra, Peter P. Burtt, Edward H., Jr. Sikaroodi, Masoumeh Gillevet, Patrick M. TI Variation in Plumage Microbiota Depends on Season and Migration SO MICROBIAL ECOLOGY LA English DT Article ID FEATHER-DEGRADING BACTERIA; WEST-NILE-VIRUS; BIRDS; DIVERSITY; INFECTION; SOIL AB Migratory birds can be efficient dispersers of pathogens, yet we know little about the effect of migration and season on the microbial community in avian plumage. This is the first study to describe and compare the microbial plumage community of adult and juvenile migratory birds during the annual cycle and compare the plumage community of migrants to that of resident birds at both neotropical and nearctic locations. We used length heterogeneity PCR (16S rRNA) to describe the microbial assemblage sampled from the plumage of 66 birds in two age classes and from 16 soil samples. Resident birds differed significantly in plumage microbial community composition from migrants (R >= 0.238, P<0.01). Nearctic resident birds had higher plumage microbial diversity than nearctic migrants (R = 0.402, P<0.01). Plumage microbial composition differed significantly between fall premigratory and either breeding (R >= 0.161, P<0.05) or nonbreeding stages (R = 0.267, P<0.01). Six bacterial operational taxonomic units contributed most to the dissimilarities found in this assay. Soil microbial community composition was significantly different from all samples of plumage microbial communities (R >= 0.700, P<0.01). The plumage microbial community varies in relation to migration strategy and stage of the annual cycle. We suggest that plumage microbial acquisition begins in the first year at natal breeding locations and reaches equilibrium at the neotropical wintering sites. These data lead us to conclude that migration and season play an important role in the dynamics of the microbial community in avian plumage and may reflect patterns of pathogen dispersal by birds. C1 [Bisson, Isabelle-A.; Marra, Peter P.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Burtt, Edward H., Jr.] Ohio Wesleyan Univ, Dept Zool, Delaware, OH 43015 USA. [Sikaroodi, Masoumeh; Gillevet, Patrick M.] George Mason Univ, Dept Environm Sci & Policy, Manassas, VA 22030 USA. RP Bisson, IA (reprint author), Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ 08544 USA. EM ibisson@princeton.edu FU Loeb fund; Smithsonian Institution; National Science Foundation [DEB-0089565] FX This research was supported, in part, by funding from the Loeb fund and a Post-doctoral fellowship from the Smithsonian Institution and a National Science Foundation DEB-0089565 grant to P. P. Marra. We thank the Petroleum Corporation of Jamaica for permission to conduct this research at the Font Hill Nature Preserve and the National Environmental Protection Agency of Jamaica for their cooperation with our research in Jamaica. Thank you to the Patuxent River Park for permission to work in the park in Maryland. The Institutional Animal Care and Use Committee of the Smithsonian Environmental Research Center approved all protocols used in this study. We also thank L. Butler, T. Sherry, C. Studds. S. Sillett, D. Brown, L. Duda, A. Logie, J. O'Neil, M. McCormick, and D. Whigham for their help in the field, useful suggestions in the laboratory analyses, and helpful comments on the manuscript. NR 33 TC 19 Z9 19 U1 3 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 J9 MICROB ECOL JI Microb. Ecol. PD JUL PY 2009 VL 58 IS 1 BP 212 EP 220 DI 10.1007/s00248-009-9490-3 PG 9 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA 457FK UT WOS:000266913700022 PM 19212698 ER PT J AU Scott, K Davis, JM Vicenzi, EP AF Scott, Keana Davis, Jeffrey M. Vicenzi, Edward P. TI Three-dimensional microanalysis using FIB SEM: Variations in technique SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Scott, Keana; Davis, Jeffrey M.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Vicenzi, Edward P.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD 20746 USA. RP Scott, K (reprint author), Natl Inst Stand & Technol, 100 Bur Dr, Gaithersburg, MD 20899 USA. RI Scott, Keana/J-5717-2015 NR 4 TC 1 Z9 1 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 476 EP 477 DI 10.1017/S143192760909744X PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100236 ER PT J AU Vicenzi, EP Meier, D Davis, J AF Vicenzi, Edward P. Meier, Douglas Davis, Jeffrey TI Challenges Involved In X-Ray Microanalysis Of The Mineral Kernite [Na2B4O6(OH)(2)center dot 3H(2)O] SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Vicenzi, Edward P.; Meier, Douglas; Davis, Jeffrey] Natl Inst Stand & Technol, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA. RP Vicenzi, EP (reprint author), Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. NR 3 TC 0 Z9 0 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 518 EP 519 DI 10.1017/S1431927609099322 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100257 ER PT J AU Carpenter, PK Zeigler, RA Jolliff, BL Vicenzi, EP Davis, JM MacRae, CM Wilson, NC Kotula, PG Donovan, JJ AF Carpenter, P. K. Zeigler, R. A. Jolliff, B. L. Vicenzi, E. P. Davis, J. M. MacRae, C. M. Wilson, N. C. Kotula, P. G. Donovan, J. J. TI Advances in Electron-Probe Microanalysis and Compositional Mapping: Applications to the Analysis of Meteorites SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Carpenter, P. K.; Zeigler, R. A.; Jolliff, B. L.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Carpenter, P. K.; Zeigler, R. A.; Jolliff, B. L.] Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Davis, J. M.] Natl Inst Stand & Technol, Microanal Res Grp, Gaithersburg, MD 20899 USA. [MacRae, C. M.; Wilson, N. C.] CSIRO Minerals, Clayton, Vic 3168, Australia. [Kotula, P. G.] Sandia Natl Labs, Albuquerque, NM 87185 USA. [Donovan, J. J.] 1241 Univ Oregon, Eugene, OR 97403 USA. RP Carpenter, PK (reprint author), Washington Univ, Dept Earth & Planetary Sci, Campus Box 1169, St Louis, MO 63130 USA. NR 10 TC 0 Z9 0 U1 1 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 534 EP 535 DI 10.1017/S1431927609098882 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100265 ER PT J AU Davis, JM Newbury, DE Ritchie, NWM Vicenzi, EP AF Davis, Jeffrey M. Newbury, Dale E. Ritchie, Nicholas W. M. Vicenzi, Edward P. TI Solving the Micro to Macro Problem: A new application for milli X-ray fluorescence X-ray spectrum imaging SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Davis, Jeffrey M.; Newbury, Dale E.; Ritchie, Nicholas W. M.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Davis, JM (reprint author), Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. NR 2 TC 0 Z9 0 U1 0 U2 2 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 542 EP 543 DI 10.1017/S1431927609098146 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100269 ER PT J AU Meier, DC Davis, J Vicenzi, EP AF Meier, Douglas C. Davis, Jeffrey Vicenzi, Edward P. TI Auger Electron Spectroscopy of Kernite: Coaxing Useful Information Out of a Recalcitrant Specimen SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Meier, Douglas C.; Davis, Jeffrey; Vicenzi, Edward P.] NIST, Chem Sci & Technol Lab, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA. [Vicenzi, Edward P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Meier, DC (reprint author), NIST, Chem Sci & Technol Lab, Surface & Microanal Sci Div, 100 Bur Dr MS8371, Gaithersburg, MD 20899 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 1384 EP 1385 DI 10.1017/S1431927609099681 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100683 ER PT J AU Yang, J Goldstein, JI Michael, JR Kotula, PG McCoy, TJ AF Yang, J. Goldstein, J. I. Michael, J. R. Kotula, P. G. McCoy, T. J. TI Microstructural Characterization of Reheated Iron Meteorites by Electron Microscopy Techniques SO MICROSCOPY AND MICROANALYSIS LA English DT Meeting Abstract C1 [Yang, J.; Goldstein, J. I.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Michael, J. R.; Kotula, P. G.] Sandia Natl Labs, Mat Characterizat Dept, Albuquerque, NM 87185 USA. [McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Yang, J (reprint author), Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. FU United States Department of Energy (DOE) [DE-AC04-94AL85000] FX Sandia is a multiprogram laboratory operated by Sandia Corporation, a Lockheed Martin Company, for the United States Department of Energy (DOE) under contract DE-AC04-94AL85000. NR 3 TC 1 Z9 1 U1 2 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1431-9276 J9 MICROSC MICROANAL JI Microsc. microanal. PD JUL PY 2009 VL 15 SU 2 BP 1514 EP 1515 DI 10.1017/S1431927609094409 PG 2 WC Materials Science, Multidisciplinary; Microscopy SC Materials Science; Microscopy GA V20CW UT WOS:000208119100744 ER PT J AU Wise, MA AF Wise, Michael A. TI Chabazite in spodumene-bearing Alpine-type fissure veins from Hiddenite, North Carolina, USA SO MINERALOGY AND PETROLOGY LA English DT Article ID CRYSTAL-CHEMISTRY; NEW-ZEALAND; ZEOLITE; PARAGENESIS; ASSEMBLAGE; BIKITAITE; MINERALS; LITHIUM; SYSTEM AB Alpine-type fissure vein mineralization in the Hiddenite area of western North Carolina, USA consists mostly of quartz, but locally contains Cr-bearing beryl (emerald) or Cr-bearing spodumene (hiddenite). These gem minerals occur in mineral-lined cavities and may be accompanied by euhedral crystals of quartz, calcite, muscovite, rutile, albite, pyrite, siderite and dolomite. Chabazite-Ca occurs as a late stage phase in spodumene-bearing veins, but is absent in emerald-bearing veins. Chabazite-Ca occurs as simple penetrating twins of pseudocubic rhombohedra and as the lens-shaped variety, phacolite. Chabazite-Ca from Hiddenite contains minor amounts of Na, Mg, Fe and K. Phacolitic chabazite-Ca shows Fe-enriched but Mg-depleted cores relative to the rims. Chemical zoning is absent in rhombohedral chabazite. The Hiddenite chabazite apparently precipitated under low temperature (< 250A degrees C) and low pressure (< 2 kbar) conditions during the waning stages of crystallization of an alkaline hydrothermal fluid. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Wise, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM wisem@si.edu NR 40 TC 0 Z9 0 U1 1 U2 3 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0930-0708 J9 MINER PETROL JI Mineral. Petrol. PD JUL PY 2009 VL 96 IS 3-4 BP 213 EP 220 DI 10.1007/s00710-009-0052-7 PG 8 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 460UL UT WOS:000267216100006 ER PT J AU Cortes, MC Gowda, V Kress, WJ Bruna, EM Uriarte, M AF Cortes, M. C. Gowda, V. Kress, W. J. Bruna, E. M. Uriarte, M. TI Characterization of 10 microsatellite markers for the understorey Amazonian herb Heliconia acuminata SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE Amazon forest; forest fragmentation; genetic relatedness; Heliconia acuminata; microsatellites; parentage analysis AB We characterized 10 microsatellite loci for the plant Heliconia acuminata from the Biological Dynamics of Forest Fragments Project (Manaus, Brazil). Markers were screened in 61 individuals from one population and were found to be polymorphic with an average of eight alleles per locus. We found moderate to high levels of polymorphic information content, and observed and expected heterozygosities. All 10 markers are suitable for spatial genetic structure and parentage analyses and will be used for understanding H. acuminata dynamics across a fragmented landscape. C1 [Cortes, M. C.; Uriarte, M.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Gowda, V.; Kress, W. J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Bruna, E. M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, E. M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. RP Cortes, MC (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. EM mcc2149@columbia.edu RI Bruna, Emilio/H-2769-2012; cortes, marina/I-2155-2012; Uriarte, Maria/L-8944-2013 OI Bruna, Emilio/0000-0003-3381-8477; NR 8 TC 1 Z9 1 U1 1 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD JUL PY 2009 VL 9 IS 4 BP 1261 EP 1264 DI 10.1111/j.1755-0998.2009.02627.x PG 4 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 473XM UT WOS:000268245500052 PM 21564896 ER PT J AU Dohrmann, M Collins, AG Worheide, G AF Dohrmann, M. Collins, A. G. Woerheide, G. TI New insights into the phylogeny of glass sponges (Porifera, Hexactinellida): Monophyly of Lyssacinosida and Euplectellinae, and the phylogenetic position of Euretidae SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID EVOLUTION; HEXACTINOSIDA; REVISION; ATLANTIC C1 [Dohrmann, M.; Woerheide, G.] Univ Munich, Dept Geo & Umweltwissensch, D-80333 Munich, Germany. [Dohrmann, M.; Woerheide, G.] Univ Munich, GeoBioCtr, D-80333 Munich, Germany. [Dohrmann, M.] Univ Gottingen, GZG, Abt Geobiol, D-37077 Gottingen, Germany. [Collins, A. G.] Natl Museum Nat Hist, NMFS, Natl Systemat Lab, Smithsonian Inst,MRC 153, Washington, DC 20013 USA. RP Worheide, G (reprint author), Univ Munich, Dept Geo & Umweltwissensch, Richard Wagner Str 10, D-80333 Munich, Germany. EM woerheide@lmu.de RI Collins, Allen/A-7944-2008; Worheide, Gert/C-1080-2008 OI Collins, Allen/0000-0002-3664-9691; Worheide, Gert/0000-0002-6380-7421 FU Deutsche Forschungsgemeinschaft (DFG) [Wo896/5-1 2]; Society of Systematic Biologists FX We thank Amanda Kahn, Justin Marshall, Shirley Pomponi, Henry Reiswig, and Rob van Soest for providing specimens, Henry Reiswig and Konstantin Tabachnick for help with identification, and Burkhard Morgenstern for providing access to computational resources of the Department of Bioinformatics, University of Gottingen. Three anonymous reviewers are acknowledged for critical comments that lead to improvement of the manuscript. This study was funded by grants Wo896/5-1 & 2 of the Deutsche Forschungsgemeinschaft (DFG) to GW and benefited from a Mini-PEET award of the Society of Systematic Biologists to MD. NR 23 TC 18 Z9 19 U1 2 U2 4 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 JUL PY 2009 VL 52 IS 1 BP 257 EP 262 DI 10.1016/j.ympev.2009.01.010 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 454OU UT WOS:000266692800024 PM 19475712 ER PT J AU Pal, A AF Pal, Andras TI An analytical solution for Kepler's problem SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; techniques: radial velocities; celestial mechanics; ephemerides ID PLANET; STAR AB In this paper, we present a framework which provides an analytical (i.e. infinitely differentiable) transformation between spatial coordinates and orbital elements for the solution of the gravitational two-body problem. The formalism omits all singular variables which otherwise would yield discontinuities. This method is based on two simple real functions for which the derivative rules are only required to be known, all other applications -e.g. calculating the orbital velocities, obtaining the partial derivatives of radial velocity curves with respect to the orbital elements - are thereafter straightforward. As it is shown, the presented formalism can be applied to find optimal instants for radial velocity measurements in transiting explanatory systems to constrain the orbital eccentricity as well as to detect secular variations in the eccentricity or in the longitude of periastron. C1 [Pal, Andras] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pal, Andras] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary. [Pal, Andras] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary. RP Pal, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apal@szofi.net NR 12 TC 25 Z9 25 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2009 VL 396 IS 3 BP 1737 EP 1742 DI 10.1111/j.1365-2966.2009.14853.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 459AM UT WOS:000267072100047 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI Phylogenetic position of Turanoceratops (Dinosauria: Ceratopsia) SO NATURWISSENSCHAFTEN LA English DT Editorial Material DE Dinosauria; Ceratopsidae; Cretaceous; Asia C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, MRC 106, Washington, DC 20013 USA. [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 106, POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; lepus@zin.ru RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 NR 6 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD JUL PY 2009 VL 96 IS 7 BP 871 EP 872 DI 10.1007/s00114-009-0552-7 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 466TE UT WOS:000267684900016 ER PT J AU Vari, RP Ferraris, CJ AF Vari, Richard P. Ferraris, Carl J., Jr. TI New species of Cetopsidium (Siluriformes: Cetopsidae: Cetopsinae) from the upper rio Branco system in Guyana SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Taxonomy; New Catfish; Takutu River basin AB Cetopsidium soniae, new species, is described from the Takutu River basin of southwestern Guyana, within the upper portions of the rio Branco of the Amazon basin. The new species differs from its congeners in details of pigmentation, the length of the pelvic fin, the form of the First rays of the dorsal and pectoral fins in mature males, the relative alignment of the dorsal and ventral profiles of the postdorsal portion of the body, the position of the anus, and the depth of the body. DNA barcodes were generated for the holotype and paratype. An examination of other samples of Cetopsidium from the rio Branco system extends the range of C. pemon into the Ireng River system of Guyana. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, MRC 159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu; carlferraris@comcast.net FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology; National Museum of Natural History; Smithsonian Institution; All Catfish Species Inventory; National Science Foundation [DEB-0315963] FX Research and museum visits associated with this publication were made possible through funding from the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, National Museum of Natural History, Smithsonian Institution, and the All Catfish Species Inventory, a program funded by the National Science Foundation (DEB-0315963). Sonia Fisch-Muller (MHNG) brought the specimens that served as the basis of the description to our attention. T. Britt Griswold provided Fig. 1, Sandra J. Raredon (USNM) technical support for the project, and Mark Sabaj Perez (ANSP) made possible a loan of other material from the type region. Barcode information was provided by Raphael Covain (MHNG) who also secured the GenBank registration numbers. NR 5 TC 2 Z9 2 U1 0 U2 3 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 JUL-SEP PY 2009 VL 7 IS 3 BP 289 EP 293 PG 5 WC Zoology SC Zoology GA 512HR UT WOS:000271237400001 ER PT J AU Menezes, NA Weitzman, SH AF Menezes, Naercio A. Weitzman, Stanley H. TI Systematics of the Neotropical fish subfamily Glandulocaudinae (Teleostei: Characiformes: Characidae) SO NEOTROPICAL ICHTHYOLOGY LA English DT Review DE South America; Lophiobrycon; Glandulocauda; Mimagoniates; Taxonomy; Biogeography ID PHYLOGENETIC ANALYSIS; CAUDAL-FIN; BRAZIL; GENUS; CHEIRODONTINAE; OSTARIOPHYSI; BIOGEOGRAPHY; PARAGUAY; PISCES AB The systematics of the Glandulocaudinae is reviewed in detail and justification for the recognition of the group as a Subfamily is discussed. The Subfamily Glandulocaudinae consists of three genera: Lophiobrycon with one species plesiomorphic in some anatomical features but some others exclusively derived relative to the species in the other genera; Glandulocauda with two species intermediate in phylogenetic derivation; and Mimagoniates with seven species (one new), all more phylogenetically derived concerning their pheromone producing caudal-fin organs and with other anatomical characters presumably more derived than in the species of the other genera. Glandulocauda melanogenys Eigenmann, 1911, is considered a junior synonym of Hyphessobrycon melanopleurus Ellis, 1911. A replacement name, Glandulocauda caerulea Menezes & Weitzman, is proposed for G. melanopleura Eigenmann, 1911. Gland cells found in the caudal-fin organs of all species are histologically indistinguishable from club cells and probably secrete a pheromone during courtship. The club cells are associated with somewhat modified to highly derived caudal scales forming a pheromone pumping organ in the more derived genera and species. This Subfamily is distributed in freshwaters of eastern and southern Brazil, Paraguay, and northeastern Uruguay. C1 [Menezes, Naercio A.] Univ Sao Paulo, Museu Zool, BR-04218970 Sao Paulo, Brazil. [Weitzman, Stanley H.] Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. RP Menezes, NA (reprint author), Univ Sao Paulo, Museu Zool, Caixa Postal 42494, BR-04218970 Sao Paulo, Brazil. EM naercio@usp.br; weitzmans@si.edu RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Smithsonian Institution; Bacon Fund, Smithsonian Institution; Conselho Nacional de Desenvolvimento Cientifico a Tecnologico (CNPq), Brazil; National Geographic Society [1797]; Herbert R. and Evelyn Axelrod Revolving Chair of the Division of Fishes, National Museum of Natural History, Smithsonian Institution FX Much of the field work in Brazil and laboratory research in Sao Paulo and Washington D.C. for this study was supported by the Neotropical Lowland Research Program (NLRP), of the International Environmental Science Program of the Smithsonian Institution. We thank the late Clifford Evans, W. Ronald Heyer, and Richard P. Vari, former principal investigators of the NLRP for their support and encouragement. The Bacon Fund, Smithsonian Institution, provided funds for part of the field work in Rio Grande do Sul and Santa Catarina. The Conselho Nacional de Desenvolvimento Cientifico a Tecnologico (CNPq), Brazil also provided travel and per diem funds for laboratory research in Sao Paulo and Washington, D. C. to NAM. Field research was supported in part by a grant (# 1797) from the National Geographic Society. Herbert R. Axelrod supported this research in part by providing payments for articles published in Tropical Fish Hobyist, TFH Publications Inc. New Jersey from 1995-1998. We are indebted to the Herbert R. and Evelyn Axelrod Revolving Chair of the Division of Fishes, National Museum of Natural History, Smithsonian Institution, for providing funds in support of this research. Many drawings were paid for by the Department of Vertebrate Zoology, Smithsonian Institution. Rosario LaCorte provided some of the color photographs of live fishes used in this publication. John R. Burns and Robert Javonillo provided information concerning and illustrations of the club cells of the male caudal glands of the three genera of the Glandulocaudinae. NR 110 TC 31 Z9 35 U1 1 U2 8 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 JUL-SEP PY 2009 VL 7 IS 3 BP 295 EP 370 PG 76 WC Zoology SC Zoology GA 512HR UT WOS:000271237400002 ER PT J AU Hong, J Allen, B Grindlay, J Chammas, N Barthelemy, S Baker, R Gehrels, N Nelson, KE Labov, S Collins, J Cook, WR McLean, R Harrison, F AF Hong, J. Allen, B. Grindlay, J. Chammas, N. Barthelemy, S. Baker, R. Gehrels, N. Nelson, K. E. Labov, S. Collins, J. Cook, W. R. McLean, R. Harrison, F. TI Building large area CZT imaging detectors for a wide-field hard X-ray telescope-ProtoEXIST1 SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article DE X-ray imaging; CZT AB We have constructed a moderately large area (32 cm(2)), fine pixel (2.5 mm pixel, 5 mm thick) CZT imaging detector which constitutes the first section of a detector module (256 cm(2)) developed for a balloon-borne wide-field hard X-ray telescope, ProtoEXIST1. ProtoEXIST1 is a prototype for the High Energy Telescope (HET) in the Energetic X-ray imaging Survey Telescope (EXIST), a next generation space-borne multi-wavelength telescope. We have constructed a large (nearly gapless) detector plane through a modularization scheme by tiling of a large number of 2 cm x 2 cm CZT crystals. Our innovative packaging method is ideal for many applications such as coded-aperture imaging, where a large, continuous detector plane is desirable for the optimal performance. Currently we have been able to achieve an energy resolution of 3.2 keV (FWHM) at 59.6 keV on average, which is exceptional considering the moderate pixel size and the number of detectors in simultaneous operation. We expect to complete two modules (512 cm(2)) within the next few months as more CZT becomes available. We plan to test the performance of these detectors in a near space environment in a series of high altitude balloon flights, the first of which is scheduled for Fall 2009. These detector modules are the first in a series of progressively more sophisticated detector units and packaging schemes planned for ProtoEXIST2 & 3, which will demonstrate the technology required for the advanced CZT imaging detectors (0.6 mm pixel, 4.5 m(2) area) required in EXIST/HET. (C) 2009 Elsevier B.V. All rights reserved. C1 [Hong, J.; Allen, B.; Grindlay, J.; Chammas, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barthelemy, S.; Baker, R.; Gehrels, N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Nelson, K. E.; Labov, S.; Collins, J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Cook, W. R.; McLean, R.; Harrison, F.] CALTECH, Pasadena, CA 91125 USA. RP Hong, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jaesub@head.cfa.harvard.edu RI Gehrels, Neil/D-2971-2012 FU NASA APRA [NNG06WC12G]; US Department of Energy [DE-AC52-07NA27344] FX This work is supported in part by NASA APRA Grant NNG06WC12G. Portions of this work were performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. NR 9 TC 18 Z9 21 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD JUL 1 PY 2009 VL 605 IS 3 BP 364 EP 373 DI 10.1016/j.nima.2009.04.004 PG 10 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 476HL UT WOS:000268430000020 ER PT J AU Hannon, SJ Wilson, S McCallum, CA AF Hannon, Susan J. Wilson, Scott McCallum, Cindy A. TI Does cowbird parasitism increase predation risk to American redstart nests? SO OIKOS LA English DT Article ID BROWN-HEADED COWBIRD; CUCULUS-CANORUS PARASITISM; BROOD PARASITISM; FOREST FRAGMENTATION; SONG SPARROWS; WARBLER NESTS; BEHAVIOR; HOST; SURVIVAL; SUCCESS AB Brood parasitism and nest predation are major causes of reproductive failure for many bird species nesting in fragmented landscapes. While brood parasites and predators may act independently, they could also interact if brood parasites increase the likelihood that predators detect nests. In this study, we examined the interaction between cowbird parasitism and nest predation in a 10 year study on 466 American redstart Setophaga ruticilla nests in central Alberta, Canada. We used advanced nest survival models to examine the support for three mechanisms that might lead to a positive correlation between brood parasitism and nest predation: 1) the presence of a cowbird nestling might increase the detection of the nest by predators, 2) nests with lower cover are more likely to be detected by both cowbirds and predators, and 3) cowbirds and predators may co-occur in landscapes of similar structure. Twelve percent of nests were parasitized and those nests had a 16-19% higher rate of failure due to predators compared to unparasitized nests. Daily nest predation rates increased during the nestling stage for both groups, but more strongly for parasitized nests. Loud begging by the cowbird nestling and/or higher parental feeding rates for the cowbird may have increased nest detectability to predators. Brood parasitism and nest predation were also positively related to forest cover, indicating landscape level effects were influential. Most nest predators were forest species and we suspect cowbirds responded positively to forest cover because of the increased abundance of songbird hosts. Nest-site features had less of an impact on nest predation or brood parasitism, although nests with higher overhead cover were less susceptible to predators. Our study shows how multiple mechanisms, particularly the behavioral effects of the brood parasite nestling and landscape structure, can lead to a positive relationship between nest predation and brood parasitism. C1 [Hannon, Susan J.; McCallum, Cindy A.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Wilson, Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Hannon, SJ (reprint author), Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. EM sue.hannon@ualberta.ca RI Hannon, Susan/A-2648-2014 OI Hannon, Susan/0000-0003-3978-3199 FU Natural Sciences and Engineering Research Council of Canada; National Geographic Society; Alberta Conservation Association; Alberta Sport, Recreation, Parks and Wildlife Foundation FX The study was funded by the Natural Sciences and Engineering Research Council of Canada, National Geographic Society, Alberta Conservation Association and Alberta Sport, Recreation, Parks and Wildlife Foundation. We thank the many assistants over the years who helped in data collection, the staff at the Meanook Biological Research Station for logistical assistance and the land owners around the station for access to breeding clusters on private land. B. K. Sandercock provided valuable comments on an earlier draft of this manuscript. This paper is dedicated to Dr. James (Jamie) N. M. Smith, a mentor and fellow cowbird enthusiast. NR 53 TC 20 Z9 20 U1 2 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 EI 1600-0706 J9 OIKOS JI Oikos PD JUL PY 2009 VL 118 IS 7 BP 1035 EP 1043 DI 10.1111/j.1600-0706.2008.17383.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 462CB UT WOS:000267322100008 ER PT J AU Zhao, L Wang, T Yelin, SE AF Zhao, L. Wang, T. Yelin, S. E. TI Two-dimensional all-optical spatial light modulation with high speed in coherent media SO OPTICS LETTERS LA English DT Article ID ORBITAL ANGULAR-MOMENTUM; ELECTROMAGNETICALLY INDUCED TRANSPARENCY; PHASE SINGULARITIES; LASER-BEAMS; PHOTONS; STATES AB We show theoretical evidence that coherent systems based on electromagnetically induced transparency (EIT) can function as optically addressed spatial light modulators with megahertz modulation rates. The transverse spatial properties of cw probe fields can be modulated fast using two-dimensional optical patterns. To exemplify our proposal, we study real-time generation and manipulation of Laguerre-Gaussian beams by means of phase or amplitude modulation using flat-top image-bearing pulse trains as coupling fields in low-cost hot vapor EIT systems. (C) 2009 Optical Society of America C1 [Zhao, L.; Wang, T.; Yelin, S. E.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. E.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. RP Zhao, L (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM zhaol@phys.uconn.edu FU National Science Foundation (NSF) FX We acknowledge funding from the National Science Foundation (NSF). L. Z. thanks J. Javanainen, G. N. Gibson, Y. Xiao, L. Fang, R. Zhou, and F. Peng for helpful discussions. NR 23 TC 7 Z9 7 U1 2 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD JUL 1 PY 2009 VL 34 IS 13 BP 1930 EP 1932 PG 3 WC Optics SC Optics GA 475QV UT WOS:000268376200006 PM 19571955 ER PT J AU Cairns, SD AF Cairns, Stephen D. TI Review of Octocorallia (Cnidaria: Anthozoa) from Hawai'i and Adjacent Seamounts. Part 2: Genera Paracalyptrophora Kinoshita, 1908; Candidella Bayer, 1954; and Calyptrophora Gray, 1866 SO PACIFIC SCIENCE LA English DT Article ID COELENTERATA; GORGONACEA; PRIMNOIDAE AB Nine deep-water primnoid octocoral species are described from Hawaiian waters, four of them as new species, bringing the total number of octocoral species known from Hawai'i to 94. Candidella gigantea is reported for the first time subsequent to its original description from Fiji In 1889. To place the two new species of Calyptrophora in context, all 16 species in the genus are keyed and analyzed in a morphology-based phylogenetic analysis. Although the analysis did not support the species complexes and species groups established by Bayer, it did suggest two distinct clades based on characters such as the opercular cowl, inclination of the polyps, and cross section and sculpture of the basal scale spines. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC-163,POB 37012, Washington, DC 20013 USA. EM cairnss@si.edu FU NOAA-OE [NA0OAR4600108, NA04OAR4600071] FX Pisces cruises were funded by NOAA-OE grants NA0OAR4600108 and NA04OAR4600071 to Amy Baco. Manuscript accepted 14 October 2008. NR 32 TC 4 Z9 7 U1 0 U2 1 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD JUL PY 2009 VL 63 IS 3 BP 413 EP 448 DI 10.2984/049.063.0309 PG 36 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 462KJ UT WOS:000267351000009 ER PT J AU Yasuhara, M Okahashi, H Cronin, TM AF Yasuhara, Moriaki Okahashi, Hisayo Cronin, Thomas M. TI TAXONOMY OF QUATERNARY DEEP-SEA OSTRACODS FROM THE WESTERN NORTH ATLANTIC OCEAN SO PALAEONTOLOGY LA English DT Review DE Deep-sea Ostracoda; Pleistocene; Holocene; North Atlantic; taxonomy ID SANTOS BASIN; BATHYAL OSTRACODES; LATE PLEISTOCENE; CLIMATE CHANGES; LAPTEV SEA; HOLOCENE; VARIABILITY; ASSEMBLAGES; CRUSTACEA; TEMPERATURE AB Late Quaternary sediments from Ocean Drilling Program (ODP) Hole 1055B, Carolina Slope, western North Atlantic (32 degrees 47.041' N, 76 degrees 17.179' W; 1798 m water depth) were examined for deep-sea ostracod taxonomy. A total of 13 933 specimens were picked from 207 samples and c. 120 species were identified. Among them, 87 species were included and illustrated in this paper. Twenty-eight new species are described. The new species are: Ambocythere sturgio, Argilloecia abba, Argilloecia caju, Argilloecia keigwini, Argilloecia robinwhatleyi, Aversovalva carolinensis, Bythoceratina willemvandenboldi, Bythocythere eugeneschornikovi, Chejudocythere tenuis, Cytheropteron aielloi, Cytheropteron demenocali, Cytheropteron didieae, Cytheropteron richarddinglei, Cytheropteron fugu, Cytheropteron guerneti, Cytheropteron richardbensoni, Eucytherura hazeli, Eucytherura mayressi, Eucytherura namericana, Eucytherura spinicorona, Posacythere hunti, Paracytherois bondi, Pedicythere atroposopetasi, Pedicythere kennettopetasi, Pedicythere klothopetasi, Pedicythere lachesisopetasi, Ruggieriella mcmanusi and Xestoleberis oppoae. Taxonomic revisions of several common species were made to reduce taxonomic uncertainty in the literature. This study provides a robust taxonomic baseline for application to palaeoceanographical reconstruction and biodiversity analyses in the deep and intermediate-depth environments of the North Atlantic Ocean. C1 [Yasuhara, Moriaki; Okahashi, Hisayo] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Cronin, Thomas M.] US Geol Survey, Reston, VA 20192 USA. RP Yasuhara, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM moriakiyasuhara@gmail.com; yasuharah@si.edu; tcronin@usgs.gov RI Yasuhara, Moriaki/A-4986-2008 OI Yasuhara, Moriaki/0000-0001-8501-4863 FU Japan Society for the Promotion of Science FX We thank the staff of the U.S. Geological Survey Eastern Earth Surface Processes Team and the Department of Paleobiology, National Museum of Natural History, Smithsonian Institution, especially Carlita Sanford, for their support throughout this project. We thank Peter B. deMenocal for kindly loaning us ODP core samples, Scott Whittaker for help in SEM imaging, Giuseppe Aiello for taxonomic input, and Mark Florence for help in depositing type and figured specimens. Gene Hunt and John Repetski deserve special thanks for valuable comments and discussion. This paper benefited from reviews by Michael A. Ayress and anonymous referee and editing by Paul Smith, David Batten, and Svend Stouge. This research used samples provided by the Ocean Drilling Program. The Ocean Drilling Program is sponsored by the National Science Foundation and participating countries under the management of Joint Oceanographic Institutions. This work was supported by Japan Society for the Promotion of Science Postdoctoral Fellowships for Research Abroad and Smithsonian Postdoctoral Fellowship (to M.Y.). NR 134 TC 26 Z9 27 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-0239 EI 1475-4983 J9 PALAEONTOLOGY JI Paleontology PD JUL PY 2009 VL 52 BP 879 EP 931 DI 10.1111/j.1475-4983.2009.00888.x PN 4 PG 53 WC Paleontology SC Paleontology GA 471MC UT WOS:000268060800013 ER PT J AU Warrit, N AF Warrit, Natapot TI A new subgeneric placement of Ceratina splendida Shiokawa (Hymenoptera; Apidae) from the subcontinent of India and Pakistan SO PAN-PACIFIC ENTOMOLOGIST LA English DT Editorial Material ID GENUS C1 [Warrit, Natapot] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20003 USA. RP Warrit, N (reprint author), Chulalongkorn Univ, Fac Sci, Ctr Excellence Entomol, Dept Biol, Bangkok 10330, Thailand. EM Natapot.W@chula.ac.th NR 12 TC 0 Z9 0 U1 0 U2 1 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 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD JUL PY 2009 VL 85 IS 3 BP 159 EP 161 DI 10.3956/2009-11.1 PG 3 WC Entomology SC Entomology GA 586QT UT WOS:000276927100003 ER PT J AU Littler, DS Littler, MM Hanisak, MD AF Littler, D. S. Littler, M. M. Hanisak, M. D. TI SUBMERSED PLANTS OF THE INDIAN RIVER LAGOON: A FLORISTIC INVENTORY AND FIELD GUIDE SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Littler, D. S.; Littler, M. M.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Hanisak, M. D.] Florida Atlantic Univ, Harbor Branch, Oceanog Inst, Ft Pierce, FL 34946 USA. EM dhanisak@hboi.fau.edu NR 0 TC 0 Z9 0 U1 0 U2 4 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2009 VL 48 IS 4 MA 112 BP 40 EP 40 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 472JN UT WOS:000268126900113 ER PT J AU Rajapakse, RM Bragdon, T Rey, AM Calarco, T Yelin, SF AF Rajapakse, R. M. Bragdon, T. Rey, A. M. Calarco, T. Yelin, S. F. TI Single-photon nonlinearities using arrays of cold polar molecules SO PHYSICAL REVIEW A LA English DT Article AB We model single-photon nonlinearities resulting from the dipole-dipole interactions of cold polar molecules. We propose utilizing "dark state polaritons" to effectively couple photon and molecular states; through this framework, coherent control of the nonlinearity can be expressed and potentially used in an optical quantum computation architecture. Due to the dipole-dipole interaction the photons pick up a measurable nonlinear phase even in the single-photon regime. A manifold of protected symmetric eigenstates is used as basis. Depending on the implementation, major sources of decoherence result from nonsymmetric interactions and phonon dispersion. We discuss the strength of the nonlinearity per photon and the feasibility of this system. C1 [Rajapakse, R. M.; Bragdon, T.; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Rey, A. M.] Univ Colorado, Natl Inst Stand & Technol, JILA, Boulder, CO 80309 USA. [Calarco, T.] Univ Ulm, Inst Quantum Informat Proc, D-89069 Ulm, Germany. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Rajapakse, RM (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU NSF; EC FX The authors wish to acknowledge NSF for funding, and Peter Rabl for fruitful discussions. Tommaso Calarco wishes to acknowledge the EC Integrated Project SCALA. NR 16 TC 16 Z9 16 U1 0 U2 2 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 JUL PY 2009 VL 80 IS 1 AR 013810 DI 10.1103/PhysRevA.80.013810 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 478VP UT WOS:000268616900163 ER PT J AU Henry, TJ AF Henry, Thomas J. TI A NEW SPECIES OF PYCNODERIELLA (HETEROPTERA: MIRIDAE: BRYOCORINAE: ECCRITOTARSINAE) FROM THE WEST INDIES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; new species; Cuba; Jamaica; relationships AB The new eccritotarsine plant bug Pycnoderiella insularis, n. sp., is described from Cuba and Jamaica and compared with the type species of Pycnoderiella Henry, P. virginiana Henry, known from only a restricted coastal area of Virginia, in the eastern United States. Color dorsal and lateral adult images, illustrations of male genitalia, and a key are provided to facilitate recognition. The relationship of Pycnoderiella with other New World eccritotarsine Bryocorinae is discussed. C1 USDA ARS, Systemat Entomol Lab, Inst Plant Sci, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Henry, TJ (reprint author), USDA ARS, Systemat Entomol Lab, Inst Plant Sci, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC-0168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 2 TC 0 Z9 0 U1 1 U2 3 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 603 EP 608 DI 10.4289/0013-8797-111.3.603 PG 6 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800006 ER PT J AU Kotrba, M Mathis, WN AF Kotrba, Marion Mathis, Wayne N. TI THE INTERNAL FEMALE REPRODUCTIVE TRACT OF THE ENIGMATIC GENUS RISA (DIPTERA: SCHIZOPHORA: EPHYDROIDEA) AND ITS PHYLOGENETIC IMPLICATIONS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Ephydridae; morphology; phylogeny; ventral receptacle ID CAMILLIDAE DIPTERA; EPHYDRIDAE; DROSOPHILA; SPERM; FLIES; COEVOLUTION; LENGTH; TRIBE AB The internal female reproductive tract of Risa is characterized by a pair of short spermathecal ducts with no spermathecae, paired short accessory glands, and a large thimble-shaped strongly sclerotized ventral receptacle. This condition is identical with that in the ground plan of Ephydridae but differs from that of their next relatives, i.e., Camillidae and Diastatidae, regarding the shape of the ventral receptacle. It therefore corroborates the close relationship of Risa with Ephydridae either as its sister taxon or within that family. C1 [Kotrba, Marion] Zool Staatssammlung Munchen, D-81247 Munich, Germany. [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Kotrba, M (reprint author), Zool Staatssammlung Munchen, Munchhausenstr 21, D-81247 Munich, Germany. EM Marion.Kotrba@zsm.mwn.de; mathisw@si.edu FU DFG [II B 3-Ko 1369/1-2] FX We thank Amnon Freidberg for his collaboration on the Risa project and for providing specimens for this study, as well as Daniel Burckhardt, Stefan Schmidt, and Holly B. Williams for useful comments on earlier drafts. Parts of this study were conducted during a postdoctoral fellowship granted by the DFG (II B 3-Ko 1369/1-2). NR 51 TC 5 Z9 5 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 627 EP 640 DI 10.4289/0013-8797-111.3.627 PG 14 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800009 ER PT J AU Kula, RR Martinez, JJ Walsh, GC AF Kula, Robert R. Jose Martinez, Juan Cabrera Walsh, Guillermo TI SUPPLEMENT TO REVISION OF NEW WORLD CHAENUSA HALIDAY SENSU LATO (HYMENOPTERA: BRACONIDAE: ALYSIINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Dacnusini; Hydrocharitaceae; Brazilian waterweed; Nearctic; Neotropical; biological control; new records; new species; parasitoid; taxonomy ID DISTRIBUTION RECORDS AB Chaenusa aurantium Kula and Martinez, new species and Chaenusa steineri Kula, new species, both from the Neotropical Region, are described. The former species was reared from an undescribed species of Hydrellia Robineau-Desvoidy (Diptera: Ephydridae) in Argentina under evaluation for control of Egeria densa (Planch.) (Alismatales: Hydrocharitaceae), Brazilian waterweed, in the United States. Chaenusa pallidinervis (Brethes), also from the Neotropical Region, is redescribed. New distribution records are reported for Chaenusa americana (Riegel), Chaenusa bergi (Riegel), Chaenusa quadriceps (Ashmead), Chaenusa trumani Kula, Chaenusa whartoni Kula, and Chaenusa woolleyi Kula from the Nearctic Region, as well as Chaenusa ireneae Kula from the Neotropical Region. These data supplement a recently published revision of New World Chaenusa Haliday sensu lato. C1 [Kula, Robert R.] USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Jose Martinez, Juan] Museo Argentino Ciencias Nat Bernardino Rivadavia, Div Entomol, Buenos Aires, DF, Argentina. [Cabrera Walsh, Guillermo] USDA ARS, S Amer Biol Control Lab, RA-1686 Buenos Aires, DF, Argentina. RP Kula, RR (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM Robert.Kula@ars.usda.gov; jjmartinez@.macn.gov.ar; gcabrera@speedy.com.ar NR 16 TC 7 Z9 7 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 641 EP 655 DI 10.4289/0013-8797-111.3.641 PG 15 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800010 ER PT J AU Linzmeier, AM Konstantinov, AS AF Linzmeier, Adelita M. Konstantinov, Alexander S. TI A NEW GENUS OF FLEA BEETLES (COLEOPTERA: CHRYSOMELIDAE) FROM THE SOUTH OF BRAZIL SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Alticini; new species; Parana; PROFAUPAR AB Deciplatus, a new genus of Monoplatina with two new species (D. jundiaiensis and D. nigritus), from the south of Brazil is described and illustrated. Deciplatus is compared to Ulrica Scherer and Laselva Furth. Use of the name Monoplatina is clarified. C1 [Linzmeier, Adelita M.] Univ Fed Parana, Lab Sistemat & Bioecol Coleoptera Insecta, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. [Konstantinov, Alexander S.] USDA, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Linzmeier, AM (reprint author), Univ Fed Parana, Lab Sistemat & Bioecol Coleoptera Insecta, Dept Zool, Caixa Postal 19020, BR-81531980 Curitiba, Parana, Brazil. EM alinzmeier@yahoo.com.br; alex.konstantinov@ars.usda.gov RI Linzmeier, Adelita/A-9239-2013 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) FX We thank Dr. Renato C. Marinoni (Departamento de Zoologia - Universidade Federal do Parana) for providing the material, Dr. Cibele S. Ribeiro-Costa for support and the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) for granting a Doctoral Fellowship to the first author. We are grateful to D. Nickle and A. L. Norrbom (Systematic Entomology Laboratory, ARS, USDA, Washington, DC) and C. Staines (Department of Entomology, Smithsonian Institution, Washington, DC) for reviewing earlier versions of this manuscript and providing valuable suggestions. This research represents contribution n degrees. 1,786 of the Departamento de Zoologia, Universidade Federal do Parana, Curitiba, Brazil. NR 11 TC 5 Z9 5 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 656 EP 665 DI 10.4289/0013-8797-111.3.656 PG 10 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800011 ER PT J AU Pogue, MG AF Pogue, Michael G. TI THREE NEW CRYPTIC SPECIES WITHIN THE DARGIDA PROCINCTUS (GROTE) COMPLEX (LEPIDOPTERA: NOCTUIDAE: HADENINAE) FROM THE NEOTROPICS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE host plants; new species; New World; taxonomy ID LIRIOMYZA-HUIDOBRENSIS DIPTERA; DNA BARCODES; SKIPPER BUTTERFLIES; AGROMYZIDAE; GENUS AB Based on morphological analysis, the species Dargida procinctus (Grote), currently considered to be widespread from Canada to Bolivia, is found to include three previously unrecognized species: Dargida spinicassida, n. sp., from northern Mexico; Dargida juxta, n. sp., from southern Mexico and Costa Rica; and Dargida lilium, n. sp., from Bolivia. Adults and male and female genitalia of all four species are illustrated. Dargida grammivora Walker and Dargida meridionalis (Hampson) are closely related species that could be confused with those of the Dargida procinctus complex. Adults and male and female genitalia of these are illustrated for comparison. A key is provided for differentiation of these six closely related species. C1 USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst, Washington, DC 20013 USA. RP Pogue, MG (reprint author), USDA ARS, Systemat Entomol Lab, PSI, Smithsonian Inst, POB 37012,NMNH,MRC-168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov NR 23 TC 1 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 686 EP 697 DI 10.4289/0013-8797-111.3.686 PG 12 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800013 ER PT J AU Kment, P Henry, TJ Fryda, J AF Kment, Petr Henry, Thomas J. Fryda, Jiri TI Neostusakia, a New Name for Preoccupied Stusakia Kment and Henry, 2008 (Hemiptera: Heteroptera: Berytidae) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Kment, Petr] Natl Museum, Dept Entomol, CZ-14800 Prague 4, Czech Republic. [Henry, Thomas J.] USDA ARS, Systemat Entomol Lab, PSI, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Fryda, Jiri] Czech Geol Survey, CZ-11821 Prague 1, Czech Republic. [Fryda, Jiri] CULS, Fac Environm Sci, Prague 16521 6, Czech Republic. RP Kment, P (reprint author), Natl Museum, Dept Entomol, Kunratice 1, CZ-14800 Prague 4, Czech Republic. EM sigara@post.cz; thomas.henry@ars.usda.gov; bellerophon@seznam.cz RI Fryda, Jiri/C-3319-2008 OI Fryda, Jiri/0000-0003-2410-3293 NR 8 TC 0 Z9 1 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 755 EP 756 DI 10.4289/0013-8797-111.3.755 PG 2 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800021 ER PT J AU Lamas, G Robbins, RK AF Lamas, Gerardo Robbins, Robert K. TI A Replacement Name for Thecla maculata Lathy, 1936 (Lepidoptera: Lycaenidae, Eumaeini) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Lamas, Gerardo] Univ Nacl Mayor San Marcos, Museo Hist Nat, Lima 14, Peru. [Robbins, Robert K.] Smithsonian Inst, Washington, DC 20013 USA. RP Lamas, G (reprint author), Univ Nacl Mayor San Marcos, Museo Hist Nat, Apartado 14-0434, Lima 14, Peru. EM glamasm@unmsm.edu.pe; RobbinsR@SI.edu NR 5 TC 1 Z9 1 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2009 VL 111 IS 3 BP 758 EP 758 DI 10.4289/0013-8797-111.3.758 PG 1 WC Entomology SC Entomology GA 481UZ UT WOS:000268838800023 ER PT J AU Silverman, JM Mazzali, P Chornock, R Filippenko, AV Clocchiatti, A Phillips, MM Ganeshalingam, M Foley, RJ AF Silverman, Jeffrey M. Mazzali, Paolo Chornock, Ryan Filippenko, Alexei V. Clocchiatti, Alejandro Phillips, Mark M. Ganeshalingam, Mohan Foley, Ryan J. TI Optical Spectroscopy of the Somewhat Peculiar Type IIb Supernova 2001ig SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CORE-COLLAPSE SUPERNOVAE; HUBBLE-SPACE-TELESCOPE; NEBULAR SPECTRA; IB SUPERNOVAE; PROGENITOR; 1993J; STAR; PHOTOMETRY; EMISSION; GALAXIES AB Here we present previously unpublished optical spectra of supernova (SN) 2001ig, a Type IIb SN, from about a week after explosion until nearly one year later. The earliest spectrum consists of only a few broad absorption features, but soon more common Type II SN features including hydrogen P Cygni profiles and helium absorption become apparent. At later times, as the H features fade and the He I absorption becomes more prominent, we observe the SN to transition from a Type II to a Type Ib. Finally, observations after 250 days past explosion show a nebular-phase SN spectrum with one of the largest magnesium to oxygen intensity ratios ever seen. Additionally, we present models of the late-time spectra which indicate that the inner ejecta consist of similar to 1.15 M(circle dot) of material, most of which (by mass) is in the form of oxygen, with similar to 0.13 M(circle dot) of (56)Ni and essentially no hydrogen. C1 [Silverman, Jeffrey M.; Chornock, Ryan; Filippenko, Alexei V.; Ganeshalingam, Mohan; Foley, Ryan J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Ist Naz Astrofis Oss Astron, I-35122 Padua, Italy. [Clocchiatti, Alejandro] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Phillips, Mark M.] Las Campanas Observ, La Serena, Chile. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Silverman, JM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM JSilverman@astro.berkeley.edu FU National Science Foundation [AST-0607485]; FONDAP [15010003]; [68.D-0571(A)]; [69.D-0438(A)]; [170.A-0519(A)]; [68.A-0443]; [P06-045-F]; [PFB 06/09] FX We are grateful to the staffs at the Keck Observatory, ESO, and Las Campanas Observatory for their support. We thank the following for their assistance with some of the observations and data reduction: F. Barrientos, R. Carlberg, M. Gladders, S. W. Jha, T. Matheson, J. L. Prieto, and B. Leibundgut. We especially thank J. Maund and his collaborators for allowing us to reproduce one of their spectra. 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 the National Aeronautics and Space Administration; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. ESO VLT data were acquired under programs 68.D-0571(A), 69.D-0438(A), and 170.A-0519(A), and La Silla data under program 68.A-0443. A. V. F.'s group is supported by the National Science Foundation through grant AST-0607485. A. C. is supported by grants P06-045-F ICM de MIDEPLAN, Basal CATA PFB 06/09, and FONDAP No. 15010003. NR 60 TC 23 Z9 23 U1 0 U2 1 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 JUL PY 2009 VL 121 IS 881 BP 689 EP 698 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 465QK UT WOS:000267601700002 ER PT J AU Songsasen, N Fickes, A Pukazhenthi, BS Wildt, DE AF Songsasen, N. Fickes, A. Pukazhenthi, B. S. Wildt, D. E. TI Follicular Morphology, Oocyte Diameter and Localisation of Fibroblast Growth Factors in the Domestic Dog Ovary SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Article; Proceedings Paper CT 6th International Symposium on Canine and Feline Reproduction CY JUL 09-11, 2008 CL Vienna Univ Vet Sci, Vienna, AUSTRIA HO Vienna Univ Vet Sci ID IMMUNOHISTOCHEMICAL LOCALIZATION; PRIMORDIAL FOLLICLE; EXPRESSION; BITCH; FOLLICULOGENESIS; DIFFERENTIATION; PROGESTERONE; TRANSITION; PROMOTES AB Remarkably little is known about folliculogenesis in the dog. Objectives were to characterise (1) changes in follicle/oocyte diameter and granulosa cell number and (2) localisation of fibroblast growth factor (FGF)-2 and FGF-7 during dog ovarian follicle development. Fourteen ovarian pairs were excised and processed for histological evaluation. Two to four serial sections/bitch were stained with hematoxylin, and follicle/oocyte diameters and granulosa cell number were determined at each developmental stage. Mean follicle and oocyte size were compared among stages by one-way analysis of variance. Relationships between follicle and oocyte size and granulosa cell number were determined using correlation and regression analysis, respectively. Another eight serial sections/bitch were processed for immunostaining to determine FGF-2 and FGF-7 localisation. Primordial and primary follicles were similar in size, but smaller than the progressively increasing (p < 0.05) diameter of the later stages. Oocyte diameter gradually increased (p < 0.05) among oocytes derived from primordial, primary, secondary and early antral follicles with no difference (p > 0.05) thereafter. Oocyte size and granulosa cell number increased (p < 0.01) with follicular diameter. Except during anoestrus, FGF-2 occurred in oocytes and granulosa cells of primordial to secondary follicles. In adult bitches, FGF-7 was localised in granulosa cells of primary and secondary follicles and also occurred in the theca layer of antral follicles during prooestrus and oestrus. In summary, folliculogenesis in the domestic dog occurs in two phases: pre-antral phase characterised by increasing follicle size in association with oocyte growth and granulosa cell proliferation and antral phase linked with marked granulosa cell proliferation and accumulation of antral cavity fluid. Finally, the temporal localisation pattern of FGF-2 implies its role in follicular activation, whereas FGF-7 activities appear related to later folliculogenesis. C1 [Songsasen, N.; Fickes, A.; Pukazhenthi, B. S.; Wildt, D. E.] Ctr Species Survival, Dept Reprod Sci, Front Royal, VA USA. RP Songsasen, N (reprint author), Conservat & Res Ctr, Smithsonians Natl Zool Pk, Front Royal, VA 22630 USA. EM songsasenn@si.edu FU NCRR NIH HHS [K01RR020564, K01 RR020564, K01 RR020564-03] NR 35 TC 15 Z9 16 U1 0 U2 8 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD JUL PY 2009 VL 44 BP 65 EP 70 DI 10.1111/j.1439-0531.2009.01424.x PG 6 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 467QF UT WOS:000267756400011 PM 19754538 ER PT J AU Schon, J Neumann, S Wildt, DE Pukazhenthi, BS Jewgenow, K AF Schoen, J. Neumann, S. Wildt, D. E. Pukazhenthi, B. S. Jewgenow, K. TI Localization of Oestrogen Receptors in the Epididymis During Sexual Maturation of the Domestic Cat SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Article; Proceedings Paper CT 6th International Symposium on Canine and Feline Reproduction CY JUL 09-11, 2008 CL Vienna Univ Vet Sci, Vienna, AUSTRIA HO Vienna Univ Vet Sci ID REPRODUCTIVE-TRACT; ALPHA; BETA; RAT; SPERMATOGENESIS; EXPRESSION; ANDROGEN; TESTIS; MICE AB Oestrogens are involved in regulation of spermatogenesis and sperm maturation and are essential for male fertility. To study the role of oestrogens on epididymal function in the domestic cat, we analyzed the localization patterns of oestrogen receptors (ERs) within the epididymis of juvenile, pubertal and adults using immunohistochemistry. Cat epididymal tissues obtained during routine castrations were fixed in chilled Bouin's solution and processed for immunohistochemistry with ER-specific antibodies. For a certain receptor type, ER localization was influenced by donor age. In the juvenile epididymis, ER alpha was localized in the nuclei of epithelial cells of efferent ducts and undifferentiated epithelium of the ductus epididymis. During puberty, ER alpha localization in the undifferentiated epithelium of the epididymis shifted from the nuclei to the cytoplasm and plasma membrane. Oestrogen receptor-alpha level was highest in the pubertal and adult epididymis, especially within the cytoplasm and in plasma membranes of caput epithelial cells. This finding was suggestive of a role in fluid reabsorption within the efferent ducts and the epididymis. In corpus and cauda regions, ER alpha was less abundant, suggesting a minor role for oestrogens in sperm storage areas. Interestingly, localization of ER beta was neither influenced by age nor location within the epididymis and was ubiquitous throughout. Results demonstrate that oestrogen actions within the epididymis may be predominantly mediated through ER alpha during sexual maturation in the domestic cat. C1 [Schoen, J.] Free Univ Berlin, Inst Vet Biochem, D-1000 Berlin, Germany. [Neumann, S.; Jewgenow, K.] Inst Zoo Biol & Wildlife Res IZW, Dept Reprod Biol, Berlin, Germany. [Wildt, D. E.; Pukazhenthi, B. S.] Smithsonians Natl Zool Pk, Dept Reprod Sci, Conservat & Res Ctr, Front Royal, VA USA. RP Schon, J (reprint author), Free Univ Berlin, Inst Vet Biochem, D-1000 Berlin, Germany. EM schoen.jennifer@vetmed.fu-berlin.de NR 28 TC 11 Z9 11 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 EI 1439-0531 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD JUL PY 2009 VL 44 SU 2 BP 294 EP 301 DI 10.1111/j.1439-0531.2009.01391.x PG 8 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 467QF UT WOS:000267756400063 PM 19754590 ER PT J AU Haffner, LM Dettmar, RJ Beckman, JE Wood, K Slavin, JD Giammanco, C Madsen, GJ Zurita, A Reynolds, RJ AF Haffner, L. M. Dettmar, R. -J. Beckman, J. E. Wood, K. Slavin, J. D. Giammanco, C. Madsen, G. J. Zurita, A. Reynolds, R. J. TI The warm ionized medium in spiral galaxies SO REVIEWS OF MODERN PHYSICS LA English DT Review DE galaxies; interstellar matter ID DIFFUSE INTERSTELLAR-MEDIUM; EDGE-ON GALAXIES; HIGH-VELOCITY CLOUDS; H-ALPHA-EMISSION; CARLO PHOTOIONIZATION CODE; TURBULENT MIXING LAYERS; HIGH GALACTIC LATITUDE; RESOLUTION X-RAY; MILKY-WAY; HII-REGIONS AB This article reviews observations and models of the diffuse ionized gas that permeates the disk and halo of our Galaxy and others. It was inspired by a series of invited talks presented during an afternoon scientific session of the 65th birthday celebration for Professor Carl Heiles held at Arecibo Observatory in August 2004. This review is in recognition of Carl's long-standing interest in and advocacy for studies of the ionized as well as the neutral components of the interstellar medium. C1 [Haffner, L. M.; Reynolds, R. J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Dettmar, R. -J.] Ruhr Univ Bochum, Astron Inst, Bochum, Germany. [Beckman, J. E.; Giammanco, C.] Inst Astrofis Canarias, Tenerife, Spain. [Beckman, J. E.] CSIC, Madrid, Spain. [Wood, K.] Univ St Andrews, St Andrews, Fife, Scotland. [Slavin, J. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Madsen, G. J.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Zurita, A.] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain. RP Haffner, LM (reprint author), Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RI Zurita, Almudena/A-2218-2015; OI Giammanco, Corrado/0000-0001-5405-0095; Haffner, Lawrence/0000-0002-9947-6396 FU National Science Foundation [AST 02-04973, AST 06-07512, AST 04-01416]; University of Wisconsin's Graduate School; University of Sydney; DFG SFB 591 [50 OR 9707]; Spanish Ministry of Science and Technology [AYA2001-0435]; Ministry of Education and Science [AYA2004-08251-C02-01]; Consejeria de Educacion y Ciencia de la Junta de Andalucia, Spain FX We thank Carl Heiles for his contributions, enthusiasm, encouragement, and insights over the years. We also thank the meeting organizers, Y.-H. Chu and T. Troland, without whom this paper would not have been written. We thank two anonymous referees, whose comments and criticisms resulted in an improved paper. We also thank A. Ferguson, C. Hoopes, and J. Rossa for access to high-quality versions of their figures as well as their permission to include them in this review. We are also very grateful to our students and collaborators for their support and contributions. R. J. R. thanks Don Cox for many valuable conversations over the years regarding the nature of the WIM. R.J.R. and L. M. H. were supported by the National Science Foundation through Grants No. AST 02-04973 and No. AST 06-07512, with assistance from the University of Wisconsin's Graduate School, Department of Astronomy, and Department of Physics. G.J.M. acknowledges support from the University of Sydney Postdoctoral Fellowship Program and the National Science Foundation through Grant No. AST 04-01416. R.-J.D.'s work at Ruhr University-Bochum in this field is supported through DFG SFB 591 and through Deutsches Zentrum fur Luft-und Raumfahrt through Grant No. 50 OR 9707. J.E.B., A.Z., and C. G. acknowledge support through Grant No. AYA2001-0435 from the Spanish Ministry of Science and Technology and Grant No. AYA2004-08251-C02-01 from the Ministry of Education and Science. A.Z. thanks the Consejeria de Educacion y Ciencia de la Junta de Andalucia, Spain, for support. NR 171 TC 100 Z9 100 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0034-6861 EI 1539-0756 J9 REV MOD PHYS JI Rev. Mod. Phys. PD JUL-SEP PY 2009 VL 81 IS 3 BP 969 EP 997 DI 10.1103/RevModPhys.81.969 PG 29 WC Physics, Multidisciplinary SC Physics GA 500DW UT WOS:000270279000002 ER PT J AU Clough, GW AF Clough, G. Wayne TI FROM THE CASTLE Forever Yours 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 JUL PY 2009 VL 40 IS 4 BP 26 EP 26 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 462ND UT WOS:000267359600012 ER PT J AU Keller, JK Weisenhorn, PB Megonigal, JP AF Keller, Jason K. Weisenhorn, Pamela B. Megonigal, J. Patrick TI Humic acids as electron acceptors in wetland decomposition SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Anaerobic decomposition; Carbon dioxide; Humic substances; Methane; Wetlands ID DISSOLVED ORGANIC-MATTER; METHANE PRODUCTION; NORTHERN WETLANDS; CARBON; RESPIRATION; SUBSTANCES; MINERALIZATION; HYDROGEN; NITROGEN; SOILS AB Decomposition of organic matter in inundated wetland soils requires a number of interdependent microbial processes that ultimately generate CO(2) and CH(4). Largely as the result of anaerobic decomposition, wetland soils store globally significant amounts of organic carbon and are currently net sources of CH(4) to the atmosphere. Given the importance of wetlands in the global carbon cycle, it is important to understand controls on anaerobic decomposition in order to predict feedbacks between wetland soils and global climate change. One perplexing pattern observed in many wetland soils is the high proportion Of CO(2) resulting from anaerobic decomposition that cannot be explained by any measured pathway of microbial respiration. Recent studies have hypothesized that humic substances, and in particular solid-phase humic substances in wetland soils, can support anaerobic microbial respiration by acting as organic electron acceptors. Humic substances may thus account for much of the currently unexplained CO(2) measured during decomposition in wetland soils. Here we demonstrate that humic acids extracted from a variety of wetland soils act as either electron donors or electron acceptors and alter the ratio of CO(2):CH(4) produced during anaerobic laboratory incubations. Our results suggest that soil-derived humic substances may play an important, and currently unexplored, role in anaerobic decomposition in wetland soils. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Keller, Jason K.] Chapman Univ, Dept Biol Sci, Orange, CA 92866 USA. [Keller, Jason K.; Weisenhorn, Pamela B.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Weisenhorn, Pamela B.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. RP Keller, JK (reprint author), Chapman Univ, Dept Biol Sci, 1 Univ Dr, Orange, CA 92866 USA. EM jkeller@chapman.edu FU National Science Foundation FX Sara McQueeney provided valuable assistance in the field and the laboratory. JKK was supported by a Smithsonian Institution Post-Doctoral Fellowship. PBW conducted her work at the Smithsonian Environmental Research Center as a Smithsonian Institution research intern. This work was funded by grants from the National Science Foundation to JKK and JPM. Comments from an anonymous reviewer greatly improved this manuscript. NR 29 TC 50 Z9 52 U1 7 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUL PY 2009 VL 41 IS 7 BP 1518 EP 1522 DI 10.1016/j.soilbio.2009.04.008 PG 5 WC Soil Science SC Agriculture GA 467XB UT WOS:000267775300019 ER PT J AU Ceruzzi, PE AF Ceruzzi, Paul E. TI "A Large Canvas" Melvin Kranzberg and Carroll W. Pursell Jr., eds., Technology in Western Civilization SO TECHNOLOGY AND CULTURE LA English DT Article ID HISTORY C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2009 VL 50 IS 3 BP 658 EP 668 PG 11 WC History & Philosophy Of Science SC History & Philosophy of Science GA 477KH UT WOS:000268517500011 ER PT J AU Warner, DJ AF Warner, Deborah Jean TI The Microscope and the Eye: A History of Reflections, 1740-1870 SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Warner, Deborah Jean] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2009 VL 50 IS 3 BP 690 EP 691 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 477KH UT WOS:000268517500022 ER PT J AU Grim, KC Wolfe, MJ Edwards, M Kaufman, J Onjukka, S Moran, P Wolf, JC AF Grim, K. C. Wolfe, M. J. Edwards, M. Kaufman, J. Onjukka, S. Moran, P. Wolf, J. C. TI Epizootic Ameloblastomas in Chinook Salmon (Oncorhynchus tshawytscha) of the Northwestern United States SO VETERINARY PATHOLOGY LA English DT Article DE Ameloblastoma; Chinook salmon; epizootic; Oncorhynchus tshawytscha ID EFFECTIVE POPULATION-SIZE; LINKAGE DISEQUILIBRIUM; ELECTRON-MICROSCOPY; PACIFIC SALMON; CELL-LINE; FISH; VIRUS; CARCINOGENESIS; PAPILLOMA; NEOPLASMS AB Abnormal growths were observed on the lips and in the oral cavities of 2- and 3-year-old Chinook salmon (Oncorhynchus tshawytscha) maintained in one freshwater and one saltwater captive fish-rearing facility in the Columbia River (Pacific Northwest). Initially presenting as bilaterally symmetrical, red, irregular plaques on oral mucosal surfaces, the lesions developed progressively into large, disfiguring masses. Of the 502 natural parr collected for captive broodstock, 432 (86%) displayed these tumors, whereas cohort salmon (i.e., same year classes) in these same facilities remained unaffected. Morphologically similar neoplasms were collected occasionally from adult Chinook salmon that had returned to their natal streams. Histologic features of the tumors suggested that they were derived from the portion of dental lamina destined to form tooth root sulci; therefore, these neoplasms were diagnosed as ameloblastomas. The lesions also resembled archived specimens of Chinook salmon oral tumors, which had been described decades earlier. Etiologic investigations performed during the current outbreak included bacteriologic, virologic, genetic, ultrastructural analyses, and cohabitation exposure studies. Results of these efforts did not indicate an obvious genetic basis for this syndrome, attempts to isolate potentially causative viruses or bacteria were negative, and disease transmission to naive fish was unsuccessful. A few intracytoplasmic hexagonal structures, possibly consistent with viral particles (similar to 100 nm), were observed ultrastructurally in a tumor cell from 1 of 6 specimens submitted for transmission electron microscopy. Although the presence of these particles does not constitute sufficient evidence for causality, an infectious or multifactorial etiology seems plausible. C1 [Wolfe, M. J.; Wolf, J. C.] Expt Pathol Labs Inc, Registry Tumors Lower Anim, Sterling, VA 20166 USA. [Grim, K. C.] US EPA, Off Sci Coordinat & Policy, Washington, DC 20460 USA. [Grim, K. C.] Smithsonian Natl Zool Pk, Conservat & Res Ctr, Ctr Species Survival, Front Royal, VA USA. [Edwards, M.] Enterprise Field Off, Nez Perce Tribe Dept Fisheries Resources Manageme, Enterprise, OR USA. [Kaufman, J.] Oregon State Univ, Dept Microbiol, Oregon Dept Fish & Wildlife, Corvallis, OR 97331 USA. [Onjukka, S.] Eastern Oregon Univ, Oregon Dept Fish & Wildlife, Fish Hlth Serv, La Grande, OR USA. [Moran, P.] NOAA, NW Fisheries Sci Ctr, Conservat Biol Div, Seattle, WA USA. RP Wolf, JC (reprint author), Expt Pathol Labs Inc, Registry Tumors Lower Anim, 45600 Terminal Dr, Sterling, VA 20166 USA. EM jwolf@epl-inc.com FU Experimental Pathology Laboratories, Inc. [N02-CB-27034]; Bonneville Power Administration [198909600] FX This project was performed, in part, by using the services provided by the National Cancer Institute's Registry of Tumors in Lower Animals, operated under contract by Experimental Pathology Laboratories, Inc., N02-CB-27034. We also thank the contributions and efforts of Phyllis Spero (RTLA) and Debbie Haegele (RTLA) for organizing slide materials. We thank Dr. Richard R. Dubielzig, DVM, for aiding in the diagnosis of these tumors, Dr. Jerry R. Heidel, DVM, for histopathologic work on tumor tissues, Dr. Lee Harrell, DVM, for tissue collection and input on managing this problem in the Captive Broodstock Program. We also thank Dr. James Casey for conducting viral-probe testing, Marla Chaney for assistance with tumor sampling and taking care of these fish, Sharon Vendshus for performing numerous fish necropsies, and Glenda O'Connor for sampling and necropsying the fish from Northeast Oregon. This work was supported in part by Bonneville Power Administration project 198909600. NR 41 TC 5 Z9 5 U1 1 U2 5 PU AMER COLL VET PATHOLOGIST PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0300-9858 J9 VET PATHOL JI Vet. Pathol. PD JUL PY 2009 VL 46 IS 4 BP 622 EP 635 DI 10.1354/vp.08-VP-0150-W-FL PG 14 WC Pathology; Veterinary Sciences SC Pathology; Veterinary Sciences GA 475UY UT WOS:000268388700011 PM 19276053 ER PT J AU Lee, CF Swietojanska, J Staines, CL AF Lee, Chi-Feng Swietojanska, Jolanta Staines, Charles L. TI Prionispa houjayi (Coleoptera: Chrysomelidae: Cassidinae: Oncocephalini), a Newly Recorded Genus and New Species from Taiwan, with a Description of Its Immature Stages and Notes on Its Bionomy SO ZOOLOGICAL STUDIES LA English DT Article DE Morphology; Larva; Pupa; Liliaceae; Disporum ID INSTAR LARVA AB Chi-Feng Lee, Jolanta Swietojanska, and Charles L. Staines (2009) Prionispa houjayi (Coleoptera: Chrysomelidae: Cassidinae: Oncocephalini), a newly recorded genus and new species from Taiwan, with a description of its immature stages and notes on its bionomy. Zoological Studies 48(4): 558-568. The larva, pupa, and adult of Prionispa houjayi sp. nov., a new species in the Oncocephalini are described and illustrated in detail. Some autapomorphies of the immature stages of this new species are proposed by comparing it to Chaeridiona picea Baly, C. thailandica Kimoto, and Oncocephala quadrilobata (Guerin), including the quadrate abdominal apex and prominent labial palpi in the larva, and the lateral scoli of the pronotum in the pupa. Prionispa houjayi sp. nov. larvae mine the leaves of Disporum Salisbury (Liliaceae). This is the first host record of the Liliaceae for the subfamily Cassidinae. http://zoolstud.sinica.edu-tw/JournaIs/48.4/558.pdf C1 [Lee, Chi-Feng] Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Taiwan. [Swietojanska, Jolanta] Univ Wroclaw, Inst Zool, PL-51148 Wroclaw, Poland. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Lee, CF (reprint author), Agr Res Inst Taiwan, Appl Zool Div, 189 Chung Cheng Rd, Taichung 413, Taiwan. EM cflee@gate.sinica.edu.tw; sindiola@biol.uni.wroc.pl; stainesc@si.edu RI stud, zool/G-4030-2011 FU University of Wroclaw [1018/DS/IZ/08]; National Science Council [NSC96-2313-B-055MY2] FX We thank C.S. Chaboo (University of Kansas, KS, USA), and TN. Seeno and C. L. Bellamy (California Department of Food and Agriculture, CA, USA) for providing valuable literature. We thank the Taiwan Chrysomelid Research Team for assisting with field collection and observations, among whom M.H. Tsou, H.J. Chen, and H.T. Cheng provided photographs, and C.K. Yang identified the host plant. J. Swietojanska thanks the University of Wroclaw (project no. 1018/DS/IZ/08), and C.F. Lee thanks the National Science Council (NSC96-2313-B-055MY2) for financial assistance. NR 18 TC 1 Z9 2 U1 0 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1021-5506 EI 1810-522X J9 ZOOL STUD JI Zool. Stud. PD JUL PY 2009 VL 48 IS 4 BP 558 EP 568 PG 11 WC Zoology SC Zoology GA 484UD UT WOS:000269072100013 ER PT J AU Giraldo-Canas, D Peterson, PM AF Giraldo-Canas, Diego Peterson, Paul M. TI Revision of the genus Sporobolus (Poaceae: Chloridoideae: Sporobolinae) for northwest South America: Peru, Ecuador, Colombia, and Venezuela SO CALDASIA LA Spanish DT Article DE Sporobolus; Sporobolinae; Chloridoideae; Poaceae; Neotropical grasses; Flora of South America ID SUBFAMILY CHLORIDOIDEAE; GRAMINEAE; EVOLUTION; GRASSES; CLASSIFICATION; PHYLOGENETICS; SEQUENCES; SYSTEMS AB A taxonomic treatment of Sporobolus for northwest South America is given. Eleven species are recognized in the study area. Keys for determining the species, morphological descriptions, and illustrations are provided. Morphological relationships, geographical distributions, ecological preferences, common uses, and vernacular names are given. Sporobolus lasiophyllus Pilg. is lectotypified. Sporobolus pilfer (Trin.) Kunth, Sporobolus tenuissimus (Mart. ex Schrank) Kuntze, and Sporobolus virginicus (L.) Kunth are reported in Colombia for the first time. Sporobolus brasiliensis (Raddi) Hack. (=Eragrostis airoides Nees) and Sporobolus domingensis (Trin.) Kunth are excluded from this treatment. C1 [Giraldo-Canas, Diego] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, DC, Colombia. [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Giraldo-Canas, D (reprint author), Univ Nacl Colombia, Inst Ciencias Nat, Apartado 7495, Bogota, DC, Colombia. EM dagiraldo@unal.edu.co; peterson@si.edu NR 66 TC 4 Z9 8 U1 0 U2 3 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 PD JUN 30 PY 2009 VL 31 IS 1 BP 41 EP 76 PG 36 WC Plant Sciences; Multidisciplinary Sciences; Zoology SC Plant Sciences; Science & Technology - Other Topics; Zoology GA 476PE UT WOS:000268453700006 ER PT J AU Kress, WJ Betancur, J AF Kress, W. John Betancur, Julio TI A New Species of Heliconia (Heliconiaceae) from the Choco Region of Colombia SO CALDASIA LA Spanish DT Article DE Flora of Colombia; Heliconia; Heliconiaceae; Neotropical plantas; Zingiberales AB Heliconia samperiana W. J. Kress & Betancur, a new species from the Colombian Choco Region is described and illustrated. Information about its taxonomic relationships, conservation status, distribution, and habitat is also presented. C1 [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Betancur, Julio] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. RP Kress, WJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM kressj@si.edu; jcbetancurb@unal.edu.co NR 10 TC 0 Z9 0 U1 0 U2 0 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 PD JUN 30 PY 2009 VL 31 IS 1 BP 99 EP 104 PG 6 WC Plant Sciences; Multidisciplinary Sciences; Zoology SC Plant Sciences; Science & Technology - Other Topics; Zoology GA 476PE UT WOS:000268453700008 ER PT J AU Brueckner, HK Lallemant, HGA Sisson, VB Harlow, GE Hemming, SR Martens, U Tsujimori, T Sorensen, SS AF Brueckner, Hannes K. Lallemant, Hans G. Ave Sisson, Virginia B. Harlow, George E. Hemming, Sidney R. Martens, Uwe Tsujimori, Tatsuki Sorensen, Sorena S. TI Metamorphic reworking of a high pressure-low temperature melange along the Motagua fault, Guatemala: A record of Neocomian and Maastrichtian transpressional tectonics SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Sm-Nd geochronology; HP/LT eclogites; strike-slip and subduction zone processes; oblique collisional tectonics ID SUBDUCTION ZONES; LAWSONITE ECLOGITE; PLATE BOUNDARY; DEFORMATION; TERRANES; AMERICA; COMPLEX; JADEITE AB The Guatemala suture zone is a major east-west left-lateral strike slip boundary that separates the North American and Caribbean plates in Guatemala. The Motagua fault, the central active strand of the suture zone, underwent two major collisional events within a system otherwise dominated by strike-slip motion. The first event is recorded by high-pressure/low temperature (HP/LT) eclogites and related rocks that occur within serpentinites both north and south of the Motagua fault. Lawsonite eclogites south of the fault are not significantly retrograded and give Ar-40/Ar-39 ages of 125-116 Ma and Sm-Nd mineral isochrons of 144-132 Ma. Eclogites north of the fault give similar Sm-Nd isochron ages (131-126 Ma) but otherwise differ in that they are strongly overprinted by a lower pressure assemblage and, along with associated HP/LT rocks, give much younger Ar-40/Ar-39 ages of 88-55 Ma indicating a later amphibolite facies metamorphic event. We propose therefore that all serpentinite hosted eclogites along the Motagua fault formed at essentially the same time in different parts of a laterally extensive Lower Cretaceous forearc subduction system, but subsequently underwent different histories. The southern assemblages were thrust southwards (present coordinates) immediately after HP metamorphism whereas the northern association was retrograded during a later collision that thrust it northward at ca. 70 Ma. They were subsequently juxtaposed opposite each other by major strike slip motion. This model implies that the HP rocks on opposing sides of the Motagua fault evolved along a plate boundary that underwent both dip slip and strike slip motion throughout the Late Cretaceous as a result of oblique convergence. The juxtaposition of a convergent and strike slip system means that HP/LT rocks within serpentinites can be found at depth along much of the modern Guatemala suture zone and its eastward extension into the northern Caribbean. Both sets of assemblages were exhumed relatively recently by the uplift of mountain ranges on both sides of the fault caused by movement along a restraining bend. Recent exhumation explains the apparently lack of offset of surface outcrops along a major strike slip fault. (C) 2009 Elsevier B.V. All rights reserved. C1 [Brueckner, Hannes K.; Hemming, Sidney R.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Brueckner, Hannes K.] CUNY Queens Coll, Sch Earth & Environm Sci, Flushing, NY 11367 USA. [Brueckner, Hannes K.] CUNY, Grad Ctr, Flushing, NY 11367 USA. [Lallemant, Hans G. Ave] Rice Univ, Dept Earth Sci, Houston, TX 77005 USA. [Sisson, Virginia B.] Univ Houston, Dept Geosci, Houston, TX 77204 USA. [Brueckner, Hannes K.; Harlow, George E.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Martens, Uwe] Stanford Univ, Dept Geog & Environm Sci, Stanford, CA 94305 USA. [Tsujimori, Tatsuki] Okayama Univ, Inst Study Earths Interior, Pheasant Mem Lab Geochem & Cosmochem, Tottori 6820193, Japan. [Sorensen, Sorena S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Brueckner, HK (reprint author), Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. EM hannes@ldeo.columbia.edu RI Tsujimori, Tatsuki/D-2677-2009 OI Tsujimori, Tatsuki/0000-0001-9202-7312 FU NSF [EAR 0309832, EAR0309320, EAR0309116]; IGCP [546]; Lamont-Doherty Earth Observatory [7265] FX This work was funded by NSF Grants EAR 0309832 to SRH and HKB, EAR0309320 to GEH, and EAR0309116 to HGAL. This project is part of IGCP Project 546 on "Subduction Zones of the Caribbean." We thank Carlos Gonzales for field assistance. We appreciate constructive reviews by Jim Pindell, Sarah Roeske, Taras Gerya, Bradley Hacker and an anonymous reviewer. This contribution is publication number 7265 of Lamont-Doherty Earth Observatory. NR 45 TC 42 Z9 43 U1 0 U2 12 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 JUN 30 PY 2009 VL 284 IS 1-2 BP 228 EP 235 DI 10.1016/j.epsl.2009.04.032 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 476KK UT WOS:000268438900025 ER PT J AU Helgen, KM Helgen, LE Wilson, DE AF Helgen, Kristofer M. Helgen, Lauren E. Wilson, Don E. TI Pacific Flying Foxes (Mammalia: Chiroptera): Two New Species of Pteropus from Samoa, Probably Extinct SO AMERICAN MUSEUM NOVITATES LA English DT Review ID BAT EMBALLONURA-SEMICAUDATA; MONKEY-FACED BATS; WORLD FRUIT BATS; AMERICAN-SAMOA; SOUTH-PACIFIC; PREHISTORIC EXTINCTION; NIUE-ISLAND; OLD-WORLD; WESTERN POLYNESIA; SEED DISPERSERS AB Two new species or flying foxes (genus Pteropus) from the Samoan archipelago are described on the basis of modern museum specimens collected in the mid-19th century. A medium-sized species (P. allenorum, n. sp.) is introduced from the island of Upolu (Independent Samoa), based on a specimen collected in 1856 and deposited in the Academy of Natural Sciences of Philadelphia. It has not been collected again, and we regard it as almost certainly extinct. This species is smaller bodied and has much smaller teeth than both extant congeners recorded in the contemporary fauna of Samoa (Pteropus samoensis and P. tonganus). The closest relative of this new species may be Pteropus fundatus of northern Vanuatu. The disjunct historical distribution of these two small-toothed flying foxes (in Vanuatu and Samoa) suggests that similar species may have been more extensively distributed in the remote Pacific in the recent past. Another species, a very large flying fox with large teeth (P. coxi, n. sp.), is described from two skulls collected in Samoa in 1839-1841 during the U.S. Exploring Expedition; it too has not been collected since. This robust species resembles Pteropus samoensis and Pteropus anetianus of Vanuatu in craniodental conformation but is larger than other Polynesian Pteropus, and in some features it is ecomorphologically convergent on the Pacific monkey-faced bats (the pteropodid genera Pteralopex and Mirimiri). On the basis of eyewitness reports from the early 1980s, it is possible that this species survived until recent decades, or is still extant. These two new Samoan species join Pteropus tokudae of Guam, P. pilosus of Palau, P. subniger of the Mascarenes, and P. brunneus of coastal north-eastern Australia as flying foxes with limited insular distributions that survived at least until the 19th century but are now most likely extinct. C1 [Helgen, Kristofer M.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, Washington, DC 20013 USA. [Helgen, Kristofer M.; Helgen, Lauren E.; Wilson, Don E.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Helgen, Kristofer M.] Bernice P Bishop Museum, Honolulu, HI USA. [Helgen, Lauren E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Helgen, KM (reprint author), Amer Museum Nat Hist, Div Vertebrate Zool Mammal, Washington, DC 20013 USA. EM helgenk@si.edu; helgenl@si.edu; wilsond@si.edu FU Smithsonian Institution; South Australian Museum; Australian-American Fulbright Foundation; National Science Foundation; American Society of Mammalogists; University of Adelaide FX Reports like ours are possible only because critical specimens have been preserved and curated since their deposition, decades and even centuries ago, in natural history museums around the world. We thank Darrin Lunde, Eileen Westwig, and Nancy Simmons (AMNH), Sandy Ingleby and Tish Ennis (AM), Paula Jenkins, Daphne H * ills, and Richard Harbord (BMNH), Robert Asher, Irene Thomas, and Peter Giere (ZMB), Hans Baagoe (ZMUC), and Geraldine Veron and Jacques Cuisin (MNHN) for access to specimens and other kindnesses during visits to museums. We thank Wirn Bergirians, Norberto Giannini, and Don Drake for insightful reviews of our manuscript; Rusty Russell, Marissa Grunes, David Steadman, Tim Flannery, Sandra Banack, Paul Cox, Adam Miles, Alfred Gardner, Storrs Olson, Dan Polhemus, Philippe Bouchet, F. Russell Cole, and Allen Allison for valuable discussion; and Suzanne Cole for assistance at the Library of Congress. We especially thank Ned Gilmore for facilitating our work in the collection and archives of ANSP, Linda Gordon and Helen Kafka for assistance at the Smithsonian Institution, and Allen and Heather Drew for their hospitality during our visit to Philadelphia. This research was completed during a postdoctoral fellowship to K.M.H. funded by the Smithsonian Institution, travel funding from the South Australian Museum, and graduate fellowships to K.M.H. from the Australian-American Fulbright Foundation, National Science Foundation, American Society of Mammalogists, and the University of Adelaide. NR 192 TC 14 Z9 14 U1 1 U2 20 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD JUN 25 PY 2009 IS 3646 BP 1 EP 37 PG 37 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 464CQ UT WOS:000267482900001 ER PT J AU Rozen, JG Ozbek, H Ascher, JS Rightmyer, MG AF Rozen, Jerome G., Jr. Ozbek, Hikmet Ascher, John S. Rightmyer, Molly G. TI Biology of the Bee Hoplitis (Hoplitis) monstrabilis Tkalcu and Descriptions of Its Egg and Larva (Megachilidae: Megachilinae: Osmiini) SO AMERICAN MUSEUM NOVITATES LA English DT Article ID HYMENOPTERA-MEGACHILIDAE AB Herein we describe the nesting biology of the solitary ground-nesting bee Hoplitis (Hoplitis) monstrabilis Tkalcu from eastern Turkey. Its shallow nests in the ground differ from the known nests of members of subgenus Hoplitis, most of which make mortar and pebble nests either on the exposed surfaces of rocks or within stems or other cavities. Cells are not lined with flower petals or other vegetative tissue, as expected for subgenus Hoplitis, but unlike other ground-nesting species of Hoplitis belonging to other subgenera such as Anthocopa. The egg of this bee is also described and illustrated, as is the fifth (last) larval instar. C1 [Rozen, Jerome G., Jr.; Ascher, John S.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. [Ozbek, Hikmet] Ataturk Univ, Fac Agr, Dept Plant Protect, TR-25240 Erzurum, Turkey. [Rightmyer, Molly G.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Rozen, JG (reprint author), Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. EM rozen@amnh.org; hozbek@atauni.edu.tr; ascher@amnh.org; rightmyerm@si.edu RI Ascher, John/D-1554-2014 NR 33 TC 3 Z9 3 U1 2 U2 2 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD JUN 25 PY 2009 IS 3645 BP 1 EP 12 PG 12 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 464CR UT WOS:000267483000001 ER PT J AU Fernandez-Marin, H Zimmerman, JK Nash, DR Boomsma, JJ Wcislo, WT AF Fernandez-Marin, Hermogenes Zimmerman, Jess K. Nash, David R. Boomsma, Jacobus J. Wcislo, William T. TI Reduced biological control and enhanced chemical pest management in the evolution of fungus farming in ants SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Attini; mutualism; Pseudonocardia; metapleural gland; public health; social complexity ID LEAF-CUTTING ANTS; METAPLEURAL GLAND SECRETION; GROWING ANTS; ACROMYRMEX-OCTOSPINOSUS; MUTUALISTIC BACTERIUM; SUBSTRATE PREPARATION; GENETIC DIVERSITY; COLONY SIZE; FORMICIDAE; PARASITES AB To combat disease, most fungus-growing ants (Attini) use antibiotics from mutualistic bacteria (Pseudonocardia) that are cultured on the ants' exoskeletons and chemical cocktails from exocrine glands, especially the metapleural glands (MG). Previous work has hypothesized that (i) Pseudonocardia antibiotics are narrow-spectrum and control a fungus (Escovopsis) that parasitizes the ants' fungal symbiont, and (ii) MG secretions have broad-spectrum activity and protect ants and brood. We assessed the relative importance of these lines of defence, and their activity spectra, by scoring abundance of visible Pseudonocardia for nine species from five genera and measuring rates of MG grooming after challenging ants with disease agents of differing virulence. Atta and Sericomyrmex have lost or greatly reduced the abundance of visible bacteria. When challenged with diverse disease agents, including Escovopsis, they significantly increased MG grooming rates and expanded the range of targets. By contrast, species of Acromyrmex and Trachymyrmex maintain abundant Pseudonocardia. When challenged, these species had lower MG grooming rates, targeted primarily to brood. More elaborate MG defences and reduced reliance on mutualistic Pseudonocardia are correlated with larger colony size among attine genera, raising questions about the efficacy of managing disease in large societies with chemical cocktails versus bacterial antimicrobial metabolites. C1 [Fernandez-Marin, Hermogenes; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Fernandez-Marin, Hermogenes; Wcislo, William T.] STRI, MRC 0580 12, Unit 9100, DPO, AA 34002 USA. [Fernandez-Marin, Hermogenes] Univ Puerto Rico, Dept Biol, San Juan, PR 00936 USA. [Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. [Fernandez-Marin, Hermogenes; Nash, David R.; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. RP Fernandez-Marin, H (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM hermogenes_f@hotmail.com; wcislow@si.edu RI Nash, David/B-2916-2009; Nash, David/H-4433-2012; Boomsma, Jacobus/M-2785-2014 OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794; Boomsma, Jacobus/0000-0002-3598-1609 FU Secretaria Nacional de Ciencia, Tecnologia e Innovacion (Republica de Panama); Smithsonian Institution Predoctoral and Postdoctoral Fellowships FX We thank A. Aguilar, A. Portugal and E. Gomez for their assistance; P. Bayman, N. Biani, C. Currie, A. Herre, E. Leigh and S. Tierney for their comments on the manuscript; and the Autoridad Nacional del Ambiente for permits. H.F.-M. was supported by the Secretaria Nacional de Ciencia, Tecnologia e Innovacion (Republica de Panama) and Smithsonian Institution Predoctoral and Postdoctoral Fellowships; STRI provided supplemental support to H.F.-M., and general research support to W.T.W. J.J.B. and D. R.N. were supported by a grant from the Danish National Research Foundation, which provided supplemental support to H.F.-M. NR 53 TC 65 Z9 65 U1 3 U2 28 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD JUN 22 PY 2009 VL 276 IS 1665 BP 2263 EP 2269 DI 10.1098/rspb.2009.0184 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 443FX UT WOS:000265896700016 PM 19324734 ER PT J AU McCarthy, MC Thaddeus, P Wilke, JJ Schaefer, HF AF McCarthy, M. C. Thaddeus, P. Wilke, Jeremiah J. Schaefer, Henry F., III TI A laboratory and theoretical study of protonated carbon disulfide, HSCS+ SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE coupled cluster calculations; Fourier transform spectra; ground states; hydrogen compounds; infrared spectra; ionisation potential; isomerism; isotope effects; molecular moments; positive ions; potential energy surfaces; radiofrequency spectra; rotational states; vibrational states ID MOLECULAR VIBRATIONAL ANHARMONICITY; HIGHER-DERIVATIVE METHODS; ASYMMETRIC-TOP MOLECULES; ROTATIONAL SPECTRA; INTERSTELLAR HOCO+; GALACTIC-CENTER; WAVE SPECTRUM; DIOXIDE; AFFINITIES; CHEMISTRY AB The rotational spectrum of protonated carbon disulfide, HSCS+, has been detected in the centimeter-wave band in a molecular beam by Fourier transform microwave spectroscopy. Rotational and centrifugal distortion constants have been determined from ten transitions in the K-a=0 ladder of the normal isotopic species, (HSCS+)-C-13, and DSCS+. The present assignment agrees well with high-level coupled cluster calculations of the HSCS+ structure, which, like earlier work, predict this isomer to be the ground state on the HCS2+ potential energy surface; HCSS+, an isomer with C-2 upsilon symmetry, is predicted to lie more than 20 kcal/mol higher in energy. Other properties of HSCS+ including its dipole moment, anharmonic vibrational frequencies, and infrared intensities have also been computed at the coupled cluster level of theory with large basis sets. Because carbon disulfide possesses a fairly large proton affinity, and because this nonpolar molecule may plausibly exist in astronomical sources, HSCS+ is a good candidate for detection with radio telescopes in the submillimeter band where the stronger b-type transitions of this protonated cation are predicted to lie. C1 [McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Wilke, Jeremiah J.; Schaefer, Henry F., III] Univ Georgia, Ctr Computat Quantum Chem, Athens, GA 30602 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu OI McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204, CHE-0749868]; NASA [NNX08AE05G] FX We thank S. Thorwirth and C. A. Gottlieb for helpful discussions. The work in Cambridge was supported by the NSF under Grant No. CHE-0701204 and the NASA under Grant No. NNX08AE05G; that in Georgia was supported by the NSF under Grant No. CHE-0749868. NR 61 TC 8 Z9 8 U1 0 U2 4 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 JUN 21 PY 2009 VL 130 IS 23 AR 234304 DI 10.1063/1.3137057 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 460DE UT WOS:000267166200025 PM 19548724 ER PT J AU Yoo, J Weinberg, DH Tinker, JL Zheng, Z Warren, MS AF Yoo, Jaiyul Weinberg, David H. Tinker, Jeremy L. Zheng, Zheng Warren, Michael S. TI EXTENDING RECOVERY OF THE PRIMORDIAL MATTER POWER SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; dark matter; galaxies: halos; large-scale structure of universe ID HALO OCCUPATION DISTRIBUTION; DIGITAL SKY SURVEY; REDSHIFT-SPACE DISTORTIONS; LUMINOUS RED GALAXIES; LARGE-SCALE STRUCTURE; COLD DARK-MATTER; COSMOLOGICAL PARAMETERS; FOURIER-ANALYSIS; ANALYTIC MODEL; MASS FUNCTION AB The shape of the primordial matter power spectrum encodes critical information on cosmological parameters. At large scales, in the linear regime, the observable galaxy power spectrum P(obs)(k) is expected to follow the shape of the linear matter power spectrum P(lin)(k), but on smaller scales the effects of nonlinearity and galaxy bias make the ratio P(obs)(k)/P(lin)(k) scale dependent. We develop a method that can extend the dynamic range of the primordial matter power spectrum recovery, taking full advantage of precision measurements on quasi-linear scales, by incorporating additional constraints on the galaxy halo occupation distribution (HOD) from the projected galaxy correlation function w(p) (r(p)). We devise an analytic model to calculate observable galaxy power spectrum P(obs)(k) in real space and redshift space, given P(lin)(k) and HOD parameters, and we demonstrate its accuracy at the few percent level with tests against a suite of populated N-body simulations. Once HOD parameters are determined by fitting w(p) (r(p)) measurements for a given cosmological model, galaxy bias is completely specified, and our analytic model predicts both the shape and normalization of P(obs)(k). Applying our method to the main galaxy redshift samples from the Sloan Digital Sky Survey (SDSS), we find that the real-space galaxy power spectrum follows the shape of the nonlinear matter power spectrum at the 1%-2% level up to k = 0.2 h Mpc(-1) and that current observational uncertainties in HOD parameters leave only few percent uncertainties in our scale-dependent bias predictions up to k = 0.5 h Mpc(-1). These uncertainties can be marginalized over in deriving cosmological parameter constraints, and they can be reduced by higher precision w(p) (r(p)) measurements. When we apply our method to the SDSS luminous red galaxy (LRG) samples, we find that the linear bias approximation is accurate to 5% at k <= 0.08 h Mpc(-1), but the strong scale dependence of LRG bias prevents the use of linear theory at k >= 0.08 h Mpc(-1). Our HOD model prediction is in good agreement with the recent SDSS LRG power spectrum measurements at all measured scales (k <= 0.2 h Mpc(-1)), naturally explaining the observed shape of P(obs)(k) in the quasi-linear regime. The phenomenological "Q-model" prescription is a poor description of galaxy bias for the LRG samples, and it can lead to biased cosmological parameter estimates when measurements at k >= 0.1 h Mpc(-1) are included in the analysis. We quantify the potential bias and constraints on cosmological parameters that arise from applying linear theory and Q-model fitting, and we demonstrate the utility of HOD modeling of high-precision measurements of P(obs)(k) on quasi-linear scales, which will be obtainable from the final SDSS data set. C1 [Yoo, Jaiyul] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yoo, Jaiyul; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Tinker, Jeremy L.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Zheng, Zheng] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Warren, Michael S.] Los Alamos Natl Lab, Div Theoret Astrophys, Los Alamos, NM 87543 USA. RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyoo@cfa.harvard.edu; dhw@astronomy.ohio-state.edu; tinker@cfcp.uchicago.edu; zhengz@ias.edu; msw@lanl.gov OI Warren, Michael/0000-0002-1218-7904 FU Ohio State University; NSF [AST-0707985, AST-0239759]; Chandra award [GO5-6120B]; Institute for Advanced Study through a John Bahcall Fellowship FX We are grateful to Max Tegmark for kindly providing his no-defog measurements used in our Figure 13. J.Y. has been supported by the Harvard College Observatory through a Donald H. Menzel Fellowship and by the Graduate School of The Ohio State University through a Presidential Fellowship. D. W. acknowledges support from NSF Grant AST-0707985. J.T. was supported by the Chandra award GO5-6120B and National Science Foundation ( NSF) under grant AST-0239759. Z.Z. gratefully acknowledges support from the Institute for Advanced Study through a John Bahcall Fellowship. NR 84 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 967 EP 985 DI 10.1088/0004-637X/698/2/967 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400001 ER PT J AU Bliss, AF Worrall, DM Birkinshaw, M Murray, SS Tananbaum, H AF Bliss, A. F. Worrall, D. M. Birkinshaw, M. Murray, S. S. Tananbaum, H. TI UNMASKING THE ACTIVE GALACTIC NUCLEUS IN PKS J2310-437 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; galaxies: individual (PKS J2310-437); galaxies: jets; X-rays: individual (PKS J2310-437) ID UNUSUAL GALAXY J2310-43; RADIO GALAXIES; JET AB PKS J2310-437 is an active galactic nucleus (AGN) with bright X-ray emission relative to its weak radio emission and optical continuum. It is believed that its jet lies far enough from the line of sight that it is not highly relativistically beamed. It thus provides an extreme test of AGN models. We present new observations aimed at refining the measurement of the source's properties. In optical photometry with the New Technology Telescope we measure a central excess with relatively steep spectrum lying above the bright elliptical galaxy emission, and we associate the excess wholly or in part with the AGN. A new full-track radio observation with the Australian Telescope Compact Array finds that the core 8.64 GHz emission has varied by about 20% over 38 months, and improves the mapping of the weak jet. With Chandra we measure a well-constrained power-law spectral index for the X-ray core, uncontaminated by extended emission from the cluster environment, with a negligible level of intrinsic absorption. Weak X-ray emission from the resolved radio jet is also measured. Our analysis suggests that the optical continuum in this radio galaxy has varied by at least a factor of 4 over a timescale of about two years, something that should be testable with further observations. We conclude that the most likely explanation for the bright central X-ray emission is synchrotron radiation from high-energy electrons. C1 [Bliss, A. F.; Worrall, D. M.; Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Murray, S. S.; Tananbaum, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bliss, AF (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. FU UK Science and Technology Facilities Council (STFC); NASA [NAS8-03060] FX A. F. B. acknowledges support from the UK Science and Technology Facilities Council (STFC) studentship. We also acknowledge support from NASA (NAS8-03060). NR 14 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1061 EP 1067 DI 10.1088/0004-637X/698/2/1061 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400009 ER PT J AU Goddi, C Greenhill, LJ Chandler, CJ Humphreys, EML Matthews, LD Gray, MD AF Goddi, C. Greenhill, L. J. Chandler, C. J. Humphreys, E. M. L. Matthews, L. D. Gray, M. D. TI MASER EMISSION FROM SiO ISOTOPOLOGUES TRACES THE INNERMOST 100 AU AROUND RADIO SOURCE I IN ORION BECKLIN-NEUGEBAUER/KLEINMANN-LOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Orion BN/KL); line: profiles; masers; stars: formation ID SILICON MONOXIDE; RELATIVE ABUNDANCES; INTERSTELLAR-MEDIUM; PROPER MOTIONS; 1ST DETECTION; GROUND-STATE; YOUNG STARS; KL; (SIO)-SI-29; REGION AB We have used the Very Large Array at 7 mm wavelength to image five rotational transitions (J = 1-0) from three SiO isotopologues toward Orion Becklin-Neugebauer/Kleinmann-Low (BN/KL): (28)SiO v = 0, 1, 2; and (29)SiO and (30)SiO v = 0. For the first time, we have mapped the (29)SiO and (30)SiO J = 1-0 emission, established the maser nature of the emission, and confirmed association with the deeply embedded high-mass young stellar object commonly denoted radio Source I. The (28)SiO v = 0 maser emission shows a bipolar structure that extends over similar to 700 AU along a northeast-southwest axis, and we propose that it traces a bipolar outflow driven by Source I. The high-brightness isotopic SiO maser emission imaged with a less than or similar to 0 ''.2 resolution has a more compact distribution, generally similar to that of the (28)SiO v = 1, 2 emission, and it probably traces bulk gas flows in a region of diameter less than or similar to 100 AU centered on Source I. On small scales of less than or similar to 10 AU, however, compact (29)SiO/(30)SiO v = 0 and (28)SiO v = 1, 2 emission features may be offset from one another in position and line-of-sight velocity. From a radiative transfer analysis based on a large velocity gradient pumping model, we derive similar temperatures and densities for the optimum excitation of both (29)SiO/(30)SiO v = 0 and (28)SiO v = 1, 2 masers, significantly higher than required for (28)SiO v = 0 maser excitation. In order to account for the small-scale differences among the isotopologues (v = 0) and the main species (v = 1, 2), follow-up radiative transfer modeling that incorporates nonlocal line overlap among transitions of all SiO isotopic species may be required. C1 [Goddi, C.; Greenhill, L. J.; Humphreys, E. M. L.; Matthews, L. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, C. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Gray, M. D.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Goddi, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Science Foundation [NSF AST 0507478] FX The data presented here were obtained under the VLA programs AG575 and AG776. This material is based upon work supported by the National Science Foundation under grant No. NSF AST 0507478. NR 42 TC 27 Z9 27 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1165 EP 1173 DI 10.1088/0004-637X/698/2/1165 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400017 ER PT J AU Maret, S Bergin, EA Neufeld, DA Green, JD Watson, DM Harwit, MO Kristensen, LE Melnick, GJ Sonnentrucker, P Tolls, V Werner, MW Willacy, K Yuan, Y AF Maret, Sebastien Bergin, Edwin A. Neufeld, David A. Green, Joel D. Watson, Dan M. Harwit, Martin O. Kristensen, Lars E. Melnick, Gary J. Sonnentrucker, Paule Tolls, Volker Werner, Michael W. Willacy, Karen Yuan, Yuan TI SPITZER MAPPING OF MOLECULAR HYDROGEN PURE ROTATIONAL LINES IN NGC 1333: A DETAILED STUDY OF FEEDBACK IN STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual (NGC 1333); ISM: molecules; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; HH 7-11; SPACE-TELESCOPE; INFRARED SPECTROGRAPH; NGC-1333 IRAS-4; WATER EMISSION; SHOCK-WAVES; BOW SHOCK; OUTFLOW AB We present mid-infrared spectral maps of the NGC 1333 star-forming region, obtained with the infrared spectrometer on board the Spitzer Space Telescope. Eight pure H(2) rotational lines, from S(0) to S(7), are detected and mapped. The H(2) emission appears to be associated with the warm gas shocked by the multiple outflows present in the region. A comparison between the observed intensities and the predictions of detailed shock models indicates that the emission arises in both slow (12-24 km s(-1)) and fast (36-53 km s(-1)) C-type shocks with an initial ortho-to-para ratio (opr) less than or similar to 1. The present H(2) opr exhibits a large degree of spatial variations. In the postshocked gas, it is usually about 2, i.e., close to the equilibrium value (similar to 3). However, around at least two outflows, we observe a region with a much lower (similar to 0.5) opr. This region probably corresponds to gas which has been heated up recently by the passage of a shock front, but whose ortho-to-para has not reached equilibrium yet. This, together with the low initial opr needed to reproduce the observed emission, provide strong evidence that H(2) is mostly in para form in cold molecular clouds. The H(2) lines are found to contribute to 25%-50% of the total outflow luminosity, and thus can be used to ascertain the importance of star formation feedback on the natal cloud. From these lines, we determine the outflow mass loss rate and, indirectly, the stellar infall rate, the outflow momentum and the kinetic energy injected into the cloud over the embedded phase. The latter is found to exceed the binding energy of individual cores, suggesting that outflows could be the main mechanism for core disruption. C1 [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, David A.; Sonnentrucker, Paule; Yuan, Yuan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Green, Joel D.; Watson, Dan M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Kristensen, Lars E.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Melnick, Gary J.; Tolls, Volker] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Werner, Michael W.; Willacy, Karen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maret, S (reprint author), Univ Grenoble 1, CNRS, Observ Grenoble, Lab Astrophys Grenoble,UMR 571, BP 53, F-38041 Grenoble, France. RI Kristensen, Lars/F-4774-2011; OI Kristensen, Lars/0000-0003-1159-3721; Maret, Sebastien/0000-0003-1104-4554 FU NASA [20378] FX 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 for program # 20378. Facilities: Spitzer (IRS) NR 70 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1244 EP 1260 DI 10.1088/0004-637X/698/2/1244 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400023 ER PT J AU McClintock, JE Remillard, RA Rupen, MP Torres, MAP Steeghs, D Levine, AM Orosz, JA AF McClintock, Jeffrey E. Remillard, Ronald A. Rupen, Michael P. Torres, M. A. P. Steeghs, D. Levine, Alan M. Orosz, Jerome A. TI THE 2003 OUTBURST OF THE X-RAY TRANSIENT H1743-322: COMPARISONS WITH THE BLACK HOLE MICROQUASAR XTE J1550-564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; black hole physics; stars: individual (H1743-322, XTE J1550-564); X-rays: stars ID QUASI-PERIODIC OSCILLATIONS; RXTE SPECTRAL OBSERVATIONS; GRO J1655-40; HIGH-FREQUENCY; OBSERVATIONAL EVIDENCE; INTEGRAL OBSERVATIONS; TIMING-EXPLORER; CROSS-SECTIONS; HIGH-STATE; BINARY AB The bright X-ray transient H1743-322 was observed daily by the Rossi X-ray Timing Explorer during most of its eight-month outburst in 2003. We present a detailed spectral analysis and a supporting timing analysis of all of these data, and we discuss the behavior and evolution of the source in terms of the three principal X-ray states defined by Remillard and McClintock. These X-ray results are complemented by Very Large Array data obtained at six frequencies that provide quite complete coverage of the entire outburst cycle at 4.860 GHz and 8.460 GHz. We also present photometric data and finding charts for the optical counterpart in both outburst and quiescence. We closely compare H1743-322 to the well-studied black hole X-ray transient XTE J1550-564 and find the behaviors of these systems to be very similar. As reported elsewhere, both H1743-322 and XTE J1550-564 are relativistic jet sources and exhibit a pair of high-frequency quasi-periodic oscillations with a 3: 2 frequency ratio. The many striking similarities between these two sources argue strongly that H1743-322 is a black hole binary, although presently no dynamical data exist to support this conclusion. C1 [McClintock, Jeffrey E.; Torres, M. A. P.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.; Levine, Alan M.] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Rupen, Michael P.] Natl Radio Astron Observ, New Mexico Array Operat Ctr VLA VLBA, Socorro, NM 87801 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP McClintock, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 NR 84 TC 75 Z9 75 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1398 EP 1421 DI 10.1088/0004-637X/698/2/1398 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400036 ER PT J AU Zapata, LA Ho, PTP Schilke, P Rodriguez, LF Menten, K Palau, A Garrod, RT AF Zapata, Luis A. Ho, Paul T. P. Schilke, Peter Rodriguez, Luis F. Menten, Karl Palau, Aina Garrod, Robin T. TI A RING/DISK/OUTFLOW SYSTEM ASSOCIATED WITH W51 NORTH: A VERY MASSIVE STAR IN THE MAKING SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instrumentation: interferometers; ISM: jets and outflows; molecular data; stars: formation; stars: individual (W51 North, W51N) ID H2O MASER SOURCES; FORMING REGIONS; ROTATING-DISK; DYNAMICAL COLLAPSE; PROPER MOTIONS; ACCRETION DISK; SIO EMISSION; ORION-KL; PROTOSTAR; OUTFLOW AB Sensitive and high angular resolution (similar to 0 ''.4) SO(2)[22(2,20) -> 22(1,21)] and SiO[5 -> 4] line and 1.3 and 7 mm continuum observations made with the Submillimeter Array (SMA) and the Very Large Array (VLA) toward the young massive cluster W51 IRS2 are presented. We report the presence of a large (of about 3000 AU) and massive (40 M(circle dot)) dusty circumstellar disk and a hot gas molecular ring around a high-mass protostar or a compact small stellar system associated with W51 North. The simultaneous observations of the silicon monoxide molecule, an outflow gas tracer, further revealed a massive (200 M(circle dot)) and collimated (similar to 14 degrees) outflow nearly perpendicular to the dusty and molecular structures suggesting thus the presence of a single very massive protostar with a bolometric luminosity on the order of 10(5) L(circle dot). A molecular hybrid local thermodynamic equilibrium model of a Keplerian and infalling disk with an inner cavity and a central stellar mass of more than 60 M(circle dot) agrees well with the SO(2)[22(2,20) -> 22(1,21)] line observations. Finally, these results suggest that mechanisms such as mergers of low-and intermediate-mass stars, might not be necessary for forming very massive stars. C1 [Zapata, Luis A.; Schilke, Peter; Menten, Karl] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Palau, Aina] LAEFF, LAEX, Ctr Astrobiol, CAB INTA CSIC, E-28691 Madrid, Spain. [Garrod, Robin T.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Zapata, LA (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. FU Smithsonian Institution; Academia Sinica; National Science Foundation FX We thank all the SMA and NRAO staff members for making these observations possible. The Submillimeter Array (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. NRAO is operated by Associated University, Inc., under contract with the National Science Foundation. NR 43 TC 37 Z9 37 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1422 EP 1428 DI 10.1088/0004-637X/698/2/1422 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400037 ER PT J AU Hopkins, PF Hernquist, L AF Hopkins, Philip F. Hernquist, Lars TI QUASARS ARE NOT LIGHT BULBS: TESTING MODELS OF QUASAR LIFETIMES WITH THE OBSERVED EDDINGTON RATIO DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: theory; galaxies: active; galaxies: evolution; quasars: general ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; LINE-OF-SIGHT; DIGITAL SKY SURVEY; PHOTOMETRICALLY CLASSIFIED QUASARS; ADVECTION-DOMINATED ACCRETION; QSO LUMINOSITY FUNCTION; SAGITTARIUS-A-ASTERISK; HUBBLE-SPACE-TELESCOPE; COSMIC STAR-FORMATION AB We use the observed distribution of Eddington ratios as a function of supermassive black hole (BH) mass to constrain models of quasar/active galactic nucleus (AGN) lifetimes and light curves. Given the observed (well constrained) AGN luminosity function, a particular model for AGN light curves L(t) or, equivalently, the distribution of AGN lifetimes (time above a given luminosity t (> L)) translates directly and uniquely (without further assumptions) to a predicted distribution of Eddington ratios at each BH mass. Models for self-regulated BH growth, in which feedback produces a self-regulating "decay" or "blowout" phase after the AGN reaches some peak luminosity/BH mass and begins to expel gas and shut down accretion, make specific predictions for the light curves/lifetimes, distinct from, e. g., the expected distribution if AGN simply shut down by gas starvation (without feedback) and very different from the prediction of simple phenomenological "light bulb" scenarios. We show that the present observations of the Eddington ratio distribution, spanning nearly 5 orders of magnitude in Eddington ratio, 3 orders of magnitude in BH mass, and redshifts z = 0-1, agree well with the predictions of self-regulated models, and rule out phenomenological "light bulb" or pure exponential models, as well as gas starvation models, at high significance (similar to 5 sigma). We also compare with observations of the distribution of Eddington ratios at a given AGN luminosity, and find similar good agreement (but show that these observations are much less constraining). We fit the functional form of the quasar lifetime distribution and provide these fits for use, and show how the Eddington ratio distributions place precise, tight limits on the AGN lifetimes at various luminosities, in agreement with model predictions. We compare with independent estimates of episodic lifetimes and use this to constrain the shape of the typical AGN light curve, and provide simple analytic fits to these for use in other analyses. Given these constraints, the average local BH must have gained its mass in no more than a couple of bright, near peak-luminosity episodes, in agreement with models of accretion triggering in interactions and mergers. C1 [Hopkins, Philip F.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Hopkins, PF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690]; NASA ATP [NAG5-12140, NAG5-13292, NAG5-13381]; Miller Institute for Basic Research in Science, University of California Berkeley FX We thank Josh Younger, T. J. Cox, and Guinevere Kauffmann for helpful discussions. This work was supported in part by NSF grants ACI 96-19019, AST 00-71019, AST 02-06299, and AST 03-07690, and NASA ATP grants NAG5-12140, NAG5-13292, and NAG5-13381. Support for P. F. H. was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. NR 161 TC 70 Z9 71 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1550 EP 1569 DI 10.1088/0004-637X/698/2/1550 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400046 ER PT J AU Shinnaga, H Young, KH Tilanus, RPJ Chamberlin, R Gurwell, MA Wilner, D Hughes, AM Yoshida, H Peng, RS Force, B Friberg, P Bottinelli, S Van Dishoeck, EF Phillips, TG AF Shinnaga, Hiroko Young, Ken H. Tilanus, Remo P. J. Chamberlin, Richard Gurwell, Mark A. Wilner, David Hughes, A. Meredith Yoshida, Hiroshige Peng, Ruisheng Force, Brian Friberg, Per Bottinelli, Sandrine Van Dishoeck, Ewine F. Phillips, Thomas G. TI IRC+10216'S INNERMOST ENVELOPE-THE eSMA'S VIEW SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; masers; stars: AGB and post-AGB; stars: individual (IRC+10216); stars: mass loss; stars: winds, outflows ID CIRCUMSTELLAR DUST SHELLS; CARBON STAR IRC+10216; VY CANIS MAJORIS; INTERFEROMETRIC OBSERVATIONS; PHYSICAL-PROPERTIES; CONTINUUM EMISSION; MOLECULAR-EMISSION; MASER EMISSION; SIO MASERS; IRC +10216 AB We used the Extended Submillimeter Array (eSMA) in its most extended configuration to investigate the innermost (within a radius of similar to 290 R(*) from the star) circumstellar envelope (CSE) of IRC+10216 where acceleration of gas and dust due to strong stellar radiation is taking place. We imaged the CSE using HCN and other molecular lines with a beam size of 0 ''.22 x 0 ''.46, deeply into the very inner edge (similar to 15 R(*)) of the envelope where the expansion velocity is only similar to 3 km s(-1). The excitation mechanisms of hot HCN and KCl lines are discussed. HCN maser components are spatially resolved for the first time on an astronomical object. We identified two discrete regions in the envelope: a region with a radius of similar to 15 R(*), where molecular species have just formed and the gas has begun to be accelerated (Region I) and a shell region (Region II) with a radius of 23 R(*) and a thickness of 15 R(*), whose expansion velocity has reached up to 13 km s(-1), nearly the terminal velocity of 15 km s(-1). The Si(34)S line detected in Region I shows a large expansion velocity of 16 km s(-1) due to strong wing components, indicating that the emission may arise from a shock region in the innermost envelope. In Region II, the position angle of the most copious mass-loss direction was found to be similar to 120 degrees +/- 10 degrees, which may correspond to the equatorial direction of the star. Region II contains a torus-like feature. These two regions may have emerged due to significant differences in the size distributions of the dust particles in the two regions. C1 [Shinnaga, Hiroko; Chamberlin, Richard; Yoshida, Hiroshige; Peng, Ruisheng; Force, Brian; Phillips, Thomas G.] CALTECH, Submillimeter Observ CSO, Hilo, HI 96720 USA. [Young, Ken H.; Gurwell, Mark A.; Wilner, David; Hughes, A. Meredith] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tilanus, Remo P. J.; Friberg, Per] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Bottinelli, Sandrine; Van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Shinnaga, H (reprint author), CALTECH, Submillimeter Observ CSO, 111 Nowelo St, Hilo, HI 96720 USA. EM shinnaga@submm.caltech.edu FU Netherlands NWO-M; Netherlands Organization for Scientific Research [614.061.416]; United Kingdom's Science and Technology Facilities Council (STFC); National Research Council Canada (NRC); Smithsonian Institution; Academia Sinica; National Science Foundation Graduate Research Fellowship FX The Caltech Submillimeter Observatory is supported by grant AST-0540882 from the National Science Foundation. The eSMA developments at the JCMT are financially supported by a Netherlands NWO-M grant, the Netherlands Organization for Scientific Research, and NWO. The development of the eSMA has been facilitated by grant 614.061.416 from the Netherlands Organisation for Scientific Research, NWO. The JCMT is supported by the United Kingdom's Science and Technology Facilities Council (STFC), the National Research Council Canada (NRC), and the Netherlands Organization for Scientific Research (NWO). 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. We sincerely appreciate strong support from Ray Blundell, Gary Davis, and Tom Phillips, the directors of the SMA, JCMT, and CSO, respectively. H. S. is grateful to Ray S. Furuya, Charlie Qi, Nick Scoville, and Frank Lovas for various discussion. A. M. H. is supported by a National Science Foundation Graduate Research Fellowship. NR 42 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 1924 EP 1933 DI 10.1088/0004-637X/698/2/1924 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400076 ER PT J AU Roederer, IU Kratz, KL Frebel, A Christlieb, N Pfeiffer, B Cowan, JJ Sneden, C AF Roederer, Ian U. Kratz, Karl-Ludwig Frebel, Anna Christlieb, Norbert Pfeiffer, Bernd Cowan, John J. Sneden, Christopher TI THE END OF NUCLEOSYNTHESIS: PRODUCTION OF LEAD AND THORIUM IN THE EARLY GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Review DE Galaxy: halo; nuclear reactions, nucleosynthesis, abundances; stars: abundances; stars: Population II ID METAL-POOR STARS; ASYMPTOTIC GIANT BRANCH; NEUTRON-CAPTURE ELEMENTS; LABORATORY TRANSITION-PROBABILITIES; ASTROPHYSICAL R-PROCESS; GLOBULAR-CLUSTER M15; NEAR-ULTRAVIOLET OBSERVATIONS; IMPROVED OSCILLATOR-STRENGTHS; S-PROCESS; LOW-MASS AB We examine the Pb and Th abundances in 27 metal-poor stars (-3.1 < [Fe/H] < -1.4) whose very heavy metal (Z > 56) enrichment was produced only by the rapid (r-) nucleosynthesis process. New abundances are derived from Hubble Space Telescope/Space Telescope Imaging Spectrograph, Keck/High Resolution Echelle Spectrograph, and Very Large Telescope/UV-Visual Echelle Spectrograph spectra and combined with other measurements from the literature to form a more complete picture of nucleosynthesis of the heaviest elements produced in the r-process. In all cases, the abundance ratios among the rare earth elements and the third r-process peak elements considered (La, Eu, Er, Hf, and Ir) are constant and equivalent to the scaled solar system r-process abundance distribution. We compare the stellar observations with r-process calculations within the classical "waiting-point" approximation. In these computations a superposition of 15 weighted neutron-density components in the range 23 <= log n(n) <= 30 is fit to the r-process abundance peaks to successfully reproduce both the stable solar system isotopic distribution and the stable heavy element abundance pattern between Ba and U in low-metallicity stars. Under these astrophysical conditions, which are typical of the "main" r-process, we find very good agreement between the stellar Pb r-process abundances and those predicted by our model. For stars with anomalously high Th/Eu ratios (the so-called actinide boost), our observations demonstrate that any nucleosynthetic deviations from the main r-process affect-at most-only the elements beyond the third r-process peak, namely Pb, Th, and U. Our theoretical calculations also indicate that possible r-process abundance "losses" by nuclear fission are negligible for isotopes along the r-process path between Pb and the long-lived radioactive isotopes of Th and U. C1 [Roederer, Ian U.; Sneden, Christopher] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kratz, Karl-Ludwig; Pfeiffer, Bernd] Max Planck Inst Chem, Otto Hahn Inst, D-55128 Mainz, Germany. [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Christlieb, Norbert] Heidelberg Univ, Zentrum Astron, D-69117 Heidelberg, Germany. [Cowan, John J.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. RP Roederer, IU (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM iur@astro.as.utexas.edu; klk@uni-mainz.de; afrebel@cfa.harvard.edu; N.Christlieb@lsw.uni-heidelberg.de; bpfeiffe@uni-mainz.de; cowan@nhn.ou.edu; chris@astro.as.utexas.edu FU Deutsche Forschungsgemeinschaft [KR 806/13-1]; Helmholtz Gemeinschaft [VH-VI-061]; U S National Science Foundation [AST 07-07447, AST 06-07708] FX We thank Satoshi Honda and David Lai for sending unpublished upper limit measurements and David Yong for providing additional abundance results. We appreciate the helpful suggestions of the referee. I. U. R. also thanks Jim Truran for an invigorating discussion on this topic. This research has made use of the NASA Astrophysics Data System (ADS), NIST Atomic Spectra Database, and the SIMBAD database, operated at CDS, Strasbourg, France. A. F. acknowledges support through theW. J. McDonald Fellowship of the McDonald Observatory. Funding for this project has also been generously provided by the Deutsche Forschungsgemeinschaft (contract KR 806/13-1), the Helmholtz Gemeinschaft (grant VH-VI-061), and the U S National Science Foundation (grants AST 07-07447 to J. J. C. and AST 06-07708 to C. S.). NR 112 TC 42 Z9 42 U1 1 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 JUN 20 PY 2009 VL 698 IS 2 BP 1963 EP 1980 DI 10.1088/0004-637X/698/2/1963 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400080 ER PT J AU Kraft, RP Forman, WR Hardcastle, MJ Birkinshaw, M Croston, JH Jones, C Nulsen, PEJ Worrall, DM Murray, SS AF Kraft, R. P. Forman, W. R. Hardcastle, M. J. Birkinshaw, M. Croston, J. H. Jones, C. Nulsen, P. E. J. Worrall, D. M. Murray, S. S. TI THE JET HEATED X-RAY FILAMENT IN THE CENTAURUS A NORTHERN MIDDLE RADIO LOBE SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; galaxies: individual (Centaurus A, NGC 5128); galaxies: jets; X-rays: galaxies ID HOT INTERSTELLAR-MEDIUM; HUBBLE-SPACE-TELESCOPE; INDUCED STAR-FORMATION; NGC 5128; CLOUD INTERACTIONS; OPTICAL FILAMENTS; GALAXY NGC-2110; IONIZED-GAS; A EVIDENCE; CHANDRA AB We present results from a 40 ks XMM-Newton observation of the X-ray filament coincident with the southeast edge of the Centaurus A Northern Middle Radio Lobe (NML). We find that the X-ray filament consists of five spatially resolved X-ray knots embedded in a continuous diffuse bridge. The spectrum of each knot is well fitted by a thermal model with temperatures ranging from 0.3 to 0.7 keV and subsolar elemental abundances. In four of the five knots, nonthermal models are a poor fit to the spectra, conclusively ruling out synchrotron or IC/CMB mechanisms for their emission. The internal pressures of the knots exceed that of the ambient interstellar medium or the equipartition pressure of the NML by more than an order of magnitude, demonstrating that they must be short lived (similar to 3 x 10(6) yr). Based on energetic arguments, it is implausible that these knots have been ionized by the beamed flux from the active galactic nucleus of Cen A or that they have been shock heated by supersonic inflation of the NML. In our view, the most viable scenario for the origin of the X-ray knots is that they are the result of cold gas shock heated by a direct interaction with the jet. The most plausible model of the NML is that it is a bubble from a previous nuclear outburst that is being re-energized by the current outburst. The northeast inner lobe and the large-scale jet are lossless channels through which the jet material rapidly travels to the NML in this scenario. We also report the discovery of a large-scale (at least 35 kpc radius) gas halo around Cen A. C1 [Kraft, R. P.; Forman, W. R.; Jones, C.; Nulsen, P. E. J.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hardcastle, M. J.; Croston, J. H.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. RP Kraft, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-4, Cambridge, MA 02138 USA. RI Hardcastle, Martin/E-2264-2012; OI Hardcastle, Martin/0000-0003-4223-1117; Nulsen, Paul/0000-0003-0297-4493 FU NASA [NAS8-03060]; Chandra X-ray Center; Smithsonian Astrophysical Observatory; Royal Society FX This work was supported by NASA contract NAS8-03060, the Chandra X-ray Center, and the Smithsonian Astrophysical Observatory. M. J. H. thanks the Royal Society for a research fellowship. NR 65 TC 32 Z9 32 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2009 VL 698 IS 2 BP 2036 EP 2047 DI 10.1088/0004-637X/698/2/2036 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455RQ UT WOS:000266782400086 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Colin, P Cui, W Daniel, MK Dickherber, R Duke, C Dwarkadas, VV Ergin, T Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Valcarcel, L Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Colin, P. Cui, W. Daniel, M. K. Dickherber, R. Duke, C. Dwarkadas, V. V. Ergin, T. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Valcarcel, L. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI OBSERVATION OF EXTENDED VERY HIGH ENERGY EMISSION FROM THE SUPERNOVA REMNANT IC 443 WITH VERITAS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma rays: observations; ISM: individual (IC 443=VER J0616.9+2230, = MAGIC J0616+225) ID GAMMA-RAY EMISSION; XMM-NEWTON OBSERVATIONS; MOLECULAR CLOUDS; MAGIC TELESCOPE; COSMIC-RAYS; IC-443; NEBULA; PULSAR; DISCOVERY; RADIATION AB We present evidence that the very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with the supernova remnant IC 443 is extended. IC 443 contains one of the best studied sites of supernova remnant/molecular cloud interaction and the pulsar wind nebula CXOU J061705.3+222127, both of which are important targets for VHE observations. VERITAS observed IC 443 for 37.9 hr during 2007 and detected emission above 300 GeV with an excess of 247 events, resulting in a significance of 8.3 standard deviations (sigma) before trials and 7.5 sigma after trials in a point-source search. The emission is centered at 6(h)16(m)51(s)+22 degrees 30'11 '' (J2000)+/- 0 degrees.03(stat)+/- 0 degrees.08(sys), with an intrinsic extension of 0 degrees.16 +/- 0 degrees.03(stat)+/- 0 degrees.04(sys). The VHE spectrum is well fit by a power law (dN/dE = N(0) x(E/TeV)(-Gamma)) with a photon index of 2.99 +/- 0.38(stat)+/- 0.3(sys) and an integral flux above 300 GeV of (4.63 +/- 0.90(stat)+/- 0.93(sys)) x 10(-12) cm(-2) s(-1). These results are discussed in the context of existing models for gamma-ray production in IC 443. C1 [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Acciari, V. A.; Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Valcarcel, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Colin, P.; Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Fortin, P.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Humensky, TB (reprint author), Univ Chicago, Enrico Fermi Inst, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM humensky@uchicago.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010; OI Cesarini, Andrea/0000-0002-8611-8610; Cui, Wei/0000-0002-6324-5772; Daniel, Michael/0000-0002-8053-7910; Ward, John E/0000-0003-1973-0794; Otte, Adam Nepomuk/0000-0002-5955-6383; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU US Department of Energy; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC FX This research is supported by grants from the US Department of Energy, the US National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument. Some of the simulations used in this work have been performed on the Joint Fermilab-KICP Supercomputing Cluster. NR 42 TC 66 Z9 66 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L133 EP L137 DI 10.1088/0004-637X/698/2/L133 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600014 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Cesarini, A Chow, YC Ciupik, L Cogan, P Dickherber, R Duke, C Ergin, T Falcone, A Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Gibbs, K Gillanders, GH Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Millis, J Moriarty, P Mukherjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Petry, D Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, S Theiling, M Toner, JA Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Dickherber, R. Duke, C. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Gibbs, K. Gillanders, G. H. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Millis, J. Moriarty, P. Mukherjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Petry, D. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. Theiling, M. Toner, J. A. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. TI EVIDENCE FOR LONG-TERM GAMMA-RAY AND X-RAY VARIABILITY FROM THE UNIDENTIFIED TeV SOURCE HESS J0632+057 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE acceleration of particles; binaries: general; gamma rays: observations; stars: individual (HESS J0632+057, MWC 148) ID BINARY; DISCOVERY; EMISSION; TELESCOPE; CATALOG; STARS AB HESS J0632+057 is one of only two unidentified very-high-energy gamma-ray sources which appear to be point-like within experimental resolution. It is possibly associated with the massive Be star MWC 148 and has been suggested to resemble known TeV binary systems like LS I + 61 303 or LS 5039. HESS J0632+057 was observed by VERITAS for 31 hr in 2006, 2008, and 2009. During these observations, no significant signal in gamma rays with energies above 1 TeV was detected from the direction of HESS J0632+057. A flux upper limit corresponding to 1.1% of the flux of the Crab Nebula has been derived from the VERITAS data. The nondetection by VERITAS excludes with a probability of 99.993% that HESS J0632+057 is a steady gamma-ray emitter. Contemporaneous X-ray observations with the Swift X-Ray Telescope reveal a factor of 1.8 +/- 0.4 higher flux in the 1-10 keV range than earlier X-ray observations of HESS J0632+057. The variability in the gamma-ray and X-ray fluxes supports interpretation of the object as a gamma-ray emitting binary. C1 [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Acciari, V. A.; Benbow, W.; Gibbs, K.; Kildea, J.; Perkins, J. S.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finley, J. P.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Finnegan, G.; Hui, C. M.; Kieda, D.; LeBohec, S.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.; Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Maier, G (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM gernot.maier@mcgill.ca OI Millis, John/0000-0002-2069-9838; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU U. S. Department of Energy; U. S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC FX This research is supported by grants from the U. S. Department of Energy, the U. S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the U. K. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument. We acknowledge the efforts of the Swift team for providing the UVOT/XRT observations. NR 27 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L94 EP L97 DI 10.1088/0004-637X/698/2/L94 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600005 ER PT J AU Clements, DL Petitpas, G Farrah, D Hatziminaoglou, E Babbedge, T Rowan-Robinson, M Perez-Fournon, I Hernan-Caballero, A Castro-Rodriguez, N Lonsdale, C Surace, J Franceschini, A Wilkes, BJ Smith, H AF Clements, D. L. Petitpas, G. Farrah, D. Hatziminaoglou, E. Babbedge, T. Rowan-Robinson, M. Perez-Fournon, I. Hernan-Caballero, Antonio Castro-Rodriguez, Nieves Lonsdale, C. Surace, J. Franceschini, A. Wilkes, B. J. Smith, H. TI RESOLVED DUST EMISSION IN A QUASAR AT z=3.65 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: high-redshift; galaxies: interactions; galaxies: starburst; quasars: individual (SDSS 160705+533558); submillimeter ID ULTRALUMINOUS INFRARED GALAXIES; DEGREE EXTRAGALACTIC SURVEY; DEEP SUBMILLIMETER SURVEY; ABSORPTION-LINE QUASARS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT; STAR-FORMATION; MOLECULAR GAS; SURVEY SHADES; STARBURST AB We present submillimeter observations of the z = 3.653 quasar SDSS 160705+533558 together with data in the optical and infrared. The object is unusually bright in the far-IR and submillimeter with an IR luminosity of similar to 10(14) L-circle dot. We ascribe this luminosity to a combination of active galactic nucleus (AGN) and starburst emission, with the starburst forming stars at a rate of a few thousand solar masses per year. Submillimeter Array imaging observations with a resolution similar to 1 '' show that the submillimeter (850 mu m) emission is extended on scales of 10 35 kpc and is offset from the optical position by similar to 10 kpc. This morphology is dissimilar to that found in submillimeter galaxies, which are generally unresolved or marginally resolved on arcsecond scales, or submillimeter-luminous AGNs where the AGN lies at the peak of the submillimeter or molecular emission. The simplest explanation is that the object is in the early stages of a merger between a gas-rich galaxy, which hosts the starburst, and a gas-poor AGN-host galaxy, which is responsible for the quasar emission. It is also possible that jet-induced star formation might contribute to the unusual morphology. C1 [Clements, D. L.; Babbedge, T.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Petitpas, G.] Submillimetre Array, Hilo, HI USA. [Farrah, D.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Hatziminaoglou, E.] European So Observ, Munich, Germany. [Hatziminaoglou, E.; Perez-Fournon, I.; Hernan-Caballero, Antonio; Castro-Rodriguez, Nieves] IAC, Tenerife, Spain. [Lonsdale, C.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Surace, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Franceschini, A.] Univ Padua, Padua, Italy. [Wilkes, B. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, H.] Univ Calif San Diego, San Diego, CA USA. RP Clements, DL (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Phys, Prince Consort Rd, London SW7 2AZ, England. OI Wilkes, Belinda/0000-0003-1809-2364 FU PPARC/STFC; NASA; Smithsonian Institution; Academia Sinica FX This work was funded in part by PPARC/STFC and NASA. 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 James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UnitedKingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. Data were taken as part of JCMT project M05AU24. The authors thank Joe Silk, George Bendo, and Pierre Chanial for useful discussions and the anonymous referee whose comments have significantly improved the paper. NR 39 TC 5 Z9 5 U1 0 U2 2 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 JUN 20 PY 2009 VL 698 IS 2 BP L188 EP L191 DI 10.1088/0004-637X/698/2/L188 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600025 ER PT J AU Marconi, A Axon, DJ Maiolino, R Nagao, T Pietrini, P Risaliti, G Robinson, A Torricelli, G AF Marconi, Alessandro Axon, David J. Maiolino, Roberto Nagao, Tohru Pietrini, Paola Risaliti, Guido Robinson, Andrew Torricelli, Guidetta TI ON THE OBSERVED DISTRIBUTIONS OF BLACK HOLE MASSES AND EDDINGTON RATIOS FROM RADIATION PRESSURE CORRECTED VIRIAL INDICATORS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: fundamental parameters; galaxies: nuclei; galaxies: Seyfert; quasars: emission lines; radiation mechanisms: general ID ACTIVE GALACTIC NUCLEI; VELOCITY DISPERSION; HOST GALAXIES; QUASARS; LUMINOSITY; FLOWS; MODEL AB The application of the virial theorem to the broad-line region (BLR) of active galactic nuclei (AGNs) allows black hole (BH) mass estimates for large samples of objects at all redshifts. In a recent paper, we showed that ionizing radiation pressure onto BLR clouds affects virial BH mass estimates and we provided empirically calibrated corrections. More recently, a new test of the importance of radiation forces has been proposed: the M(BH)-sigma relation has been used to estimate M(BH) for a sample of type-2 AGNs and virial relations (with and without radiation pressure) for a sample of type-1 AGNs extracted from the same parent population. The observed L/L(Edd) distribution based on virial BH masses is in good agreement with that based on M(BH)-sigma only if radiation pressure effects are negligible, otherwise significant discrepancies are observed. In this Letter, we investigate the effects of intrinsic dispersions associated with the virial relations providing M(BH), and we show that they explain the discrepancies between the observed L/L(Edd) distributions of type-1 and type-2 AGNs. These discrepancies in the L/L(Edd) distributions are present regardless of the general importance of radiation forces, which must be negligible only for a small fraction of sources with large L/L(Edd). Average radiation pressure corrections should then be applied in virial M(BH) estimators until their dependence on observed source physical properties has been fully calibrated. Finally, the comparison between M(BH) and L/L(Edd) distributions derived from sigma-based and virial estimators can constrain the variance of BLR physical properties in AGNs. C1 [Marconi, Alessandro; Pietrini, Paola] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. [Axon, David J.; Robinson, Andrew] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Maiolino, Roberto] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Nagao, Tohru] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Risaliti, Guido; Torricelli, Guidetta] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marconi, A (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Largo E Fermi 2, I-50125 Florence, Italy. EM marconi@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X FU PRIN-MIUR [2006025203]; ASI-INAF [I/088/06/0] FX We are indebted to Hagai Netzer, Marianne Vestergaard, Brad Peterson, and Ric Davies for useful discussions. This work has been partly supported by grants PRIN-MIUR 2006025203 and ASI-INAF I/088/06/0. NR 22 TC 39 Z9 39 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L103 EP L107 DI 10.1088/0004-637X/698/2/L103 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600007 ER PT J AU Pannella, M Carilli, CL Daddi, E McCracken, HJ Owen, FN Renzini, A Strazzullo, V Civano, F Koekemoer, AM Schinnerer, E Scoville, N Smolcic, V Taniguchi, Y Aussel, H Kneib, JP Ilbert, O Mellier, Y Salvato, M Thompson, D Willott, CJ AF Pannella, M. Carilli, C. L. Daddi, E. McCracken, H. J. Owen, F. N. Renzini, A. Strazzullo, V. Civano, F. Koekemoer, A. M. Schinnerer, E. Scoville, N. Smolcic, V. Taniguchi, Y. Aussel, H. Kneib, J. P. Ilbert, O. Mellier, Y. Salvato, M. Thompson, D. Willott, C. J. TI STAR FORMATION AND DUST OBSCURATION AT z approximate to 2: GALAXIES AT THE DAWN OF DOWNSIZING SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM; galaxies: luminosity function, mass function; galaxies: statistics; surveys ID VLA-COSMOS SURVEY; ACTIVE GALACTIC NUCLEI; FORS-DEEP-FIELD; GOODS-S-FIELD; MASSIVE GALAXIES; STELLAR MASS; SUBMILLIMETER GALAXIES; FORMATION HISTORY; FORMING GALAXIES; FORMATION RATES AB We present first results of a study aimed to constrain the star formation rate (SFR) and dust content of galaxies at z approximate to 2. We use a sample of BzK-selected star-forming galaxies, drawn from the Cosmic Evolution Survey, to perform a stacking analysis of their 1.4 GHz radio continuum as a function of different stellar population properties, after cleaning the sample from contamination by active galactic nuclei. Dust unbiased SFRs are derived from radio fluxes assuming the local radio-IR correlation. The main results of this work are: (1) specific star formation rate (SSFR) s are constant over about 1 dex in stellar mass and up to the highest stellar mass probed, (2) the dust attenuation is a strong function of galaxy stellar mass with more massive galaxies being more obscured than lower mass objects, (3) a single value of the UV extinction applied to all galaxies would lead to a gross underestimate of the SFR in massive galaxies, (4) correcting the observed UV luminosities for dust attenuation based on the Calzetti recipe provides results in very good agreement with the radio derived ones, (5) the mean SSFR of our sample steadily decreases by a factor of similar to 4 with decreasing redshift from z = 2.3 to 1.4 and a factor of similar to 40 down the local universe. These empirical SFRs would cause galaxies to dramatically overgrow in mass if maintained all the way to low redshifts; we suggest that this does not happen because star formation is progressively quenched, likely starting from the most massive galaxies. C1 [Pannella, M.; Carilli, C. L.; Owen, F. N.; Strazzullo, V.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Daddi, E.; Aussel, H.] Univ Paris Diderot, CNRS, CEA, Lab AIM,Irfu SAp, F-91191 Gif Sur Yvette, France. [McCracken, H. J.; Mellier, Y.] Inst Astrophys, F-75014 Paris, France. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Scoville, N.; Smolcic, V.; Salvato, M.] CALTECH, Pasadena, CA 91125 USA. [Taniguchi, Y.] Ehime Univ, Grad Sch Sci & Engn, Bunkyo, Matsuyama 7908577, Japan. [Kneib, J. P.] Lab Astrophys Marseille, F-13388 Marseille 13, France. [Ilbert, O.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ilbert, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Thompson, D.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ USA. [Willott, C. J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Pannella, M (reprint author), Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. EM mpannell@nrao.edu RI Daddi, Emanuele/D-1649-2012; Kneib, Jean-Paul/A-7919-2015 OI Daddi, Emanuele/0000-0002-3331-9590; Kneib, Jean-Paul/0000-0002-4616-4989 FU ASI; NASA [G07-8136A, HST-GO-09822]; [ANR-07-BLAN-0228-03]; [ANR-08-JCJC-0008] FX We thank the anonymous referee for constructive comments that improved the presentation of our results. M. P., V. S., and C. L. C. acknowledge partial support from the Max-Planck Forschungspreise 2005. E. D. and H. J. Mc. C. acknowledge support from the French grants ANR-07-BLAN-0228-03 and ANR-08-JCJC-0008. A. R. acknowledges support from the ASI grant COFIS. F. C. acknowledges support from NASA-Chandra grant G07-8136A. This work is based in part on data products produced at TERAPIX. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. We gratefully acknowledge the contributions of the entire COSMOS collaboration. NR 53 TC 190 Z9 190 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2009 VL 698 IS 2 BP L116 EP L120 DI 10.1088/0004-637X/698/2/L116 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 458VB UT WOS:000267052600010 ER PT J AU McElwain, JC Wagner, PJ Hesselbo, SP AF McElwain, Jennifer C. Wagner, Peter J. Hesselbo, Stephen P. TI Fossil Plant Relative Abundances Indicate Sudden Loss of Late Triassic Biodiversity in East Greenland SO SCIENCE LA English DT Article ID JURASSIC BOUNDARY; EXTINCTION EVENT; NORTHERN; DISTRIBUTIONS; STRATIGRAPHY; TERRESTRIAL; TRANSITION; VEGETATION AB The pace of Late Triassic (LT) biodiversity loss is uncertain, yet it could help to decipher causal mechanisms of mass extinction. We investigated relative abundance distributions (RADs) of six LT plant assemblages from the Kap Stewart Group, East Greenland, to determine the pace of collapse of LT primary productivity. RADs displayed not simply decreases in the number of taxa, but decreases in the number of common taxa. Likelihood tests rejected a hypothesis of continuously declining diversity. Instead, the RAD shift occurred over the upper two-to-four fossil plant assemblages and most likely over the last three (final 13 meters), coinciding with increased atmospheric carbon dioxide concentration and global warming. Thus, although the LT event did not induce mass extinction of plant families, it accompanied major and abrupt change in their ecology and diversity. C1 [McElwain, Jennifer C.] Natl Univ Ireland Univ Coll Dublin, UCD Sch Biol & Environm Sci, Dublin 4, Ireland. [Wagner, Peter J.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. [Hesselbo, Stephen P.] Univ Oxford, Dept Earth Sci, Oxford OX1 3PR, England. RP McElwain, JC (reprint author), Natl Univ Ireland Univ Coll Dublin, UCD Sch Biol & Environm Sci, Dublin 4, Ireland. EM jennifer.mcelwain@ucd.ie RI Wagner, Peter/A-5514-2009; OI Wagner, Peter/0000-0002-9083-9787; McElwain, Jennifer/0000-0002-1729-6755 FU Marie Curie [MEXT-CT- 2006-042531, NSF-EAR-0207874] FX J.C.M. collected plant paleoecological data, S.P.H collected isotopic and stratigraphic data, and P.J.W. undertook data analyses. J.C.M and P.J.W cowrote the paper, and all authors contributed equally to interpretation. We gratefully acknowledge funding from a Marie Curie Excellence Grant (MEXT-CT- 2006-042531) to J.C.M. and NSF-EAR-0207874 to P.J.W. This is Paleobiology Database contribution 95. NR 28 TC 54 Z9 55 U1 2 U2 19 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 JUN 19 PY 2009 VL 324 IS 5934 BP 1554 EP 1556 DI 10.1126/science.1171706 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 459SU UT WOS:000267130600042 PM 19541995 ER PT J AU Rufus, J Stark, G Thorne, AP Pickering, JC Blackwell-Whitehead, RJ Blackie, D Smith, PL AF Rufus, J. Stark, G. Thorne, A. P. Pickering, J. C. Blackwell-Whitehead, R. J. Blackie, D. Smith, Peter L. TI High-resolution photoabsorption cross-section measurements of SO2 at 160 K between 199 and 220 nm SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID STATE-SELECTIVE DETECTION; HUBBLE-SPACE-TELESCOPE; JET-COOLED SO2; IOS PELE PLUME; SULFUR-DIOXIDE; FLUORESCENCE SPECTROSCOPY; ATMOSPHERE; VENUS; ULTRAVIOLET; PHOTODISSOCIATION AB Photoabsorption cross sections of sulfur dioxide over a range of temperatures are required to interpret observations and to support models of the atmospheres of Io and Venus. We report high-resolution (lambda/Delta lambda approximate to 450,000) photoabsorption cross-section measurements by Fourier transform spectrometry of SO2 at 160 K in the wavelength region 199 to 220 nm, which encompasses the strongest features in the prominent (C) over tilde (1) B-2 -(X) over tilde (1)A(1) system. Our results are compared with literature values obtained at lower resolutions and with 295 K cross sections recorded earlier with the same instrument. C1 [Rufus, J.; Thorne, A. P.; Pickering, J. C.; Blackwell-Whitehead, R. J.; Blackie, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Stark, G.] Wellesley Coll, Dept Phys, Wellesley, MA 02481 USA. [Smith, Peter L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blackwell-Whitehead, R. J.] Lund Observ, S-22100 Lund, Sweden. RP Rufus, J (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. EM gstark@wellesley.edu FU NASA [NNX08AE78G]; STFC(PPARC) of the United Kingdom FX This work was supported by NASA grant NNX08AE78G to Wellesley College and by the STFC(PPARC) of the United Kingdom. NR 59 TC 13 Z9 13 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN 16 PY 2009 VL 114 AR E06003 DI 10.1029/2008JE003319 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460LU UT WOS:000267190000002 ER PT J AU Gowaty, PA Hubbell, SP AF Gowaty, Patricia Adair Hubbell, Stephen P. TI Reproductive decisions under ecological constraints: It's about time SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE demographic stochasticity; encounter probability; mate choice; sexual selection; survival probability ID BLUEBIRDS SIALIA-SIALIS; DECREASE OFFSPRING VIABILITY; FEMALE MATE CHOICE; PREDATION RISK; DROSOPHILA-PSEUDOOBSCURA; SEXUAL SELECTION; ANAS-PLATYRHYNCHOS; MATING SUCCESS; PREFERENCES; EVOLUTION AB The switch point theorem (SPT) is the quantitative statement of the hypothesis that stochastic effects on survival, mate encounter, and latency affect individuals' time available for mating, the mean and variance in fitness, and thus, originally favored the evolution of individuals able to make adaptively flexible reproductive decisions. The SPT says that demographic stochasticity acting through variation in (i) individual survival probability, s; (ii) individual encounter probability, e; (iii) latency, l; (iv) the number of potential mates in the population, n; and (v) the distribution of fitness conferred, the w distribution, together affect average lifetime fitness, and induce adaptive switches in individual reproductive decisions. The switch point is the rank of potential mates at which focal individuals switch from accepting to rejecting potential mates, a decision rule that the SPT proves maximizes the average lifetime fitness of a focal individual under given values of ecological constraints on time. The SPT makes many predictions, including that the shape of the distribution of fitness conferred affects individual switch points. All else equal, higher probabilities of individual survival and encounter decrease the fraction of acceptable potential mates, such that focal individuals achieve higher average lifetime fitness by rejecting more potential mates. The primary prediction of the SPT is that each decision a focal individual makes is determined jointly by e, s, l, n, and the w distribution. C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. Univ Calif Los Angeles, Inst Environm, Los Angeles, CA 90095 USA. Smithsonian Trop Res Inst, APO, AA 34002 USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu FU National Science Foundation FX We thank John Avise and Francisco Ayala for inviting P. A. G. to contribute to the Arthur M. Sackler Colloquia of "In the Light of Evolution III: Two Centuries of Darwin'' and J. P. Drury, Brant Faircloth, Graham Pyke, Steve Shuster, and Elliott Sober for comments on a previous version of the manuscript. This work was supported by National Science Foundation grant "Beyond Bateman,'' which has allowed us and our collaborators, W. W. Anderson and Y. K. Kim, to study variances in number of mates and reproductive success in 3 species of flies with different gamete size asymmetries. NR 60 TC 45 Z9 45 U1 2 U2 40 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 JUN 16 PY 2009 VL 106 BP 10017 EP 10024 DI 10.1073/pnas.0901130106 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 458TP UT WOS:000267046700012 PM 19528648 ER PT J AU Eberhard, WG AF Eberhard, William G. TI Postcopulatory sexual selection: Darwin's omission and its consequences SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE cryptic female choice; sexually antagonistic coevolution ID CRYPTIC FEMALE CHOICE; COPULATORY COURTSHIP; ANTAGONISTIC COEVOLUTION; REPRODUCTIVE PROTEINS; SPERM COMPETITION; FERTILIZATION SUCCESS; MOLECULAR EVOLUTION; ADAPTIVE EVOLUTION; MATING-BEHAVIOR; WATER STRIDERS AB In one of his few major oversights, Darwin failed to appreciate that male-male competition and sexual selection can continue even after copulation has begun. The postcopulatory equivalents of both direct male-male battles (sperm competition) and female choice (cryptic female choice) occur within the female's body. Recognition of this hidden, but intense, sexual competition provides new insights into a variety of fields. These include the hyperdiverse and paradoxically elaborate morphology of both sperm and male genitalia, the equally puzzling and elaborate morphology of nongenitalic male structures that are specialized to grasp and stimulate females, powerful manipulative effects of substances in male semen on female reproductive physiology, paradoxical male courtship behavior that occurs after copulation has already begun, variability in parental investments, and the puzzlingly complex and diverse interactions between sperm and female products that surround animal eggs and between male gametophytes and female tissues in flowering plants. Many bizarre traits are involved, including male genitalia that are designed to explode or fall apart during copulation leaving behind parts within the female, male genitalia that "sing'' during copulation, potent seminal products that invade the female's body cavity and her nervous system to influence her behavior, and a virtual Kama Sutra of courtship behavior performed after rather than before genital coupling, including male-female dialogues during copulation. 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, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Sminthsonian Tropical Research Institute; Universidad de Costa Rica FX I thank F. Ayala and J. Avise for inviting me to participate in the colloquium and M.-J. West-Eberhard, H. Lessios, and 2 referees for useful comments. This work was supported by the Sminthsonian Tropical Research Institute and the Universidad de Costa Rica. NR 98 TC 74 Z9 76 U1 5 U2 97 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 JUN 16 PY 2009 VL 106 BP 10025 EP 10032 DI 10.1073/pnas.0901217106 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 458TP UT WOS:000267046700013 PM 19528642 ER PT J AU Williams, RME Irwin, RP Zimbelman, JR AF Williams, Rebecca M. E. Irwin, Rossman P., III Zimbelman, James R. TI Evaluation of paleohydrologic models for terrestrial inverted channels: Implications for application to martian sinuous ridges SO GEOMORPHOLOGY LA English DT Review DE Fluvial geomorphology; Mars; Hydrologic models ID MARS GLOBAL SURVEYOR; GRAVEL-BED RIVERS; FLOW RESISTANCE; MOUNTAIN RIVERS; ORBITER CAMERA; SURFACE; SCALE; BASIN; CONSTRAINTS; HYDRAULICS AB Fluvial systems can be preserved in inverted relief on both Earth and Mars. Few studies have evaluated the applicability of various paleohydrological models to inverted fluvial systems. The first phase of this investigation focused on an extensive (spanning similar to 12 km) inverted paleochannel system that consists of four sandstone-capped, carbonate-cemented, sinuous ridges within the Early Cretaceous Cedar Mountain Formation located southwest of Green River, Utah. Morphologic and sedimentologic observations of the exhumed paleochannels were used to evaluate multiple numerical models for reconstructing paleofluvial hydrological parameters. Another objective of the study was to determine whether aerial or orbital observations yield model results that are consistent with those constrained by field data. The models yield an envelope of plausible dominant discharge values (100-500 m(3)/s), reflecting the limitations of the approach, and no single model can be used to reliably estimate paleodischarge. On Mars, landforms with attributes consistent with inverted channels have been identified. In spite of differences in the formation history between these martian landforms and the terrestrial analog described here, including potential differences in cement composition and the erosional agent that was responsible for relief inversion, these numerical models can be applied (with modification) to the martian landforms and yield an envelope of plausible values for dominant discharge. (C) 2009 Elsevier B.V. All rights reserved. C1 [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Irwin, Rossman P., III; Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Williams, RME (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM williams@psi.edu FU NASA Mars Fundamental Research [NNX06AB21 G]; Smithsonian Institution; Planetary Science Institute [444] FX The authors are grateful to A. Johnston (Smithsonian Institution) for technical advice, T. Chidsey (Utah Geologial Survey) and Brian S. Curie (Miami University-Ohio) for information regarding the study site, and Doug Cox for development of USAPhotoMaps. This manuscript was improved by comments of V. Baker, G. Komatsu, A. Howard and two anonymous reviewers. This research was supported by a NASA Mars Fundamental Research Grant #NNX06AB21 G and a research grant from the Becker Endowment from the Smithsonian Institution awarded to R.M.E. Williams. This is Planetary Science Institute contribution #444. NR 112 TC 29 Z9 29 U1 1 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X J9 GEOMORPHOLOGY JI Geomorphology PD JUN 15 PY 2009 VL 107 IS 3-4 BP 300 EP 315 DI 10.1016/j.geomorph.2008.12.015 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 451FI UT WOS:000266455700015 ER PT J AU Riley, S AF Riley, Sheila TI American Adulterer SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila] Smithsonian Inst Libs, Washington, DC USA. RP Riley, S (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 JUN 15 PY 2009 VL 134 IS 11 BP 63 EP 63 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 460QQ UT WOS:000267202600049 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Social Web Evolution: Integrating Semantic Applications and Web 2.0 Technologies. SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUN 15 PY 2009 VL 134 IS 11 BP 93 EP 93 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 460QQ UT WOS:000267202600181 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Modern Language Association. MLA Handbook for Writers of Research Papers, 7th edition. SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. RP Guz, SS (reprint author), Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 4 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 JUN 15 PY 2009 VL 134 IS 11 BP 94 EP 94 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 460QQ UT WOS:000267202600186 ER PT J AU Carvajal-Ortiz, H Mora, G Jaramillo, C AF Carvajal-Ortiz, H. Mora, G. Jaramillo, C. TI A molecular evaluation of bulk organic carbon-isotope chemostratigraphy for terrestrial correlations: An example from two Paleocene-Eocene tropical sequences SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Late Cretaceous-Early Eocene; Carbon-isotope chemostratigraphy; Geochemical biomarker ratios; Terrestrial-derived organic matter; Diagenesis ID CRETACEOUS-TERTIARY BOUNDARY; FOSSIL WOOD; CYCLE PERTURBATION; THERMAL MAXIMUM; METHANE HYDRATE; BASIN; BIOMARKERS; SEDIMENTS; MARINE; MATTER AB The dynamics associated with the carbon cycle and the linkage between the oceans, the atmosphere, and land plants provide an opportunity to correlate marine and terrestrial sedimentary sequences using stable isotopes of carbon (delta(13)C), but few studies have tested this approach. For instance, it has been proposed that changes in plant community (e.g., gymnosperm-dominated vs. angiosperm-dominated) could have significantly altered/amplified the carbon-isotope ratios of bulk sedimentary organic matter derived from land plants (delta(13)C(TOM)), compared to that of the marine carbonates (delta(13)C(carbonate)). Here, delta(13)C(TOM) values in a terrestrial sequence of the Colombian tropics are compared to the composite Paleocene-Eocene delta(13)C(carbonate) curve from Zachos et al. (2001) to evaluate the use of delta(13)C(TOM) values as a reliable chronostratigraphic tool. Sediments of the studied terrestrial sequences were deposited in a transitional setting dominated by mudstones, coals, and small lenses of sandstones (Late Cretaceous-Middle Paleocene sediments) and in a mixture of deltaic and fluvial conditions (Late Paleocene-Early Eocene sediments). The biostratigraphic control was based on palynological zones for the region. The delta(13)C(TOM) values for the studied terrestrial sequence show three carbon-isotope excursions, which correlate closely with those present in the marine record. The delta(13)C(TOM) values decreased from -24.2 parts per thousand to -26.5 parts per thousand in sediments accumulated during Early to Middle Paleocene, increased from -26.5 parts per thousand to -23.8 parts per thousand during the Late Paleocene, and decreased from -23.8 parts per thousand to -26.5 parts per thousand near the Paleocene-Eocene boundary (52-50 Ma). Selected biomarkers indicate that most of the organic matter derived from both gymnosperms and angiosperms. Moreover, the analyses of selected biomarker ratios (CPI, Pr/Ph, P(aq), and beta beta/beta beta + alpha beta hopanes) show some diagenetic transformation in the preserved organic matter. However, no correlation between diagenesis and delta(13)C(TOM) values was detected, thus suggesting that delta(13)C(TOM) could be correlated with delta(13)C(carbonate) values. The close correspondence that was found between delta(13)C(TOM) and delta(13)C(carbonate) values (Delta(13)C(TOM-carbonate) similar to -27%.) provides support to the hypothesis that a tight land-plant-oceans linkage exists through geologic timescales via atmospheric carbon dioxide. (C) 2009 Elsevier B.V. All rights reserved. C1 [Carvajal-Ortiz, H.; Mora, G.] Iowa State Univ, Dept Geol & Atmospher Sci, Ames, IA 50011 USA. [Jaramillo, C.] Smithsonian Trop Res Inst, Balboa, Panama. RP Carvajal-Ortiz, H (reprint author), Indiana Univ, Dept Geol Sci, Bloomington, IN 47405 USA. EM carvajah@indiana.edu; gmora@iastate.edu; JaramilloC@si.edu FU Smithsonian Tropical Research Institute; Instituto Colombiano, del Petroleo, and Geological Society of America [8229-06] FX The authors thank Smithsonian Tropical Research Institute, Instituto Colombiano, del Petroleo, and Geological Society of America (grant 8229-06) for financial and logistic support. Thanks to Dr. S. Hesselbo and an anonymous reviewer for the detailed comments on the manuscript. Thanks to Maria Ines Barreto for her continuous source of ideas. Thanks in general to our families for their patience and continuous support. NR 54 TC 10 Z9 10 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD JUN 15 PY 2009 VL 277 IS 3-4 BP 173 EP 183 DI 10.1016/j.palaeo.2009.03.015 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 462FS UT WOS:000267336000003 ER PT J AU de Santana, CD Vari, RP AF de Santana, Carlos David Vari, Richard P. TI The South American Electric Fish Genus Platyurosternarchus (Gymnotiformes: Apteronotidae) SO COPEIA LA English DT Article ID TELEOSTEI; KNIFEFISH AB The electric fish genus Platyurosternarchus, family Apteronotidae, is reviewed based on both external morphology and osteology. Synapomorphies for Platyurosternarchus are identified, the genus is diagnosed, and a key to the species is provided. Platyurosternarchus crypticus, a new species, is described from the upper reaches of the Rio Branco in the northern portions of the Amazon basin. Platyurosternarchus macrostoma from the Amazonas, Orinoco, and Essequibo River basins is redescribed. The species differ In the form of the laterosensory canal segment in the soft tissues of the ventral portion of the head and within the preopercle, the posterior extent of the mid-dorsal electroreceptive filament, and the morphology of the first and fourth branchiostegal rays. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, MRC-159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu FU Smithsonian Predoctoral Fellowship in the Division of Fishes, National Museum of Natural History; Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, National Museum of Natural History, Smithsonian Institution FX Support for this project came from a Smithsonian Predoctoral Fellowship in the Division of Fishes, National Museum of Natural History (CDS), and the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, National Museum of Natural History, Smithsonian Institution (RPV). We thank J. Alves-Gomes, J. Armbruster, L. Chao, J. Friel, K. Hartel, C, Hopkins, Z. Lucena, J. Lundberg, D. Nelson, F. Provenzano, M. Sabaj Perez, L. Rapp Py-Daniel, R. Reis, M. Retzer, R. Robins, M. Rogers, D. Taphorn, and D. Werneke for access to specimens and information. J. Maclaine provided invaluable assistance in clarifying the identity of the holotype of Sternarchus inacrostoma and generously provided us with photographs and radiographs of specimens pertinent to the question of the identity of that species along with other information. M. Sabaj Perez provided information on habitats where several samples of both species of Platyurosternarchus originated along with photographs that were the basis of the life coloration descriptions. Figures 1 and 5 were prepared by T. Britt Griswold, Figures 2 and 3 by D. Marques, and Figure 4 by S. Raredon who also provided assistance throughout the study. The paper benefited from the comments and suggestions of T. Munroe and C. Ferraris, Jr. NR 37 TC 6 Z9 9 U1 1 U2 5 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD JUN 12 PY 2009 IS 2 BP 233 EP 244 DI 10.1643/CI-08-082 PG 12 WC Zoology SC Zoology GA 459YX UT WOS:000267151100005 ER PT J AU Girart, JM Beltran, MT Zhang, QZ Rao, R Estalella, R AF Girart, Josep M. Beltran, Maria T. Zhang, Qizhou Rao, Ramprasad Estalella, Robert TI Magnetic Fields in the Formation of Massive Stars SO SCIENCE LA English DT Article ID SUBMILLIMETER ARRAY; CLOUD CORES; ACCRETION; COLLAPSE; POLARIZATION; G31.41+0.31; BRAKING; GAS; FRAGMENTATION; OUTFLOW AB Massive stars play a crucial role in the production of heavy elements and in the evolution of the interstellar medium, yet how they form is still a matter of debate. We report high-angular-resolution submillimeter observations toward the massive hot molecular core (HMC) in the high-mass star-forming region G31.41+0.31. We find that the evolution of the gravitational collapse of the HMC is controlled by the magnetic field. The HMC is simultaneously contracting and rotating, and the magnetic field lines threading the HMC are deformed along its major axis, acquiring an hourglass shape. The magnetic energy dominates over the centrifugal and turbulence energies, and there is evidence of magnetic braking in the contracting core. C1 [Girart, Josep M.] Inst Estudis Catalunya IEEC, CSIC, Inst Ciencies Espai, Bellaterra 08193, Catalunya, Spain. [Beltran, Maria T.; Estalella, Robert] Univ Barcelona, Dept Astron & Meteorol IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Catalunya, Spain. [Beltran, Maria T.; Estalella, Robert] Univ Barcelona, Unitat Assoc CSIC, E-08028 Barcelona, Catalunya, Spain. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rao, Ramprasad] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. RP Girart, JM (reprint author), Inst Estudis Catalunya IEEC, CSIC, Inst Ciencies Espai, Campus Univ Autonoma Barcelona,Torre C5 Parell 2A, Bellaterra 08193, Catalunya, Spain. EM girart@ieec.cat RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Zhang, Qizhou/0000-0003-2384-6589 FU Ministerio de Ciencia e Innovacion (Spain) [AYA2005-08523-C03, AYA2008-06189-C03]; Agencia de Gestio d Ajuts Universitaris i de Recerca [2005-SGR00489] 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. We thank D. Galli, R. R. Cesaroni, and J. M. Torrelles for helpful comments. J.M.G., M.T.B., and R.E. acknowledge Ministerio de Ciencia e Innovacion (Spain) for support through grants AYA2005-08523-C03 and AYA2008-06189-C03. J.M.G. also acknowledges support from Agencia de Gestio d Ajuts Universitaris i de Recerca 2005-SGR00489 grant. NR 29 TC 106 Z9 107 U1 0 U2 4 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 JUN 12 PY 2009 VL 324 IS 5933 BP 1408 EP 1411 DI 10.1126/science.1171807 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 456VD UT WOS:000266878700035 PM 19520952 ER PT J AU Degenaar, N Wijnands, R Wolff, MT Ray, PS Wood, KS Homan, J Lewin, WHG Jonker, PG Cackett, EM Miller, JM Brown, EF AF Degenaar, N. Wijnands, R. Wolff, M. T. Ray, P. S. Wood, K. S. Homan, J. Lewin, W. H. G. Jonker, P. G. Cackett, E. M. Miller, J. M. Brown, E. F. TI Chandra and Swift observations of the quasi-persistent neutron star transient EXO 0748-676 back to quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: eclipsing; stars: individual: EXO 0748-676; stars: neutron; X-rays: binaries ID X-RAY TRANSIENT; KS-1731-260; EMISSION; MXB-1659-29; CRUST; MASS; BURSTS AB The quasi-persistent neutron star X-ray transient and eclipsing binary EXO 0748-676 recently started the transition to quiescence following an accretion outburst that lasted more than 24 years. We report on two Chandra and 12 Swift observations performed within five months after the end of the outburst. The Chandra spectrum is composed of a soft, thermal component that fits to a neutron star atmosphere model with kT8(infinity) similar to 0.12 keV, joined by a hard power-law tail that contributes similar to 20 per cent of the total 0.5-10 keV unabsorbed flux. The combined Chandra/Swift data set reveals a relatively hot and luminous quiescent system with a temperature of kT8(infinity) similar to 0.11-0.13 keV and a bolometric thermal luminosity of similar to 8.1 x 10(33)-1.6 x 10(34) (d/7.4 kpc)(2) erg s(-1). We discuss our results in the context of cooling neutron star models. C1 [Degenaar, N.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Wolff, M. T.; Ray, P. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Homan, J.; Lewin, W. H. G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cackett, E. M.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48105 USA. [Brown, E. F.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Degenaar, N (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM N.D.Degenaar@uva.nl RI Brown, Edward/F-1721-2011; OI Brown, Edward/0000-0003-3806-5339; Ray, Paul/0000-0002-5297-5278 FU NASA; United States Office of Naval Research; Chandra [GO8-9045X] FX We are grateful to the referee, Nathalie Webb, for very useful comments. This work was supported by the Netherlands Organization for Scientific Research (NWO). We acknowledge the use of the Swift public data archive. EMC was supported by NASA through the Chandra Fellowship Program. MTW, PSR and KSW acknowledge the United States Office of Naval Research. JH and WHGL gratefully acknowledge support from Chandra grant GO8-9045X. NR 35 TC 28 Z9 28 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2009 VL 396 IS 1 BP L26 EP L30 DI 10.1111/j.1745-3933.2009.00655.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000006 ER PT J AU Karastergiou, A Hotan, AW van Straten, W McLaughlin, MA Ord, SM AF Karastergiou, A. Hotan, A. W. van Straten, W. McLaughlin, M. A. Ord, S. M. TI Radio polarization measurements from RRAT J1819-1458 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE polarization; pulsars: individual: J1819-1458 ID SOUTHERN PULSARS; TRANSIENT J1819-1458; TIMING OBSERVATIONS; EMISSION; MAGNETAR; POLARIMETRY; GEOMETRY; BEAMS; MODEL AB We present the first polarization measurements of the radio emission from RRAT J1819-1458. Our observations, conducted in parallel to regular timing sessions, have yielded a small number of bright and polarized pulses. The polarization characteristics and integrated profile resemble those of normal pulsars with average spin-down energy. E : moderate to low linear polarization in the integrated profile despite relatively high polarization in the individual pulses. On average, a small degree of circular polarization is also observed. The polarization position angle (PA) executes a remarkably smooth, steep S-shaped curve, interrupted by two orthogonal jumps. Based on the shape of the PA swing, we place some constraints on the emission geometry. We compare these polarization properties to those of other radio-emitting neutron star populations, including young pulsars, pulsars with a high surface magnetic field and radio-emitting magnetars. From the polarization measurements, the Faraday rotation measure of this rotating radio transient is derived. C1 [Karastergiou, A.] Univ Oxford, Oxford OX1 3RH, England. [Hotan, A. W.] Curtin Univ Technol, Curtin Inst Radio Astron, Perth, WA 6845, Australia. [van Straten, W.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [McLaughlin, M. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. [McLaughlin, M. A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Ord, S. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Karastergiou, A (reprint author), Univ Oxford, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM aris.karastergiou@gmail.com RI Ord, Stephen/C-6138-2013; OI van Straten, Willem/0000-0003-2519-7375 NR 31 TC 8 Z9 9 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2009 VL 396 IS 1 BP L95 EP L99 DI 10.1111/j.1745-3933.2009.00671.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000020 ER PT J AU Watabe, Y Risaliti, G Salvati, M Nardini, E Sani, E Marconi, A AF Watabe, Y. Risaliti, G. Salvati, M. Nardini, E. Sani, E. Marconi, A. TI The active galactic nuclei/starburst content in high-redshift ultraluminous infrared galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: nuclei; galaxies: starburst ID SPITZER-SPACE-TELESCOPE; SUBMILLIMETER GALAXIES; MIDINFRARED SPECTROSCOPY; SPECTRA; DIAGNOSTICS; STARBURSTS; EVOLUTION; SCUBA; IRS AB We apply a simple model, tested on local ultraluminous infrared galaxies (ULIRGs), to disentangle the active galactic nuclei (AGN) and starburst contributions in submillimetre and 24 mu m-selected ULIRGs observed with the Spitzer-Infrared Spectrograph spectrometer. We quantitatively estimate the average AGN contribution to the stacked 6-8 mu m rest-frame spectra of these sources in different luminosity and redshift ranges and, under the assumption of similar infrared-to-bolometric ratios as in local ULIRGs, the relative AGN/starburst contributions to the total infrared luminosity. Though the starburst component is always dominant in submillimetre-selected ULIRGs, we find a significant increase of the AGN contribution at redshift z > 2.3 with respect to lower z objects. Finally, we quantitatively confirm that the mid-infrared emission of 24 mu m-selected ULIRGs is dominated by the AGN component, but the starburst component contributes significantly to the bolometric luminosity. C1 [Watabe, Y.; Risaliti, G.; Salvati, M.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nardini, E.; Sani, E.; Marconi, A.] Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. RP Watabe, Y (reprint author), Osserv Astrofis Arcetri, INAF, Lgo E Fermi 5, I-50125 Florence, Italy. EM watabe@arcetri.astro.it RI Marconi, Alessandro/C-5880-2009; OI Marconi, Alessandro/0000-0002-9889-4238; Risaliti, Guido/0000-0002-3556-977X FU PRIN [MUR 2006025203]; ASI [INAF I/088/06/0] FX We thank the anonymous reviewer for valuable comments. This work has been partly supported by grant PRIN-MUR 2006025203 and ASI-INAF I/088/06/ NR 28 TC 12 Z9 12 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2009 VL 396 IS 1 BP L1 EP L5 DI 10.1111/j.1745-3933.2009.00649.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000001 ER PT J AU Younger, JD Hayward, CC Narayanan, D Cox, TJ Hernquist, L Jonsson, P AF Younger, Joshua D. Hayward, Christopher C. Narayanan, Desika Cox, T. J. Hernquist, Lars Jonsson, Patrik TI The merger-driven evolution of warm infrared luminous galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; galaxies: starburst; infrared: galaxies ID SUPERMASSIVE BLACK-HOLES; PARTICLE HYDRODYNAMICS SIMULATIONS; STAR-FORMATION HISTORY; RADIATIVE-TRANSFER; SUBMILLIMETER GALAXIES; ULTRALUMINOUS GALAXIES; ORBITAL PARAMETERS; ELLIPTIC GALAXIES; MAJOR MERGERS; DUST AB We present a merger-driven evolutionary model for the production of luminous (LIRGs) and ultraluminous infrared galaxies (ULIRGs) with warm infrared (IR) colours. Our results show that simulations of gas-rich major mergers including star formation, black hole growth and feedback can produce warm (U) LIRGs. We also find that while the warm evolutionary phase is associated with increased active galactic nucleus (AGN) activity, star formation alone may be sufficient to produce warm IR colours. However, the transition can be suppressed entirely - even when there is a significant AGN contribution - when we assume a single-phase interstellar medium, which maximizes the attenuation. Finally, our evolutionary models are consistent with the 25-to-60 mu m flux density ratio versus L(HX)/L(IR) relation for local LIRGs and ULIRGs, and predict the observed scatter in IR colour at fixed L(HX)/L(IR). Therefore, our models suggest a cautionary note in the interpretation of warm IR colours: while associated with periods of active black hole growth, they are probably produced by a complex mix of star formation and AGN activity intermediate between the cold star formation dominated phase and the birth of a bright, unobscured quasar. C1 [Younger, Joshua D.; Hayward, Christopher C.; Narayanan, Desika; Cox, T. J.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonsson, Patrik] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Younger, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyounger@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU Performance Computing Cluster in Boston, MA [HST-AR-10678, 10958]; NASA; Space Telescope Science Institute; Association of Universities for Research in Astronomy [NAS5-26555]; Spitzer Theory; Jet Propulsion Laboratory; National Science Foundation Graduate Research Fellowship; W. M. Keck Foundation FX We thank Giovanni G. Fazio, Stephanie J. Bush, Dusan Keres and Phillip F. Hopkins for helpful discussions. The simulations and radiative transfer calculations presented here were performed on the Harvard FAS High Performance Computing Cluster in Boston, MA. PJ was supported by programs HST-AR-10678 and 10958, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and by Spitzer Theory Grant 30183 from the Jet Propulsion Laboratory. CCHacknowledges support from a National Science Foundation Graduate Research Fellowship. This work was supported in part by a grant from the W. M. Keck Foundation. NR 72 TC 42 Z9 42 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2009 VL 396 IS 1 BP L66 EP L70 DI 10.1111/j.1745-3933.2009.00663.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 453KT UT WOS:000266610000014 ER PT J AU Currie, T Lada, CJ Plavchan, P Robitaille, TP Irwin, J Kenyon, SJ AF Currie, Thayne Lada, Charles J. Plavchan, Peter Robitaille, Thomas P. Irwin, Jonathan Kenyon, Scott J. TI THE LAST GASP OF GAS GIANT PLANET FORMATION: A SPITZER STUDY OF THE 5 Myr OLD CLUSTER NGC 2362 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; open clusters and associations (individual: NGC 2362); planetary systems: formation; planetary systems: protoplanetary disks; stars: pre-main sequence ID LOW-MASS STARS; YOUNG STELLAR OBJECTS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; DEBRIS DISK CANDIDATES; INFRARED ARRAY CAMERA; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISK; SPACE-TELESCOPE; CHI-PERSEI AB Expanding upon the Infrared Array Camera (IRAC) survey from Dahm & Hillenbrand, we describe Spitzer IRAC and Multiband Imaging Photometer for Spitzer observations of the populous, 5 Myr old open cluster NGC 2362. We analyze the mid-IR colors of cluster members and compared their spectral energy distributions (SEDs) to star+circumstellar disk models to constrain the disk morphologies and evolutionary states. Early/intermediate-type confirmed/candidate cluster members either have photospheric mid-IR emission or weak, optically thin IR excess emission at lambda >= 24 mu m consistent with debris disks. Few late-type, solar/subsolar-mass stars have primordial disks. The disk population around late-type stars is dominated by disks with inner holes (canonical "transition disks") and "homologously depleted" disks. Both types of disks represent an intermediate stage between primordial disks and debris disks. Thus, in agreement with previous results, we find that multiple paths for the primordial-to-debris disk transition exist. Because these "evolved primordial disks" greatly outnumber primordial disks, our results undermine standard arguments in favor of a less than or similar to 10(5) yr timescale for the transition based on data from Taurus-Auriga. Because the typical transition timescale is far longer than 10(5) yr, these data also appear to rule out standard ultraviolet photoevaporation scenarios as the primary mechanism to explain the transition. Combining our data with other Spitzer surveys, we investigate the evolution of debris disks around high/intermediate-mass stars and investigate timescales for giant planet formation. Consistent with Currie et al., the luminosity of 24 mu m emission in debris disks due to planet formation peaks at approximate to 10-20 Myr. If the gas and dust in disks evolve on similar timescales, the formation timescale for gas giant planets surrounding early-type, high/intermediate-mass (greater than or similar to 1.4 M-circle dot) stars is likely 1-5 Myr. Most solar/subsolar-mass stars detected by Spitzer have SEDs that indicate their disks may be actively leaving the primordial disk phase. Thus, gas giant planet formation may also occur by similar to 5 Myr around solar/subsolar-mass stars as well. C1 [Currie, Thayne; Lada, Charles J.; Robitaille, Thomas P.; Irwin, Jonathan; Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. [Plavchan, Peter] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Irwin, Jonathan] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. EM tcurrie@cfa.harvard.edu; clada@cfa.harvard.edu; plavchan@ipac.caltech.edu; trobitaille@cfa.harvard.edu; jirwin@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Robitaille, Thomas/0000-0002-8642-1329 FU NASA through the Spitzer Space Telescope Fellowship Program (TPR) FX We thank Richard Alexander for useful comments about UV photoevaporation and Adam Kraus for very informative discussions on the role of binarity in disk evolution. We also thank Carol Grady for pointing out constraints on the formation of Saturn from the planetary science community. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program (TPR). NR 90 TC 103 Z9 103 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 JUN 10 PY 2009 VL 698 IS 1 BP 1 EP 27 DI 10.1088/0004-637X/698/1/1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700001 ER PT J AU Hughes, AM Andrews, SM Espaillat, C Wilner, DJ Calvet, N D'Alessio, P Qi, CH Williams, JP Hogerheijde, MR AF Hughes, A. Meredith Andrews, Sean M. Espaillat, Catherine Wilner, David J. Calvet, Nuria D'Alessio, Paola Qi, Chunhua Williams, Jonathan P. Hogerheijde, Michiel R. TI A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems: protoplanetary disks; stars: individual (GM Aurigae) ID T-TAURI STARS; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; ACCRETION DISKS; DUST EMISSION; EVOLUTION; PLANET AB We present 0 ''.3 resolution observations of the disk around GM Aurigae with the Submillimeter Array (SMA) at a wavelength of 860 mu m and with the Plateau de Bure Interferometer at a wavelength of 1.3 mm. These observations probe the distribution of disk material on spatial scales commensurate with the size of the inner hole predicted by models of the spectral energy distribution (SED). The data clearly indicate a sharp decrease in millimeter optical depth at the disk center, consistent with a deficit of material at distances less than similar to 20 AU from the star. We refine the accretion disk model of Calvet et al. based on the unresolved SED and demonstrate that it reproduces well the spatially resolved millimeter continuum data at both available wavelengths. We also present complementary SMA observations of CO J = 3-2 and J = 2-1 emission from the disk at 2 '' resolution. The observed CO morphology is consistent with the continuum model prediction, with two significant deviations: (1) the emission displays a larger CO J = 3-2/J = 2-1 line ratio than predicted, which may indicate additional heating of gas in the upper disk layers; and (2) the position angle of the kinematic rotation pattern differs by 11 degrees +/- 2 degrees from that measured at smaller scales from the dust continuum, which may indicate the presence of a warp. We note that photoevaporation, grain growth, and binarity are unlikely mechanisms for inducing the observed sharp decrease in opacity or surface density at the disk center. The inner hole plausibly results from the dynamical influence of a planet on the disk material. Warping induced by a planet could also potentially explain the difference in position angle between the continuum and CO data sets. C1 [Hughes, A. Meredith; Andrews, Sean M.; Wilner, David J.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espaillat, Catherine; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Hughes, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhughes@cfa.harvard.edu; sandrews@cfa.harvard.edu; ccespa@umich.edu; dwilner@cfa.harvard.edu; ncalvet@umich.edu; p.dalessio@astrosmo.unam.mx; cqi@cfa.harvard.edu; jpw@ifa.hawaii.edu; michiel@strw.leidenuniv.nl OI Williams, Jonathan/0000-0001-5058-695X FU NASA [NAG5-11777, HF-01203-A, NAS 5-26555, NNG05GI26G]; JPL [AR50406]; CONACyT, Mexico; NSF [AST-0808144] FX The authors thank the IRAM staff, particularly Roberto Neri, for their help with the observations and data reduction. They thank Lee Hartmann for helpful discussions in the early stages of this project, and Adam Kraus and Michael Ireland for sharing the results of their Keck observations of GM Aurigae. Partial support for this work was provided by NASA Origins of Solar Systems Program Grant NAG5-11777. A. M. H. acknowledges support from a National Science Foundation Graduate Research Fellowship. Support for S. M. A. was provided by NASA through Hubble Fellowship grant #HF-01203-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. N.C. acknowledges support from NASA Origins Grant NNG05GI26G and JPL grant AR50406. P. D. acknowledges grants from CONACyT, Mexico. J.P.W. acknowledges support from NSF grant AST-0808144. NR 82 TC 104 Z9 104 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 JUN 10 PY 2009 VL 698 IS 1 BP 131 EP 142 DI 10.1088/0004-637X/698/1/131 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700010 ER PT J AU Korn, AJ Richard, O Mashonkina, L Bessell, MS Frebel, A Aoki, W AF Korn, A. J. Richard, O. Mashonkina, L. Bessell, M. S. Frebel, A. Aoki, W. TI HE 1327-2326, AN UNEVOLVED STAR WITH [Fe/H] <-5.0. III. DOES ITS ATMOSPHERE REFLECT ITS NATAL COMPOSITION? SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffusion; stars: abundances; stars: evolution; stars: fundamental parameters; stars: individual (HE 1327-2326); stars: Population II ID METAL-POOR STARS; RADIATIVE ACCELERATION CALCULATIONS; LESS-THAN -5.0; NON-LTE; WMAP OBSERVATIONS; ATOMIC DIFFUSION; LINE FORMATION; 1ST STARS; FGK STARS; OLD STARS AB Based on spectroscopic constraints derived from nonlocal thermodynamic equilibrium line formation, we explore the likely range of stellar parameters (T-eff and log g) for the hyper-metal-poor (HMP) star HE 1327-2326. Combining the constraints from Balmer line profiles and the Ca I/II ionization equilibrium, a subgiant stage of evolution is indicated. This result is further supported by spectrophotometric observations of the Balmer jump. If a higher T-eff value was used (as favored by some photometric calibrations), the spectroscopic analysis would indicate a turnoff-point stage of evolution. Using a stellar-structure code that treats the effects of atomic diffusion throughout the star in detail, we evolve a low-mass model star to reach the Hertzsprung-Russell-diagram position of HE 1327-2326 after roughly 13 Gyr. While the surface abundances are modified significantly (by more than 1 dex for the case of uninhibited diffusion), such corrections cannot resolve the discrepancy between the abundance inferred from the nondetection of the Li I resonance line at 6707 angstrom and the Wilkinson Microwave Anisotropy Probe based primordial lithium abundance. As there are numerous processes that can destroy lithium, any cosmological interpretation of a lower-than-expected lithium abundance at the lowest metallicities will have to await sample sizes of unevolved HMP stars that are 1 order of magnitude larger. The situation remains equally inconclusive concerning atomic-diffusion corrections. Here, attempts have to be made to better constrain internal mixing processes, both observationally and by means of sophisticated modeling. With constraints on additional mixing processes taken from a recent globular-cluster study, the likeliest scenario is that HE 1327-2326's surface abundances have undergone mild depletion (of order 0.2 dex). C1 [Korn, A. J.] Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, S-75120 Uppsala, Sweden. [Richard, O.] Univ Montpellier 2, CNRS, GRAAL, F-34095 Montpellier, France. [Mashonkina, L.] Russian Acad Sci, Inst Astron, Moscow 119017, Russia. [Mashonkina, L.] Univ Munich, Inst Astron & Astrophys, D-81679 Munich, Germany. [Bessell, M. S.] Australian Natl Univ, RSAA, Weston, ACT 2611, Australia. [Frebel, A.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Frebel, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aoki, W.] Natl Astron Observ Japan, Tokyo 1818588, Japan. RP Korn, AJ (reprint author), Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, Box 515, S-75120 Uppsala, Sweden. EM andreas.korn@fysast.uu.se RI Richard, Olivier/B-9301-2012 OI Richard, Olivier/0000-0002-0342-5093 FU Swedish Research Council (Vetenskapradet); Presidium RAS Programme "Origin and evolution of stars and the Galaxy"; Deutsche Forschungsgemeinschaft [GE 490/34-1]; W. J. McDonald Fellowship of the McDonald Observatory; JSPS [18104003] FX A.J.K. acknowledges a research fellowship by the Swedish Research Council (Vetenskapradet). O.R. thanks the Centre Informatique National de l'Enseignement Superieur (CINES) and the Reseau Quebecoisde Calcul de Haute Performance (RQCHP) for providing the computational resources required for this work. M. L. is supported by Presidium RAS Programme "Origin and evolution of stars and the Galaxy" and the Deutsche Forschungsgemeinschaft with grant GE 490/34-1. A.F. is supported through the W. J. McDonald Fellowship of the McDonald Observatory. W.A. is supported by a Grant-in-Aid for Science Research from JSPS (grant 18104003). NR 37 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 JUN 10 PY 2009 VL 698 IS 1 BP 410 EP 416 DI 10.1088/0004-637X/698/1/410 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700030 ER PT J AU Munoz-Jaramillo, A Nandy, D Martens, PCH AF Munoz-Jaramillo, Andres Nandy, Dibyendu Martens, Petrus C. H. TI HELIOSEISMIC DATA INCLUSION IN SOLAR DYNAMO MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: helioseismology; Sun: interior; Sun: magnetic fields; Sun: rotation ID FLUX-TRANSPORT DYNAMO; DEEP MERIDIONAL FLOW; MAGNETIC-FIELD; DIFFERENTIAL ROTATION; CONVECTION ZONE; ACTIVE REGIONS; CYCLE; CIRCULATION; SUBSURFACE; EVOLUTION AB An essential ingredient in kinematic dynamo models of the solar cycle is the internal velocity field within the simulation domain-the solar convection zone (SCZ). In the last decade or so, the field of helioseismology has revolutionized our understanding of this velocity field. In particular, the internal differential rotation of the Sun is now fairly well constrained by helioseismic observations almost throughout the SCZ. Helioseismology also gives us some information about the depth dependence of the meridional circulation in the near-surface layers of the Sun. The typical velocity inputs used in solar dynamo models, however, continue to be an analytic fit to the observed differential rotation profile and a theoretically constructed meridional circulation profile that is made to match the flow speed only at the solar surface. Here, we take the first steps toward the use of more accurate velocity fields in solar dynamo models by presenting methodologies for constructing differential rotation and meridional circulation profiles that more closely conform to the best observational constraints currently available. We also present kinematic dynamo simulations driven by direct helioseismic measurements for the rotation and four plausible profiles for the internal meridional circulation-all of which are made to match the helioseismically inferred near-surface depth dependence, but whose magnitudes are made to vary. We discuss how the results from these dynamo simulations compare with those that are driven by purely analytic fits to the velocity field. Our results and analysis indicate that the latitudinal shear in the rotation in the bulk of the SCZ plays a more important role, than either the tachocline or surface radial shear, in the induction of the toroidal field. We also find that it is the speed of the equatorward counterflow in the meridional circulation right at the base of the SCZ, and not how far into the radiative interior it penetrates, that primarily determines the dynamo cycle period. Improved helioseismic constraints are expected to be available from future space missions such as the Solar Dynamics Observatory and through analysis of more long-term continuous data sets from ground-based instruments such as the Global Oscillation Network Group. Our analysis lays the basis for the assimilation of these helioseismic data within dynamo models to make future solar cycle simulations more realistic. C1 [Munoz-Jaramillo, Andres] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Research Kolkata, Kolkata 741252, WB, India. [Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM munoz@solar.physics.montana.edu; dnandi@iiserkol.ac.in; pmartens@cfa.harvard.edu OI Munoz-Jaramillo, Andres/0000-0002-4716-0840 NR 60 TC 28 Z9 28 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 JUN 10 PY 2009 VL 698 IS 1 BP 461 EP 478 DI 10.1088/0004-637X/698/1/461 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700036 ER PT J AU Morales, EFE Mardones, D Garay, G Brooks, KJ Pineda, JE AF Morales, Esteban F. E. Mardones, Diego Garay, Guido Brooks, Kate J. Pineda, Jaime E. TI A MULTIWAVELENGTH STUDY OF YOUNG MASSIVE STAR-FORMING REGIONS. III. MID-INFRARED EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; stars: early-type; stars: formation ID INFRARED ARRAY CAMERA; MULTIBAND IMAGING PHOTOMETER; SPECTRAL ENERGY-DISTRIBUTION; SPITZER-SPACE-TELESCOPE; PHYSICAL PARAMETERS; PROTOSTELLAR CORES; MOLECULAR CLOUDS; METHANOL MASERS; STELLAR OBJECTS; GALACTIC PLANE AB We present mid-infrared (MIR) observations, made with the TIMMI2 camera on the ESO 3.6 m telescope, toward 14 young massive star-forming regions. All regions were imaged in the N band, and nine in the Q band, with an angular resolution of similar or equal to 1 ''. Typically, the regions exhibit a single or two compact sources (with sizes in the range 0.008-0.18 pc) plus extended diffuse emission. The Spitzer- Galactic Legacy Infrared Mid-Plane Survey Extraordinaire images of these regions show much more extended emission than that seen by TIMMI2, and this is attributed to polycyclic aromatic hydrocarbon (PAH) bands. For the MIR sources associated with radio continuum radiation (Paper I) there is a close morphological correspondence between the two emissions, suggesting that the ionized gas (radio source) and hot dust (MIR source) coexist inside the H II region. We found five MIR compact sources which are not associated with radio continuum emission, and are thus prime candidates for hosting young massive protostars. In particular, objects IRAS 14593-5852 II (only detected at 17.7 mu m) and 17008-4040 I are likely to be genuine O-type protostellar objects. We also present TIMMI2 N-band spectra of eight sources, all of which are dominated by a prominent silicate absorption feature (similar or equal to 9.7 mu m). From these data we estimate column densities in the range (7-17) x 10(22) cm(-2), in good agreement with those derived from the 1.2 mm data (Paper II). Seven sources show bright [Ne II] line emission, as expected from ionized gas regions. Only IRAS 12383-6128 shows detectable PAH emission at 8.6 and 11.3 mu m. C1 [Morales, Esteban F. E.; Mardones, Diego; Garay, Guido] Univ Chile, Dept Astron, Santiago, Chile. [Brooks, Kate J.] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Pineda, Jaime E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brooks, Kate J.; Pineda, Jaime E.] Univ Chile, Dept Astron, Santiago, Chile. RP Morales, EFE (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM emorales@mpifr-bonn.mpg.de RI Garay, Guido/H-8840-2013; Pineda, Jaime/J-7405-2013; Mardones, Diego/I-5719-2016; OI Garay, Guido/0000-0003-1649-7958; Pineda, Jaime/0000-0002-3972-1978; Brooks, Kate/0000-0001-9373-8992 FU Chilean Centro de Astrofisica FONDAP [15010003]; Proyecto BASAL PFB-06 FX E.F.E.M., D.M., G.G., K.J.B., and J.E.P. gratefully acknowledge support from the Chilean Centro de Astrofisica FONDAP No. 15010003 and Proyecto BASAL PFB-06. NR 54 TC 4 Z9 4 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 JUN 10 PY 2009 VL 698 IS 1 BP 488 EP 501 DI 10.1088/0004-637X/698/1/488 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700038 ER PT J AU Kaltenegger, L Traub, WA AF Kaltenegger, Lisa Traub, Wesley A. TI TRANSITS OF EARTH-LIKE PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; planets and satellites: general; techniques: spectroscopic ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; MOLECULAR SPECTROSCOPIC DATABASE; HARPS SEARCH; SUPER-EARTH; HD 189733B; M-DWARFS; TERRESTRIAL PLANETS; THERMAL EMISSION; NEARBY-STAR AB Transmission spectroscopy of Earth-like exoplanets is a potential tool for habitability screening. Transiting planets are present-day "Rosetta Stones" for understanding extrasolar planets because they offer the possibility to characterize giant planet atmospheres and should provide an access to biomarkers in the atmospheres of Earth-like exoplanets, once they are detected. Using the Earth itself as a proxy we show the potential and limits of the transiting technique to detect biomarkers on an Earth-analog exoplanet in transit. We quantify the Earth's cross section as a function of wavelength, and show the effect of each atmospheric species, aerosol, and Rayleigh scattering. Clouds do not significantly affect this picture because the opacity of the lower atmosphere from aerosol and Rayleigh losses dominates over cloud losses. We calculate the optimum signal-to-noise ratio for spectral features in the primary eclipse spectrum of an Earth-like exoplanet around a Sun-like star and also M stars, for a 6.5 m telescope in space. We find that the signal-to-noise values for all important spectral features are on the order of unity or less per transit-except for the closest stars-making it difficult to detect such features in one single transit, and implying that coadding of many transits will be essential. C1 [Kaltenegger, Lisa; Traub, Wesley A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Traub, Wesley A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kaltenegger, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkaltenegger@cfa.harvard.edu FU NASA [NAG5-13045] FX We are grateful to Neill Reid for providing us with the M-star data and Todd Henry for providing us with a list of the closest M stars. Special thanks to Ken Jucks, Sara Seager, and Phillip Nutzman for stimulating discussion and comments. This work was sponsored by NASA grant NAG5-13045 at the Harvard Smithsonian Center for Astrophysics and the Origins of Life Initiative at Harvard. Part of 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. NR 47 TC 116 Z9 116 U1 2 U2 24 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 JUN 10 PY 2009 VL 698 IS 1 BP 519 EP 527 DI 10.1088/0004-637X/698/1/519 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700042 ER PT J AU McNamara, BR Kazemzadeh, F Rafferty, DA Birzan, L Nulsen, PEJ Kirkpatrick, CC Wise, MW AF McNamara, B. R. Kazemzadeh, F. Rafferty, D. A. Birzan, L. Nulsen, P. E. J. Kirkpatrick, C. C. Wise, M. W. TI AN ENERGETIC AGN OUTBURST POWERED BY A RAPIDLY SPINNING SUPERMASSIVE BLACK HOLE OR AN ACCRETING ULTRAMASSIVE BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: clusters: individual (MS0735.6+7421); X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; X-RAY CAVITIES; COOLING FLOW CLUSTERS; EXTRAGALACTIC RADIO-SOURCES; LUMINOUS ELLIPTIC GALAXIES; JET POWER; STAR-FORMATION; ELECTROMAGNETIC EXTRACTION AB Powering the 10(62) erg nuclear outburst in the MS0735.6+7421 cluster central galaxy by accretion with a 10% mass-to-energy conversion efficiency implies that its putative supermassive black hole (SMBH) grew by similar to 6 x 10(8) M-circle dot over the past 100 Myr. Guided by data at several wavelengths, we place upper limits on the amount of cold gas and star formation near the nucleus of < 10(9) M-circle dot and < 2 M-circle dot yr(-1), respectively. These limits imply that an implausibly large fraction of the preexisting cold gas in the inner several kpc must have been consumed by its SMBH at the rate of similar to 3-5 M-circle dot yr(-1) during the past 100 Myr while leaving no trace of star formation. Such a high accretion rate would be difficult to maintain by stellar accretion or the Bondi mechanism, unless the black hole mass approaches 10(11) M circle dot. Furthermore, its feeble nuclear luminosities in the UV, I, and X-ray bands compared to its enormous mechanical power are inconsistent with rapid accretion onto a similar to 5 x 10(9) M-circle dot black hole. We suggest instead that the active galactic nucleus (AGN) outburst is powered by angular momentum released from a rapidly spinning black hole. The rotational energy and power available from a spinning black hole are consistent with the cavity and shock energetics inferred from X-ray observations. A maximally spinning 10(9) M-circle dot black hole contains enough rotational energy, similar to 10(62) erg, to quench a cooling flow over its lifetime and to contribute significantly to the excess entropy found in the hot atmospheres of groups and clusters. Two modes of AGN feedback may be quenching star formation in elliptical galaxies centered in cooling halos at late times. An accretion mode that operates in gas-rich systems, and a spin mode operating at modest accretion rates. The spin conjecture may be avoided in MS0735 by appealing to Bondi accretion onto a central black hole whose mass greatly exceeds 10(10) M-circle dot. The host galaxy's unusually large 3.8 kpc stellar core radius (light deficit) may witness the presence of an ultramassive black hole. C1 [McNamara, B. R.; Kazemzadeh, F.; Kirkpatrick, C. C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rafferty, D. A.; Birzan, L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wise, M. W.] Univ Amsterdam, Astron & Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP McNamara, BR (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. EM mcnamara@uwaterloo.ca OI Nulsen, Paul/0000-0003-0297-4493 FU NASA; Natural Sciences and Engineering Research Council of Canada FX We thank Tod Lauer and the referee Mateusz Ruszkowski for comments that improved the paper, and we acknowledge insightful discussions with Dan Evans, Bob O'Connell, Megan Donahue, Genevieve de Messi` eres, and Hui Li. We thank Eugene Churazov and Bill Forman for permission to reproduce their diagram shown in Figure 10, and Mina Rohanizadegan for assistance with the analysis. This work was supported by generous grants from NASA and the Natural Sciences and Engineering Research Council of Canada. NR 127 TC 45 Z9 46 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 JUN 10 PY 2009 VL 698 IS 1 BP 594 EP 605 DI 10.1088/0004-637X/698/1/594 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700049 ER PT J AU Reale, F Testa, P Klimchuk, JA Parenti, S AF Reale, Fabio Testa, Paola Klimchuk, James A. Parenti, Susanna TI EVIDENCE OF WIDESPREAD HOT PLASMA IN A NONFLARING CORONAL ACTIVE REGION FROM HINODE/X-RAY TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: X-rays, gamma rays ID X-RAY; SOLAR CORONA; LOOPS; EMISSION; DIAGNOSTICS; MISSION AB Nanoflares, short and intense heat pulses within spatially unresolved magnetic strands, are now considered a leading candidate to solve the coronal heating problem. However, the frequent occurrence of nanoflares requires that flare-hot plasma be present in the corona at all times. Its detection has proved elusive until now, in part because the intensities are predicted to be very faint. Here, we report on the analysis of an active region observed with five filters by Hinode/X-Ray Telescope (XRT) in 2006 November. We have used the filter ratio method to derive maps of temperature and emission measure (EM) both in soft and hard ratios. These maps are approximate in that the plasma is assumed to be isothermal along each line of sight. Nonetheless, the hardest available ratio reveals the clear presence of plasma around 10 MK. To obtain more detailed information about the plasma properties, we have performed Monte Carlo simulations assuming a variety of nonisothermal EM distributions along the lines of sight. We find that the observed filter ratios imply bi-modal distributions consisting of a strong cool (log T similar to 6.3-6.5) component and a weaker (few percent) and hotter (6.6 < logT < 7.2) component. The data are consistent with bi-modal distributions along all lines of sight, i.e., throughout the active region. We also find that the isothermal temperature inferred from a filter ratio depends sensitively on the precise temperature of the cool component. A slight shift of this component can cause the hot component to be obscured in a hard ratio measurement. Consequently, temperature maps made in hard and soft ratios tend to be anti-correlated. We conclude that this observation supports the presence of widespread nanoflaring activity in the active region. C1 [Reale, Fabio] Univ Palermo, Dipartimento Sci Fis & Astron, Sez Astron, I-90134 Palermo, Italy. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klimchuk, James A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Parenti, Susanna] Observ Royal Belgique, B-1180 Brussels, Belgium. RP Reale, F (reprint author), INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy. RI Klimchuk, James/D-1041-2012; OI Klimchuk, James/0000-0003-2255-0305; Reale, Fabio/0000-0002-1820-4824 NR 23 TC 58 Z9 58 U1 2 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 JUN 10 PY 2009 VL 698 IS 1 BP 756 EP 765 DI 10.1088/0004-637X/698/1/756 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700063 ER PT J AU Czerny, B Siemiginowska, A Janiuk, A Nikiel-Wroczynski, B Stawarz, L AF Czerny, Bozena Siemiginowska, Aneta Janiuk, Agnieszka Nikiel-Wroczynski, Blazej Stawarz, Lukasz TI ACCRETION DISK MODEL OF SHORT-TIMESCALE INTERMITTENT ACTIVITY IN YOUNG RADIO SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Review DE accretion, accretion disks; galaxies: active; instabilities ID COMPACT-STEEP-SPECTRUM; DOUBLE-DOUBLE MORPHOLOGY; RADIATION PRESSURE INSTABILITY; MICROQUASAR GRS 1915+105; BLACK-HOLE MASSES; X-RAY-PROPERTIES; GALACTIC NUCLEI; SYMMETRIC OBJECTS; JET ACTIVITY; ENERGY-DISTRIBUTIONS AB We associate the existence of short-lived compact radio sources with the intermittent activity of the central engine caused by a radiation pressure instability within an accretion disk. Such objects may constitute a numerous subclass of gigahertz-peaked spectrum sources, in accordance with the population studies of radio-loud active galaxies, as well as detailed investigations of their radio morphologies. We perform the model computations assuming the viscosity parameterization as proportional to a geometrical mean of the total and gas pressure. The implied timescales are consistent with the observed ages of the sources. The duration of an active phase for a moderate accretion rate is short enough (less than 10(3)-10(4) yr) that the ejecta are confined within the host galaxy and thus these sources cannot evolve into large size radio galaxies unless they are close to the Eddington limit. C1 [Czerny, Bozena; Janiuk, Agnieszka; Nikiel-Wroczynski, Blazej] Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nikiel-Wroczynski, Blazej; Stawarz, Lukasz] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Stawarz, Lukasz] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Czerny, B (reprint author), Nicholas Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland. EM bcz@camk.edu.pl RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 118 TC 58 Z9 58 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 JUN 10 PY 2009 VL 698 IS 1 BP 840 EP 851 DI 10.1088/0004-637X/698/1/840 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700071 ER PT J AU Kelly, BC Bechtold, J Siemiginowska, A AF Kelly, Brandon C. Bechtold, Jill Siemiginowska, Aneta TI ARE THE VARIATIONS IN QUASAR OPTICAL FLUX DRIVEN BY THERMAL FLUCTUATIONS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; methods: data analysis; quasars: general ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; RADIO-QUIET QUASARS; X-RAY VARIABILITY; RADIATION PRESSURE INSTABILITY; MICROQUASAR GRS 1915+105; HOLE ACCRETION DISCS; BLACK-HOLES; OBSERVATIONAL CONSTRAINTS; CONTINUUM VARIABILITY AB We analyze a sample of optical light curves for 100 quasars, 70 of which have black hole mass estimates. Our sample is the largest and broadest used yet for modeling quasar variability. The sources in our sample have z < 2.8, 10(42) less than or similar to lambda L-lambda (5100 angstrom) less than or similar to 10(46), and 10(6) less than or similar to M-BH/M-circle dot less than or similar to 10(10). We model the light curves as a continuous time stochastic process, providing a natural means of estimating the characteristic timescale and amplitude of quasar variations. We employ a Bayesian approach to estimate the characteristic timescale and amplitude of flux variations; our approach is not affected by biases introduced from discrete sampling effects. We find that the characteristic timescales strongly correlate with black hole mass and luminosity, and are consistent with disk orbital or thermal timescales. In addition, the amplitude of short-timescale variations is significantly anticorrelated with black hole mass and luminosity. We interpret the optical flux fluctuations as resulting from thermal fluctuations that are driven by an underlying stochastic process, such as a turbulent magnetic field. In addition, the intranight variations in optical flux implied by our empirical model are less than or similar to 0.02 mag, consistent with current microvariability observations of radio-quiet quasars. Our stochastic model is therefore able to unify both long-and short-timescale optical variations in radio-quiet quasars as resulting from the same underlying process, while radio-loud quasars have an additional variability component that operates on timescales less than or similar to 1 day. C1 [Kelly, Brandon C.; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kelly, Brandon C.; Bechtold, Jill] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bckelly@cfa.harvard.edu NR 86 TC 185 Z9 185 U1 2 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 JUN 10 PY 2009 VL 698 IS 1 BP 895 EP 910 DI 10.1088/0004-637X/698/1/895 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 450AP UT WOS:000266373700075 ER PT J AU Clark, CJ Dudley, R AF Clark, Christopher James Dudley, Robert TI Flight costs of long, sexually selected tails in hummingbirds SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Anna's hummingbird; flight cost; flight speed; metabolism; sexual selection; tail ID HOVERING HUMMINGBIRDS; OXYGEN-CONSUMPTION; BIRDS TAILS; PERFORMANCE; LENGTH; ENERGETICS; EVOLUTION; ORNAMENT; STREAMER; SWALLOW AB The elongated tails adorning many male birds have traditionally been thought to degrade flight performance by increasing body drag. However, aerodynamic interactions between the body and tail can be substantial in some contexts, and a short tail may actually reduce rather than increase overall drag. To test how tail length affects flight performance, we manipulated the tails of Anna's hummingbirds (Calypte anna) by increasing their length with the greatly elongated tail streamers of the red-billed streamertail (Trochilus polytmus) and reducing their length by removing first the rectrices and then the entire tail (i.e. all rectrices and tail covert feathers). Flight performance was measured in a wind tunnel by measuring (i) the maximum forward speed at which the birds could fly and (ii) the metabolic cost of flight while flying at airspeeds from 0 to 14 m s(-1). We found a significant interaction effect between tail treatment and airspeed: an elongated tail increased the metabolic cost of flight by up to 11 per cent, and this effect was strongest at higher flight speeds. Maximum flight speed was concomitantly reduced by 3.4 per cent. Also, removing the entire tail decreased maximum flight speed by 2 per cent, suggesting beneficial aerodynamic effects for tails of normal length. The effects of elongation are thus subtle and airspeed-specific, suggesting that diversity in avian tail morphology is associated with only modest flight costs. C1 [Clark, Christopher James; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Clark, CJ (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM cclark@berkeley.edu NR 44 TC 36 Z9 36 U1 5 U2 30 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD JUN 7 PY 2009 VL 276 IS 1664 BP 2109 EP 2115 DI 10.1098/rspb.2009.0090 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 436XZ UT WOS:000265450700025 PM 19324747 ER PT J AU Combes, SA Dudley, R AF Combes, Stacey A. Dudley, Robert TI Turbulence-driven instabilities limit insect flight performance SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE forward flight; rolling; orchid bees; stability; maximum speed ID PERCH DIAMETER; FLOW; AEROECOLOGY; AEROSPHERE; CAPACITY; LIZARDS; SPEED; FISH; BEES AB Environmental turbulence is ubiquitous in natural habitats, but its effect on flying animals remains unknown because most flight studies are performed in still air or artificially smooth flow. Here we show that variability in external airflow limits maximum flight speed in wild orchid bees by causing severe instabilities. Bees flying in front of an outdoor, turbulent air jet become increasingly unstable about their roll axis as airspeed and flow variability increase. Bees extend their hindlegs ventrally at higher speeds, improving roll stability but also increasing body drag and associated power requirements by 30%. Despite the energetic cost, we observed this stability-enhancing behavior in 10 euglossine species from 3 different genera, spanning an order of magnitude in body size. A field experiment in which we altered the level of turbulence demonstrates that flight instability and maximum flight speed are directly related to flow variability. The effect of environmental turbulence on flight stability is thus an important and previously unrecognized determinant of flight performance. C1 [Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [Combes, Stacey A.] Harvard Univ, Concord Field Stn, Dept Organism & Evolut Biol, Bedford, MA 01730 USA. RP Combes, SA (reprint author), 100 Old Causeway Rd, Bedford, MA 01730 USA. EM scombes@oeb.harvard.edu FU Miller Institute for Basic Research in Science FX We thank A. Biewener, E. Goldman, J. Crall, and D. Young for comments on the manuscript; A. Richardson for assistance with statistical analysis; and T. Hedrick for access to digitizing software. The Smithsonian Tropical Research Institute provided permits and logistical support. This work was supported in part by a fellowship from the Miller Institute for Basic Research in Science (to S. C.). NR 26 TC 40 Z9 40 U1 4 U2 25 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 JUN 2 PY 2009 VL 106 IS 22 BP 9105 EP 9108 DI 10.1073/pnas.0902186106 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 452ZU UT WOS:000266580500059 PM 19458254 ER PT J AU Freeman, EW Whyte, I Brown, JL AF Freeman, Elizabeth W. Whyte, Ian Brown, Janine L. TI Reproductive evaluation of elephants culled in Kruger National Park, South Africa between 1975 and 1995 SO AFRICAN JOURNAL OF ECOLOGY LA English DT Article ID LOXODONTA-AFRICANA; LIFE-HISTORIES; POPULATION; EVOLUTION; ULTRASONOGRAPHY; ENDOCRINOLOGY; PROGESTERONE; CONCEPTION; DEMOGRAPHY; DYNAMICS AB To reduce elephant densities and preserve biological diversity, 14,629 elephants were culled from Kruger National Park, South Africa (1967-1999). Data were catalogued between 1975 and 1996 on 2737 male and female elephants, including pregnancy and lactational status for 1620 females (>= 5 years of age) and, uterine and/or ovarian characteristics for 1279. This study used these data to investigate the effects of age and precipitation on reproduction. The youngest age of conception was 8 years (n = 6) and by 12 years of age all females were sexually mature. From the age of 14 years, the percentage of reproductively active females (pregnant and/or lactating) was > 90%; however, this percentage declined when females reached 50 years of age. Overall, one-tenth of females were nonreproductive (not pregnant or lactating) at any given time, mostly in the youngest (< 15 years) and oldest (> 50 years) age classes. Eighteen (3.3%) of the nonpregnant females had reproductive tract pathologies, including endometrial, uterine or ovarian cysts. There was a seasonal distribution of mating activity that correlated with the rainy season. As has been demonstrated in other populations of free-ranging African elephants, most of the females in Kruger National Park were reproductively active; however, age and climate affected reproductive activity. C1 [Freeman, Elizabeth W.; Brown, Janine L.] Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. [Whyte, Ian] Kruger Natl Pk, ZA-1350 Skukuza, South Africa. RP Freeman, EW (reprint author), Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, Front Royal, VA 22630 USA. EM freemane@si.edu FU International Elephant Foundation; Friends of the National Zoo; Smithsonian's Undersecretary of Science Walcott Endowment Fund FX The authors wish to acknowledge Mrs Collen Wood and Mr Obert Mathebula for aiding in the collection and cataloguing of field data and Mr Nick Zambatis for tallying the precipitation data. Funding for this analysis was generously provided by the International Elephant Foundation, the Friends of the National Zoo, and the Smithsonian's Undersecretary of Science Walcott Endowment Fund. NR 47 TC 10 Z9 10 U1 4 U2 28 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0141-6707 J9 AFR J ECOL JI Afr. J. Ecol. PD JUN PY 2009 VL 47 IS 2 BP 192 EP 201 DI 10.1111/j.1365-2028.2008.00957.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 453FK UT WOS:000266595500009 ER PT J AU Kidwell, PA AF Kidwell, Peggy Aldrich TI Maria Mitchell and the Sexing of Science: An Astronomer among the American Romantics SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [Kidwell, Peggy Aldrich] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD JUN PY 2009 VL 114 IS 3 BP 757 EP 758 PG 2 WC History SC History GA 459UV UT WOS:000267137000071 ER PT J AU Biani, NB Mueller, UG Wcislo, WT AF Biani, Natalia B. Mueller, Ulrich G. Wcislo, William T. TI Cleaner Mites: Sanitary Mutualism in the Miniature Ecosystem of Neotropical Bee Nests SO AMERICAN NATURALIST LA English DT Article DE acari; bee; cleaning mutualism; Megalopta genalis; Megalopta ecuadoria; symbiosis ID ECUADORIA HYMENOPTERA; MEGALOPTA-GENALIS; LIFE-HISTORY; SWEAT BEES; EVOLUTION; WASP; ASSOCIATIONS; HALICTIDAE; ACARI; ANTS AB Cleaning symbioses represent classic models of mutualism, and some bee mites are thought to perform cleaning services for their hosts in exchange for suitable environments for reproduction and dispersal. These mutual benefits, however, have not been rigorously demonstrated. We tested the sanitary role of bee mites by correlating mite loads with fungal contamination in natural nests of Megalopta genalis and Megalopta ecuadoria and by experimentally manipulating mite loads in artificial cells with developing brood. Field observations revealed significant correlations between the presence of mites and the absence of fungi inside the brood cells, as well as between the absence of mites and increased bee mortality. Likewise, experimental brood cells with mites have fewer fungal colonies than do cells without mites. Field observations and experimental manipulations, therefore, provide clear evidence of the sanitary effect of mites in nests of Megalopta bees. This bee-mite association constitutes one of the few examples of terrestrial cleaning mutualisms. C1 [Biani, Natalia B.; Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Wcislo, William T.] Smithsonian Trop Res Inst, Balboa 03092, Panama. RP Biani, NB (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. EM megaloptabee@gmail.com FU Smithsonian Tropical Research Institute (STRI); Program of Ecology, Evolution, and Behavior of the University of Texas at Austin; STRI; STRI's Office of Education FX This work was supported by the Smithsonian Tropical Research Institute (STRI) short-term fellowships as well as research grants from the Program of Ecology, Evolution, and Behavior of the University of Texas at Austin to N.B.B. Additional support came from general research funds from STRI to W. T. W.; support for an intern came from STRI's Office of Education. We are extremely grateful to J. C. Santos for his statistical advice and help with figures; A. Rodrigues for his suggestions on microbiology methods; T. Gonzales, A. Smith, and S. Tierney for their invaluable help and company during nest collections; H. Fernandez-Marin for logistic help in the lab; H. Klompen and J. Shik for their help in the identification of the mite species; and R. Adams, H. Ishak, B. Klein, A. Mikheyev, and C. Rabeling for their comments on earlier versions of the manuscript. G. Otis and an anonymous reviewer offered very helpful The Autoridad Nacional del Ambiente de la Republica de Panama provided collecting and export permits. And, of course, we thank the bees and the mites. NR 54 TC 9 Z9 9 U1 1 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD JUN PY 2009 VL 173 IS 6 BP 841 EP 847 DI 10.1086/598497 PG 7 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 439KJ UT WOS:000265625700014 PM 19371167 ER PT J AU Burgasser, AJ Blake, CH AF Burgasser, Adam J. Blake, Cullen H. TI AN AGE CONSTRAINT FOR THE VERY LOW MASS STELLAR/BROWN DWARF BINARY 2MASS J03202839-0446358AB SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: fundamental parameters; stars: individual (2MASS J03202839-0446358); stars: low mass, brown dwarfs ID EXTRASOLAR GIANT PLANETS; DIGITAL SKY SURVEY; BROWN DWARF; T-DWARFS; ULTRACOOL DWARFS; LITHIUM DEPLETION; STAR-FORMATION; MAIN-SEQUENCE; GLIESE 569B; COOL STARS AB 2MASS J03202839-0446358AB is a recently identified, late-type M dwarf/T dwarf spectroscopic binary system for which both the radial velocity orbit for the primary and spectral types for both components have been determined. By combining these measurements with predictions from four different sets of evolutionary models, we determine a minimum age of 2.0 +/- 0.3 Gyr for this system, corresponding to minimum primary and secondary masses of 0.080 M(circle dot) and 0.053 M(circle dot), respectively. We find broad agreement in the inferred age and mass constraints between the evolutionary models, including those that incorporate atmospheric condensate grain opacity; however, we are not able to independently assess their accuracy. The inferred minimum age agrees with the kinematics and absence of magnetic activity in this system, but not the rapid rotation of its primary, further evidence of a breakdown in angular momentum evolution trends amongst the lowest luminosity stars. Assuming a maximum age of 10 Gyr, we constrain the orbital inclination of this system to i greater than or similar to 53 degrees. More precise constraints on the orbital inclination and/or component masses of 2MASS 0320-0446AB, through either measurement of the secondary radial velocity orbit (optimally in the 1.2-1.3 mu m band) or detection of an eclipse (only 0.3% probability based on geometric constraints), would yield a bounded age estimate for this system, and the opportunity to use it as an empirical test for brown dwarf evolutionary models at late ages. C1 [Burgasser, Adam J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Blake, Cullen H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burgasser, AJ (reprint author), MIT, Kavli Inst Astrophys & Space Res, Bldg 37,Room 664B,77 Massachusetts Ave, Cambridge, MA 02139 USA. EM ajb@mit.edu FU Harvard Origins of Life Initiative FX The authors thank I. Baraffe, A. Burrows, M. Marley, and D. Saumon for making electronic versions of their evolutionary models available; and M. Liu for identifying the roundoff errors in the Mbol/spectral type relation in Burgasser (2007a). We also thank our referee, K. Luhman, for his helpful critique of the original manuscript. C. B. acknowledges support from the Harvard Origins of Life Initiative. This publication has made use of the VLM Binaries Archive maintained by Nick Siegler at Web site http://www.vlmbinaries.org. NR 71 TC 8 Z9 8 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4621 EP 4626 DI 10.1088/0004-6256/137/6/4621 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300008 ER PT J AU Tsai, CW Turner, JL Beck, SC Meier, DS Ho, PTP AF Tsai, Chao-Wei Turner, Jean L. Beck, Sara C. Meier, David S. Ho, Paul T. P. TI LOCATING THE YOUNGEST H II REGIONS IN M82 WITH 7 mm CONTINUUM MAPS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (M 82, NGC 3034); galaxies: ISM; galaxies: starburst; galaxies: star clusters; H II regions; radio continuum: galaxies ID COMPACT RADIO-SOURCES; STARBURST GALAXY M82; SUPER-STAR-CLUSTERS; LINE INTERFEROMETRY OBSERVATIONS; EXPANDING MOLECULAR SUPERBUBBLE; ACTIVE GALACTIC NUCLEUS; HUBBLE-SPACE-TELESCOPE; X-RAY SOURCE; HIGH-RESOLUTION; BLACK-HOLES AB We present 7 mm Very Large Array continuum images of the starburst galaxy M82. On arcsecond scales, two-thirds of the 7 mm continuum consists of free-free emission from H II regions. In the subarcsecond resolution map, we identify 14 compact sources, including 9 bright H II regions with N(lyc) > 10(51) s(-1). Four of the H II regions have rising spectra, implying emission measures > 10(8) cm(-6) pc. Except for one compact source with peculiar features, all other compact radio sources are found in dust lanes and do not have optical or near-infrared continuum counterparts. Four regions of extended, high brightness (EM > 10(7) cm(-6) pc) radio emission are found in our high-resolution map, including some as large as similar to 2 '', or 30 pc, representing either associations of small H II regions, or sheet-like structures of denser gas. The good correlation between 7 mm emission and Spitzer IRAC 8 mu m continuum-removed polycyclic aromatic hydrocarbon (PAH) feature suggests that PAH emission may track the recently formed OB stars. We find an excellent correlation between molecular gas and star formation, particularly dense gas traced by HCN, down to the similar to 45 pc scale in M82. We also find star formation efficiencies (SFEs) of 1%-10% on the same scale, based on CO maps. The highest SFE are found in regions with the highest dense gas fractions. C1 [Tsai, Chao-Wei; Turner, Jean L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beck, Sara C.] Tel Aviv Univ, Dept Phys & Astron, Ramat Aviv, Israel. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Tsai, CW (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM cwtsai@astro.ucla.edu; turner@astro.ucla.edu; sara@wise1.tau.ac.il; dmeier@nmt.edu; ho@cfa.harvard.edu FU NASA [NAS5-26555] FX The authors gratefully acknowledge the anonymous referee for the valuable comments. We also thank Almudena Alonso-Herrero, Sarah Lipscy, and Peter Schilke for their generosity in providing their data. C. W. T. appreciates helpful discussions with Yu Gao. Some of the data used 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. This research has also made use of the NASA/IPAC Extragalactic Database (NED) and the NASA/IPAC Infrared Science Archive (IRSA) which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 94 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4655 EP 4669 DI 10.1088/0004-6256/137/6/4655 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300012 ER PT J AU Winston, E Megeath, ST Wolk, SJ Hernandez, J Gutermuth, R Muzerolle, J Hora, JL Covey, K Allen, LE Spitzbart, B Peterson, D Myers, P Fazio, GG AF Winston, E. Megeath, S. T. Wolk, S. J. Hernandez, J. Gutermuth, R. Muzerolle, J. Hora, J. L. Covey, K. Allen, L. E. Spitzbart, B. Peterson, D. Myers, P. Fazio, G. G. TI A SPECTROSCOPIC STUDY OF YOUNG STELLAR OBJECTS IN THE SERPENS CLOUD CORE AND NGC 1333 SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: pre-main sequence; X-rays: stars ID LOW-MASS STARS; T-TAURI STARS; INFRARED CLASSIFICATION SPECTROSCOPY; FUNDAMENTAL MK STANDARDS; MAIN-SEQUENCE EVOLUTION; SPITZER-SPACE-TELESCOPE; IR IMAGING PHOTOMETRY; ORION NEBULA CLUSTER; FORMING REGIONS; MOLECULAR CLOUD AB We present spectral observations of 130 young stellar objects (YSOs) in the Serpens Cloud Core and NGC 1333 embedded clusters. The observations consist of near-IR spectra in the H and K bands from SpeX on the IRTF and far-red spectra (6000-9000 angstrom) from Hectospec on the Multi-Mirror Telescope. These YSOs were identified in previous Spitzer and Chandra observations, and the evolutionary classes of the YSOs were determined from the Spitzer mid-IR photometry. With these spectra we search for corroborating evidence for the pre-main-sequence nature of the objects, study the properties of the detected emission lines as a function of evolutionary class, and obtain spectral types for the observed YSOs. The temperatures implied by the spectral types are combined with luminosities determined from the near-IR photometry to construct Hertzsprung-Russell (H-R) diagrams for the clusters. By comparing the positions of the YSOs in the H-R diagrams with the pre-main-sequence tracks of Baraffe (1998), we determine the ages of the embedded sources and study the relative ages of the YSOs with and without optically thick circumstellar disks. The apparent isochronal ages of the YSOs in both clusters range from less than 1 Myr to 10 Myr, with most objects below 3 Myr. The observed distributions of ages for the Class II and Class III objects are statistically indistinguishable. We examine the spatial distribution and extinction of the YSOs as a function of their isochronal ages. We find the sources < 3 Myr to be concentrated in the molecular cloud gas, while the older sources are spatially dispersed and are not deeply embedded. Nonetheless, the sources with isochronal ages > 3 Myr show all the characteristics of YSOs in their spectra, their IR spectral energy distributions, and their X-ray emission; we find no evidence that they are contaminating background giants or foreground dwarfs. However, we find no corresponding decrease in the fraction of sources with infrared excess with isochronal age; this suggests that the older isochronal ages may not measure the true age of the > 3 Myr YSOs. Thus, the nature of the apparently older sources and their implications for cluster formation remain unresolved. C1 [Winston, E.; Megeath, S. T.; Wolk, S. J.; Gutermuth, R.; Hora, J. L.; Covey, K.; Allen, L. E.; Spitzbart, B.; Peterson, D.; Myers, P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winston, E.] Univ Coll Dublin, Sch Phys, Sci Ctr N, Dublin 4, Ireland. [Hernandez, J.] Ctr Invest Astron, Merida 5101 A, Venezuela. [Hernandez, J.] Univ Michigan, Ann Arbor, MI 48109 USA. [Muzerolle, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Winston, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ewinston@cfa.harvard.edu OI Hora, Joseph/0000-0002-5599-4650; Covey, Kevin/0000-0001-6914-7797 FU NASA [1407, 1256790, 960541, NAS8-03060]; National Science Foundation; Irish Research Council for Science, Engineering, and Technology (IRCSET) FX This work is based on observations taken with the Hectospec instrument on the MMT, a joint venture of the Smithsonian Institute and the University of Arizona. This work is based on observations made with the Spitzer Space Telescope (PID 6, PID 174), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through contract 1256790 issued by JPL/Caltech. Support for the IRAC instrument was provided by NASA through contract 960541 issued by the Jet Propulsion Laboratory (JPL). 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 the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the JPL, California Institute of Technology, under contract with the National Aeronautics and Space Administration. S.J.W. was supported by NASA contract NAS8-03060. This represents the results of VLA program S60872. E. W. thanks the Irish Research Council for Science, Engineering, and Technology (IRCSET) for funding and support. NR 78 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4777 EP 4794 DI 10.1088/0004-6256/137/6/4777 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300022 ER PT J AU Srinivasan, S Meixner, M Leitherer, C Vijh, U Volk, K Blum, RD Babler, BL Block, M Bracker, S Cohen, M Engelbracht, CW For, BQ Gordon, KD Harris, J Hora, JL Indebetouw, R Markwick-Kemper, F Meade, M Misselt, KA Sewilo, M Whitney, B AF Srinivasan, Sundar Meixner, Margaret Leitherer, Claus Vijh, Uma Volk, Kevin Blum, Robert D. Babler, Brian L. Block, Miwa Bracker, Steve Cohen, Martin Engelbracht, Charles W. For, Bi-Qing Gordon, Karl D. Harris, Jason Hora, Joseph L. Indebetouw, Remy Markwick-Kemper, Francisca Meade, Marilyn Misselt, Karl A. Sewilo, Marta Whitney, Barbara TI THE MASS LOSS RETURN FROM EVOLVED STARS TO THE LARGE MAGELLANIC CLOUD: EMPIRICAL RELATIONS FOR EXCESS EMISSION AT 8 AND 24 mu m SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; Magellanic Clouds; stars: AGB and post-AGB; stars: carbon; stars: mass loss ID ASYMPTOTIC GIANT BRANCH; SPITZER-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; LOCAL GROUP DWARFS; AGB STARS; CARBON STARS; LOSS RATES; SAGE SURVEY; CIRCUMSTELLAR ENVELOPES; INFRARED PHOTOMETRY AB We present empirical relations describing excess emission from evolved stars in the Large Magellanic Cloud (LMC) using data from the Spitzer Space Telescope Surveying the Agents of a Galaxy's Evolution (SAGE) survey which includes the Infrared Array Camera (IRAC) 3.6, 4.5, 5.8, and 8.0 mu m and Multiband Imaging Photometer (MIPS) 24, 70, and 160 mu m bands. We combine the SAGE data with the Two Micron All Sky Survey (2MASS; J, H, and K(s)) and the optical Magellanic Cloud Photometric Survey (MCPS; U, B, V, and I) point source catalogs in order to create complete spectral energy distributions (SEDs) of the asymptotic giant branch (AGB) star candidates in the LMC. AGB star outflows are among the main producers of dust in a galaxy, and this mass loss results in an excess in the fluxes observed in the 8 and 24 mu m bands. The aim of this work is to investigate the mass loss return by AGB stars to the interstellar medium of the LMC by studying the dependence of the infrared excess flux on the total luminosity. We identify oxygen-rich, carbon-rich, and extreme AGB star populations in our sample based on their 2MASS and IRAC colors. The SEDs of oxygen-and carbon-rich AGB stars are compared with appropriate stellar photosphere models to obtain the excess flux in all the IRAC bands and the MIPS 24 mu m band. Extreme AGB stars are dominated by circumstellar emission at 8 and 24 mu m; thus we approximate their excesses with the flux observed in these bands. We find about 16,000 O-rich, 6300 C-rich, and 1000 extreme sources with reliable 8 mu m excesses, and about 4500 O-rich, 5300 C-rich, and 960 extreme sources with reliable 24 mu m excesses. The excesses are in the range 0.1 mJy to 5 Jy. The 8 and 24 mu m excesses for all three types of AGB candidates show a general increasing trend with luminosity. The color temperature of the circumstellar dust derived from the ratio of the 8 and 24 mu m excesses decreases with an increase in excess, while the 24 mu m optical depth increases with excess. The extreme AGB candidates are the major contributors to the mass loss, and we estimate the total AGB mass loss return to the LMC to be (5.9-13) x 10(-3) M(circle dot) yr(-1). C1 [Srinivasan, Sundar] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Meixner, Margaret; Leitherer, Claus; Vijh, Uma; Gordon, Karl D.; Sewilo, Marta] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Volk, Kevin] Gemini Observ, Hilo, HI 96720 USA. [Blum, Robert D.; Harris, Jason] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Babler, Brian L.; Bracker, Steve; Meade, Marilyn] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Block, Miwa; Engelbracht, Charles W.; For, Bi-Qing; Misselt, Karl A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Cohen, Martin] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Markwick-Kemper, Francisca] Univ Manchester, Jodrell Bank, Sch Phys & Astron, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Whitney, Barbara] Space Sci Inst, Boulder, CO 80301 USA. RP Srinivasan, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM sundar@pha.jhu.edu RI Kemper, Francisca/D-8688-2011 OI Kemper, Francisca/0000-0003-2743-8240 FU NASA/Spitzer [1275598, NAG5-12595] FX The authors wish to thank Rita Gautschy-Loidl and Peter Hauschildt for providing us with their photospheric models. We would also like to thank the anonymous referee for their helpful comments. The SAGE Project is supported by NASA/Spitzer grant 1275598 and NASA NAG5-12595. NR 70 TC 71 Z9 71 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4810 EP 4823 DI 10.1088/0004-6256/137/6/4810 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300024 ER PT J AU Hogerheijde, MR Qi, CH de Pater, I Blake, GA Friedel, DN Forster, JR Palmer, P Remijan, AJ Snyder, LE Wright, MCH AF Hogerheijde, Michiel R. Qi, Chunhua de Pater, Imke Blake, Geoffrey A. Friedel, D. N. Forster, J. R. Palmer, Patrick Remijan, Anthony J. Snyder, L. E. Wright, M. C. H. TI SIMULTANEOUS OBSERVATIONS OF COMET C/2002 T7 (LINEAR) WITH THE BERKELEY-ILLINOIS-MARYLAND ASSOCIATION AND OWENS VALLEY RADIO OBSERVATORY INTERFEROMETERS: HCN AND CH3OH SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: individual (LINEAR C/2002 T7); molecular processes; radio lines: solar system; techniques: interferometric ID BOPP 1995 O1; HALE-BOPP; RADIATIVE-TRANSFER; PARENT MOLECULES; C/1995 O1; EXCITATION; SUBMILLIMETER; EMISSION; METHANOL; ARRAY AB We present observations of HCN J = 1-0 and CH3OH J (K-a, K-c) = 3(1, 3)-4(0, 4) A(+) emission from comet C/2002 T7 (LINEAR) obtained simultaneously with the Owens Valley Radio Observatory (OVRO) and Berkeley-Illinois-Maryland Association (BIMA) millimeter interferometers. We combined the data from both arrays to increase the (u, v) sampling and signal to noise of the detected line emission. We also report the detection of CH3OH J (Ka, Kc) = 8(0, 8)-7(1, 7) A(+) with OVRO data alone. Using a molecular excitation code that includes the effects of collisions with water and electrons, as well as pumping by the Solar infrared photons (for HCN alone), we find a production rate of HCN of 2.9 x 10(26) s(-1) and for CH3OH of 2.2 x 10(27) s(-1). Compared to the adopted water production rate of 3 x 10(29) s(-1), this corresponds to an HCN/H2O ratio of 0.1% and a CH3OH/H2O ratio of 0.7%. We critically assess the uncertainty of these values due to the noise (similar to 10%), the uncertainties in the adopted comet model (similar to 50%), and the uncertainties in the adopted collisional excitation rates (up to a factor of 2). Pumping by Solar infrared photons is found to be a minor effect for HCN, because our 15 '' synthesized beam is dominated by the region in the coma where collisions dominate. Since the uncertainties in the derived production rates are at least as large as one-third of the differences found between comets, we conclude that reliable collision rates and an accurate comet model are essential. Because the collisionally dominated region critically depends on the water production rate, using the same approximate method for different comets may introduce biases in the derived production rates. Multiline observations that directly constrain the molecular excitation provide much more reliable production rates. C1 [Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [de Pater, Imke; Wright, M. C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Palmer, Patrick] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22901 USA. [Friedel, D. N.; Snyder, L. E.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Blake, Geoffrey A.] CALTECH, Div Geophys & Planetary Sci, Pasadena, CA 91125 USA. [Forster, J. R.] Hat Creek Radio Observ, Hat Creek, CA 96040 USA. RP Hogerheijde, MR (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM michiel@strw.leidenuniv.nl NR 32 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4837 EP 4845 DI 10.1088/0004-6256/137/6/4837 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300027 ER PT J AU Fernandez, JM Holman, MJ Winn, JN Torres, G Shporer, A Mazeh, T Esquerdo, GA Everett, ME AF Fernandez, Jose M. Holman, Matthew J. Winn, Joshua N. Torres, Guillermo Shporer, Avi Mazeh, Tsevi Esquerdo, Gilbert A. Everett, Mark E. TI THE TRANSIT LIGHT CURVE PROJECT. XII. SIX TRANSITS OF THE EXOPLANET XO-2b SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (XO-2, GSC 03413-00005) ID EXTRASOLAR PLANETS; EFFECTIVE TEMPERATURES; ANGULAR DIAMETERS; SMALLER RADIUS; Y-2 ISOCHRONES; STELLAR; STARS; PARAMETERS; MASS; PHOTOMETRY AB We present photometry of six transits of the exoplanet XO-2b. By combining the light-curve analysis with theoretical isochrones to determine the stellar properties, we find the planetary radius to be 0.996(-0.018)(+0.031) R(Jup) and the planetary mass to be 0.565 +/- 0.054 M(Jup). These results are consistent with those reported previously, and are also consistent with theoretical models for gas giant planets. The midtransit times are accurate to within 1 minute and are consistent with a constant period. However, the period we derive differs by 2.5 sigma from the previously published period. More data are needed to tell whether the period is actually variable (as it would be in the presence of an additional body) or if the timing errors have been underestimated. C1 [Fernandez, Jose M.; Holman, Matthew J.; Torres, Guillermo; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fernandez, Jose M.] Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile. [Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Shporer, Avi; Mazeh, Tsevi] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Fernandez, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jfernand@cfa.harvard.edu FU NASA Origins [NNX09AB33G]; United States-Israel Binational Science Foundation [2006234]; Kepler Mission; NASA Cooperative Agreement [NCC2-1390] FX This work was partly supported by NASA Origins Grant No. NNX09AB33G, and by Grant No. 2006234 from the United States-Israel Binational Science Foundation (BSF). KeplerCam was developed with partial support from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 and the Keplercam observations described in this paper were partly supported by grants from the Kepler Mission to SAO and PSI. NR 35 TC 22 Z9 22 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4911 EP 4916 DI 10.1088/0004-6256/137/6/4911 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300033 ER PT J AU Kavelaars, JJ Jones, RL Gladman, BJ Petit, JM Parker, JW Van Laerhoven, C Nicholson, P Rousselot, P Scholl, H Mousis, O Marsden, B Benavidez, P Bieryla, A Bagatin, AC Doressoundiram, A Margot, JL Murray, I Veillet, C AF Kavelaars, J. J. Jones, R. L. Gladman, B. J. Petit, J. -M. Parker, Joel Wm. Van Laerhoven, C. Nicholson, P. Rousselot, P. Scholl, H. Mousis, O. Marsden, B. Benavidez, P. Bieryla, A. Campo Bagatin, A. Doressoundiram, A. Margot, J. L. Murray, I. Veillet, C. TI THE CANADA-FRANCE ECLIPTIC PLANE SURVEY-L3 DATA RELEASE: THE ORBITAL STRUCTURE OF THE KUIPER BELT SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper Belt; surveys ID TRANS-NEPTUNIAN OBJECTS; JUPITER-FAMILY COMETS; SOLAR-SYSTEM; DYNAMICAL CLASSIFICATION; INCLINATION DISTRIBUTION; LUMINOSITY FUNCTION; SIZE DISTRIBUTION; HAWAII-TELESCOPE; ORIGIN; AU AB We report the orbital distribution of the trans-Neptunian comets discovered during the first discovery year of the Canada-France Ecliptic Plane Survey (CFEPS). CFEPS is a Kuiper Belt object survey based on observations acquired by the Very Wide component of the Canada-France-Hawaii Telescope Legacy Survey (LS-VW). The first year's detections consist of 73 Kuiper Belt objects, 55 of which have now been tracked for three years or more, providing precise orbits. Although this sample size is small compared to the world-wide inventory, because we have an absolutely calibrated and extremely well-characterized survey (with known pointing history) we are able to de-bias our observed population and make unbiased statements about the intrinsic orbital distribution of the Kuiper Belt. By applying the (publically available) CFEPS Survey Simulator to models of the true orbital distribution and comparing the resulting simulated detections to the actual detections made by the survey, we are able to rule out several hypothesized Kuiper Belt object orbit distributions. We find that the main classical belt's so-called 'cold' component is confined in semimajor axis (a) and eccentricity (e) compared to the more extended "hot" component; the cold component is confined to lower e and does not stretch all the way out to the 2: 1 resonance but rather depletes quickly beyond a = 45 AU. For the cold main classical belt population we find a robust population estimate of N(H(g) < 10) = 50 +/- 5 x 103 and find that the hot component of the main classical belt represents similar to 60% of the total population. The inner classical belt (sunward of the 3: 2 mean-motion resonance) has a population of roughly 2000 trans-Neptunian objects with absolute magnitudes H(g) < 10, and may not share the inclination distribution of the main classical belt. We also find that the plutino population lacks a cold low-inclination component, and so, the population is somewhat larger than recent estimates; our analysis shows a plutino population of N(H(g) < 10) similar to 25(-12)(+25) x 10(3) compared to our estimate of the size of main classical Kuiper Belt population of N(H(g) < 10) similar to (126(-46)(+50)) x 10(3). C1 [Kavelaars, J. J.; Jones, R. L.; Murray, I.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Nicholson, P.; Margot, J. L.] Cornell Univ, Ithaca, NY 14853 USA. [Veillet, C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Marsden, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Scholl, H.] Observ Cote Azur, F-06304 Nice 4, France. [Parker, Joel Wm.; Bieryla, A.] SW Res Inst, Space Sci & Engn Div, Boulder, CO 80302 USA. [Doressoundiram, A.] Observ Paris, LESIA, F-92195 Meudon, France. [Benavidez, P.; Campo Bagatin, A.] Univ Alicante, EPSA, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain. [Petit, J. -M.; Rousselot, P.; Mousis, O.] Observ Besancon, Inst UTINAM, CNRS, UMR 6213, F-25010 Besancon, France. [Jones, R. L.; Gladman, B. J.; Petit, J. -M.; Van Laerhoven, C.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. RP Kavelaars, JJ (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RI Margot, Jean-Luc/A-6154-2012; Campo Bagatin, Adriano/L-2809-2014 OI Margot, Jean-Luc/0000-0001-9798-1797; Campo Bagatin, Adriano/0000-0001-9840-2216 FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Research Council of Canada; NASA Planetary Astronomy Program [NNG04GI29G] FX This research was supported by funding from the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, the National Research Council of Canada, NASA Planetary Astronomy Program NNG04GI29G. This project could not have been a success without the dedicated staff of the Canada-France-Hawaii telescope as well as the assistance of the skilled telescope operators at KPNO and Mount Palomar. NR 52 TC 41 Z9 41 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4917 EP 4935 DI 10.1088/0004-6256/137/6/4917 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300034 ER PT J AU Romanowsky, AJ Strader, J Spitler, LR Johnson, R Brodie, JP Forbes, DA Ponman, T AF Romanowsky, Aaron J. Strader, Jay Spitler, Lee R. Johnson, Ria Brodie, Jean P. Forbes, Duncan A. Ponman, Trevor TI MAPPING THE DARK SIDE WITH DEIMOS: GLOBULAR CLUSTERS, X-RAY GAS, AND DARK MATTER IN THE NGC 1407 GROUP SO ASTRONOMICAL JOURNAL LA English DT Review DE dark matter; galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: kinematics and dynamics; globular clusters: general; X-rays: galaxies ID EARLY-TYPE GALAXIES; ULTRACOMPACT DWARF GALAXIES; HOT INTERSTELLAR-MEDIUM; GALACTIC NUCLEUS FEEDBACK; NORMAL ELLIPTIC GALAXIES; MASSIVE STAR-CLUSTERS; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; TO-LIGHT RATIOS; HALO MASS AB NGC 1407 is the central elliptical in a nearby evolved group of galaxies apparently destined to become a galaxy cluster core. We use the kinematics of globular clusters (GCs) to probe the dynamics and mass profile of the group's center, out to a radius of 60 kpc (similar to 10 galaxy effective radii)-the most extended data set to date around an early-type galaxy. This sample consists of 172 GC line-of-sight velocities, most of them newly obtained using Keck/DEIMOS, with a few additional objects identified as dwarf-globular transition objects or as intragroup GCs. We find weak rotation for the outer parts of the GC system (v/sigma similar to 0.2), with a rotational misalignment between the metal-poor and metal-rich GCs. The velocity dispersion profile declines rapidly to a radius of similar to 20 kpc, and then becomes flat or rising to similar to 60 kpc. There is evidence that the GC orbits have a tangential bias that is strongest for the metal-poor GCs-in possible contradiction to theoretical expectations. We construct cosmologically motivated galaxy+dark halo dynamical models and infer a total mass within 60 kpc of similar to 3 x 10(12) M-circle dot, which extrapolates to a virial mass of similar to 6 x 10(13) M-circle dot for a typical lambda cold dark matter (Lambda CDM) halo-in agreement with results from kinematics of the group galaxies. We present an independent Chandra-based analysis, whose relatively high mass at similar to 20 kpc disagrees strongly with the GC-based result unless the GCs are assumed to have a peculiar orbit distribution, and we therefore discuss more generally some comparisons between X-ray and optical results. The group's B-band mass-to-light ratio of similar to 800 (uncertain by a factor of similar to 2) in Solar units is extreme even for a rich galaxy cluster, much less a poor group-placing it among the most dark matter (DM) dominated systems in the universe, and also suggesting a massive reservoir of baryons lurking in an unseen phase, in addition to the nonbaryonic DM. We compare the kinematical and mass properties of the NGC 1407 group to other nearby groups and clusters, and discuss some implications of this system for structure formation. C1 [Romanowsky, Aaron J.; Strader, Jay; Brodie, Jean P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Romanowsky, Aaron J.] Univ Concepcion, Dept Fis, Concepcion, Chile. [Johnson, Ria; Ponman, Trevor] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Spitler, Lee R.; Forbes, Duncan A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Romanowsky, AJ (reprint author), Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. EM romanow@ucolick.org RI Spitler, Lee/A-9867-2013 OI Spitler, Lee/0000-0001-5185-9876 FU W. M. Keck Foundation; NSF [AST-0071048]; National Science Foundation [AST-0507729, AST-0808099]; NASA [HST-GO-09766.01-A, HST-GO-10402.06-A, NAS5-26555]; FONDAP Center for Astrophysics [15010003]; ARC FX We thank Jurg Diemand, Sandy Faber, Caroline Foster, Oleg Gnedin, Brijesh Kumar, Bill Mathews, Nicola Napolitano, Julio Navarro, Joel Primack, Simon White, and Marcel Zemp for helpful discussions, and Mark Wilkinson for a constructive review. We thank Eugene Churazov, Vince Eke, Yasushi Fukazawa, Fill Humphrey, Kyoko Matsushita, and Haiguang Xu for providing their results in tabular form, and Javier Cenarro, George Hau, Rob Proctor, and Max Spolaor for supplying their data to us prior to publication. 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 the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Based in part on data collected at Subaru Telescope (which is operated by the National Astronomical Observatory of Japan), via a Gemini Observatory time exchange (Program ID GC-2006B-C-18). We usedmethods and code provided in Numerical Recipes (Press et al. 1992). This material is based upon work supported by the National Science Foundation under grants AST-0507729 and AST-0808099, and by NASA grants HST-GO-09766.01-A and HST-GO-10402.06-A. A. J. R. was further supported by the FONDAP Center for Astrophysics CONICYT 15010003. J. S. was supported by NASA through a Hubble Fellowship, administered by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. L. S. and D. F. thank the ARC for financial support. NR 275 TC 77 Z9 77 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 4956 EP 4987 DI 10.1088/0004-6256/137/6/4956 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300037 ER PT J AU de Gregorio-Monsalvo, I Gomez, JF Anglada, G Torrelles, JM Kuiper, TBH Suarez, O Patel, NA AF de Gregorio-Monsalvo, Itziar Gomez, Jose F. Anglada, Guillem Torrelles, Jose M. Kuiper, Thomas B. H. Suarez, Olga Patel, Nimesh A. TI RADIO CONTINUUM EMISSION AND WATER MASERS TOWARD CB 54 SO ASTRONOMICAL JOURNAL LA English DT Article DE ISM: globules; ISM: jets and outflows; ISM: molecules; masers; radio continuum: ISM; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS STARS; BOK GLOBULES; POWERING SOURCES; NORTHERN SKY; H2O MASERS; OUTFLOWS; REGIONS; PROTOSTARS; AMMONIA AB We present high angular resolution observations of water masers at 1.3 cm and radio continuum emission at 1.3, 3.6, and 6 cm to ward the Bok globule CB 54 using the Very Large Array. At 1.3 cm, with subarcsecond angular resolution, we detect a radio continuum compact source located to the southwest of the globule and spatially coincident with a mid-infrared (mid-IR) embedded object (MIR-b). The spectral index derived between 6 and 1.3 cm (alpha = 0.3 +/- 0.4) is flat, consistent with optically thin free-free emission from ionized gas. We propose the shock-ionization scenario as a viable mechanism for producing the radio continuum emission observed at cm frequencies. Water masers are detected at two different positions separated by 2 ''.3, and coincide spatially with two mid-IR sources: MIR-b and MIR-c. The association of these mid-IR sources with water masers confirms that they are likely protostars undergoing mass loss, and they are the best candidate as driving sources of the molecular outflows in the region. C1 [de Gregorio-Monsalvo, Itziar] European So Observ, Santiago 19, Chile. [Gomez, Jose F.; Anglada, Guillem; Suarez, Olga] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Torrelles, Jose M.] Univ Barcelona, Fac Fis, Inst Ciencias Espacio CSIC IEEC, E-08028 Barcelona, Spain. [Kuiper, Thomas B. H.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Suarez, Olga] Univ Nice Sophia Antipolis, CNRS, UMR H Fizeau 6525, F-06108 Nice 2, France. [Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP de Gregorio-Monsalvo, I (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU Ministerio de Ciencia e Innovacion (Spain) [AYA 2008-06189-C03]; Consejeria de Innovacion; Ciencia y Empresa of Junta de Andalucia, (Spain); National Aeronautics and Space Administration; California Institute of Technology FX We thank the referee for providing constructive comments and help in improving the contents of this paper. We are thankful to Per Bergman for his suggestions. G. A., I. d. G., J. F. G., J. M. T., and O. S. are partially supported by Ministerio de Ciencia e Innovacion (Spain), grant AYA 2008-06189-C03 (including FEDER funds), and by Consejeria de Innovacion, Ciencia y Empresa of Junta de Andalucia, (Spain). The work by TBHK was performed in part at the Jet Propulsion Laboratory under contract between the National Aeronautics and Space Administration and the California Institute of Technology. NR 37 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 5080 EP 5085 DI 10.1088/0004-6256/137/6/5080 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300045 ER PT J AU Meibom, S Grundahl, F Clausen, JV Mathieu, RD Frandsen, S Pigulski, A Narwid, A Steslicki, M Lefever, K AF Meibom, Soren Grundahl, Frank Clausen, Jens Viggo Mathieu, Robert D. Frandsen, Soren Pigulski, Andrzej Narwid, Artur Steslicki, Marek Lefever, Karolien TI AGE AND DISTANCE FOR THE OLD OPEN CLUSTER NGC 188 FROM THE ECLIPSING BINARY MEMBER V 12 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; open clusters and associations: general; open clusters and associations: individual (NGC 188); stars: evolution; techniques: photometric; techniques: spectroscopic ID WIYN OPEN CLUSTER; LOWER MAIN-SEQUENCE; ABSOLUTE DIMENSIONS; RADIAL-VELOCITIES; VARIABLE-STARS; STELLAR PHOTOMETRY; STANDARD CANDLES; CCD PHOTOMETRY; T-EFF; NGC-188 AB We present time series radial velocity, and photometric observations of a solar-type double-lined eclipsing binary star (V 12) in the old open cluster NGC 188. We use these data to determine the spectroscopic orbit and the photometric elements for V 12. From our analysis, we determine accurate masses (M(p) = 1.103 +/- 0.007 M(circle dot), M(s) = 1.081 +/- 0.007 M(circle dot)) and radii (R(p) = 1.424 +/- 0.019 R(circle dot), R(s) = 1.373 +/- 0.019 R(circle dot)) for the primary (p) and secondary (s) binary components. We adopt a reddening of E(B-V) = 0.087 for NGC 188, and derive component effective temperatures of 5900 +/- 100 K and 5875 +/- 100 K, respectively, for the primary and secondary stars. From their absolute dimensions, the two components of V 12 yield identical distance moduli of V(0) - M(V) = 11(m).24 +/- 0(m).09, corresponding to 1770 +/- 75 pc. Both stars are near the end of their main-sequence evolutionary phase, and are located at the cluster turnoff in the color-magnitude diagram. We determine an age of 6.2 +/- 0.2 Gyr for V 12 and NGC 188, from a comparison with theoretical isochrones in the mass-radius diagram. This age is independent of distance, reddening, and color-temperature transformations. We use isochrones from Victoria-Regina (VRSS) and Yonsei-Yale (Y(2)) with [Fe/H]= -0.1 and [Fe/H] = 0.0. From the solar metallicity isochrones, an age of 6.4 Gyr provides the best fit to the binary components for both sets of models. For the isochrones with [Fe/H]= -0.1, ages of 6.0 Gyr and 5.9 Gyr provide the best fits for the (VRSS) and (Y(2)) models, respectively. We use the distance and age estimates for V 12, together with best estimates for the metallicity and reddening of NGC 188, to investigate the locations of the corresponding VRSS and Y(2) isochrones relative to cluster members in the color-magnitude diagram. Plausible changes in the model metallicity and distance to better match the isochrones to the cluster sequences, result in a range of ages for NGC 188 that is more than 3 times that resulting from our analysis of V 12. C1 [Lefever, Karolien] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Meibom, Soren; Mathieu, Robert D.] Univ Wisconsin, Madison, WI USA. [Clausen, Jens Viggo] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Grundahl, Frank; Frandsen, Soren] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus, Denmark. [Pigulski, Andrzej; Narwid, Artur; Steslicki, Marek] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu NR 79 TC 40 Z9 40 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 5086 EP 5098 DI 10.1088/0004-6256/137/6/5086 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300046 ER PT J AU Beasley, MA Cenarro, AJ Strader, J Brodie, JP AF Beasley, Michael A. Javier Cenarro, A. Strader, Jay Brodie, Jean P. TI EVIDENCE FOR THE DISKY ORIGIN OF LUMINOUS VIRGO DWARF ELLIPTICALS FROM THE KINEMATICS OF THEIR GLOBULAR CLUSTER SYSTEMS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: kinematics and dynamics; galaxies: star clusters ID EARLY-TYPE GALAXIES; INTERNAL DYNAMICS; M31; SPECTROSCOPY; POPULATIONS; HARASSMENT; EVOLUTION; CATALOG; GIANTS; VI AB We report evidence for dynamically significant rotation in the globular cluster systems of two luminous Virgo dwarf ellipticals, VCC1261 and VCC1528. Including previous results for VCC1087, the globular cluster systems of all three Virgo dwarf ellipticals studied in detail to date exhibit nu(rot)/sigma(los) > 1. Taking the rotation seen in the globular clusters as a maximal disk rotation, and accounting for the possible fading of any hypothetical progenitor galaxy, we find all three dwarf elliptical galaxies (dEs) lie on the r-band Tully-Fisher relation. We argue that these data support the hypothesis that luminous dEs are the remnants of transformed disk galaxies. We also obtained deep, longslit data for the stars in VCC1261 and VCC1528. Both these galaxies show rapid rotation in their inner regions, with spatial scales of similar to 0.5 kpc. These rotation velocities are surprisingly similar to those seen in the globular cluster systems. At larger radii, we see little rotation in the dEs themselves. Since our longslit data for Virgo dEs extend out to 1-2 effective radii (typical of deep observations), whereas the globular clusters extend out to 4-7 effective radii, we conclude that nondetections of rotation in many luminous dEs may simply be due to a lack of radial coverage in the stellar data, and that globular clusters represent singularly sensitive probes of the dynamics of dEs. Based on these data, we suggest that gas disks are significant sites of globular cluster formation in the early universe. C1 [Beasley, Michael A.; Javier Cenarro, A.] Inst Astrofis Canarias, Tenerife, Spain. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, Jean P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. RP Beasley, MA (reprint author), Inst Astrofis Canarias, Via Lactea S-N, Tenerife, Spain. EM beasley@iac.es; cenarro@iac.es; jstrader@cfa.harvard.edu; brodie@ucolick.org FU NSF [AST-0507729]; NASA through a Hubble Fellowship [NAS 5-26555]; Space Telescope Science Institute FX Funding support comes from NSF grant AST-0507729. J.S. was supported 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., under NASA contract NAS 5-26555. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. They are most fortunate to have the opportunity to conduct observations from this mountain. NR 42 TC 30 Z9 30 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 5146 EP 5153 DI 10.1088/0004-6256/137/6/5146 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300051 ER PT J AU Evans, NR Massa, D Proffitt, C AF Evans, Nancy Remage Massa, Derck Proffitt, Charles TI MASSIVE STAR MULTIPLICITY: THE CEPHEID W SGR (vol 137, pg 3700, 2009) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Proffitt, Charles] Comp Sci Corp, Sci Programs, Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Massa, Derck] SGT Inc, Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2009 VL 137 IS 6 BP 5154 EP 5154 DI 10.1088/0004-6256/137/6/5154 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454DQ UT WOS:000266662300052 ER PT J AU Lammer, H Bredehoft, JH Coustenis, A Khodachenko, ML Kaltenegger, L Grasset, O Prieur, D Raulin, F Ehrenfreund, P Yamauchi, M Wahlund, JE Griessmeier, JM Stangl, G Cockell, CS Kulikov, YN Grenfell, JL Rauer, H AF Lammer, H. Bredehoeft, J. H. Coustenis, A. Khodachenko, M. L. Kaltenegger, L. Grasset, O. Prieur, D. Raulin, F. Ehrenfreund, P. Yamauchi, M. Wahlund, J. -E. Griessmeier, J. -M. Stangl, G. Cockell, C. S. Kulikov, Yu. N. Grenfell, J. L. Rauer, H. TI What makes a planet habitable? SO ASTRONOMY AND ASTROPHYSICS REVIEW LA English DT Review DE Habitability; Origin of life; Terrestrial planets; Subsurface oceans; Atmosphere evolution; Earth-like exoplanets; Space weather; Astrobiology ID EARTH-LIKE PLANETS; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; EJECTION CME ACTIVITY; MASS-LOSS RATES; MAGNETIC-FIELD; ATMOSPHERIC EVOLUTION; TERRESTRIAL PLANETS; INTERSTELLAR-MEDIUM; ISHTAR TERRA AB This work reviews factors which are important for the evolution of habitable Earth-like planets such as the effects of the host star dependent radiation and particle fluxes on the evolution of atmospheres and initial water inventories. We discuss the geodynamical and geophysical environments which are necessary for planets where plate tectonics remain active over geological time scales and for planets which evolve to one-plate planets. The discoveries of methane-ethane surface lakes on Saturn's large moon Titan, subsurface water oceans or reservoirs inside the moons of Solar System gas giants such as Europa, Ganymede, Titan and Enceladus and more than 335 exoplanets, indicate that the classical definition of the habitable zone concept neglects more exotic habitats and may fail to be adequate for stars which are different from our Sun. A classification of four habitat types is proposed. Class I habitats represent bodies on which stellar and geophysical conditions allow Earth-analog planets to evolve so that complex multi-cellular life forms may originate. Class II habitats includes bodies on which life may evolve but due to stellar and geophysical conditions that are different from the class I habitats, the planets rather evolve toward Venus- or Mars-type worlds where complex life-forms may not develop. Class III habitats are planetary bodies where subsurface water oceans exist which interact directly with a silicate-rich core, while class IV habitats have liquid water layers between two ice layers, or liquids above ice. Furthermore, we discuss from the present viewpoint how life may have originated on early Earth, the possibilities that life may evolve on such Earth-like bodies and how future space missions may discover manifestations of extraterrestrial life. C1 [Lammer, H.; Khodachenko, M. L.; Stangl, G.] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. [Bredehoeft, J. H.] Univ Bremen, Inst Angew & Phys Chem, D-2800 Bremen, Germany. [Coustenis, A.] Observ Meudon, LESIA, F-92195 Meudon, France. [Kaltenegger, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grasset, O.] Lab Planetol & Geodynam, UMR, Nantes, France. [Prieur, D.] Univ Bretagne Occidentale, Lab Microbiol Environnements Extremes, Brest, France. [Raulin, F.] Hop Henri Mondor, CNRS, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. [Raulin, F.] Univ Paris 12, Creteil, France. [Raulin, F.] Univ Paris 07, Creteil, France. [Ehrenfreund, P.] Leiden Univ, Leiden Inst Chem, Astrobiol Grp, NL-2300 RA Leiden, Netherlands. [Yamauchi, M.] Swedish Inst Space Phys, S-98128 Kiruna, Sweden. [Wahlund, J. -E.] Swedish Inst Space Phys, Uppsala, Sweden. [Griessmeier, J. -M.] ASTRON, Dwingeloo, Netherlands. [Cockell, C. S.] Open Univ, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. [Kulikov, Yu. N.] Russian Acad Sci, Polar Geophys Inst, Murmansk, Russia. [Grenfell, J. L.] Tech Univ Berlin, Zentrum Astron & Astrophys, Berlin, Germany. [Grenfell, J. L.; Rauer, H.] Inst Planetenforsch, Deutsch Zentrum Luft Raumfahrt, Berlin, Germany. RP Lammer, H (reprint author), Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. EM helmut.lammer@oeaw.ac.at; thoralf@uni-bremen.de; athena.coustenis@obspm.fr; maxim.khodachenko@oeaw.ac.at; lkaltene@cfa.harvard.edu; olivier.grasset@univ-nantes.fr; daniel.prieur@univ-brest.fr; p.ehrenfreund@chem.leidenuniv.nl; yama@irf.se; jwe@irfu.se; griessmeier@astron.nl; guenter.stangl@oeaw.ac.at; c.s.cockell@open.ac.uk; kulikov@pgi.ru; lee.grenfell@dlr.de; heike.rauer@dlr.de RI Bredehoft, Jan Hendrik/E-4221-2012; Kulikov, Yuri/B-7866-2017; Kulikov, Yuri/H-7799-2013 OI Bredehoft, Jan Hendrik/0000-0002-7977-6762; Kulikov, Yuri/0000-0002-1741-3907; Kulikov, Yuri/0000-0001-5475-3284 FU Helmholtz Association through the research alliance "Planetary Evolution and Life; International Space Science Institute; Murmansk, Russian Federation; NASA [NAG5-13045]; Harvard Smithsonian Center for Astrophysics, USA; NASA Astrobiology Institute FX H. Lammer, J. H. Bredehoft and P. Ehrenfreund acknowledge the Fondation des Treilles, France who hosted an Astrobiology meeting where the ideas for this review article originated. Gemeinschaft as this research has been supported by the Helmholtz Association through the research alliance "Planetary Evolution and Life". H. Lammer, L. Kaltenegger, M. L. Khodachenko, J.-M. Griebmeier, J.-L. Grenfell, H. Rauer and Yu. N. Kulikov also acknowledge the International Space Science Institute (ISSI; Bern, Switzerland) and the ISSI teams "Evolution of Habitable Planets" and " Evolution of Exoplanet Atmospheres and their Characterization". The authors also acknowledge fruitful discussions during various meetings related to the Europlanet N2 activities as well as within the N2 Discipline working groups DWG 6 and DWG 7. Yu. N. Kulikov and H. Lammer furthermore acknowledge support by the Austrian Academy of Sciences, " Verwaltungsstelle for Auslandsbeziehungen", by the Russian Academy of Sciences (RAS), for supporting working visits to the PGI/ RAS in Murmansk, Russian Federation. L. Kaltenegger acknowledges also NASA for support of this study by NAG5-13045 at the Harvard Smithsonian Center for Astrophysics, USA. J.H. Bredehft gratefully acknowledges financial support from the Royal Society and from the European Science Foundation under their " Archean Environmental Studies: The Habitat of Early Life" programme. P. Ehenfreund acknowledges the support of NASA Astrobiology Institute (NAI Team Wisconsin). Finally the authors thank an unknown referee for constructive recommendations. NR 215 TC 114 Z9 116 U1 36 U2 304 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0935-4956 EI 1432-0754 J9 ASTRON ASTROPHYS REV JI Astron. Astrophys. Rev. PD JUN PY 2009 VL 17 IS 2 BP 181 EP 249 DI 10.1007/s00159-009-0019-z PG 69 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 454EW UT WOS:000266666200003 ER PT J AU Grindlay, JE AF Grindlay, J. E. TI Unveiling cosmic X-ray/gamma-ray sources from their scattering screen COMMENTARY ON: SUNYAEV R. A. AND TITARCHUK L. G., 1980, A&A, 86, 121 SO ASTRONOMY & ASTROPHYSICS LA English DT Editorial Material ID COMPTONIZATION; SPECTRA; BURSTS; MODEL C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Grindlay, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM josh@head-cfa.harvard.edu NR 15 TC 0 Z9 0 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 JUN PY 2009 VL 500 IS 1 BP 185 EP 186 DI 10.1051/0004-6361/200912156 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 462OD UT WOS:000267363200014 ER PT J AU Eckart, A Baganoff, FK Morris, MR Kunneriath, D Zamaninasab, M Witzel, G Schodel, R Garcia-Marin, M Meyer, L Bower, GC Marrone, D Bautz, MW Brandt, WN Garmire, GP Ricker, GR Straubmeier, C Roberts, DA Muzic, K Mauerhan, J Zensus, A AF Eckart, A. Baganoff, F. K. Morris, M. R. Kunneriath, D. Zamaninasab, M. Witzel, G. Schoedel, R. Garcia-Marin, M. Meyer, L. Bower, G. C. Marrone, D. Bautz, M. W. Brandt, W. N. Garmire, G. P. Ricker, G. R. Straubmeier, C. Roberts, D. A. Muzic, K. Mauerhan, J. Zensus, A. TI Modeling mm- to X-ray flare emission from Sagittarius A* SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE black hole physics; X-rays: general; infrared: general; accretion, accretion disks; Galaxy: center; Galaxy: nucleus ID SUPERMASSIVE BLACK-HOLE; DOMINATED ACCRETION FLOWS; NEAR-INFRARED FLARES; SGR-A; GALACTIC-CENTER; XMM-NEWTON; LINEAR-POLARIZATION; STELLAR DYNAMICS; PROPER MOTIONS; INTRINSIC SIZE AB Context. We report on new modeling results based on the mm- to X-ray emission of the SgrA* counterpart associated with the massive similar to 4 x 10(6) M(circle dot) black hole at the Galactic Center. Aims. We investigate the physical processes responsible for the variable emission from SgrA*. Methods. Our modeling is based on simultaneous observations carried out on 07 July, 2004, using the NACO adaptive optics (AO) instrument at the European Southern Observatory's Very Large Telescope(star) and the ACIS-I instrument aboard the Chandra X-ray Observatory as well as the Submillimeter Array SMA(star star) on Mauna Kea, Hawaii, and the Very Large Array(star star star) in New Mexico. Results. The observations revealed several flare events in all wavelength domains. Here we show that the flare emission can be described with a combination of a synchrotron self-Compton (SSC) model followed by an adiabatic expansion of the source components. The SSC emission at NIR and X-ray wavelengths involves up-scattered sub-millimeter photons from a compact source component. At the start of the flare, spectra of these components peak at frequencies between several 100 GHz and 2 THz. The adiabatic expansion then accounts for the variable emission observed at sub-mm/mm wavelengths. The derived physical quantities that describe the flare emission give a blob expansion speed of v(exp) similar to 0.005 c, magnetic field of B around 60 G or less and spectral indices of alpha = 0.8 to 1.4, corresponding to a particle spectral index p similar to 2.6 to 3.8. Conclusions. A combined SSC and adiabatic expansion model can fully account for the observed flare flux densities and delay times covering the spectral range from the X-ray to the mm- radio domain. The derived model parameters suggest that the adiabatic expansion takes place in source components that have a bulk motion larger than vexp or the expanding material contributes to a corona or disk, confined to the immediate surroundings of SgrA*. C1 [Eckart, A.; Kunneriath, D.; Zamaninasab, M.; Witzel, G.; Garcia-Marin, M.; Straubmeier, C.; Muzic, K.; Zensus, A.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Eckart, A.; Kunneriath, D.; Zamaninasab, M.; Muzic, K.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Baganoff, F. K.; Bautz, M. W.; Ricker, G. R.] MIT, Ctr Space Res, Cambridge, MA 02139 USA. [Morris, M. R.; Meyer, L.; Mauerhan, J.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Schoedel, R.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Bower, G. C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bower, G. C.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Marrone, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brandt, W. N.; Garmire, G. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Roberts, D. A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Eckart, A (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM eckart@ph1.uni-koeln.de; fkb@space.mit.edu; morris@astro.ucla.edu; rainer@iaa.es; gbower@astro.berkeley.edu; dmarrone@cfa.harvard.edu RI Schoedel, Rainer/D-4751-2014; Kunneriath, Devaky/G-8513-2014; Brandt, William/N-2844-2015; OI Schoedel, Rainer/0000-0001-5404-797X; Brandt, William/0000-0002-0167-2453; Marrone, Daniel/0000-0002-2367-1080 FU Deutsche Forschungsgemeinschaft (DFG) [SFB 494]; Max Planck Society; NASA [NAS8-00128, NAS8-38252, GO2-3115B, G05-6093X]; German federal department for education and research (BMBF) [50OS0502, 50OS0801]; Ministerio de Ciencia e Innovacion of the government of Spain FX This work was supported in part by the Deutsche Forschungsgemeinschaft (DFG) via grant SFB 494, the Max Planck Society through the International Max Planck Research School, as well as special funds through the University of Cologne. Chandra research is supported by NASA grants NAS8-00128, NAS8-38252, GO2-3115B, and G05-6093X. We are grateful to all members of the NAOS/CONICA and the ESO PARANAL team. Macarena Garcia-Marin is supported by the German federal department for education and research (BMBF) under the project numbers: 50OS0502 & 50OS0801. M. Zamaninasab, D. Kunneriath, are members of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the MPIfR and the Universities of Bonn and Cologne. R. Schoel acknowledges support by the Ramo y Cajal program by the Ministerio de Ciencia e Innovacion of the government of Spain. NR 98 TC 39 Z9 39 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 JUN PY 2009 VL 500 IS 3 BP 935 EP 946 DI 10.1051/0004-6361/200811354 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 466GX UT WOS:000267650500001 ER PT J AU Bujarrabal, V Young, K Castro-Carrizo, A AF Bujarrabal, V. Young, K. Castro-Carrizo, A. TI The physical conditions in Gomez's Hamburger (IRAS 18059-3211), a pre-MS rotating disk SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: circumstellar matter; stars: planetary systems: protoplanetary disks; stars: formation; stars: individual: Gomez's Hamburger ID INTERMEDIATE-MASS STARS; HERBIG AE SYSTEMS; AB-AURIGAE; PROTOPLANETARY DISKS; HIGH-RESOLUTION; T-TAURI; DM-TAU; EMISSION; GAS; CHEMISTRY AB Aims. We aim to study the structure, dynamics, and physical conditions of Gomez's Hamburger (IRAS 18059-3211; GoHam), and in particular confirm that GoHam mainly consists of a flaring disk in Keplerian rotation around a young, probably pre-MS star. Methods. We present high resolution SMA maps of (12)CO J = 2-1, (13)CO J = 2-1, (12)CO J = 3-2, and C(17)O J = 3-2, as well as data on (12)CO J = 6-5 and the continuum flux at these wavelengths. Spatial resolutions as high as 1 '' are attained. Except for the C(17)O data, the dynamical ranges are larger than 10. The maps are compared with a numerical model, which simulates the emission of a rotating disk with the expected general properties of such objects, and a very satisfactory fitting of our maps is obtained. The meaning and reliability of our results are thoroughly discussed. Results. Our observations allow measurement of the main properties of GoHam on scales of between similar to 1 '' (similar to 5 x 10(15) cm, for the assumed distance, 300 pc) and the total extent of the nebula, 14 ''. We are able to measure the global structure of the gas-rich disk, which is found to be flaring, and its dynamics, which is clearly dominated by Keplerian rotation, with a small degree of turbulence. The combination of different lines, in particular of different opacities, allows us to estimate reasonably the distributions of gas temperature and density. We clearly find a significant and sharp increase in temperature at large distances from the equator, accompanied by a decrease in density of the same order. Finally, we identify a condensation in the southern part of the disk that has no counterparts in the northern nebula. This condensation is quite extended (about 5 x 10(15) cm), contains a significant amount of mass (roughly, similar to 6 x 10(-3) M(circle dot)), and seems to be associated with a detectable distortion of the global rotation kinematics. We discuss several possible interpretations of that feature. C1 [Bujarrabal, V.] OAN IGN, Alcala De Henares 28803, Spain. [Young, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro-Carrizo, A.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Bujarrabal, V (reprint author), OAN IGN, Apartado 112, Alcala De Henares 28803, Spain. EM v.bujarrabal@oan.es; rtm@cfa.harvard.edu; ccarrizo@iram.fr NR 31 TC 3 Z9 3 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 JUN PY 2009 VL 500 IS 3 BP 1077 EP U167 DI 10.1051/0004-6361/200811233 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 466GX UT WOS:000267650500011 ER PT J AU Marti-Vidal, I Marcaide, JM Alberdi, A Guirado, JC Perez-Torres, MA Ros, E Shapiro, II Beswick, RJ Muxlow, TWB Pedlar, A Argo, MK Immler, S Panagia, N Stockdale, CJ Sramek, RA Van Dyk, S Weiler, KW AF Marti-Vidal, I. Marcaide, J. M. Alberdi, A. Guirado, J. C. Perez-Torres, M. A. Ros, E. Shapiro, I. I. Beswick, R. J. Muxlow, T. W. B. Pedlar, A. Argo, M. K. Immler, S. Panagia, N. Stockdale, C. J. Sramek, R. A. Van Dyk, S. Weiler, K. W. TI 23 GHz VLBI observations of SN 2008ax (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: NGC 4490; radio continuum: stars; supernovae: individual: SN 2008ax; supernovae: general AB We report on phase-referenced 23 GHz Very-Long-Baseline-Interferometry (VLBI) observations of the type IIb supernova SN 2008ax, made with the Very Long Baseline Array (VLBA) on 2 April 2008 (33 days after explosion). These observations resulted in a marginal detection of the supernova. The total flux density recovered from our VLBI image is 0.8 +/- 0.3 mJy (one standard deviation). As it appears, the structure may be interpreted as either a core-jet or a double source. However, the supernova structure could be somewhat confused with a possible close by noise peak. In such a case, the recovered flux density would decrease to 0.48 +/- 0.12 mJy, compatible with the flux densities measured with the VLA at epochs close in time to our VLBI observations. The lowest average expansion velocities derived from our observations are (1.90 +/- 0.30) x 10(5) km s(-1) (case of a double source) and (5.2 +/- 1.3) x 10(4) km s(-1) (taking the weaker source component as a spurious, close by, noise peak, which is the more likely interpretation). These velocities are 7.3 and 2 times higher, respectively, than the maximum ejecta velocity inferred from optical-line observations. C1 [Marti-Vidal, I.; Marcaide, J. M.; Guirado, J. C.; Ros, E.] Univ Valencia, Dpt Astron & Astrofis, E-46100 Burjassot, Spain. [Weiler, K. W.] USN, Res Lab, Washington, DC 20375 USA. [Van Dyk, S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shapiro, I. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marti-Vidal, I.; Ros, E.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Beswick, R. J.; Muxlow, T. W. B.; Pedlar, A.] Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Alberdi, A.; Perez-Torres, M. A.] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Sramek, R. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Stockdale, C. J.] Marquette Univ, Dept Phys, Milwaukee, WI 53201 USA. [Immler, S.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Argo, M. K.] Curtin Univ Technol, Dept Imaging & Appl Phys, Bentley, WA 6845, Australia. [Panagia, N.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. RP Marti-Vidal, I (reprint author), Univ Valencia, Dpt Astron & Astrofis, C Dr Moliner 50, E-46100 Burjassot, Spain. EM I.Marti-Vidal@uv.es RI Marti-Vidal, Ivan/A-8799-2017; OI Marti-Vidal, Ivan/0000-0003-3708-9611; Muxlow, Thomas/0000-0001-5797-8796; Ros, Eduardo/0000-0001-9503-4892; Argo, Megan/0000-0003-3594-0214; Van Dyk, Schuyler/0000-0001-9038-9950 FU Spanish DGICYT [AYA2006-14986-CO2-01, AYA2006-14986-C02-02]; Office of Naval Research; Alexander von Humboldt Foundation FX The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. This work has been partially funded by grants AYA2006-14986-CO2-01 and AYA2006-14986-C02-02 of the Spanish DGICYT. K. W. W. thanks the Office of Naval Research for the 6.1 funding supporting this research. I. M. V. is a fellow of the Alexander von Humboldt Foundation. NR 15 TC 5 Z9 5 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 JUN PY 2009 VL 499 IS 3 BP 649 EP 652 DI 10.1051/0004-6361/200912034 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BK UT WOS:000266730600006 ER PT J AU Murgia, M Govoni, F Markevitch, M Feretti, L Giovannini, G Taylor, GB Carretti, E AF Murgia, M. Govoni, F. Markevitch, M. Feretti, L. Giovannini, G. Taylor, G. B. Carretti, E. TI Comparative analysis of the diffuse radio emission in the galaxy clusters A1835, A2029, and Ophiuchus SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: A1835, A2029, Ophiuchus; radio continuum: galaxies ID FIELD POWER SPECTRUM; NORTHERN SKY SURVEY; X-RAY-PROPERTIES; MAGNETIC-FIELD; RELIC CANDIDATES; LOW-FREQUENCY; HALO SURVEY; REACCELERATION; ACCELERATION; ABELL-2163 AB Aims. We recently performed a study of a sample of relaxed, cooling core galaxy clusters with deep Very Large Array observations at 1.4 GHz. We find that in the central regions of A1835, A2029, and Ophiuchus the dominant radio galaxy is surrounded by a diffuse low-brightness radio emission that takes the form of a mini-halo. Here we present the results of the analysis of the extended diffuse radio emission in these mini-halos. Methods. In order to investigate the morphological properties of the diffuse radio emission in clusters of galaxies we propose to fit their azimuthally averaged brightness profile with an exponential, obtaining the central brightness and the e-folding radius from which the radio emissivity can be calculated. We investigate the radio properties of the mini-halos in A1835, A2029, and Ophiuchus in comparison with the radio properties of a representative sample of mini-halos and halos already known in the literature. Results. We find that radio halos can have quite different length-scales but their emissivity is remarkably similar from one halo to the other. In contrast, mini-halos span a wide range of radio emissivity. Some of them, like the Perseus mini-halo, are characterized by a radio emissivity which is more than 100 times greater than that of radio halos. On the other hand, the new mini-halos in cooling core clusters analyzed in this work, namely A2029, Ophiuchus, and A1835, have a radio emissivity which is much more typical of halos in merging clusters rather than similar to that of the other mini-halos previously known. C1 [Murgia, M.; Govoni, F.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [Murgia, M.; Feretti, L.; Giovannini, G.; Carretti, E.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Taylor, G. B.] Univ New Mexico, Albuquerque, NM 87131 USA. [Taylor, G. B.] Natl Radio Astron Observ, Charlottesville, VA USA. RP Murgia, M (reprint author), INAF Osservatorio Astron Cagliari, Poggio Pini,Str 54, I-09012 Capoterra, CA, Italy. EM m.murgia@ira.inaf.it OI Govoni, Federica/0000-0003-3644-3084; Feretti, Luigina/0000-0003-0312-6285; Murgia, Matteo/0000-0002-4800-0806; Giovannini, Gabriele/0000-0003-4916-6362 FU Italian Ministry of University and Research (MUR); Chandra grants [GO5-6123X, GO6-7126X]; NASA [NAS8-39073]; Smithsonian Institution; ASI-INAF [I/088/06/0]; High Energy Astrophysics [PRIN-INAF2005]; National Aeronautics and Space Administration FX We are grateful to an anonymous referee for very useful comments that improved the paper. This work is part of the "Cybersar" Project, which is managed by the COSMOLAB Regional Consortium with the financial support of the Italian Ministry of University and Research (MUR), in the context of the "Piano Operativo Nazionale Ricerca Scientifica, Sviluppo Tecnologico, Alta Formazione (PON 2000-2006)". F. G. and M. M. thank the hospitality of the Harvard-Smithsonian Center for Astrophysics where most of this research was done. Support was provided by Chandra grants GO5-6123X and GO6-7126X, NASA contract NAS8-39073, and the Smithsonian Institution. This research was partially supported by ASI-INAF I/088/06/0 - High Energy Astrophysics and PRIN-INAF2005. We wish to thank Pasquale Mazzotta for his valuable comments on the original draft. We are also grateful to Rossella Cassano and Chiara Ferrari for very useful discussions. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Data Base (NED) which is operated by the JPL, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 44 TC 46 Z9 46 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 JUN PY 2009 VL 499 IS 3 BP 679 EP 695 DI 10.1051/0004-6361/200911659 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BK UT WOS:000266730600010 ER PT J AU Vrsnak, B Poletto, G Vujic, E Vourlidas, A Ko, YK Raymond, JC Ciaravella, A Zic, T Webb, DF Bemporad, A Landini, F Schettino, G Jacobs, C Suess, ST AF Vrsnak, B. Poletto, G. Vujic, E. Vourlidas, A. Ko, Y. -K. Raymond, J. C. Ciaravella, A. Zic, T. Webb, D. F. Bemporad, A. Landini, F. Schettino, G. Jacobs, C. Suess, S. T. TI Morphology and density structure of post-CME current sheets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: corona; Sun: solar wind; magnetohydrodynamics (MHD) ID CORONAL MASS EJECTIONS; FLARE SUPRA-ARCADE; SOLAR-FLARE; MAGNETIC RECONNECTION; ENERGY-RELEASE; 2-RIBBON FLARE; ACTIVE-REGION; II BURSTS; MODEL; DYNAMICS AB Context. Eruption of a coronal mass ejection (CME) drags and "opens" the coronal magnetic field, presumably leading to the formation of a large-scale current sheet and field relaxation by magnetic reconnection. Aims. We analyze the physical characteristics of ray-like coronal features formed in the aftermath of CMEs, to confirm whether interpreting this phenomenon in terms of a reconnecting current sheet is consistent with observations. Methods. The study focuses on measurements of the ray width, density excess, and coronal velocity field as a function of the radial distance. Results. The morphology of the rays implies that they are produced by Petschek-like reconnection in the large-scale current sheet formed in the wake of CME. The hypothesis is supported by the flow pattern, often showing outflows along the ray, and sometimes also inflows into the ray. The inferred inflow velocities range from 3 to 30 km s(-1), and are consistent with the narrow opening-angle of rays, which add up to a few degrees. The density of rays is an order of magnitude higher than in the ambient corona. The density-excess measurements are compared with the results of the analytical model in which the Petschek-like reconnection geometry is applied to the vertical current sheet, taking into account the decrease in the external coronal density and magnetic field with height. Conclusions. The model results are consistent with the observations, revealing that the main cause of the density excess in rays is a transport of the dense plasma from lower to higher heights by the reconnection outflow. C1 [Vrsnak, B.; Zic, T.] Fac Geodesy, Hvar Observ, Zagreb, Croatia. [Poletto, G.] INAF Arcetri Observ, Florence, Italy. [Vourlidas, A.; Ko, Y. -K.] USN, Res Lab, Washington, DC 20375 USA. [Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Ciaravella, A.] INAF Palermo Observ, Palermo, Italy. [Webb, D. F.] Boston Coll, Hanscom AFB, MA USA. [Bemporad, A.] INAF Torino Astrophys Observ, Pino Torinese, Italy. [Landini, F.; Schettino, G.] Univ Florence, Dept Astron & Space Sci, I-50121 Florence, Italy. [Jacobs, C.] Katholieke Univ Leuven, Ctr Plasma Astrofys, Louvain, Belgium. RP Vrsnak, B (reprint author), Fac Geodesy, Hvar Observ, Zagreb, Croatia. EM bvrsnak@geof.hr RI Vourlidas, Angelos/C-8231-2009; OI Vourlidas, Angelos/0000-0002-8164-5948; Ciaravella, Angela/0000-0002-3127-8078; Schettino, Giulia/0000-0003-0819-5052; Bemporad, Alessandro/0000-0001-5796-5653 NR 67 TC 32 Z9 35 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 JUN PY 2009 VL 499 IS 3 BP 905 EP 916 DI 10.1051/0004-6361/200810844 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BK UT WOS:000266730600031 ER PT J AU Perets, HB Fabrycky, DC AF Perets, Hagai B. Fabrycky, Daniel C. TI ON THE TRIPLE ORIGIN OF BLUE STRAGGLERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; blue stragglers; open clusters and associations: general; stellar dynamics ID OPEN CLUSTER M67; GLOBULAR-CLUSTERS; ADDITIONAL COMPONENTS; CONTACT BINARIES; TIDAL FRICTION; SPECTROSCOPIC BINARIES; ORBITAL EVOLUTION; MASS-TRANSFER; STARS; SYSTEMS AB Blue straggler stars (BSSs) are stars observed to be hotter and bluer than other stars with the same luminosity in their environment. As such they appear to be much younger than the rest of the stellar population. Two main channels have been suggested to produce such stars: (1) collisions between stars in clusters or (2) mass transfer between, or merger of, the components of primordial short-period binaries. Here we suggest a third scenario, in which the progenitors of BSSs are formed in primordial (or dynamically formed) hierarchical triple stars. In such configurations, the dynamical evolution of the triples through the Kozai mechanism and tidal friction can induce the formation of very close inner binaries. Angular momentum loss in a magnetized wind or stellar evolution could then lead to the merger of these binaries (or to mass transfer between them) and produce BSSs in binary (or triple) systems. We study this mechanism and its implications and show that it could naturally explain many of the characteristics of the BSS population in clusters, most notably the large binary fraction of long-period BSS binaries; their unique period-eccentricity distribution (with typical periods > 700 days); and the typical location of these BSSs in the color-magnitude diagram, far from the cluster turnoff point of their host clusters. We suggest that this scenario has a major (possibly dominant) role in the formation of BSSs in open clusters and give specific predictions for the BSSs population formed in this manner. We also note that triple systems may be the progenitors of the brightest planetary nebulae in old elliptical galaxies, which possibly evolved from BSSs. C1 [Perets, Hagai B.] Weizmann Inst Sci, IL-76100 Rehovot, Israel. [Fabrycky, Daniel C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Perets, HB (reprint author), Weizmann Inst Sci, IL-76100 Rehovot, Israel. EM hagai.perets@weizmann.ac RI Perets, Hagai/K-9605-2015; OI Perets, Hagai/0000-0002-5004-199X; Fabrycky, Daniel/0000-0003-3750-0183 FU ISF [928/06]; National Aeronautics and Space Administration FX We thank Bob Mathieu and Aaron Geller for helpful discussions and for supplying us with their prepublished data on BSS binaries in NGC 188. We thank Scott Tremaine and the referee Peter Eggleton for helpful comments and discussions. H. B. P. is supported by ISF grant 928/06 and gratefully acknowledges support from a Michelson Fellowship, which is supported by the National Aeronautics and Space Administration and administered by the Michelson Science Center. NR 62 TC 96 Z9 96 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1048 EP 1056 DI 10.1088/0004-637X/697/2/1048 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500010 ER PT J AU Henry, AL Siana, B Malkan, MA Ashby, MLN Bridge, CR Chary, RR Colbert, JW Giavalisco, M Teplitz, HI McCarthy, PJ AF Henry, Alaina L. Siana, Brian Malkan, Matthew A. Ashby, Matthew L. N. Bridge, Carrie R. Chary, Ranga-Ram Colbert, James W. Giavalisco, Mauro Teplitz, Harry I. McCarthy, Patrick J. TI EXPANDING THE SEARCH FOR GALAXIES AT z similar to 7-10 WITH NEW NICMOS PARALLEL FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift ID STAR-FORMING GALAXIES; ULTRA-DEEP-FIELD; LYMAN-CONTINUUM EMISSION; ULTRAVIOLET LUMINOSITY DENSITY; NEAR-INFRARED PROPERTIES; STELLAR MASS DENSITY; I'-DROP GALAXIES; UDF05 FOLLOW-UP; BREAK GALAXIES; COSMIC REIONIZATION AB We have carried out a search for galaxies at z similar to 7-10 in similar to 14.4 arcmin(2) of new NICMOS parallel imaging taken in the Great Observatories Origins Deep Survey (5.9 arcmin(2)), the Cosmic Origins Survey (7.2 arcmin(2)), and SSA22 (1.3 arcmin(2)). These images reach 5 sigma sensitivities of J(110) = 26.0-27.5 (AB), and combined they increase the amount of deep near-infrared data by more than 60% in fields where the investment in deep optical data has already been made. We find no z > 7 candidates in our survey area, consistent with the Bouwens et al. measurements at z similar to 7 and 9 (over 23 arcmin(2)), which predict 0.7 galaxies at z similar to 7 and <0.03 galaxies at z similar to 9. We estimate that 10%-20% of z > 7 galaxies are missed by this survey, due to incompleteness from foreground contamination by faint sources. For the case of luminosity evolution, assuming a Schecter parameterization with a typical phi* = 10(-3) Mpc(-3), we find M* > -20.0 for z similar to 7 and M* > -20.7 for z similar to 9 (68% confidence). This suggests that the downward luminosity evolution of Lyman break galaxies continues to z similar to 7, although our result is marginally consistent with the z similar to 6 luminosity function of Bouwens et al. In addition, we present newly acquired deep MMT/Megacam imaging of the z similar to 9 candidate JD2325+1433, first presented in Henry et al. The resulting weak but significant detection at i' indicates that this galaxy is most likely an interloper at z similar to 2.7. C1 [Henry, Alaina L.; Malkan, Matthew A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Siana, Brian] CALTECH, Pasadena, CA 91125 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bridge, Carrie R.; Chary, Ranga-Ram; Colbert, James W.; Teplitz, Harry I.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [McCarthy, Patrick J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. RP Henry, AL (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Box 951547, Los Angeles, CA 90095 USA. EM ahenry@astro.ucla.edu FU University of California President's Dissertation Year Fellowship FX This work is funded in part by the University of California President's Dissertation Year Fellowship. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The authors thank S. Furlanetto for helpful discussions, and K. Kornei and R. Bouwens for comments that improved this manuscript. NR 59 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1128 EP 1137 DI 10.1088/0004-637X/697/2/1128 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500015 ER PT J AU Mason, BS Robishaw, T Heiles, C Finkbeiner, D Dickinson, C AF Mason, B. S. Robishaw, T. Heiles, C. Finkbeiner, D. Dickinson, C. TI A LIMIT ON THE POLARIZED ANOMALOUS MICROWAVE EMISSION OF LYNDS 1622 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual (Lynds 1622); polarization; radio continuum: ISM ID SPINNING DUST; COSMOSOMAS EXPERIMENT; CROSS-CORRELATION; ANISOTROPY-PROBE; GALACTIC DUST; GRAINS; RADIATION; MAPS; FOREGROUNDS; CLOUD AB The dark cloud Lynds 1622 is one of a few specific sites in the Galaxy where, relative to observed free-free and vibrational dust emission, there is a clear excess of microwave emission. In order to constrain models for this microwave emission, and to better establish the contribution which it might make to ongoing and near-future microwave background polarization experiments, we have used the Green Bank Telescope to search for linear polarization at 9.65 Ghz toward Lynds 1622. We place a 95.4% upper limit of 88 mu K (123 mu K at 99.7% confidence) on the total linear polarization of this source averaged over a 1'.3 FWHM beam. Relative to the observed level of anomalous emission in Stokes I these limits correspond to fractional linear polarizations of 2.7% and 3.5%. C1 [Mason, B. S.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. [Robishaw, T.; Heiles, C.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Finkbeiner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dickinson, C.] CALTECH, Infrrrared Proc & Anal Ctr, Pasadena, CA 91125 USA. RP Mason, BS (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22904 USA. EM bmason@nrao.edu RI Robishaw, Timothy/B-2654-2014 OI Robishaw, Timothy/0000-0002-4217-5138 NR 28 TC 19 Z9 19 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1187 EP 1193 DI 10.1088/0004-637X/697/2/1187 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500020 ER PT J AU Moodley, K Warne, R Goheer, N Trac, H AF Moodley, K. Warne, R. Goheer, N. Trac, H. TI DETECTION OF HOT GAS IN GALAXY GROUPS VIA THE THERMAL SUNYAEV-ZEL'DOVICH EFFECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; galaxies: clusters: general ID ANGULAR POWER SPECTRA; X-RAY-PROPERTIES; ATACAMA-COSMOLOGY-TELESCOPE; LY-ALPHA FOREST; INTERGALACTIC MEDIUM; INTRACLUSTER MEDIUM; DUST EMISSION; STATISTICAL PROPERTIES; COMPONENT SEPARATION; ABSORPTION SYSTEMS AB Motivated by the observed shortfall of baryons in the local universe, we investigate the ability of high-resolution cosmic microwave background (CMB) experiments to detect hot gas in the outer regions of nearby group halos. We construct hot gas models with the gas in hydrostatic equilibrium with the dark matter and described by a polytropic equation of state. We also consider models that add entropy to the gas in line with constraints from X-ray observations. We calculate the thermal Sunyaev-Zel'dovich (tSZ) signal in these halos and compare it to the anticipated sensitivities of forthcoming tSZ survey experiments such as Antenna Cosmology Telescope, PLANCK, and South Pole Telescope. Using a multifrequency Wiener filter we derive tSZ detectability limits as a function of halo mass and redshift in the presence of galactic and extragalactic foregrounds and the CMB. We find that group-sized halos with virial masses below 10(14) M(circle dot) can be detected at z less than or similar to 0.05 with the threshold mass dropping to (3-4) x 10(13) M(circle dot) at z less than or similar to 0.01. The tSZ distortion of nearby group-sized halos can thus be mapped out to the virial radius by these CMB experiments, beyond the sensitivity limits of X-ray observations. These measurements will provide a unique probe of hot gas in the outer regions of group halos, shedding insight into the local census of baryons and the injection of entropy into the intragroup medium from nongravitational feedback. C1 [Moodley, K.; Warne, R.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. [Goheer, N.] Univ Cape Town, Dept Math & Appl Math, ZA-7700 Rondebosch, South Africa. [Trac, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Moodley, K (reprint author), Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. EM moodleyk41@ukzn.ac.za RI Trac, Hy/N-8838-2014 OI Trac, Hy/0000-0001-6778-3861 NR 94 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1392 EP 1409 DI 10.1088/0004-637X/697/2/1392 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500038 ER PT J AU Ly, C Malkan, MA Treu, T Woo, JH Currie, T Hayashi, M Kashikawa, N Motohara, K Shimasaku, K Yoshida, M AF Ly, Chun Malkan, Matthew A. Treu, Tommaso Woo, Jong-Hak Currie, Thayne Hayashi, Masao Kashikawa, Nobunari Motohara, Kentaro Shimasaku, Kazuhiro Yoshida, Makiko TI LYMAN BREAK GALAXIES AT z approximate to 1.8-2.8: GALEX/NUV IMAGING OF THE SUBARU DEEP FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: photometry ID STAR-FORMING GALAXIES; REST-FRAME ULTRAVIOLET; HIGH-REDSHIFT GALAXIES; LY-ALPHA-EMISSION; UV LUMINOSITY FUNCTION; FORMATION HISTORY; H-ALPHA; EVOLUTION; DENSITY; Z-SIMILAR-TO-3 AB A photometric sample of similar to 8000 V < 25.3 candidate Lyman break galaxies (LBGs) has been selected by combining Subaru/Suprime-Cam BVR(C)i'z' optical data with deep GALEX/NUV imaging of the Subaru Deep Field. Follow-up spectroscopy confirmed 24 LBGs at 1.5 less than or similar to z less than or similar to 2.7. Among the optical spectra, 12 have Lya emission with rest-frame equivalent widths of approximate to 5-60 angstrom. The success rate for identifying LBGs as NUV-dropouts at 1.5 < z < 2.7 is 86%. The rest-frame UV (1700 angstrom) luminosity function (LF) is constructed from the photometric sample with corrections for stellar contamination and z < 1.5 interlopers (lower limits). The LF is 1.7 +/- 0.1 (1.4 +/- 0.1 with a hard upper limit on stellar contamination) times higher than those of z similar to 2 BXs and z similar to 3 LBGs. Three explanations were considered, and it is argued that significantly underestimating low-z contamination or effective comoving volume is unlikely: the former would be inconsistent with the spectroscopic sample at 93% confidence, and the second explanation would not resolve the discrepancy. The third scenario is that different photometric selection of the samples yields nonidentical galaxy populations, such that some BX galaxies are LBGs and vice versa. This argument is supported by a higher surface density of LBGs at all magnitudes while the redshift distribution of the two populations is nearly identical. This study, when combined with other star formation rate (SFR) density UV measurements from LBG surveys, indicates that there is a rise in the SFR density: a factor of 3-6 (3-10) increase from z similar to 5 (z similar to 6) to z similar to 2, followed by a decrease to z similar to 0. This result, along with past sub-mm studies that find a peak at z similar to 2 in their redshift distribution, suggests that z similar to 2 is the epoch of peak star formation. C1 [Ly, Chun; Malkan, Matthew A.; Woo, Jong-Hak] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Treu, Tommaso] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Currie, Thayne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hayashi, Masao; Shimasaku, Kazuhiro; Yoshida, Makiko] Univ Tokyo, Dept Astron, Sch Sci, Bunkyo Ku, Tokyo 113, Japan. [Kashikawa, Nobunari] Natl Astron Observ, Div Opt & Infrared Astron, Tokyo 181, Japan. [Kashikawa, Nobunari] Grad Univ Adv Studies, Sch Sci, Dept Astron, Tokyo, Japan. [Motohara, Kentaro] Univ Tokyo, Inst Astron, Tokyo 113, Japan. [Shimasaku, Kazuhiro] Univ Tokyo, Res Ctr Early Universe, Sch Sci, Tokyo, Japan. RP Ly, C (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM chun@astro.ucla.edu RI Woo, Jong-Hak/A-2790-2014; MOTOHARA, KENTARO/G-4905-2014; OI MOTOHARA, KENTARO/0000-0002-0724-9146; Ly, Chun/0000-0002-4245-2318 NR 67 TC 23 Z9 23 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1410 EP 1432 DI 10.1088/0004-637X/697/2/1410 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500039 ER PT J AU Friesen, RK Di Francesco, J Shirley, YL Myers, PC AF Friesen, R. K. Di Francesco, J. Shirley, Y. L. Myers, P. C. TI THE INITIAL CONDITIONS OF CLUSTERED STAR FORMATION. I. NH3 OBSERVATIONS OF DENSE CORES IN OPHIUCHUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; ISM: molecules; ISM: structure; radio lines: ISM; stars: formation ID C2D LEGACY CLOUDS; MOLECULAR CLOUDS; RHO-OPHIUCHI; MAIN CLOUD; CONTINUUM OBSERVATIONS; INTERNAL STRUCTURE; PRESTELLAR CORES; FORMING REGIONS; DARK CLOUDS; 850 MICRONS AB We present combined interferometer and single dish telescope data of NH3 (J, K)=(1,1) and (2,2) emission toward the clustered star forming Ophiuchus B, C, and F Cores at high spatial resolution (similar to 1200 AU) using the Australia Telescope Compact Array, the Very Large Array, and the Green Bank Telescope. While the large-scale features of the NH3 (1,1) integrated intensity appear similar to 850 mu m continuum emission maps of the Cores, on 15 '' (1800 AU) scales we find significant discrepancies between the dense gas tracers in Oph B, but good correspondence in Oph C and F. Using the CLUMPFIND structure identifying algorithm, we identify 15 NH3 clumps in Oph B, and three each in Oph C and F. Only five of the Oph B NH3 clumps are coincident within 30 '' (3600 AU) of a submillimeter clump. We find nu(LSR) varies little across any of the cores, and additionally varies by only similar to 1.5 km s(-1) between them. The observed NH3 line widths within the Oph B and F Cores are generally large and often mildly supersonic, while Oph C is characterized by narrow line widths which decrease to nearly thermal values. We find several regions of localized narrow line emission (Delta nu less than or similar to 0.4 km s(-1)), some of which are associated with NH3 clumps. We derive the kinetic temperatures of the gas, and find they are remarkably constant across Oph B and F, with a warmer mean value (T-K = 15 K) than typically found in isolated regions and consistent with previous results in clustered regions. Oph C, however, has a mean T-K = 12 K, decreasing to a minimum T-K = 9.4 K toward the submillimeter continuum peak, similar to previous studies of isolated starless clumps. There is no significant difference in temperature toward protostars embedded in the Cores. NH3 column densities, N(NH3), and abundances, X(NH3), are similar to previous work in other nearby molecular clouds. We find evidence for a decrease in X(NH3) with increasing N(H-2) in Oph B2 and C, suggesting the NH3 emission may not be tracing well the densest core gas. C1 [Friesen, R. K.; Di Francesco, J.] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [Friesen, R. K.; Di Francesco, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Shirley, Y. L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Friesen, RK (reprint author), Univ Victoria, Dept Phys & Astron, STN CSC, POB 3055, Victoria, BC V8W 3P6, Canada. EM rachel.friesen@nrc-cnrc.gc.ca NR 60 TC 50 Z9 50 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 JUN 1 PY 2009 VL 697 IS 2 BP 1457 EP 1480 DI 10.1088/0004-637X/697/2/1457 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500042 ER PT J AU Gaspar, A Rieke, GH Su, KYL Balog, Z Trilling, D Muzzerole, J Apai, D Kelly, BC AF Gaspar, A. Rieke, G. H. Su, K. Y. L. Balog, Z. Trilling, D. Muzzerole, J. Apai, D. Kelly, B. C. TI THE LOW LEVEL OF DEBRIS DISK ACTIVITY AT THE TIME OF THE LATE HEAVY BOMBARDMENT: A SPITZER STUDY OF PRAESEPE SO ASTROPHYSICAL JOURNAL LA English DT Review DE circumstellar matter; infrared: stars; open clusters and associations: individual (Praesepe M44, NGC 2632, Beehive); planetary systems: formation; stars: evolution ID SOLAR-TYPE STARS; SUN-LIKE STARS; LOW-MASS STARS; YOUNG OPEN CLUSTER; DIGITAL SKY SURVEY; MULTIBAND IMAGING PHOTOMETER; TERRESTRIAL PLANET FORMATION; STELLAR KINEMATIC GROUPS; PICTORIS MOVING GROUP; UVBY-BETA PHOTOMETRY AB We present 24 mu m photometry of the intermediate-age open cluster Praesepe. We assemble a catalog of 193 probable cluster members that are detected in optical databases, the Two Micron All Sky Survey (2MASS), and at 24 mu m, within an area of similar to 2.47 deg(2). Mid-IR excesses indicating debris disks are found for one early-type and for three solar-type stars. Corrections for sampling statistics yield a 24 mu m excess fraction (debris disk fraction) of 6.5% +/- 4.1% for luminous and 1.9% +/- 1.2% for solar-type stars. The incidence of excesses is in agreement with the decay trend of debris disks as a function of age observed for other cluster and field stars. The values also agree with those for older stars, indicating that debris generation in the zones that emit at 24 mu m falls to the older 1-10 Gyr field star sample value by roughly 750 Myr. We discuss our results in the context of previous observations of excess fractions for early- and solar-type stars. We show that solar-type stars lose their debris disk 24 mu m excesses on a shorter timescale than early- type stars. Simplistic Monte Carlo models suggest that, during the first Gyr of their evolution, up to 15%-30% of solar-type stars might undergo an orbital realignment of giant planets such as the one thought to have led to the Late Heavy Bombardment, if the length of the bombardment episode is similar to the one thought to have happened in our solar system. In the Appendix, we determine the cluster's parameters via bootstrap Monte Carlo isochrone fitting, yielding an age of 757 Myr (+/- 36 Myr at 1 sigma confidence) and a distance of 179 pc (+/- 2 pc at 1 sigma confidence), not allowing for systematic errors. C1 [Gaspar, A.; Rieke, G. H.; Su, K. Y. L.; Balog, Z.; Trilling, D.; Muzzerole, J.; Apai, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Trilling, D.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Muzzerole, J.; Apai, D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kelly, B. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gaspar, A (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM agaspar@as.arizona.edu OI Su, Kate/0000-0002-3532-5580; Gaspar, Andras/0000-0001-8612-3236 NR 120 TC 43 Z9 43 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1578 EP 1596 DI 10.1088/0004-637X/697/2/1578 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500050 ER PT J AU Narayan, R Li, J Tchekhovskoy, A AF Narayan, Ramesh Li, Jason Tchekhovskoy, Alexander TI STABILITY OF RELATIVISTIC FORCE-FREE JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; instabilities; MHD ID CURRENT-DRIVEN INSTABILITIES; HOLE ACCRETION SYSTEMS; BLACK-HOLE; MAGNETOHYDRODYNAMIC SIMULATIONS; ASTROPHYSICAL JETS; SCREW INSTABILITY; NUMERICAL SCHEME; RADIO JETS; MODES; FIELD AB We consider a two-parameter family of cylindrical force-free equilibria, modeled to match numerical simulations of relativistic force-free jets. We study the linear stability of these equilibria, assuming a rigid impenetrable wall at the outer cylindrical radius R(j). Equilibria in which the Lorentz factor gamma(R) increases monotonically with increasing radius R are found to be stable. On the other hand, equilibria in which gamma(R) reaches a maximum value at an intermediate radius and then declines to a smaller value gamma(j) at R(j) are unstable. A feature of these unstable equilibria is that poloidal field line curvature plays a prominent role in maintaining transverse force balance. The most rapidly growing mode is an m = 1 kink instability which has a growth rate similar to(0.4/gamma(j))(c/R(j)). The e-folding length of the equivalent convected instability is similar to 2.5 gamma(j)R(j). For a typical jet with an opening angle theta(j) similar to few/gamma(j), the mode amplitude grows only weakly with increasing distance from the base of the jet. The growth is much slower than one might expect from a naive application of the Kruskal-Shafranov stability criterion. C1 [Narayan, Ramesh; Tchekhovskoy, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Jason] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX08AH32G] FX The authors thank Alison Farmer for assistance during the early stages of this work and Jonathan McKinney for numerous helpful discussions and comments on the paper. This work was supported in part by NASA grant NNX08AH32G. NR 39 TC 41 Z9 41 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2009 VL 697 IS 2 BP 1681 EP 1694 DI 10.1088/0004-637X/697/2/1681 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500056 ER PT J AU Antoniou, V Zezas, A Hatzidimitriou, D McDowell, JC AF Antoniou, V. Zezas, A. Hatzidimitriou, D. McDowell, J. C. TI THE CHANDRA SURVEY OF THE SMALL MAGELLANIC CLOUD "BAR". II. OPTICAL COUNTERPARTS OF X-RAY SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Review DE Magellanic Clouds; pulsars: general; stars: early-type; stars: emission-line, Be; stars: formation; X-rays: binaries ID GRAVITATIONAL LENSING EXPERIMENT; XMM-NEWTON OBSERVATIONS; STAR-FORMATION CONDITIONS; ECLIPSING BINARY STARS; MULTIWAVELENGTH PROJECT; FUNDAMENTAL PARAMETERS; LUMINOSITY FUNCTION; PHOTOMETRIC SURVEY; STELLAR CATALOG; EXTINCTION MAP AB We present the most likely optical counterparts of 113 X-ray sources detected in our Chandra survey of the central region of the Small Magellanic Cloud (SMC) based on the OGLE-II and Magellanic Clouds Photometric Survey catalogs. We estimate that the foreground contamination and chance coincidence probability are minimal for the bright optical counterparts (corresponding to OB type stars; 35 in total). We propose here for the first time 13 high-mass X-ray binaries, of which four are Be/X-ray binaries (Be-XRBs), and we confirm the previous classification of 18 Be-XRBs. We estimate that the new candidate Be-XRBs have an age of similar to 15-85 Myr, consistent with the age of Be stars. We also examine the "overabundance" of Be-XRBs in the SMC fields covered by Chandra, in comparison with the Galaxy. In luminosities down to similar to 10(34) erg s(-1), we find that SMC Be-XRBs are similar to 1.5 times more common when compared to the Milky Way even after taking into account the difference in the formation rates of OB stars. This residual excess can be attributed to the lower metallicity of the SMC. Finally, we find that the mixing of Be-XRBs with other than their natal stellar population is not an issue in our comparisons of Be-XRBs and stellar populations in the SMC. Instead, we find indication for variation of the SMC XRB populations on kiloparsec scales, related to local variations of the formation rate of OB stars and slight variation of their age, which results in different relative numbers of Be stars and therefore XRBs. C1 [Antoniou, V.; Zezas, A.; McDowell, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Antoniou, V.; Hatzidimitriou, D.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Antoniou, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vantoniou@head.cfa.harvard.edu RI Hatzidimitriou, Despina/A-3732-2015; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 NR 106 TC 16 Z9 16 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 JUN 1 PY 2009 VL 697 IS 2 BP 1695 EP 1716 DI 10.1088/0004-637X/697/2/1695 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500057 ER PT J AU Bartko, H Martins, F Fritz, TK Genzel, R Levin, Y Perets, HB Paumard, T Nayakshin, S Gerhard, O Alexander, T Dodds-Eden, K Eisenhauer, F Gillessen, S Mascetti, L Ott, T Perrin, G Pfuhl, O Reid, MJ Rouan, D Sternberg, A Trippe, S AF Bartko, H. Martins, F. Fritz, T. K. Genzel, R. Levin, Y. Perets, H. B. Paumard, T. Nayakshin, S. Gerhard, O. Alexander, T. Dodds-Eden, K. Eisenhauer, F. Gillessen, S. Mascetti, L. Ott, T. Perrin, G. Pfuhl, O. Reid, M. J. Rouan, D. Sternberg, A. Trippe, S. TI EVIDENCE FOR WARPED DISKS OF YOUNG STARS IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Review DE Galaxy: center; stars: early-type; stars: formation; stars: luminosity function, mass function; stellar dynamics ID SUPERMASSIVE BLACK-HOLE; SGR-A-ASTERISK; STELLAR ORBITS; CENTRAL PARSEC; MILKY-WAY; MASSIVE STARS; SAGITTARIUS-A; DYNAMICAL FRICTION; ACCRETION DISKS; WIND PROPERTIES AB The central parsec around the supermassive black hole in the Galactic center (GC) hosts more than 100 young and massive stars. Outside the central cusp (R similar to 1 '') the majority of these O and Wolf-Rayet (W-R) stars reside in a main clockwise system, plus a second, less prominent disk or streamer system at large angles with respect to the main system. Here we present the results from new observations of the GC with the AO-assisted near-infrared imager NACO and the integral field spectrograph SINFONI on the ESO/VLT. These include the detection of 27 new reliably measured W-R/O stars in the central 12 '' and improved measurements of 63 previously detected stars, with proper motion uncertainties reduced by a factor of 4 compared to our earlier work. Based on the sample of 90 well measured W-R/O stars, we develop a detailed statistical analysis of their orbital properties and orientations. We show that half of the W-R/O stars are compatible with being members of a clockwise rotating system. The rotation axis of this system shows a strong transition from the inner to the outer regions as a function of the projected distance from Sgr A*. The main clockwise system either is either a strongly warped single disk with a thickness of about 10 degrees, or consists of a series of streamers with significant radial variation in their orbital planes. Eleven out of 61 clockwise moving stars have an angular separation of more than 30 degrees from the local angular momentum direction of the clockwise system. The mean eccentricity of the clockwise system is 0.36 +/- 0.06. The distribution of the counterclockwise W-R/O star is not isotropic at the 98% confidence level. It is compatible with a coherent structure such as stellar filaments, streams, small clusters or possibly a disk in a dissolving state: 10 out of 29 counterclockwise moving W-R/O stars have an angular separation of more than 30 degrees from the local angular momentum direction of the counterclockwise system. The observed disk warp and the steep surface density distribution favor in situ star formation in gaseous accretion disks as the origin of the young massive stars. C1 [Bartko, H.; Fritz, T. K.; Genzel, R.; Gerhard, O.; Dodds-Eden, K.; Eisenhauer, F.; Gillessen, S.; Mascetti, L.; Ott, T.; Pfuhl, O.; Trippe, S.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Martins, F.] Univ Montpellier 2, CNRS, GRAAL, Montpellier, France. [Genzel, R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Levin, Y.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Levin, Y.] Leiden Univ, Inst Lorentz, NL-2300 RA Leiden, Netherlands. [Perets, H. B.; Alexander, T.] Weizmann Inst Sci, Fac Phys, IL-76100 Rehovot, Israel. [Paumard, T.; Perrin, G.; Rouan, D.] Univ C Paris Direrot, UPMC, CNRS, Observ Paris,LESIA, Meudon, France. [Nayakshin, S.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sternberg, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. RP Bartko, H (reprint author), Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. EM hbartko@mpe.mpg.de RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X FU ISF [968/06]; Minerva [8563]; ERC [202996] FX We thank J. Cuadra for his useful comments. T. A. is supported by ISF grant 968/06, Minerva grant 8563, and ERC Starting Grant 202996. NR 108 TC 128 Z9 128 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 JUN 1 PY 2009 VL 697 IS 2 BP 1741 EP 1763 DI 10.1088/0004-637X/697/2/1741 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500060 ER PT J AU Kenworthy, MA Mamajek, EE Hinz, PM Meyer, MR Heinze, AN Miller, DL Sivanandam, S Freed, M AF Kenworthy, Matthew A. Mamajek, Eric E. Hinz, Philip M. Meyer, Michael R. Heinze, Aren N. Miller, Douglas L. Sivanandam, Suresh Freed, Melanie TI MMT/AO 5 mu m IMAGING CONSTRAINTS ON THE EXISTENCE OF GIANT PLANETS ORBITING FOMALHAUT AT similar to 13-40 AU SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; instrumentation: adaptive optics; planetary systems; stars: individual (Fomalhaut) ID ADAPTIVE OPTICS SYSTEM; BROWN DWARFS; SOLAR-SYSTEM; DEBRIS DISKS; MASS; EXOPLANETS; COMPANION; SCATTERING; TELESCOPE; STABILITY AB A candidate less than or similar to 3 M-Jup extrasolar planet was recently imaged by Kalas et al. using Hubble Space Telescope/Advanced Camera for Surveys and Keck II at 12 ''.7 (96 AU) separation from the nearby (d = 7.7 pc) young (similar to 200 Myr) A2V star Fomalhaut. Here, we report results from M-band (4.8 mu m) imaging of Fomalhaut on 2006 December 5 using the Clio IR imager on the 6.5 m MMT with the adaptive secondary mirror. Our images are sensitive to giant planets at orbital radii comparable to the outer solar system (similar to 10-40 AU). Comparing our 5 sigma M-band photometric limits to theoretical evolutionary tracks for substellar objects, our results rule out the existence of planets with masses >2 M-Jup from similar to 13 to 40 AU and objects > 13 M-Jup from similar to 8 to 40 AU. C1 [Kenworthy, Matthew A.; Hinz, Philip M.; Meyer, Michael R.; Miller, Douglas L.; Sivanandam, Suresh; Freed, Melanie] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mamajek, Eric E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heinze, Aren N.] Swarthmore Coll, Swarthmore, PA 19081 USA. RP Kenworthy, MA (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM mkenworthy@as.arizona.edu FU NNG [04-GN39G]; NASA Terrestrial Planet Finder Foundation Science Program; NASA Terrestrial Planet Finder Foundation Science Program [NNG 06-GE26G]; Clay Postdoctoral Fellowship; NASA Astrobiology Institute FX We thank the referees for their detailed comments that made a significant contribution to this paper. We thank the CfA TAC for allocating the MMT time that made these observations possible. We thank the MMT staff, especially John McAfee, Alejandra Milone, Mike Alegria, and Tim Pickering. We also thank Vidhya Vaitheeswaran and Thomas Stalcup for their support of the MMT/AO system. Clio is supported by grant NNG 04-GN39G from the NASA Terrestrial Planet Finder Foundation Science Program. M. A. K. is supported by grant NNG 06-GE26G from the NASA Terrestrial Planet Finder Foundation Science Program. E. E. M. was supported by a Clay Postdoctoral Fellowship during this observing program. M. R. M. acknowledges support through LAPLACE from the NASA Astrobiology Institute. M. A. K. thanks Andrew Skemer for discussions on atmospheric dispersion at thermal infrared wavelengths. NR 48 TC 20 Z9 20 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 JUN 1 PY 2009 VL 697 IS 2 BP 1928 EP 1933 DI 10.1088/0004-637X/697/2/1928 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446YT UT WOS:000266159500075 ER PT J AU Blanton, EL Randall, SW Douglass, EM Sarazin, CL Clarke, TE McNamara, BR AF Blanton, E. L. Randall, S. W. Douglass, E. M. Sarazin, C. L. Clarke, T. E. McNamara, B. R. TI SHOCKS AND BUBBLES IN A DEEP CHANDRA OBSERVATION OF THE COOLING FLOW CLUSTER ABELL 2052 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cooling flows; galaxies: clusters: general; galaxies: clusters: individual (A2052); intergalactic medium; radio continuum: galaxies; X-rays: galaxies: clusters ID RAY-EMITTING GAS; X-RAY; PERSEUS CLUSTER; VORONOI TESSELLATIONS; INTRACLUSTER MEDIUM; GALAXY CLUSTERS; RADIO LOBES; HYDRA-A; ROSAT; TEMPERATURE AB We present results from a deep Chandra observation of Abell 2052. A2052 is a bright, nearby, cooling flow cluster, at a redshift of z = 0.035. Concentric surface brightness discontinuities are revealed in the cluster center, and these features are consistent with shocks driven by the active galactic nucleus (AGN), both with Mach numbers of approximately 1.2. The southern cavity in A2052 now appears to be split into two cavities with the southernmost cavity likely representing a ghost bubble from earlier radio activity. There also appears to be a ghost bubble present to the NW of the cluster center. The cycle time measured for the radio source is t approximate to 2 x 10(7) yr using either the shock separation or the rise time of the bubbles. The energy deposited by the radio source, including a combination of direct shock heating and heating by buoyantly rising bubbles inflated by the AGN, can offset the cooling in the core of the cluster. C1 [Blanton, E. L.; Douglass, E. M.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Randall, S. W.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA. [Clarke, T. E.] Interferometrics Inc, Herndon, VA 20171 USA. [McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. RP Blanton, EL (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM eblanton@bu.edu; srandall@head.cfa.harvard.edu; emdoug@bu.edu; sarazin@virginia.edu; tracy.clarke@nrl.navy.mil; mcnamara@sciborg.uwaterloo.ca RI Blanton, Elizabeth/H-4501-2014; OI Randall, Scott/0000-0002-3984-4337 NR 29 TC 39 Z9 39 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2009 VL 697 IS 2 BP L95 EP L98 DI 10.1088/0004-637X/697/2/L95 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 445TG UT WOS:000266073800005 ER PT J AU Gladman, B Kavelaars, J Petit, JM Ashby, MLN Parker, J Coffey, J Jones, RL Rousselot, P Mousis, O AF Gladman, B. Kavelaars, J. Petit, J. -M. Ashby, M. L. N. Parker, J. Coffey, J. Jones, R. L. Rousselot, P. Mousis, O. TI DISCOVERY OF THE FIRST RETROGRADE TRANSNEPTUNIAN OBJECT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Kuiper Belt; Oort Cloud; solar system: formation ID EXTENDED SCATTERED DISK; TRANS-NEPTUNIAN OBJECTS; JUPITER-FAMILY COMETS; KUIPER-BELT OBJECTS; LONG-PERIOD COMETS; OORT CLOUD; STELLAR ENCOUNTERS; SOLAR-SYSTEM; ORBITS; ORIGIN AB We report the discovery of the first transneptunian object known to be on a retrograde orbit. The discovery was made during an outer solar system survey using the Canada-France-Hawaii Telescope (CFHT). After recovery observations on the MMT, CTIO-Blanco, Gemini-South, and CFHT telescopes, we can state with certainty that the object is both transneptunian and orbits the Sun in a retrograde sense, with an orbital inclination i = 104 deg. The object has IAU Minor Planet Center provisional designation 2008 KV(42) and temporary nickname "Drac." Numerical integration of a set of initial states consistent with the astrometry shows that the semimajor axis is a similar or equal to 42 AU, the perihelion distance is q similar to 21 AU, and that the object's orbit evolves on similar to 30 million year timescales via gravitational encounters with Uranus and Neptune. The object is unlikely to be primordial and thus needs a supply mechanism from a long-lived source. We outline several scenarios which could have emplaced the object on its current orbit, including a currently unobserved reservoir of large-inclination orbits beyond Neptune which may also supply the Halley-type comets. C1 [Gladman, B.; Petit, J. -M.; Coffey, J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kavelaars, J.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Petit, J. -M.; Rousselot, P.; Mousis, O.] Univ Franche Comte, CNRS, Inst UTINAM, F-25010 Besancon, France. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parker, J.] SW Res Inst, Boulder, CO 80302 USA. [Jones, R. L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Gladman, B (reprint author), Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM gladman@astro.ubc.ca NR 30 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2009 VL 697 IS 2 BP L91 EP L94 DI 10.1088/0004-637X/697/2/L91 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 445TG UT WOS:000266073800004 ER PT J AU Krupnick, GA Kress, WJ Wagner, WL AF Krupnick, Gary A. Kress, W. John Wagner, Warren L. TI Achieving Target 2 of the Global Strategy for Plant Conservation: building a preliminary assessment of vascular plant species using data from herbarium specimens SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Conservation assessments; Database; Herbarium; Plant specimens; IUCN Red List; Threatened species ID RED LIST ASSESSMENTS; COLLECTIONS; THREAT; PALMS AB The Global Strategy for Plant Conservation calls for a preliminary assessment of the conservation status of all known plant species by the year 2010. To date insufficient progress has been made on meeting this target. New efforts to develop a preliminary list beyond using the full IUCN criteria in plant assessments are needed. Here we present an algorithm that provides a preliminary assessment of the conservation status of plant species using data from herbarium specimens. We use Hawaiian specimen data from the United States National Herbarium to calibrate the parameters of the algorithm and then use specimen data from the Arecaceae, Commelinaceae, Gesneriaceae and Heliconiaceae as examples of the application of the algorithm. The algorithm was calibrated to insure 95% accuracy in placing the Hawaiian plant species into previously and independently determined threatened categories. Our results indicate that 28% of the Hawaiian taxa, 27% of the species of Arecaceae, 45% of the species of Commelinaceae, 32% of the species of Gesneriaceae, and 35% of the species of Heliconiaceae are Not Threatened and will not need any further evaluation for the preliminary assessment. Species identified here as Potentially Extinct and Potentially Threatened can be further assessed by additional herbarium material and/or conservation specialists for final evaluation using other assessment strategies (e.g., regional and national lists, taxonomic expert assessment, etc.). C1 [Krupnick, Gary A.; Kress, W. John; Wagner, Warren L.] Smithsonian Inst, Dept Bot, US Natl Herbarium, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Krupnick, GA (reprint author), Smithsonian Inst, Dept Bot, US Natl Herbarium, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA. EM krupnickg@si.edu OI Krupnick, Gary/0000-0002-1357-4826 NR 29 TC 9 Z9 12 U1 0 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 EI 1572-9710 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JUN PY 2009 VL 18 IS 6 BP 1459 EP 1474 DI 10.1007/s10531-008-9494-1 PG 16 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 446RD UT WOS:000266137900003 ER PT J AU Coscaron, MC Melo, MC Coddington, J Corronca, J AF Coscaron, M. C. Melo, M. C. Coddington, J. Corronca, J. TI Estimating biodiversity: a case study on true bugs in argentinian wetlands SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Biodiversity estimation; Collecting methods; Heteroptera; Ibera watershed ID SPIDER SPECIES RICHNESS; TROPICAL RAIN-FOREST; DIVERSITY; EARTH AB The species richness and relative abundance of faunas in defined areas are the raw materials in biodiversity science. The research methodology to acquire these data is inventory, and inventory quality depends on a number of parameters, for example collecting methods, season, and collector experience. To assess the ability of rapid inventory techniques to estimate local richness seven collectors sampled the fauna of true bugs in the Ibera watershed (Corrientes, Argentina) with seven methods during early spring, summer, and late summer (December, May, September) of 1 year. Twenty-three families, 225 spp. and 4,678 adults were found. We also applied various statistical techniques to correct the observed data for undersampling bias, which suggested the lower bound of annual heteropteran species richness at Pellegrini was about 250-300 species. Among heteropteran families, the particular inventory methodology was especially efficient in sampling Miridae. C1 [Coscaron, M. C.; Melo, M. C.] Natl Univ La Plata, Fac Ciencias Nat & Museo, Div Entomol, RA-1900 La Plata, Argentina. [Coddington, J.] Smithsonian Inst, Dept Entomol, Nacl Museum Nat Hist, Washington, DC 20560 USA. [Corronca, J.] Univ Nacl Salta, CONICET IEBI, Fac Ciencias Nat, RA-4400 Salta, Argentina. RP Coscaron, MC (reprint author), Natl Univ La Plata, Fac Ciencias Nat & Museo, Div Entomol, RA-1900 La Plata, Argentina. EM mcoscaron@museo.fcnym.unlp.edu.ar OI Melo, Maria Cecilia/0000-0003-4612-452X FU National Geographic Society [7104]; Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) [5261]; Universidad Nacional del Nordeste (UNNE) FX We thank M. Fraga from the Reserva Provincial Ibera, for permission to work in Pellegrini and the forest rangers for help and assistance in the field. We would like to thank the other members of our field team in Pellegrini, M. Chayle, G. Lopez, M. Magnanelli and S. Montemayor, for collecting assistance. Specimens of Alydidae, Miridae, Pentatomidae and Tingidae were identified by D. L. Carpintero, L. Miller, E. Saini and C. Schaefer, to whom we thank. Also, to T. Dobbs and T. Henry for the critical reading of the manuscript. This study was supported in part by grants from National Geographic Society (No. 7104 to Coscaron), Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) (PIP No. 5261 to Coscaron), Universidad Nacional del Nordeste (UNNE). NR 46 TC 11 Z9 13 U1 1 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JUN PY 2009 VL 18 IS 6 BP 1491 EP 1507 DI 10.1007/s10531-008-9515-0 PG 17 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 446RD UT WOS:000266137900005 ER PT J AU Laurance, WF AF Laurance, William F. TI Conserving the hottest of the hotspots Preface SO BIOLOGICAL CONSERVATION LA English DT Editorial Material C1 [Laurance, William F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Laurance, William F.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM laurancew@si.edu RI Laurance, William/B-2709-2012 NR 0 TC 68 Z9 69 U1 2 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD JUN PY 2009 VL 142 IS 6 BP 1137 EP 1137 DI 10.1016/j.biocon.2008.10.011 PG 1 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 446XD UT WOS:000266154000001 ER PT J AU Little, AEF Currie, CR AF Little, Ainslie E. F. Currie, Cameron R. TI Parasites may help stabilize cooperative relationships SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID FUNGUS-GROWING ANTS; YUCCA MOTHS; MICROBE SYMBIOSIS; MUTUALISM; EVOLUTION; AGRICULTURE; COEVOLUTION; PROTECTION; SELECTION; CONFLICT AB Background: The persistence of cooperative relationships is an evolutionary paradox; selection should favor those individuals that exploit their partners (cheating), resulting in the breakdown of cooperation over evolutionary time. Our current understanding of the evolutionary stability of mutualisms (cooperation between species) is strongly shaped by the view that they are often maintained by partners having mechanisms to avoid or retaliate against exploitation by cheaters. In contrast, we empirically and theoretically examine how additional symbionts, specifically specialized parasites, potentially influence the stability of bipartite mutualistic associations. In our empirical work we focus on the obligate mutualism between fungus-growing ants and the fungi they cultivate for food. This mutualism is exploited by specialized microfungal parasites (genus Escovopsis) that infect the ant's fungal gardens. Using sub-colonies of fungus-growing ants, we investigate the interactions between the fungus garden parasite and cooperative and experimentally-enforced uncooperative ("cheating") pairs of ants and fungi. To further examine if parasites have the potential to help stabilize some mutualisms we conduct Iterative Prisoner's Dilemma (IPD) simulations, a common framework for predicting the outcomes of cooperative/non-cooperative interactions, which incorporate parasitism as an additional factor. Results: In our empirical work employing sub-colonies of fungus-growing ants, we found that Escovopsis-infected sub-colonies composed of cheating populations of ants or fungi lost significantly more garden biomass than sub-colonies subjected to infection or cheating (ants or fungi) alone. Since the loss of fungus garden compromises the fitness of both mutualists, our findings suggest that the potential benefit received by the ants or fungi for cheating is outweighed by the increased concomitant cost of parasitism engendered by non-cooperation (cheating). IPD simulations support our empirical results by confirming that a purely cooperative strategy, which is unsuccessful in the classic IPD model, becomes stable when parasites are included. Conclusion: Here we suggest, and provide evidence for, parasitism being an external force that has the potential to help stabilize cooperation by aligning the selfish interests of cooperative partners in opposition to a common enemy. Specifically, our empirical results and IPD simulations suggest that when two mutualists share a common enemy selection can favor cooperation over cheating, which may help explain the evolutionary stability of some mutualisms. C1 [Little, Ainslie E. F.; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Little, Ainslie E. F.; Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Little, Ainslie E. F.; Currie, Cameron R.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. RP Currie, CR (reprint author), Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM ainslie.little@gmail.com; currie@bact.wisc.edu FU NSF IRCEB [DEB-0110073]; NSF CAREER [DEB-747002]; NSF Doctoral Dissertation Improvement Grant [DEB-0608078] FX We are grateful to STRI and ANAM of the Republic of Panama for facilitating the research and granting collecting permits. For valuable logistical support we thank: M. Bergsbaken, M. Cafaro, S. Covington, P. Foley, S. Ingram, M. Leone, H. Reynolds, and M. Tourtellot. We are thankful to K. Boomsma, J. Bull, E. Caldera, N. Gerardo, K. Grubbs, H. Goodrich- Blair, S. Hoover, J. Kelly, A. Pinto, M. Poulsen, G. Roberts, R. Steffensen, and S. West for invaluable comments on this study and/ or paper. This work was supported by NSF IRCEB grant DEB-0110073 to CRC, NSF CAREER grant DEB-747002 to CRC, and NSF Doctoral Dissertation Improvement Grant DEB-0608078 to CRC and AEFL. NR 51 TC 10 Z9 10 U1 11 U2 38 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 JUN 1 PY 2009 VL 9 AR 124 DI 10.1186/1471-2148-9-124 PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 467QZ UT WOS:000267758800003 PM 19486536 ER PT J AU Petaev, MI AF Petaev, Michail I. TI The GRAINS thermodynamic and kinetic code for modeling nebular condensation SO CALPHAD-COMPUTER COUPLING OF PHASE DIAGRAMS AND THERMOCHEMISTRY LA English DT Article DE Thermodynamics; Equilibrium; Grain growth; Condensation; Solar nebula ID SOLAR NEBULA; CHEMICAL FRACTIONATIONS; METAL GRAINS; MULTICOMPONENT PYROXENES; CARBONACEOUS CHONDRITES; MIXING PROPERTIES; PHASE-RELATIONS; FENI METAL; SYSTEM; OLIVINE AB The GRAINS thermodynamic and kinetic code for modeling condensation and grain growth in the solar nebula is described. The code calculates CWPI-type (Condensation With Partial Isolation) equilibrium partitioning of 33 chemical elements among 242 gaseous and 520 condensed phases, and growth in the nebula of metal and olivine grains by condensation from the nebular gas accompanied by diffusional redistribution of major and trace elements in those grains. Several examples of the GRAINS application to cosmochemical problems are briefly discussed. (C) 2008 Elsevier Ltd. All rights reserved. C1 [Petaev, Michail I.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Petaev, MI (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St,Hoffman 208, Cambridge, MA 02138 USA. EM mpetaev@fas.harvard.edu FU NASA [NNG05G166G, NNX08AH79G] FX I deeply appreciate advice, help, and support of Dr. John A. Wood who had started the development of these models and encouraged me to continue. Valuable comments by two anonymous reviewers and the editor Z.-K. Liu helped to improve the paper and are greatly appreciated. This work was supported by NASA grants NNG05G166G and NNX08AH79G. NR 74 TC 3 Z9 3 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0364-5916 J9 CALPHAD JI Calphad-Comput. Coupling Ph. Diagrams Thermochem. PD JUN PY 2009 VL 33 IS 2 BP 317 EP 327 DI 10.1016/j.calphad.2008.12.001 PG 11 WC Thermodynamics; Chemistry, Physical; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Thermodynamics; Chemistry; Materials Science; Metallurgy & Metallurgical Engineering GA 457AS UT WOS:000266897700007 ER PT J AU Rye, O AF Rye, Owen TI Critical Care Required? Response SO CERAMICS-ART AND PERCEPTION LA English DT Editorial Material C1 [Rye, Owen] Smithsonian Inst, Washington, DC 20560 USA. [Rye, Owen] Australian Natl Univ, Canberra, ACT 0200, Australia. RP Rye, O (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CERAMICS-ART & PERCEPTION PTY LTD PI SHERIDAN PA 23 N SCOTT ST, STE 16, SHERIDAN, WYOMING 82801 USA SN 1035-1841 J9 CERAMICS-ART PERCEPT JI Ceramics-Art Percept. PD JUN-SEP PY 2009 IS 76 BP 106 EP 107 PG 2 WC Art SC Art GA 453LY UT WOS:000266613200027 ER PT J AU Paquette, A Hawryshyn, J Senikas, AV Potvin, C AF Paquette, Alain Hawryshyn, Jessica Senikas, Alexandra Vyta Potvin, Catherine TI Enrichment Planting in Secondary Forests: a Promising Clean Development Mechanism to Increase Terrestrial Carbon Sinks SO ECOLOGY AND SOCIETY LA English DT Article DE biodiversity; carbon sequestration; clean development mechanism; enrichment planting; indigenous communities; payments for environmental services; secondary forests ID HUMID TROPICAL REGION; ENVIRONMENTAL SERVICES; COSTA-RICA; PLANTATION FORESTRY; SPECIES LOSS; LAND-USE; BIODIVERSITY; CONSERVATION; MANAGEMENT; PAYMENTS AB With the increasing need to reduce greenhouse gas concentrations, afforestation and reforestation (A/R) projects are being implemented under the Kyoto Clean Development Mechanism (CDM) and under the voluntary carbon (C) market. The specific objective of A/R C projects is to enhance terrestrial sinks. They could also provide low-income communities in developing countries with a source of revenue, as well as a number of ecological and social services. However, feasibility issues have hindered implementation of A/R CDMs. We propose enrichment planting (EP) in old fallow using high-value native timber species as a land-use alternative and a small-scale C projects opportunity. We present EP in the context of ongoing work in a poor indigenous community in eastern Panama. We consider economic risks and advantages and concordance with existing modalities under the compliance market. The potential storage capacity for EP at the site of our study was similar to 113 Mg C ha(-1), which is comparable to other land uses with high C storage, such as industrial teak plantations and primary forest. Because secondary forests show high aboveground biomass production, C projects using EP could harness large amounts of atmospheric C while improving diversity. Carbon projects using EP can also provide high levels of social, cultural, and ecological services by planting native tree species of traditional importance to local communities and preserving most of the secondary forest's ecological attributes. Therefore, EP planting could be considered as a way to promote synergies between two UN Conventions: climate change and biodiversity. C1 [Paquette, Alain] Univ Quebec, Ctr Etude Foret, Montreal, PQ H3C 3P8, Canada. [Hawryshyn, Jessica; Senikas, Alexandra Vyta; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 2T5, Canada. [Hawryshyn, Jessica; Senikas, Alexandra Vyta; Potvin, Catherine] McGill Univ, McGill Sch Environm, Montreal, PQ H3A 2T5, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Panama. RP Paquette, A (reprint author), Univ Quebec, Ctr Etude Foret, Montreal, PQ H3C 3P8, Canada. RI Paquette, Alain/F-4919-2011 FU McGill Panama Field Study Semester; NSERC FX The authors wish to express their deepest thanks to the community of Ipet-Embea. Other thanks to M. Boenke, J. L. Bonilla, G. U. Cabrera, S. Hutchinson, R. Ibanez, O. Ramos, and to J. Hall and the staff at PRORENA for their help. This work was carried out in part by J. H. and A. V. S. as a requirement for the McGill Panama Field Study Semester. NSERC financial support to C. P. and A. P. is acknowledged. NR 70 TC 17 Z9 17 U1 2 U2 18 PU RESILIENCE ALLIANCE PI WOLFVILLE PA ACADIA UNIV, BIOLOGY DEPT, WOLFVILLE, NS B0P 1X0, CANADA SN 1708-3087 J9 ECOL SOC JI Ecol. Soc. PD JUN PY 2009 VL 14 IS 1 AR 31 PG 15 WC Ecology; Environmental Studies SC Environmental Sciences & Ecology GA 468TY UT WOS:000267846300041 ER PT J AU Kuntner, M Coddington, JA Schneider, JM AF Kuntner, Matjaz Coddington, Jonathan A. Schneider, Jutta M. TI INTERSEXUAL ARMS RACE? GENITAL COEVOLUTION IN NEPHILID SPIDERS (ARANEAE, NEPHILIDAE) SO EVOLUTION LA English DT Article DE Cryptic female choice; monogamy; morphological complexity; polyandry; reproductive character displacement; sexual conflict; sexually antagonistic coevolution; sperm competition ID ORB-WEB SPIDER; REPRODUCTIVE CHARACTER DISPLACEMENT; SEXUALLY ANTAGONISTIC COEVOLUTION; SPERM COMPETITION; MATE CHOICE; MORPHOLOGICAL COMPLEXITY; CANNIBALISTIC SPIDER; PLUMIPES ARANEOIDEA; SIZE DIMORPHISM; WATER STRIDERS AB Genital morphology is informative phylogenetically and strongly selected sexually. We use a recent species-level phylogeny of nephilid spiders to synthesize phylogenetic patterns in nephilid genital evolution that document generalized conflict between male and female interests. Specifically, we test the intersexual coevolution hypothesis by defining gender-specific indices of genital complexity that summarize all relevant and phylogenetically informative traits. We then use independent contrasts to show that male and female genital complexity indices correlate significantly and positively across the phylogeny rather than among sympatric sister species, as predicted by reproductive character displacement. In effect, as females respond to selection for fecundity-driven fitness via giantism and polyandry (perhaps responding to male-biased effective sex ratios), male mechanisms evolve to monopolize females (male monogamy) via opportunistic mating, pre- and postcopulatory mate guarding, and/or plugging of female genitalia to exclude subsequent suitors. In males morphological symptoms of these phenomena range from self-mutilated genitalia to total castration. Although the results are compatible with both recently favored sexual selection hypotheses, sexually antagonistic coevolution, and cryptic female choice, the evidence of strong intersexual conflict and genitalic damage in both sexes is more easily explained as sexually antagonistic coevolution due to an evolutionary arms race. C1 [Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, SI-1001 Ljubljana, Slovenia. [Kuntner, Matjaz; Coddington, Jonathan A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Schneider, Jutta M.] Univ Hamburg, Biozentrum Grindel, D-20146 Hamburg, Germany. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2,POB 306, SI-1001 Ljubljana, Slovenia. EM kuntner@gmail.com; Coddington@si.edu; js@gilgamesh.de RI Schneider, Jutta /G-3727-2010 FU Slovenian Research Agency [Z1-7082-0618]; European Commission [MIRG-CT-2005 036536]; U. S. National Science Foundation [EAR-0228699] FX We thank W. Eberhard, G. Arnqvist, I. Agnarsson, L. May-Collado, and S. Kralj-Fiser for constructive comments on the manuscript and on the analysis. This research was supported by the Slovenian Research Agency (postdoctoral grant Z1-7082-0618 to MK and USA-Slovenian bilateral grant to MK and JC) by the European Commission's 6th Framework Programme (MIRG-CT-2005 036536 grant to MK), and the U. S. National Science Foundation (EAR-0228699 to JC). NR 85 TC 68 Z9 70 U1 3 U2 48 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUN PY 2009 VL 63 IS 6 BP 1451 EP 1463 DI 10.1111/j.1558-5646.2009.00634.x PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 448MZ UT WOS:000266268000006 PM 19492993 ER PT J AU Melo, MC Salazar, C Jiggins, CD Linares, M AF Melo, Maria C. Salazar, Camilo Jiggins, Chris D. Linares, Mauricio TI ASSORTATIVE MATING PREFERENCES AMONG HYBRIDS OFFERS A ROUTE TO HYBRID SPECIATION SO EVOLUTION LA English DT Article DE Homoploid speciation; introgression; mating preference; pleiotropy; transgressive segregation ID REPRODUCTIVE ISOLATION; HELICONIUS BUTTERFLIES; SEXUAL SELECTION; WILD SUNFLOWERS; COLOR PATTERN; MIMICRY; HYBRIDIZATION; EVOLUTION; MELPOMENE AB Homoploid speciation generates species without a change in chromosome number via introgressive hybridization and has been considered rare in animals. Heliconius butterflies exhibit bright aposematic color patterns that also act as cues in assortative mating. Heliconius heurippa has a color pattern that can be recreated by introgression of the H. melpomene red band into an H. cydno genetic background. Wild H. heurippa males show assortative mating based on color pattern and we here investigate the origin of this preference by studying first-generation backcross hybrids between H. melpomene and H. cydno that resemble H. heurippa. These hybrids show assortative mating preferences, showing a strong preference for their own color pattern over that of either parental species. This is consistent with a genetic basis to wing pattern preference and implies, first, that assortative mating preferences would facilitate the initial establishment of a homozygous hybrid color pattern by increasing the likelihood that early generation hybrids mate among themselves. Second, once established such a lineage would inherit assortative mating preferences that would lead to partial reproductive isolation from parental lineages. C1 [Melo, Maria C.; Linares, Mauricio] Univ Los Andes, Inst Genet, Bogota, Colombia. [Salazar, Camilo] Smithsonian Trop Res Inst, Panama City, Panama. [Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Melo, MC (reprint author), Univ Los Andes, Inst Genet, Carrera 1E 18A-10,POBox 4976, Bogota, Colombia. EM mar-melo@uniandes.edu.co; salazarc@si.edu; c.jiggins@zoo.cam.ac.uk; mlinares@uniandes.edu.co RI Jiggins, Chris/B-9960-2008; Salazar, camilo/A-1647-2010; Linares, Mauricio/I-3509-2016 OI Jiggins, Chris/0000-0002-7809-062X; Salazar, camilo/0000-0001-9217-6588; Linares, Mauricio/0000-0002-1021-0226 FU Banco de la Republica [2297]; Los Andes University; Fondo Colombiano de Invesigaciones Cientificas y Proyectos Especiales Francisco Jose de Caldas [120440520138]; Royal Society; BBSRC; Leverhulme Trust FX We would like to thank Banco de la Republica grant 2297, Los Andes University science faculty, and Fondo Colombiano de Invesigaciones Cientificas y Proyectos Especiales Francisco Jose de Caldas COLCIENCIAS grant 120440520138 for funding to CS and ML. CJ was funded by the Royal Society, BBSRC and the Leverhulme Trust. NR 29 TC 39 Z9 41 U1 5 U2 21 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0014-3820 J9 EVOLUTION JI Evolution PD JUN PY 2009 VL 63 IS 6 BP 1660 EP 1665 DI 10.1111/j.1558-5646.2009.00633.x PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 448MZ UT WOS:000266268000023 PM 19492995 ER PT J AU Seid, MA Brown, BV AF Seid, Marc A. Brown, Brian V. TI A NEW HOST ASSOCIATION OF COMMOPTERA SOLENOPSIDIS (DIPTERA: PHORIDAE) WITH THE ANT PHEIDOLE DENTATA (HYMENOPTERA: FORMICIDAE) AND BEHAVIORAL OBSERVATIONS SO FLORIDA ENTOMOLOGIST LA English DT Article DE Pheidole; Solenopsis; social parasitism; phorid; Commoptera ID ATTA-CEPHALOTES HYMENOPTERA; IMPORTED FIRE ANTS; DIVISION-OF-LABOR; FLIES DIPTERA; PSEUDACTEON-TRICUSPIS; DEFENSE BEHAVIOR; GENUS PHEIDOLE; ARMY ANTS; PARASITOIDS; FLY AB Phorid flies are well known myrmecophilic organisms and are often parasitoids of ants. In some cases, phorids live commensally with ants, with the colony offering protection and/or feeding opportunities. In this study we examined the phorid Commoptera solenopsidis in association with a new host species, Pheidole dentata. An ethogram was performed describing the fly and its association with different P. dentata castes. The flies spent most of their time performing grooming behaviors, allogrooming ants, or self-grooming and most commonly were associated with the major workers. We discuss the significance of this association as well as the possible evolutionary driving force behind C. solenopsidis having multiple hosts. C1 [Seid, Marc A.] Smithsonian Trop Res Inst, Balboa, Panama. [Brown, Brian V.] Nat Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA. RP Seid, MA (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. FU Levinson Foundation FX We thank Dr. James F. A. Traniello for support in the early part of this work and the Levinson Foundation for providing funding. We thank Lloyd Davis for help in field collecting the specimens and Dr. Sanford Porter for use of his laboratory while in the field. We thank William Weislo for providing research space and helpful discussions. NR 22 TC 2 Z9 2 U1 1 U2 7 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 J9 FLA ENTOMOL JI Fla. Entomol. PD JUN PY 2009 VL 92 IS 2 BP 309 EP 313 PG 5 WC Entomology SC Entomology GA 457VP UT WOS:000266962700015 ER PT J AU Liu, HP Hershler, R AF Liu, H. -P. Hershler, R. TI Genetic diversity and population structure of the threatened Bliss Rapids snail (Taylorconcha serpenticola) SO FRESHWATER BIOLOGY LA English DT Article DE dams; microsatellites; population structure; Snake River; Taylorconcha serpenticola ID SPRING SNAIL; F-STATISTICS; DIFFERENTIATION; RIVER; RECONSTRUCTION; SUBDIVISION; DISPERSAL; LANDSCAPE; PATTERNS; DISTANCE AB 1. The Bliss Rapids snail is a federally listed yet poorly known small caenogastropod which lives in the Snake River drainage (main stem river and spring-fed tributaries) of south-central Idaho. The construction of three large dams along this portion of the Snake River during the 20th century is thought to have fragmented a single, ancestral population of this species into genetically isolated subunits that are vulnerable to extinction. We assessed variation of 11 microsatellite loci within and among 29 samples (820 snails) from across the entire range of the Bliss Rapids snail to assess genetic structure and test whether habitat fragmentation resulting from dam construction has impacted population connectivity. 2. The overall F(ST) (0.15133, P < 0.05) and pairwise comparisons among samples (384/406 significant) indicated extensive population subdivision in general. A consistent trend of isolation by distance trend was not detected by Mantel tests. We found no evidence of reduced genetic diversity attributable to segmentation of the Snake River, and genetic variation among portions of drainage separated by the dams was not significant. Population structuring in spring-tributary habitats was considerably greater than in the main stem river as evidenced by differences in F(ST) (0.18370, 0.06492) and the number of private alleles detected (16, 4), and by the results of an assignment test (69.4%, 58.7% correctly classified to sample of origin) and Bayesian genetic clustering algorithm. 3. Our results provide no evidence that dam construction has genetically impacted extant populations of the Bliss Rapids snail. We speculate that the generally weaker genetic structuring of riverine populations of this species is a result of passive dispersal within the water column, which may enable occasional passage through the dams. The somewhat stronger structuring observed in a portion of the river (Shoshone reach) which receives discharge from many springs may be due to local mixing of main stem and more highly differentiated tributary populations. Our findings parallel recent, genetically based studies of other western North American freshwater gastropods that also demonstrate complex population structure that conflicts with traditional concepts of dispersal ability and sensitivity to putative barriers. C1 [Hershler, R.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, H. -P.] Metropolitan State Coll, Dept Biol, Denver, CO 80204 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu FU Idaho Power Company [1600] FX Barry Bean, William Clark and Mike Stephenson (Idaho Power Company) provided a large amount of field and logistical assistance. Mike Radko (Idaho Power Company) calculated the stream distances between sampling sites and Molly Ryan (Smithsonian Institution) assisted with preparation of the figures. Tom Quinn (University of Denver) and Sara Oyler-McCance (United States Geological Survey) generously shared bench space and equipment in the Rocky Mountain Center for Conservation Genetics and Systematics. We thank two anonymous reviewers for providing useful comments of an earlier version of this study. This project was supported by a contract from the Idaho Power Company (Award #1600). NR 51 TC 8 Z9 8 U1 1 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0046-5070 J9 FRESHWATER BIOL JI Freshw. Biol. PD JUN PY 2009 VL 54 IS 6 BP 1285 EP 1299 DI 10.1111/j.1365-2427.2009.02175.x PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 443TW UT WOS:000265934700011 ER PT J AU Poisbleau, M Demongin, L Angelier, F Dano, S Lacroix, A Quillfeldt, P AF Poisbleau, M. Demongin, L. Angelier, F. Dano, S. Lacroix, A. Quillfeldt, P. TI What ecological factors can affect albumen corticosterone levels in the clutches of seabirds? Timing of breeding, disturbance and laying order in rockhopper penguins (Eudyptes chrysocome chrysocome) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Albumen corticosterone; Maternal investment; Disturbance; Reversed hatching asynchrony; Laying sequence; Laying date; Southern rockhopper penguins (Eudyptes chrysocome chrysocome) ID GALLUS-GALLUS-DOMESTICUS; OFFSPRING SEX-RATIO; EMBRYONIC-DEVELOPMENT; MAGELLANIC PENGUINS; YOLK CORTICOSTERONE; MATERNAL HORMONES; PRENATAL EXPOSURE; CRESTED PENGUINS; EGG-YOLK; BIRDS AB Female birds deposit corticosterone into their eggs. Elevated concentrations of this hormone may interfere with the development of their offspring, and mothers should thus regulate corticosterone levels deposited into the eggs adaptively. However, if females are unable to regulate deposition, then the corticosterone concentration in eggs should reflect that in female plasma and should be influenced by stressors to the females. We measured corticosterone levels in the albumen of rockhopper penguins, and assessed their relationship with hatching order, human disturbance and laying date. Rockhopper penguins (Eudyptes chrysocome chrysocome) lay two eggs, of which the second egg (B-egg) is larger and hatches faster than the first egg (A-egg). The chick hatching from the B-egg is also much more likely to survive than its sibling. Albumen corticosterone concentrations were lower in B-eggs. However, as B-eggs contained more albumen than A-eggs, the total corticosterone deposited in the albumen was not significantly different between the two eggs. Daily disturbance by human observers during albumen production did not influence albumen corticosterone levels. Laying date had an effect on total albumen corticasterone through a higher albumen mass. However, we observed a high individual component in the composition of eggs from the same clutch. Thus, more work is required to explore the hypotheses of passive versus active transfer to eggs and to understand the adaptive value of contrary effects on the amount and concentration of corticosterone. (C) 2009 Elsevier Inc. All rights reserved. C1 [Poisbleau, M.; Demongin, L.; Quillfeldt, P.] Max Planck Inst Ornithol, D-78315 Radolfzell am Bodensee, Germany. [Angelier, F.] Smithsonian Migratory Bird Ctr, Smithsonian Inst, Washington, DC 20008 USA. [Dano, S.; Lacroix, A.] CNRS, UPR 1934, Ctr Etudes Biol Chize, F-79360 Beauvoir Sur Niort, France. RP Poisbleau, M (reprint author), Univ Antwerp, Dept Biol Ethol, Campus Drie Eiken,Univ Pl 1, B-2610 Antwerp, Belgium. EM Maud.Poisbleau@ua.ac.be RI Quillfeldt, Petra/A-9549-2009; Poisbleau, Maud/B-9968-2014 OI Quillfeldt, Petra/0000-0002-4450-8688; Poisbleau, Maud/0000-0002-0729-3251 NR 39 TC 15 Z9 15 U1 0 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD JUN PY 2009 VL 162 IS 2 BP 139 EP 145 DI 10.1016/j.ygcen.2009.03.022 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 449HG UT WOS:000266320800003 PM 19341737 ER PT J AU Amelia, M Logan, V AF Amelia, M. Logan, V. TI Trace element contents in the Smithsonian reference materials collection: A program to continue Eugene Jarosewich's legacy SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Amelia, M.; Logan, V.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A788 EP A788 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902035 ER PT J AU Cora, I Weiszburg, TG Post, J AF Cora, I. Weiszburg, T. G. Post, J. TI Application of micro X-ray diffraction on lamellar, black shale related Mn ore, Urkut, Hungary SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Cora, I.; Weiszburg, T. G.] Eotvos Lorand Univ, Budapest, Hungary. [Post, J.] Smithsonian Inst, Dept Marine Sci, Washington, DC 20560 USA. EM coraildiko@gmail.com NR 1 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A243 EP A243 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900498 ER PT J AU Fischer, TB Heaney, PJ Post, JE Brantley, SL Tien, M AF Fischer, Timothy B. Heaney, Peter J. Post, Jeffrey E. Brantley, Susan L. Tien, Ming TI Using time-resolved synchrotron XRD and XAS to analyze Mn oxide dissolution in response to biotic and abiotic stimuli SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Fischer, Timothy B.; Heaney, Peter J.; Brantley, Susan L.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, Jeffrey E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Tien, Ming] Penn State Univ, Dept Biochem & Mol Biol, University Pk, PA 16802 USA. EM tfischer@geosc.psu.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A380 EP A380 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229900773 ER PT J AU Halfar, J Hetzinger, S Zack, T Simon, K Kronz, A Steneck, RS Adey, W Lebednik, PA Schone, BR Fietzke, J AF Halfar, J. Hetzinger, S. Zack, T. Simon, K. Kronz, A. Steneck, R. S. Adey, W. Lebednik, P. A. Schoene, B. R. Fietzke, J. TI High-resolution analysis of trace elements in encrusting coralline red algae by laser ablation ICP-MS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Halfar, J.; Hetzinger, S.] Univ Toronto, CPS Dept, Toronto, ON M5S 1A1, Canada. [Zack, T.; Schoene, B. R.] Johannes Gutenberg Univ Mainz, Inst Geosci, D-6500 Mainz, Germany. [Simon, K.; Kronz, A.] Geowissensch Zentrum, Gottingen, Germany. [Steneck, R. S.] Univ Maine, Darling Marine Ctr, Orono, ME 04469 USA. [Adey, W.] Smithsonian Inst, Washington, DC 20560 USA. [Fietzke, J.] IFM GEOMAR, Kiel, Germany. EM jochen.halfar@utoronto.ca RI Zack, Thomas/C-6153-2009; Schone, Bernd/B-6294-2011; Adey, Walter/G-2858-2011; Halfar, Jochen/C-7317-2014; Hetzinger, Steffen/B-5778-2016 NR 0 TC 0 Z9 0 U1 2 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A487 EP A487 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229901206 ER PT J AU Martin, RV van Donkelaar, A Lee, C Lamsal, L AF Martin, Randall V. van Donkelaar, Aaron Lee, Chulkyu Lamsal, Lok TI Satellite remote sensing estimate of global ground-level aerosol concentrations and precursors SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Martin, Randall V.; van Donkelaar, Aaron; Lee, Chulkyu; Lamsal, Lok] Dalhousie Univ, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM randall.martin@dal.ca RI Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 NR 0 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A839 EP A839 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902138 ER PT J AU Penniston-Dorland, SC Ash, RD Piccoli, PM Sorensen, SS AF Penniston-Dorland, S. C. Ash, R. D. Piccoli, P. M. Sorensen, S. S. TI Lithium as a tracer of fluids in subduction zones: The Franciscan Complex, CA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Penniston-Dorland, S. C.; Ash, R. D.; Piccoli, P. M.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Sorensen, S. S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. EM sarahpd@umd.edu NR 0 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1011 EP A1011 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229902482 ER PT J AU Stubbs, JE Post, JE Elbert, DC Heaney, PJ Veblen, DR AF Stubbs, Joanne E. Post, Jeffrey E. Elbert, David C. Heaney, Peter J. Veblen, David R. TI Uranyl phosphate sheet reconstruction during dehydration of metatorbernite [Cu(UO2)(2)(PO4)(2)center dot 8H(2)O] SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND ID META-AUTUNITE C1 [Stubbs, Joanne E.; Elbert, David C.; Veblen, David R.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM jstubbs1@jhu.edu; postj@si.edu; heaney@geosc.psu.edu RI Stubbs, Joanne/F-9710-2013 OI Stubbs, Joanne/0000-0002-8509-2009 NR 2 TC 0 Z9 0 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 SU S BP A1285 EP A1285 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903257 ER PT J AU Wall, AJ Heaney, PJ Brantley, SL Mathur, R Post, JE AF Wall, A. J. Heaney, P. J. Brantley, S. L. Mathur, R. Post, J. E. TI Copper isotope fractionation during leach layer development on Cu-sulfide minerals SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT 19th Annual VM Goldschmidt Conference CY JUN 21, 2009 CL Davos, SWITZERLAND C1 [Wall, A. J.; Heaney, P. J.; Brantley, S. L.] Penn State Univ, Ctr Environm Kinet Anal, Dept Geosci, University Pk, PA 16802 USA. [Mathur, R.] Juniata Coll, Dept Geol, Huntingdon, PA 16652 USA. [Post, J. E.] Smithsonian NMNH, Dept Mineral Sci, Washington, DC 20013 USA. EM awall@geosc.psu.edu RI mathur, ryan/A-5278-2010 NR 0 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2009 VL 73 IS 13 BP A1402 EP A1402 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 460YS UT WOS:000267229903491 ER PT J AU Ryabchun, S Tong, CYE Paine, S Lobanov, Y Blundell, R Gol'tsman, G AF Ryabchun, Sergey Tong, Cheuk-yu Edward Paine, Scott Lobanov, Yury Blundell, Raymond Gol'tsman, Gregory TI Temperature Resolution of an HEB Receiver at 810 GHz SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Allan variance; HEB mixer; heterodyne spectroscopy; receiver temperature resolution AB We present the results of direct measurements of the temperature resolution of an HEB receiver operating at 810 GHz, in both continuum and spectroscopic modes. In the continuum mode, the input of the receiver was switched between black bodies with different physical temperatures. With a system noise temperature of around 1100 K, the receiver was able to resolve loads which differed in temperature by about 1 K over an integration time of 5 seconds. This resolution is significantly worse than the value of 0.07 K given by the radiometer equation. In the spectroscopic mode, a gas cell filled with carbonyl sulphide (OCS) gas was used and the emission line at 813.3537060 GHz was measured using the receiver in conjunction with a digital spectrometer. From the observed spectra, we determined that the measurement uncertainty of the equivalent emission temperature was 2.8 K for an integration time of 0.25 seconds and a spectral resolution of 12 MHz, compared to a 1.4 K temperature resolution given by the radiometer equation. This relative improvement is due to the fact that at short integration times the contribution from 1/f noise and drift are less dominant. In both modes, the temperature resolution was improved by about 40% with the use of a feedback loop which adjusted the level of an injected microwave radiation to maintain a constant operating current of the HEB mixer. This stabilization scheme has proved to be very effective to keep the temperature resolution of the HEB receiver to close to the theoretical value given by the radiometer equation. C1 [Ryabchun, Sergey; Gol'tsman, Gregory] Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119992, Russia. [Ryabchun, Sergey; Tong, Cheuk-yu Edward; Paine, Scott; Lobanov, Yury; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ryabchun, S (reprint author), Moscow State Pedag Univ, Dept Phys & Informat Technol, Moscow 119992, Russia. EM sryabchun@rplab.ru; etong@cfa.harvard.edu; spaine@cfa.harvard.edu; ylobanov@cfa.har-vard.edu; rblundell@cfa.harvard.edu; goltsman@rplab.ru RI Lobanov, Yury/A-3615-2014; OI Lobanov, Yury/0000-0001-7801-0223; Tong, Edward/0000-0002-7736-4203; Paine, Scott/0000-0003-4622-5857 NR 8 TC 4 Z9 4 U1 1 U2 8 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 293 EP 296 DI 10.1109/TASC.2009.2019585 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000040 ER PT J AU Tong, CYE Hedden, A Blundell, R AF Tong, Cheuk-yu Edward Hedden, Abigail Blundell, Raymond TI Gain Expansion and Compression of SIS Mixers SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY LA English DT Article; Proceedings Paper CT Applied Superconductivity Conference CY AUG 17-22, 2008 CL Chicago, IL SP ATI Wah Chang, Coalit Commercial Applicat Superconductors, CryoZone, GE Global Res Ctr, IEEE Council Superconductiv, IEEE Magnet Soc, PHPK Technologies, SuperPower Inc, Teax Ctr Superconductiv, Univ Houston DE Gain measurements; submillimeter wave measurements; superconductor-insulator-superconductor mixers ID SATURATION AB It is a well known fact that SIS mixers exhibit gain compression when the output IF voltage swing becomes non-negligible compared to the width of the photon step. In this paper, we show that under certain circumstances, SIS mixers can also exhibit the inverse phenomenon-gain expansion. This non-linear behavior has been observed experimentally when the output power-voltage curve of an SIS mixer has a double peak feature over the photon step. In this case, if the device is biased at the valley position between the two peaks, the conversion gain of the mixer will increase with input signal power. Consequently, the noise temperature of the mixer deduced from a Y-factor measurement will be artificially reduced. Two different experimental methods have been used to characterize the linearity of SIS mixers. The accuracies of both methods are analysed. C1 [Tong, Cheuk-yu Edward; Hedden, Abigail; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.harvard.edu; ahedden@cfa.har-vard.edu; rblundell@cfa.harvard.edu OI Tong, Edward/0000-0002-7736-4203 NR 7 TC 1 Z9 1 U1 0 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1051-8223 J9 IEEE T APPL SUPERCON JI IEEE Trans. Appl. Supercond. PD JUN PY 2009 VL 19 IS 3 BP 309 EP 312 DI 10.1109/TASC.2009.2019102 PG 4 WC Engineering, Electrical & Electronic; Physics, Applied SC Engineering; Physics GA 474KK UT WOS:000268282000044 ER PT J AU Reid, MJ AF Reid, Mark J. TI IS THERE A SUPERMASSIVE BLACK HOLE AT THE CENTER OF THE MILKY WAY? SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Review DE Supermassive black hole; Sgr A*; galactic center ID SAGITTARIUS-A-ASTERISK; STELLAR PROPER MOTIONS; SMALL-SCALE STRUCTURE; GALACTIC-CENTER; RADIO-SOURCE; IONIZED-GAS; INTENSITY VARIATIONS; VELOCITY DISPERSION; HYPERVELOCITY STARS; LUMINOUS QUASARS AB This review outlines the observations that now provide an overwhelming scientific case that the center of the Milky Way harbors a supermassive black hole. Observations at infrared wavelength trace stars that orbit about a common focal position and require a central mass (M) of 4 x 10(6) M(circle dot) within a radius of 100 AU. Orbital speeds have been observed to exceed 5,000 km s(-1). At the focal position there is an extremely compact radio source (Sgr A*), whose apparent size is near the Schwarzschild radius (2GM/c(2)). This radio source is motionless at the similar to 1 km s(-1) level at the dynamical center of the Galaxy. The mass density required by these observations is now approaching the ultimate limit of a supermassive black hole within the last stable orbit for matter near the event horizon. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mreid@cfa.harvard.edu NR 105 TC 28 Z9 27 U1 0 U2 2 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 JUN PY 2009 VL 18 IS 6 BP 889 EP 910 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 469BC UT WOS:000267868900001 ER PT J AU Hacker, BC AF Hacker, Barton C. TI Mr. Gatling's Terrible Marvel: The Gun That Changed Everything and the Misunderstood Genius Who Invented It. SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 [Hacker, Barton C.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 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 JUN PY 2009 VL 96 IS 1 BP 204 EP 204 PG 1 WC History SC History GA 460GI UT WOS:000267175800037 ER PT J AU Phillips, SC Speakman, RJ AF Phillips, S. Colby Speakman, Robert J. TI Initial source evaluation of archaeological obsidian from the Kuril Islands of the Russian Far East using portable XRF SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Kuril Islands; Obsidian; XRF; Exchange networks; Hokkaido; Kamchatka ID OKHOTSK SEA; SOCIAL NETWORKS; IODIDE DETECTOR; SILICATE ROCKS; EDXRF ANALYSIS; SOUTHERN PERU; EL-HIBEH; ORGANIZATION; PREHISTORY; SAMPLES AB Obsidian artifacts recently have been recovered from 18 archaeological sites on eight islands across the Kuril Island archipelago in the North Pacific Ocean, suggesting a wide-ranging distribution of obsidian throughout the island chain over the last 2,500 years. Although there are no geologic sources of obsidian in the Kurils that are known to have been used prehistorically, sources exist in Hokkaido, Japan, and Kamchatka, Russia, the southern and northern geographic regions respectively from which obsidian may have entered the Kuril Islands. This paper reports on the initial sourcing attempt of Kuril Islands obsidian through the analysis of 131 obsidian artifacts. Data from this research were generated through the application of portable XRF technology, and are used to address research questions concerning prehistoric mobility, exchange, and social networking in the Kuril Islands. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Phillips, S. Colby] Univ Washington, Dept Anthropol, Seattle, WA 98195 USA. [Speakman, Robert J.] Smithsonian Inst, Museum Conservat Inst, Washington, DC 20560 USA. RP Phillips, SC (reprint author), Univ Washington, Dept Anthropol, Box 353100, Seattle, WA 98195 USA. EM colbyp@u.washington.edu OI Speakman, Robert/0000-0003-2063-154X NR 66 TC 50 Z9 50 U1 0 U2 10 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD JUN PY 2009 VL 36 IS 6 BP 1256 EP 1263 DI 10.1016/j.jas.2009.01.014 PG 8 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 433GY UT WOS:000265193500007 ER PT J AU Birnboim, Y Loeb, A AF Birnboim, Yuval Loeb, Abraham TI The kinetic Sunyaev-Zel'dovich effect of the milky way halo SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE Sunyaev-Zeldovich effect; galaxy evolution ID HIGH-VELOCITY CLOUDS; SENSITIVITY HI SURVEY; FINAL DATA RELEASE; X-RAY-ABSORPTION; LOCAL GROUP; GALAXY FORMATION; GALACTIC HALO; DARK-MATTER; MASSIVE GALAXIES; ALPHA-EMISSION AB We calculate the expected imprint of the ionized gas in the Milky-Way halo on the Cosmic Microwave Background (CMB) through the kinetic Sunyaev-Zel'dovich (kSZ) effect. Unlike other Galactic foregrounds, the halo kSZ signature covers the full sky, generates anisotropies on large angular scales, is not accompanied by spectral distortions, and could therefore be confused with primordial CMB anisotropies. We construct theoretical models for various halo components, including smooth diffuse gas, filaments of cold inflowing gas and high velocity clouds. We find that the kSZ effect for all components is above the sensitivity of the Planck satellite, over a range of angular scales. However, the typical halo contribution is well below the cosmic variance noise in the primordial CMB power spectrum. High velocity clouds could dominate the halo contribution and better observational data is required to mask them out. We derive expected kSZ maps based on existing data from tracers of the halo gas distribution, such as 21cm maps of neutral hydrogen and H-alpha maps of recombining gas. The cross-correlation of these maps with the WMAP5 data does not yield any statistically significant signal. C1 [Birnboim, Yuval; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Birnboim, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ybirnboim@cfa.harvard.edu; aloeb@cfa.harvard.edu OI Birnboim, Yuval/0000-0002-6547-8545 FU Harvard University; National Science Foundation FX We thank Tobias Westmeier for making the HVC and outlier map available to us digitally, and Matt McQuinn, Anthony Stark and Matias Zaldarriaga for useful discussions and comments. The Wisconsin H-Alpha Mapper is funded by the National Science Foundation. Some of the results in this paper have been derived using the HEALPix [50] package. This work was supported in part by the Harvard University. NR 60 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD JUN PY 2009 IS 6 AR 008 DI 10.1088/1475-7516/2009/06/008 PG 21 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 467XJ UT WOS:000267776100030 ER PT J AU Lambert, JB Heckenbach, EA Hurtley, AE Wu, YY Santiago-Blay, JA AF Lambert, Joseph B. Heckenbach, Eric A. Hurtley, Anna E. Wu, Yuyang Santiago-Blay, Jorge A. TI Nuclear Magnetic Resonance Spectroscopic Characterization of Legume Exudates SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID RESINS AB Exudates from the plant family Fabaceae have been characterized by proton and carbon-13 nuclear magnetic resonance spectroscopy. The 79 identified species from 38 genera represent all three subfamilies of this widespread and economically important angiospermous (flowering) family. The observed exudates include resins, gums, kinos, gum resins, and a few materials as yet unclassified molecularly. Exudates from the subfamily Caesalpinoideae are primarily resins, whereas those from the Mimoisoideae and Faboideae are primarily gums. Three species of the Mimoisoideae produce both gums and kinos. C1 [Lambert, Joseph B.; Heckenbach, Eric A.; Hurtley, Anna E.; Wu, Yuyang] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Santiago-Blay, Jorge A.] Gallaudet Univ, Dept Biol, Washington, DC 20002 USA. RP Lambert, JB (reprint author), Northwestern Univ, Dept Chem, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM jlambert@northwestern.edu FU Gallaudet University FX We are grateful to several individuals and institutions for providing resin samples and for allowing us to collect on their premises, as listed in Table S1. Furthermore, we are indebted to B. R. Maslin (Department of Conservation and Land Management, Bentley Delivery Centre, Western Australia), J. A. Lackey (Department of Botany, National Museum of Natural History, Smithsonian Institution, -Washington, DC), and M. M. McMahon (Division of Plant Biology, University of Arizona) for assistance in taxonomic issues and to P. Peltier (Gaithersburg, MD) for painstaking preparation of the sample of Psorothatnnus spinosus. This work was supported by a Small Grant to J.A.S.B. from the Graduate Research Institute of Gallaudet University, to which we are deeply grateful. NR 13 TC 4 Z9 9 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 J9 J NAT PROD JI J. Nat. Prod. PD JUN PY 2009 VL 72 IS 6 BP 1028 EP 1035 DI 10.1021/np900188j PG 8 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 463LB UT WOS:000267432600009 PM 19492830 ER PT J AU Miller, HL Neale, PJ Dunton, KH AF Miller, Harlan L., III Neale, Patrick J. Dunton, Kenneth H. TI BIOLOGICAL WEIGHTING FUNCTIONS FOR UV INHIBITION OF PHOTOSYNTHESIS IN THE KELP LAMINARIA HYPERBOREA (PHAEOPHYCEAE) SO JOURNAL OF PHYCOLOGY LA English DT Article DE acclimation; biological weighting function; carbon-13; Laminaria hyperborea; oxygen; ozone depletion; photoinhibition; photosynthesis; photosynthetic quotient; UV radiation ID IRRADIATED YOUNG SPOROPHYTES; ULTRAVIOLET-RADIATION; MARINE MACROALGAE; ARCTIC MACROALGAE; AMINO-ACIDS; B RADIATION; BLUE-LIGHT; CHLOROPHYLL FLUORESCENCE; SACCHARINA PHAEOPHYTA; ALARIA-ESCULENTA AB Different wavelengths of sunlight either drive or inhibit macroalgal production. Ultraviolet radiation (UVR) effectively disrupts photosynthesis, but since UVR is rapidly absorbed in coastal waters, macroalgal photoinhibition and tolerance to UVR depend on the depth of attachment and acclimation state of the individual. The inhibition response to UVR is quantified with a biological weighting function (BWF), a spectrum of empirically derived weights that link irradiance at a specific wavelength to overall biological effect. We determined BWFs for shallow (0 m, mean low water [MLW]) and deep (10 m) Laminaria hyperborea (Gunnerus) Foslie collected off the island of Finnoy, Norway. For each replicate sporophyte, we concurrently measured both O(2) evolution and (13)C uptake in 48 different light treatments, which varied in UV spectral composition and irradiance. The relative shape of the kelp BWF was most similar to that of a land plant, and the absolute spectral weightings and sensitivity were typically less than phytoplankton, particularly in the ultraviolet radiation A (UVA) region. Differences in BWFs between O(2) and (13)C photosynthesis and between shallow (high light) and deep (low light) kelp were also most significant in the UVA. Because of its greater contribution to total incident irradiance, UVA was more important to daily loss of production in kelp than ultraviolet radiation B (UVB). Photosynthetic quotient (PQ) also decreased with increased UVR stress, and the magnitude of PQ decline was greater in deepwater kelp. Significantly, BWFs assist in the comparison of biological responses to experimental light sources versus in situ sunlight and are critical to quantifying kelp production in a changing irradiance environment. C1 [Miller, Harlan L., III] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. [Neale, Patrick J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Dunton, Kenneth H.] Univ Texas Austin, Inst Marine Sci, Port Aransas, TX 78373 USA. EM lanny.miller@mac.com RI Neale, Patrick/A-3683-2012 FU National Science Foundation [OPP-9622483]; Smithsonian Institute; University of Texas at Austin FX We extend our great appreciation to S. Fredriksen and the kelp team from the University of Oslo, Norway, and our special thanks to R. Myklebust and his gracious crew at Finnoy Sjohus. We also acknowledge the contributions of J. Lempa, E. Tang, A. Banaszak, K. Jackson, and J. Keller and critical readings by J. Brandes, E. Buskey, T. Villareal, H. Alexander, M. Scanlin, and C. Aumack. A. Stangelmayer of PreSens is appreciated for the generous loan of the Microx TX oxygen system. J. Biedenbach donated instrument time on the IO Analytical TOC analyzer. This research was funded in part by the National Science Foundation (OPP-9622483), the Smithsonian Institute predoctoral fellowship program, and the Environmental Science Institute Summer Fellowship program at the University of Texas at Austin. NR 64 TC 6 Z9 7 U1 0 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 2009 VL 45 IS 3 BP 571 EP 584 DI 10.1111/j.1529-8817.2009.00694.x PG 14 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 454WJ UT WOS:000266714200005 PM 27034033 ER PT J AU Rothman, LS Brown, LR Vander Auwera, J AF Rothman, Laurence S. Brown, Linda R. Vander Auwera, Jean TI SPECIAL ISSUE HITRAN Preface SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02318 USA. [Brown, Linda R.] CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. [Vander Auwera, Jean] Univ Libre Bruxelles, FRS FNRS, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02318 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 0 TC 0 Z9 0 U1 0 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN-JUL PY 2009 VL 110 IS 9-10 BP 531 EP 532 DI 10.1016/j.jqsrt.2009.02.025 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300001 ER PT J AU Rothman, LS Gordon, IE Barbe, A Benner, DC Bernath, PE Birk, M Boudon, V Brown, LR Campargue, A Champion, JP Chance, K Coudert, LH Dana, V Devi, VM Fally, S Flaud, JM Gamache, RR Goldman, A Jacquemart, D Kleiner, I Lacome, N Lafferty, WJ Mandin, JY Massie, ST Mikhailenko, SN Miller, CE Moazzen-Ahmadi, N Naumenko, OV Nikitin, AV Orphal, J Perevalov, VI Perrin, A Predoi-Cross, A Rinsland, CP Rotger, M Simeckova, M Smith, MAH Sung, K Tashkun, SA Tennyson, J Toth, RA Vandaele, AC Vander Auwera, J AF Rothman, L. S. Gordon, I. E. Barbe, A. Benner, D. Chris Bernath, P. E. Birk, M. Boudon, V. Brown, L. R. Campargue, A. Champion, J. -P. Chance, K. Coudert, L. H. Dana, V. Devi, V. M. Fally, S. Flaud, J. -M. Gamache, R. R. Goldman, A. Jacquemart, D. Kleiner, I. Lacome, N. Lafferty, W. J. Mandin, J. -Y. Massie, S. T. Mikhailenko, S. N. Miller, C. E. Moazzen-Ahmadi, N. Naumenko, O. V. Nikitin, A. V. Orphal, J. Perevalov, V. I. Perrin, A. Predoi-Cross, A. Rinsland, C. P. Rotger, M. Simeckova, M. Smith, M. A. H. Sung, K. Tashkun, S. A. Tennyson, J. Toth, R. A. Vandaele, A. C. Vander Auwera, J. TI The HITRAN 2008 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE HITRAN; Spectroscopic database; Molecular spectroscopy; Molecular absorption; Spectroscopic line parameters; Absorption cross-sections; Aerosols ID ABSORPTION CROSS-SECTIONS; ABSOLUTE LINE-INTENSITIES; FOURIER-TRANSFORM SPECTROSCOPY; SELF-BROADENING COEFFICIENTS; DIODE-LASER MEASUREMENTS; HIGH-RESOLUTION ANALYSIS; WATER-VAPOR TRANSITIONS; OXYGEN A-BAND; MU-M REGION; CONSTRAINED MULTISPECTRUM ANALYSIS AB This paper describes the status of the 2008 edition of the HITRAN molecular spectroscopic database. The new edition is the first official public release since the 2004 edition, although a number of crucial updates had been made available online since 2004. The HITRAN compilation consists of several components that serve as input for radiative-transfer calculation codes: individual line parameters for the microwave through visible spectra of molecules in the gas phase; absorption cross-sections for molecules having dense spectral features, i.e. spectra in which the individual lines are not resolved; individual line parameters and absorption cross-sections for bands in the ultraviolet; refractive indices of aerosols, tables and files of general properties associated with the database; and database management software. The line-by-line portion of the database contains spectroscopic parameters for 42 molecules including many of their isotopologues. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.; Chance, K.; Simeckova, M.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Barbe, A.; Rotger, M.] Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. [Benner, D. Chris; Devi, V. M.] Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. [Bernath, P. E.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England. [Birk, M.] DLR Remote Sensing Technol Inst, Wessling, Germany. [Boudon, V.; Champion, J. -P.; Rotger, M.] Univ Bourgogne, CNRS, Inst Carnot Bourgogne, F-21078 Dijon, France. [Brown, L. R.; Miller, C. E.; Sung, K.; Toth, R. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Campargue, A.] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Dana, V.; Mandin, J. -Y.] Univ Paris 06, UPMC, UMR 7092, Lab Phys Mol & Applicat, F-75252 Paris, France. [Fally, S.] Univ Libre Bruxelles, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. [Gamache, R. R.] Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Jacquemart, D.] Univ Paris 06, UPMC, UMR 7075, Lab Dynam Interact & React, F-75252 Paris, France. [Lafferty, W. J.] NIST, Gaithersburg, MD 20899 USA. [Massie, S. T.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Mikhailenko, S. N.; Naumenko, O. V.; Nikitin, A. V.; Perevalov, V. I.; Tashkun, S. A.] Inst Atmospher Opt, Tomsk 634055, Russia. [Moazzen-Ahmadi, N.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Predoi-Cross, A.] Univ Lethbridge, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. [Rinsland, C. P.; Smith, M. A. H.] NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. [Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Vandaele, A. C.] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI BOUDON, Vincent/A-4504-2010; Champion, Jean-Paul/C-3963-2009; Lacome, Nelly/A-7043-2008; Bernath, Peter/B-6567-2012; Tennyson, Jonathan/I-2222-2012; Orphal, Johannes/A-8667-2012; Nikitin, Andrei/K-2624-2013; Tashkun, Sergey/E-8682-2014; Sung, Keeyoon/I-6533-2015; OI Rothman, Laurence/0000-0002-3837-4847; Gordon, Iouli/0000-0003-4763-2841; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Orphal, Johannes/0000-0002-1943-4496; Nikitin, Andrei/0000-0002-4280-4096; Chance, Kelly/0000-0002-7339-7577 NR 368 TC 2138 Z9 2222 U1 32 U2 260 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 JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 533 EP 572 DI 10.1016/j.jqsrt.2009.02.013 PG 40 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300002 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Carleere, MR Csaszar, AG Gamache, RR Hodges, JT Jenouvrier, A Naumenko, OV Polyansky, OL Rothman, LS Toth, RA Vandaele, AC Zobov, NF Daumont, L Fazliev, AZ Furtenbacher, T Gordon, IE Mikhailenko, SN Shirin, SV AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Carleere, Michel R. Csaszar, Attila G. Gamache, Robert R. Hodges, Joseph T. Jenouvrier, Alain Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Toth, Robert A. Vandaele, Ann Carine Zobov, Nikolai F. Daumont, Ludovic Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Mikhailenko, Semen N. Shirin, Sergei V. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part I-Energy levels and transition wavenumbers for (H2O)-O-17 and (H2O)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Review DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; MARVEL; Information system; Database; Infrared spectra; Microwave spectra ID SUBMILLIMETER MICROWAVE-SPECTRUM; LORENTZ-BROADENING COEFFICIENTS; CENTRIFUGAL-DISTORTION ANALYSIS; FOURIER-TRANSFORM SPECTROSCOPY; RESOLUTION INFRARED SPECTRA; LINE-SHIFT COEFFICIENTS; RING-DOWN SPECTROSCOPY; 1.39 MU-M; INTERACTING STATES; ABSORPTION-SPECTRA AB This is the first part of a series of articles reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependence and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. The present article contains energy levels and data for line positions of the singly substituted isotopologues (H2O)-O-17 and (H2O)-O-18. The procedure and code MARVEL, standing for measured active rotational-vibrational energy levels, is used extensively in all stages of determining the validated levels and lines and their self-consistent uncertainties. The spectral regions covered for both isotopologues (H2O)-O-17 and (H2O)-O-18 are 0-17 125 cm(-1). The energy levels are checked against ones determined from accurate variational calculations. The number of critically evaluated and recommended levels and lines are, respectively, 2687 and 8614 for (H2O)-O-17, and 4839 and 29364 for (H2O)-O-18. The extensive lists of MARVEL lines and levels obtained are deposited in the Supplementary Material, as well as in a distributed information system applied to water, W@DIS, where they can easily be retrieved. A distinguishing feature of the present evaluation of water spectroscopic data is the systematic use of all available experimental data and validation by first-principles theoretical calculations. (c) 2009 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Univ York, York YO10 5DD, N Yorkshire, England. [Brown, Linda R.; Toth, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble 1, Grenoble, France. [Carleere, Michel R.] Univ Libre Brussels, Brussels, Belgium. [Csaszar, Attila G.; Furtenbacher, Tibor] Eotvos Lorand Univ, Budapest, Hungary. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA. [Jenouvrier, Alain; Daumont, Ludovic] Univ Reims, Reims, France. [Naumenko, Olga V.; Fazliev, Alexander Z.; Mikhailenko, Semen N.] 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 Belgique, B-1180 Brussels, Belgium. [Zobov, Nikolai F.; Shirin, Sergei V.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603600, Russia. RP Tennyson, J (reprint author), UCL, Dept Phys & Astron, Mortimer St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.uk RI Csaszar, Attila/A-5241-2009; Bernath, Peter/B-6567-2012; Hodges, Joseph/B-4578-2009; Tennyson, Jonathan/I-2222-2012; 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 Union of Pure and Applied Chemistry [2004-035-1-100]; UK Engineering and Physical Science Research Council; UK Natural Environment Research Council; Royal Society; British Council; INTAS foundation [WWLC-008535-MCA FP6 EC]; Scientific Research Fund of Hungary [OTKA T47185, K72885]; NKTH; European Union QUASAAR Marie Curie research training network; NATO; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 151490INLSFe(IC)]; Belgian National Fund for Scientific Research (FRFC contracts); Communaut de Belgique (Action de Recherche Concertees); NASA Earth Observing System (EOS) [NAG5-13534]; NASA laboratory astrophysics program; Programme National LEFE (CHAT) of CNRS (INSU); The National Aeronaudcs and Space Administratio 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 Engineering and Physical Science Research Council, the UK Natural Environment Research Council, the Royal Society, the British Council, the INTAS foundation, Grant WWLC-008535-(reintegration) MCA FP6 EC, the Scientific Research Fund of Hungary (Grants OTKA T47185 and K72885), the NKTH, the European Union QUASAAR Marie Curie research training network, NATO, the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (Contracts EV/35/3A, SD/AT/01A, PRODEX 151490INLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaut de Belgique (Action de Recherche Concertees), NASA Earth Observing System (EOS), under the Grant NAG5-13534, the NASA laboratory astrophysics program. Alain Campargue and Ludovic Daumont are grateful for the financial support provided by the Programme National LEFE (CHAT) of CNRS (INSU). Part of the research described in this paper was performed at the jet Propulsion Laboratory, California Institute of Technology, under contract with The National Aeronaudcs and Space Administration. NR 127 TC 90 Z9 95 U1 4 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN-JUL PY 2009 VL 110 IS 9-10 SI SI BP 573 EP 596 DI 10.1016/j.jqsrt.2009.02.014 PG 24 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 447HD UT WOS:000266181300003 ER PT J AU Wachowiak, MJ Karas, BV AF Wachowiak, Melvin J. Karas, Basiliki Vicky TI 3D SCANNING AND REPLICATION FOR MUSEUM AND CULTURAL HERITAGE APPLICATIONS SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article AB The recent proliferation of commercial three-dimensional digital scanning devices has made 3D scanning, and virtual and physical replication, a practical reality in the field of heritage preservation. 3D scanning produces a high-precision digital reference document that records condition, provides a virtual model for replication, and makes possible easy mass distribution of digital data. In addition to research, documentation, and replication, 3D data of artifacts are increasingly being used for museum collections storage and packing designs. The cost and complexity of 3D imaging technologies have made 3D scanning impractical for many heritage institutions in the past, but this is changing, as an increasing number of commercial systems are being tailored and marketed for heritage applications. This paper presents a review of the current state of 3D imaging in the cultural heritage field, methods of physical replication, the different systems used in heritage applications, criteria for choosing a system, and the techniques used for working with the data. Attention is given to identifying those objects that are not likely to be suited for 3D scanning. C1 [Wachowiak, Melvin J.; Karas, Basiliki Vicky] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Wachowiak, MJ (reprint author), Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM wachowiakm@si.edu; karasb@si.edu NR 15 TC 9 Z9 9 U1 2 U2 3 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD SUM PY 2009 VL 48 IS 2 BP 141 EP 158 PG 18 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V29YH UT WOS:000208783200003 ER PT J AU Boyero, L Ramirez, A Dudgeon, D Pearson, RG AF Boyero, Luz Ramirez, Alonso Dudgeon, David Pearson, Richard G. TI Are tropical streams really different? SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article ID RAIN-FOREST STREAM; LEAF-LITTER; TROPHIC RELATIONSHIPS; COMMUNITY STRUCTURE; NEOTROPICAL STREAM; NEW-GUINEA; FOOD WEBS; HONG-KONG; SHREDDERS; PATTERNS C1 [Boyero, Luz; Pearson, Richard G.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Boyero, Luz] Smithsonian Trop Res Inst, Balboa 2072, Panama. [Ramirez, Alonso] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00931 USA. [Dudgeon, David] Univ Hong Kong, Sch Biol Sci, Div Ecol & Biodivers, Hong Kong, Hong Kong, Peoples R China. RP Boyero, L (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM luz.boyero@jcu.edu.au; alonso_ites@yahoo.com; ddudgeon@hkucc.hku.hk; richard.pearson@jcu.edu.au RI Dudgeon, David/A-2733-2010; Ramirez, Alonso/E-4462-2012; Boyero, Luz/L-5822-2014; OI Ramirez, Alonso/0000-0001-9985-5719; Boyero, Luz/0000-0001-7366-9299; Pearson, Richard/0000-0001-6047-031X NR 54 TC 48 Z9 53 U1 3 U2 29 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD JUN PY 2009 VL 28 IS 2 BP 397 EP 403 DI 10.1899/08-146.1 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 453XH UT WOS:000266645700012 ER PT J AU Yule, CM Leong, MY Liew, KC Ratnarajah, L Schmidt, K Wong, HM Pearson, RG Boyero, L AF Yule, Catherine M. Leong, Mun Yi Liew, Kong Cheng Ratnarajah, Lavenia Schmidt, Katrin Wong, Hooi Ming Pearson, Richard G. Boyero, Luz TI Shredders in Malaysia: abundance and richness are higher in cool upland tropical streams SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE tropics; macroinvertebrate shredders; forested headwater streams; dipterocarp forests ID LEAF-LITTER BREAKDOWN; FOREST STREAM; BODY-SIZE; MANDIBLE SIZE; FOOD WEBS; MACROINVERTEBRATES; ASSEMBLAGES; TEMPERATE; PATTERNS; BEETLES AB Stream shredders have been reported as scarce in several tropical areas. This pattern is in contrast to observations in temperate streams, which support an abundant and diverse shredder fauna. Two possible explanations for this pattern are that most shredders are adapted to cool conditions and that temperate riparian vegetation often produces more palatable and more nutritious leaves than do the more diverse, tropical rainforests. In peninsular Malaysia, most streams flow through lowland dipterocarp forests that are characterized by strikingly high tree diversity and by many species with tough leathery leaves that are high in lignin and toxic secondary compounds and low in protein. In contrast, highland streams flow through montane rain forests and are more similar to temperate streams. We hypothesized that shredder fauna would be distributed along an altitudinal gradient, with more abundant and diverse assemblages in highland streams. We sampled leaf litter in 12 sites at altitudes from 55 to 1560 m above sea level. As expected, highland sites supported higher abundance and diversity of shredders (9-15 species per site) than did lowland sites (3-8 species per site). Shredder densities were similar among lowland sites, but species composition was variable. Large snails (Brotia spp.) were the dominant shredders in nonacidic streams in Taman Negara, but they were absent from acidic streams and from streams elsewhere in peninsular Malaysia. Shredder biomass was generally high because of the large body size of most species (e.g., crabs, snails, semiaquatic cockroaches, calamoceratids, and tipulids). Large mouthparts might allow these species to shred tough leaves efficiently, and large body size might enable them to tolerate a wide variety of toxic secondary compounds. Our results suggest that shredder diversity might depend on elevation, water temperature, characteristics of the riparian vegetation along altitudinal gradients, and variation in water chemistry at local scales. C1 [Yule, Catherine M.; Leong, Mun Yi; Liew, Kong Cheng; Ratnarajah, Lavenia; Schmidt, Katrin; Wong, Hooi Ming] Monash Univ, Sch Sci, Selangor 46150, Malaysia. [Pearson, Richard G.; Boyero, Luz] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Boyero, Luz] Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Yule, CM (reprint author), Monash Univ, Sch Sci, Bandar Sunway, Selangor 46150, Malaysia. EM catherine.yule@sci.monash.edu.my; richard.pearson@jcu.edu.au; luz.boyero@jcu.edu.au RI Boyero, Luz/L-5822-2014; YULE, Catherine/F-9733-2015; OI Boyero, Luz/0000-0001-7366-9299; Pearson, Richard/0000-0001-6047-031X; YULE, CATHERINE/0000-0002-1085-2798 FU Committee for Research and Exploration of the National Geographic Society [7980-06] FX We are grateful to Tan Man Yong and Alison Lewis, who provided assistance in the field. We thank Dato' Haji Musa Nordin, Director General, Department of Wildlife and National Parks Malaysia for permission to collect samples in Taman Negara. This study was partially funded by a grant from the Committee for Research and Exploration of the National Geographic Society to LB (grant number 7980-06). We thank Pamela Silver for her careful editing and 2 anonymous referees for their suggestions that resulted in significant improvements to this paper. NR 49 TC 47 Z9 50 U1 1 U2 26 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD JUN PY 2009 VL 28 IS 2 BP 404 EP 415 DI 10.1899/07-161.1 PG 12 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 453XH UT WOS:000266645700013 ER PT J AU Pearson, RG Boyero, L AF Pearson, Richard G. Boyero, Luz TI Gradients in regional diversity of freshwater taxa SO JOURNAL OF THE NORTH AMERICAN BENTHOLOGICAL SOCIETY LA English DT Article DE diversity; species richness; tropics; latitudinal gradients; Ephemeroptera; Plecoptera; Odonata; Trichoptera; Anura; Caudata; Osteichthyes ID RAIN-FOREST STREAM; GLOBAL DIVERSITY; SPECIES-RICHNESS; LATITUDINAL GRADIENTS; MAYFLIES EPHEMEROPTERA; TROPICAL STREAM; YUCCABINE CREEK; LIFE-HISTORY; PATTERNS; SCALE AB Opinion about latitudinal diversity gradients in freshwater fauna has varied over past decades. Global data have been compiled for diversity of Ephemeroptera, Plecoptera, and Trichoptera at the site scale, but no assessment of global variability in regional diversity has been done for any taxon except fish. Global variation cannot be inferred from site-scale data because the relationship between site and regional diversity is not necessarily linear. We have assembled global data on regional diversity for 7 freshwater taxa. Here, we plot diversity against regional area, develop diversity-area regressions, and then plot the residuals against latitude to investigate latitudinal diversity gradients. The existence and directions of gradients vary substantially among taxa. For Ephemeroptera and Plecoptera, significant latitudinal gradients exist, and diversity is greater at higher latitudes. For Trichoptera and Caudata, latitudinal gradients are not apparent, although taxa within the Caudata show distinct patterns. For Odonata, Osteichthyes, and Anura, latitudinal gradients are highly significant, and diversity is greatest at low latitudes. A clear distinction between the life cycles of tropically diverse taxa and of other taxa (excluding fish) is a long terrestrial phase in the tropically diverse taxa (e.g., Odonata). We discuss reasons for the gradients and this contrast in ecological and evolutionary contexts (e.g., habitat complexity and cross-habitat adaptation). C1 [Pearson, Richard G.; Boyero, Luz] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Boyero, Luz] Smithsonian Trop Res Inst, Balboa 2072, Panama. RP Pearson, RG (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM richard.pearson@jcu.edu.au; luz.boyero@jcu.edu.au RI Boyero, Luz/L-5822-2014; OI Boyero, Luz/0000-0001-7366-9299; Pearson, Richard/0000-0001-6047-031X FU James Cook University FX We thank T. A. Crowl, P Silver, and an anonymous referee for very helpful comments on the manuscript. LB was supported by a postdoctoral fellowship from James Cook University. NR 72 TC 33 Z9 33 U1 4 U2 31 PU NORTH AMER BENTHOLOGICAL SOC PI LAWRENCE PA 1041 NEW HAMSPHIRE STREET, LAWRENCE, KS 66044 USA SN 0887-3593 J9 J N AM BENTHOL SOC JI J. N. Am. Benthol. Soc. PD JUN PY 2009 VL 28 IS 2 BP 504 EP 514 DI 10.1899/08-118.1 PG 11 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 453XH UT WOS:000266645700021 ER PT J AU Bruna, EM Fiske, IJ Trager, MD AF Bruna, Emilio M. Fiske, Ian J. Trager, Mathew D. TI Habitat fragmentation and plant populations: is what we know demographically irrelevant? SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Demography; Elasticity analyses; Fertility; Lambda; Matrix models; Pollination; Seed banks; Seedling recruitment; Vital rates ID AMAZONIAN FOREST FRAGMENTS; TABLE RESPONSE EXPERIMENTS; OLD-GROWTH FOREST; RAIN-FOREST; SEEDLING RECRUITMENT; PROJECTION MATRICES; TREE COMMUNITIES; CONSERVATION; POLLINATION; PATTERNS AB Habitat fragmentation is considered a leading cause of plant extinction, and matrix models provide a powerful set of tools with which to identifying mechanisms that influence population declines. We surveyed the ecological literature to determine what components of plant demography have been studied in fragmented habitats, and determined the elasticity values of the vital rates influenced by these components. We found that there is a major disparity between the ecological processes and stages of life history with large demographic impacts and the focus of empirical research on plants in fragmented habitats. While the growth and survivorship of large, established individuals have the highest elasticity values, the focus of empirical research has been on components of reproduction and seedling dynamics. We argue that elucidating the demographic mechanisms underlying population declines in fragmented habitats, and developing strategies for mitigating these declines, will be challenging without a greater focus on understanding how fragmentation alters adult plant growth and survivorship. C1 [Bruna, Emilio M.; Fiske, Ian J.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011 Manaus, Amazonas, Brazil. [Bruna, Emilio M.] Smithsonian Trop Res Inst, BR-69011 Manaus, Amazonas, Brazil. [Trager, Mathew D.] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA. RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, POB 110430, Gainesville, FL 32611 USA. EM embruna@ufl.edu RI Bruna, Emilio/H-2769-2012 OI Bruna, Emilio/0000-0003-3381-8477 FU University of Florida's College of Agriculture and Natural Resources (IJF); School for Natural Resources and the Environment (MDT) FX We thank B. D. Inouye, C. Zartman, L. Galetto, and four anonymous reviewers for enlightening discussions and comments on the manuscript. Financial support was provided by the University of Florida's College of Agriculture and Natural Resources (IJF) and the School for Natural Resources and the Environment (MDT). This is publication number 523 in the BDFFP Technical Series. NR 60 TC 27 Z9 29 U1 2 U2 23 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1100-9233 J9 J VEG SCI JI J. Veg. Sci. PD JUN PY 2009 VL 20 IS 3 BP 569 EP 576 DI 10.1111/j.1654-1103.2009.01060.x PG 8 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 448DU UT WOS:000266244100019 ER PT J AU Vieira, TB Mendes, P Oprea, M Ditchfield, AD AF Vieira, Thiago B. Mendes, Poliana Oprea, Monik Ditchfield, Albert D. TI New record of Lasiurus blossevillii (Chiroptera: Vespertilionidae) for the restinga ecosystem, and second occurrence for the state of Espirito Santo, southeastern Brazil SO MAMMALIA LA English DT Article DE bats; distribution; restinga ecosystem; vespertilionid C1 [Vieira, Thiago B.; Mendes, Poliana; Ditchfield, Albert D.] Univ Fed Espirito Santo, Dept Ciencias Biol, Lab Estudos Quiropteros, BR-29040090 Vitoria, ES, Brazil. [Oprea, Monik] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, MRC 108, Washington, DC 20560 USA. RP Vieira, TB (reprint author), Univ Fed Espirito Santo, Dept Ciencias Biol, Lab Estudos Quiropteros, Ave Marechal Campos 1468, BR-29040090 Vitoria, ES, Brazil. EM thiagobernardi007@gmail.com RI Oprea, Monik/E-6204-2010; Vieira, Thiago/P-5233-2015 OI Vieira, Thiago/0000-0003-1762-8294 FU Conselho Nacional de Pesquisa (CNPq) FX We thank Daniel Brito, the associate editor and two anonymous reviewers, who gave valuable comments and suggestions that substantially improved the manuscript. The authors thank the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis (IBAMA) and the Instituto Estadual do Meio Ambiente (IEMA) for the fieldwork licences. We also thank the manager of Parque Estatual Paulo Cesar Vinha for permission to work in the park, and all colleagues who participated in the fieldwork. T. B. V. thanks Conselho Nacional de Pesquisa (CNPq) for a scholarship. NR 26 TC 1 Z9 1 U1 0 U2 2 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 J9 MAMMALIA JI Mammalia PD JUN PY 2009 VL 73 IS 2 BP 155 EP 157 DI 10.1515/MAMM.2009.025 PG 3 WC Zoology SC Zoology GA 465HL UT WOS:000267573300014 ER PT J AU Foltz, DW Mah, CL AF Foltz, David W. Mah, Christopher L. TI Recent relaxation of purifying selection on the tandem-repetitive early-stage histone H3 gene in brooding sea stars SO MARINE GENOMICS LA English DT Article DE Nonsynonymous substitutions; Larval habitat; Multigene family; Forcipulatida; Echinoderms; Sea stars ID LIKELIHOOD-RATIO TESTS; DEVELOPMENTAL MODE; DEATH EVOLUTION; EXPRESSION; FAMILY; LARVAE; SUBSTITUTIONS; ECHINODERMS; PATTERNS; HELIOCIDARIS AB Patterns of nucleotide substitution differ between marine species that have a pelagic feeding (plankto-trophic) larval stage and related species that lack such a stage, for both adaptive and non-adaptive reasons. Here, patterns of nucleotide and inferred amino acid substitution are analyzed for the tandem-repetitive early-stage histone H3 gene in 36 sea star species of the order Forcipulatida with documented larval habitat. The relative rate of nonsynonymous substitution (expressed as omega=d(N)/d(s)) was significantly higher in lineages with a brooded non-feeding (lecithotrophic) larval form than in lineages with a planktotrophic larval form. There was also a significant excess of conservative over radical substitutions. The increase in omega for brooders as compared to non-brooders was much greater than for previously analyzed mitochondrial sequences in echinoderms. These data are consistent with the hypothesis that purifying selection on this gene has been relaxed in brooding lineages compared to non-brooding lineages. The hypotheses of adaptive or neutral evolution are less plausible, although recent pseudogenization following a period of relaxed purifying selection could also explain the results. (C) 2009 Elsevier B.V. All rights reserved. C1 [Foltz, David W.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20007 USA. RP Foltz, DW (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM dfoltz@lsu.edu RI Mah, Christopher/B-5771-2008 FU NSF [OPP-0631245]; Office of Research and Economic Development at Louisiana State University FX We thank Dr. Robert Van Syoc for arranging loan of material from the California Academy of Sciences and Drs. Mark A. Batzer and John C. Larkin for suggestions and comments on the manuscript. James W. Halk and Cali M. Meyer assisted in the laboratory. Financial support was provided by NSF grant OPP-0631245 to CL Mah and an award from the Office of Research and Economic Development at Louisiana State University to DW Foltz. NR 35 TC 5 Z9 5 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1874-7787 EI 1876-7478 J9 MAR GENOM JI Mar. Genom. PD JUN PY 2009 VL 2 IS 2 BP 113 EP 118 DI 10.1016/j.margen.2009.06.002 PG 6 WC Genetics & Heredity; Marine & Freshwater Biology SC Genetics & Heredity; Marine & Freshwater Biology GA 545NK UT WOS:000273739100005 PM 21798179 ER PT J AU Koblmuller, S Nord, M Wayne, RK Leonard, JA AF Koblmuller, Stephan Nord, Maria Wayne, Robert K. Leonard, Jennifer A. TI Origin and status of the Great Lakes wolf SO MOLECULAR ECOLOGY LA English DT Article DE aDNA; Canis latrans; Canis lupus lycaon; conservation; hybridization; introgression; Y chromosome ID COYOTE MITOCHONDRIAL-DNA; ALLELE FREQUENCY DATA; WOLVES CANIS-LUPUS; POPULATION BOTTLENECKS; GENOTYPING ERRORS; GENETIC-STRUCTURE; NULL ALLELES; GRAY WOLF; HYBRIDIZATION; INTROGRESSION AB An extensive debate concerning the origin and taxonomic status of wolf-like canids in the North American Great Lakes region and the consequences for conservation politics regarding these enigmatic predators is ongoing. Using maternally, paternally and biparentally inherited molecular markers, we demonstrate that the Great Lakes wolves are a unique population or ecotype of gray wolves. Furthermore, we show that the Great Lakes wolves experienced high degrees of ancient and recent introgression of coyote and western gray wolf mtDNA and Y-chromosome haplotypes, and that the recent demographic bottleneck caused by persecution and habitat depletion in the early 1900s is not reflected in the genetic data. C1 [Koblmuller, Stephan; Nord, Maria; Leonard, Jennifer A.] Uppsala Univ, Evolutionary Biol Ctr, Dept Evolutionary Biol, SE-75236 Uppsala, Sweden. [Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Leonard, Jennifer A.] Ctr Conservat & Evolutionary Genet, Natl Zool Pk & Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Leonard, Jennifer A.] Estn Biol Donana CSIC, Seville 41092, Spain. RP Leonard, JA (reprint author), Uppsala Univ, Evolutionary Biol Ctr, Dept Evolutionary Biol, Norbyvagen 18D, SE-75236 Uppsala, Sweden. EM jennifer.leonard@ebc.uu.se RI CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010 OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819 FU Carl Tryggers Foundation; Sven and Lilly Lawski Foundation; Swedish Research Council; National Science Foundation [0352634, 0733033] FX For providing samples we would like to thank Tom Cooley (Michigan Department of Natural Resources), John Hart, Bill Paul, D. Pete Sahr, Shawn Mcdowell (USDA APHIS Wildlife Services, Minnesota), John Hobbs, Ronald Fryder, Wayne Homan, Randy Benben (USDA APHIS Wildlife Services, Nebraska), Roland Kays (New York State Museum), Thomas Decker (Vermont Department of Fish & Wildlife), Craig Coolahan (USDA APHIS Wildlife Services, California), Bob Beach (USDA Wildlife Services, Nevada), George Hubert (Illinois Department of Natural Resources) and Bob Fisher (National Museum of Natural History, Smithsonian Institution). We are grateful to Kristina M. Sefc for valuable comments on the analyses and for providing scripts to handle large amounts of data; and to Carles Vila for comments on the manuscript. Financial support was provided by the Carl Tryggers Foundation, the Sven and Lilly Lawski Foundation, the Swedish Research Council and the National Science Foundation (NSF; OPP 0352634 and OPP-IOS 0733033). Logistical support was provided by Jesus Maldonado and the Center for Conservation and Evolutionary Genetics, National Zoological Park, Smithsonian Institution, USA. NR 68 TC 57 Z9 62 U1 1 U2 22 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD JUN PY 2009 VL 18 IS 11 BP 2313 EP 2326 DI 10.1111/j.1365-294X.2009.04176.x PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 448NH UT WOS:000266268800003 PM 19366404 ER PT J AU Bacci, M Solomon, SE Mueller, UG Martins, VG Carvalho, AOR Vieira, LGE Silva-Pinhati, ACO AF Bacci, Mauricio, Jr. Solomon, Scott E. Mueller, Ulrich G. Martins, Vanderlei G. Carvalho, Alfredo O. R. Vieira, Luiz G. E. Silva-Pinhati, Ana Carla O. TI Phylogeny of leafcutter ants in the genus Atta Fabricius (Formicidae: Attini) based on mitochondrial and nuclear DNA sequences SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cytochrome oxidase I; Cytochrome oxidase II; tRNA leucine; Elongation factor 1-alpha; Molecular systematics ID LEAF-CUTTING ANTS; SEXDENS-RUBROPILOSA; NESTS; HYMENOPTERA; EVOLUTION; CEPHALOTES; FOREST; DIVERSIFICATION; SUBSTITUTION; DIVERSITY AB Leafcutting ants of the genus Atta are the most conspicuous members of the tribe Attini, the fungus-growing ants. Atta species have long attracted the attention of naturalists, and have since become a common model system for the study of complex insect societies as well as for the study of coevolutionary dynamics due to their numerous interactions with fungi and other microbes. Nevertheless, systematics and taxonomy of the 15 species in the genus Atta have proven challenging, due in part to the extreme levels of worker polymorphism these species display, leading to disagreements about the validity of as many as five different subgenera and calling into question the monophyly of the genus. Here, we use DNA sequence information from fragments of three mitochondrial genes (COI, tRNA leucine and COII) and one nuclear gene (EF1-alpha F1), totaling 1070 base pairs, to reconstruct the phylogenetic relationships of Atta species using maximum parsimony, maximum likelihood and Bayesian inference techniques. Our results provide support for monophyly of the genus Atta, and suggest that the genus is divided into four monophyletic groups, which correspond to four of the five previously erected Atta subgenera: Atta sensu stricto and Archeatta, each with species composition identical to earlier proposals; Neoatta and Epiatta, with major differences in species composition from earlier proposals. The current geographic ranges of these species suggest that the historical separation of South America from Central and North America has played a role in speciation within this genus. (C) 2008 Elsevier Inc. All rights reserved. C1 [Bacci, Mauricio, Jr.; Solomon, Scott E.; Martins, Vanderlei G.] Sao Paulo State Univ, Ctr Study Social Insects, BR-13506900 Rio Claro, SP, Brazil. [Solomon, Scott E.; Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Univ Stn 1, Austin, TX 78712 USA. [Solomon, Scott E.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Carvalho, Alfredo O. R.; Vieira, Luiz G. E.] Inst Agron Parana, BR-86001970 Tres Marcos Londrina, PR, Brazil. [Silva-Pinhati, Ana Carla O.] Inst Agron Campinas, BR-13490970 Cordeiropolis, SP, Brazil. RP Bacci, M (reprint author), Sao Paulo State Univ, Ctr Study Social Insects, Ave 24-A,1515, BR-13506900 Rio Claro, SP, Brazil. EM mbacci@rc.unesp.br FU Funda do de Apoio a Pesquisa do Estado de Sao Paulo; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; National Science Foundation [DEB 0407772, IRFP 07012333]; graduate program in Ecology, Evolution and Behavior at UT-Austin FX The authors thank F. Cuezzo, E. Economo, A.G. Himler, A.S. Mikheyev, C. Rabeling, S. Sanchez-Pena, Adriana Ortiz and Luiz Carlos Forti for providing valuable material. J. Brown, U.G. Mueller and C. Rabeling offered helpful suggestions on an earlier version of this manuscript. We also acknowledge financial support from Funda do de Apoio a Pesquisa do Estado de Sao Paulo and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico to MB and from the National Science Foundation (DEB 0407772 and IRFP 07012333), the IGERT program in computational phylogenetics at UT-Austin, and from the graduate program in Ecology, Evolution and Behavior at UT-Austin to S.E.S. NR 61 TC 24 Z9 26 U1 5 U2 21 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD JUN PY 2009 VL 51 IS 3 BP 427 EP 437 DI 10.1016/j.ympev.2008.11.005 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 447WO UT WOS:000266222900002 PM 19041407 ER PT J AU Croston, JH Kraft, RP Hardcastle, MJ Birkinshaw, M Worrall, DM Nulsen, PEJ Penna, RF Sivakoff, GR Jordan, A Brassington, NJ Evans, DA Forman, WR Gilfanov, M Goodger, JL Harris, WE Jones, C Juett, AM Murray, SS Raychaudhury, S Sarazin, CL Voss, R Woodley, KA AF Croston, J. H. Kraft, R. P. Hardcastle, M. J. Birkinshaw, M. Worrall, D. M. Nulsen, P. E. J. Penna, R. F. Sivakoff, G. R. Jordan, A. Brassington, N. J. Evans, D. A. Forman, W. R. Gilfanov, M. Goodger, J. L. Harris, W. E. Jones, C. Juett, A. M. Murray, S. S. Raychaudhury, S. Sarazin, C. L. Voss, R. Woodley, K. A. TI High-energy particle acceleration at the radio-lobe shock of Centaurus A SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: active; galaxies: elliptical and lenticular: cD; galaxies: individual: Cen A; radio continuum: galaxies; X-rays: galaxies ID MAGNETIC-FIELD STRENGTHS; DEEP CHANDRA OBSERVATION; COSMIC-RAY ACCELERATION; X-RAY; SUPERNOVA-REMNANTS; PERSEUS CLUSTER; HOT GAS; GALAXY; EMISSION; NUCLEUS AB We present new results on the shock around the south-west radio lobe of Centaurus A using data from the Chandra Very Large Programme observations (740 ks total observing time). The X-ray spectrum of the emission around the outer south-western edge of the lobe is well described by a single power-law model with Galactic absorption - thermal models are strongly disfavoured, except in the region closest to the nucleus. We conclude that a significant fraction of the X-ray emission around the south-west part of the lobe is synchrotron, not thermal. We infer that in the region where the shock is strongest and the ambient gas density lowest, the inflation of the lobe is accelerating particles to X-ray synchrotron emitting energies, similar to supernova remnants such as SN1006. This interpretation resolves a problem of our earlier, purely thermal, interpretation for this emission, namely that the density compression across the shock was required to be much larger than the theoretically expected factor of 4. We describe a self-consistent model for the lobe dynamics and shock properties using the shell of thermal emission to the north of the lobe to estimate the lobe pressure. Based on this model, we estimate that the lobe is expanding to the south-west with a velocity of similar to 2600 km s(-1), roughly Mach 8 relative to the ambient medium. We discuss the spatial variation of spectral index across the shock region, concluding that our observations constrain gamma(max) for the accelerated particles to be similar to 10(8) at the strongest part of the shock, consistent with expectations from diffusive shock acceleration theory. Finally, we consider the implications of these results for the production of ultra-high energy cosmic rays (UHECRs) and TeV emission from Centaurus A, concluding that the shock front region is unlikely to be a significant source of UHECRs, but that TeV emission from this region is expected at levels comparable to current limits at TeV energies, for plausible assumed magnetic field strengths. C1 [Croston, J. H.; Hardcastle, M. J.; Goodger, J. L.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kraft, R. P.; Birkinshaw, M.; Worrall, D. M.; Nulsen, P. E. J.; Penna, R. F.; Jordan, A.; Brassington, N. J.; Evans, D. A.; Forman, W. R.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sivakoff, G. R.; Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Sivakoff, G. R.] Ohio State Univ, Dept Astron, McPherson Lab 4055, Columbus, OH 43210 USA. [Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Evans, D. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gilfanov, M.; Voss, R.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Harris, W. E.; Woodley, K. A.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Juett, A. M.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Voss, R.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany. [Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. RP Croston, JH (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM J.H.Croston@herts.ac.uk RI Hardcastle, Martin/E-2264-2012; Sivakoff, Gregory/G-9602-2011; OI Hardcastle, Martin/0000-0003-4223-1117; Sivakoff, Gregory/0000-0001-6682-916X; Nulsen, Paul/0000-0003-0297-4493; Goodger, Joanna/0000-0002-5738-4768; Jordan, Andres/0000-0002-5389-3944 FU NASA [NAS8-03060, GO7-8105X]; Hubble [HST-GO-10597.03-A]; Royal Society FX This work was partially supported by NASA grants NAS8-03060 and GO7-8105X, and Hubble grant HST-GO-10597.03-A. We gratefully acknowledge support from the Royal Society (research fellowship for MJH). NR 52 TC 63 Z9 63 U1 0 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2009 VL 395 IS 4 BP 1999 EP 2012 DI 10.1111/j.1365-2966.2009.14715.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600018 ER PT J AU Elebert, P Callanan, PJ Torres, MAP Garcia, MR AF Elebert, P. Callanan, P. J. Torres, M. A. P. Garcia, M. R. TI Optical spectroscopy and Doppler tomography of Cygnus X-2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; stars: individual: Cygnus X-2, V1341 Cygni; stars: neutron; X-rays: binaries ID X-RAY BINARIES; NEUTRON-STAR; RADIAL-VELOCITIES; V1341 CYGNI; BLACK-HOLE; MASS; TRANSIENTS; TELESCOPE; CURVE; DONOR AB We present phase resolved optical spectroscopy and Doppler tomography of V1341 Cygni, the optical counterpart to the neutron star low-mass X-ray binary (LMXB) Cygnus X-2 (Cyg X-2). We derive a radial velocity (RV) curve for the secondary star, finding a projected RV semi-amplitude of K(2) = 79 +/- 3 km s(-1), leading to a mass function of 0.51 +/- 0.06 M(circle dot), similar to 30 per cent lower than the previous estimate. We tentatively attribute the lower value of K(2) (compared to that obtained by other authors) to variations in the X-ray irradiation of the secondary star at different epochs of observations. The limited phase coverage and/or longer timebase of previous observations may also contribute to the difference in K(2). Our value for the mass function implies a primary mass of 1.5 +/- 0.3 M(circle dot), somewhat lower than previous dynamical estimates, but consistent with the value found by analysis of type-I X-ray bursts from this system. Our Doppler tomography of the broad He II lambda 4686 line reveals that most of the emission from this line is produced on the irradiated face of the donor star, with little emission from the accretion disc. In contrast, the Doppler tomogram of the N III lambda 4640.64 Bowen blend line shows bright emission from near the gas stream/accretion disc impact region, with fainter emission from the gas stream and secondary star. This is the first LMXB for which the Bowen blend is dominated by emission from the gas stream/accretion disc impact region, without comparable emission from the secondary star. This has implications for the interpretation of Bowen blend Doppler tomograms of other LMXBs for which the ephemeris may not be accurately known. C1 [Elebert, P.; Callanan, P. J.] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Torres, M. A. P.; Garcia, M. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elebert, P (reprint author), Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. EM p.elebert@ucc.ie FU Science Foundation Ireland; NASA [NAS8-03060] FX We acknowledge the use of the 1.5-m Tillinghast telescope at Fred L. Whipple Observatory, Mt. Hopkins, Arizona, and we thank observers M. L. Calkins, P. Berlind, T. M. Currie, E. E. Mamajek and W. Peters. We thank S. Tokarz, N. Caldwell and N. Martimbeau for assistance with the sky line correction to the wavelength calibration. This research made use of NASA's Astrophysics Data System, and the SIMBAD data base, operated at CDS, Strasbourg, France. 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 the National Aeronautics and Space Administration and the National Science Foundation. We thank J. A. Orosz for providing us with the ELC code. We acknowledge the use of MOLLY and DOPPLER software packages developed by T. R. Marsh, University of Warwick. We thank the anonymous referee for the helpful suggestions which improved our paper. PE and PJC acknowledge support from Science Foundation Ireland. MRG acknowledges partial support from NASA contract NAS8-03060 to the Chandra X-ray Center. NR 37 TC 12 Z9 12 U1 0 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2009 VL 395 IS 4 BP 2029 EP 2038 DI 10.1111/j.1365-2966.2009.14685.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600020 ER PT J AU O'Leary, RM Kocsis, B Loeb, A AF O'Leary, Ryan M. Kocsis, Bence Loeb, Abraham TI Gravitational waves from scattering of stellar-mass black holes in galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE black hole physics; gravitational waves; galaxies: kinematics and dynamics; galaxies: nuclei ID DENSE STAR-CLUSTERS; SGR A-ASTERISK; GLOBULAR-CLUSTERS; HYPERVELOCITY STARS; CENTRAL PARSEC; POINT-MASSES; COMPACT REMNANTS; MILKY-WAY; BINARIES; GALAXY AB Stellar-mass black holes (BHs) are expected to segregate and form a steep density cusp around supermassive black holes (SMBHs) in galactic nuclei. We follow the evolution of a multimass system of BHs and stars by numerically integrating the Fokker-Planck energy diffusion equations for a variety of BH mass distributions. We find that the BHs 'self-segregate', and that the rarest, most massive BHs dominate the scattering rate closest to the SMBH(less than or similar to 10(-1) pc). BH-BH binaries form out of gravitational wave emission during BH encounters. We find that the expected rate of BH coalescence events detectable by Advanced LIGO is similar to 1-10(2) yr(-1), depending on the initial mass function of stars in galactic nuclei and the mass of the most massive BHs. We find that the actual merger rate is likely similar to 10 times larger than this due to the intrinsic scatter of stellar densities in many different galaxies. The BH binaries that form this way in galactic nuclei have significant eccentricities as they enter the LIGO band (90 per cent with e > 0.9), and are therefore distinguishable from other binaries, which circularize before becoming detectable. We also show that eccentric mergers can be detected to larger distances and greater BH masses than circular mergers, up to similar to 700M(circle dot). Future ground-based gravitational wave observatories will be able to constrain both the mass function of BHs and stars in galactic nuclei. C1 [O'Leary, Ryan M.; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, Bence] Inst Adv Studies, Princeton, NJ 08540 USA. RP O'Leary, RM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM roleary@cfa.harvard.edu; bkocsis@ias.edu; aloeb@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU OTKA [68228]; Polanyi Program of the Hungarian National Office for Research and Technology (NKTH); NASA [NNX08AL43G]; FQXi; Harvard University FX We thank Krzysztof Belczynski, Sam Finn, Scott Hughes, Pablo Laguna, Ilya Mandel, Szabolcs Marka and Coleman Miller for useful discussions and Andras Pal for helping with Fig. 9. This work is supported by in part by NASA grant NNX08AL43G, by FQXi and by Harvard University funds. BK acknowledges support from OTKA Grant 68228 and Polanyi Program of the Hungarian National Office for Research and Technology (NKTH). NR 113 TC 98 Z9 98 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 JUN 1 PY 2009 VL 395 IS 4 BP 2127 EP 2146 DI 10.1111/j.1365-2966.2009.14653.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600029 ER PT J AU Yuan, F Lin, J Wu, KW Ho, LC AF Yuan, Feng Lin, Jun Wu, Kinwah Ho, Luis C. TI A magnetohydrodynamical model for the formation of episodic jets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; MHD; ISM: jets and outflow ID MAGNETICALLY DRIVEN ACCRETION; ADVECTION-DOMINATED ACCRETION; CORONAL MASS EJECTIONS; BLACK-HOLES; SAGITTARIUS-A; SOLAR ERUPTIONS; GRS 1915+105; DISKS; FLOWS; FIELD AB Episodic ejection of plasma blobs has been observed in many black hole systems. While steady, continuous jets are believed to be associated with large-scale open magnetic fields, what causes the episodic ejection of blobs remains unclear. Here by analogy with the coronal mass ejection on the Sun, we propose a magnetohydrodynamical model for episodic ejections from black holes associated with the closed magnetic fields in an accretion flow. Shear and turbulence of the accretion flow deform the field and result in the formation of a flux rope in the disc corona. Energy and helicity are accumulated and stored until a threshold is reached. The system then loses its equilibrium and the flux rope is thrust outward by the magnetic compression force in a catastrophic way. Our calculations show that for parameters appropriate for the black hole in our Galactic centre, the plasmoid can attain relativistic speeds in about 35 min. C1 [Yuan, Feng] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, JOINGC SHAO & USTC, Shanghai 200030, Peoples R China. [Lin, Jun] Chinese Acad Sci, Natl Astron Observ, Yunnan Observ, Kunming 650011, Peoples R China. [Lin, Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wu, Kinwah] Univ Coll London, Mullard Space Sci Lab, Holmbury RH5 6NT, Surrey, England. [Ho, Luis C.] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA. RP Yuan, F (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, JOINGC SHAO & USTC, 80 Nandan Rd, Shanghai 200030, Peoples R China. EM fyuan@shao.ac.cn; jlin@ynao.ac.cn; kw@mssl.ucl.ac.uk; lho@ociw.edu RI LIN, JUN/B-9890-2017 FU Natural Science Foundation of China [10773024, 10833002, 10821302, 10825314, 10873030, 40636031]; One-Hundred-Talent Program of CAS; National Basic Research Program of China [2009CB824800, 2006CB806303]; Chinese Academy of Sciences [KJCX2-YWT04]; NASA [NNX07AL72G] FX We thank R. Matsumoto, J. E. Pringle, D. Uzdensky, F. Yusef-Zadeh and especially the anonymous referee for helpful comments and encouragements. This work was supported by the Natural Science Foundation of China (grants 10773024, 10833002, 10821302, 10825314, 10873030 and 40636031), One-Hundred-Talent Program of CAS and the National Basic Research Program of China (grants 2009CB824800 and 2006CB806303). JL was supported also by the Chinese Academy of Sciences (grant number KJCX2-YWT04) and NASA (grant number NNX07AL72G) when visiting CfA. NR 39 TC 53 Z9 57 U1 1 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2009 VL 395 IS 4 BP 2183 EP 2188 DI 10.1111/j.1365-2966.2009.14673.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446HL UT WOS:000266112600034 ER PT J AU Alyabyshev, SV Tscherbul, TV Krems, RV AF Alyabyshev, S. V. Tscherbul, T. V. Krems, R. V. TI Microwave-laser-field modification of molecular collisions at low temperatures SO PHYSICAL REVIEW A LA English DT Article DE atom-molecule collisions; calcium compounds; helium neutral atoms; molecule-photon collisions ID POLAR-MOLECULES; COLD; ATOMS; GAS AB We present a rigorous study of low-temperature collisions of polar molecules and atoms in a microwave laser field. Our calculations show that inelastic relaxation of molecules in a microwave cavity may occur through collision-induced absorption of photons stimulated by the anisotropy of the atom-molecule interaction potential. Our results indicate that molecular collisions at temperatures below 1 K can be efficiently manipulated with microwave laser fields of moderate strength. C1 [Alyabyshev, S. V.; Krems, R. V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Alyabyshev, SV (reprint author), Univ British Columbia, Dept Chem, 2036 Main Mall, Vancouver, BC V6T 1Z1, Canada. RI Tscherbul, Timur/K-3286-2014 OI Tscherbul, Timur/0000-0001-5689-040X FU NSERC; NSF FX We acknowledge useful discussions with Moshe Shapiro. This work was supported by NSERC and NSF grants to the Harvard-MIT Center for Ultracold Atoms and the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 22 TC 13 Z9 13 U1 1 U2 4 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 JUN PY 2009 VL 79 IS 6 AR 060703 DI 10.1103/PhysRevA.79.060703 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100012 ER PT J AU Chen, GX Kirby, K Brickhouse, NS Lin, T Silver, E AF Chen, G. X. Kirby, K. Brickhouse, N. S. Lin, T. Silver, E. TI Dirac R-matrix method for the calculation of x-ray line polarization SO PHYSICAL REVIEW A LA English DT Article DE atom-electron collisions; electron impact excitation; excited states; iron; positive ions ID ELECTRON-BEAM; FE-XVII; SOLAR-FLARES; HE-LIKE; EXCITATION; EMISSION; IONS; DIAGNOSTICS; RADIATION; SUBLEVELS AB We have developed a method within the Dirac R-matrix theory to calculate x-ray line polarization resulting from electron-impact excitation to excited-state magnetic sublevels of complex ions. We apply this method to the excitation of two well-known x-ray lines of Fe XVII, 3C (lambda=15.015 A degrees) and 3D (lambda=15.262 A degrees). We find strong resonance effects which contribute to complicated energy dependence in the polarization. Our results show large differences, up to 30% or more, from earlier theoretical work, and thus provide a stimulus for direct experimental measurement of the 3C and 3D line polarizations and further theoretical studies. C1 [Chen, G. X.; Kirby, K.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Chen, GX (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 FU NSF; Smithsonian Astrophysical Observatory (SAO); NASA to SAO [TM8-9001X, NAS8-03060, NNX08AK33G-R] FX This work was supported by NSF through a grant to the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory (SAO) and by NASA to SAO through Grants No. TM8-9001X, No. NAS8-03060, and No. NNX08AK33G-R. NR 27 TC 8 Z9 8 U1 0 U2 0 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 JUN PY 2009 VL 79 IS 6 AR 062715 DI 10.1103/PhysRevA.79.062715 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100095 ER PT J AU Kastel, J Fleischhauer, M Yelin, SF Walsworth, RL AF Kaestel, Juergen Fleischhauer, Michael Yelin, Susanne F. Walsworth, Ronald L. TI Low-loss negative refraction by laser-induced magnetoelectric cross coupling SO PHYSICAL REVIEW A LA English DT Article DE impedance matching; magnetic permeability; magnetoelectric effects; optical losses; quantum interference phenomena; refraction; refractive index ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; INDEX METAMATERIALS; BIANISOTROPIC MEDIA; LEFT-HANDEDNESS; PERFECT-LENS; PERMEABILITY; WAVELENGTHS; OPTICS AB We discuss the feasibility of negative refraction with reduced absorption in coherently driven atomic media. Coherent coupling of an electric and a magnetic dipole transition by laser fields induces magnetoelectric cross coupling and negative refraction at dipole densities which are considerably smaller than necessary to achieve a negative permeability. At the same time the absorption gets minimized due to destructive quantum interference and the ratio of negative refraction index to absorption becomes orders of magnitude larger than in systems without coherent cross coupling. The proposed scheme allows for a fine tuning of the refractive index. We derive a generalized expression for the impedance of a medium with magnetoelectric cross coupling and show that impedance matching to vacuum can easily be achieved. Finally we discuss the tensorial properties of the medium response and derive expressions for the dependence of the refractive index on the propagation direction. C1 [Kaestel, Juergen; Fleischhauer, Michael] Tech Univ Kaiserslautern, Fachbereich Phys, D-67663 Kaiserslautern, Germany. [Yelin, Susanne F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kastel, J (reprint author), Tech Univ Kaiserslautern, Fachbereich Phys, D-67663 Kaiserslautern, Germany. RI Fleischhauer, Michael/G-6716-2011 NR 52 TC 13 Z9 13 U1 0 U2 2 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 JUN PY 2009 VL 79 IS 6 AR 063818 DI 10.1103/PhysRevA.79.063818 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100168 ER PT J AU Tang, LY Yan, ZC Shi, TY Babb, JF AF Tang, Li-Yan Yan, Zong-Chao Shi, Ting-Yun Babb, James F. TI Nonrelativistic ab initio calculations for 2 S-2, 2 P-2, and 3 D-2 lithium isotopes: Applications to polarizabilities and dispersion interactions SO PHYSICAL REVIEW A LA English DT Article DE ab initio calculations; excited states; ground states; lithium; polarisability; wave functions ID LONG-RANGE INTERACTIONS; VARIATIONAL CALCULATIONS; QUADRUPOLE POLARIZABILITIES; DIPOLE POLARIZABILITIES; ATOMIC LITHIUM; EXCITED-STATES; STARK SHIFTS; ALKALI ATOMS; HYPERPOLARIZABILITY; IONS AB The electric dipole polarizabilities and hyperpolarizabilities for the lithium isotopes Li-6 and Li-7 in the ground state 2 S-2 and the excited states 2 P-2 and 3 D-2, as well as the leading resonance and dispersion long-range coefficients for the Li(2 S-2)-Li(2 S-2) and Li(2 S-2)-Li(2 P-2) systems, are calculated nonrelativistically using variational wave functions in Hylleraas basis sets. Comparisons are made with published results, where available. We find that the value of the second hyperpolarizability of the 2 S-2 state is sensitive to the isotopic mass due to a near cancellation between two terms. For the 3 D-2 state polarizability tensor, the calculated components disagree with those measured in the sole experiment and with those calculated semiempirically. C1 [Tang, Li-Yan; Shi, Ting-Yun] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. [Tang, Li-Yan] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Yan, Zong-Chao] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. [Yan, Zong-Chao] Harbin Inst Technol, Acad Fundamental & Interdisciplinary Sci, Ctr Theoret Atom & Mol Phys, Harbin 150080, Peoples R China. [Babb, James F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Tang, LY (reprint author), Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. RI Shi, Tingyun/I-6022-2013; Yan, Zong-Chao/F-6668-2014 NR 57 TC 34 Z9 35 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 2009 VL 79 IS 6 AR 062712 DI 10.1103/PhysRevA.79.062712 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100092 ER PT J AU Tscherbul, TV Zhang, P Sadeghpour, HR Dalgarno, A AF Tscherbul, T. V. Zhang, P. Sadeghpour, H. R. Dalgarno, A. TI Collision-induced spin exchange of alkali-metal atoms with He-3: An ab initio study SO PHYSICAL REVIEW A LA English DT Article DE ab initio calculations; atom-atom collisions; helium neutral atoms; lithium; potassium; potential energy surfaces; rubidium; sodium ID CORRELATED MOLECULAR CALCULATIONS; HYPERFINE COUPLING-CONSTANTS; GAUSSIAN-BASIS SETS; GROUND-STATE; MILLIKELVIN TEMPERATURES; ROTATION INTERACTION; CROSS-SECTIONS; EARTH ATOMS; GAS; SCATTERING AB We present a rigorous quantum study of spin-exchange transitions in collisions of the alkali-metal atoms with He-3 in the presence of an external magnetic field. Using accurate ab initio interaction potentials, we obtain refined estimates for the Fermi contact interaction constants for complexes of Na, K, and Rb atoms with He-3. Ab initio calculations show that the Fermi contact interaction in Li-He-3 varies more slowly with internuclear distance than predicted by the atomic model [R. M. Herman, Phys. Rev. 37, A1062 (1965)]. The calculated spin-exchange rate constants for Na, K, and Rb atoms in a gas of He-3 are in good agreement with experimental data. Our calculations demonstrate that at a temperature of 0.5 K, collision-induced spin exchange of the alkali-metal atoms occurs at a very slow rate of similar to 10(-22) cm(3)/s, suggesting potential applications in cryogenic cooling, precision spectroscopy, and quantum optics. C1 [Tscherbul, T. V.; Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.; Zhang, P.; Sadeghpour, H. R.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM tshcherb@cfa.harvard.edu RI Tscherbul, Timur/K-3286-2014 OI Tscherbul, Timur/0000-0001-5689-040X FU Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U. S. Department of Energy; NSF FX This work was supported by the Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, U. S. Department of Energy and NSF grants to the Harvard-MIT Center for Ultracold Atoms and the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 59 TC 13 Z9 13 U1 0 U2 10 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 JUN PY 2009 VL 79 IS 6 AR 062707 DI 10.1103/PhysRevA.79.062707 PG 11 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 466XZ UT WOS:000267700100087 ER PT J AU Su, M Yadav, APS Zaldarriaga, M AF Su, Meng Yadav, Amit P. S. Zaldarriaga, Matias TI Impact of instrumental systematic contamination on the lensing mass reconstruction using the CMB polarization SO PHYSICAL REVIEW D LA English DT Article ID MICROWAVE BACKGROUND POLARIZATION; POWER SPECTRUM; GRAVITY-WAVES; DARK-MATTER; ANISOTROPIES; PROBE; MAPS; GHZ AB In this paper, we study the effects of instrumental systematics on the reconstruction of the deflection angle power spectrum from weak lensing of cosmic microwave background (CMB) temperature and polarization observations. We consider 7 types of effects which are related to known instrumental systematics: calibration, rotation, pointing, spin-flip, monopole leakage, dipole leakage, and quadrupole leakage. These effects can result in the distortion in the CMB field and can be characterized by 11 distortion fields. Each of these systematic effects can mimic the effective projected matter power spectrum and hence contaminate the lensing reconstruction. To demonstrate the effect of these instrumental systematics on CMB lensing measurements, we consider two types of experiments: one with a detector noise level for polarization of 9.6 mu K arcmin and FWHM of 8.0', typical of upcoming ground and balloon-based CMB experiments; and a CMBPol-like instrument with a detector noise level for polarization of 2.0 mu K arcmin and FWHM of 4.0', typical of future space-based CMB experiments. For each systematics field, we consider various choices of coherence scale alpha(s), starting from alpha(s) = 10' to the maximum of alpha(s) = 120'. Among all the 11 systematic parameters, rotation omega, and monopole leakage gamma(a) & gamma(b) place the most stringent requirements, while quadrupole leakage q, pointing error p(a) and p(b), and calibration a are among the least demanding. The requirements from lensing extraction are about 1-2 orders of magnitude less stringent than the requirements to measure the primordial B modes with an inflationary energy scale of 1.0 X 10(16) GeV. On the other hand, the requirements for lensing reconstruction are comparable or even more stringent for some systematic parameters than the requirements to detect primordial B modes with an inflationary scale of E(i) = 3.0 X 10(16) GeV. C1 [Su, Meng; Yadav, Amit P. S.; Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP Su, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mengsu@cfa.harvard.edu RI Su, Meng/J-4211-2013 FU Harard University; NASA [NNG05GJ40G]; NSF [AST-0506556]; David and Lucile Packard, Alfred P. Sloan, and John D. and Catherine T. MacArthur foundations FX M. S. was supported in part by Philip Putnam Chase. A.P.S.Y. thanks Daniel Baumann, Ben Wandelt, Scott Kruger, Oliver Zahn, and Jaiyul Yoo for useful discussions and help during the project, and acknowledge support from Harard University. M.Z. was supported by NASA NNG05GJ40G and NSF AST-0506556 as well as the David and Lucile Packard, Alfred P. Sloan, and John D. and Catherine T. MacArthur foundations. We especially thank Daniel Baumann for reading the manuscript and providing useful feedback. NR 63 TC 7 Z9 7 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD JUN PY 2009 VL 79 IS 12 AR 123002 DI 10.1103/PhysRevD.79.123002 PG 22 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 466YN UT WOS:000267701500008 ER PT J AU Brostoff, LB Maynor, CI Speakman, RJ AF Brostoff, Lynn B. Maynor, Catherine I. Speakman, Robert J. TI Preliminary study of a Georgia O'Keeffe pastel drawing using XRF and mu XRD SO POWDER DIFFRACTION LA English DT Article DE XRF; XRD; pastel; pigment; red lead; O'Keeffe AB X-ray fluorescence spectrometry (XRF) and micro-X-ray diffraction (mu XRD) were used to analyze the composition of pigments on a pastel drawing, Special No. 32, by Georgia O'Keeffe. XRF analyses showed that, among other pigments present in the drawing, the red, orange, and yellow pigments may possibly be identified with lead- and chromium-based pigments: lead chromates, red and yellow lead oxides, and/or lead carbonates, plus calcium-based pastel fillers, such as whiting or gypsum. XRD examination of a sample removed from a dark mottled area of coral red pastel confirmed that this pigment layer, which is associated with a darkened appearance and high Pb:Cr ratios, matches the red lead oxide, minium (2PbO center dot PbO(2)). (C) 2009 International Centre for Diffraction Data. [DOI: 10.1154/1.3133137] C1 [Brostoff, Lynn B.] Lib Congress, Preservat Res & Testing Div, Washington, DC 20540 USA. [Brostoff, Lynn B.] Smithsonian Inst, Museum Conservat Inst, Washington, DC 20560 USA. [Maynor, Catherine I.] Lunder Conservat Ctr, Smithsonian Amer Art Museum, Washington, DC 20013 USA. [Speakman, Robert J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Brostoff, LB (reprint author), Lib Congress, Preservat Res & Testing Div, 101 Independence Ave SE, Washington, DC 20540 USA. NR 9 TC 5 Z9 5 U1 0 U2 3 PU J C P D S-INT CENTRE DIFFRACTION DATA PI NEWTOWN SQ PA 12 CAMPUS BLVD, NEWTOWN SQ, PA 19073-3273 USA SN 0885-7156 J9 POWDER DIFFR JI Powder Diffr. PD JUN PY 2009 VL 24 IS 2 BP 116 EP 123 DI 10.1154/1.3133137 PG 8 WC Materials Science, Characterization & Testing SC Materials Science GA 464RB UT WOS:000267522300013 ER PT J AU Launius, RD AF Launius, Roger D. TI Abandoned in Place: Interpreting the US Material Culture of the Moon Race SO PUBLIC HISTORIAN LA English DT Article DE Apollo program; Kennedy Space Center; Mission Control Center; Apollo Command Modules; Apollo lunar landing sites ID CHALLENGE; MEMORY AB The U.S. space race of the 1960 was an enormous undertaking, costing $25.4 billion (about $125 billion in 2009 dollars) with only the building of the Panama Canal rivalling the Apollo program's size as the largest nonmilitary technological endeavor ever undertaken by the United States. In the process, the United States built a massive infrastructure to support missions to the Moon. In the aftermath of the successful completion of the program, much of this infrastructure was abandoned, some was altered for other uses, and much torn down. This paper surveys six major cultural landmarks of the Moon race, assessing their differing fates: 1. The Apollo Launch Pads-LC 39A and B-Kennedy Space Center, Florida. 2. The Vertical Assembly Building (VAB), Kennedy Space Center, Florida. 3. Mission Control Center (MCC), Johnson Space Center, Houston, Texas. 4. Six Apollo landing sites on the Moon. 5. Lunar Landing Research Facility, Langley Research Center, Hampton, Virginia. 6. Apollo Command Modules on display in various museums around the nation, and in London. C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. [Launius, Roger D.] NASA, Washington, DC USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20560 USA. NR 91 TC 0 Z9 0 U1 3 U2 7 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SUM PY 2009 VL 31 IS 3 BP 9 EP 38 DI 10.1525/tph.2009.31.3.9 PG 30 WC History SC History GA 492YL UT WOS:000269698700002 ER PT J AU Clough, GW AF Clough, G. Wayne TI Lincoln Login 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 JUN PY 2009 VL 40 IS 3 BP 20 EP 20 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 448ID UT WOS:000266255400014 ER PT J AU Hudson, TM Turner, BL Herz, H Robinson, JS AF Hudson, Theresa M. Turner, Benjamin L. Herz, Hubert Robinson, James S. TI Temporal patterns of nutrient availability around nests of leaf-cutting ants (Atta colombica) in secondary moist tropical forest SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Barro Colorado Island; Nitrogen; Nutrient cycling; Panama; Phosphorus; Soil ID SOIL NUTRIENTS; CEPHALOTES; CHEMISTRY; HERBIVORY; AMAZONIA; COLONIES; PLANTS; PANAMA AB Leaf-cutting ants consume up to 10% of canopy leaves in the foraging area of their colony and therefore represent a key perturbation in the nutrient cycle of tropical forests. We used a chronosequence of nest sites on Barro, Colorado Island, Panama, to assess the influence of leaf-cutting ants (Atta colombica) on nutrient availability in a neotropical rainforest. Twelve nest sites were sampled, including active nests, recently abandoned nests (<1 year) and long-abandoned nests (>1 year). Waste material discarded by the ants down-slope from the nests contained large concentrations of nitrogen and phosphorus in both total and soluble forms, but decomposed within one year after the nests were abandoned. Despite this, soil under the waste material contained high concentrations of nitrate and ammonium that persisted after the disappearance of the waste, although soluble phosphate returned to background concentrations within one year of nest abandonment. Fine roots were more abundant in soil under waste than control soils up to one year after nest abandonment, but were not significantly different for older sites. In contrast to the waste dumps, soil above the underground nest chambers consistently contained lower nutrient concentrations than control soils, although this was not statistically significant. We conclude that the 'islands of fertility' created by leaf-cutting ants provide a nutritional benefit to nearby plants for less than one year after nest abandonment in the moist tropical environment of Barro Colorado Island. Published by Elsevier Ltd. C1 [Turner, Benjamin L.; Herz, Hubert] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hudson, Theresa M.; Robinson, James S.] Univ Reading, Dept Soil Sci, Sch Human & Environm Sci, Reading RG6 6DW, Berks, England. [Herz, Hubert] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM turnerbl@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Natural Environment Research Council FX This work was funded by the Natural Environment Research Council. We thank Carolina Chanis and Valerie Garrish for field and laboratory assistance and Alberto Vidal (University of Reading) for statistical advice. NR 24 TC 18 Z9 18 U1 0 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUN PY 2009 VL 41 IS 6 BP 1088 EP 1093 DI 10.1016/j.soilbio.2009.02.014 PG 6 WC Soil Science SC Agriculture GA 457OZ UT WOS:000266942900008 ER PT J AU Grim, KC Wolfe, M Braunbeck, T Iguchi, T Ohta, Y Tooi, O Touart, L Wolf, DC Tietge, J AF Grim, K. Christiana Wolfe, Marilyn Braunbeck, Thomas Iguchi, Taisen Ohta, Yasuhiko Tooi, Osamu Touart, Les Wolf, Douglas C. Tietge, Joe TI Thyroid Histopathology Assessments for the Amphibian Metamorphosis Assay to Detect Thyroid-active Substances SO TOXICOLOGIC PATHOLOGY LA English DT Article DE amphibia; metamorphosis; thyroid; histopathology; histology; Xenopus laevis ID ENDOCRINE DISRUPTORS; MODEL AB In support of an Organization for Economic Cooperation and Development (OECD) Amphibian Metamorphosis Assay (AMA) Test Guideline for the detection of substances that interact with the hypothalamic-pituitary-thyroid axis, a document was developed that provides a standardized approach for evaluating the histology/histopathology of thyroid glands in metamorphosing Xenopus laevis tadpoles. Here, a consolidated description of histology evaluation practices, core diagnostic criteria and severity grading schemes for the AMA, an atlas of the normal architecture of amphibian thyroid glands over the course of metamorphosis, and the core diagnostic criteria with examples of severity grades is provided. Core diagnostic criteria include thyroid gland hypertrophy/atrophy, follicular cell hypertrophy, and follicular cell hyperplasia. The severity grading scheme is semiquantitative and employs a four-grade approach describing ranges of variation within assigned ordinal classes: not remarkable, mild, moderate, and severe. The purpose of this severity grading approach is to provide an efficient, semi-objective tool for comparing changes (compound-related effects) among animals, treatment groups, and studies. Proposed descriptions of lesions for scoring the four core criteria are also given. C1 [Grim, K. Christiana] Ctr Species Survival, Conservat Res Ctr, Front Royal, VA 22630 USA. [Grim, K. Christiana; Touart, Les] US EPA, Off Sci Coordinat & Policy, Washington, DC 20460 USA. [Wolfe, Marilyn] Expt Pathol Labs Inc, Sterling, VA USA. [Braunbeck, Thomas] Univ Heidelberg, Dept Zool, Aquat Ecol & Toxicol Grp, D-6900 Heidelberg, Germany. [Iguchi, Taisen] Natl Inst Nat Sci, Natl Inst Basic Biol, Dept Bioenvironm Sci, Okazaki Inst Integrat Biosci,Div Bioenvironm Sci, Aichi, Japan. [Ohta, Yasuhiko] Tottori Univ, Fac Agr, Dept Vet Med, Anim Expt Lab, Koyama, Japan. [Tooi, Osamu] IDEA Consultants Inc, Inst Environm Ecol, Shizuoka, Japan. [Wolf, Douglas C.; Tietge, Joe] US EPA, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Res Triangle Pk, NC 27711 USA. [Wolf, Douglas C.; Tietge, Joe] US EPA, Natl Hlth & Environm Effects Res Lab, Off Res & Dev, Duluth, MN USA. RP Grim, KC (reprint author), Ctr Species Survival, Conservat Res Ctr, Smithsonian Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM grim.christiana@epa.gov OI Braunbeck, Thomas/0000-0002-1785-6759 NR 10 TC 22 Z9 23 U1 0 U2 3 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0192-6233 J9 TOXICOL PATHOL JI Toxicol. Pathol. PD JUN PY 2009 VL 37 IS 4 BP 415 EP 424 DI 10.1177/0192623309335063 PG 10 WC Pathology; Toxicology SC Pathology; Toxicology GA 463YW UT WOS:000267471200002 PM 19387088 ER PT J AU Mawdsley, JR AF Mawdsley, Jonathan R. TI Taxonomy, ecology, and phylogeny of species of Lophyra Motschulsky 1859, subgenus Eriolophyra Rivalier 1948 (Coleoptera Cicindelidae) SO TROPICAL ZOOLOGY LA English DT Article DE Eriolophyra; Cicindelidae; ecology; phylogeny; morphology; distribution ID TIGER BEETLES; CONSERVATION; PATTERNS AB A key is provided for the identification of the five species of the subgenus Eriolophyra Rivalier 1948 of the genus Lophyra Motschulsky 1859 (Coleoptera Cicindelidae): L. (E.) alba (Horn 1894); L. (E.) albens (Horn 1895); L. (E.) arnoldi (Horn 1904); L. (E.) barbifrons (Boheman 1848); and L. (E.) somalia (Fairmaire 1882). The taxonomy of this subgenus is reviewed and Lophyra (Eriolophyra) barbifrons marqueza (Peringuey 1896) is placed as a synonym of L. (E.) barbifrons. Information about the ecology of species of Lophyra (Eriolophyra) is summarized: Lophyra (Eriolophyra) alba, L. (E.) albens, and L. (E.) arnoldi are associated with sandy riverine areas in southern, central, and west-central Africa, respectively, while L. (E.) barbifrons and L. (E.) somalia are associated with coastal sand beaches in southern and eastern Africa, respectively. Descriptions of adult foraging, thermoregulatory, reproductive, and defensive behaviors are provided for L. (E.) alba, based on recent observations at sites along the Letaba River in Kruger National Park, South Africa. A hypothesis of phylogenetic relationships is proposed for the five species of the subgenus Eriolophyra on the basis of adult morphological characteristics. Morphological characters suggest that this group forms a monophyletic clade within the broader complex of species allied to Lophyra. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzctr.org NR 41 TC 4 Z9 4 U1 0 U2 2 PU CENTRO STUDIO FAUNISTICA ECOLOGIA TROPICALI, C N R PI FLORENCE PA VIA ROMANA 17, 50125 FLORENCE, ITALY SN 0394-6975 J9 TROP ZOOL JI Trop. Zool. PD JUN PY 2009 VL 22 IS 1 BP 57 EP 70 PG 14 WC Zoology SC Zoology GA 492BG UT WOS:000269628400004 ER PT J AU Keogh, E Wei, L Xi, XP Vlachos, M Lee, SH Protopapas, P AF Keogh, Eamonn Wei, Li Xi, Xiaopeng Vlachos, Michail Lee, Sang-Hee Protopapas, Pavlos TI Supporting exact indexing of arbitrarily rotated shapes and periodic time series under Euclidean and warping distance measures SO VLDB JOURNAL LA English DT Article DE Shape; Indexing; Dynamic time warping ID RECOGNITION; CONTOUR; CURVES; REPRESENTATION; APPROXIMATE; ALGORITHM; SPACES AB Shape matching and indexing is important topic in its own right, and is a fundamental subroutine in most shape data mining algorithms. Given the ubiquity of shape, shape matching is an important problem with applications in domains as diverse as biometrics, industry, medicine, zoology and anthropology. The distance/similarity measure for used for shape matching must be invariant to many distortions, including scale, offset, noise, articulation, partial occlusion, etc. Most of these distortions are relatively easy to handle, either in the representation of the data or in the similarity measure used. However, rotation invariance is noted in the literature as being an especially difficult challenge. Current approaches typically try to achieve rotation invariance in the representation of the data, at the expense of discrimination ability, or in the distance measure, at the expense of efficiency. In this work, we show that we can take the slow but accurate approaches and dramatically speed them up. On real world problems our technique can take current approaches and make them four orders of magnitude faster without false dismissals. Moreover, our technique can be used with any of the dozens of existing shape representations and with all the most popular distance measures including Euclidean distance, dynamic time warping and Longest Common Subsequence. We further show that our indexing technique can be used to index star light curves, an important type of astronomical data, without modification. C1 [Keogh, Eamonn; Wei, Li; Xi, Xiaopeng] Univ Calif Riverside, Dept Comp Sci & Engn, Riverside, CA 92521 USA. [Vlachos, Michail] IBM TJ Watson Res Ctr, Yorktown Hts, NY USA. [Lee, Sang-Hee] UCR, Dept Anthropol, Riverside, CA USA. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keogh, E (reprint author), Univ Calif Riverside, Dept Comp Sci & Engn, Riverside, CA 92521 USA. EM eamonn@cs.ucr.edu OI Vlachos, Michail/0000-0003-1008-5290 NR 43 TC 45 Z9 48 U1 1 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1066-8888 J9 VLDB J JI VLDB J. PD JUN PY 2009 VL 18 IS 3 BP 611 EP 630 DI 10.1007/s00778-008-0111-4 PG 20 WC Computer Science, Hardware & Architecture; Computer Science, Information Systems SC Computer Science GA 451GV UT WOS:000266459600002 ER PT J AU Whigham, D Verhoeven, JTA AF Whigham, Dennis Verhoeven, Jos T. A. TI Wetlands of the World: the next installment SO WETLANDS ECOLOGY AND MANAGEMENT LA English DT Editorial Material C1 [Whigham, Dennis] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Verhoeven, Jos T. A.] Univ Utrecht, Utrecht, Netherlands. RP Whigham, D (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM whighamd@si.edu; j.t.a.verhoeven@uu.nl RI Verhoeven, Jos/B-9514-2011; OI Whigham, Dennis/0000-0003-1488-820X NR 0 TC 0 Z9 2 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-4861 J9 WETL ECOL MANAG JI Wetl. Ecol. Manag. PD JUN PY 2009 VL 17 IS 3 BP 167 EP 167 DI 10.1007/s11273-009-9133-y PG 1 WC Environmental Sciences; Water Resources SC Environmental Sciences & Ecology; Water Resources GA 442QV UT WOS:000265856600001 ER PT J AU Cappellaro, P Jiang, L Hodges, JS Lukin, MD AF Cappellaro, P. Jiang, L. Hodges, J. S. Lukin, M. D. TI Coherence and Control of Quantum Registers Based on Electronic Spin in a Nuclear Spin Bath SO PHYSICAL REVIEW LETTERS LA English DT Article ID COUPLED ELECTRON; DIAMOND; DYNAMICS; ENTANGLEMENT; PULSES; DESIGN; QUBITS; ATOM AB We consider a protocol for the control of few-qubit registers comprising one electronic spin embedded in a nuclear spin bath. We show how to isolate a few proximal nuclear spins from the rest of the bath and use them as building blocks for a potentially scalable quantum information processor. We describe how coherent control techniques based on magnetic resonance methods can be adapted to these solid-state spin systems, to provide not only efficient, high fidelity manipulation but also decoupling from the spin bath. As an example, we analyze feasible performances and practical limitations in the realistic setting of nitrogen-vacancy centers in diamond. C1 [Cappellaro, P.; Lukin, M. D.] Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cappellaro, P.; Jiang, L.; Hodges, J. S.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hodges, J. S.] MIT, Dept Nucl Sci & Engn, Cambridge, MA 02139 USA. RP Cappellaro, P (reprint author), Harvard Univ, Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RI Hodges, Jonathan/G-1034-2010; Cappellaro, Paola/B-1413-2010; Jiang, Liang/A-9847-2008; OI Cappellaro, Paola/0000-0003-3207-594X; Jiang, Liang/0000-0002-0000-9342; Hodges, Jonathan/0000-0002-3487-6698 FU NSF; ITAMP; DARPA; David and Lucile Packard Foundation FX This work was supported by NSF, ITAMP, DARPA, and the David and Lucile Packard Foundation. NR 36 TC 62 Z9 62 U1 0 U2 11 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 MAY 29 PY 2009 VL 102 IS 21 AR 210502 DI 10.1103/PhysRevLett.102.210502 PG 4 WC Physics, Multidisciplinary SC Physics GA 451WM UT WOS:000266501600005 PM 19519089 ER PT J AU Miller, AW Reynolds, AC Sobrino, C Riedel, GF AF Miller, A. Whitman Reynolds, Amanda C. Sobrino, Cristina Riedel, Gerhardt F. TI Shellfish Face Uncertain Future in High CO2 World: Influence of Acidification on Oyster Larvae Calcification and Growth in Estuaries SO PLOS ONE LA English DT Article AB Background: Human activities have increased atmospheric concentrations of carbon dioxide by 36% during the past 200 years. One third of all anthropogenic CO2 has been absorbed by the oceans, reducing pH by about 0.1 of a unit and significantly altering their carbonate chemistry. There is widespread concern that these changes are altering marine habitats severely, but little or no attention has been given to the biota of estuarine and coastal settings, ecosystems that are less pH buffered because of naturally reduced alkalinity. Methodology/Principal Findings: To address CO2-induced changes to estuarine calcification, veliger larvae of two oyster species, the Eastern oyster (Crassostrea virginica), and the Suminoe oyster (Crassostrea ariakensis) were grown in estuarine water under four pCO(2) regimes, 280, 380, 560 and 800 mu atm, to simulate atmospheric conditions in the pre-industrial era, present, and projected future concentrations in 50 and 100 years respectively. CO2 manipulations were made using an automated negative feedback control system that allowed continuous and precise control over the pCO(2) in experimental aquaria. Larval growth was measured using image analysis, and calcification was measured by chemical analysis of calcium in their shells. C. virginica experienced a 16% decrease in shell area and a 42% reduction in calcium content when pre-industrial and end of 21(st) century pCO(2) treatments were compared. C. ariakensis showed no change to either growth or calcification. Both species demonstrated net calcification and growth, even when aragonite was undersaturated, a result that runs counter to previous expectations for invertebrate larvae that produce aragonite shells. Conclusions and Significance: Our results suggest that temperate estuarine and coastal ecosystems are vulnerable to the expected changes in water chemistry due to elevated atmospheric CO2 and that biological responses to acidification, especially calcifying biota, will be species-specific and therefore much more variable and complex than reported previously. RP Miller, AW (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM millerw@si.edu OI Sobrino, Cristina/0000-0003-0431-1220; Miller, Whitman/0000-0003-0484-182X NR 47 TC 131 Z9 135 U1 9 U2 116 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 MAY 27 PY 2009 VL 4 IS 5 AR e5661 DI 10.1371/journal.pone.0005661 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 450QD UT WOS:000266415000003 PM 19478855 ER PT J AU Hoppenrath, M Bachvaroff, TR Handy, SM Delwiche, CF Leander, BS AF Hoppenrath, Mona Bachvaroff, Tsvetan R. Handy, Sara M. Delwiche, Charles F. Leander, Brian S. TI Molecular phylogeny of ocelloid-bearing dinoflagellates (Warnowiaceae) as inferred from SSU and LSU rDNA sequences SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID RIBOSOMAL-RNA GENE; REAL-TIME PCR; GYRODINIUM DINOPHYCEAE; WARNOWIIDAE-LINDEMANN; EVOLUTIONARY HISTORY; NOV GYMNODINIALES; DNA-SEQUENCES; SUBUNIT RDNA; ULTRASTRUCTURE; AMPHIDINIUM AB Background: Dinoflagellates represent a major lineage of unicellular eukaryotes with unparalleled diversity and complexity in morphological features. The monophyly of dinoflagellates has been convincingly demonstrated, but the interrelationships among dinoflagellate lineages still remain largely unresolved. Warnowiid dinoflagellates are among the most remarkable eukaryotes known because of their possession of highly elaborate ultrastructural systems: pistons, nematocysts, and ocelloids. Complex organelles like these are evolutionary innovations found only in a few athecate dinoflagellates. Moreover, the taxonomy of warnowiids is extremely confusing and inferences about the evolutionary history of this lineage are mired by the absence of molecular phylogenetic data from any member of the group. In this study, we provide the first molecular phylogenetic data for warnowiids and couple them with a review of warnowiid morphological features in order to formulate a hypothetical framework for understanding character evolution within the group. These data also enabled us to evaluate the evolutionary relationship(s) between warnowiids and the other group of dinoflagellates with complex organelles: polykrikoids. Results: Molecular phylogenetic analyses of SSU and LSU rDNA sequences demonstrated that warnowiids form a well-supported clade that falls within the more inclusive Gymnodinium sensu stricto clade. These data also confirmed that polykrikoids are members of the Gymnodinium sensu stricto clade as well; however, a specific sister relationship between the warnowiid clade and the polykrikoid clade was unresolved in all of our analyses. Nonetheless, the new DNA sequences from different isolates of warnowiids provided organismal anchors for several previously unidentified sequences derived from environmental DNA surveys of marine biodiversity. Conclusion: Comparative morphological data and molecular phylogenetic data demonstrate that the polykrikoid and the warnowiid clade are closely related to each other, but the precise branching order within the Gymnodinium sensu stricto clade remains unresolved. We regard the ocelloid as the best synapomorphy for warnowiids and infer that the most recent common ancestor of polykrikoids and warnowiids possessed both nematocysts and photosynthetic plastids that were subsequently lost during the early evolution of warnowiids. Our summary of species and genus concepts in warnowiids demonstrate that the systematics of this poorly understood group is highly problematic and a comprehensive revision is needed. C1 [Hoppenrath, Mona; Leander, Brian S.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Bachvaroff, Tsvetan R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hoppenrath, Mona; Leander, Brian S.] Univ British Columbia, Dept Bot, Vancouver, BC V6T 1Z4, Canada. [Handy, Sara M.; Delwiche, Charles F.] Univ Maryland, Dept Mol Genet & Cell Biol, College Pk, MD 20742 USA. RP Hoppenrath, M (reprint author), DZMB, Forsch Inst Senckenberg, Sudstrand 44, D-26382 Wilhelmshaven, Germany. EM mhoppenrath@senckenberg.de; bachvarofft@si.edu; shandy@umd.edu; delwiche@umd.edu; bleander@interchange.ubc.ca RI Handy, Sara/C-6195-2008; OI Delwiche, Charles/0000-0001-7854-8584 FU Deutsche Forschungsgemeinschaft [Ho3267/1-1]; Science Foundation - Assembling the Tree of Life [EF-0629624]; National Science and Engineering Research Council of Canada [283091-04] FX This work was supported by a postdoctoral research salary to MH from the Deutsche Forschungsgemeinschaft ( grant Ho3267/1-1) and operating funds from the Science Foundation - Assembling the Tree of Life ( NSF #EF-0629624) and the National Science and Engineering Research Council of Canada ( NSERC 283091-04). BSL is a fellow of the Canadian Institute for Advanced Research, Program in Integrated Microbial Biodiversity. NR 70 TC 31 Z9 33 U1 3 U2 23 PU BIOMED CENTRAL LTD PI LONDON PA CURRENT SCIENCE GROUP, MIDDLESEX HOUSE, 34-42 CLEVELAND ST, LONDON W1T 4LB, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD MAY 25 PY 2009 VL 9 AR 116 DI 10.1186/1471-2148-9-116 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 467QV UT WOS:000267758400001 PM 19467154 ER PT J AU Squyres, SW Knoll, AH Arvidson, RE Ashley, JW Bell, JF Calvin, WM Christensen, PR Clark, BC Cohen, BA de Souza, PA Edgar, L Farrand, WH Fleischer, I Gellert, R Golombek, MP Grant, J Grotzinger, J Hayes, A Herkenhoff, KE Johnson, JR Jolliff, B Klingelhofer, G Knudson, A Li, R Mccoy, TJ McLennan, SM Ming, DW Mittlefehldt, DW Morris, RV Rice, JW Schroder, C Sullivan, RJ Yen, A Yingst, RA AF Squyres, S. W. Knoll, A. H. Arvidson, R. E. Ashley, J. W. Bell, J. F., III Calvin, W. M. Christensen, P. R. Clark, B. C. Cohen, B. A. de Souza, P. A., Jr. Edgar, L. Farrand, W. H. Fleischer, I. Gellert, R. Golombek, M. P. Grant, J. Grotzinger, J. Hayes, A. Herkenhoff, K. E. Johnson, J. R. Jolliff, B. Klingelhoefer, G. Knudson, A. Li, R. McCoy, T. J. McLennan, S. M. Ming, D. W. Mittlefehldt, D. W. Morris, R. V. Rice, J. W., Jr. Schroeder, C. Sullivan, R. J. Yen, A. Yingst, R. A. TI Exploration of Victoria Crater by the Mars Rover Opportunity SO SCIENCE LA English DT Article ID MERIDIANI-PLANUM; BURNS FORMATION AB The Mars rover Opportunity has explored Victoria crater, a similar to 750-meter eroded impact crater formed in sulfate-rich sedimentary rocks. Impact-related stratigraphy is preserved in the crater walls, and meteoritic debris is present near the crater rim. The size of hematite-rich concretions decreases up-section, documenting variation in the intensity of groundwater processes. Layering in the crater walls preserves evidence of ancient wind-blown dunes. Compositional variations with depth mimic those similar to 6 kilometers to the north and demonstrate that water-induced alteration at Meridiani Planum was regional in scope. C1 [Squyres, S. W.; Bell, J. F., III; Sullivan, R. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Knoll, A. H.] Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. [Arvidson, R. E.; Jolliff, B.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63031 USA. [Ashley, J. W.; Christensen, P. R.; Knudson, A.; Rice, J. W., Jr.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Calvin, W. M.] Univ Nevada, Reno, NV 89557 USA. [Clark, B. C.] Lockheed Martin Corp, Littleton, CO 80127 USA. [Cohen, B. A.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [de Souza, P. A., Jr.] CSIRO, Tasmanian Informat & Commun Technol Ctr, Hobart, Tas 7000, Australia. [Edgar, L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Fleischer, I.; Klingelhoefer, G.; Schroeder, C.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Golombek, M. P.; Yen, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grant, J.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Herkenhoff, K. E.; Johnson, J. R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Li, R.] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. [McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [McLennan, S. M.] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA. [Ming, D. W.; Mittlefehldt, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Yingst, R. A.] Univ Wisconsin, Green Bay, WI 54311 USA. RP Squyres, SW (reprint author), Cornell Univ, Dept Astron, Space Sci Bldg, Ithaca, NY 14853 USA. EM squyres@astro.cornell.edu RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011; Hayes, Alexander/P-2024-2014; Johnson, Jeffrey/F-3972-2015 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; Hayes, Alexander/0000-0001-6397-2630; FU NASA FX This research was carried out for the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 23 TC 76 Z9 76 U1 0 U2 24 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 MAY 22 PY 2009 VL 324 IS 5930 BP 1058 EP 1061 DI 10.1126/science.1170355 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448EU UT WOS:000266246700038 PM 19461001 ER PT J AU Western, D Behrensmeyer, AK AF Western, David Behrensmeyer, Anna K. TI Bone Assemblages Track Animal Community Structure over 40 Years in an African Savanna Ecosystem SO SCIENCE LA English DT Article ID DEATH ASSEMBLAGES; FIDELITY; PRESERVATION; ABUNDANCE; CLIMATE; RECORD; KENYA; SIZE AB Reconstructing ancient communities depends on how accurately fossil assemblages retain information about living populations. We report a high level of fidelity between modern bone assemblages and living populations based on a 40-year study of the Amboseli ecosystem in southern Kenya. Relative abundance of 15 herbivorous species recorded in the bone assemblage accurately tracks the living populations through major changes in community composition and habitat over intervals as short as 5 years. The aggregated bone sample provides an accurate record of community structure time-averaged over four decades. These results lay the groundwork for integrating paleobiological and contemporary ecological studies across evolutionary and ecological time scales. Bone surveys also provide a useful method of assessing population changes and community structure for modern vertebrates. C1 [Western, David] African Conservat Ctr, Nairobi, Kenya. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. RP Western, D (reprint author), African Conservat Ctr, Box 62844, Nairobi, Kenya. EM dwestern@africaonline.co.ke; behrensa@si.edu FU Ford Foundation; Wildlife Conservation Society; Liz Claiborne Art Ortenberg Foundation; National Geographic Society [1508, 4339-90, 7525-03]; Simithsonian Institution FX D.W.'s ecological studies have been supported by the Ford Foundation, Wildlife Conservation Society, and Liz Claiborne Art Ortenberg Foundation. We acknowledge the statistical assistance of V. Mose, T. Faith, G. Hunt, S. Kidwell, and A. Tomasovych and the field support of D. Maitumo. A.K.B.'s taphonomic research has been supported by the National Geographic Society (grants 1508, 4339-90, and 7525-03) and the Simithsonian Institution. Particular thanks are due to D.D. Boaz, J. Altmann, E. Kanga, F. Odock, and many other individuals who provided essential advice and help with the bone surveys. Permission for the studies was granted by the Office of the President, Kenya, and institutional support over the years was provided by the Kenya Wildlife Service and the National Museums of Kenya. NR 30 TC 38 Z9 39 U1 0 U2 3 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 MAY 22 PY 2009 VL 324 IS 5930 BP 1061 EP 1064 DI 10.1126/science.1171155 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 448EU UT WOS:000266246700039 PM 19461002 ER PT J AU Richardson, JD Stone, EC Kasper, JC Belcher, JW Decker, RB AF Richardson, J. D. Stone, E. C. Kasper, J. C. Belcher, J. W. Decker, R. B. TI Plasma flows in the heliosheath SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WIND TERMINATION SHOCK; SOLAR-WIND AB Voyager 2 is making the first plasma measurements in the heliosheath. The radial flow speeds in the heliosheath vary between 80 and 200 km/s with an average speed of 138 km/s. The flow in the T (azimuthal) direction is fairly constant and averages about 48 km/s; the flow direction is consistent with flow away from the heliospheric nose. Flow in the N (meridional) direction is also away from the nose and averages -14 km/s. These flows suggest that the shock is blunter in the T than in the N direction, so that the heliosphere is wider than it is high. The flow in the RN plane has quasi-periodic oscillation with a period of 110 days and an amplitude of 21 km/s. The oscillation in flow angle is about 6 degrees in the RN plane and 17 degrees in the TN plane and may result from periodic variations of the termination shock normal direction. Citation: Richardson, J. D., E. C. Stone, J. C. Kasper, J. W. Belcher, and R. B. Decker (2009), Plasma flows in the heliosheath, Geophys. Res. Lett., 36, L10102, doi: 10.1029/2009GL038421. C1 [Richardson, J. D.; Belcher, J. W.] MIT, Kavli Ctr Astrophys & Space Sci, Cambridge, MA 02139 USA. [Decker, R. B.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stone, E. C.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Richardson, JD (reprint author), MIT, Kavli Ctr Astrophys & Space Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM jdr@space.mit.edu; ecs@srl.caltech.edu; jkasper@cfa.harvard.edu; jwb@space.mit.edu; robert.decker@jhuapl.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NASA [959203, NNX07AB02G.]; Massachusetts Institute of Technology and NASA [NAG5-8947, NNX08AC04G, NAS7-03001] FX The work at MIT was supported under NASA contract 959203 from the Jet Propulsion Laboratory to the Massachusetts Institute of Technology and NASA grants NAG5-8947 and NNX08AC04G. The work at JHU/APL was supported by the Voyager Interstellar Mission under NASA grant NNX07AB02G. The work at Caltech was supported by NASA grant NAS7-03001. NR 15 TC 25 Z9 25 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD MAY 21 PY 2009 VL 36 AR L10102 DI 10.1029/2009GL038421 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 449XC UT WOS:000266363000006 ER PT J AU Wyithe, JSB Loeb, A AF Wyithe, J. Stuart B. Loeb, Abraham TI Evidence for merger-driven activity in the clustering of high-redshift quasars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE large scale structure of Universe; cosmology: theory; quasars: general ID DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES; LYMAN BREAK GALAXIES; DARK-MATTER HALOES; BH-SIGMA RELATION; LUMINOSITY FUNCTION; Z-SIMILAR-TO-6 QUASARS; SPATIAL-DISTRIBUTION; HIERARCHICAL-MODELS; STAR-FORMATION AB Recently, a very large clustering length has been measured for quasars at a redshift of z similar to 4. In combination with the observed quasar luminosity function, we assess the implications of this clustering for the relationship between quasar luminosity and dark matter halo mass. Our analysis allows for non-linearity and finite scatter in the relation between quasar luminosity and halo mass, as well as a luminosity dependent quasar lifetime. The additional novel ingredient in our modelling is the allowance for an excess in the observed bias over the underlying halo bias owing to the merger driven nature of quasar activity. We find that the observations of clustering and luminosity function can be explained only if both of the following conditions hold: (i) the luminosity to halo mass ratio increases with halo mass; (ii) the observed clustering amplitude is in excess of that expected solely from halo bias. The latter result is statistically significant at the 99 per cent level. Taken together, the observations provide compelling evidence for merger driven quasar activity, with a black-hole growth that is limited by feedback. In difference from previous analyses, we show that there could be scatter in the luminosity-halo mass relation of up to 1 dex, and that quasar clustering cannot be used to estimate the quasar lifetime. C1 [Wyithe, J. Stuart B.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyithe, JSB (reprint author), Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. EM swyithe@unimelb.edu.au; loeb@cfa.harvard.edu OI Wyithe, Stuart/0000-0001-7956-9758 FU Australian Research Council (JSBW); NASA [NNX08AL43G]; Harvard University funds FX The research was supported by the Australian Research Council (JSBW), by NASA grants NNX08AL43G and by Harvard University funds (AL). NR 66 TC 13 Z9 13 U1 1 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 MAY 21 PY 2009 VL 395 IS 3 BP 1607 EP 1619 DI 10.1111/j.1365-2966.2009.14647.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 443UJ UT WOS:000265936000039 ER PT J AU Cresci, G Hicks, EKS Genzel, R Schreiber, NMF Davies, R Bouche, N Buschkamp, P Genel, S Shapiro, K Tacconi, L Sommer-Larsen, J Burkert, A Eisenhauer, F Gerhard, O Lutz, D Naab, T Sternberg, A Cimatti, A Daddi, E Erb, DK Kurk, J Lilly, SL Renzini, A Shapley, A Steidel, CC Caputi, K AF Cresci, G. Hicks, E. K. S. Genzel, R. Schreiber, N. M. Foerster Davies, R. Bouche, N. Buschkamp, P. Genel, S. Shapiro, K. Tacconi, L. Sommer-Larsen, J. Burkert, A. Eisenhauer, F. Gerhard, O. Lutz, D. Naab, T. Sternberg, A. Cimatti, A. Daddi, E. Erb, D. K. Kurk, J. Lilly, S. L. Renzini, A. Shapley, A. Steidel, C. C. Caputi, K. TI THE SINS SURVEY: MODELING THE DYNAMICS OF z similar to 2 GALAXIES AND THE HIGH-z TULLY-FISHER RELATION SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: evolution; galaxies: high-redshift; galaxies: kinematics and dynamics; infrared: galaxies ID STAR-FORMING GALAXIES; INTEGRAL FIELD SPECTROSCOPY; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; STELLAR MASS DENSITY; DISK GALAXIES; ROTATION CURVES; H-ALPHA; INTERMEDIATE REDSHIFT; ADAPTIVE OPTICS AB We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z similar to 2 from Ha line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (M(gas) approximate to M*) are required to explain the are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity V(max) from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z similar to 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z similar to 2.2 there is an offset in log(M*) for a given rotational velocity of 0.41 +/- 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z similar to 2 galaxies. C1 [Cresci, G.; Hicks, E. K. S.; Genzel, R.; Schreiber, N. M. Foerster; Davies, R.; Bouche, N.; Buschkamp, P.; Genel, S.; Tacconi, L.; Eisenhauer, F.; Gerhard, O.; Lutz, D.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Genzel, R.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Shapiro, K.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Sommer-Larsen, J.] Tech Univ Munich, D-85748 Garching, Germany. [Sommer-Larsen, J.] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Burkert, A.; Naab, T.] Univ Munich, Univ Sternwarte, D-81679 Munich, Germany. [Sternberg, A.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Cimatti, A.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Daddi, E.] Univ Paris Diderot, Irfu SAp, CEA, Lab AIM,CNRS, F-91191 Gif Sur Yvette, France. [Erb, D. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lilly, S. L.; Caputi, K.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Renzini, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Shapley, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Steidel, C. C.] CALTECH, Pasadena, CA 91125 USA. RP Cresci, G (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM gcresci@mpe.mpg.de RI Daddi, Emanuele/D-1649-2012; OI Daddi, Emanuele/0000-0002-3331-9590; Genel, Shy/0000-0002-3185-1540; Cresci, Giovanni/0000-0002-5281-1417 FU Deutsche Forschungsgemeinschaft [SPP1177]; Max-Planck-Gesellschaft FX We thank the ESO staff, and in particular at Paranal Observatory and the SINFONI and PARSEC teams, for their helpful and enthusiastic support during the several observing runs over which the SINS program was carried out. We also thank the referee for useful comments and suggestions. N.M.F.S. acknowledges support by the Schwerpunkt Programm SPP1177 of the Deutsche Forschungsgemeinschaft and by the Minerva Program of the Max-Planck-Gesellschaft. NR 110 TC 143 Z9 143 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 115 EP 132 DI 10.1088/0004-637X/697/1/115 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000012 ER PT J AU Wang, X Li, W Filippenko, AV Foley, RJ Kirshner, RP Modjaz, M Bloom, J Brown, PJ Carter, D Friedman, AS Gal-Yam, A Ganeshalingam, M Hicken, M Krisciunas, K Milne, P Silverman, JM Suntzeff, NB Wood-Vasey, WM Cenko, SB Challis, P Fox, DB Kirkman, D Li, JZ Li, TP Malkan, MA Moore, MR Reitzel, DB Rich, RM Serduke, FJD Shang, RC Steele, TN Swift, BJ Tao, C Wong, DS Zhang, SN AF Wang, X. Li, W. Filippenko, A. V. Foley, R. J. Kirshner, R. P. Modjaz, M. Bloom, J. Brown, P. J. Carter, D. Friedman, A. S. Gal-Yam, A. Ganeshalingam, M. Hicken, M. Krisciunas, K. Milne, P. Silverman, J. M. Suntzeff, N. B. Wood-Vasey, W. M. Cenko, S. B. Challis, P. Fox, D. B. Kirkman, D. Li, J. Z. Li, T. P. Malkan, M. A. Moore, M. R. Reitzel, D. B. Rich, R. M. Serduke, F. J. D. Shang, R. C. Steele, T. N. Swift, B. J. Tao, C. Wong, D. S. Zhang, S. N. TI THE GOLDEN STANDARD TYPE Ia SUPERNOVA 2005cf: OBSERVATIONS FROM THE ULTRAVIOLET TO THE NEAR-INFRARED WAVEBANDS SO ASTROPHYSICAL JOURNAL LA English DT Review DE supernovae: general; supernovae: individual (SN 2005cf) ID HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT SUPERNOVAE; HIGH-VELOCITY FEATURES; BVRI LIGHT CURVES; DARK ENERGY; SN 2001EL; 3-DIMENSIONAL MODELS; OPTICAL OBSERVATIONS; ESC OBSERVATIONS; MAXIMUM LIGHT AB We present extensive photometry at ultraviolet (UV), optical, and near-infrared (NIR) wavelengths, as well as dense sampling of optical spectra, for the normal Type Ia supernova (SN Ia) 2005cf. The optical photometry, performed at eight different telescopes, shows a 1 sigma scatter of less than or similar to 0.03 mag after proper corrections for the instrument responses. From the well-sampled light curves, we find that SN 2005cf reached a B-band maximum at 13.63 +/- 0.02 mag, with an observed luminosity decline rate Delta m(15)(B) = 1.05 +/- 0.03 mag. The correlations between the decline rate and various color indexes, recalibrated on the basis of an expanded SN Ia sample, yield a consistent estimate for the host-galaxy reddening of SN 2005cf, E(B-V)(host) = 0.10 +/- 0.03 mag. The UV photometry was obtained with the Hubble Space Telescope and the Swift Ultraviolet/Optical Telescope, and the results match each other to within 0.1-0.2 mag. The UV light curves show similar evolution to the broadband U, with an exception in the 2000-2500 angstrom spectral range (corresponding to the F220W/uvm2 filters), where the light curve appears broader and much fainter than that on either side (likely owing to the intrinsic spectral evolution). Combining the UV data with the ground-based optical and NIR data, we establish the generic UV-optical-NIR bolometric light curve for SN 2005cf and derive the bolometric corrections in the absence of UV and/or NIR data. The overall spectral evolution of SN 2005cf is similar to that of a normal SN Ia, but with variety in the strength and profile of the main feature lines. The spectra at early times displayed strong, high-velocity (HV) features in the Ca II H&K doublet and NIR triplet, which were distinctly detached from the photosphere (upsilon approximate to 10,000 km s(-1)) at a velocity ranging from 20,000 to 25,000 km s(-1). One interesting feature is the flat-bottomed absorption observed near 6000 angstrom in the earliest spectrum, which rapidly evolved into a triangular shape and then became a normal Si II lambda 6355 absorption profile at about one week before maximum brightness. This premaximum spectral evolution is perhaps due to the blending of the Si II lambda 6355 at photospheric velocity and another HV absorption component (e. g., an Si II shell at a velocity similar to 18,000 km s(-1)) in the outer ejecta, and may be common in other normal SNe Ia. The possible origin of the HV absorption features is briefly discussed. C1 [Wang, X.; Li, W.; Filippenko, A. V.; Foley, R. J.; Modjaz, M.; Bloom, J.; Ganeshalingam, M.; Silverman, J. M.; Cenko, S. B.; Moore, M. R.; Serduke, F. J. D.; Steele, T. N.; Swift, B. J.; Wong, D. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wang, X.; Li, J. Z.; Li, T. P.; Shang, R. C.; Zhang, S. N.] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, X.; Li, J. Z.; Li, T. P.; Shang, R. C.; Zhang, S. N.] Tsinghua Univ, THCA, Beijing 100084, Peoples R China. [Foley, R. J.; Kirshner, R. P.; Modjaz, M.; Friedman, A. S.; Hicken, M.; Wood-Vasey, W. M.; Challis, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, P. J.; Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Carter, D.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rhovot, Israel. [Krisciunas, K.; Suntzeff, N. B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Milne, P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys, Pittsburgh, PA 15260 USA. [Cenko, S. B.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Kirkman, D.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Malkan, M. A.; Reitzel, D. B.; Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Tao, C.] Univ Aix Marseille 2, Ctr Phys Particules Marseille, CNRS, IN2P2 Luminy, F-13288 Marseille 9, France. RP Wang, X (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM wangxf@astro.berkeley.edu RI Friedman, Andrew/I-4691-2013; Wang, Xiaofeng/J-5390-2015 OI Friedman, Andrew/0000-0003-1334-039X; NR 137 TC 91 Z9 92 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 380 EP 408 DI 10.1088/0004-637X/697/1/380 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000033 ER PT J AU Dai, X Assef, RJ Kochanek, CS Brodwin, M Brown, MJI Caldwell, N Cool, RJ Dey, A Eisenhardt, P Eisenstein, D Gonzalez, AH Jannuzi, BT Jones, C Murray, SS Stern, D AF Dai, X. Assef, R. J. Kochanek, C. S. Brodwin, M. Brown, M. J. I. Caldwell, N. Cool, R. J. Dey, A. Eisenhardt, P. Eisenstein, D. Gonzalez, A. H. Jannuzi, B. T. Jones, C. Murray, S. S. Stern, D. TI MID-INFRARED GALAXY LUMINOSITY FUNCTIONS FROM THE AGN AND GALAXY EVOLUTION SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: luminosity function, mass function ID SPITZER-SPACE-TELESCOPE; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; ARRAY CAMERA IRAC; WIDE-FIELD SURVEY; VLT DEEP SURVEY; REDSHIFT SURVEY; RED SEQUENCE; DATA RELEASE; DENSITY AB We present galaxy luminosity functions at 3.6, 4.5, 5.8, and 8.0 mu m measured by combining photometry from the IRAC Shallow Survey with redshifts from the AGN and Galaxy Evolution Survey ( AGES) of the NOAO Deep Wide-Field Survey Bootes field. The well defined IRAC samples contain 3800-5800 galaxies for the 3.6-8.0 mu m bands with spectroscopic redshifts and z < 0.6. We obtained relatively complete luminosity functions in the local redshift bin of z < 0.2 for all four IRAC channels that are well fitted by Schechter functions. After analyzing the samples for the whole redshift range, we found significant evolution in the luminosity functions for all four IRAC channels that can be fitted as an evolution in M-* with redshift, Delta M-* = Qz. While we measured Q = 1.2 +/- 0.4 and 1.1 +/- 0.4 in the 3.6 and 4.5 mu m bands consistent with the predictions from a passively evolving population, we obtained Q = 1.8 +/- 1.1 in the 8.0 mu m band consistent with other evolving star formation rate estimates. We compared our luminosity functions with the predictions of semianalytical galaxy formation and found the best agreement at 3.6 and 4.5 mu m, rough agreement at 8.0 mu m, and a large mismatch at 5.8 mu m. These models also predicted a comparable Q-value to our luminosity functions at 8.0 mu m, but predicted smaller values at 3.6 and 4.5 mu m. We also measured the luminosity functions separately for early- and late-type galaxies. While the luminosity functions of late-type galaxies resemble those for the total population, the luminosity functions of early- type galaxies in the 3.6 and 4.5 mu m bands indicate deviations from the passive evolution model, especially from the measured flat luminosity density evolution. Combining our estimates with other measurements in the literature, we found 53 +/- 18% of the present stellar mass of early- type galaxies was assembled at z = 0.7. C1 [Dai, X.; Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Brodwin, M.; Dey, A.; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Caldwell, N.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, R. J.; Eisenstein, D.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Eisenhardt, P.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Dai, X (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM xinyu@astronomy.ohio-state.edu RI Brown, Michael/B-1181-2015; Dai, Xinyu/B-5735-2011 OI Brown, Michael/0000-0002-1207-9137; Dai, Xinyu/0000-0001-9203-2808 NR 54 TC 21 Z9 21 U1 1 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 MAY 20 PY 2009 VL 697 IS 1 BP 506 EP 521 DI 10.1088/0004-637X/697/1/506 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000042 ER PT J AU Patnaude, DJ Fesen, RA AF Patnaude, Daniel J. Fesen, Robert A. TI PROPER MOTIONS AND BRIGHTNESS VARIATIONS OF NONTHERMAL X-RAY FILAMENTS IN THE CASSIOPEIA A SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; ISM: individual (Cassiopeia A); radiation mechanisms: non-thermal ID A SUPERNOVA; PARTICLE-ACCELERATION; SYNCHROTRON EMISSION; MAGNETIC-FIELDS; REVERSE SHOCKS; EXPANSION; EJECTA; CHANDRA; MASS; VARIABILITY AB We present Chandra ACIS X-ray observations of the Galactic supernova remnant Cassiopeia A taken in 2007 December. Combining these data with previous archival Chandra observations taken in 2000, 2002, and 2004, we estimate the remnant's forward shock velocity at various points around the outermost shell to range between 4200 and 5200 +/- 500 km s(-1). Using these results together with previous analyses of Cas A's X-ray emission, we present a model for the evolution of Cas A and find that it's expansion is well fit by a rho(ej) proportional to r(-(7-9)) ejecta profile running into a circumstellar wind. We further find that while the position of the reverse shock in this model is consistent with that measured in the X-rays, in order to match the forward shock velocity and radius we had to assume that similar to 30% of the explosion energy has gone into accelerating cosmic rays at the forward shock. The new X-ray images also show that brightness variations can occur for some forward shock filaments like that seen for several nonthermal filaments seen projected in the interior of the remnant. Spectral fits to exterior forward shock filaments and interior nonthermal filaments show that they exhibit similar spectra. This together with similar flux variations suggests that interior nonthermal filaments might be simply forward shock filaments seen in projection and not located at the reverse shock as has been recently proposed. C1 [Patnaude, Daniel J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Patnaude, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. FU NASA [GO8-9065A, NAS8-39073] FX We thank Don Ellison, Stephen Reynolds, and Martin Laming formany useful discussions during the preparation of this paper. We also thank the anonymous referee whose many suggestions and corrections significantly improved the paper. This work was supported by NASA grant GO8-9065A which is administered by the CXC at SAO. D. J. P. acknowledges support from NASA contract NAS8-39073. NR 47 TC 48 Z9 48 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 535 EP 543 DI 10.1088/0004-637X/697/1/535 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000044 ER PT J AU Sozzetti, A Torres, G Latham, DW Stefanik, RP Korzennik, SG Boss, AP Carney, BW Laird, JB AF Sozzetti, Alessandro Torres, Guillermo Latham, David W. Stefanik, Robert P. Korzennik, Sylvain G. Boss, Alan P. Carney, Bruce W. Laird, John B. TI A KECK HIRES DOPPLER SEARCH FOR PLANETS ORBITING METAL-POOR DWARFS. II. ON THE FREQUENCY OF GIANT PLANETS IN THE METAL-POOR REGIME SO ASTROPHYSICAL JOURNAL LA English DT Review DE planetary systems: formation; stars: abundances; stars: statistics; techniques: radial velocities ID EXTRA-SOLAR PLANETS; HORIZONTAL-BRANCH STARS; PROPER-MOTION STARS; M-CIRCLE-PLUS; HARPS SEARCH; MASS COMPANION; SUPER-EARTHS; HOT JUPITER; RED GIANT; SUBSTELLAR COMPANIONS AB We present an analysis of three years of precision radial velocity (RV) measurements of 160 metal-poor stars observed with HIRES on the Keck 1 telescope. We report on variability and long-term velocity trends for each star in our sample. We identify several long-term, low-amplitude RV variables worthy of followup with direct imaging techniques. We place lower limits on the detectable companion mass as a function of orbital period. Our survey would have detected, with a 99.5% confidence level, over 95% of all companions on low-eccentricity orbits with velocity semiamplitude K greater than or similar to 100 m s(-1), or M(p) sin i greater than or similar to 3.0 M(J)(P/yr)((1/3)), for orbital periods P less than or similar to 3 yr. None of the stars in our sample exhibits RV variations compatible with the presence of Jovian planets with periods shorter than the survey duration. The resulting average frequency of gas giants orbiting metal-poor dwarfs with -2.0 less than or similar to[Fe/H]less than or similar to -0.6 is f(p) < 0.67% (at the 1 sigma confidence level). We examine the implications of this null result in the context of the observed correlation between the rate of occurrence of giant planets and the metallicity of their main-sequence solar-type stellar hosts. By combining our data set with the Fischer & Valenti (2005) uniform sample, we confirm that the likelihood of a star to harbor a planet more massive than Jupiter within 2 AU is a steeply rising function of the host's metallicity. However, the data for stars with -1.0 less than or similar to[Fe/H]less than or similar to 0.0 are compatible, in a statistical sense, with a constant occurrence rate fp similar or equal to 1%. Our results can usefully inform theoretical studies of the process of giant-planet formation across two orders of magnitude in metallicity. C1 [Sozzetti, Alessandro; Torres, Guillermo; Latham, David W.; Stefanik, Robert P.; Korzennik, Sylvain G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sozzetti, Alessandro] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Boss, Alan P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Carney, Bruce W.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Laird, John B.] Bowling Green State Univ, Dept Phys & Astron, Bowling Green, OH 43403 USA. RP Sozzetti, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asozzett@cfa.harvard.edu; gtorres@cfa.harvard.edu; dlatham@cfa.harvard.edu; skorzennik@cfa.harvard.edu; rstefanik@cfa.harvard.edu; boss@dtm.ciw.edu; bruce@physics.unc.edu; laird@bgsu.edu OI Sozzetti, Alessandro/0000-0002-7504-365X NR 111 TC 43 Z9 43 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 544 EP 556 DI 10.1088/0004-637X/697/1/544 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000045 ER PT J AU Orosz, JA Steeghs, D McClintock, JE Torres, MAP Bochkov, I Gou, LJ Narayan, R Blaschak, M Levine, AM Remillard, RA Bailyn, CD Dwyer, MM Buxton, M AF Orosz, Jerome A. Steeghs, Danny McClintock, Jeffrey E. Torres, Manuel A. P. Bochkov, Ivan Gou, Lijun Narayan, Ramesh Blaschak, Michael Levine, Alan M. Remillard, Ronald A. Bailyn, Charles D. Dwyer, Morgan M. Buxton, Michelle TI A NEW DYNAMICAL MODEL FOR THE BLACK HOLE BINARY LMC X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; black hole physics; stars: early-type; X-rays: binaries; X-rays: individual (LMC X-1) ID LARGE-MAGELLANIC-CLOUD; X-RAY-SPECTRA; O-TYPE STARS; STELLAR PHOTOMETRY; VELOCITY CURVES; 3U 0900-40; MASS; SPECTROSCOPY; ATMOSPHERES; CANDIDATES AB We present a dynamical model of the high mass X-ray binary LMC X-1 based on high-resolution optical spectroscopy and extensive optical and near-infrared photometry. From our new optical data we find an orbital period of P = 3.90917 +/- 0.00005 days. We present a refined analysis of the All Sky Monitor data from RXTE and find an X-ray period of P = 3.9094 +/- 0.0008 days, which is consistent with the optical period. A simple model of Thomson scattering in the stellar wind can account for the modulation seen in the X-ray light curves. The V-K color of the star (1.17 +/- 0.05) implies A(V) = 2.28 +/- 0.06, which is much larger than previously assumed. For the secondary star, we measure a radius of R(2) = 17.0 +/- 0.8 R(circle dot) and a projected rotational velocity of V(rot) sin i = 129.9 +/- 2.2 km s(-1). Using these measured properties to constrain the dynamical model, we find an inclination of i = 36 degrees.38 +/- 1 degrees.92, a secondary star mass of M(2) = 31.79 +/- 3.48 M(circle dot), and a black hole mass of 10.91 +/- 1.41 M(circle dot). The present location of the secondary star in a temperature-luminosity diagram is consistent with that of a star with an initial mass of 35 M(circle dot) that is 5 Myr past the zero-age main sequence. The star nearly fills its Roche lobe (approximate to 90% or more), and owing to the rapid change in radius with time in its present evolutionary state, it will encounter its Roche lobe and begin rapid and possibly unstable mass transfer on a timescale of a few hundred thousand years. C1 [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, Danny; McClintock, Jeffrey E.; Torres, Manuel A. P.; Bochkov, Ivan; Gou, Lijun; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blaschak, Michael] Calif State Polytech Univ Pomona, Dept Phys, Pomona, CA 91768 USA. [Levine, Alan M.; Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bailyn, Charles D.; Dwyer, Morgan M.; Buxton, Michelle] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM orosz@sciences.sdsu.edu; D.T.H.Steeghs@warwick.ac.uk; jem@cfa.harvard.edu; mtorres@cfa.harvard.edu; ibochkov@cfa.harvard.edu; lgou@cfa.harvard.edu; narayan@cfa.harvard.edu; mgblaschak@csupomona.edu; aml@space.mit.edu; rr@space.mit.edu; charles.bailyn@yale.edu; morgan.dwyer@aya.yale.edu; michelle.buxton@yale.edu RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Narayan, Ramesh/0000-0002-1919-2730 NR 66 TC 55 Z9 55 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 573 EP 591 DI 10.1088/0004-637X/697/1/573 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000047 ER PT J AU Mohanty, S Stassun, KG Mathieu, RD AF Mohanty, Subhanjoy Stassun, Keivan G. Mathieu, Robert D. TI CIRCUMSTELLAR ENVIRONMENT AND EFFECTIVE TEMPERATURE OF THE YOUNG SUBSTELLAR ECLIPSING BINARY 2MASS J05352184-0546085 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: fundamental parameters; stars: low-mass, brown dwarfs; stars: pre-main sequence; techniques: photometric ID LOW-MASS STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; ORION-NEBULA-CLUSTER; MAIN-SEQUENCE STARS; BROWN DWARFS; PROTOSTELLAR ENVELOPES; CHROMOSPHERIC ACTIVITY; EVOLUTIONARY MODELS; ATMOSPHERES; ACCRETION AB We present new Spitzer IRAC/PU/MIPS photometry from 3.6 to 24 mu m, and new Gemini GMOS photometry at 0.48 mu m, of the young brown dwarf eclipsing binary 2MASS J05352184-0546085, located in the Orion Nebula Cluster. No excess disk emission is detected. The measured fluxes at lambda <= 8 mu m are within 1 sigma (less than or similar to 0.1 mJy) of a bare photosphere, and the 3 sigma upper limit at 16 mu m is a mere 0.04 mJy above the bare photospheric level. Together with the known properties of the system, this implies the absence of optically thick disks around the individual components. It also implies that if any circumbinary disk is present, it must either be optically thin and extremely tenuous (10(-10) M(circle dot)) if it extends in to within similar to 0.1 AU of the binary (the approximate tidal truncation radius), or it must be optically thick with a large inner hole, >0.6-10 AU in radius depending on degree of flaring. The consequence in all cases is that disk accretion is likely to be negligible or absent. This supports the recent proposal that the strong H alpha emission in the primary (more massive) brown dwarf results from chromospheric activity, and thereby bolsters the hypothesis that the surprising T(eff) inversion observed between the components is due to strong magnetic fields on the primary. Our data also set constraints on the T(eff) of the components independent of spectral type, and thereby on models of the aforementioned magnetic field effects. We discuss the consequences for the derived fundamental properties of young brown dwarfs and very low mass stars in general. Specifically, if very active isolated young brown dwarfs and very low mass stars suffer the same activity/field related effects as the 2M0535-05 primary, the low-mass stellar/substellar initial mass function currently derived from standard evolutionary tracks may be substantially in error. C1 [Mohanty, Subhanjoy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Mathieu, Robert D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Mohanty, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smohanty@cfa.harvard.edu FU Spitzer Fellowship; Spitzer Cycle-4 GO; Research Corporation FX M. is grateful to the Spitzer Fellowship program for funding this research. K. G. S. acknowledges funding support from a Spitzer Cycle-4 GO grant and a Cottrell Scholar award from the Research Corporation. NR 33 TC 12 Z9 12 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 713 EP 720 DI 10.1088/0004-637X/697/1/713 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000059 ER PT J AU Kirkpatrick, CC McNamara, BR Rafferty, DA Nulsen, PEJ Birzan, L Kazemzadeh, F Wise, MW Gitti, M Cavagnolo, KW AF Kirkpatrick, C. C. McNamara, B. R. Rafferty, D. A. Nulsen, P. E. J. Birzan, L. Kazemzadeh, F. Wise, M. W. Gitti, M. Cavagnolo, K. W. TI A CHANDRA X-RAY ANALYSIS OF ABELL 1664: COOLING, FEEDBACK, AND STAR FORMATION IN THE CENTRAL CLUSTER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies: clusters: individual (A1664); galaxies: starburst; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASS; FLOW CLUSTERS; MOLECULAR GAS; COLD FRONTS; INTRACLUSTER MEDIUM; THERMAL CONDUCTION; OPTICAL SPECTROSCOPY; VISCOUS DISSIPATION; BRIGHTEST CLUSTERS AB The brightest cluster galaxy (BCG) in the Abell 1664 cluster is unusually blue and is forming stars at a rate of similar to 23 M(circle dot) yr(-1). The BCG is located within 5 kpc of the X-ray peak, where the cooling time of 3.5 x 10(8) yr and entropy of 10.4 keV cm(2) are consistent with other star-forming BCGs in cooling flow clusters. The center of A1664 has an elongated, "barlike" X-ray structure whose mass is comparable to the mass of molecular hydrogen, similar to 10(10) M(circle dot) in the BCG. We show that this gas is unlikely to have been stripped from interloping galaxies. The cooling rate in this region is roughly consistent with the star formation rate, suggesting that the hot gas is condensing onto the BCG. We use the scaling relations of Birzan et al. to show that the active galactic nucleus (AGN) is underpowered compared to the central X-ray cooling luminosity by roughly a factor of three. We suggest that A1664 is experiencing rapid cooling and star formation during a low state of an AGN feedback cycle that regulates the rates of cooling and star formation. Modeling the emission as a single-temperature plasma, we find that the metallicity peaks 100 kpc from the X-ray center, resulting in a central metallicity dip. However, a multi-temperature cooling flow model improves the fit to the X-ray emission and is able to recover the expected, centrally peaked metallicity profile. C1 [Kirkpatrick, C. C.; McNamara, B. R.; Kazemzadeh, F.; Cavagnolo, K. W.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rafferty, D. A.; Birzan, L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Gitti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. RP Kirkpatrick, CC (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. OI Gitti, Myriam/0000-0002-0843-3009; Nulsen, Paul/0000-0003-0297-4493 FU Chandra [G07-8122X]; Natural Science and Engineering Research Council of Canada FX C. K. thank Sean McGee and Michael Balogh for helpful discussions. This work was funded in part by Chandra grant G07-8122X and a generous grant from the Natural Science and Engineering Research Council of Canada. NR 93 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 867 EP 879 DI 10.1088/0004-637X/697/1/867 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000074 ER PT J AU Brunken, S Gottlieb, CA McCarthy, MC Thaddeus, P AF Bruenken, S. Gottlieb, C. A. McCarthy, M. C. Thaddeus, P. TI LABORATORY DETECTION OF HOCN AND TENTATIVE IDENTIFICATION IN Sgr B2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (Sgr B2); ISM: molecules; line: identification; molecular data; molecular processes; radio lines: ISM ID MOLECULAR QUASI-LINEARITY; MILLIMETER-WAVE SPECTRUM; SAGITTARIUS B2; ISOCYANIC ACID; EQUILIBRIUM STRUCTURE; ROTATIONAL SPECTRA; RIGOROUS ATTEMPT; GALACTIC-CENTER; FULMINIC ACID; CHNO ISOMERS AB The rotational spectrum of cyanic acid, HOCN, has been detected in the centimeter-wave band in a molecular beam by Fourier transform microwave spectroscopy and in the millimeter-wave band by conventional spectroscopy in a low-pressure laboratory discharge. Spectroscopic constants, including the nitrogen hyperfine coupling constant, derived from 31 a-type transitions between 21 and 360 GHz with J up to 17 and K(a) <= 2 allow the spectrum in the only rotational ladders populated in the interstellar gas to be calculated well into the submillimeter-wave band to 1 km s(-1) or better in equivalent radial velocity. Four consecutive transitions of HOCN between 83.9 and 146.8 GHz were tentatively identified in published spectral line surveys of Sgr B2(OH). An approximate column density in Sgr B2(OH) of 6 x 10(12) cm(-2) implies that the HOCN/HNCO ratio is about 0.5%. Because HNCO is widely distributed in the interstellar gas, HOCN may be as well. C1 [Bruenken, S.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruenken, S.; Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Brunken, S (reprint author), Ecole Polytech Fed Lausanne, Lab Chim Phys Mol, Stn 6, CH-1015 Lausanne, Switzerland. EM sbruenken@cfa.harvard.edu; cgottlieb@cfa.harvard.edu; mccarthy@cfa.harvard.edu; pthaddeus@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; McCarthy, Michael/0000-0001-9142-0008 FU National Science Foundation [CHE-0701204]; NASA [NNX08AE05G]; Harvard College Observatory FX We wish to thank E. Herbst, R. Garrod, and D. Quan for helpful discussions regarding the formation of HNCO isomers in space; B. Winnewisser and M. Winnewisser for sharing their knowledge about quasi-linear molecules; and M. Mladenovic for providing the results of her quantum chemical calculations prior to publication. This work is supported by National Science Foundation grant CHE-0701204 and NASA grant NNX08AE05G. S. B. is grateful to the Harvard College Observatory for the Menzel fellowship. NR 44 TC 31 Z9 31 U1 1 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2009 VL 697 IS 1 BP 880 EP 885 DI 10.1088/0004-637X/697/1/880 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441JB UT WOS:000265764000075 ER PT J AU Hollweg, TA Gilmour, CC Mason, RP AF Hollweg, T. A. Gilmour, C. C. Mason, R. P. TI Methylmercury production in sediments of Chesapeake Bay and the mid-Atlantic continental margin SO MARINE CHEMISTRY LA English DT Article DE Mercury; Methylmercury; Methylation; Sediment; Chesapeake Bay; Continental shelf; Continental slope; Organic matter; Sulfide; Partitioning; Redox; Flux ID DISSOLVED ORGANIC-CARBON; STABLE MERCURY ISOTOPES; LONG-ISLAND SOUND; METHYL MERCURY; SURFICIAL SEDIMENTS; ESTUARINE SEDIMENTS; SURFACE SEDIMENTS; PORE WATERS; PERMEABLE SEDIMENTS; MONOMETHYL MERCURY AB Methylmercury (MeHg) concentration and production rates were studied in bottom sediments along the mainstem of Chesapeake Bay and on the adjoining continental shelf and slope. Our objectives were to 1) observe spatial and temporal changes in total mercury (HgT) and MeHg concentrations in the mid-Atlantic coastal region, 2) investigate biogeochemical factors that affect MeHg production, and 3) examine the potential of these sediments as sources of MeHg to coastal and open waters. Estuarine, shelf and slope sediments contained on average 0.5 to 1.5% Hg as MeHg (% MeHg), which increased significantly with salinity across our study site, with weak seasonal trends. Methylation rate constants (k(meth)), estimated using enriched stable mercury isotope spikes to intact cores, showed a similar, but weaker, salinity trend, but strong seasonality, and was highly correlated with % MeHg. Together, these patterns suggest that some fraction of MeHg is preserved thru seasons, as found by others [Orihel, D.M., Paterson, MJ., Blanchfield, P.J., Bodaly, RA., Gilmour, C.C., Hintelmann, H., 2008. Temporal changes in the distribution, methylation, and bioaccumulation of newly deposited mercury in an aquatic ecosystem. Environmental Pollution 154, 77] Similar to other ecosystems, methylation was most favored in sediment depth horizons where sulfate was available, but sulfide concentrations were low (between 0.1 and 10 mu M). MeHg production was maximal at the sediment surface in the organic sediments of the upper and mid Bay where oxygen penetration was small, but was found at increasingly deeper depths. and across a wider vertical range, as salinity increased, where oxygen penetration was deeper. Vertical trends in MeHg production mirrored the deeper, vertically expanded redox boundary layers in these offshore sediments. The organic content of the sediments had a strong impact on the sediment:water partitioning of Hg, and therefore, on methylation rates. However. the HgT distribution coefficient (K(D)) normalized to organic matter varied by more than an order of magnitude across the study area, suggesting an important role of organic matter quality in Hg sequestration. We hypothesize that the lower sulfur content organic matter of shelf and slope sediments has a lower binding capacity for Hg resulting in higher MeHg production, relative to sediments in the estuary. Substantially higher MeHg concentrations in pore water relative to the water column indicate all sites are sources of MeHg to the water column throughout the seasons studied. Calculated diffusional fluxes for MeHg averaged similar to 1 pmol m(-2) day(-1). It is likely that the total MeHg flux in sediments of the lower Bay and continental margin are significantly higher than their estimated diffusive fluxes due to enhanced MeHg mobilization by biological and/or physical processes. Our flux estimates across the full salinity gradient of Chesapeake Bay and its adjacent slope and shelf strongly suggest that the flux from coastal sediments is of the same order as other sources and contributes substantially to the coastal MeHg budget. (C) 2009 Elsevier B.V. All rights reserved. C1 [Hollweg, T. A.; Mason, R. P.] Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. [Gilmour, C. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Hollweg, TA (reprint author), Univ Connecticut, Dept Marine Sci, Groton, CT 06340 USA. EM terill.hollweg@uconn.edu RI Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 NR 100 TC 77 Z9 82 U1 1 U2 55 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-4203 J9 MAR CHEM JI Mar. Chem. PD MAY 20 PY 2009 VL 114 IS 3-4 BP 86 EP 101 DI 10.1016/j.marchem.2009.04.004 PG 16 WC Chemistry, Multidisciplinary; Oceanography SC Chemistry; Oceanography GA 465CM UT WOS:000267558800003 ER PT J AU Morales, MN Massardo, D Moreira, GRP Thompson, FC AF Morales, Mirian Nunes Massardo, Darli Moreira, Gilson R. P. Thompson, F. Christian TI A new species of Alipumilio Shannon (Diptera, Syrphidae) found in association with the exudate resin of Schinus terebinthifolius Raddi (Anacardiaceae) SO ZOOTAXA LA English DT Article DE insect taxonomy; insect morphology; insect fine structure; neotropics; flower flies; brazilian peppertree; tree resins ID PHYLOGENY AB The adult stage of a new species of flower fly, Alipumilio athesphatus Thompson (Diptera, Syrphidae) is described. The gross morphology and external integumentary features of the egg, third-instar larva and pupa are also presented. All immature stages were found in association with the exudate resin of Schinus terebinthifolius Raddi (Anacardiaceae) in Porto Alegre, Rio Grande do Sul State, Brazil. C1 [Morales, Mirian Nunes] Univ Fed Parana, Dept Zool Posgrad & Entomol, BR-81531980 Curitiba, Parana, Brazil. [Massardo, Darli; Moreira, Gilson R. P.] Univ Fed Rio Grande do Sul, Inst Biociencias, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil. [Thompson, F. Christian] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. RP Morales, MN (reprint author), Univ Fed Parana, Dept Zool Posgrad & Entomol, Caixa Postal 19020, BR-81531980 Curitiba, Parana, Brazil. EM mirian_nm@yahoo.com.br; darlimassardo@yahoo.com.br; gilson.moreira@ufrgs.br; thompsonfc@si.edu RI Moreira, Gilson/D-2209-2013; Morales, Mirian/Q-2051-2015 OI Morales, Mirian/0000-0003-2114-8656 FU CNPq Doctoral Thesis Scholarship; CAPES Master Thesis Scholarship FX We are especially grateful to Maria Carmen Sestren-Bastos and the Secretaria Municipal do Meio Ambiente staff ( Porto Alegre city) for allowing collection of specimens and for help with the field work at Morro do Osso municipal park. Thanks are also due to Centro de Microscopia Eletronica (CME) of Universidade Federal do Rio Grande do Sul (UFRGS) for the use of SEM facilities. We would like to thank Vitor Antonio Nardino and project Taxon line - Network of Biological Collections from Parana State (www.taxonline.ufpr.br) for helping with the Automontage images. M.N. Morales has been supported by a CNPq Doctoral Thesis Scholarship. D. Massardo has been supported by a CAPES Master Thesis Scholarship. G.R.P. Moreira has been financed by a CNPq grant. NR 14 TC 3 Z9 5 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 MAY 20 PY 2009 IS 2112 BP 53 EP 64 PG 12 WC Zoology SC Zoology GA 448AQ UT WOS:000266233900005 ER PT J AU Brawley, SH Coyer, JA Blakeslee, AMH Hoarau, G Johnson, LE Byers, JE Stam, WT Olsen, JL AF Brawley, Susan H. Coyer, James A. Blakeslee, April M. H. Hoarau, Galice Johnson, Ladd E. Byers, James E. Stam, Wytze T. Olsen, Jeanine L. TI Historical invasions of the intertidal zone of Atlantic North America associated with distinctive patterns of trade and emigration SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Fucus serratus; Littorina littorea; propagule pressure ID PROPAGULE PRESSURE; FUCUS-SERRATUS; BIOLOGICAL INVASIONS; FUCACEAE POPULATIONS; SPECIES INVASIONS; HETEROKONTOPHYTA; RECOLONIZATION; INVADERS; SUCCESS; ORIGIN AB Early invasions of the North American shore occurred mainly via deposition of ballast rock, which effectively transported pieces of the intertidal zone across the Atlantic. From 1773- 1861, > 880 European ships entered Pictou Harbor, Nova Scotia, as a result of emigration and trade from Europe. The rockweed Fucus serratus (1868) and the snail Littorina littorea (approximate to 1840) were found in Pictou during this same period. With shipping records (a proxy for propagule pressure) to guide sampling, we used F. serratus as a model to examine the introductions because of its relatively low genetic diversity and dispersal capability. Microsatellite markers and assignment tests revealed 2 introductions of the rockweed into Nova Scotia: 1 from Galway (Ireland) to Pictou and the other from Greenock (Scotland) to western Cape Breton Island. To examine whether a high-diversity, high-dispersing species might have similar pathways of introduction, we analyzed L. littorea, using cytochrome b haplotypes. Eight of the 9 Pictou haplotypes were found in snails collected from Ireland and Scotland. Our results contribute to a broader understanding of marine communities, because these 2 conspicuous species are likely to be the tip of an "invasion iceberg'' to the NW Atlantic from Great Britain and Ireland in the 19th Century. C1 [Brawley, Susan H.] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. [Coyer, James A.; Hoarau, Galice; Stam, Wytze T.; Olsen, Jeanine L.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Dept Marine Benth Ecol & Evolut, NL-9750 AA Haren, Netherlands. [Blakeslee, April M. H.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. [Johnson, Ladd E.] Univ Laval, Dept Biol, Quebec City, PQ G1V 0A6, Canada. [Byers, James E.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. RP Brawley, SH (reprint author), Univ Maine, Sch Marine Sci, Orono, ME 04469 USA. EM brawley@maine.edu RI hoarau, galice/C-3152-2009; Coyer, James/B-3295-2010; Olsen, Jeanine/D-3213-2013 FU National Geographic Society [7827-05]; NSF [OCE 0622439, OCE 0503932]; Canadian-American Center; The Alfred P. Sloan Foundation FX We thank J. Hey, C. Cunningham, J. Carlton, and M. Guiry for discussion. S. H. B. thanks archivists at Public Archives of Nova Scotia (Philip Hartley), Hector Archive (Darrell Burke), National Archives of Scotland, National University of Ireland, Galway, Ireland, and Galway County libraries, and the University of Maine (Susan Buzzell and Barbara Jones); the DNA Sequencing Center (University of Maine); Michael Guiry (Galway), DavidMann (Edinburgh), Suzanne Craig and Daniel Rochaix (Mabou, Nova Scotia) for hospitality. The National Science Foundation (NSF) Research Coordination Networks-CORONA (C. Cunningham, principal investigator) aided in project development. J. L. O., J. A. C. and G. H. thank Jan Veldsink for additional genotyping of F. serratus. This work was supported by National Geographic Society Grant 7827-05 (to S. H. B. and L. E. J.), NSF Grants OCE 0622439 (to S. H. B.) and OCE 0503932 (to J. E. B.), the Canadian-American Center (University of Maine, S. H. B.), and The Alfred P. Sloan Foundation (HMAP funding, A. M. H. B.; A. Rosenberg, principal investigator). NR 47 TC 41 Z9 42 U1 5 U2 32 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 MAY 19 PY 2009 VL 106 IS 20 BP 8239 EP 8244 DI 10.1073/pnas.0812300106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 447RH UT WOS:000266209000029 PM 19416814 ER PT J AU Schmidt, ME Farrand, WH Johnson, JR Schroder, C Hurowitz, JA Mccoy, TJ Ruff, SW Arvidson, RE Marais, DJD Lewis, KW Ming, DW Squyres, SW de Souza, PA AF Schmidt, M. E. Farrand, W. H. Johnson, J. R. Schroeder, C. Hurowitz, J. A. Mccoy, T. J. Ruff, S. W. Arvidson, R. E. Marais, D. J. Des Lewis, K. W. Ming, D. W. Squyres, S. W. de Souza, P. A., Jr. TI Spectral, mineralogical, and geochemical variations across Home Plate, Gusev Crater, Mars indicate high and low temperature alteration SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars geology; Gusev Crater; hydrothermal alteration ID SOILS; ROCKS; WATER; DUST AB Over the last similar to 3 years in Gusev Crater, Mars, the Spirit rover observed coherent variations in color, mineralogy, and geochemistry across Home Plate, an similar to 80 m-diameter outcrop of basaltic tephra. Observations of Home Plate from orbit and from the summit of Husband Hill reveal clear differences in visible/near-infrared (VNIR) colors between its eastern and western regions that are consistent with mineralogical compositions indicated by Mossbauer spectrometer (MB) and by Miniature Thermal Emission Spectrometer (Mini-TES). Pyroxene and magnetite dominate the east side, while olivine, nanophase Fe oxide (npOx) and glass are more abundant on the western side. Alpha Particle X-Ray Spectrometer (APXS) observations reveal that eastern Home Plate has higher Si/Mg, Al, Zn, Ni, and K, while Cl and Br are higher in the west. We propose that these variations are the result of two distinct alteration regimes that may or may not be temporally related: a localized, higher temperature recrystallization and alteration of the east side of Home Plate and lower temperature alteration of the western side that produced npOx. Published by Elsevier B.V. C1 [Schmidt, M. E.; Mccoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Johnson, J. R.] US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. [Schroeder, C.] Johannes Gutenberg Univ Mainz, Inst Anorgan Chem & Analyt Chem, D-55128 Mainz, Germany. [Hurowitz, J. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Arvidson, R. E.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Marais, D. J. Des] NASA, Ames Res Ctr, Exobiol Branch, Moffett Field, CA 94035 USA. [Lewis, K. W.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Ming, D. W.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [de Souza, P. A., Jr.] CSIRO, Tasmanian ICT Ctr, Hobart, Tas 7000, Australia. RP Schmidt, ME (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM schmidtm@si.edu RI de Souza, Paulo/B-8961-2008; Schroder, Christian/B-3870-2009; Centre, TasICT/D-1212-2011; Lewis, Kevin/E-5557-2012; Johnson, Jeffrey/F-3972-2015 OI de Souza, Paulo/0000-0002-0091-8925; Schroder, Christian/0000-0002-7935-6039; NR 41 TC 30 Z9 30 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD MAY 15 PY 2009 VL 281 IS 3-4 BP 258 EP 266 DI 10.1016/j.epsl.2009.02.030 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 456SQ UT WOS:000266869000012 ER PT J AU Cottrell, E Walter, MJ Walker, D AF Cottrell, Elizabeth Walter, Michael J. Walker, David TI Metal-silicate partitioning of tungsten at high pressure and temperature: Implications for equilibrium core formation in Earth SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE core formation; partitioning; siderophile; tungsten; W; experiments; carbon ID TERRESTRIAL MAGMA OCEAN; SIDEROPHILE ELEMENTS; OXIDATION-STATE; OXYGEN FUGACITY; MELT COMPOSITION; DIFFERENTIATION; CONSTRAINTS; SOLUBILITY; LIQUID; MANTLE AB Tungsten partitioning between liquid metal and liquid silicate, D(W), from 1723-2673 K, 0.5-18 GPa, and over a wide range of metal and silicate compositions provides constraints on planetary core formation models. We find that W partitioning is extremely sensitive to the carbon content of the metal alloy, becoming about an order of magnitude more siderophile at carbon saturation. Activity-composition corrections based on interactions between W-C and Fe-C in metal solution shift calculated D(W) to more lithophile values, and calculated oxygen fugacities (fO(2)) to more oxidizing values, than uncorrected data. W exists as a highly charged cation in silicate solution, displaying a mixture of oxidation states from +4 to + 6 in experiments at fO(2) of similar to 0.5-2 log units below the iron-wilstite buffer. At constant fO(2), the average calculated valence decreases with pressure from similar to + 5.5 at 0.5 GPa to similar to +4 at 11-18 GPa. As a result of its high oxidation state, W partitioning is strongly dependent on silicate melt polymerization and fO(2),. In contrast to some previous results, we find that D(W) may decrease slightly in response to increasing temperature in the pressure range of our experiments. Pressure exerts a non-monotonic effect: D(W) increases with pressure up to similar to 3 to 4 GPa, but decreases at higher pressures. Previous models for the effects of pressure and temperature on W partitioning that conflict with our results appear to result from a conflation of the intensive parameters of pressure, temperature, and carbon content. The mantle abundance of W could have been set by single-stage metal-silicate equilibration along the liquidus in a deep peridotite magma ocean at pressures from 20-50 GPa, and at oxygen fugacities consistent with the mantle's present iron budget (IW-2 to -2.5). Equilibration at higher pressure is viable if the core-forming metal contained a significant, but not unreasonable, abundance of carbon (similar to 2 wt.%). Recent continuous accretion models involving multi-stage metal-silicate equilibration in a deepening magma ocean with progressive oxidation of the silicate remain permissible given our new treatment of W partitioning data. Published by Elsevier B.V. C1 [Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Walter, Michael J.] Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England. [Walker, David] Columbia Univ, Dept Earth & Environm Sci, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Cottrell, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Ave, Washington, DC 20560 USA. EM CottrellE@si.edu FU Smithsonian Institution; NSF; NERC FX The authors thank Hugh O'Neill for sharing data in press, Amelia Logan for assistance with the electron microprobe, Yves Thibault for help with experiments, and Bernard Wood for supplying us with the code for program METAL The manuscript benefited from reviews by Kevin Righter, Bernard Wood, Herbert Palme, and Nancy Chabot. This work was supported by the Smithsonian Institution, NSF, and NERC. NR 60 TC 51 Z9 52 U1 2 U2 19 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 MAY 15 PY 2009 VL 281 IS 3-4 BP 275 EP 287 DI 10.1016/j.epsl.2009.02.024 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 456SQ UT WOS:000266869000014 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Musical Groups in the Movies, 1929-1970 SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 MAY 15 PY 2009 VL 134 IS 9 BP 103 EP 103 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 446XR UT WOS:000266155500233 ER PT J AU Jamieson, MJ Dalgarno, A Aymar, M Tharamel, J AF Jamieson, M. J. Dalgarno, A. Aymar, M. Tharamel, J. TI A study of exchange interactions in alkali molecular ion dimers with application to charge transfer in cold Cs SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID POLARIZATION PERTURBATION-THEORY; MODEL-POTENTIAL CALCULATIONS; HOLSTEIN-HERRING METHOD; DISPERSION COEFFICIENTS; SCATTERING LENGTH; EFFECTIVE-RANGE; ENERGY; STATES; CATIONS; DIPOLE AB The formulation of Bardsley et al (Phys. Rev. A 11 1911) for evaluating the asymptotic electron exchange interaction between an alkali ion and its parent atom is extended by the use of a more accurate representation of the asymptotic wavefunction of the isolated atom and also by the inclusion of a further term in the series that accounts for the presence of the ion. The Bardsley analysis is compared with a purely numerical approach in which the Holstein- Herring integrand is constructed from a polarized wavefunction built from numerical solutions of the differential equations of Rayleigh-Schrodinger perturbation theory and the required quadrature is performed numerically. Values of the asymptotic exchange interactions are given for the molecular ions Li-2(+), Na-2(+), K-2(+), Rb-2(+) and Cs-2(+). As an example, exchange interactions for Cs-2(+) evaluated by an ab initio method are compared to those predicted by the Bardsley formula. Potentials for the lowest states of Cs-2(+) are constructed from the ab initio values matched to the asymptotic exchange and long-range polarization interactions, and these potentials are used to predict the 1(2) Sigma(+)(g) and 1(2) Sigma(+)(u) scattering lengths and low-energy charge transfer cross sections. C1 [Jamieson, M. J.; Dalgarno, A.; Tharamel, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jamieson, M. J.] Univ Glasgow, Dept Comp Sci, Glasgow G12 8QQ, Lanark, Scotland. [Aymar, M.] CNRS 2, Aime Cotton Lab, F-91405 Orsay, France. RP Jamieson, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mjj@dcs.gla.ac.uk FU Chemical Sciences, Geosciences and Biosciences Division of the Office of Basic Energy Sciences, Office of Science, US Department of Energy; Institute for Theoretical Atomic and Molecular Physics at the Harvard-Smithsonian Center for Astrophysics; National Science Foundation FX We acknowledge the support of the Chemical Sciences, Geosciences and Biosciences Division of the Office of Basic Energy Sciences, Office of Science, US Department of Energy and the Institute for Theoretical Atomic and Molecular Physics at the Harvard-Smithsonian Center for Astrophysics; the Institute is supported by a grant from the National Science Foundation. NR 38 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD MAY 14 PY 2009 VL 42 IS 9 AR 095203 DI 10.1088/0953-4075/42/9/095203 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 438UW UT WOS:000265582000009 ER PT J AU Kuznetsova, E Gacesa, M Pellegrini, P Yelin, SF Cote, R AF Kuznetsova, Elena Gacesa, Marko Pellegrini, Philippe Yelin, Susanne F. Cote, Robin TI Efficient formation of ground-state ultracold molecules via STIRAP from the continuum at a Feshbach resonance SO NEW JOURNAL OF PHYSICS LA English DT Article ID COLD-ATOM SCATTERING; PHOTOASSOCIATION AB We develop a theoretical description of photoassociative stimulated Raman adiabatic passage (STIRAP) near a Feshbach resonance in a thermal atomic gas. We show that it is possible to use low-intensity laser pulses to directly excite pairs of atoms in the continuum near a Feshbach resonance and to transfer most of the atomic cloud to the lowest rovibrational level of the molecular ground state. For a broad resonance, commonly found in several mixtures of alkali atoms, our model predicts a transfer efficiency up to 97% for a given atom pair, and up to 70% when averaged over an atomic ensemble. The laser intensities and pulse durations needed for such an optimal transfer, 10(2)-10(3) W cm(-2) and several microseconds, are easily achievable experimentally. A single pair of STIRAP pulses converts an estimated fraction f similar to 10(-6)-10(-4) of atoms in an atomic ensemble, leading to the production of 10-1000 molecules in a large sample of 10(7) atoms. A total of similar to 10(4)-10(6) pulse pairs are thus required to transfer most atoms into molecules. Such an efficiency compares with or surpasses currently available techniques for creating stable diatomic molecules, and the versatility of this approach simplifies its potential use for many molecular species. C1 [Kuznetsova, Elena; Gacesa, Marko; Pellegrini, Philippe; Yelin, Susanne F.; Cote, Robin] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kuznetsova, Elena; Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Yelin, SF (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM syelin@phys.uconn.edu; rcote@phys.uconn.edu RI Gacesa, Marko/F-8027-2011 OI Gacesa, Marko/0000-0001-5145-051X NR 34 TC 32 Z9 32 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD MAY 14 PY 2009 VL 11 AR 055028 DI 10.1088/1367-2630/11/5/055028 PG 18 WC Physics, Multidisciplinary SC Physics GA 448AW UT WOS:000266234500019 ER PT J AU Tscherbul, TV Suleimanov, YV Aquilanti, V Krems, RV AF Tscherbul, T. V. Suleimanov, Yu V. Aquilanti, V. Krems, R. V. TI Magnetic field modification of ultracold molecule-molecule collisions SO NEW JOURNAL OF PHYSICS LA English DT Article ID POTENTIAL-ENERGY SURFACES; O-2-O-2 DIMER; FESHBACH RESONANCES; POLAR-MOLECULES; QUANTUM; SCATTERING; DYNAMICS; THRESHOLD; STATES; CHEMISTRY AB We present an accurate quantum mechanical study of molecule-molecule collisions in the presence of a magnetic field. The work focuses on the analysis of elastic scattering and spin relaxation in collisions of O-2((3)Sigma(-)(g)) molecules at cold (similar to 0.1 K) and ultracold (similar to 10(-6) K) temperatures. Our calculations show that magnetic spin relaxation in molecule-molecule collisions is extremely efficient except at magnetic fields below 1 mT. The rate constant for spin relaxation at T = 0.1 K and a magnetic field of 0.1 T is found to be as large as 6.1 x 10(-11) cm(-3) s(-1). The magnetic field dependence of elastic and inelastic scattering cross sections at ultracold temperatures is dominated by a manifold of Feshbach resonances with the density of similar to 100 resonances per Tesla for collisions of molecules in the absolute ground state. This suggests that the scattering length of ultracold molecules in the absolute ground state can be effectively tuned in a very wide range of magnetic fields. Our calculations demonstrate that the number and properties of the magnetic Feshbach resonances are dramatically different for molecules in the absolute ground and excited spin states. The density of Feshbach resonances for molecule-molecule scattering in the low-field-seeking Zeeman state is reduced by a factor of 10. C1 [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Suleimanov, Yu V.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, Russia. [Aquilanti, V.] Univ Perugia, Dipartimento Chim, I-06123 Perugia, Italy. [Krems, R. V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. RP Tscherbul, TV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. EM tshcherb@cfa.harvard.edu RI Tscherbul, Timur/K-3286-2014 OI Tscherbul, Timur/0000-0001-5689-040X NR 60 TC 36 Z9 36 U1 0 U2 6 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 MAY 14 PY 2009 VL 11 AR 055021 DI 10.1088/1367-2630/11/5/055021 PG 21 WC Physics, Multidisciplinary SC Physics GA 448AW UT WOS:000266234500012 ER PT J AU Sanderson, AJR O'Sullivan, E Ponman, TJ AF Sanderson, Alastair J. R. O'Sullivan, Ewan Ponman, Trevor J. TI A statistically selected Chandra sample of 20 galaxy clusters - II. Gas properties and cool core/non-cool core bimodality SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE conduction; galaxies: clusters: general; cooling flows; X-rays: galaxies: clusters ID X-RAY-CLUSTERS; MASS-TEMPERATURE RELATION; INTRACLUSTER MEDIUM; ABUNDANCE PROFILES; THERMAL CONDUCTION; STAR-FORMATION; XMM-NEWTON; ENTROPY PROFILES; SCALING PROJECT; FLOW CLUSTERS AB We investigate the thermodynamic and chemical structure of the intracluster medium (ICM) across a statistical sample of 20 galaxy clusters analysed with the Chandra X-ray satellite. In particular, we focus on the scaling properties of the gas density, metallicity and entropy and the comparison between clusters with and without cool cores (CCs). We find marked differences between the two categories except for the gas metallicity, which declines strongly with radius for all clusters (Z alpha r(-0.31)), outside similar to 0.02r(500). The scaling of gas entropy is non-self-similar and we find clear evidence of bimodality in the distribution of logarithmic slopes of the entropy profiles. With only one exception, the steeper sloped entropy profiles are found in CC clusters whereas the flatter slope population are all non-CC clusters. We explore the role of thermal conduction in stabilizing the ICM and conclude that this mechanism alone is sufficient to balance cooling in non-CC clusters. However, CC clusters appear to form a distinct population in which heating from feedback is required in addition to conduction. Under the assumption that non-CC clusters are thermally stabilized by conduction alone, we find the distribution of Spitzer conduction suppression factors, f(c), to be lognormal, with a log (base 10) mean of -1.50 +/- 0.03 (i.e. f(c) = 0.032) and log standard deviation 0.39 +/- 0.02. C1 [Sanderson, Alastair J. R.; 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. 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 NASA [AR4-5012X, NNX07AQ24G]; NASA/IPAC Extragalactic Data base (NED FX AJRS thanks Ria Johnson for useful discussions and for porting the BCES regression code to R. We thank the referee, Megan Donahue, for useful comments which have improved the clarity of the paper. AJRS acknowledges support from STFC, and EOS acknowledges support from NASA awards AR4-5012X and NNX07AQ24G. This work made use of the NASA/IPAC Extragalactic Data base (NED) and the R tutorials at the Penn State Center for Astrostatistics. NR 69 TC 52 Z9 52 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2009 VL 395 IS 2 BP 764 EP 776 DI 10.1111/j.1365-2966.2009.14613.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 437TJ UT WOS:000265509500012 ER PT J AU Bryant, JJ Johnston, HM Broderick, JW Hunstead, RW De Breuck, C Gaensler, BM AF Bryant, J. J. Johnston, H. M. Broderick, J. W. Hunstead, R. W. De Breuck, C. Gaensler, B. M. TI A new search for distant radio galaxies in the Southern hemisphere - III. Optical spectroscopy and analysis of the MRCR-SUMSS sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies: active; galaxies: high-redshift; infrared: galaxies; radio continuum: galaxies ID K-Z RELATION; ACTIVE GALACTIC NUCLEI; STAR-FORMATION HISTORY; COMPOSITE QUASAR SPECTRA; 7C REDSHIFT SURVEY; EIS-NVSS SURVEY; SKY SURVEY; ELLIPTIC GALAXIES; IMAGING SURVEY; FIND OBJECTS AB We have compiled a sample of 234 ultra-steep-spectrum-selected (USS-selected) radio sources in order to find high-redshift radio galaxies (HzRGs). The sample is in the southern sky at -40 degrees < delta < -30 degrees which is the overlap region of the 408-MHz Revised Molonglo Reference Catalogue, 843-MHz Sydney University Molonglo Sky Survey ( the MRCR-SUMSS sample) and the 1400-MHz National Radio Astronomy Observatory Very Large Array Sky Survey (NVSS). This is the third in a series of papers on the MRCR-SUMSS sample. Here, we present optical spectra from the Australian National University 2.3-m telescope, European Southern Observatory (ESO) New Technology Telescope and ESO Very Large Telescope for 52 of the identifications from Paper II, yielding redshifts for 36 galaxies, 13 of which have z > 2. We analyse the K - z distribution and compare 4-arcsec-aperture magnitudes with 64-kpc aperture magnitudes in several surveys from the literature; the MRCR-SUMSS sample is found to be consistent with models for 10(11) - 10(12)M(circle dot) galaxies. Dispersions about the fits in the K - z plot support passive evolution of radio galaxy hosts since z > 3. By comparing USS-selected samples in the literature, we find that the resultant median redshift of the samples shown is not dependent on the flux density distribution or selection frequency of each sample. In addition, our finding that the majority of the radio spectral energy distributions remain straight over a wide frequency range suggests that a k-correction is not responsible for the success of USS selection in identifying HzRGs and therefore the steep radio spectra may be intrinsic to the source or a product of the environment. Two galaxies have been found to have both compact radio structures and strong self-absorption in the Ly alpha line, suggesting that they are surrounded by a dense medium. For the bulk of the sources, spectral line ratios show that photoionization is the primary excitation process. C1 [Bryant, J. J.; Johnston, H. M.; Broderick, J. W.; Hunstead, R. W.; Gaensler, B. M.] Univ Sydney, Sch Phys A29, SIfA, Sydney, NSW 2006, Australia. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Gaensler, B. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bryant, JJ (reprint author), Univ Sydney, Sch Phys A29, SIfA, Sydney, NSW 2006, Australia. EM jbryant@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010; OI Gaensler, Bryan/0000-0002-3382-9558 FU Australian Government's innovation statement, Backing Australia's Ability.; Major National Research Facilities programme of the Australian Federal Government; Australian Postgraduate Award; Denison Merit Award; Australian Research Council and the University of Sydney Bridging; Australian Research Council [FF0561298]; Research Council [FF0561298]; Commonwealth of Australia; CSIRO; National Science Foundation FX The ATCA is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. SuperCOSMOS Sky Survey material is based on photographic data originating from the UK, Palomar and ESO Schmidt telescopes and is provided by theWide- Field Astronomy Unit, Institute for Astronomy, University of Edinburgh. This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. This publication makes use of data products from the Two- Micron All- Sky Survey ( 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 98 TC 22 Z9 22 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2009 VL 395 IS 2 BP 1099 EP 1120 DI 10.1111/j.1365-2966.2009.14607.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 437TJ UT WOS:000265509500043 ER PT J AU Trump, JR Impey, CD Elvis, M McCarthy, PJ Huchra, JP Brusa, M Salvato, M Capak, P Cappelluti, N Civano, F Comastri, A Gabor, J Hao, H Hasinger, G Jahnke, K Kelly, BC Lilly, SJ Schinnerer, E Scoville, NZ Smolcic, V AF Trump, Jonathan R. Impey, Chris D. Elvis, Martin McCarthy, Patrick J. Huchra, John P. Brusa, Marcella Salvato, Mara Capak, Peter Cappelluti, Nico Civano, Francesca Comastri, Andrea Gabor, Jared Hao, Heng Hasinger, Gunther Jahnke, Knud Kelly, Brandon C. Lilly, Simon J. Schinnerer, Eva Scoville, Nick Z. Smolcic, Vernesa TI THE COSMOS ACTIVE GALACTIC NUCLEUS SPECTROSCOPIC SURVEY. I. XMM-NEWTON COUNTERPARTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; quasars: general; surveys; X-rays: galaxies ID DIGITAL SKY SURVEY; CHANDRA MULTIWAVELENGTH PROJECT; BRIGHT QUASAR SURVEY; STAR-FORMING GALAXIES; BROAD EMISSION-LINES; FIELD NORTH SURVEY; X-RAY SOURCES; HELLAS2XMM SURVEY; DEEP SURVEY; OPTICAL IDENTIFICATIONS AB We present optical spectroscopy for an X-ray and optical flux-limited sample of 677 XMM-Newton selected targets covering the 2 deg(2) Cosmic Evolution Survey field, with a yield of 485 high-confidence redshifts. The majority of the spectra were obtained over three seasons (2005-2007) with the Inamori Magellan Areal Camera and Spectrograph instrument on the Magellan (Baade) telescope. We also include in the sample previously published Sloan Digital Sky Survey spectra and supplemental observations with MMT/Hectospec. We detail the observations and classification analyses. The survey is 90% complete to flux limits of f(0.5-10 keV) > 8 x 10(-16) erg cm(-2) s(-1) and i(AB)(+) < 22, where over 90% of targets have high-confidence redshifts. Making simple corrections for incompleteness due to redshift and spectral type allows for a description of the complete population to i(AB)(+) < 23. The corrected sample includes a 57% broad emission line (Type 1, unobscured) active galactic nucleus (AGN) at 0.13 < z < 4.26, 25% narrow emission line (Type 2, obscured) AGN at 0.07 < z < 1.29, and 18% absorption line (host-dominated, obscured) AGN at 0 < z < 1.22 (excluding the stars that made up 4% of the X-ray targets). We show that the survey's limits in X-ray and optical fluxes include nearly all X-ray AGNs (defined by L(0.5-10 keV) > 3 x 10(42) erg s(-1)) to z < 1, of both optically obscured and unobscured types. We find statistically significant evidence that the obscured-to-unobscured AGN ratio at z < 1 increases with redshift and decreases with luminosity. C1 [Trump, Jonathan R.; Impey, Chris D.; Gabor, Jared; Kelly, Brandon C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Elvis, Martin; Huchra, John P.; Civano, Francesca; Hao, Heng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, Patrick J.; Scoville, Nick Z.; Smolcic, Vernesa] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Brusa, Marcella; Cappelluti, Nico; Hasinger, Gunther] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Salvato, Mara; Capak, Peter] CALTECH, Pasadena, CA 91125 USA. [Comastri, Andrea] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Jahnke, Knud; Schinnerer, Eva] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lilly, Simon J.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. RP Trump, JR (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. RI Comastri, Andrea/O-9543-2015; OI Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Jahnke, Knud/0000-0003-3804-2137; Schinnerer, Eva/0000-0002-3933-7677; Brusa, Marcella/0000-0002-5059-6848 FU NASA [HST-GO-09822]; ARCS foundation FX We thank the anonymous referee for thorough and helpful comments. We additionally thank A. Dressler and the IMACS team for creating an excellent instrument, as well as telescope operators H. Nunez, F. Sanchez, G. Valladares, S. Vera, H. Rivera, and the Las Campanas Observatory staff for support while observing. We thank M. Westover, A. Coil, S. Burles, and the Carnegie queue mode scientists for help with some of the IMACS observations. We thank D. Fabricant for designing the excellent instrument Hectospec and thank MMT operators and Hectospec queue mode scientists for their help during observations. We also thank the COSMOS team for their work in creating the catalogs used for selecting our targets. We thank P. Shopbell, A. Alexov, and the NASAIPAC/IRSA team for assisting in uploading the data and catalogs to public IRSA archives. Observations reported here were obtained at the Magellan Telescopes, which are operated by the Carnegie Observatories, as well as the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. The HST COSMOS Treasury program was supported through NASA grant HST-GO-09822. J.R.T. acknowledges support from an ARCS foundation fellowship. NR 97 TC 84 Z9 84 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1195 EP 1212 DI 10.1088/0004-637X/696/2/1195 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700011 ER PT J AU Fabrycky, DC Winn, JN AF Fabrycky, Daniel C. Winn, Joshua N. TI EXOPLANETARY SPIN-ORBIT ALIGNMENT: RESULTS FROM THE ENSEMBLE OF ROSSITER-MCLAUGHLIN OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; methods: statistical; planetary systems; stars: rotation ID EXTRASOLAR PLANETARY SYSTEMS; LOW-MASS COMPANIONS; SPECTROSCOPIC TRANSIT; GIANT PLANETS; DYNAMICAL RELAXATION; MIGRATING PLANETS; ROTATION PERIOD; TIDAL EVOLUTION; HOT JUPITERS; HD 147506B AB One possible diagnostic of planet formation, orbital migration, and tidal evolution is the angle Psi between a planet's orbital axis and the spin axis of its parent star. In general, Psi cannot be measured, but for transiting planets one can measure the angle gamma between the sky projections of the two axes via the Rossiter-McLaughlin effect. Here, we show how to combine measurements of gamma in different systems to derive statistical constraints on Psi. We apply the method to 11 published measurements of gamma, using two different single-parameter distributions to describe the ensemble. First, assuming a Rayleigh distribution (or more precisely, a Fisher distribution on a sphere), we find that the peak value is less than 22 degrees with 95% confidence. Second, assuming that a fraction f of the orbits have random orientations relative to the stars, and the remaining fraction (1 - f) are perfectly aligned, we find f < 0.36 with 95% confidence. This latter model fits the data better than the Rayleigh distribution, mainly because the XO-3 system was found to be strongly misaligned while the other 10 systems are consistent with perfect alignment. If the XO-3 result proves robust, then our results may be interpreted as evidence for two distinct modes of planet migration. C1 [Fabrycky, Daniel C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Fabrycky, DC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM daniel.fabrycky@gmail.com OI Fabrycky, Daniel/0000-0003-3750-0183 FU Michelson Fellowship; National Aeronautics and Space Administration (NASA) [JPL 1326712, NNX09AD36G] FX We thank Ed Turner for helpful conversations about astrostatistics and Scott Tremaine for comments on the manuscript. We thank the referee, Frederic Pont, for suggesting we quantitatively analyze non-Gaussian and catastrophic errors, for the XO-3 system in particular. D. F. gratefully acknowledges support from the Michelson Fellowship, supported by the National Aeronautics and Space Administration and administered by the Michelson Science Center. This work was partly supported by a grant from the NASA Keck PI Data Analysis Fund (JPL 1326712), and from the NASA Origins program (NNX09AD36G). NR 63 TC 127 Z9 127 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1230 EP 1240 DI 10.1088/0004-637X/696/2/1230 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700014 ER PT J AU Povich, MS Churchwell, E Bieging, JH Kang, M Whitney, BA Brogan, CL Kulesa, CA Cohen, M Babler, BL Indebetouw, R Meade, MR Robitaille, TP AF Povich, Matthew S. Churchwell, Ed Bieging, John H. Kang, Miju Whitney, Barbara A. Brogan, Crystal L. Kulesa, Craig A. Cohen, Martin Babler, Brian L. Indebetouw, Remy Meade, Marilyn R. Robitaille, Thomas P. TI THE EXTENDED ENVIRONMENT OF M17: A STAR FORMATION HISTORY SO ASTROPHYSICAL JOURNAL LA English DT Review DE H II regions; infrared: ISM; radio continuum: ISM; radio lines: ISM; stars: formation ID YOUNG STELLAR OBJECTS; 2-DIMENSIONAL RADIATIVE-TRANSFER; INFRARED ARRAY CAMERA; SPECTRAL ENERGY-DISTRIBUTIONS; RADIO-CONTINUUM SURVEY; LARGE-MAGELLANIC-CLOUD; GALACTIC HII-REGIONS; X-RAY-EMISSION; MOLECULAR CLOUD; MASSIVE STARS AB M17 is one of the youngest and most massive nearby star-formation regions in the Galaxy. It features a bright H II region erupting as a blister from the side of a giant molecular cloud (GMC). Combining photometry from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) with complementary infrared (IR) surveys, we identify candidate young stellar objects (YSOs) throughout a 1 degrees.5 x 1 degrees field that includes the M17 complex. The long sightline through the Galaxy behind M17 creates significant contamination in our YSO sample from unassociated sources with similar IR colors. Removing contaminants, we produce a highly reliable catalog of 96 candidate YSOs with a high probability of association with the M17 complex. We fit model spectral energy distributions to these sources and constrain their physical properties. Extrapolating the mass function of 62 intermediate-mass YSOs (M(star) > 3 M(circle dot)), we estimate that > 1000 stars are in the process of forming in the extended outer regions of M17. The remaining 34 candidate YSOs are found in a 0.17 deg(2) field containing the well-studied M17 H II region and photodissociation region (PDR), where bright diffuse mid-IR emission drastically reduces the sensitivity of the GLIMPSE point-source detections. By inspecting IR survey images from IRAS and GLIMPSE, we find that M17 lies on the rim of a large shell structure similar to 0 degrees.5 in diameter (similar to 20 pc at 2.1 kpc). We present maps of (12)CO and (13)CO (J = 2 -> 1) emission observed with the Heinrich Hertz Telescope. The CO emission shows that the shell is a coherent, kinematic structure associated with M17, centered at v = 19 km s(-1). The shell is an extended bubble outlining the PDR of a faint, diffuse H II region several Myr old. We identify a group of candidate ionizing stars within the bubble. YSOs in our catalog are concentrated around the bubble rim, providing evidence that massive star formation has been triggered by the expansion of the bubble. The formation of the massive cluster ionizing the M17 H II region itself may have been similarly triggered. We conclude that the star formation history in the extended environment of M17 has been punctuated by successive waves of massive star formation propagating through a GMC complex. C1 [Povich, Matthew S.; Churchwell, Ed; Babler, Brian L.; Meade, Marilyn R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Bieging, John H.; Kang, Miju; Kulesa, Craig A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kang, Miju] Chungnam Natl Univ, Korea Astron & Space Sci Inst, Taejon, South Korea. [Whitney, Barbara A.] Univ Colorado, Space Sci Inst, Boulder, CO 80303 USA. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Cohen, Martin] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Povich, MS (reprint author), Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53706 USA. EM povich@astro.wisc.edu OI Babler, Brian/0000-0002-6984-5752; Robitaille, Thomas/0000-0002-8642-1329 FU NASA/JPL [1275394]; NSF [AST-0303689, AST-0708131]; Spitzer Theoretical Research Program [1290701, 1310231]; NASA Theory Program [NNG05GH35G]; Korea Research Foundation [KRF-2007-612-C00050] FX We are indebted to Leisa Townsley for keen insights and suggestions that helped guide this work and for sharing early results from Chandra. We thank the anonymous referee for numerous comments that helped to substantially improve this work. Frank D. Ghigo, Ronald J. Maddalena, and Dana S. Balser provided the GBT 3 cm image used in our analysis. We thank Steve Bracker for IR color analysis of candidate AGB stars, David Pooley for finding the Einstein image, and Cormac Purcell for inspecting the CORNISH survey images on our behalf. Conversations with Debra Shepherd, Fabian Heitsch, and Kyle Westfall helped improve this work. We thank Dr. A. R. Kerr of the National Radio Astronomy Observatory for providing the single-sideband ALMA Band 6 prototype mixers used in this study. The Heinrich Hertz Telescope is operated by the Arizona Radio Observatory, a part of Steward Observatory at The University of Arizona. This work was supported by NASA/JPL contract 1275394 and NSF grant AST-0303689 to the University of Wisconsin. Additional support was provided by the Spitzer Theoretical Research Program (1290701 & 1310231; B. A. W., T. P. R.), the NASA Theory Program (NNG05GH35G; B. A. W.), and NSF grant AST-0708131 to The University of Arizona (M.K., J.H.B.). M. K. gratefully acknowledges support from a Korea Research Foundation Grant (KRF-2007-612-C00050). Additional support was provided by NASA through the Spitzer Space Telecopse Fellowship Program (T. P. R.). This work relies on observations made using the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory under a contract with NASA. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has also made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. NR 101 TC 55 Z9 56 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1278 EP 1306 DI 10.1088/0004-637X/696/2/1278 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700017 ER PT J AU Ghavamian, P Raymond, JC Blair, WP Long, KS Tappe, A Park, S Winkler, PF AF Ghavamian, Parviz Raymond, John C. Blair, William P. Long, Knox S. Tappe, Achim Park, Sangwook Winkler, P. Frank TI SPITZER SPECTROSCOPY OF THE GALACTIC SUPERNOVA REMNANT G292.0+1.8: STRUCTURE AND COMPOSITION OF THE OXYGEN-RICH EJECTA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; ISM: individual (G292.0+1.8); ISM: kinematics and dynamics; plasmas; shock waves; supernova remnants ID LARGE-MAGELLANIC-CLOUD; SPACE-TELESCOPE OBSERVATIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; MAJOR DUST FACTORIES; SHOCK-WAVE MODEL; NOVA REMNANT; X-RAY; INFRARED-EMISSION; OPTICAL-EMISSION; INTERSTELLAR DUST AB We present mid-infrared (mid-IR; 5-40 mu m) spectra of shocked ejecta in the Galactic oxygen-rich supernova remnant (SNR) G292.0+1.8, acquired with the Infrared Spectrograph onboard the Spitzer Space Telescope. The observations targeted two positions within the brightest oxygen-rich feature in G292.0+1.8. Emission lines of [Ne II] lambda 12.8, [Ne III] lambda lambda 15.5,36.0, [Ne V] lambda 24.3, and [O IV] lambda 25.9 mu m are detected from the shocked ejecta. In marked contrast to what is observed in Cassiopeia A, no discernible mid-IR emission from heavier species such as Mg, Si, S, Ar, or Fe is detected in G292.0+1.8. We also detect a broad emission bump between 15 and 28 mu m in spectra of the radiatively shocked O-rich ejecta in G292.0+1.8. We suggest that this feature arises from either shock-heated Mg(2)SiO(4) (forsterite) dust in the radiatively shocked O-rich ejecta or collisional excitation of polycyclic aromatic hydrocarbons in the blast wave of the SNR. If the former interpretation is correct, this would be the first mid-IR detection of ejecta dust in G292.0+1.8. A featureless dust continuum is also detected from nonradiative shocks in the circumstellar medium around G292.0+1.8. The mid-IR continuum from these structures, which lack mid-IR line emission, is seen in Chandra images as bright X-ray filaments, is well described by a two-component silicate dust model. The temperature of the hot dust component (M(d) similar to 2 x 10(-3) M(circle dot)) is similar to 115 K, while that of the cold component (roughly constrained to be less than or similar to 3 M(circle dot)) is similar to 35 K. We attribute the hot component to collisionally heated dust in the circumstellar shocks in G292.0+1.8, and attribute the cold component to dust heated by the hard FUV radiation from the circumstellar shocks. Using average O/Ne and O/Si mass ratios measured for a sample of ejecta knots in the X-rays, our models yield line strengths consistent with mass ratios M(O)/M(Ne) approximate to 3, M(O)/M(Si) greater than or similar to 61, and M(O)/M(S) approximate to 50. These ratios (especially the large O/Ne mass ratio) are difficult to reproduce with standard nucleosynthesis models of well-mixed supernova ejecta. This reinforces the conclusions of existing X-ray studies that the reverse shock in G292.0+1.8 is currently propagating into the hydrostatic nucleosynthetic layers of the progenitor star, and has not yet penetrated the layers dominated by explosive nucleosynthetic products. C1 [Ghavamian, Parviz; Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Raymond, John C.; Tappe, Achim] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Park, Sangwook] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Ghavamian, P (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM parviz@stsci.edu; jraymond@cfa.harvard.edu; parviz@pha.jhu.edu; long@stsci.edu; atappe@cfa.harvard.edu; park@astro.psu.edu; winkler@middlebury.edu FU NASA FX 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 the work of P. G. was supported by NASA through the Spitzer Guest Observer Program. NR 58 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1307 EP 1318 DI 10.1088/0004-637X/696/2/1307 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700018 ER PT J AU Langland-Shula, LE Vogt, SS Charbonneau, D Butler, P Marcy, G AF Langland-Shula, Laura E. Vogt, Steven S. Charbonneau, David Butler, Paul Marcy, Geoff TI A HIRES/KECK SPECTROSCOPIC INVESTIGATION OF THE MEASUREMENT OF SODIUM IN THE ATMOSPHERE OF HD 209458b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: atmospheres; stars: individual (HD 209458); techniques: photometric ID GIANT PLANET TRANSITS; TRANSMISSION SPECTRUM; NA-I; EXTRASOLAR; STAR; ABSORPTION; HD209458B; TELESCOPE; COMPANION; HD-209458 AB We present high-resolution High Resolution Echelle Spectrometer (HIRES)/Keck spectra of HD 209458, and a Monte Carlo variation on the basic method used by other workers, to look for the excess in-transit absorption in the NaD doublet at 5893 angstrom due to the extrasolar planet. The HIRES data, binned by bandpass, allow a direct comparison with previous results. We find >3 sigma results in most test bandpasses around the NaD doublet, including relative absorption of (-108.8 +/- 25.7) x 10(-5) in the "narrow" bandpass used by other workers. This is approximate to 4.7 times larger than the "narrow" results reported by Charbonneau et al. for HD 209458b. However, >2 sigma absorption is detected in some weak Fe I and Ni I lines that were tested for comparison, raising concern about the uncertainties introduced by continuum-fitting and terrestrial atmosphere subtraction. C1 [Langland-Shula, Laura E.; Vogt, Steven S.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Butler, Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Marcy, Geoff] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Langland-Shula, LE (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. OI Charbonneau, David/0000-0002-9003-484X FU NSF [AST-0307493] FX This work was supported by grant NSF AST-0307493. We are grateful to Al Conrad of the W. M. Keck Observatory, for heroic work in restoring the computer system in time for the night's transit. The anonymous referee provided useful suggestions to improve the manuscript. We also owe respectful appreciation to our gracious hosts, the native people of Hawaii, whose allowance of our scientific visits to the Mauna Kea summit gives us the opportunity to explore the processes of nature. NR 32 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1355 EP 1366 DI 10.1088/0004-637X/696/2/1355 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700022 ER PT J AU Randall, SW Jones, C Kraft, R Forman, WR O'Sullivan, E AF Randall, S. W. Jones, C. Kraft, R. Forman, W. R. O'Sullivan, E. TI MERGING COLD FRONTS IN THE GALAXY PAIR NGC 7619 AND NGC 7626 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (Pegasus, U842); galaxies: individual (NGC 7619, NGC 7626); X-rays: galaxies ID ELLIPTICAL GALAXIES; XMM-NEWTON; CLUSTERS; CATALOG; MERGER; CORES AB We present results from Chandra observations of the galaxy pair NGC 7619 and NGC 7626, the two dominant members of the Pegasus group. The X-ray images show a brightness edge associated with each galaxy, which we identify as merger cold fronts. The edges are sharp, and the axes of symmetry of the edges are roughly antiparallel, suggesting that these galaxies are falling toward one another in the plane of the sky. The detection of merger cold fronts in each of the two dominant member galaxies implies a merging subgroup scenario, since the alternative is that the galaxies are falling into a preexisting similar to 1 keV halo without a dominant galaxy of its own, and such objects are not observed. We estimate the three-dimensional velocities from the cold fronts and, using the observed radial velocities of the galaxies, show that the velocity vectors are indeed most likely close to the plane of the sky, with a relative velocity of similar to 1190 km s(-1). The relative velocity is consistent with what is expected from the infall of two roughly equal mass subgroups whose total viral mass equals that of the Pegasus group. We conclude that the Pegasus cluster is most likely currently forming from a major merger of two subgroups, dominated by NGC 7619 and NGC 7626. NGC 7626 contains a strong radio source, consisting of a core with two symmetric jets, and radio lobes. Although we find no associated structure in the X-ray surface brightness map, the temperature map reveals a clump of cool gas just outside the southern lobe, presumably entrained by the lobe, and possibly an extension of cooler gas into the lobe itself. The jet axis is parallel with the projected direction of motion of NGC 7626 (inferred from the symmetry axis of the merger cold front), and the southern leading jet is foreshortened as compared to the northern trailing one, possibly due to the additional ram pressure encountered by the forward jet. C1 [Randall, S. W.; Jones, C.; Kraft, R.; Forman, W. R.; O'Sullivan, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Randall, SW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Randall, Scott/0000-0002-3984-4337; O'Sullivan, Ewan/0000-0002-5671-6900 FU NASA [GO0-1026X]; Chandra X-ray Center [NAS8-03060]; Smithsonian Institution FX The financial support for this work was partially provided for by the NASA Chandra grant GO0-1026X, the Chandra X-ray Center through NAS8-03060, and the Smithsonian Institution. We thank Pasquale Mazzotta for useful comments. NR 28 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1431 EP 1440 DI 10.1088/0004-637X/696/2/1431 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700029 ER PT J AU Koutroumpa, D Lallement, R Raymond, JC Kharchenko, V AF Koutroumpa, D. Lallement, R. Raymond, J. C. Kharchenko, V. TI THE SOLAR WIND CHARGE-TRANSFER X-RAY EMISSION IN THE 1/4 keV ENERGY RANGE: INFERENCES ON LOCAL BUBBLE HOT GAS AT LOW Z SO ASTROPHYSICAL JOURNAL LA English DT Article DE interplanetary medium; ISM: bubbles; ISM: general; supernova remnants; X-rays: diffuse background; X-rays: general; X-rays: ISM ID EXTREME-ULTRAVIOLET EMISSION; PLASMA-SPECTROMETER CHIPS; HIGHLY IONIZED-GAS; INTERSTELLAR GAS; TERRESTRIAL MAGNETOSHEATH; SPECTROSCOPIC-EXPLORER; EXCHANGE EMISSION; BACKGROUND FLUX; GALACTIC HALO; HELIOSPHERE AB We present calculations of the heliospheric solar wind charge-exchange (SWCX) emission spectra and the resulting contributions of this diffuse background in the ROSAT 1/4 keV bands. We compare our results with the soft X-ray background (SXRB) emission detected in front of 378 identified shadowing regions during the ROSAT All-Sky Survey. This foreground component is principally attributed to the hot gas of the so-called Local Bubble (LB), an irregularly shaped cavity of similar to 50-150 pc around the Sun, which is supposed to contain similar to 10(6) K plasma. Our results suggest that the SWCX emission from the heliosphere is bright enough to account for most of the foreground emission toward the majority of low galactic latitude directions, where the LB is the least extended. On the other hand, in a large part of directions with galactic latitude above 30 degrees, the heliospheric SWCX intensity is significantly smaller than the measured one. However, the SWCX R2/R1 band ratio differs slightly from the data in the galactic center direction, and more significantly in the galactic anticentre direction where the observed ratio is the smallest. Assuming that both SWCX and hot gas emission are present and their relative contributions vary with direction, we tested a series of thermal plasma spectra for temperatures ranging from 10(5) to 10(6.5) K and searched for a combination of SWCX spectra and thermal emission matching the observed intensities and band ratios, while simultaneously being compatible with O VI emission measurements. In the frame of collisional equilibrium models and for solar abundances, the range we derive for hot gas temperature and emission measure cannot reproduce the Wisconsin C/B band ratio. This implies that accounting for SWCX contamination does not remove these known disagreements between data and classical hot gas models. We emphasize the need for additional atomic data, describing consistently EUV and X-ray photon spectra of the charge-exchange emission of heavier solar wind ions. C1 [Koutroumpa, D.; Lallement, R.] Univ Paris 06, Univ Versailles St Quentin en Yvellines, CNRS,IPSL Serv Aeron, UMR 7620, F-91371 Verrieres Le Buisson, France. [Raymond, J. C.; Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koutroumpa, D (reprint author), Univ Paris 06, Univ Versailles St Quentin en Yvellines, CNRS,IPSL Serv Aeron, UMR 7620, F-91371 Verrieres Le Buisson, France. NR 59 TC 48 Z9 48 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1517 EP 1525 DI 10.1088/0004-637X/696/2/1517 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700038 ER PT J AU Bakos, GA Pal, A Torres, G Sipocz, B Latham, DW Noyes, RW Kovacs, G Hartman, J Esquerdo, GA Fischer, DA Johnson, JA Marcy, GW Butler, RP Howard, AW Sasselov, DD Kovacs, G Stefanik, RP Lazar, J Papp, I Sari, P AF Bakos, G. A. Pal, A. Torres, G. Sipocz, B. Latham, D. W. Noyes, R. W. Kovacs, Geza Hartman, J. Esquerdo, G. A. Fischer, D. A. Johnson, J. A. Marcy, G. W. Butler, R. P. Howard, A. W. Sasselov, D. D. Kovacs, Gabor Stefanik, R. P. Lazar, J. Papp, I. Sari, P. TI HAT-P-10b: A LIGHT AND MODERATELY HOT JUPITER TRANSITING A K DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-10, GSC 02340-01714); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR GIANT PLANETS; ECCENTRIC ORBIT; BRIGHT STAR; MASSIVE PLANET; Y-2 ISOCHRONES; STELLAR; SEARCH; FIELD; TELESCOPE; PROJECT AB We report on the discovery of HAT-P-10b, one of the lowest mass (0.487 +/- 0.018 M(J)) transiting extrasolar planets (TEPs) discovered to date by transit searches. HAT-P-10b orbits the moderately bright V = 11.89 K dwarf GSC 02340-01714, with a period P = 3.7224747 +/- 0.0000065 days, transit epoch T(c) = 2454759.68683 +/- 0.00016 (BJD), and duration 0.1090 +/- 0.0008 days. HAT-P-10b has a radius of 1.005(-0.027)(+0.032) R(J) yielding a mean density of 0.594 +/- 0.052 g cm(-3). Comparing these observations with recent theoretical models we find that HAT-P10b is consistent with a similar to 4.5Gyr, almost pure hydrogen and helium gas giant planet with a 10 M(circle plus) core. With an equilibrium temperature of T(eq) = 1020 +/- 17 K, HAT-P-10b is one of the coldest TEPs. Curiously, its Safronov number theta = 0.053 +/- 0.002 falls close to the dividing line between the two suggested TEP populations. C1 [Bakos, G. A.; Pal, A.; Torres, G.; Sipocz, B.; Latham, D. W.; Noyes, R. W.; Hartman, J.; Esquerdo, G. A.; Sasselov, D. D.; Kovacs, Gabor; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary. [Pal, A.; Sipocz, B.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Fischer, D. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Johnson, J. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Butler, R. P.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20005 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Bakos, GA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbakos@cfa.harvard.edu RI Butler, Robert/B-1125-2009; Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G, NCC2-1390, N128Hr]; SAO IR D; NSF [AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation (OTKA) [K-60750]; NOAO [A285Hr] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR& D grants. The efforts of G.A.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). We also acknowledge partial support from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (PI: D. W. L.). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-60750. This research has made use of Keck telescope time granted through NOAO (program A285Hr) and NASA (N128Hr). NR 51 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1950 EP 1955 DI 10.1088/0004-637X/696/2/1950 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700075 ER PT J AU Patnaude, DJ Ellison, DC Slane, P AF Patnaude, Daniel J. Ellison, Donald C. Slane, Patrick TI THE ROLE OF DIFFUSIVE SHOCK ACCELERATION ON NONEQUILIBRIUM IONIZATION IN SUPERNOVA REMNANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; radiation mechanisms: thermal; shock waves; supernova remnants; X-rays: ISM ID X-RAY-EMISSION; NONLINEAR PARTICLE-ACCELERATION; FAST COLLISIONLESS SHOCKS; CASSIOPEIA-A; COSMIC-RAYS; TEMPERATURE EQUILIBRATION; RADIATIVE SHOCKS; RX J1713.7-3946; REVERSE SHOCKS; BLAST WAVE AB We present results of semianalytic calculations which show clear evidence for changes in the nonequilibrium ionization behind a supernova remnant forward shock undergoing efficient diffusive shock acceleration (DSA). The efficient acceleration of particles (i. e., cosmic rays (CRs)) lowers the shock temperature and raises the density of the shocked gas, thus altering the ionization state of the plasma in comparison to the test-particle (TP) approximation where CRs gain an insignificant fraction of the shock energy. The differences between the TP and efficient acceleration cases are substantial and occur for both slow and fast temperature equilibration rates: in cases of higher acceleration efficiency, particular ion states are more populated at lower electron temperatures. We also present results which show that, in the efficient shock acceleration case, higher ionization fractions are reached noticeably closer to the shock front than in the TP case, clearly indicating that DSA may enhance thermal X-ray production. We attribute this to the higher postshock densities which lead to faster electron temperature equilibration and higher ionization rates. These spatial differences should be resolvable with current and future X-ray missions, and can be used as diagnostics in estimating the acceleration efficiency in CR-modified shocks. C1 [Patnaude, Daniel J.; Slane, Patrick] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Patnaude, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. EM don_ellison@ncsu.edu FU Smithsonian Endowment Grant; NASA [NNH04Zss001N-LTSA, 06-ATP06-21] FX We thank Dick Edgar, John Raymond, and Cara Rakowski for several useful discussions on how to thoughtfully display and interpret ionization fractions. This work was partially supported through a Smithsonian Endowment Grant. D. J. P. and P. S. acknowledge support from NASA contract NAS8-39073 and D. C. E. acknowledges support from NASA grants NNH04Zss001N-LTSA and 06-ATP06-21. NR 39 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1956 EP 1963 DI 10.1088/0004-637X/696/2/1956 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700076 ER PT J AU Hachisuka, K Brunthaler, A Menten, KM Reid, MJ Hagiwara, Y Mochizuki, N AF Hachisuka, K. Brunthaler, A. Menten, K. M. Reid, M. J. Hagiwara, Y. Mochizuki, N. TI THE DISTANCE TO A STAR-FORMING REGION IN THE OUTER ARM OF THE GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; Galaxy: structure; masers; stars: distances ID MILKY-WAY-GALAXY; 3-DIMENSIONAL DISTRIBUTION; SOLAR CIRCLE; IRAS SOURCES; CO; DISK; ISM AB We performed astrometric observations with the Very Long Baseline Army of WB89-437, an H(2)O maser source in the Outer spiral arm of the Galaxy. We measure an annual parallax of 0.167 +/- 0.006 mas, corresponding to a heliocentric distance of 6.0 +/- 0.2 kpc or a Galactocentric distance of 13.4 +/- 0.2 kpc. This value for the heliocentric distance is considerably smaller than the kinematic distance of 8.6 kpc. This confirms the presence of a faint Outer arm toward l = 135 degrees. We also measured the full space motion of the object and find a large peculiar motion of similar to 20 km s(-1) toward the Galactic center. This peculiar motion explains the large error in the kinematic distance estimate. We also find that WB89-437 has the same rotation speed as the LSR, providing more evidence for a flat rotation curve and thus the presence of dark matter in the outer Galaxy. C1 [Hachisuka, K.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Hachisuka, K.; Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hagiwara, Y.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Mochizuki, N.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. RP Hachisuka, K (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. FU National Natural Science Foundation of China [10573029, 10625314, 10633010, 10821302]; Knowledge Innovation Program of the Chinese Academy of Sciences [KJCX2-YW-T03]; National Key Basic Research Development Program of China [2007CB815405]; China Postdoctoral Science Foundation [20070410745]; DFG [1177] FX This work was supported, in part, by the National Natural Science Foundation of China ( grants 10573029, 10625314, 10633010, and 10821302) and the Knowledge Innovation Program of the Chinese Academy of Sciences ( grant No. KJCX2-YW-T03), and the National Key Basic Research Development Program of China ( No. 2007CB815405). K. H. acknowledges the support by China Postdoctoral Science Foundation ( grant 20070410745). A. B. was supported by the DFG Priority Programme 1177. NR 24 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 1981 EP 1986 DI 10.1088/0004-637X/696/2/1981 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700079 ER PT J AU Kilic, M Kowalski, PM Reach, WT von Hippel, T AF Kilic, Mukremin Kowalski, Piotr M. Reach, William T. von Hippel, Ted TI SPITZER OBSERVATIONS OF THE OLDEST WHITE DWARFS IN THE SOLAR NEIGHBORHOOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: atmospheres; white dwarfs ID DIGITAL-SKY-SURVEY; INFRARED ARRAY CAMERA; VERY-LOW LUMINOSITY; SPACE-TELESCOPE; HELIUM-ATMOSPHERE; COOLING SEQUENCE; GALACTIC DISK; METAL-RICH; WARM DUST; AGE AB We present Spitzer 5-15 mu m spectroscopy of one cool white dwarf and 3.6-8 mu m photometry of 51 cool white dwarfs with T(eff) < 6000 K. The majority of our targets have accurate BVRIJHK photometry and trigonometric parallax measurements available, which enables us to perform a detailed model atmosphere analysis using their optical, near-and mid-infrared photometry with state-of-the-art model atmospheres. We demonstrate that the optical and infrared spectral energy distributions of cool white dwarfs are well reproduced by our grid of models. Our best-fit models are consistent with the observations within 5% in all filters except the IRAC 8 mu m band, which has the lowest signal-to-noise ratio photometry. Excluding the ultracool white dwarfs, none of the stars in our sample show significant mid-infrared flux deficits or excesses. The nondetection of mid-infrared excess flux around our approximate to 2-9 Gyr old targets constrain the fraction of cool white dwarfs with warm debris disks to 0.8(-0.8)(+1.5)%. C1 [Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kowalski, Piotr M.] Ruhr Univ Bochum, Lehrstuhl Theoret Chem, D-44780 Bochum, Germany. [Reach, William T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [von Hippel, Ted] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Kowalski, Piotr/L-7411-2013; OI Kowalski, Piotr/0000-0001-6604-3458; Reach, William/0000-0001-8362-4094 FU NASA; Caltech; NBR [1359963, 1288635]; University of Texas; NASA [1407] FX M. K. thanks D. Winget and S. Kenyon for useful discussions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech, and also award projects NBR 1359963 and 1288635 issued by JPL/Caltech to Ohio State University and the University of Texas. P. M. K. thanks D. Marx and the theoretical chemistry group at Ruhr-Universitat Bochum for their hospitality and support. 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 NASA contract 1407. NR 45 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 2094 EP 2103 DI 10.1088/0004-637X/696/2/2094 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700090 ER PT J AU Koposov, SE Yoo, J Rix, HW Weinberg, DH Maccio, AV Escude, JM AF Koposov, Sergey E. Yoo, Jaiyul Rix, Hans-Walter Weinberg, David H. Maccio, Andrea V. Miralda Escude, Jordi TI A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: formation; Galaxy: halo; Galaxy: structure; Local Group ID COLD DARK-MATTER; DIGITAL SKY SURVEY; DWARF SPHEROIDAL GALAXIES; LAMBDA-CDM UNIVERSE; ULTRA-FAINT DWARFS; STAR-FORMATION; LOCAL GROUP; GALACTIC SATELLITES; DISK GALAXIES; LUMINOSITY FUNCTION AB We revisit the well known discrepancy between the observed number of Milky Way (MW) dwarf satellite companions and the predicted population of cold dark matter (CDM) subhalos, in light of the dozen new low-luminosity satellites found in imaging data from the Sloan Digital Sky Survey (SDSS) and our recent calibration of the SDSS satellite detection efficiency, which implies a total satellite population far larger than these dozen discoveries. We combine a detailed dynamical model for the CDM subhalo population with simple, physically motivated prescriptions for assigning a stellar content to each subhalo, then apply observational selection effects and compare to the current observational census. Reconciling the observed satellite population with CDM predictions still requires strong mass-dependent suppression of star formation in low-mass subhalos: models in which the stellar mass is a constant fraction F-*(Omega(b)/Omega(m)) of the subhalo mass M-sat at the time it becomes a satellite fail for any choice of F-*. However, previously advocated models that invoke suppression of gas accretion after reionization in halos with circular velocity V-circ <= V-crit approximate to 35 km s(-1) can reproduce the observed satellite counts for -15 <= M-V <= 0. Successful models require F-* approximate to 10(-3) in halos with V-circ > V-crit and strong suppression of star formation before reionization in halos with V-circ less than or similar to 10 km s(-1); models without pre-reionization suppression predict far too many satellites with -5 <= M-V <= 0. In this successful model, the dominant fraction of stars formed after reionization at all luminosities. Models that match the satellite luminosity distribution also match the observed heliocentric radius distribution, and they reproduce the observed characteristic stellar velocity dispersion sigma(*) approximate to 5-10 km s(-1) of the SDSS dwarfs given the observed sizes (similar to 50-200 pc) of their stellar distributions. The model satellites have M(< 300 pc) similar to 10(7) M-circle dot as observed even though their present-day total halo masses span more than two orders of magnitude; the constancy of central masses mainly reflects the profiles of CDM halos. Our modeling shows that natural physical mechanisms acting within the CDM framework can quantitatively explain the properties of the MW satellite population as it is presently known, thus providing a convincing solution to the "missing satellite" problem. C1 [Koposov, Sergey E.; Rix, Hans-Walter; Maccio, Andrea V.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Koposov, Sergey E.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Koposov, Sergey E.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Yoo, Jaiyul] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron & CCAPP, Columbus, OH 43210 USA. [Miralda Escude, Jordi] Univ Barcelona, Inst Ciencies Cosmos, E-08007 Barcelona, Spain. [Miralda Escude, Jordi] Inst Catalana Rec & Estudis Avancats, Barcelona, Spain. RP Koposov, SE (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM koposov@mpia.de RI Koposov, Sergey/F-2754-2012; OI Koposov, Sergey/0000-0003-2644-135X; Miralda-Escude, Jordi/0000-0002-2316-8370; Maccio, Andrea/0000-0002-8171-6507 FU DFG [SFB 439]; EARA-EST Marie Curie Visiting fellowship; Harvard College Observatory; NSF [AST-0707985] FX S. K. was supported by the DFG through SFB 439 and by a EARA-EST Marie Curie Visiting fellowship. J. Y. is supported by the Harvard College Observatory under the Donald H. Menzel fund. D. W. acknowledges support from NSF grant AST-0707985 and the hospitality of the Institut d'Astrophysique de Paris during part of this work. S. K. acknowledges hospitality from the Kavli Institute for Theoretical Physics (KITP) Santa Barbara during the workshop "Building the Milky Way." We thank James Bullock for his helpful comments on the paper and the anonymous referee for prompt review and constructive comments. NR 87 TC 150 Z9 152 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 MAY 10 PY 2009 VL 696 IS 2 BP 2179 EP 2194 DI 10.1088/0004-637X/696/2/2179 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700097 ER PT J AU Watson, CR Kochanek, CS Forman, WR Hickox, RC Jones, CJ Brown, MJI Brand, K Dey, A Jannuzi, BT Kenter, AT Murray, SS Vikhlinin, A Eisenstein, DJ Fazio, GG Green, PJ McNamara, BR Rieke, M Shields, JC AF Watson, Casey R. Kochanek, Christopher S. Forman, William R. Hickox, Ryan C. Jones, Christine J. Brown, Michael J. I. Brand, Kate Dey, Arjun Jannuzi, Buell T. Kenter, Almus T. Murray, Steve S. Vikhlinin, Alexey Eisenstein, Daniel J. Fazio, Giovani G. Green, Paul J. McNamara, Brian R. Rieke, Marcia Shields, Joseph C. TI THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES IN THE AGES SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; Galaxy: evolution ID DEEP-FIELD NORTH; X-RAY-PROPERTIES; LYMAN BREAK GALAXIES; PRINCIPAL COMPONENT ANALYSIS; ALPHA LUMINOSITY FUNCTION; FORMATION RATE INDICATOR; FIBER-FED SPECTROGRAPH; FORMING GALAXIES; H-ALPHA; ELLIPTIC GALAXIES AB We combine IR, optical, and X-ray data from the overlapping, 9.3 deg(2) NOAO Deep Wide-Field Survey, AGN and Galaxy Evolution Survey (AGES), and XBootes Survey to measure the X-ray evolution of 6146 normal galaxies as a function of absolute optical luminosity, redshift, and spectral type over the largely unexplored redshift range 0.1 less than or similar to z less than or similar to 0.5. Because only the closest or brightest of the galaxies are individually detected in X-rays, we use a stacking analysis to determine the mean properties of the sample. Our results suggest that X-ray emission from spectroscopically late-type galaxies is dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like similar to (1 + z)(3 +/- 1), in agreement with the trends found for samples of bright, individually detectable starburst galaxies and AGN. Our work also corroborates the results of many previous stacking analyses of faint source populations, with improved statistics. C1 [Watson, Casey R.] Millikin Univ, Dept Phys & Astron, Decatur, IL 62522 USA. [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. [Forman, William R.; Hickox, Ryan C.; Jones, Christine J.; Kenter, Almus T.; Murray, Steve S.; Vikhlinin, Alexey; Fazio, Giovani G.; Green, Paul J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Brand, Kate] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dey, Arjun; Jannuzi, Buell T.; Rieke, Marcia] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Eisenstein, Daniel J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McNamara, Brian R.; Shields, Joseph C.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. RP Watson, CR (reprint author), Millikin Univ, Dept Phys & Astron, 1184 W Main St, Decatur, IL 62522 USA. EM crwatson@millikin.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Forman, William/0000-0002-9478-1682 FU National Optical Astronomy Observatory FX 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. Spectroscopic observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We thank the CXC for scheduling the Chandra X-ray Observatory observations that made this work possible and the CXC Data Processing Team for the pipeline data. NR 96 TC 11 Z9 11 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 2206 EP 2219 DI 10.1088/0004-637X/696/2/2206 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700099 ER PT J AU Shetty, R Kauffmann, J Schnee, S Goodman, AA Ercolano, B AF Shetty, Rahul Kauffmann, Jens Schnee, Scott Goodman, Alyssa A. Ercolano, Barbara TI THE EFFECT OF LINE-OF-SIGHT TEMPERATURE VARIATION AND NOISE ON DUST CONTINUUM OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; ISM: clouds; methods: miscellaneous; stars: formation ID ISOLATED STAR-FORMATION; PRE-STELLAR CORES; DARK CLOUD; INTERSTELLAR DUST; EMISSION MAPS; SUBMILLIMETER EMISSION; INITIAL CONDITIONS; INFRARED-EMISSION; SPECTRAL INDEX; COLUMN DENSITY AB We investigate the effect of line-of-sight temperature variations and noise on two commonly used methods to determine dust properties from dust-continuum observations of dense cores. One method employs a direct fit to a modified blackbody spectral energy distribution (SED); the other involves a comparison of flux ratios to an analytical prediction. Fitting fluxes near the SED peak produces inaccurate temperature and dust spectral index estimates due to the line-of-sight temperature (and density) variations. Longer wavelength fluxes in the Rayleigh-Jeans part of the spectrum (greater than or similar to 600 mu m for typical cores) may more accurately recover the spectral index, but both methods are very sensitive to noise. The temperature estimate approaches the density-weighted temperature, or "column temperature," of the source as short wavelength fluxes are excluded. An inverse temperature-spectral index correlation naturally results from SED fitting, due to the inaccurate isothermal assumption, as well as noise uncertainties. We show that above some " threshold" temperature, the temperatures estimated through the flux ratio method can be highly inaccurate. In general, observations with widely separated wavelengths, and including shorter wavelengths, result in higher threshold temperatures; such observations thus allow for more accurate temperature estimates of sources with temperatures less than the threshold temperature. When only three fluxes are available, a constrained fit, where the spectral index is fixed, produces less scatter in the temperature estimate when compared to the estimate from the flux ratio method. C1 [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.; Ercolano, Barbara] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.] Harvard Univ, Inst Innovat Comp, Cambridge, MA 02138 USA. [Schnee, Scott] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Ercolano, Barbara] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Shetty, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rshetty@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU Owens Valley Radio Observatory; National Science Foundation [AST 05-40399]; Harvard Initiative in Innovative Computing FX We thank P. Myers, D. Johnstone, J. Foster, J. Pineda, E. Rosolowsky, and S. Chakrabarti for useful discussions. We also thank N. Wright for help in executing MOCASSIN. In our analysis, we have made extensive use of NEMO software (Teuben 1995). S. S. acknowledges support from the Owens Valley Radio Observatory, which is supported by the National Science Foundation through grant AST 05-40399. R. S., J. K., and A. G. acknowledge support from the Harvard Initiative in Innovative Computing, which hosts the Star-Formation Taste Tests Community at which further details on these results can be found and discussed (see http://www.cfa.harvard.edu/similar to agoodman/tastetests). NR 43 TC 112 Z9 112 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2009 VL 696 IS 2 BP 2234 EP 2251 DI 10.1088/0004-637X/696/2/2234 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 441IO UT WOS:000265762700101 ER PT J AU Gluckman, PD Hanson, MA Bateson, P Beedle, AS Law, CM Bhutta, ZA Anokhin, KV Bougneres, P Chandak, GR Dasgupta, P Smith, GD Ellison, PT Forrester, TE Gilbert, SF Jablonka, E Kaplan, H Prentice, AM Simpson, SJ Uauy, R West-Eberhard, MJ AF Gluckman, Peter D. Hanson, Mark A. Bateson, Patrick Beedle, Alan S. Law, Catherine M. Bhutta, Zulfiqar A. Anokhin, Konstantin V. Bougneres, Pierre Chandak, Giriraj Ratan Dasgupta, Partha Smith, George Davey Ellison, Peter T. Forrester, Terrence E. Gilbert, Scott F. Jablonka, Eva Kaplan, Hillard Prentice, Andrew M. Simpson, Stephen J. Uauy, Ricardo West-Eberhard, Mary Jane TI Towards a new developmental synthesis: adaptive developmental plasticity and human disease SO LANCET LA English DT Editorial Material ID CHILD UNDERNUTRITION; DIABETES-MELLITUS; RANDOMIZED-TRIAL; EARLY-LIFE; HEALTH; CONSEQUENCES; NUTRITION; OBESITY; FETAL; GROWTH C1 [Gluckman, Peter D.; Beedle, Alan S.] Univ Auckland, Liggins Inst, Auckland 1023, New Zealand. [Hanson, Mark A.] Univ Southampton, Inst Dev Sci, Southampton, Hants, England. [Bateson, Patrick] Univ Cambridge, Subdept Anim Behav, Cambridge CB3 8AA, England. [Law, Catherine M.] UCL, Inst Child Hlth, London, England. [Bhutta, Zulfiqar A.] Aga Khan Univ, Dept Paediat, Karachi, Pakistan. [Anokhin, Konstantin V.] Russian Acad Med Sci, PK Anokhin Inst Normal Physiol, Dept Systemogenesis, Moscow, Russia. [Bougneres, Pierre] Hop St Vincent de Paul, Dept Pediat Endocrinol, F-75674 Paris, France. [Bougneres, Pierre] Hop St Vincent de Paul, INSERM, U561, F-75674 Paris, France. [Chandak, Giriraj Ratan] Ctr Cellular & Mol Biol, Genome Res Grp, Hyderabad 500007, Andhra Pradesh, India. [Dasgupta, Partha] Univ Cambridge, Fac Econ, Cambridge, England. [Smith, George Davey] Univ Bristol, Dept Social Med, Bristol, Avon, England. [Ellison, Peter T.] Harvard Univ, Dept Anthropol, Cambridge, MA 02138 USA. [Forrester, Terrence E.] Univ W Indies, Res Inst Trop Med, Kingston 7, Jamaica. [Gilbert, Scott F.] Swarthmore Coll, Dept Biol, Swarthmore, PA 19081 USA. [Jablonka, Eva] Tel Aviv Univ, Cohn Inst Hist & Philosophy Sci & Ideas, IL-69978 Tel Aviv, Israel. [Kaplan, Hillard] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Prentice, Andrew M.] London Sch Hyg & Trop Med, Int Nutr Grp, London WC1, England. [Simpson, Stephen J.] Univ Sydney, Sch Biol Sci, Sydney, NSW 2006, Australia. [Uauy, Ricardo] Univ Chile, Inst Nutr & Food Technol, Santiago, Chile. [West-Eberhard, Mary Jane] Univ Costa Rica, Smithsonian Trop Res Inst, Sch Biol, San Pedro, Costa Rica. RP Gluckman, PD (reprint author), Univ Auckland, Liggins Inst, Private Bag 92019, Auckland 1023, New Zealand. EM pd.gluckman@auckland.ac.nz OI Monsalve, Beatriz Elena/0000-0002-5994-866X; Law, Catherine/0000-0002-1777-9386 FU Medical Research Council [G0600705] NR 43 TC 170 Z9 173 U1 4 U2 54 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0140-6736 EI 1474-547X J9 LANCET JI Lancet PD MAY 9 PY 2009 VL 373 IS 9675 BP 1654 EP 1657 PG 4 WC Medicine, General & Internal SC General & Internal Medicine GA 445QJ UT WOS:000266066300036 PM 19427960 ER PT J AU Winterton, SL Woodley, NE AF Winterton, Shaun L. Woodley, Norman E. TI New species of Metatrichia Coquillett (Diptera: Scenopinidae) from Australia and Venezuela SO ZOOTAXA LA English DT Article DE Metatrichia; Asiloidea; Therevoid clade; Scenopinidae AB Two new species of the cosmopolitan genus Metatrichia Coquillett are described. Metatrichia dhimurru sp. nov. is described from Arnhem Land (Northern Territory), Australia and represents the third species of the genus to be described from the Australasian region. Metatrichia venezuelensis sp. nov. from Venezuela is the third extant species of the genus to be described from the New World. C1 [Winterton, Shaun L.] Queensland Dept Primary Ind & Fisheries, Indooroopilly, Qld, Australia. [Winterton, Shaun L.] Univ Queensland, Sch Biol Sci, St Lucia, Qld, Australia. [Woodley, Norman E.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Winterton, SL (reprint author), Queensland Dept Primary Ind & Fisheries, 80 Meiers Rd, Indooroopilly, Qld, Australia. EM wintertonshaun@gmail.com; norman.woodley@ars.usda.gov RI Woodley, Norman/M-6160-2014 FU National Science Foundation (USA) [DEB-0614213] FX Thank you to the Dhimurru and Northern Territory Land Councils for permission to collect in Arnhem Land (Parks and Wildlife Commission of the Northern Territory permit number: 26827). Permits applications and logistical support were provided in part by the Australian National Insect Collection (ANIC). This research was supported by a National Science Foundation (USA) grant (DEB-0614213) to SLW. Statements and viewpoints expressed herein do not necessarily reflect the opinion of NSF. We thank Steven W. Lingafelter and Allen L. Norrbom (both Systematic Entomology Laboratory), Wayne N. Mathis (Smithsonian Institution) and two anonymous reviewers for comments on the draft manuscript. NR 19 TC 4 Z9 4 U1 0 U2 0 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 MAY 8 PY 2009 IS 2094 BP 42 EP 51 PG 10 WC Zoology SC Zoology GA 447ZT UT WOS:000266231600005 ER PT J AU Haiman, Z Kocsis, B Menou, K Lippai, Z Frei, Z AF Haiman, Zoltan Kocsis, Bence Menou, Kristen Lippai, Zoltan Frei, Zsolt TI Identifying decaying supermassive black hole binaries from their variable electromagnetic emission SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article; Proceedings Paper CT 7th International LISA Symposium CY JUN 16-20, 2008 CL Barcelona, SPAIN SP LISA Int Sci Team, Inst Estudis Espacials Catalunya ID WAVE STANDARD SIRENS; DISK; AFTERGLOW; ACCRETION; LISA AB Supermassive black hole binaries (SMBHBs) with masses in the mass range similar to(10(4)-10(7)) M-circle dot/(1 + z), produced in galaxy mergers, are thought to complete their coalescence due to the emission of gravitational waves (GWs). The anticipated detection of the GWs by the future Laser Interferometric Space Antenna (LISA) will constitute a milestone for fundamental physics and astrophysics. While the GW signatures themselves will provide a treasure trove of information, if the source can be securely identified in electromagnetic (EM) bands, this would open up entirely new scientific opportunities, to probe fundamental physics, astrophysics and cosmology. We discuss several ideas, involving wide-field telescopes, that may be useful in locating electromagnetic counterparts to SMBHBs detected by LISA. In particular, the binary may produce a variable electromagnetic flux, such as a roughly periodic signal due to the orbital motion prior to coalescence, or a prompt transient signal caused by shocks in the circumbinary disc when the SMBHB recoils and 'shakes' the disc. We discuss whether these time-variable EM signatures may be detectable, and how they can help in identifying a unique counterpart within the localization errors provided by LISA. We also discuss a possibility of identifying a population of coalescing SMBHBs statistically, in a deep optical survey for periodically variable sources, before LISA detects the GWs directly. The discovery of such sources would confirm that gas is present in the vicinity and is being perturbed by the SMBHB-serving as a proof of concept for eventually finding actual LISA counterparts. C1 [Haiman, Zoltan; Menou, Kristen] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Kocsis, Bence] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kocsis, Bence] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Lippai, Zoltan; Frei, Zsolt] Eotvos Lorand Univ, Inst Phys, Budapest, Hungary. RP Haiman, Z (reprint author), Columbia Univ, Dept Astron, New York, NY 10027 USA. RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 NR 30 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2009 VL 26 IS 9 AR 094032 DI 10.1088/0264-9381/26/9/094032 PG 11 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 435NC UT WOS:000265349600033 ER PT J AU Barros, W Gochberg, DF Gore, JC AF Barros, Wilson, Jr. Gochberg, Daniel F. Gore, John C. TI Nuclear magnetic resonance signal dynamics of liquids in the presence of distant dipolar fields, revisited SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article DE diffusion; iterative methods; magnetisation; nuclear magnetic resonance; perturbation theory ID MULTIPLE-QUANTUM COHERENCES; SPIN-ECHO METHOD; DIFFUSION MEASUREMENTS; SOLUTION NMR; MOLECULAR-DIFFUSION; GRADIENT; ENHANCEMENT; IDQC AB The description of the nuclear magnetic resonance magnetization dynamics in the presence of long-range dipolar interactions, which is based upon approximate solutions of Bloch-Torrey equations including the effect of a distant dipolar field, has been revisited. New experiments show that approximate analytic solutions have a broader regime of validity as well as dependencies on pulse-sequence parameters that seem to have been overlooked. In order to explain these experimental results, we developed a new method consisting of calculating the magnetization via an iterative formalism where both diffusion and distant dipolar field contributions are treated as integral operators incorporated into the Bloch-Torrey equations. The solution can be organized as a perturbative series, whereby access to higher order terms allows one to set better boundaries on validity regimes for analytic first-order approximations. Finally, the method legitimizes the use of simple analytic first-order approximations under less demanding experimental conditions, it predicts new pulse-sequence parameter dependencies for the range of validity, and clarifies weak points in previous calculations. C1 [Barros, Wilson, Jr.; Gochberg, Daniel F.; Gore, John C.] Vanderbilt Univ, Med Ctr, Inst Imaging Sci VUIIS, AA MCN 1105, Nashville, TN 37232 USA. RP Barros, W (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 59,60 Garden St, Cambridge, MA 02138 USA. EM wbarros@cfa.harvard.edu FU NCRR NIH HHS [1S10RR17799-01]; NIBIB NIH HHS [5R21EB004040-2, R21 EB004040] NR 40 TC 6 Z9 6 U1 1 U2 4 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 MAY 7 PY 2009 VL 130 IS 17 AR 174506 DI 10.1063/1.3116107 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 448LC UT WOS:000266263100029 PM 19425789 ER PT J AU Bromm, V Yoshida, N Hernquist, L Mckee, CF AF Bromm, Volker Yoshida, Naoki Hernquist, Lars McKee, Christopher F. TI The formation of the first stars and galaxies SO NATURE LA English DT Review ID INITIAL MASS FUNCTION; GAMMA-RAY BURSTS; HIGH-REDSHIFT UNIVERSE; POPULATION-III STARS; COLD-DARK-MATTER; LARGE-SCALE STRUCTURE; METAL-POOR STARS; RADIATIVE FEEDBACK; SUPERNOVA EXPLOSIONS; PRIMORDIAL STAR AB Observations made using large ground-based and space-borne telescopes have probed cosmic history from the present day to a time when the Universe was less than one-tenth of its present age. Earlier still lies the remaining frontier, where the first stars, galaxies and massive black holes formed. They fundamentally transformed the early Universe by endowing it with the first sources of light and chemical elements beyond the primordial hydrogen and helium produced in the Big Bang. The interplay of theory and upcoming observations promises to answer the key open questions in this emerging field. C1 [Bromm, Volker] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Yoshida, Naoki] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McKee, Christopher F.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. RP Bromm, V (reprint author), Univ Texas Austin, Dept Astron, 2511 Speedway, Austin, TX 78712 USA. EM vbromm@astro.as.utexas.edu RI Yoshida, Naoki/A-4305-2011 FU NSF; NASA FX We are grateful for the hospitality of KITP, University of California Santa Barbara. This work was supported in part by NSF and NASA. NR 100 TC 184 Z9 185 U1 1 U2 15 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 7 PY 2009 VL 459 IS 7243 BP 49 EP 54 DI 10.1038/nature07990 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 441WN UT WOS:000265801300026 PM 19424148 ER PT J AU Jungers, WL Harcourt-Smith, WEH Wunderlich, RE Tocheri, MW Larson, SG Sutikna, T Due, RA Morwood, MJ AF Jungers, W. L. Harcourt-Smith, W. E. H. Wunderlich, R. E. Tocheri, M. W. Larson, S. G. Sutikna, T. Due, Rhokus Awe Morwood, M. J. TI The foot of Homo floresiensis SO NATURE LA English DT Article ID PRESSURE DISTRIBUTION; LATE PLEISTOCENE; HADAR HOMINIDS; EVOLUTION; LOCOMOTION; BIPEDALISM; INDONESIA; DMANISI; FOSSILS; GAIT AB Homo floresiensis is an endemic hominin species that occupied Liang Bua, a limestone cave on Flores in eastern Indonesia, during the Late Pleistocene epoch(1,2). The skeleton of the type specimen (LB1) of H. floresiensis includes a relatively complete left foot and parts of the right foot(3). These feet provide insights into the evolution of bipedalism and, together with the rest of the skeleton, have implications for hominin dispersal events into Asia. Here we show that LB1's foot is exceptionally long relative to the femur and tibia, proportions never before documented in hominins but seen in some African apes. Although the metatarsal robusticity sequence is human-like and the hallux is fully adducted, other intrinsic proportions and pedal features are more ape-like. The postcranial anatomy of H. floresiensis is that of a biped(1-3), but the unique lower-limb proportions and surprising combination of derived and primitive pedal morphologies suggest kinematic and biomechanical differences from modern human gait. Therefore, LB1 offers the most complete glimpse of a bipedal hominin foot that lacks the full suite of derived features characteristic of modern humans and whose mosaic design may be primitive for the genus Homo. These new findings raise the possibility that the ancestor of H. floresiensis was not Homo erectus but instead some other, more primitive, hominin whose dispersal into southeast Asia is still undocumented. C1 [Jungers, W. L.; Larson, S. G.] SUNY Stony Brook, Med Ctr, Dept Anat Sci, Stony Brook, NY 11794 USA. [Harcourt-Smith, W. E. H.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Wunderlich, R. E.] James Madison Univ, Dept Biol Sci, Harrisonburg, VA 22807 USA. [Tocheri, M. W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Humans Origins Program, Washington, DC 20013 USA. [Sutikna, T.; Due, Rhokus Awe] Natl Res & Dev Ctr Archaeol, Jakarta 12001, Indonesia. [Morwood, M. J.] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW 2522, Australia. RP Jungers, WL (reprint author), SUNY Stony Brook, Med Ctr, Dept Anat Sci, Stony Brook, NY 11794 USA. EM william.jungers@stonybrook.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU Australian Research Council; National Geographic Society; Wenner-Gren Foundation for Anthropological Research; Wellcome Trust and the Leakey Foundation FX This work was supported by grants from the Australian Research Council, the National Geographic Society, the Wenner-Gren Foundation for Anthropological Research, the Wellcome Trust and the Leakey Foundation. We also thank our colleagues Jatmiko, E. Wahyu Saptomo and T. Djubiantono for their encouragement and assistance in the excavations. NR 30 TC 81 Z9 83 U1 11 U2 67 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 7 PY 2009 VL 459 IS 7243 BP 81 EP 84 DI 10.1038/nature07989 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 441WN UT WOS:000265801300033 PM 19424155 ER PT J AU Reudink, MW Marra, PP Kyser, TK Boag, PT Langin, KM Ratcliffe, LM AF Reudink, Matthew W. Marra, Peter P. Kyser, T. Kurt Boag, Peter T. Langin, Kathryn M. Ratcliffe, Laurene M. TI Non-breeding season events influence sexual selection in a long-distance migratory bird SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE non-breeding; sexual selection; American redstart; carry-over; extra-pair paternity; polygyny ID REDSTARTS SETOPHAGA-RUTICILLA; SOCIALLY MONOGAMOUS BIRD; EXTRAPAIR PATERNITY; AMERICAN-REDSTARTS; ECOLOGICAL CONDITIONS; REPRODUCTIVE SUCCESS; HABITAT SEGREGATION; ARRIVAL DATE; WINTER; WARBLER AB The study of sexual selection has traditionally focused on events and behaviours immediately surrounding copulation. In this study, we examine whether carry-over effects from the non-breeding season can influence the process of sexual selection in a long-distance migratory bird, the American redstart (Setophaga ruticilla). Previous work on American redstarts demonstrated that overwintering in a high-quality habitat influences spring departure dates from the wintering grounds, advances arrival dates on the breeding grounds and increases apparent reproductive success. We show that the mixed-mating strategy of American redstarts compounds the benefits of overwintering in high-quality winter habitats. Males arriving to breed in Canada from high-quality winter habitats arrive earlier than males from poor-quality habitats, resulting in a lower probability of paternity loss, a higher probability of achieving polygyny and ultimately higher realized reproductive success. Such results suggest that the process of sexual selection may be influenced by events interacting throughout the annual cycle. C1 [Reudink, Matthew W.; Boag, Peter T.; Langin, Kathryn M.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Reudink, Matthew W.; Marra, Peter P.] Queens Univ, Dept Geol Sci & Geol Engn, Kingston, ON K7L 3N6, Canada. [Kyser, T. Kurt] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Reudink, MW (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. EM mattreudink@gmail.com RI Boag, Peter/B-2907-2014 OI Boag, Peter/0000-0003-0050-2089 FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation; National Science Foundation [0085965]; Smithsonian Institution; Queen's University; Ontario Innovation Trust; Sigma Xi; American Ornithologists; Society of Canadian Ornithologists; American Museum of Natural History FX We gratefully acknowledge the many field assistants who contributed to this study. R. Reudink, R. Germain, A. McKellar, C. Studds, A. Tottrup, S. Bearhop and an anonymous reviewer provided insightful comments on this manuscript. C. Studds provided invaluable statistical help. K. Klassen and A. Vuletich provided critical isotope analysis assistance and we thank C. Scott for molecular assistance. Funding was provided by the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, a National Science Foundation grant to P. P. M. ( 0085965), the Smithsonian Institution, Queen's University, Ontario Innovation Trust, Sigma Xi, the American Ornithologists' Union, the Society of Canadian Ornithologists and the American Museum of Natural History. NR 43 TC 79 Z9 79 U1 7 U2 52 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD MAY 7 PY 2009 VL 276 IS 1662 BP 1619 EP 1626 DI 10.1098/rspb.2008.1452 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 422RI UT WOS:000264445000010 PM 19203918 ER PT J AU Garen, EJ Saltonstall, K Slusser, JL Mathias, S Ashton, MS Hall, JS AF Garen, Eva J. Saltonstall, Kristin Slusser, Jacob L. Mathias, Shane Ashton, Mark S. Hall, Jefferson S. TI An evaluation of farmers' experiences planting native trees in rural Panama: implications for reforestation with native species in agricultural landscapes SO AGROFORESTRY SYSTEMS LA English DT Article DE On-farm trials; Project evaluation; Tree planting; Agroforestry; Silvopastoral; Smallholder farmers; PRORENA ID CENTRAL-AMERICA; COSTA-RICA; AGROFORESTRY; PREFERENCES; CULTIVATION; PERCEPTIONS; BANGLADESH; COMMUNITY; FORESTRY; PROJECTS AB In the Republic of Panama, reforestation with native species is of great interest, but many landholders often do not participate in tree planting projects and little information exists about landholder interest in, or experiences with, native trees. This study evaluates the experiences of farmers participating in a native species reforestation initiative in rural Panama to identify lessons learned that can guide on-going or future tree planting efforts. Based on the results of a questionnaire administered to program participants and non-participants (n = 68), we found that trees are important to farmers for multiple reasons, primary a variety of environmental and economic benefits. No relationship between the size of landholdings or land tenure status and the desire to plant trees was found. All participants in the program considered their experience to be positive, few had problems with their plantations, and most were interested in planting more native trees. The program's frequent and ongoing technical support was an important factor for farmers. These results indicate widespread interest in, and success with, planting native species and underscore the need to systematically examine farmers' interests and perceptions when planning, implementing, and evaluating reforestation initiatives. C1 [Garen, Eva J.; Saltonstall, Kristin; Hall, Jefferson S.] Smithsonian Trop Res Inst, CTFS, Balboa, Ancon, Panama. [Slusser, Jacob L.; Mathias, Shane] Panama Amer Embassy, Ciudad Del Saber, Clayton, Panama. [Ashton, Mark S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Garen, EJ (reprint author), Smithsonian Trop Res Inst, CTFS, Apartado 0843-03092, Balboa, Ancon, Panama. EM eva.garen@yale.edu FU Agora Foundation; Frank Levinson Family Foundation FX We would like to thank the farmers of Rio Hato and Los Santos for their participation and patience with this study. We are also grateful to PRORENA staff-members and affiliates who contributed to aspects of the design and implementation of this research, including Jairo Batista, Jose Deago, Brian Love, Emilio Mariscal, Anayansi Batista Vera, and Mark Wishnie. A special thank you to Dr. Amity Doolittle, Dr. Michael Dove, Bradford Gentry, and Helen Poulos from the Yale School of Forestry and Environmental Studies, as well as to Jose Manuel Perez, Dr. Rick Condit, and Dr. Stanley Heckadon for their guidance and input in various stages of this research. We also appreciate the efforts of Milton Sorano from STRI who produced the map for this analysis. Funding for this research was provided by the Agora Foundation and the Frank Levinson Family Foundation. NR 36 TC 24 Z9 24 U1 1 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-4366 J9 AGROFOREST SYST JI Agrofor. Syst. PD MAY PY 2009 VL 76 IS 1 BP 219 EP 236 DI 10.1007/s10457-009-9203-4 PG 18 WC Agronomy; Forestry SC Agriculture; Forestry GA 437XZ UT WOS:000265521500017 ER PT J AU Wallace, LE Weller, SG Wagner, WL Sakai, AK Nepokroeff, M AF Wallace, Lisa E. Weller, Stephen G. Wagner, Warren L. Sakai, Ann K. Nepokroeff, Molly TI PHYLOGEOGRAPHIC PATTERNS AND DEMOGRAPHIC HISTORY OF SCHIEDEA GLOBOSA (CARYOPHYLLACEAE) ON THE HAWAIIAN ISLANDS SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE ancestral polymorphism; Caryophyllaceae; gene coalescence; DNA sequence; intraspecific variation; migration; phylogeography; Schiedea globosa ID MAXIMUM-LIKELIHOOD-ESTIMATION; POPULATION-GROWTH; MIGRATION RATES; NORTH-AMERICA; UNSAMPLED POPULATIONS; PHYLOGENETIC NETWORKS; SAMPLED POPULATIONS; COALESCENT APPROACH; ADAPTIVE RADIATION; MITOCHONDRIAL-DNA AB Geomorphological changes have been demonstrated to have had profound impacts on biodiversity, often leading to demographic expansions and contractions and allopatric divergence of taxa. We examined DNA sequence variation at two nuclear and one maternally inherited plastid locus among 10 populations of Schiedea globosa on the Hawaiian Islands to assess the Primary factors shaping genetic structure, phylogeographic patterns, and the importance of geogaphic isolation to population divergence. Schiedea globosa has characteristics that may promote gene flow, including wind pollination and rafting of plants in ocean currents. However we detected significant differentiation among populations on all islands except Hawaii, with the maternally inherited plastid locus having the the greatest genetic structure (F(ST) = 0.81). Migration rates across all loci are less than ine migrant pergeneration. We found evidence of growth in several populations and on the islands of Molokai and Maui, which supports population expansion associated with the formation of Maui Nui during the last glacial maximum. Similar to data for many other Hawaiian taxa, these data suggest S. globosa originated on Oahu and subsequently colonized Molokai, Maui, and Hawaii in progression. Given the high level of genetic structure, allopatric divergence will likely contribute to further diverence of populations. C1 [Wallace, Lisa E.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. [Weller, Stephen G.; Sakai, Ann K.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Nepokroeff, Molly] Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA. RP Wallace, LE (reprint author), Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. EM Lisawallace@biology.msstate.edu FU National Science Foundation [DEB-0445410] FX This work was funded by grant DEB-0445410 from the National Science Foundation. NR 68 TC 12 Z9 12 U1 1 U2 12 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD MAY PY 2009 VL 96 IS 5 BP 958 EP 967 DI 10.3732/ajb.0800243 PG 10 WC Plant Sciences SC Plant Sciences GA 443HN UT WOS:000265900900010 PM 21628248 ER PT J AU Lopano, CL Heaney, PJ Post, JE AF Lopano, Christina L. Heaney, Peter J. Post, Jeffrey E. TI Cs-exchange in birnessite: Reaction mechanisms inferred from time-resolved X-ray diffraction and transmission electron microscopy SO AMERICAN MINERALOGIST LA English DT Article DE Cation exchange; cesium; birnessite; synchrotron; X-ray diffraction; transmission electron microscopy ID POWDER DIFFRACTION; MANGANESE-DIOXIDE; CATION-EXCHANGE; ION-EXCHANGE; RIETVELD REFINEMENT; CRYSTAL-STRUCTURES; HANFORD SITE; CHEMISTRY; MINERALS; OXIDES AB We have explored the exchange of Cs for interlayer Na in birnessite using several techniques, including transmission electron microscopy (TEM) and time-resolved synchrotron X-ray diffraction (XRD). Our goal was to test which of two possible exchange mechanisms is operative during the reaction: (1) diffusion of cations in and out of the interlayer or (2) dissolution of Na-birnessite and reprecipitation of Cs-birnessite. The appearance of distinct XRD peaks for Na- and Cs-rich phases in partially exchanged samples offered support for a simple diffusion model, but it was inconsistent with the compositional and crystallographic homogeneity of (Na,Cs)-birnessite platelets from core to rim as ascertained by TEM. Time-resolved XRD revealed systematic changes in the structure of the emergent Cs-rich birnessite phase during exchange, in conflict with a dissolution and reprecipitation model. Instead, we propose that exchange Occurred by sequential delamination of Mn oxide octahedral sheets. Exfoliation of a given interlayer region allowed for wholesale replacement of Na by Cs and was rapidly followed by reassembly. This model accounts for the rapidity of metal exchange ill birnessite, the co-existence of distinct Na- and Cs-birnessite phases during the process of exchange, and the uniformly mixed Na- and Cs-compositions ascertained from point analyses by selected area electron diffraction and energy dispersive spectroscopy of partially exchanged grains. C1 [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Lopano, Christina L.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Lopano, CL (reprint author), RJ Lee Grp Inc, 350 Hochberg Rd, Monroeville, PA 15146 USA. EM clopano@rjlg.com FU NSF [EAR01-25908, EAR04-17741, CHE-0431328]; Center for Environmental Kinetics Analysis (CEKA); MSA; National Synchrotron Light Source; Brookhaven National Laboratory; U.S. Department of Energy [DE-AC02-98CH10886] FX Funding for this research was provided by NSF grants EAR01-25908, EAR04-17741, the Center for Environmental Kinetics Analysis (CEKA), an NSF- and DOE-sponsored Environmental Molecular Science Institute (NSF CHE-0431328), and by the MSA Grant from the Edward H. Kraus Crystallographic Research Fund. A portion of this research was carried out at the National Synchrotron Light Source, Brookhaven National Laboratory, which is supported by the U.S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences, under Contract No. DE-AC02-98CH10886. NR 49 TC 17 Z9 17 U1 2 U2 24 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X J9 AM MINERAL JI Am. Miner. PD MAY-JUN PY 2009 VL 94 IS 5-6 BP 816 EP 826 DI 10.2138/am.2009.3068 PG 11 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 445VA UT WOS:000266078400019 ER PT J AU Hultgren, KM Stachowicz, JJ AF Hultgren, K. M. Stachowicz, J. J. TI Evolution of Decoration in Majoid Crabs: A Comparative Phylogenetic Analysis of the Role of Body Size and Alternative Defensive Strategies SO AMERICAN NATURALIST LA English DT Article DE Majoidea; camouflage; independent contrasts; decoration; color change ID INDEPENDENT CONTRASTS; SPIDER CRAB; CONSPICUOUS COLORATION; CHIONOECETES-JAPONICUS; CORRELATED EVOLUTION; CRYPTIC COLORATION; WARNING COLORATION; CHEMICAL DEFENSE; MAJA SQUINADO; CAMOUFLAGE AB Although experimental studies have demonstrated the antipredatory advantages of camouflage and its associated costs, few studies have examined the evolution of camouflage in a phylogenetic context. We use phylogenetic comparative methods to examine evolutionary trade-offs associated with camouflage in the crab superfamily Majoidea. The majoids, or spider crabs, are known for their decoration behavior in which they attach materials from their environment to hooked setae on their carapace. We found that coverage of hooked setae on a crab (morphology) strongly predicts decoration cover in the field (behavior). Half of the species examined exhibited decreases in the coverage of hooked setae with ontogeny, and we also found a strong negative correlation between the extent of hooked setae and adult body size among species using independent contrasts, suggesting that size may constrain the evolution of camouflage. Finally, using a well-resolved clade of epialtids (kelp crabs)-many of which decorate little but use color change as an alternative camouflage strategy-we found a negative correlation between utilization of decoration versus color camouflage strategies. Our findings suggest that the costs of hook production and decoration maintenance and/or the lowered adaptive value of camouflage for larger species may limit the evolutionary distribution of decoration camouflage among the majoids. C1 [Hultgren, K. M.; Stachowicz, J. J.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Hultgren, K. M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Hultgren, KM (reprint author), Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. EM hultgrenk@si.edu RI Hultgren, Kristin/F-6862-2011 FU National Science Foundation [OCE 0082049] FX This work could not have been done without the generous help of curators and collection managers who provided access to majoid specimens at several museums, including the Los Angeles County Natural History Museum, the Smithsonian Institution, the California Academy of Sciences, and the British Natural History Museum. J. Byrnes, C. Duluc, M. Hickerson, M. Ishida, L. LaPlante, B. Mahon, A. Palma, E. Sotka, and P. Wirtz also provided specimens and, in some cases, taxonomic help in identifying specimens. S. Aubery, J. Byrnes, M. Ishida, T. Mai, M. Nydam, P. Thanh, and K. Wada provided field and data collection assistance. The National Science Foundation provided support through grant OCE 0082049 (to J. J. S.) and a graduate research fellowship (to K. M. H.). This manuscript was greatly improved by the comments of A. Crawford, J. Davis, and two anonymous reviewers. In addition, G. Davis, J. Martin, J. Neigel, and P. Wainwright provided important insights about the phylogeny and systematics work. NR 75 TC 19 Z9 21 U1 3 U2 29 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD MAY PY 2009 VL 173 IS 5 BP 566 EP 578 DI 10.1086/597797 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 427XQ UT WOS:000264812800003 PM 19278336 ER PT J AU Bokony, V Lendvai, AZ Liker, A Angelier, F Wingfield, JC Chastel, O AF Bokony, Veronika Lendvai, Adam Z. Liker, Andras Angelier, Frederic Wingfield, John C. Chastel, Olivier TI Stress Response and the Value of Reproduction: Are Birds Prudent Parents? SO AMERICAN NATURALIST LA English DT Article DE corticosterone; life history; brood value; evolution; comparative method; birds ID ADRENOCORTICAL RESPONSES; CORTICOSTERONE RESPONSES; OLDER PARENTS; BASE-LINE; TESTOSTERONE; SUCCESS; MODULATION; EVOLUTION; SELECTION; COSTS AB In vertebrates, stressors such as starvation or predator attacks stimulate the rapid elevation of circulating glucocorticoid hormones, triggering physiological and behavioral responses that aid immediate survival but simultaneously inhibit reproduction. This stress response has been proposed to serve as a physiological mediator of life-history trade-offs: when the value of current reproduction is high relative to the value of future reproduction and survival, a mitigated stress response is expected to enable successful breeding and maximize fitness. Using phylogenetic comparative analyses, we investigated baseline and peak stress-induced plasma corticosterone levels during parental care in 64 bird species. We found that (1) species with a higher value of the current brood relative to future breeding mounted weaker corticosterone responses during acute stress, and (2) females in species with more female-biased parental care had weaker corticosterone responses. These results support the brood value hypothesis, suggesting that the stress response evolves as an adaptive basis for life-history strategies. Further, we found that (3) baseline corticosterone correlated positively with brood value and negatively with body mass, and (4) peak corticosterone was greater in species breeding at higher latitudes. The latter findings suggest that circulating corticosterone concentrations might be matched to the anticipated demands and risks during nesting. C1 [Bokony, Veronika; Lendvai, Adam Z.; Angelier, Frederic; Chastel, Olivier] CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, Beauvoir Sur Ni, France. [Lendvai, Adam Z.] Coll Nyiregyhaza, Inst Biol, H-4400 Nyiregyhaza, Hungary. [Bokony, Veronika; Liker, Andras] Univ Pannonia, Dept Limnol, H-8201 Veszprem, Hungary. [Angelier, Frederic] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Wingfield, John C.] Univ Calif Davis, Dept Neurobiol Physiol & Behav, Davis, CA 95616 USA. RP Bokony, V (reprint author), CNRS, Ctr Etud Biol Chize, F-79360 Villiers En Bois, Beauvoir Sur Ni, France. EM vbokony@enternet.hu RI Lendvai, Adam/B-8546-2008; OI Lendvai, Adam/0000-0002-8953-920X; Bokony, Veronika/0000-0002-2136-5346 FU Centre Nationale de la Recherche Scientifique (CNRS); Hungarian Academy of Sciences; Hungarian Scholarship Board; National Office for Research and Technology [NKTH; FR-33/2007]; Fyssen Foundation [17348RC]; Hungarian Scientific Research Fund [PD76862]; National Science Foundation [IOS-0750540]; Institut Polaire Francais [109, 330]; Direction Regionale de l'Environnement (DIREN) Reunion,; DIREN Guyane; CNRS/Region Poitou-Charentes FX We thank R. Freckleton for providing unpublished R functions for the PGLS procedure. V. B. and A A. Z. L. were supported by joint grants from the Centre Nationale de la Recherche Scientifique (CNRS) and the Hungarian Academy of Sciences; V. B. was supported by an Eotvos State Grant from the Hungarian Scholarship Board (MOB); A. Z. L. was supported by the National Office for Research and Technology (NKTH; FR-33/2007) and E Egide (17348RC), a postdoctoral grant from the Fyssen Foundation, and a grant from the Hungarian Scientific Research Fund (OTKA; PD76862); and J. C. W. was funded by a National Science Foundation grant (IOS-0750540). Field operations for O. C. and F. A. were funded by Institut Polaire Francais (IPEV, programmes 109 and 330), CNRS, Direction Regionale de l'Environnement (DIREN) Reunion, and DIREN Guyane. F. A. was supported by a Bourses de Doctorat pour Ingenieurs grant from CNRS/Region Poitou-Charentes. At the Centre d'Etudes Biologiques de Chize, we are grateful to S. Dano, A. Lacroix, and C. Trouve for their technical assistance in hormone assays and molecular sexing and to D. Besson for help in the management of the long-term database. NR 52 TC 133 Z9 135 U1 4 U2 85 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD MAY PY 2009 VL 173 IS 5 BP 589 EP 598 DI 10.1086/597610 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 427XQ UT WOS:000264812800005 PM 19281425 ER PT J AU Kawashima, T Thorington, RW Whatton, JF AF Kawashima, Tomokazu Thorington, Richard W., Jr. Whatton, James F. TI Comparative Anatomy and Evolution of the Cardiac Innervation in New World Monkeys (Platyrrhini, E. Geoffroy, 1812) SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE cardiac nerve; cardiac branch; heart; New World monkey; comparative anatomy; primate evolution ID AUTONOMIC NERVOUS-SYSTEM; CHICK HEART AB The morphology of the autonomic cardiac nervous system (ACNS) was examined in 24 sides of 12 New World monkeys (Platyrrhini) of all four families to document the morphology systematically and to study the evolutionary changes of the ACNS in this primate lineage. We report the following: (1) Although several trivial intra- and inter-specific variations are present, a family-dependent morphology of the ACNS does not exist in New World monkeys. (2) The sympathetic ganglia in New World monkeys consist of the superior cervical, the middle cervical, and the cervicothoracic which is composed of the inferior cervical and first and second thoracic, and the thoracic ganglia starting with the third thoracic. The general cardiac nervous system is the sympathetic middle and inferior cardiac nerves and all parasympathetic vagal cardiac branches. (3) The morphology of the ACNS in the New World monkeys is almost consistent regardless of the number of vertebrae, the cardiac position and deviation (axis), and the great arterial branching pattern of the aortic arch, and it is very similar to that in the Old World monkeys, with only one difference: the superior cervical ganglion in the New World monkeys tends to be relatively smaller, higher, and provides a narrower contribution to the spinal nerves than in the Old World monkeys. The ACNS morphology exhibits significant evolutionary changes within the primate lineage from New and Old World monkeys to humans. The comparative morphology within the lineage is concordant with the phylogeny, suggesting that the primate ACNS preserves its evolutionary history in close alignment with phylogeny. Anat Rec, 292:670-691, 2009. (C) 2009 Wiley-Liss, Inc. C1 [Kawashima, Tomokazu; Thorington, Richard W., Jr.; Whatton, James F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, Washington, DC 20013 USA. RP Kawashima, T (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Mammals, 10th & Constitut Ave NW,NHB 390,MRC 108, Washington, DC 20013 USA. EM kawashimat@si.edu FU Japanese Ministry of Education, Culture, Sports, Science, and Technology [16790804, 19790985, 12008-2009] FX Grant sponsor: Scientific Research from the Japanese Ministry of Education, Culture, Sports, Science, and Technology (2004-2006 and 2007-2009); Grant numbers: 16790804, 19790985; Grant sponsor: International Research Program by the Japanese Ministry of Education, Culture, Sports, Science, and Technology (12008-2009). NR 50 TC 8 Z9 8 U1 2 U2 5 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD MAY PY 2009 VL 292 IS 5 BP 670 EP 691 DI 10.1002/ar.20894 PG 22 WC Anatomy & Morphology SC Anatomy & Morphology GA 441JV UT WOS:000265766000007 PM 19382232 ER PT J AU Sharp, K Arthur, KE Gu, L Ross, C Harrison, G Gunasekera, SP Meickle, T Matthew, S Luesch, H Thacker, RW Sherman, DH Paul, VJ AF Sharp, Koty Arthur, Karen E. Gu, Liangcai Ross, Cliff Harrison, Genelle Gunasekera, Sarath P. Meickle, Theresa Matthew, Susan Luesch, Hendrik Thacker, Robert W. Sherman, David H. Paul, Valerie J. TI Phylogenetic and Chemical Diversity of Three Chemotypes of Bloom-Forming Lyngbya Species (Cyanobacteria: Oscillatoriales) from Reefs of Southeastern Florida SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BIOSYNTHETIC GENE-CLUSTER; TURTLES CHELONIA-MYDAS; MARINE CYANOBACTERIA; NATURAL-PRODUCTS; CURACIN-A; LINEAR LIPOPEPTIDES; CYCLIC-PEPTIDES; MAJUSCULA; TOXINS; IDENTIFICATION AB The cyanobacterial genus Lyngbya includes free-living, benthic, filamentous cyanobacteria that form periodic nuisance blooms in lagoons, reefs, and estuaries. Lyngbya spp. are prolific producers of biologically active compounds that deter grazers and help blooms persist in the marine environment. Here, our investigations reveal the presence of three distinct Lyngbya species on nearshore reefs in Broward County, FL, sampled in 2006 and 2007. With a combination of morphological measurements, molecular biology techniques, and natural products chemistry, we associated these three Lyngbya species with three distinct Lyngbya chemotypes. One species, identified as Lyngbya cf. confervoides via morphological measurements and 16S rRNA gene sequencing, produces a diverse array of bioactive peptides and depsipeptides. Our results indicate that the other two Lyngbya species produce either microcolins A and B or curacin D and dragonamides C and D. Results from screening for the biosynthetic capacity for curacin production among the three Lyngbya chemotypes in this study correlated that capacity with the presence of curacin D. Our work on these bloom-forming Lyngbya species emphasizes the significant phylogenetic and chemical diversity of the marine cyanobacteria on southern Florida reefs and identifies some of the genetic components of those differences. C1 [Sharp, Koty; Arthur, Karen E.; Harrison, Genelle; Gunasekera, Sarath P.; Meickle, Theresa; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Gu, Liangcai; Sherman, David H.] Univ Michigan, Inst Life Sci, Ann Arbor, MI 48109 USA. [Gu, Liangcai; Sherman, David H.] Univ Michigan, Dept Med Chem, Ann Arbor, MI 48109 USA. [Gu, Liangcai; Sherman, David H.] Univ Michigan, Dept Chem, Ann Arbor, MI 48109 USA. [Gu, Liangcai; Sherman, David H.] Univ Michigan, Dept Microbiol & Immunol, Ann Arbor, MI 48109 USA. [Ross, Cliff] Univ N Florida, Jacksonville, FL 32224 USA. [Matthew, Susan; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Thacker, Robert W.] Univ Alabama, Dept Biol, Birmingham, AL 35294 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM paul@si.edu RI Gu, Lin/F-3980-2010; Gu, Liangcai/E-4600-2010; Arthur, Karen/A-3089-2012; Matthew, Susan/E-3817-2012; Ross, Cliff/B-8291-2011 FU National Oceanic and Atmospheric Administration's; Mote Marine Laboratory's Protect Our Reefs [POR-2006-18]; National Oceanic and Atmospheric Administration's Sea Grant Office, U. S Department of Commerce [NA06OAR4170014]; Smithsonian; Florida Fish and Wildlife Conservation Commission/Fish and Wildlife Research Institute [05011]; David and Ursula Blackburn; Rackham; NIH [CA108874] FX This is Smithsonian Marine Station at Fort Pierce contribution no. 774. NR 65 TC 27 Z9 30 U1 2 U2 17 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 MAY 1 PY 2009 VL 75 IS 9 BP 2879 EP 2888 DI 10.1128/AEM.02656-08 PG 10 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 438WO UT WOS:000265586900034 PM 19270119 ER PT J AU Ness, JU Drake, JJ Beardmore, AP Boyd, D Bode, MF Brady, S Evans, PA Gaensicke, BT Kitamoto, S Knigge, C Miller, I Osborne, JP Page, KL Rodriguez-Gil, P Schwarz, G Staels, B Steeghs, D Takei, D Tsujimoto, M Wesson, R Zijlstra, A AF Ness, J. -U. Drake, J. J. Beardmore, A. P. Boyd, D. Bode, M. F. Brady, S. Evans, P. A. Gaensicke, B. T. Kitamoto, S. Knigge, C. Miller, I. Osborne, J. P. Page, K. L. Rodriguez-Gil, P. Schwarz, G. Staels, B. Steeghs, D. Takei, D. Tsujimoto, M. Wesson, R. Zijlstra, A. TI SWIFT X-RAY AND ULTRAVIOLET MONITORING OF THE CLASSICAL NOVA V458 VUL (NOVA VUL 2007) SO ASTRONOMICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: individual (V458 Vul) ID INTERSTELLAR-MEDIUM; SPECTRAL EVOLUTION; HERCULIS 1991; V382 VELORUM; RS-OPHIUCHI; V1974 CYGNI; GK-PERSEI; H-I; EMISSION; OUTBURST AB We describe the highly variable X-ray and UV emission of V458 Vul (Nova Vul 2007), observed by Swift between 1 and 422 days after outburst. Initially bright only in the UV, V458 Vul became a variable hard X-ray source due to optically thin thermal emission at kT = 0.64 keV with an X-ray band unabsorbed luminosity of 2.3 x 10(34) erg s(-1) during days 71-140. The X-ray spectrum at this time requires a low Fe abundance (0.2(-0.1)(+ 0.3) solar), consistent with a Suzaku measurement around the same time. On day 315 we find a new X-ray spectral component which can be described by a blackbody with temperature of kT = 23(-5)(+9) eV, while the previous hard X-ray component has declined by a factor of 3.8. The spectrum of this soft X-ray component resembles those typically seen in the class of supersoft sources (SSS) which suggests that the nova ejecta were starting to clear and/or that the white dwarf photosphere is shrinking to the point at which its thermal emission reaches into the X-ray band. We find a high degree of variability in the soft component with a flare rising by an order of magnitude in count rate in 0.2 days. In the following observations on days 342.4-383.6, the soft component was not seen, only to emerge again on day 397. The hard component continued to evolve, and we found an anticorrelation between the hard X-ray emission and the UV emission, yielding a Spearman rank probability of 97%. After day 397, the hard component was still present, was variable, and continued to fade at an extremely slow rate but could not be analyzed owing to pile-up contamination from the bright SSS component. C1 [Ness, J. -U.] European Space Astron Ctr, Madrid 28691, Spain. [Ness, J. -U.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Drake, J. J.; Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beardmore, A. P.; Evans, P. A.; Osborne, J. P.; Page, K. L.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Boyd, D.] BAA VSS, W Challow OX12 9TX, Wantage, England. [Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Brady, S.] AAVSO, Hudson, NH 03051 USA. [Gaensicke, B. T.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Kitamoto, S.; Takei, D.] Rikkyo Univ, Dept Phys, Tokyo 1718501, Japan. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Miller, I.] BAA VSS, Swansea SA2 7LE, W Glam, Wales. [Rodriguez-Gil, P.] Isaac Newton Grp, Santa Cruz de La Palma 38700, Spain. [Rodriguez-Gil, P.] Inst Astrofis Canarias, E-38205 Santa Cruz de Tenerife, Spain. [Schwarz, G.] W Chester Univ, Dept Geol & Astron, W Chester, PA 19383 USA. [Staels, B.] Alan Guth Observ, CBA Flanders, Hofstade, Aalst, Belgium. [Tsujimoto, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Tsujimoto, M.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Kanagawa 2290015, Japan. [Wesson, R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Zijlstra, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. RP Ness, JU (reprint author), European Space Astron Ctr, POB 78, Madrid 28691, Spain. EM juness@sciops.esa.int RI Gaensicke, Boris/A-9421-2012; Steeghs, Danny/C-5468-2009; XRAY, SUZAKU/A-1808-2009; Rodriguez-Gil, Pablo/H-7709-2015 OI Gaensicke, Boris/0000-0002-2761-3005; Steeghs, Danny/0000-0003-0771-4746; Rodriguez-Gil, Pablo/0000-0002-4717-5102 FU NASA [PF5-60039, PF6-70044, NAS8-03060, NAS8-39073]; NSF; STFC FX We thank the Swift PI Neil Gehrels and Swift schedulers for their support of these TOOobservations. J.-U.N. and M. T. gratefully acknowledge support provided by NASA through Chandra Postdoctoral Fellowship grants PF5-60039 and PF6-70044, respectively, awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. J. J. D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center during the course of this research. D. T. acknowledges support from a JSPS fellowship. S. S. received partial support from NSF and NASA grants to ASU. K. L. P., A. P. B, P. A. E., and J. P. O. acknowledge support from STFC. D. S. acknowledges an STFC Advanced Fellowship. NR 47 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2009 VL 137 IS 5 BP 4160 EP 4168 DI 10.1088/0004-6256/137/5/4160 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900009 ER PT J AU Meszaros, S Dupree, AK Szalai, T AF Meszaros, Sz. Dupree, A. K. Szalai, T. TI MASS OUTFLOW AND CHROMOSPHERIC ACTIVITY OF RED GIANT STARS IN GLOBULAR CLUSTERS. II. M13 AND M92 SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (M13, M15, M92, NGC 2808); stars: AGB and post-AGB; stars: chromospheres; stars: mass loss ID HORIZONTAL-BRANCH STARS; COLOR-MAGNITUDE DIAGRAMS; RADIAL-VELOCITIES; 2ND PARAMETER; RELATIVE AGES; H-ALPHA; INTRACLUSTER MEDIUM; OMEGA-CENTAURI; GALACTIC HALO; MAIN-SEQUENCE AB High-resolution spectra of 123 red giant stars in the globular cluster M13 and 64 red giant stars in M92 were obtained with Hectochelle at the MMT telescope. Emission and line asymmetries in H alpha and Ca II K are identified, characterizing motions in the extended atmospheres and seeking differences attributable to metallicity in these clusters and M15. On the red giant branch, emission in H alpha generally appears in stars with T(eff) less than or similar to 4500 K and log L/L(circle dot) greater than or similar to 2.75. Fainter stars showing emission are asymptotic giant branch (AGB) stars or perhaps binary stars. The line-bisector for H alpha reveals the onset of chromospheric expansion in stars more luminous than log (L/L(circle dot)) similar to 2.5 in all clusters, and this outflow velocity increases with stellar luminosity. However, the coolest giants in the metal-rich M13 show greatly reduced outflow in H alpha most probably due to decreased Teff and changing atmospheric structure. The Ca II K(3) outflow velocities are larger than shown by H alpha at the same luminosity and signal accelerating outflows in the chromospheres. Stars clearly on the AGB show faster chromospheric outflows in H alpha than RGB objects. While the H alpha velocities on the RGB are similar for all metallicities, the AGB stars in the metal-poor M15 and M92 have higher outflow velocities than in the metal-rich M13. Comparison of these chromospheric line profiles in the paired metal-poor clusters, M15 and M92, shows remarkable similarities in the presence of emission and dynamical signatures, and does not reveal a source of the "second-parameter" effect. C1 [Meszaros, Sz.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meszaros, Sz.; Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6701 Szeged, Hungary. RP Meszaros, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM meszi@cfa.harvard.edu; dupree@cfa.harvard.edu; szaszi@titan.physx.u-szeged.hu RI Meszaros, Szabolcs/N-2287-2014 OI Meszaros, Szabolcs/0000-0001-8237-5209 FU NASA; Hungarian OTKA [TS049872, T042509, K76816]; Smithsonian Astrophysical Observatory FX We thank the referee for very detailed comments that significantly improved the presentation. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We are grateful to the scientists at CfA who are developing and characterizing Hectochelle: Nelson Caldwell, Daniel G. Fabricant, Gabor Furesz, David W. Latham, and Andrew Szentgyorgyi. The authors also thank John Roll and Maureen A. Conroy for developing SPICE software, and Mike Alegria, John McAfee, Ale Milone, Michael Calkins, and Perry Berlind for their help during the observations. Kyle Cudworth kindly provided coordinates and photometry for M13 and M92 stars. Szabolcs Meszaros is supported in part by a SAO Predoctoral Fellowship, NASA, and the Hungarian OTKA grants TS049872, T042509, and K76816. This research is also supported in part by the Smithsonian Astrophysical Observatory. NR 74 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2009 VL 137 IS 5 BP 4282 EP 4295 DI 10.1088/0004-6256/137/5/4282 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900013 ER PT J AU Bayliss, DDR Weldrake, DTF Sackett, PD Tingley, BW Lewis, KM AF Bayliss, Daniel D. R. Weldrake, David T. F. Sackett, Penny D. Tingley, Brandon W. Lewis, Karen M. TI THE LUPUS TRANSIT SURVEY FOR HOT JUPITERS: RESULTS AND LESSONS SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric ID PHOTOMETRIC STANDARD STARS; EXTRASOLAR PLANET; IMAGE SUBTRACTION; LIGHT CURVES; FIELD; SEARCH; ATMOSPHERE; RADIATION; EMISSION; CATALOG AB We present the results of a deep, wide-field transit survey targeting "Hot Jupiter" planets in the Lupus region of the Galactic plane conducted over 53 nights concentrated in two epochs separated by a year. Using the Australian National University 40-inch telescope at Siding Spring Observatory (SSO), the survey covered a 0.66 deg(2) region close to the Galactic plane (b = 11 degrees) and monitored a total of 110,372 stars (15.0 <= V <= 22.0). Using difference imaging photometry, 16,134 light curves with a photometric precision of sigma < 0.025 mag were obtained. These light curves were searched for transits, and four candidates were detected that displayed low-amplitude variability consistent with a transiting giant planet. Further investigations, including spectral typing and radial velocity measurements for some candidates, revealed that of the four, one is a true planetary companion (Lupus-TR-3), two are blended systems (Lupus-TR-1 and 4), and one is a binary (Lupus-TR-2). The results of this successful survey are instructive for optimizing the observational strategy and follow-up procedure for deep searches for transiting planets, including an upcoming survey using the SkyMapper telescope at SSO. C1 [Bayliss, Daniel D. R.; Sackett, Penny D.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Weldrake, David T. F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tingley, Brandon W.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Lewis, Karen M.] Monash Univ, Sch Math Sci, Clayton, Vic 3800, Australia. RP Bayliss, DDR (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Cotter Rd, Weston, ACT 2611, Australia. EM daniel@mso.anu.edu.au; dweldrak@cfa.harvard.edu; penny.sackett@anu.edu.au; btingley@iac.es; karen.lewis@sci.monash.edu.au RI Bayliss, Daniel/I-4635-2012; Tingley, Brandon/E-5146-2014 OI Tingley, Brandon/0000-0003-4483-2661 NR 30 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2009 VL 137 IS 5 BP 4368 EP 4376 DI 10.1088/0004-6256/137/5/4368 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430WB UT WOS:000265019900020 ER PT J AU Fontani, F Zhang, Q Caselli, P Bourke, TL AF Fontani, F. Zhang, Q. Caselli, P. Bourke, T. L. TI Linking pre- and proto-stellar objects in the intermediate-/high-mass star forming region IRAS 05345+3157 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules ID ULTRACOMPACT HII-REGIONS; PROTOSTELLAR CANDIDATES; EVOLUTIONARY STATUS; MOLECULAR OUTFLOWS; INITIAL CONDITIONS; TEMPERATURE PROBE; GAS EMISSION; CLOUD CORES; DENSE GAS; MILLIMETER AB Context. To better understand the initial conditions of the high-mass star formation process, it is crucial to study at high angular resolution the morphology, the kinematics, and the interactions of the coldest condensations associated with intermediate-/high-mass star forming regions. Aims. This paper studies the cold condensations in the intermediate-/high-mass proto-cluster IRAS 05345+ 3157, focusing on the interaction with the other objects in the cluster. Methods. We performed millimeter high-angular resolution observations, both in the continuum and several molecular lines, with the PdBI and the SMA. In a recent paper, we published part of these data. The main finding of that work was the detection of two cold and dense gaseous condensations, called N and S (masses similar to 2 and similar to 9M(circle dot)), characterised by high values of deuterium fractionation (similar to 0.1 in both cores) obtained from the column density ratio N(N2D+)/N(N2H+). In this paper, we present a full report of the observations, and a complete analysis of the data obtained. Results. The millimeter maps reveal the presence of 3 cores inside the interferometer primary beam, called C1-a, C1-b and C2. None of them are associated with cores N and S. C1-b is very likely associated with a newly formed early-B ZAMS star embedded inside a hot core, while C1-a is more likely associated with a class 0 intermediate-mass protostar. The nature of C2 is unclear. Both C1-a and C1-b are good candidates as driving sources of a powerful (CO)-C-12 outflow, which strongly interacts with N, as demonstrated by the velocity gradient of the gas along this condensation. The N2H+ linewidths are between similar to 1 and 2 kms(-1) in the region where the continuum cores are located, and smaller (similar to 0.5 - 1.5 km s(-1)) towards N and S, indicating that the gas in the deuterated condensations is more quiescent than that associated with the continuum sources. This is consistent with the fact that they are still in the pre-stellar phase and hence the star formation process has not yet taken place there. Conclusions. The study of the gas kinematics across the source indicates a tight interaction between deuterated condensations and the sources embedded in millimeter cores. For the nature of N and S, we propose two scenarios: they can be low-mass pre-stellar condensations or "seeds" of future high-mass star(s). However, from these data it is not possible to establish how the turbulence triggered by the neghbouring cluster of protostars can influence the evolution of the condensations. C1 [Fontani, F.] ISDC, CH-1290 Versoix, Switzerland. [Fontani, F.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Zhang, Q.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Fontani, F (reprint author), ISDC, Ch Ecogia 16, CH-1290 Versoix, Switzerland. EM Francesco.Fontani@unige.ch OI Fontani, Francesco/0000-0003-0348-3418; Zhang, Qizhou/0000-0003-2384-6589 FU Swiss National Science Foundation [PP002-110504]; US National Science Foundation [0708158] FX Many thanks to the anonymous referee for his/her useful comments and suggestions. It is a pleasure to thank the staff of the Smithsonian Astrophysical Observatory for the SMA observations. We also thank the IRAM staff and Riccardo Cesaroni for their help in the calibration of the PdBI data. F. F. is deeply grateful to Marc Audard, Carla Baldovin and Andres Carmona for useful discussion, and to Keping Qiu for fitting the CH3CN spectrum. P. C. thanks Jonathan Tan for useful discussions on protocluster dynamics. F. F. acknowledges support by Swiss National Science Foundation grant (PP002-110504). T. B. acknowledges support from US National Science Foundation grant (0708158). NR 65 TC 20 Z9 20 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 2009 VL 499 IS 1 BP 233 EP 247 DI 10.1051/0004-6361/200911617 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 448UD UT WOS:000266286600021 ER PT J AU Govoni, F Murgia, M Markevitch, M Feretti, L Giovannini, G Taylor, GB Carretti, E AF Govoni, F. Murgia, M. Markevitch, M. Feretti, L. Giovannini, G. Taylor, G. B. Carretti, E. TI A search for diffuse radio emission in the relaxed, cool-core galaxy clusters A1068, A1413, A1650, A1835, A2029, and Ophiuchus SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; NORTHERN SKY SURVEY; X-RAY-EMISSION; ABELL CLUSTERS; CHANDRA OBSERVATIONS; NONTHERMAL EMISSION; RELIC CANDIDATES; FLOW CLUSTERS; COLD FRONTS AB Aims. We analyze sensitive, high-dynamic-range, observations to search for extended, diffuse, radio emission in relaxed and cool-core galaxy clusters. Methods. We performed deep 1.4 GHz Very Large Array observations, of A1068, A1413, A1650, A1835, A2029, and complemented our dataset with archival observations of Ophiuchus. Results. We find that, in the central regions of A1835, A2029, and Ophiuchus, the dominant radio galaxy is surrounded by diffuse low-brightness radio emission that takes the form of a mini-halo. We detect no diffuse emission in A1650, at a surface brightness level of the other mini-halos. We find low significance indications of diffuse emission in A1068 and A1413, although to be classified as mini-halos they would require further investigation, possibly with data of higher signal-to-noise ratio. In the Appendix, we report on the serendipitous detection of a giant radio galaxy with a total spatial extension of similar to 1.6 Mpc. C1 [Govoni, F.; Murgia, M.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [Murgia, M.; Feretti, L.; Giovannini, G.; Carretti, E.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Taylor, G. B.] Univ New Mexico, Albuquerque, NM 87131 USA. RP Govoni, F (reprint author), INAF Osservatorio Astron Cagliari, Str 54, I-09012 Capoterra, CA, Italy. EM fgovoni@ca.astro.it OI Govoni, Federica/0000-0003-3644-3084; Feretti, Luigina/0000-0003-0312-6285; Murgia, Matteo/0000-0002-4800-0806; Giovannini, Gabriele/0000-0003-4916-6362 NR 64 TC 44 Z9 44 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 MAY PY 2009 VL 499 IS 2 BP 371 EP 383 DI 10.1051/0004-6361/200811180 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BJ UT WOS:000266730500004 ER PT J AU Brunthaler, A Menten, KM Reid, MJ Henkel, C Bower, GC Falcke, H AF Brunthaler, A. Menten, K. M. Reid, M. J. Henkel, C. Bower, G. C. Falcke, H. TI Discovery of a bright radio transient in M82: a new radio supernova? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: supernovae: general; radio continuum: general; galaxies: individual: M82 ID FLUX-DENSITY VARIATIONS; SN 1993J VLBI; X-RAY SOURCES; GEOMETRIC DISTANCE; STARBURST GALAXIES; TIDAL DISRUPTION; PROPER MOTION; SN-1993J VLBI; BLACK-HOLE; REMNANTS AB In this Letter, we report the discovery of a new bright radio transient in M82. Using the Very Large Array, we observed the nuclear region of M82 at several epochs at 22 GHz and detected a new bright radio source in this galaxy's central region. We find a flux density for this flaring source that is similar to 300 times larger than the upper limits determined in previous observations. The flare must have started between 2007 October 29 and 2008 March 24. Over the past year, the flux density of this new source has decreased from similar to 100 mJy to similar to 11 mJy. The lightcurve (based on only three data points) can be fitted better with an exponential decay than with a power law. Based on the current data we cannot identify the nature of this transient source. However, a new radio supernova seems to be the most natural explanation. With its flux density of more than 100 mJy, it is at least 1.5 times brighter than SN1993J in M81 at the peak of its lightcurve at 22 GHz. C1 [Brunthaler, A.; Menten, K. M.; Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bower, G. C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bower, G. C.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Falcke, H.] Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM brunthal@mpifr-bonn.mpg.de RI Falcke, Heino/H-5262-2012 OI Falcke, Heino/0000-0002-2526-6724 NR 37 TC 25 Z9 25 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 MAY PY 2009 VL 499 IS 2 BP L17 EP L20 DI 10.1051/0004-6361/200912327 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 455BJ UT WOS:000266730500002 ER PT J AU Mieske, S Hilker, M Misgeld, I Jordan, A Infante, L Kissler-Patig, M AF Mieske, S. Hilker, M. Misgeld, I. Jordan, A. Infante, L. Kissler-Patig, M. TI A search for massive ultra-compact dwarf galaxies in the Centaurus galaxy cluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: individual: Centaurus; galaxies: dwarf; galaxies: fundamental parameters; galaxies: nuclei; galaxies: star clusters ID VIRGO-CLUSTER; GLOBULAR-CLUSTERS; FORNAX CLUSTER; LUMINOSITY FUNCTION; STELLAR-SYSTEMS; STAR-CLUSTERS; SPECTROSCOPY; DISTANCE; SAMPLE; HYDRA AB Context. In a previous paper, we initiated a search for ultra-compact dwarf galaxies (UCDs) in the Centaurus galaxy cluster, resulting in the discovery of 27 compact objects with -12.2 < M(V) < -10.9 mag. Our overall survey completeness was 15-20% within 120 kpc projected clustercentric distance. Aims. To constrain the luminosity distribution of the brightest UCDs in Centaurus in a more accurate way, we continue our search by improving substantially our survey completeness specifically for brightnesses of M(V) < -12 mag (V(0) < 21.3 mag). Methods. Using VIMOS at the VLT, we obtained low resolution spectra of 400 compact objects with 19.3 < V(0) < 21.3 mag (-14 < M(V) < -12 mag at the Centaurus distance) in the central 25' of the Centaurus cluster, which corresponds to a projected radius of similar to 150 kpc. Our survey had complete area coverage within a radius of similar to 120 kpc. Results. For 94% of the sources included in the masks, we measure successfully a redshift. Because of incompleteness in the slit assignment, our final completeness in the area surveyed is 52%. Among our targets, we find three new UCDs in the magnitude range -12.2 < M(V) < -12 mag, hence at the faint limit of our survey. For one of these targets HST WFPC2 imaging is available, yielding a size estimate of r(n) less than or similar to 8-9 pc. At 95% confidence, we can reject the hypothesis that in the area surveyed there are more than 2 massive UCDs with M(V) < -12.2 mag and r(eff) less than or similar to 70 pc. Hence our survey confirms the extreme rarity of massive UCDs. We find that the radial distributions of Centaurus and Fornax UCDs with respect to their host clusters' centres agree within the 2 sigma level. C1 [Mieske, S.] European So Observ, Santiago, Chile. [Hilker, M.; Misgeld, I.; Kissler-Patig, M.] European So Observ, D-85748 Garching, Germany. [Misgeld, I.] Argelander Inst Astron, D-53121 Bonn, Germany. [Jordan, A.; Infante, L.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Jordan, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mieske, S (reprint author), European So Observ, Alonso de Cordova 3107, Santiago, Chile. EM smieske@eso.org OI Jordan, Andres/0000-0002-5389-3944 NR 39 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 MAY PY 2009 VL 498 IS 3 BP 705 EP 710 DI 10.1051/0004-6361/200811248 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 446KZ UT WOS:000266121800005 ER PT J AU Smolcic, V Zamorani, G Schinnerer, E Bardelli, S Bondi, M Birzan, L Carilli, CL Ciliegi, P Elvis, M Impey, CD Koekemoer, AM Merloni, A Paglione, T Salvato, M Scodeggio, M Scoville, N Trump, JR AF Smolcic, V. Zamorani, G. Schinnerer, E. Bardelli, S. Bondi, M. Birzan, L. Carilli, C. L. Ciliegi, P. Elvis, M. Impey, C. D. Koekemoer, A. M. Merloni, A. Paglione, T. Salvato, M. Scodeggio, M. Scoville, N. Trump, J. R. TI COSMIC EVOLUTION OF RADIO SELECTED ACTIVE GALACTIC NUCLEI IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; galaxies: active; galaxies: evolution; galaxies: fundamental parameters; radio continuum: galaxies ID SUPERMASSIVE BLACK-HOLES; STAR-FORMING GALAXIES; DIGITAL-SKY-SURVEY; X-RAY CAVITIES; LUMINOSITY FUNCTION; HIGH-REDSHIFT; COSMOLOGICAL EVOLUTION; COOLING FLOWS; MOLECULAR GAS; LOUD AGN AB We explore the cosmic evolution of radio luminous active galactic nuclei (AGNs) with low radio powers (L(1.4) (GHz) less than or similar to 5 x 10(25) W Hz(-1)) out to z = 1.3 using to date the largest sample of similar to 600 low-luminosity radio AGN at intermediate redshift drawn from the VLA-COSMOS survey. We derive the radio-luminosity function for these AGNs, and its evolution with cosmic time assuming two extreme cases: (1) pure luminosity and (2) pure density evolution. The former and latter yield L* alpha (1+ z)(0.8 +/- 0.1), and Phi* alpha (1+ z)(1.1 +/- 0.1), respectively, both implying a fairly modest change in properties of low-radio-power AGNs since z = 1.3. We show that this is in stark contrast with the evolution of powerful (L(1.4) (GHz) > 5 x 10(25) W Hz(-1)) radio AGN over the same cosmic time interval, constrained using the 3CRR, 6CE, and 7CRS radio surveys by Willot et al. We demonstrate that this can be explained through differences in black hole fueling and triggering mechanisms, and a dichotomy in host galaxy properties of weak and powerful AGNs. Our findings suggest that high- and low-radio-power AGN activities are triggered in different stages during the formation of massive red galaxies. We show that weak radio AGN occur in the most massive galaxies already at z similar to 1, and they may significantly contribute to the heating of their surrounding medium and thus inhibit gas accretion onto their host galaxies, as recently suggested for the "radio mode" in cosmological models. C1 [Smolcic, V.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Zamorani, G.; Bardelli, S.; Ciliegi, P.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bondi, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Birzan, L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Birzan, L.] Ohio Univ, Dept Phys & Astron, Clippinger Labs, Athens, OH 45701 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Impey, C. D.; Trump, J. R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Merloni, A.] Tech Univ Munich, D-85748 Garching, Germany. [Merloni, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Paglione, T.] CUNY York Coll, Jamaica, NY 11451 USA. [Paglione, T.] Amer Museum Nat Hist, New York, NY 10024 USA. [Scodeggio, M.] IASF Milano INAF, Milan, Italy. RP Smolcic, V (reprint author), CALTECH, MC 105-24,1200 E Calif Blvd, Pasadena, CA 91125 USA. RI Bardelli, Sandro/O-9369-2015; OI Bardelli, Sandro/0000-0002-8900-0298; Ciliegi, Paolo/0000-0002-0447-4620; Scodeggio, Marco/0000-0002-2282-5850; Paglione, Tim/0000-0001-9139-0945; Koekemoer, Anton/0000-0002-6610-2048; Zamorani, Giovanni/0000-0002-2318-301X; Schinnerer, Eva/0000-0002-3933-7677 FU Max-Planck Society; Alexander von Humboldt Foundation through Max-Planck-Forschungspreis; INAF [PRIN-2006/1.06.10.08]; ASI [ASI/COFISI/026/07/0]; PSC-CUNY [69612-00 38] FX The authors are grateful to P. N. Best for especially deriving the SDSS/NVSS radio source fractions as a function of stellar mass with a radio luminosity cut that matches the VLA-COSMOS survey data. C. C. acknowledges support from the Max-Planck Society and the Alexander von Humboldt Foundation through the Max-Planck-Forschungspreis 2005. G.Z. and S.B. acknowledge support from an INAF contract PRIN-2006/1.06.10.08 and an ASI grant ASI/COFISI/026/07/0. TP acknowledges support from PSC-CUNY grant no. 69612-00 38. NR 114 TC 73 Z9 73 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 24 EP 39 DI 10.1088/0004-637X/696/1/24 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100003 ER PT J AU Qiu, KP Zhang, QZ Wu, JW Chen, HR AF Qiu, Keping Zhang, Qizhou Wu, Jingwen Chen, Huei-Ru TI SUBMILLIMETER ARRAY OBSERVATIONS OF THE MOLECULAR OUTFLOW IN HIGH-MASS STAR-FORMING REGION G240.31+0.07 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (G240.31+0.07); ISM: jets and outflows; stars: formation; stars: early-type ID YOUNG STARS; BIPOLAR OUTFLOWS; EMISSION; PROTOSTARS; DRIVEN; CORES; MODEL; GHZ AB We present Submillimeter Array observations toward the 10(4.7)L(circle dot) star-forming region G240.31+0.07, in the J = 2-1 transition of (12)CO and (13)CO and at 1.3 mm continuum, as well as the (12)CO and (13)CO observations from the Caltech Submillimeter Observatory to recover the extended emission filtered out by the interferometer. Maps of the (12)CO and (13)CO emission show a bipolar, wide-angle, quasi-parabolic molecular outflow, roughly coincident with an infrared nebula revealed by the Spitzer 3.6 and 4.5 mu m emission. The outflow has similar to 98 M(circle dot) molecular gas, making it one of the most massive molecular outflows known, and resulting in a very high mass-loss rate of 4.1 x 10(-3) M(circle dot) yr(-1) over a dynamical timescale of 2.4 x 10(4) yr. The 1.3 mm continuum observations with a 4 '' x 3 '' beam reveal a flattened dusty envelope of similar to 150 M(circle dot), which is further resolved with a 1.'' 2 x 1 '' beam into three dense cores with a total mass of similar to 40 M(circle dot). The central mm core, showing evidence of active star formation, approximately coincides with the geometric center of the bipolar outflow thus most likely harbors the powering source of the outflow. Overall, our observations provide the best case to date of a well defined wide-angle molecular outflow in a higher than 10(4) L(circle dot) star-forming region. The outflow is morphologically and kinematically similar to low-mass protostellar outflows but has two to three orders of magnitude greater mass, momentum, and energy, and is apparently driven by an underlying wide-angle wind, hence further supports that high-mass stars up to late-O types, even in a crowded clustering environment, can form as a scaled-up version of low-mass star formation. C1 [Qiu, Keping] Nanjing Univ, Dept Astron, Nanjing 210008, Peoples R China. [Qiu, Keping; Zhang, Qizhou; Wu, Jingwen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, Huei-Ru] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Chen, Huei-Ru] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. [Chen, Huei-Ru] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. RP Qiu, KP (reprint author), Nanjing Univ, Dept Astron, Nanjing 210008, Peoples R China. OI Zhang, Qizhou/0000-0003-2384-6589 NR 41 TC 39 Z9 39 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 66 EP 74 DI 10.1088/0004-637X/696/1/66 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100006 ER PT J AU Fuentes, CI George, MR Holman, MJ AF Fuentes, Cesar I. George, Matthew R. Holman, Matthew J. TI A SUBARU PENCIL-BEAM SEARCH FOR m(R) similar to 27 TRANS-NEPTUNIAN BODIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE solar system: formation ID KUIPER-BELT OBJECTS; SIZE DISTRIBUTION; DISCOVERY AB We present the results of an archival search for trans-Neptunian objects (TNOs) in an ecliptic field observed with Subaru in 2002. The depth of the search allowed us to find 20 new TNOs with magnitudes between R = 24 and 27. We fit a double power-law model to the data; the most likely values for the bright and faint power-law exponents are alpha(1) = 0.73(-0.09)(+0.08) and alpha(2) = 0.20(-0.14)(+0.12); the differential number density at R = 23 is sigma(23) = 1.46(-0.12)(+0.14) and the break magnitude is R-eq = 25.0(-0.6)(+0.8). This is the most precise measurement of the break in the TNO luminosity function to date. The break in the size distribution corresponds to a diameter of D = 90 +/- 30 km assuming a 4% albedo. C1 [Fuentes, Cesar I.; George, Matthew R.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fuentes, CI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cfuentes@cfa.harvard.edu RI Fuentes, Cesar /G-7506-2016 NR 27 TC 47 Z9 47 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 MAY 1 PY 2009 VL 696 IS 1 BP 91 EP 95 DI 10.1088/0004-637X/696/1/91 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100009 ER PT J AU Risaliti, G Miniutti, G Elvis, M Fabbiano, G Salvati, M Baldi, A Braito, V Bianchi, S Matt, G Reeves, J Soria, R Zezas, A AF Risaliti, G. Miniutti, G. Elvis, M. Fabbiano, G. Salvati, M. Baldi, A. Braito, V. Bianchi, S. Matt, G. Reeves, J. Soria, R. Zezas, A. TI VARIABLE PARTIAL COVERING AND A RELATIVISTIC IRON LINE IN NGC 1365 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1365); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; PHOTON IMAGING CAMERA; X-RAY-SPECTRUM; XMM-NEWTON; SEYFERT-GALAXIES; COMPTON-THIN; VARIABILITY; REFLECTION; LUMINOSITY AB We present a complete analysis of the hard X-ray (2-10 keV) properties of the Seyfert galaxy NGC 1365, based on a 60 ks XMM-Newton observation performed in 2004 January. The two main results are as follows. (1) We detect an obscuring cloud with N(H) similar to 3.5 x 10(23) cm(-2) crossing the line of sight in similar to 25 ks. This implies a dimension of the X-ray source not larger than a few 1013 cm and a distance of the obscuring cloud of the order of 1016 cm. Adopting the black hole mass M(BH) estimated from the M(BH)-velocity dispersion relation, the source size is D(S) < 20R(G) and the distance and density of the obscuring clouds are R similar to 3000-10,000R(G) and n similar to 10(10) cm(-3), i.e., typical values for broad-line region clouds. (2) An iron emission line with a relativistic profile is detected with high statistical significance. A time-integrated fit of the line+continuum reflection components suggests a high iron abundance (approximately three times solar) and an origin of these components in the inner part (within similar to 10R(G)) of the accretion disk, in agreement with the small source size inferred from the analysis of the absorption variability. C1 [Risaliti, G.; Elvis, M.; Fabbiano, G.; Baldi, A.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.; Salvati, M.] INAF Osservatorio Arcetri, I-50125 Florence, Italy. [Miniutti, G.] Lab Astroparticule & Cosmol APC, UMR 7164, F-75205 Paris, France. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bianchi, S.; Matt, G.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Reeves, J.] Univ Keele, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Soria, R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM grisaliti@cfa.harvard.edu RI Bianchi, Stefano/B-4804-2010; Miniutti, Giovanni/L-2721-2014; Zezas, Andreas/C-7543-2011; OI Bianchi, Stefano/0000-0002-4622-4240; Miniutti, Giovanni/0000-0003-0707-4531; Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X; Braito, Valentina/0000-0002-2629-4989 FU NASA [G06-7102X, NNX07AR90G] FX We are grateful to the referee for helpful comments which significantly improved the clarity of the paper. This work was partially supported by NASA grants G06-7102X and NNX07AR90G. NR 42 TC 79 Z9 79 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 160 EP 171 DI 10.1088/0004-637X/696/1/160 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100015 ER PT J AU Neilsen, J Lee, JC Nowak, MA Dennerl, K Vrtilek, SD AF Neilsen, Joseph Lee, Julia C. Nowak, Michael A. Dennerl, Konrad Vrtilek, Saeqa Dil TI SPECTROSCOPIC SIGNATURES OF THE SUPERORBITAL PERIOD IN THE NEUTRON STAR BINARY LMC X-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; pulsars: individual (LMC X-4); stars: neutron; X-rays: binaries ID HUBBLE-SPACE-TELESCOPE; ION LINE-INTENSITIES; X-RAY SPECTROSCOPY; HELIUM-LIKE IONS; SMC X-1; PHOTOIONIZED PLASMA; ACCRETION DISK; PULSE PROFILE; STELLAR WIND; LIGHT-CURVE AB We present the first high-resolution X-ray study of emission line variability with superorbital phase in the neutron star binary LMC X-4. Our analysis provides new evidence from X-ray spectroscopy confirming accretion disk precession as the origin of the superorbital period. The spectra, obtained with the Chandra High-Energy Transmission Grating Spectrometer and the XMM-Newton Reflection Grating Spectrometer, contain a number of emission features, including lines from hydrogen-like and helium-like species of N, O, Ne, and Fe, a narrow O VII radiative recombination continua (RRCs), and fluorescent emission from cold Fe. We use the narrow RRC and the He alpha triplets to constrain the temperature and density of the (photoionized) gas. By comparing spectra from different superorbital phases, we attempt to isolate the contributions to line emission from the accretion disk and the stellar wind. There is also evidence for highly ionized iron redshifted and blueshifted by similar to 25,000 km s(-1). We argue that this emission originates in the inner accretion disk and show that the emission line properties in LMC X-4 are natural consequences of accretion disk precession. C1 [Neilsen, Joseph; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Neilsen, Joseph; Lee, Julia C.; Vrtilek, Saeqa Dil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nowak, Michael A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Dennerl, Konrad] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Neilsen, J (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM jneilsen@cfa.harvard.edu RI Lee, Julia/G-2381-2015; OI Lee, Julia/0000-0002-7336-3588; Neilsen, Joseph/0000-0002-8247-786X FU Chandra [GO7-8044X]; Harvard University Graduate School of Arts and Sciences FX We gratefully acknowledge funding support from the Chandra grant GO7-8044X and the Harvard University Graduate School of Arts and Sciences. We thank the referee for useful comments and Jack Steiner for many helpful discussions. 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. NR 44 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 182 EP 191 DI 10.1088/0004-637X/696/1/182 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100018 ER PT J AU Sato, T Martin, CL Noeske, KG Koo, DC Lotz, JM AF Sato, Taro Martin, Crystal L. Noeske, Kai G. Koo, David C. Lotz, Jennifer M. TI AEGIS: THE NATURE OF THE HOST GALAXIES OF LOW-IONIZATION OUTFLOWS AT z < 0.6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: stellar content; ISM: jets and outflows ID DIGITAL SKY SURVEY; STAR-FORMATION HISTORY; LUMINOUS INFRARED GALAXIES; STELLAR POPULATION SYNTHESIS; DUSTY STARBURST GALAXIES; SCALE GASEOUS OUTFLOWS; MASS ASSEMBLY HISTORY; EXTENDED GROTH STRIP; II ESI SPECTRA; REDSHIFT SURVEY AB We report on a signal-to-noise (S/N) limited search for low-ionization gas outflows in the spectra of the 0.11 < z < 0.54 objects in the Extended Groth Strip portion of the DEEP2 survey. Doppler shifts from the host galaxy redshifts are systematically searched for in the Na I lambda 5890, 96 doublet (Na I D). Although the spectral resolution and S/N limit us to study the interstellar gas kinematics from fitting a single doublet component to each observed Na I D profile, the typical outflow often seen in local luminous-infrared galaxies (LIRGs) should be detected at greater than or similar to 6 sigma in absorption equivalent width down to the survey limiting S/N (similar to 5 pixel(-1)) in the continuum around Na I D. The detection rate of LIRG-like outflow clearly shows an increasing trend with star-forming activity and infrared luminosity. However, by virtue of not selecting our sample on star formation, we also find a majority of outflows in galaxies on the red sequence in the rest-frame (U-B, MB) color-magnitude diagram. Most of these red-sequence galaxies hosting outflows are of early-type morphology and show the sign of recent star formation in their UV-optical colors; some show enhanced Balmer H beta absorption lines indicative of poststarburst as well as high dust extinction. These findings demonstrate that outflows outlive starbursts and suggest that galactic-scale outflows play a role in quenching star formation in the host galaxies on their way to the red sequence. The fate of relic winds, as well as the observational constraints on gaseous feedback models, may be studied in galaxies during their poststarburst phase. We also note the presence of inflow candidates in red, early-type galaxies, some with signs of active galactic nuclei/LINERs but little evidence for star formation. C1 [Sato, Taro; Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Noeske, Kai G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koo, David C.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. RP Sato, T (reprint author), Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. EM nomo17k@gmail.com OI Koo, David/0000-0003-3385-6799 FU David and Lucille Packard Foundation; NSF [AST-0071048, AST-0071198]; W. M. Keck Foundation; NASA; Korean Ministry of Science and Technology FX Last but not least, we recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 99 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 214 EP 232 DI 10.1088/0004-637X/696/1/214 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100020 ER PT J AU Carter, JA Winn, JN Gilliland, R Holman, MJ AF Carter, Joshua A. Winn, Joshua N. Gilliland, Ronald Holman, Matthew J. TI NEAR-INFRARED TRANSIT PHOTOMETRY OF THE EXOPLANET HD 149026b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HD 149026); techniques: photometric; stars: fundamental parameters ID GIANT PLANET TRANSITS; LIGHT-CURVE PROJECT; EXTRASOLAR PLANETS; TRANSMISSION SPECTRA; SURFACE GRAVITIES; Y-2 ISOCHRONES; STELLAR; ATMOSPHERE; PARAMETERS; EVOLUTION AB The transiting exoplanet HD 149026b is an important case for theories of planet formation and planetary structure, for the planet's relatively small size has been interpreted as evidence for a highly metal-enriched composition. We present observations of four transits with the Near-Infrared Camera and Multi-Object Spectrometer (NICMOS) on the Hubble Space Telescope within a wavelength range of 1.1-2.0 mu m. Analysis of the light curve gives the most precise estimate yet of the stellar mean density, rho(star) = 0.497(-0.057)(+0.042) g cm(-3). By requiring agreement between the observed stellar properties (including rho(star)) and stellar evolutionary models, we refine the estimate of the stellar radius: R(star) = 1.541(-0.042)(+0.046) R(circle dot). We also find a deeper transit than has been measured at optical and mid-infrared wavelengths. Taken together, these findings imply a planetary radius of R(p) = 0.813(-0.025)(+0.027) R(Jup), which is larger than earlier estimates. Models of the planetary interior still require a metal-enriched composition, although the required degree of metal enrichment is reduced. It is also possible that the deeper NICMOS transit is caused by wavelength-dependent absorption by constituents in the planet's atmosphere, although simple model atmospheres do not predict this effect to be strong enough to account for the discrepancy. We use the four newly measured transit times to compute a refined transit ephemeris. C1 [Carter, Joshua A.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Carter, Joshua A.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. RP Carter, JA (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM carterja@mit.edu RI Carter, Joshua/A-8280-2013; OI Carter, Joshua/0000-0001-8152-2561 FU NASA [HST-GO-11165, NAS5-26555] FX We thank G. Torres for helpful discussions concerning the determination of stellar parameters. This work was supported by NASA grant HST-GO-11165 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 47 TC 42 Z9 42 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 241 EP 253 DI 10.1088/0004-637X/696/1/241 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100022 ER PT J AU Zhang, QZ Wang, Y Pillai, T Rathborne, J AF Zhang, Qizhou Wang, Yang Pillai, Thushara Rathborne, Jill TI FRAGMENTATION AT THE EARLIEST PHASE OF MASSIVE STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: clouds; ISM: kinematics and dynamics; stars: formation ID INFRARED-DARK CLOUDS; ULTRACOMPACT HII REGION; SUBMILLIMETER ARRAY; MOLECULAR CLOUDS; PROTOSTELLAR CORES; INITIAL CONDITIONS; ACCRETION; CLUSTERS; DISK; EXTINCTION AB We present 1.3 mm continuum and spectral line images of two massive molecular clumps P1 and P2 in the G28.34+0.06 region with the Submillimeter Array (SMA). While the two clumps contain masses of 1000 and 880 M(circle dot), respectively, P1 has a luminosity OF < 10(2) L(circle dot), and a lower gas temperature and smaller line width than P2. Thus, P1 appears to be at a much earlier stage of massive star formation than P2. The high-resolution SMA observations reveal two distinctive cores in P2 with masses of 97 and 49 M(circle dot), respectively. The 4 GHz spectral bandpass captures line emission from CO isotopologues, SO, CH(3)OH, and CH(3)CN, similar to hot molecular cores harboring massive young stars. The P1 clump, on the other hand, is resolved into five cores along the filament with masses from 22 to 64 M(circle dot) and an average projected separation of 0.19 pc. Except (12)CO, no molecular line emission is detected toward the P1 cores at a 1 sigma rms of 0.1 K. Since strong (12)CO and C(18)O emissions are seen with the single-dish telescope at a resolution of 11 '', the nondetection of these lines with the SMA indicates a depletion factor up to 10(3). While the spatial resolution of the SMA is better than the expected Jeans length, the masses in P1 cores are much larger than the thermal Jeans mass, indicating the importance of turbulence and/or magnetic fields in cloud fragmentation. The hierarchical structures in the P1 region provide a glimpse of the initial phase of massive star and cluster formation. C1 [Zhang, Qizhou; Wang, Yang; Pillai, Thushara; Rathborne, Jill] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM qzhang@cfa.harvard.edu OI Zhang, Qizhou/0000-0003-2384-6589 NR 42 TC 84 Z9 84 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 268 EP 273 DI 10.1088/0004-637X/696/1/268 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100025 ER PT J AU Foster, JB Rosolowsky, EW Kauffmann, J Pineda, JE Borkin, MA Caselli, P Myers, PC Goodman, AA AF Foster, Jonathan B. Rosolowsky, Erik W. Kauffmann, Jens Pineda, Jaime E. Borkin, Michelle A. Caselli, Paola Myers, Phil C. Goodman, Alyssa A. TI DENSE CORES IN PERSEUS: THE INFLUENCE OF STELLAR CONTENT AND CLUSTER ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: molecules; radio lines: ISM ID INITIAL MASS FUNCTION; SPITZER C2D SURVEY; STAR-FORMATION; DARK CLOUDS; INTERSTELLAR AMMONIA; MOLECULAR CLOUDS; PIPE NEBULA; PROTOSTELLAR CORES; DUST OPACITIES; EVOLUTION AB We present the chemistry, temperature, and dynamical state of a sample of 193 dense cores or core candidates in the Perseus Molecular cloud and compare the properties of cores associated with young stars and clusters with those which are not. The combination of our NH(3) and CCS observations with previous millimeter, submillimeter, and Spitzer data available for this cloud enables us both to determine core properties precisely and to accurately classify cores as starless or protostellar. The properties of cores in different cluster environments and before-and-after star formation provide important constraints on simulations of star formation, particularly under the paradigm that the essence of star formation is set by the turbulent formation of prestellar cores. We separate the influence of stellar content from that of the cluster environment and find that cores within clusters have ( 1) higher kinetic temperatures (12.9 K versus 10.8 K) and, (2) lower fractional abundances of CCS (0.6 x 10(-9) versus 2.0 x 10(-9)) and NH(3) (1.2 x 10(-8) versus 2.9 x 10(-8)). Cores associated with protostars have (1) slightly higher kinetic temperatures (11.9 K versus 10.6 K), (2) higher NH(3) excitation temperatures (7.4 K versus 6.1 K), (3) are at higher column density (1.2 x 10(22) cm(-2) versus 0.6 x 10(22) cm(-2)), have (4) slightly more nonthermal/turbulent NH(3) line widths (0.14 km s(-1) versus 0.11 km s(-1) FWHM), have (5) higher masses (1.5 M(circle dot) versus 1.0 M(circle dot)), and have (6) lower fractional abundance of CCS (1.4 x 10(-9) versus 2.4 x 10(-9)). All values are medians. We find that neither cluster environment nor protostellar content makes a significant difference to the dynamical state of cores as estimated by the virial parameter-most cores in each category are gravitationally bound. Only the high precision of our measurements and the size of our sample make such distinctions possible. Overall, cluster environment and protostellar content have a smaller influence on the properties of the cores than is typically assumed, and the variation within categories is larger than the differences between categories. C1 [Foster, Jonathan B.; Kauffmann, Jens; Pineda, Jaime E.; Myers, Phil C.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosolowsky, Erik W.] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada. [Kauffmann, Jens; Borkin, Michelle A.; Goodman, Alyssa A.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. RP Foster, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010 OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477 FU NRAO Student Observing Support Program [GSSP06-0015]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-0502605] FX The Green Bank Telescope is operated by 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. J.E.P. and J.B.F. are supported by a generous grant from the NRAO Student Observing Support Program (GSSP06-0015). The work of E. R. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST-0502605). We thank our anonymous referee who helped to improve this paper. NR 58 TC 41 Z9 41 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 298 EP 319 DI 10.1088/0004-637X/696/1/298 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100029 ER PT J AU Wuyts, S Franx, M Cox, TJ Hernquist, L Hopkins, PF Robertson, BE van Dokkum, PG AF Wuyts, Stijn Franx, Marijn Cox, Thomas J. Hernquist, Lars Hopkins, Philip F. Robertson, Brant E. van Dokkum, Pieter G. TI RECOVERING STELLAR POPULATION PROPERTIES AND REDSHIFTS FROM BROADBAND PHOTOMETRY OF SIMULATED GALAXIES: LESSONS FOR SED MODELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies: ISM; galaxies: stellar content ID LYMAN BREAK GALAXIES; STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; MASS-METALLICITY RELATION; DEEP FIELD-SOUTH; BLACK-HOLES; RED GALAXIES; STARBURST GALAXIES; SPITZER OBSERVATIONS AB We present a detailed analysis of our ability to determine stellar masses, ages, reddening, and extinction values, and star formation rates (SFRs) of high-redshift galaxies by modeling broadband spectral energy distributions (SEDs) with stellar population synthesis. In order to do so, we computed synthetic optical-to-NIR SEDs for model galaxies taken from hydrodynamical merger simulations placed at redshifts 1.5 <= z <= 2.9. Viewed under different angles and during different evolutionary phases, the simulations represent a wide variety of galaxy types (disks, mergers, spheroids). We show that simulated galaxies span a wide range in SEDs and color, comparable to those of observed galaxies. In all star-forming phases, dust attenuation has a large effect on colors, SEDs, and fluxes. The broadband SEDs were then fed to a standard SED modeling procedure, and resulting stellar population parameters were compared to their true values. Disk galaxies generally show a decent median correspondence between the true and estimated mass and age, but suffer from large uncertainties (Delta logM = -0.06(-0.13)(+0.06), Delta log age(w) = +0.03(-0.42)(+0.19)). During the merger itself, we find larger offsets: Delta logM = -0.13(-0.14)(+ 0.10), Delta log age(w) = -0.12(-0.26)(+0.40). E(B - V) values are generally recovered well, but the estimated total visual absorption A(V) is consistently too low, increasingly so for larger optical depths (Delta A(V) = -0.54(-0.46)(+0.40) in the merger regime). Since the largest optical depths occur during the phases of most intense star formation, it is for the highest SFRs that we find the largest underestimates (Delta log SFR = -0.44(-0.31)(+0.32) in the merger regime). The masses, ages, E(B - V), A(V), and SFRs of merger remnants (spheroids) are very well reproduced. We discuss possible biases in SED modeling results caused by mismatch between the true and template star formation history (SFH), dust distribution, metallicity variations, and active galactic nucleus contribution. Mismatch between the real and template SFH, as is the case during the merging event, drives the age, and consequently mass estimate, down with respect to the true age and mass. However, the larger optical depth toward young stars during this phase reduces the effect considerably. Finally, we tested the photometric redshift code EAZY on the simulated galaxies placed at high redshift. We find a small scatter in Delta z/(1+z) of 0.031. C1 [Wuyts, Stijn; Cox, Thomas J.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wuyts, Stijn; Franx, Marijn] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Robertson, Brant E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Robertson, Brant E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Robertson, Brant E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Wuyts, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM swuyts@cfa.harvard.edu FU W.M. Keck Foundation.; Spitzer Fellowship; Spitzer Science Center FX S.W. and T.J.C. acknowledge support from the W.M. Keck Foundation. B.E.R. gratefully acknowledges support from a Spitzer Fellowship through a NASA grant administrated by the Spitzer Science Center. We thank Natascha Forster Schreiber for useful discussions on stellar populations. NR 88 TC 50 Z9 50 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 348 EP 369 DI 10.1088/0004-637X/696/1/348 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100032 ER PT J AU Silverman, JD Lamareille, F Maier, C Lilly, SJ Mainieri, V Brusa, M Cappelluti, N Hasinger, G Zamorani, G Scodeggio, M Bolzonella, M Contini, T Carollo, CM Jahnke, K Kneib, JP Le Fevre, O Merloni, A Bardelli, S Bongiorno, A Brunner, H Caputi, K Civano, F Comastri, A Coppa, G Cucciati, O de la Torre, S de Ravel, L Elvis, M Finoguenov, A Fiore, F Franzetti, P Garilli, B Gilli, R Iovino, A Kampczyk, P Knobel, C Kovac, K Le Borgne, JF Le Brun, V Mignoli, M Pello, R Peng, Y Montero, EP Ricciardelli, E Tanaka, M Tasca, L Tresse, L Vergani, D Vignali, C Zucca, E Bottini, D Cappi, A Cassata, P Fumana, M Griffiths, R Kartaltepe, J Koekemoer, A Marinoni, C McCracken, HJ Memeo, P Meneux, B Oesch, P Porciani, C Salvato, M AF Silverman, J. D. Lamareille, F. Maier, C. Lilly, S. J. Mainieri, V. Brusa, M. Cappelluti, N. Hasinger, G. Zamorani, G. Scodeggio, M. Bolzonella, M. Contini, T. Carollo, C. M. Jahnke, K. Kneib, J. -P. Le Fevre, O. Merloni, A. Bardelli, S. Bongiorno, A. Brunner, H. Caputi, K. Civano, F. Comastri, A. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Elvis, M. Finoguenov, A. Fiore, F. Franzetti, P. Garilli, B. Gilli, R. Iovino, A. Kampczyk, P. Knobel, C. Kovac, K. Le Borgne, J. -F. Le Brun, V. Mignoli, M. Pello, R. Peng, Y. Montero, E. Perez Ricciardelli, E. Tanaka, M. Tasca, L. Tresse, L. Vergani, D. Vignali, C. Zucca, E. Bottini, D. Cappi, A. Cassata, P. Fumana, M. Griffiths, R. Kartaltepe, J. Koekemoer, A. Marinoni, C. McCracken, H. J. Memeo, P. Meneux, B. Oesch, P. Porciani, C. Salvato, M. TI ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: evolution; quasars: emission lines; quasars: general; X-rays: galaxies ID DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; SUPERMASSIVE BLACK-HOLES; HARD X-RAY; BH-SIGMA RELATION; VLT DEEP SURVEY; COSMOS FIELD; FORMING GALAXIES; LUMINOSITY FUNCTION; FORMATION HISTORY AB We present a study of the host galaxies of active galactic nucleus (AGN) selected from the zCOSMOS survey to establish if accretion onto supermassive black holes (SMBHs) and star formation are explicitly linked up to z similar to 1. We identify 152 galaxies that harbor AGN, based on their X-ray emission (L(0.5-10keV) > 10(42) erg s(-1)) detected by XMM-Newton observations of 7543 galaxies (i(acs) < 22.5). Star formation rates (SFRs), including those weighted by stellar mass, of a subsample are determined using the [O II]lambda 3727 emission-line luminosity, corrected for an AGN contribution based on the observed [O III]lambda 5007 strength or that inferred by their hard (2-10 keV) X-ray luminosity. We find that an overwhelming majority of AGN host galaxies have significant levels of star formation with a distribution spanning similar to 1-100 M(circle dot) yr(-1); their average SFR is higher than that of galaxies with equivalent stellar mass (M(*) > 4 x 10(10) M(circle dot)). The close association between AGN activity and star formation is further substantiated by an increase in the fraction of galaxies hosting AGN with the youthfulness of their stars as indicated by the rest-frame color (U-V) and spectral index D(n)(4000); we demonstrate that a mass-selected sample is required to alleviate an artificial peak in the AGN fraction falling in the transition region due to the fact that many "blue cloud" galaxies have low mass-to-light ratios in luminosity-limited samples. We also find that the SFRs of AGN hosts evolve with cosmic time in a manner that closely mirrors the overall galaxy population and naturally explains the low SFRs in AGNs (z < 0.3) from the SDSS. We conclude that the conditions most conducive for AGN activity are a massive host galaxy and a large reservoir of gas. Furthermore, a direct correlation between mass-accretion rate onto SMBHs and SFR is shown to be weak although the average ratio (similar to 10(-2)) is constant with redshift, effectively shifting the evidence for a co-evolution scenario in a statistical manner to smaller physical scales (i.e., within the same galaxies). The order-of-magnitude increase in this ratio compared to the locally measured value of M(BH)/M(bulge) is consistent with an AGN lifetime substantially shorter than that of star formation. Our findings illustrate an intermittent scenario with underlying complexities regarding fueling over vastly different physical (and temporal) scales yet to be firmly determined. C1 [Silverman, J. D.; Maier, C.; Lilly, S. J.; Carollo, C. M.; Caputi, K.; Kampczyk, P.; Knobel, C.; Kovac, K.; Peng, Y.; Oesch, P.; Porciani, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Lamareille, F.; Contini, T.; Le Borgne, J. -F.; Pello, R.; Montero, E. Perez] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Mainieri, V.; Tanaka, M.] European So Observ, D-85748 Garching, Germany. [Brusa, M.; Cappelluti, N.; Hasinger, G.; Merloni, A.; Bongiorno, A.; Brunner, H.; Finoguenov, A.; Meneux, B.] Max Planck Inst Extraterr Phys, D-84571 Garching, Germany. [Zamorani, G.; Bolzonella, M.; Bardelli, S.; Comastri, A.; Coppa, G.; Gilli, R.; Mignoli, M.; Vergani, D.; Zucca, E.; Cappi, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Scodeggio, M.; Franzetti, P.; Garilli, B.; Bottini, D.; Fumana, M.; Memeo, P.] INAF IASF Milano, Milan, Italy. [Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kneib, J. -P.; Le Fevre, O.; de la Torre, S.; de Ravel, L.; Le Brun, V.; Tasca, L.; Tresse, L.; Cassata, P.] Lab Astrophys Marseille, Marseille, France. [Merloni, A.] Excellence Cluster Univ, D-85748 Garching, Germany. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cucciati, O.; Iovino, A.] INAF Osservatorio Astron Brera, Milan, Italy. [Fiore, F.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Griffiths, R.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Kartaltepe, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Marinoni, C.] Ctr Phys Theor, Marseille, France. [McCracken, H. J.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Meneux, B.] Univ Sternwarte, D-81679 Munich, Germany. [Salvato, M.] CALTECH, Pasadena, CA 91125 USA. RP Silverman, JD (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. RI Pello, Roser/G-4754-2010; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Cappi, Alberto/O-9391-2015; Bolzonella, Micol/O-9495-2015; Zucca, Elena/O-9396-2015; Mignoli, Marco/O-9426-2015; Bardelli, Sandro/O-9369-2015; OI Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Cappi, Alberto/0000-0002-9200-7167; Bolzonella, Micol/0000-0003-3278-4607; Zucca, Elena/0000-0002-5845-8132; Mignoli, Marco/0000-0002-9087-2835; Scodeggio, Marco/0000-0002-2282-5850; Bardelli, Sandro/0000-0002-8900-0298; Fumana, Marco/0000-0001-6787-5950; Iovino, Angela/0000-0001-6958-0304; bottini, dario/0000-0001-6917-041X; Bongiorno, Angela/0000-0002-0101-6624; Franzetti, Paolo/0000-0002-6986-0127; Vergani, Daniela/0000-0003-0898-2216; Cappelluti, Nico/0000-0002-1697-186X; Jahnke, Knud/0000-0003-3804-2137; Oesch, Pascal/0000-0001-5851-6649; Maier, Christian/0000-0001-6405-2182; Koekemoer, Anton/0000-0002-6610-2048; Garilli, Bianca/0000-0001-7455-8750; Zamorani, Giovanni/0000-0002-2318-301X; Perez Montero, E/0000-0003-3985-4882; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157 NR 110 TC 149 Z9 149 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 396 EP 410 DI 10.1088/0004-637X/696/1/396 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100035 ER PT J AU Shetty, R Kauffmann, J Schnee, S Goodman, AA AF Shetty, Rahul Kauffmann, Jens Schnee, Scott Goodman, Alyssa A. TI THE EFFECT OF NOISE ON THE DUST TEMPERATURE-SPECTRAL INDEX CORRELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; infrared: ISM; methods: miscellaneous ID ENERGY-DISTRIBUTIONS; INTERSTELLAR DUST; INFRARED GALAXIES; SUBMILLIMETER; EMISSION; DEPENDENCE; COMPLEX AB We investigate how uncertainties in flux measurements affect the results from modified blackbody spectral energy distribution (SED) fits. We show that an inverse correlation between the dust temperature T and spectral index beta naturally arises from least-squares fits due to the uncertainties, even for sources with a single T and beta. Fitting SEDs to noisy fluxes solely in the Rayleigh-Jeans regime produces unreliable T and beta estimates. Thus, for long wavelength observations (lambda greater than or similar to 200 mu m), or for warm sources (T greater than or similar to 60 K), it becomes difficult to distinguish sources with different temperatures. We assess the role of noise in recent observational results that indicate an inverse and continuously varying T-beta relation. Though an inverse and continuous T-beta correlation may be a physical property of dust in the interstellar medium, we find that the observed inverse correlation may be primarily due to noise. C1 [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Schnee, Scott] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Shetty, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rshetty@cfa.harvard.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU OVRO; NSF [AST 05-40399]; Harvard Initiative in Innovative Computing FX We are grateful to Brandon Kelly, Xavier Dupac, and Jonathan Foster for comments on the draft and useful discussions. We thank the referee for comments that helped improve this paper. We also thank Peter Teuben for assistance using NEMO software (Teuben 1995) to carry out our analysis. S. S. acknowledges support from the OVRO, which is supported by the NSF through grant AST 05-40399. R. S., J. K., and A. A. G. acknowledge support from the Harvard Initiative in Innovative Computing, which hosts the Star-Formation Taste Tests Community at which further details on these results can be found and discussed ( see http://www.cfa.harvard.edu/similar to agoodman/tastetests). NR 16 TC 92 Z9 92 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 676 EP 680 DI 10.1088/0004-637X/696/1/676 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100055 ER PT J AU Stritzinger, M Mazzali, P Phillips, MM Immler, S Soderberg, A Sollerman, J Boldt, L Braithwaite, J Brown, P Burns, CR Contreras, C Covarrubias, R Folatelli, G Freedman, WL Gonzalez, S Hamuy, M Krzeminski, W Madore, BF Milne, P Morrell, N Persson, SE Roth, M Smith, M Suntzeff, NB AF Stritzinger, Maximilian Mazzali, Paolo Phillips, Mark M. Immler, Stefan Soderberg, Alicia Sollerman, Jesper Boldt, Luis Braithwaite, Jonathan Brown, Peter Burns, Christopher R. Contreras, Carlos Covarrubias, Ricardo Folatelli, Gaston Freedman, Wendy L. Gonzalez, Sergio Hamuy, Mario Krzeminski, Wojtek Madore, Barry F. Milne, Peter Morrell, Nidia Persson, S. E. Roth, Miguel Smith, Mathew Suntzeff, Nicholas B. TI THE HE-RICH CORE-COLLAPSE SUPERNOVA 2007Y: OBSERVATIONS FROM X-RAY TO RADIO WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1187); supernovae: general; supernovae: individual (SN 2007Y) ID 25 APRIL 1998; IB SUPERNOVA; LIGHT CURVES; CIRCUMSTELLAR INTERACTION; STANDARD STARS; NEUTRON-STAR; SN 1993J; PHOTOMETRIC CALIBRATION; OPTICAL SPECTROSCOPY; UBVRI PHOTOMETRY AB A detailed study spanning approximately a year has been conducted on the Type Ib supernova (SN) 2007Y. Imaging was obtained from X-ray to radio wavelengths, and a comprehensive set of multi-band (w2m2w1u'g'r'i'UBVYJHK(s)) light curves and optical spectroscopy is presented. A virtually complete bolometric light curve is derived, from which we infer a (56)Ni mass of 0.06 M(circle dot). The early spectrum strongly resembles SN 2005bf and exhibits high- velocity features of Ca II and H alpha; during late epochs the spectrum shows evidence of an ejecta-wind interaction. Nebular emission lines have similar widths and exhibit profiles that indicate a lack of major asymmetry in the ejecta. Late phase spectra are modeled with a non-LTE code, from which we find (56)Ni, O, and total-ejecta masses (excluding He) to be 0.06, 0.2, and 0.42 M(circle dot), respectively, below 4500 km s(-1). The (56)Ni mass confirms results obtained from the bolometric light curve. The oxygen abundance suggests that the progenitor was most likely a approximate to 3.3 M(circle dot) He core star that evolved from a zero-age-main-sequence mass of 10-13 M(circle dot). The explosion energy is determined to be approximate to 10(50) erg, and the mass-loss rate of the progenitor is constrained from X-ray and radio observations to be less than or similar to 10(-6) M(circle dot) yr(-1). SN 2007Y is among the least energetic normal Type Ib SNe ever studied. C1 [Stritzinger, Maximilian; Phillips, Mark M.; Boldt, Luis; Contreras, Carlos; Covarrubias, Ricardo; Gonzalez, Sergio; Krzeminski, Wojtek; Morrell, Nidia; Roth, Miguel] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian; Sollerman, Jesper] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Mazzali, Paolo] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, XrayAstrophys Lab, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Soderberg, Alicia] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Soderberg, Alicia] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sollerman, Jesper] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Braithwaite, Jonathan] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Brown, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Burns, Christopher R.; Freedman, Wendy L.; Madore, Barry F.; Persson, S. E.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Folatelli, Gaston; Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Madore, Barry F.] CALTECH, Jet Prop Lab, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Milne, Peter] Univ Arizona, Dept Astron & Steward Observ, Tucson, AZ 85721 USA. [Smith, Mathew] Univ Cape Town, Cosmol & Grav Grp, Dept Math & Appl Math, ZA-7700 Rondebosch, South Africa. [Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. RP Stritzinger, M (reprint author), Carnegie Observ, Las Campanas Observ, Casilla 601, La Serena, Chile. EM mstritzinger@lco.cl; mazzali@mpa-garching.mpg.de; mmp@lco.cl; stefan.m.immler@nasa.gov; alicia@astro.princeton.edu; jesper@dark-cosmology.dk; lboldt@lco.cl; jon@cita.utoronto.ca; pbrown@astro.psu.edu; cburns@ociw.edu; ccontreras@lco.cl; ricardo@lco.cl; gaston@das.uchile.cl; wendy@ociw.edu; sgonzalez@lco.cl; mhamuy@das.uchile.cl; wojtek@lco.cl; barry@ociw.edu; pmilne@as.asrizona.edu; nmorrell@lco.cl; persson@ociw.edu; miguel@lco.cl; mathew.smith@uct.ac.za; nsuntzeff@tamu.edu RI Folatelli, Gaston/A-4484-2011; Hamuy, Mario/G-7541-2016; OI Sollerman, Jesper/0000-0003-1546-6615; stritzinger, maximilian/0000-0002-5571-1833 NR 97 TC 54 Z9 54 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 713 EP 728 DI 10.1088/0004-637X/696/1/713 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100061 ER PT J AU Hickox, RC Jones, C Forman, WR Murray, SS Kochanek, CS Eisenstein, D Jannuzi, BT Dey, A Brown, MJI Stern, D Eisenhardt, PR Gorjian, V Brodwin, M Narayan, R Cool, RJ Kenter, A Caldwell, N Anderson, ME AF Hickox, Ryan C. Jones, Christine Forman, William R. Murray, Stephen S. Kochanek, Christopher S. Eisenstein, Daniel Jannuzi, Buell T. Dey, Arjun Brown, Michael J. I. Stern, Daniel Eisenhardt, Peter R. Gorjian, Varoujan Brodwin, Mark Narayan, Ramesh Cool, Richard J. Kenter, Almus Caldwell, Nelson Anderson, Michael E. TI HOST GALAXIES, CLUSTERING, EDDINGTON RATIOS, AND EVOLUTION OF RADIO, X-RAY, AND INFRARED-SELECTED AGNs SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; large-scale structure of universe; quasars: general; radio continuum: galaxies; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; DEEP FIELD-SOUTH; QUASAR LUMINOSITY FUNCTION; STAR-FORMATION HISTORY; DARK-MATTER HALOES; ADVECTION-DOMINATED ACCRETION; COLOR-MAGNITUDE RELATION; IRAC SHALLOW SURVEY AB We explore the connection between different classes of active galactic nuclei (AGNs) and the evolution of their host galaxies, by deriving host galaxy properties, clustering, and Eddington ratios of AGNs selected in the radio, Xray, and infrared (IR) wavebands. We study a sample of 585 AGNs at 0.25 < z < 0.8 using redshifts from the AGN and Galaxy Evolution Survey ( AGES). We select AGNs with observations in the radio at 1.4 GHz from the Westerbork Synthesis Radio Telescope, X-rays from the Chandra XBootes Survey, and mid-IR from the Spitzer IRAC Shallow Survey. The radio, X-ray, and IR AGN samples show only modest overlap, indicating that to the flux limits of the survey, they represent largely distinct classes of AGNs. We derive host galaxy colors and luminosities, as well as Eddington ratios, for obscured or optically faint AGNs. We also measure the two-point cross-correlation between AGNs and galaxies on scales of 0.3-10 h(-1) Mpc, and derive typical dark matter halo masses. We find that: (1) radio AGNs are mainly found in luminous red sequence galaxies, are strongly clustered (with M(halo) similar to 3 x 10(13) h(-1) M(circle dot)), and have very low Eddington ratios lambda less than or similar to 10(-3); (2) X-ray-selected AGNs are preferentially found in galaxies that lie in the "green valley" of color-magnitude space and are clustered similar to the typical AGES galaxies (M(halo) similar to 10(13) h(-1) M(circle dot)), with 10(-3) less than or similar to lambda less than or similar to 1; (3) IR AGNs reside in slightly bluer, slightly less luminous galaxies than X-ray AGNs, are weakly clustered (M(halo) less than or similar to 10(12)h(-1) M(circle dot)), and have lambda > 10(-2). We interpret these results in terms of a simple model of AGN and galaxy evolution, whereby a "quasar" phase and the growth of the stellar bulge occurs when a galaxy's dark matter halo reaches a critical mass between similar to 10(12) and 10(13) M(circle dot). After this event, star formation ceases and AGN accretion shifts from radiatively efficient (optical- and IR-bright) to radiatively inefficient ( optically faint, radio-bright) modes. C1 [Hickox, Ryan C.; Jones, Christine; Forman, William R.; Murray, Stephen S.; Brodwin, Mark; Narayan, Ramesh; Kenter, Almus; Caldwell, Nelson; Anderson, Michael E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [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. [Eisenstein, Daniel] Steward Observ, Tucson, AZ 85721 USA. [Jannuzi, Buell T.; Dey, Arjun; Brodwin, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Stern, Daniel; Eisenhardt, Peter R.; Gorjian, Varoujan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cool, Richard J.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Anderson, Michael E.] CALTECH, Dept Astron, Pasadena, CA 91109 USA. RP Hickox, RC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rhickox@cfa.harvard.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Narayan, Ramesh/0000-0002-1919-2730 NR 209 TC 227 Z9 227 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 891 EP 919 DI 10.1088/0004-637X/696/1/891 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100075 ER PT J AU Massaro, F Harris, DE Chiaberge, M Grandi, P Macchetto, FD Baum, SA O'Dea, CP Capetti, A AF Massaro, F. Harris, D. E. Chiaberge, M. Grandi, P. Macchetto, F. D. Baum, S. A. O'Dea, C. P. Capetti, A. TI THE JET OF 3C 17 AND THE USE OF JET CURVATURE AS A DIAGNOSTIC OF THE X-RAY EMISSION PROCESS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (3C 17); galaxies: jets; radiation mechanisms: non-thermal; radio continuum: galaxies; X-rays: general ID 2-JY RADIO-SOURCES; CHANDRA OBSERVATIONS; GALAXIES; SAMPLE; RADIATION; SPECTRA AB We report on the X-ray emission from the radio jet of 3C 17 from Chandra observations and compare the X-ray emission with radio maps from the VLA archive and with the optical-IR archival images from the Hubble Space Telescope. X-ray detections of two knots in the 3C 17 jet are found and both of these features have optical counterparts. We derive the spectral energy distribution for the knots in the jet and give source parameters required for the various X-ray emission models, finding that both inverse Compton (IC)/cosmic microwave background (CMB) and synchrotron are viable to explain the high energy emission. A curious optical feature (with no radio or X-ray counterparts) possibly associated with the 3C 17 jet is described. We also discuss the use of curved jets for the problem of identifying IC X-ray emission via scattering on CMB photons. C1 [Massaro, F.; Harris, D. E.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chiaberge, M.; Macchetto, F. D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chiaberge, M.] INAF, Ist Radioastron Bologna, I-40129 Bologna, Italy. [Grandi, P.] INAF IASF, Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [O'Dea, C. P.] Rochester Inst Technol, Carlson Ctr Imaging Sci 76 3144, Dept Phys, Rochester, NY 14623 USA. [Capetti, A.] INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. RP Massaro, F (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. RI Massaro, Francesco/L-9102-2016; OI Massaro, Francesco/0000-0002-1704-9850; capetti, alessandro/0000-0003-3684-4275; Grandi, Paola/0000-0003-1848-6013 FU National Aeronautics and Space Administration; National Science Foundation; NASA [GO8-9114A] FX We thank the anonymous referee for useful comments that led to improvements in the paper. We thank R. Morganti for giving us her 5 GHz VLA map of 3C 17. F. M. is grateful to G. Migliori and S. Bianchi for their suggestions in the Chandra data analysis, A. Siemiginowska for her help in the use of the Chandra CIAO data reduction analysis software, and E. Liuzzo and S. Giacintucci for their suggestions about the radio data analysis. This research has made use of NASA's Astrophysics Data System; SAOImage DS9, developed by the Smithsonian Astrophysical Observatory; 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. The National Radio Astronomy Observatory is operated by the Associated Universities, Inc., under contract with the National Science Foundation. The work at SAO is supported by NASA Grant GO8-9114A. NR 20 TC 13 Z9 13 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2009 VL 696 IS 1 BP 980 EP 985 DI 10.1088/0004-637X/696/1/980 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 435NH UT WOS:000265350100081 ER PT J AU Cieza, LA Padgett, DL Allen, LE McCabe, CE Brooke, TY Carey, SJ Chapman, NL Fukagawa, M Huard, TL Noriga-Crespo, A Peterson, DE Rebull, LM AF Cieza, Lucas A. Padgett, Deborah L. Allen, Lori E. McCabe, Caer E. Brooke, Timothy Y. Carey, Sean J. Chapman, Nicholas L. Fukagawa, Misato Huard, Tracy L. Noriga-Crespo, Alberto Peterson, Dawn E. Rebull, Luisa M. TI PRIMORDIAL CIRCUMSTELLAR DISKS IN BINARY SYSTEMS: EVIDENCE FOR REDUCED LIFETIMES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; circumstellar matter; infrared: stars; planetary systems: protoplanetary disks; stars: pre-main sequence ID T-TAURI STARS; GIANT PLANET FORMATION; SPITZER C2D SURVEY; FORMING REGIONS; YOUNG STARS; PROTOPLANETARY DISKS; CORONAE-AUSTRALIS; IMAGING SURVEY; CHAMELEON-I; MULTIPLICITY AB We combine the results from several multiplicity surveys of pre-main-sequence stars located in four nearby star-forming regions with Spitzer data from three different Legacy Projects. This allows us to construct a sample of 349 targets, including 125 binaries, which we use to to investigate the effect of companions on the evolution of circumstellar disks. We find that the distribution of projected separations of systems with Spitzer excesses is significantly different (P similar to 2.4e-5, according to the K-S test for binaries with separations less than 400AU) from that of systems lacking evidence for a disk. As expected, systems with projected separations less than 40AU are half as likely to retain at least one disk than are systems with projected separations in the 40-400 AU range. These results represent the first statistically significant evidence for a correlation between binary separation and the presence of an inner disk (r similar to 1AU). Several factors (e. g., the incompleteness of the census of close binaries, the use of unresolved disk indicators, and projection effects) have previously masked this correlation in smaller samples. We discuss the implications of our findings for circumstellar disk lifetimes and the formation of planets in multiple systems. C1 [Cieza, Lucas A.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Padgett, Deborah L.; McCabe, Caer E.; Brooke, Timothy Y.; Carey, Sean J.; Noriga-Crespo, Alberto; Rebull, Luisa M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Allen, Lori E.; Peterson, Dawn E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chapman, Nicholas L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Fukagawa, Misato] Osaka Univ, Osaka 5600043, Japan. [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Cieza, LA (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM lcieza@ifa.hawaii.edu OI Rebull, Luisa/0000-0001-6381-515X FU NASA through the Spitzer Fellowship Program FX We thank Jonathan Williams, Jonathan Swift, Michael Liu, and the anonymous referee for their valuable comments. Support for this work was provided by NASA through the Spitzer Fellowship Program under an award from Caltech. This work makes use of data obtained with the Spitzer Space Telescope, which is operated by JPL/Caltech, under a contract with NASA. NR 45 TC 63 Z9 63 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD MAY 1 PY 2009 VL 696 IS 1 BP L84 EP L88 DI 10.1088/0004-637X/696/1/L84 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 434CP UT WOS:000265253100020 ER PT J AU Rathborne, JM Johnson, AM Jackson, JM Shah, RY Simon, R AF Rathborne, J. M. Johnson, A. M. Jackson, J. M. Shah, R. Y. Simon, R. TI MOLECULAR CLOUDS AND CLUMPS IN THE BOSTON UNIVERSITY-FIVE COLLEGE RADIO ASTRONOMY OBSERVATORY GALACTIC RING SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; Galaxy: kinematics and dynamics; ISM: clouds; ISM: molecules; molecular data ID PLANE-CO SURVEY; MILKY-WAY; GALAXY; QUADRANT AB The Boston University-Five College Radio Astronomy Observatory (BU-FCRAO) Galactic Ring Survey (GRS) of (13)CO J = 1 -> 0 emission covers Galactic longitudes 18 degrees < l < 55 degrees.7 and Galactic latitudes vertical bar b vertical bar <= 1 degrees. Using the SEQUOIA array on the FCRAO 14 m telescope, the GRS fully sampled the (13)CO Galactic emission (46 '' angular resolution on a 22 '' grid) and achieved a spectral resolution of 0.21 km s(-1). Because the GRS uses (13)CO, an optically thin tracer, rather than (12)CO, an optically thick tracer, the GRS allows a much better determination of column density and also a cleaner separation of velocity components along a line of sight. With this homogeneous, fully sampled survey of (13)CO emission, we have identified 829 molecular clouds and 6124 clumps throughout the inner Galaxy using the CLUMPFIND algorithm. Here we present details of the catalog and a preliminary analysis of the properties of the molecular clouds and their clumps. Moreover, we compare clouds inside and outside of the 5 kpc ring and find that clouds within the ring typically have warmer temperatures, higher column densities, larger areas, and more clumps compared with clouds located outside the ring. This is expected if these clouds are actively forming stars. This catalog provides a useful tool for the study of molecular clouds and their embedded young stellar objects. C1 [Simon, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Rathborne, J. M.; Johnson, A. M.; Jackson, J. M.; Shah, R. Y.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP Rathborne, JM (reprint author), Harvard Smithsonian Ctr Astrophys, Mail Stop 42,60 Garden St, Cambridge, MA 02138 USA. EM rathborn@bu.edu; alexj@bu.edu; jackson@bu.edu; ronak@bu.edu; simonr@ph1.uni-koeln.de OI Shah, Ronak/0000-0002-2801-6317 FU National Science Foundation [AST-9800334, AST-0098562, AST-0100793, AST-0228993, AST-0507657] FX This publication makes use of molecular line data from the Boston University-FCRAO Galactic Ring Survey (GRS). The GRS is a joint project of the Boston University and the Five College Radio Astronomy Observatory, funded by the National Science Foundation under grants AST-9800334, AST-0098562, AST-0100793, AST-0228993, and AST-0507657. NR 14 TC 60 Z9 60 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2009 VL 182 IS 1 BP 131 EP 142 DI 10.1088/0067-0049/182/1/131 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 442BX UT WOS:000265815900009 ER PT J AU Bagatini, MD Vasconcelos, TG Laughinghouse, HD Martins, AF Tedesco, SB AF Bagatini, M. D. Vasconcelos, T. G. Laughinghouse, H. D. Martins, A. F. Tedesco, S. B. TI Biomonitoring Hospital Effluents by the Allium cepa L. Test SO BULLETIN OF ENVIRONMENTAL CONTAMINATION AND TOXICOLOGY LA English DT Article DE Hospital effluent; Genotoxicity; Allium cepa; Toxicology; Cell cycle AB Hospital effluents are serious problems in developing countries like Brazil, and when not treated adequately, can cause mutagenic effects on live organisms. Biomonitors, like Allium cepa L., which is one of the most used plant species when monitoring effluent genotoxicity, have been used to alert the world population about environmental contamination and genotoxic chemical emissions. The Allium cepa test was used to evaluate the genotoxicity of a hospital effluent in Santa Maria, Rio Grande do Sul State, Brazil. During the study, chromosomal disruptions, anaphasic bridges, and micronuclei during telophase were observed, indicating environmental toxicity risk. C1 [Bagatini, M. D.; Tedesco, S. B.] Univ Fed Santa Maria, Ctr Ciencias Nat & Exatas, Dept Biol, Lab Plant Cytogenet, BR-97105900 Santa Maria, RS, Brazil. [Vasconcelos, T. G.; Martins, A. F.] Univ Fed Santa Maria, Ctr Ciencias Nat & Exatas, Dept Chem, LATER, BR-97105900 Santa Maria, RS, Brazil. [Laughinghouse, H. D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Tedesco, SB (reprint author), Univ Fed Santa Maria, Ctr Ciencias Nat & Exatas, Dept Biol, Lab Plant Cytogenet, Av Roraima,1000 Cidade Univ, BR-97105900 Santa Maria, RS, Brazil. EM solatedesco@yahoo.com.br RI Laughinghouse, Haywood/M-5836-2016; Bagatini, Margarete/K-3756-2016; Martins, Ayrton/G-2644-2012 OI Laughinghouse, Haywood/0000-0003-1018-6948; Bagatini, Margarete/0000-0001-9263-4980; Martins, Ayrton/0000-0002-8931-7877 NR 11 TC 11 Z9 13 U1 0 U2 0 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-4861 J9 B ENVIRON CONTAM TOX JI Bull. Environ. Contam. Toxicol. PD MAY PY 2009 VL 82 IS 5 BP 590 EP 592 DI 10.1007/s00128-009-9666-z PG 3 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA 420VP UT WOS:000264317600014 PM 19224103 ER PT J AU Yu, IJ Leibo, SP Songsasen, N Dresser, BL Kim, IS AF Yu, Il-jeoung Leibo, S. P. Songsasen, Nucharin Dresser, Betsy L. Kim, In-shik TI CRYOPRESERVATION OF CANINE OVARIAN AND TESTICULAR FIBROBLASTS SO CRYOLETTERS LA English DT Article DE canine; testicular fibroblasts; ovarian fibroblasts; cryopreservation; membrane integrity; functional survival ID IN-VITRO MATURATION; NUCLEAR TRANSFER; ETHYLENE-GLYCOL; BITCH OOCYTES; SPERMATOZOA; FROZEN; CELLS; PRESERVATION; EXTINCTION; EMBRYOS AB To derive a practical procedure to store canine somatic cells, fibroblasts isolated from testicular or ovarian tissues were cryopreserved in 1.2 M ethylene glycol or in 1.2 M dimethylsulfoxide prepared in Dulbecco's Modified Eagle Medium as cryoprotectants, and were frozen either in plastic straws or vials. Thawed cells were cultured for 24 hr at 38.5 degrees C in a humidified atmosphere of 5% CO2 + 95% air, and then their membrane integrity was assayed with a double fluorescent stain, Fertilight(R). In addition, frozen-thawed fibroblasts were cultured for 4 days, and then their functional survival was measured after staining small colonies with trypan blue. After freezing and thawing, membrane integrity of testicular fibroblasts was 55-70% and functional survival ranged from 20-.40%. With frozen-thawed ovarian cells, the average membrane integrity was 55-75% and the average functional survival was 35-40%. When frozen in ethylene glycol, functional survival of ovarian fibroblasts was significantly higher than that of testicular cells (P<0.05). These methods should prove useful to preserve cells collected from canids in the wild. C1 [Yu, Il-jeoung; Kim, In-shik] Chonbuk Natl Univ, Coll Vet Med & Biosafety Res Inst, Jeonju 561756, South Korea. [Leibo, S. P.; Dresser, Betsy L.] Univ New Orleans, Dept Biol Sci, Audubon Ctr Res Endangered Species, New Orleans, LA 70131 USA. [Songsasen, Nucharin] Smithsonians Zool Pk, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Yu, IJ (reprint author), Chonbuk Natl Univ, Coll Vet Med & Biosafety Res Inst, Jeonju 561756, South Korea. EM iyu@chonbuk.ac.kr NR 34 TC 1 Z9 1 U1 0 U2 0 PU CRYO LETTERS PI LONDON PA C/O ROYAL VETERINARY COLLEGE, ROYAL COLLEGE ST, LONDON NW1 0TU, ENGLAND SN 0143-2044 EI 1742-0644 J9 CRYOLETTERS JI CryoLetters PD MAY-JUN PY 2009 VL 30 IS 3 BP 190 EP 201 PG 12 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 479JY UT WOS:000268656800004 PM 19750243 ER PT J AU Seid, MA Wehner, R AF Seid, Marc A. Wehner, Ruediger TI Delayed Axonal Pruning in the Ant Brain: A Study of Developmental Trajectories SO DEVELOPMENTAL NEUROBIOLOGY LA English DT Article DE desert ants; axonal pruning; synapse; insect brain; glia ID AGE-RELATED-CHANGES; DIVISION-OF-LABOR; MUSHROOM BODIES; GLIAL-CELLS; PHEIDOLE-DENTATA; CATAGLYPHIS-BICOLOR; BIOGENIC-AMINES; VOLUME CHANGES; DESERT ANTS; BODY AB The coordination of neuronal maturation and behavioral development is a vital component of survival. The degradation of excessive axonal processes and neuronal networks is a ubiquitous developmental process. In Drosophila, a great portion of axonal pruning occurs during metamorphosis and transpires within hours after pupation. In contrast, we show, using EM-serial sectioning and 3D-reconstructions, that axonal pruning occurs after eclosion and over the course of 60 days in Cataglyphis albicans. Using the mushroom bodies of the brains of Cataglyphis, which have well-developed lip (olfactory integrator) and collar (visual integrator) regions, we show that axonal pruning is dependent upon the differences in the developmental trajectory of the lip and the collar brain regions and happens after eclosion. The elimination of the axonal boutons is most delayed in the collar region, where it is postponed until the ant has had extensive visual experience. We found that individual brain components within a single neuropil can develop at different rates that correlate with the behavioral ecology of these ants and suggest that glia may be mediating the axonal pruning. Our study provides evidence that adult ants may have relatively neotenous brains, and thus more flexibility, allowing them to neuronally adapt to the environment. This neoteny may, in part, explain the neural basis for age-dependent division of labor and the amazing behavioral flexibility exhibited by ants. (C) 2009 Wiley Periodicals, Inc. Develop Neurobiol 69: 350-364, 2009 C1 [Seid, Marc A.; Wehner, Ruediger] Univ Zurich, Inst Zool, CH-8057 Zurich, Switzerland. [Seid, Marc A.] Smithsonian Trop Res Inst, Panama City, Panama. RP Seid, MA (reprint author), Univ Zurich, Inst Zool, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM pheidole@ymail.com FU Institute of Zoology of the University of Zurich (Swiss National Science Foundation) FX We thank Dr. M. Knaden and Mr. T. Seidl for help in the collection of colonies and Mrs. S. Kuhn and Mrs. V. Domanico for technical assistance. We also thank three anonymous reviewers for helpful comments and incites. The work was done while Dr. Seid was a postdoctoral Fellow at the Institute of Zoology of the University of Zurich (Swiss National Science Foundation grant to Prof. Wehner). NR 58 TC 24 Z9 24 U1 0 U2 3 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1932-8451 J9 DEV NEUROBIOL JI Dev. Neurobiol. PD MAY PY 2009 VL 69 IS 6 BP 350 EP 364 DI 10.1002/dneu.20709 PG 15 WC Developmental Biology; Neurosciences SC Developmental Biology; Neurosciences & Neurology GA 435FK UT WOS:000265329100002 PM 19263416 ER PT J AU Temeles, EJ Koulouris, CR Sander, SE Kress, WJ AF Temeles, Ethan J. Koulouris, Carolyn R. Sander, Sarah E. Kress, W. John TI Effect of flower shape and size on foraging performance and trade-offs in a tropical hummingbird SO ECOLOGY LA English DT Article DE coevolution; Eulampis jugularis; foraging trade-offs; Heliconia; hummingbird; mutualism; Purple-throated Carib; specialization; species interactions; West Indies ID PURPLE-THROATED CARIB; NECTAR-FEEDING BIRDS; SEXUAL-DIMORPHISM; CHARACTER DISPLACEMENT; EULAMPIS-JUGULARIS; LONG TONGUES; BILL LENGTH; DRY FOREST; MORPHOLOGY; COMMUNITY AB Matches between the bills of hummingbirds and the flowers they visit have been interpreted as examples of coadaptation and feeding specialization. Observations of birds feeding at flowers longer or shorter than their bills combined with a lack of experimental evidence for foraging trade-offs, however, fail to support these interpretations. We addressed these inconsistencies by considering a seldom-studied dimension of hummingbird-flower relationships, the shape of bills and flowers, through experiments on the Purple-throated Carib, Eulampis jugularis, and its major food plant, Heliconia, in the eastern Caribbean. Bills of male E. jugularis are considerably shorter and straighter than bills of females. We examined foraging performances and trade-offs during visits to natural heliconias and 34 artificial flowers of differing length and curvature. Supporting predictions based on matches between bill and flower morphology, handling times of females were significantly shorter than those of males at the long, curved flowers of a green morph of H. bihai. Contrary to predictions, handling times of males were not significantly shorter than handling times of females at the short flowers of H. caribaea. At artificial flowers, maximum extraction depths of females were significantly longer than maximum extraction depths of males at all curved flowers, but not at straight flowers. Handling times of females were significantly shorter than handling times of males at the longest artificial flowers for all curvatures, whereas handling times of males were significantly shorter at short, straight, artificial flowers, but only while hover-feeding without a perch. Within each sex, handling times were inversely related to bill length at long flowers for all shapes. Taken together, these performance trade-offs suggest that the long, curved bills of females are adapted for feeding from long, curved flowers, whereas the short bills of males are adapted for hover-feeding from short, straighter flowers. In addition, the finding that differences in feeding performance occur at the extremes of floral phenotypes suggests that the evolution of bill morphology may be driven by a small subset of the flowers visited by a hummingbird species. C1 [Temeles, Ethan J.; Koulouris, Carolyn R.; Sander, Sarah E.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA. [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA. EM ejtemeles@amherst.edu FU Amherst College Faculty Research Awards; NSF [IBN-0078483, DEB-0614218] FX We thank D. Anthony and A. Dornelly of the St. Lucia Forestry Department for advice and cooperation, J. Tucker for field assistance, E. and F. Louis-Fernand for accommodations and hospitality, R. Hebert for construction of the artificial flowers, and especially C. B. Fenster, G. R. Graves, J. S. Miller, J. V. Remsen, Jr., and two anonymous reviewers for comments. This research was supported by Amherst College Faculty Research Awards and NSF grants IBN-0078483 and DEB-0614218. NR 64 TC 29 Z9 29 U1 11 U2 75 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 MAY PY 2009 VL 90 IS 5 BP 1147 EP 1161 DI 10.1890/08-0695.1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 442CA UT WOS:000265816200001 PM 19537537 ER PT J AU Rivadeneira, MM Hunt, G Roy, K AF Rivadeneira, Marcelo M. Hunt, Gene Roy, Kaustuv TI The use of sighting records to infer species extinctions: an evaluation of different methods SO ECOLOGY LA English DT Article DE extinction probability; extinction time; false extinctions; local extinctions; sighting record; sudden vs. gradual extinction ID CONFIDENCE-INTERVALS; STRATIGRAPHIC RANGES; FOSSIL HORIZONS; THREAT; RATES; COLLECTIONS; COLONIZATION; TURNOVER; MODELS AB In the absence of long-term monitoring data, inferences about extinctions of species and populations are generally based on past observations about the presence of a particular species at specified places and times (sightings). Several methods have been developed to estimate the probability and timing of extinctions from records of such sightings, but they differ in their computational complexity and assumptions about the nature of the sighting record. Here we use simulations to evaluate the performance of seven methods proposed to estimate the upper confidence limit on extinction times under different extinction and sampling scenarios. Our results show that the ability of existing methods to correctly estimate the timing of extinctions varies with the type of extinction (sudden vs. gradual) and the nature of sampling effort over time. When the probability of sampling a species declines over time, many of the methods perform poorly. On the other hand, the simulation results also suggest that as long as the choice of the method is determined by the nature of the underlying sighting data, existing methods should provide reliable inferences about the timing of past extinctions. C1 [Rivadeneira, Marcelo M.; Roy, Kaustuv] Univ Calif San Diego, Sect Ecol Behav & Evolut, Div Biol Sci, La Jolla, CA 92093 USA. [Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, NHB MRC 121, Washington, DC 20013 USA. RP Rivadeneira, MM (reprint author), Univ Catolica Norte, Fac Ciencias Mar, CEAZA, Larrondo 1281, Coquimbo 1781421, Chile. EM mrivadeneira@ucn.cl RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 FU NOAA-California Sea; FONDECYT [11070147] FX We thank two anonymous reviewers for insightful comments that substantially improved the manuscript. This work was supported by a grant from NOAA-California Sea Grant to K. Roy, and by a FONDECYT grant (11070147) to M. M. Rivadeneira. NR 39 TC 50 Z9 50 U1 0 U2 10 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 MAY PY 2009 VL 90 IS 5 BP 1291 EP 1300 DI 10.1890/08-0316.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 442CA UT WOS:000265816200011 PM 19537549 ER PT J AU Mettke-Hofmann, C Lorentzen, S Schlicht, E Schneider, J Werner, F AF Mettke-Hofmann, Claudia Lorentzen, Sandy Schlicht, Emmi Schneider, Janine Werner, Franziska TI Spatial Neophilia and Spatial Neophobia in Resident and Migratory Warblers (Sylvia) SO ETHOLOGY LA English DT Article ID TERRITORY ACQUISITION; REALIZED HERITABILITY; EXPLORATION; MEMORY; BEHAVIOR; FOOD; BIRDS; INFORMATION; CUES; PERSONALITIES AB Residents and migrants use their environment very differently - the former remain in a given habitat throughout the year, whereas the latter are repeatedly confronted with unfamiliar environments. The difference in ecology may influence decision-making processes whether, when and to which extent to explore an unfamiliar environment. We have investigated spatial neophobia and spatial neophilia - two important novelty reactions that may underlie decision-making - in two closely related warbler species, the resident Sardinian warbler and the migratory garden warbler. Individuals of both species could access an unfamiliar room from a familiar cage. We assessed the conflict between the motivation to enter the novel room (spatial neophilia) and the motivation to avoid it (spatial neophobia) as the frequency and duration of perching on the dowel in the cage, which led to the unfamiliar room before entering it. Furthermore, we measured the latency to enter the novel room and compared the number of individuals of each species entering the room. The combination of the parameters measured allowed assessing the degree of both neophobia and neophilia. Finally, the time spent on each branch in the novel room was taken as a measure for spatial exploration. The migrants perched less often and spent less time on the dowel leading to the room, and entered the novel room quicker than the residents. Additionally, more migrants than residents entered the room. The migrants' decision to enter the novel room can best be explained with a combination of low spatial neophobia coupled with high spatial neophilia, whereas the residents' decision-making is best explained with high spatial neophobia coupled with high spatial neophilia. The differences in neophobia support the migrant-neophobia hypothesis. When in the room, the migrants spent less time on each branch than the residents, possibly indicating that the former collect less spatial information than the latter. C1 [Mettke-Hofmann, Claudia] Max Planck Inst Ornithol, Dept Biol Rhythms & Behaviour, Andechs, Germany. [Mettke-Hofmann, Claudia] Smithsonian Migratory Bird Ctr, Washington, DC USA. [Lorentzen, Sandy] Univ Jena, Inst Ecol, Jena, Germany. [Schlicht, Emmi] Max Planck Inst Ornithol, Dept Behav Ecol & Evolutionary Genet, Seewiesen, Germany. [Schneider, Janine] Univ Munich, Inst Anim Physiol, Munich, Germany. [Werner, Franziska] Univ Halle Wittenberg, Inst Pharmacol & Toxicol, Dept Med, Halle, Germany. RP Mettke-Hofmann, C (reprint author), Liverpool John Moores Univ, Sch Nat Sci & Psychol, James Parsons Bldg,Byrom St, Liverpool L3 3AF, Merseyside, England. EM c.c.mettke-hofmann@ljmu.ac.uk FU German Zoological Society FX Part of the study was conducted during the Summer School 'Spatial Memory and Cognition'. We would like to thank the Max Planck Institute for Ornithology, Andechs, and the German Zoological Society for financial support of this Summer School. We also thank Barbara Helm for conducting the Genstat analyses. NR 51 TC 20 Z9 21 U1 3 U2 35 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0179-1613 J9 ETHOLOGY JI Ethology PD MAY PY 2009 VL 115 IS 5 BP 482 EP 492 DI 10.1111/j.1439-0310.2009.01632.x PG 11 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 433RZ UT WOS:000265224800009 ER PT J AU Corrigan, CM Chabot, NL Mccoy, TJ McDonough, WF Watson, HC Saslow, SA Ash, RD AF Corrigan, Catherine M. Chabot, Nancy L. McCoy, Timothy J. McDonough, William F. Watson, Heather C. Saslow, Sarah A. Ash, Richard D. TI The iron-nickel-phosphorus system: Effects on the distribution of trace elements during the evolution of iron meteorites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID FE-NI ALLOYS; LIQUID-METAL; DISTRIBUTION COEFFICIENTS; S-P; FRACTIONATION; CRYSTALLIZATION; SOLIDIFICATION; SEGREGATION; PHASES; IIIAB AB To better understand the partitioning behavior of elements during the formation and evolution of iron meteorites, two sets of experiments were conducted at 1 atm in the Fe-Ni-P system. The first set examined the effect of P on solid metal/liquid metal partitioning behavior of 22 elements, while the other set explored the effect of the crystal structures of body-centered cubic (alpha)- and face-centered cubic (gamma)-solid Fe alloys on partitioning behavior. Overall, the effect of P on the partition coefficients for the majority of the elements was minimal. As, Au, Ga, Ge, Ir, Os, Pt, Re, and Sb showed slightly increasing partition coefficients with increasing P-content of the metallic liquid. Co, Cu, Pd, and Sn showed constant partition coefficients. Rh, Ru, W, and Mo showed phosphorophile (P-loving) tendencies. Parameterization models were applied to solid metal/ liquid metal results for 12 elements. As, Au, Pt, and Re failed to match previous parameterization models, requiring the determination of separate parameters for the Fe-Ni-S and Fe-Ni-P systems. Experiments with coexisting alpha and gamma Fe alloy solids produced partitioning ratios close to unity, indicating that an alpha versus gamma Fe alloy crystal structure has only a minor influence on the partitioning behaviors of the trace element studied. A simple relationship between an element's natural crystal structure and its alpha/gamma partitioning ratio was not observed. If an iron meteorite crystallizes from a single metallic liquid that contains both S and P, the effect of P on the distribution of elements between the crystallizing solids and the residual liquid will be minor in comparison to the effect of S. This indicates that to a first order, fractional crystallization models of the Fe-Ni-S-P system that do not take into account P are appropriate for interpreting the evolution of iron meteorites if the effects of S are appropriately included in the effort. Published by Elsevier Ltd. C1 [Corrigan, Catherine M.; McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McDonough, William F.; Ash, Richard D.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Watson, Heather C.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. RP Corrigan, CM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th St & Constitut Ave NW, Washington, DC 20560 USA. EM corriganc@si.edu RI McDonough, William/C-4791-2009; Chabot, Nancy/F-5384-2015; McDonough, William/I-7720-2012; OI McDonough, William/0000-0001-9154-3673; Chabot, Nancy/0000-0001-8628-3176; McDonough, William/0000-0001-9154-3673; Watson, Heather/0000-0003-4307-6518 FU NASA [NNG06GF56G, NNG06GI13G, NNG04GG17G]; NSF [EAR0337621] FX We would like to thank John Jones (JSC) for discussion on experimental technique. Tim Gooding (NMNH) and Vern Lauer (JSC) for their assistance/instruction with vacuum sealing silica tubes, and Lisa Collins for weighing out and mixing powders. In addition, we would like to thank Jijin Yang, David Mittlefehldt and two anonymous reviewers for their comments and suggestions for improvements to this paper. This work was funded by NASA Grants NNG06GF56G to T.J. McCoy, NNG06GI13G to N.L. Chabot, NNG04GG17G to W.F. McDonough, and NSF EAR0337621 grant to W. F. McDonough. NR 39 TC 17 Z9 17 U1 3 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY 1 PY 2009 VL 73 IS 9 BP 2674 EP 2691 DI 10.1016/j.gca.2008.11.045 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 433TF UT WOS:000265228000014 ER PT J AU Schmidt, ME Grunder, AL AF Schmidt, Mariek E. Grunder, Anita L. TI The evolution of North Sister: A volcano shaped by extension and ice in the central Oregon Cascade Arc SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE Oregon; Cascade Arc; Three Sisters; dike swarm; subglacial volcanism ID PLATE BENEATH WASHINGTON; SAN-PEDRO COMPLEX; SOUTHERN WASHINGTON; PRIMITIVE MAGMAS; ERUPTIVE HISTORY; CHILEAN ANDES; FORE-ARC; RANGE; GEOCHRONOLOGY; SEGMENTATION AB Along with magma supply rates, glacial ice and local tectonics influence the eruptive style and preservation of arc volcanoes. We present the results of geologic mapping and 20 new (40)Ar/(39)Ar dates for the mafic composite North Sister Volcano, the adjoining Little Brother shield volcano, and Matthieu Lakes Fissure in the central Oregon Cascade Arc, along with major- and trace-element analyses. North Sister is the oldest and most mafic of the Three Sisters Volcanoes and has produced dike-fed, low-K basaltic andesitic (52.5%-55% SiO(2)) agglutinated lava, scoria, and tuffs over its < ca. 400 k.y. history. Severe erosion of the North Sister edifice has revealed the largest radial dike swarm in the Cascade Arc as well as abundant subglacially erupted, palagonitic tuffs and breccias and dramatic unconformities. Slight, but systematic changes in composition coincide with changes in eruptive style, indicating that North Sister was constructed in four central volcano eruptive stages. Stages are bounded by unconformities and include (1) the Lower Shield Stage (ca. 400 ka), (2) the Glacial Stage (99-182 ka), (3) the Upper Shield Stage (ca. 80 ka), and (4) the Stratocone Stage (55 70 ka). We estimate that similar to 90% of the total 40 km(3) volume of North Sister was produced during the first two stages. The >11-km- long, north-trending Matthieu Lakes Fissure (75 11 ka) transects North Sister and erupted in three magmatic pulses, yielding a series of thick lavas, scoria cones, and subglacially erupted flow-dominated tuyas. Glacial ice has been present during much of the eruptive history of North Sister. Palagonitic tuffs, tuyas, and ice-contact lava flows as well as major unconformities between eruptive stages correlate with the delta(18)O of seawater global climate record at ca. 250 ka, 180-130 ka, and 80-18 ka. Time-integrated eruption rates at North Sister appear to have slowed from 0.18 to 0.12 km(3) per k.y. between < ca. 400-300 ka and 100 ka to 0.08 km(3) per k.y. between ca. 100 ka and 50 ka. The waning of volcanism at North Sister coincides with a decrease in Ni and MgO concentrations, indicating that olivine fractionation dominated the later stages. Also, toward the end of volcanism at North Sister, dikes changed from a radial pattern to a N-S pattern, parallel to faults and vent alignments associated with E-W extension of the High Cascades graben. The Matthieu Lakes Fissure represents the final overprinting of the edifice and distribution of magma supply away from the North Sister center. C1 [Schmidt, Mariek E.; Grunder, Anita L.] Oregon State Univ, Dept Geosci, Corvallis, OR 97330 USA. RP Schmidt, ME (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, 10th & Constitut Ave,NW, Washington, DC 20560 USA. EM schmidtm@si.edu FU National Science Foundation [EAR-0230359] FX This work was supported by the National Science Foundation grant EAR-0230359 to Anita Grunder and a 2002 Jack Kleinman graduate research grant to Mariek Schmidt. Insightful reviews by Brad Singer, Dennis Geist, and Michelle Coombs greatly improved the paper. Members of the Oregon State University Advanced Writers Workshop, including Erik Klemetti, Emily Larkin, Emily Lundblad, and Rose Wallick, contributed guidance and support at this paper's inception. Rick Conrey, Robert Duncan, Reid Glassman, Diane Johnson, and John Huard assisted in analytical aspects of this research. Andy Uhrig helped to summit the hazardous North Sister and contributed point counts. Conversations with Robert Duncan, Wes Hildreth, Andy Calvert, Rick Conrey, and Ed Taylor were particularly helpful. Anders Carlson, Denise Giles, Dana Johnston, Erik Klemetti, Katherine Knox, Celeste Mercer, Mike Rowe, and Tammo Huppertz assisted in the field. NR 59 TC 14 Z9 14 U1 2 U2 5 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAY PY 2009 VL 121 IS 5-6 BP 643 EP 662 DI 10.1130/B26442.1 PG 20 WC Geosciences, Multidisciplinary SC Geology GA 438YH UT WOS:000265592200001 ER PT J AU Fiske, RS Rose, TR Swanson, DA Champion, DE McGeehin, JP AF Fiske, Richard S. Rose, Timothy R. Swanson, Donald A. Champion, Duane E. McGeehin, John P. TI Kulanaokuaiki Tephra (ca. AD 400-1000): Newly recognized evidence for highly explosive eruptions at Kilauea Volcano, Hawai'i SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Article DE Kilauea volcano; pyroclastic eruptions; high TiO2 and K2O marker unit; pyroclastic surges; stratigraphy; radiocarbon ages; paleo-magnetism ID AGE CALIBRATION; ASH MEMBER AB Kilauea may be one of the world's most intensively monitored volcanoes, but its eruptive history over the past several thousand years remains rather poorly known. Our study has revealed the vestiges of thin basaltic tephra deposits, overlooked by previous workers, that originally blanketed wide, near-summit areas and extended more than 17 km to the south coast of Hawaii. These deposits, correlative with parts of tephra units at the summit and at sites farther north and northwest, show that Kilauea, commonly regarded as a gentle volcano, was the site of energetic pyroclastic eruptions and indicate the volcano is significantly more hazardous than previously realized. Seventeen new calibrated accelerator mass spectrometry (AMS) radiocarbon ages suggest these deposits, here named the Kulanaokuaiki Tephra, were emplaced ca. A.D. 400-1000, a time of no previously known pyroclastic activity at the volcano. Tephra correlations are based chiefly on a marker unit that contains unusually high values of TiO2 and K2O and on paleo-magnetic signatures of associated lava flows, which show that the Kulanaokuaiki deposits are the time-stratigraphic equivalent of the upper part of a newly exhumed section of the Uwekahuna Ash in the volcano's northwest caldera wall. This section, thought to have been permanently buried by rockfalls in 1983, is thicker and more complete than the previously accepted type Uwekahuna at the base of the caldera wall. Collectively, these findings justify the elevation of the Uwekahuna Ash to formation status; the newly recognized Kulanaokuaiki Tephra to the south, the chief focus of this study, is defined as a member of the Uwekahuna Ash. The Kulanaokuaiki Tephra is the product of energetic pyroclastic falls; no surge- or pyroclastic-flow deposits were identified with certainty, despite recent interpretations that Uwekahuna surges extended 10-20 km from Kilauea's summit. C1 [Fiske, Richard S.; Rose, Timothy R.] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20013 USA. [Swanson, Donald A.] US Geol Survey, Hawaiian Volcano Observ, Hawaii Natl Pk, HI 96718 USA. [Champion, Duane E.] US Geol Survey, Menlo Pk, CA 94025 USA. [McGeehin, John P.] US Geol Survey, Reston, VA 20192 USA. RP Fiske, RS (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM fisker@si.edu NR 37 TC 18 Z9 18 U1 1 U2 6 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 EI 1943-2674 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAY PY 2009 VL 121 IS 5-6 BP 712 EP 728 DI 10.1130/B26327.1 PG 17 WC Geosciences, Multidisciplinary SC Geology GA 438YH UT WOS:000265592200004 ER PT J AU Parra, M Mora, A Jaramillo, C Strecker, MR Sobel, ER Quiroz, L Rueda, M Torres, V AF Parra, Mauricio Mora, Andres Jaramillo, Carlos Strecker, Manfred R. Sobel, Edward R. Quiroz, Luis Rueda, Milton Torres, Vladimir TI Orogenic wedge advance in the northern Andes: Evidence from the Oligocene-Miocene sedimentary record of the Medina Basin, Eastern Cordillera, Colombia SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN LA English DT Review DE Andes; Columbia; Cenozoic; inversion tectonics; foreland basin; fold-and-thrust belts ID MIDDLE MAGDALENA VALLEY; FISSION-TRACK THERMOCHRONOLOGY; FORELAND-BASIN; THRUST BELT; STRUCTURAL EVOLUTION; GROUNDWATER-FLOW; TECTONIC HISTORY; LLANOS FOOTHILLS; THERMAL HISTORY; SOUTH-AMERICA AB Foreland basin development in the Andes of central Colombia has been suggested to have started in the Late Cretaceous through tectonic loading of the Central Cordillera. Eastward migration of the Cenozoic orogenic front has also been inferred from the foreland basin record west of the Eastern Cordillera. However, farther east, limited data provided by foreland basin strata and the adjacent Eastern Cordillera complicate any correlation among mountain building, exhumation, and foreland basin sedimentation. In this study, we present new data from the Medina Basin in the eastern foothills of the Eastern Cordillera of Colombia. We report sedimentological data and palynological ages that link an eastward-thinning early Oligocene to early Miocene syntectonic wedge containing rapid facies changes with an episode of fast tectonic subsidence starting at ca. 31 Ma. This record may represent the first evidence of topographic loading generated by slip along the principal basement-bounding thrusts in the Eastern Cordillera to the southwest of the basin. Zircon fission-track ages and paleo-current analysis reveal the location of these thrust loads and illustrate a time lag between the sedimentary signal of topographic loading and the timing of exhumation (ca. 18 Ma). This lag may reflect the period between the onset of range uplift and significant removal of overburden. Vitrinite reflectance data document northward along-strike propagation of the deformation front and folding of the Oligocene syntectonic wedge. This deformation was coupled with a nonuniform incorporation of the basin into the wedge-top depozone. Thus, our data set constitutes unique evidence for the early growth and propagation of the deformation front in the Eastern Cordillera, which may also improve our understanding of spatiotemporal patterns of foreland evolution in other mountain belts. C1 [Parra, Mauricio; Mora, Andres; Strecker, Manfred R.; Sobel, Edward R.] Univ Potsdam, Inst Geowissensch, D-14476 Potsdam, Germany. [Jaramillo, Carlos; Quiroz, Luis] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama. [Rueda, Milton; Torres, Vladimir] Ecopetrol, Inst Colombiano Petr, Bucaramanga 4185, Colombia. RP Parra, M (reprint author), Univ Potsdam, Inst Geowissensch, D-14476 Potsdam, Germany. EM mauricio@geo.uni-potsdam.de RI Parra, Mauricio/B-7497-2013 OI Parra, Mauricio/0000-0002-5955-6105 FU German Academic Exchange Service [A/02/11325, A/01/12054]; Deutsche Forschungsgemeinschaft (DFG) [Str 373/19-1]; DFG-Leibniz Center for Earth Surface and Climate Studies at Potsdam University; Universidad Nacional de Colombia FX This research was supported by grants and scholarships from the German Academic Exchange Service ( scholarships A/02/11325 and A/01/12054 to M. Parra and A. Mora, respectively), Deutsche Forschungsgemeinschaft (DFG; Str 373/19-1 to M. Strecker), funds from the DFG-Leibniz Center for Earth Surface and Climate Studies at Potsdam University, and the Universidad Nacional de Colombia (Beca de Honor to M. Parra). We also thank the Instituto Colombiano del Petroleo and the Smithsonian Tropical Research Institute for financial support. Seismic profiles were kindly provided by the ANH (Agencia Nacional de Hidrocarburos) of Colombia. We thank B. Horton, G. Bayona, and C. Uba for discussions that helped improve the paper. We also greatly appreciate discussions with A. Kammer and E. Lopez on the Cenozoic stratigraphy of the area. N. Cardozo generously provided us with his program OSXBackstrip for one-dimensional backstripping. A. Gomez kindly identified fossils. G. Veloza and R. Lopez are thanked for their assistance in the field. We are grateful for thorough reviews by D. Barbeau, M. Giovanni, and E. Gomez, and helpful suggestions by Associate Editor J. Schmitt. NR 103 TC 56 Z9 59 U1 1 U2 16 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0016-7606 J9 GEOL SOC AM BULL JI Geol. Soc. Am. Bull. PD MAY PY 2009 VL 121 IS 5-6 BP 780 EP 800 DI 10.1130/B26257.1 PG 21 WC Geosciences, Multidisciplinary SC Geology GA 438YH UT WOS:000265592200008 ER PT J AU Ando, A Huber, BT MacLeod, KG Ohta, T Khim, BK AF Ando, Atsushi Huber, Brian T. MacLeod, Kenneth G. Ohta, Tomoko Khim, Boo-Keun TI Blake Nose stable isotopic evidence against the mid-Cenomanian glaciation hypothesis SO GEOLOGY LA English DT Article ID GLASSY FORAMINIFERAL CALCITE; NORTHERN GERMANY; PALAEOCEANOGRAPHIC EVENTS; GREENHOUSE WORLD; NORTHWEST EUROPE; DEMERARA RISE; ICE SHEETS; CARBONATE; SEA; ATLANTIC AB Detailed multitaxon stable isotope (delta(18)O and delta(13)C) data from Blake Nose (western North Atlantic) argue against a mid-Cenomanian glaciation event during the mid-Cretaceous greenhouse. Results generated are precisely correlated to sea-level changes inferred from European sequence stratigraphy using the twin delta(13)C excursions mid-Cenomanian event (MCE) Ia and MCE Ib. Microfossils analyzed (surface-dwelling to deep-dwelling planktonic foraminifera, benthic foraminifera, coccoliths) show remarkably consistent intertaxon delta(18)O and delta(13)C offsets; comparative scanning electron microscope and Sr/Ca analyses allow some delta(18)O data to be eliminated because of selective diagenesis. Across MCE Ia, the proposed interval of major glacioeustatic regression, the planktonic delta(18)O values are constant for each taxon. The absence of a mean seawater delta(18)O shift contradicts predictions for the mid-Cenomanian glaciation episode. The benthic delta(18)O records show significant fluctuations during MCE I, implying short-term variability in North Atlantic intermediate-water and deep-water circulation patterns and/or sources at that time. C1 [Ando, Atsushi; Huber, Brian T.] Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Ando, Atsushi] Chiba Univ, Fac Sci, Dept Earth Sci, Chiba 2638522, Japan. [Ando, Atsushi] Res Inst Humanity & Nat, Kyoto 6038047, Japan. [Ando, Atsushi; Khim, Boo-Keun] Pusan Natl Univ, Div Earth Environm Syst, Pusan 609735, South Korea. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Ohta, Tomoko] Kyoto Univ, Inst Res Reactor, Div Nucl Engn Sci, Osaka 5900494, Japan. RP Ando, A (reprint author), Smithsonian Natl Museum Nat Hist, Dept Paleobiol, MRC NHB 121, Washington, DC 20013 USA. EM ando@pusan.ac.kr RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU Japan Society for the Promotion of Science Research Fellow; Smithsonian Charles Walcott Fund; U.S. National Science Foundation; Korea Integrated Ocean Drilling Program FX We thank the Ocean Drilling Program for providing sediment samples; Y. Ando for help with sample processing; T. Nakano, S. Ueda, and N. Yuzen for support of laboratory work at the Research Institute for Humanity and Nature; H.-S. Yun for assistance in scanning electron microscopy; I. Jarvis for providing a numerical delta13C data set; and T. Steuber, P. A. Wilson, and an anonymous reviewer for helpful comments. This work was financially supported by a grant-in-aid for the Japan Society for the Promotion of Science Research Fellow (to Ando), the Smithsonian Charles Walcott Fund (to Huber), a U.S. National Science Foundation grant (to MacLeod), and the Korea Integrated Ocean Drilling Program (to Khim). NR 32 TC 33 Z9 34 U1 0 U2 6 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAY PY 2009 VL 37 IS 5 BP 451 EP 454 DI 10.1130/G25580A.1 PG 4 WC Geology SC Geology GA 441EC UT WOS:000265751100017 ER PT J AU Urashima, T Odaka, G Asakuma, S Uemura, Y Goto, K Senda, A Saito, T Fukuda, K Messer, M Oftedal, OT AF Urashima, Tadasu Odaka, Go Asakuma, Sadaki Uemura, Yusuke Goto, Kohta Senda, Akitsugu Saito, Tadao Fukuda, Kenji Messer, Michael Oftedal, Olav T. TI Chemical characterization of oligosaccharides in chimpanzee, bonobo, gorilla, orangutan, and siamang milk or colostrum SO GLYCOBIOLOGY LA English DT Article DE apes; bonobo; chimpanzee; gorilla; milk oligosaccharides; orangutan; siamang ID HUMAN-EVOLUTION; MARSUPIAL MILK; SIALIC ACIDS; LACTATION; LACTOSE; BEAR; TETRASACCHARIDE; SPECTROSCOPY AB Neutral and acidic oligosaccharides were isolated from the milk or colostrum of four great ape species (chimpanzee (Pan troglodytes), bonobo (Pan paniscus), gorilla (Gorilla gorilla), and orangutan (Pongo pygmaeus)) and one lesser ape species (siamang (Symphalangus syndactylus)), and their chemical structures were characterized by (1)H-NMR spectroscopy. Oligosaccharides containing the type II unit (Gal(beta 1-4)GlcNAc) were found exclusively (gorilla and siamang) or predominately (chimpanzee, bonobo, and orangutan) over those containing the type I unit (Gal(beta 1-3)GlcNAc). In comparison, type I oligosaccharides predominate over type II oligosaccharides in human milk, whereas nonprimate milk almost always contains only type II oligosaccharides. The milk or colostrum of the great apes contained oligosaccharides bearing both N-glycolylneuraminic acid and N-acetylneuraminic acid, whereas human milk contains only the latter. Great ape milk, like that of humans, contained fucosylated oligosaccharides whereas siamang milk did not. Since these analyses are based on a limited number of individuals, further research on additional samples of great and lesser ape milk is needed to confirm phylogenetic patterns. C1 [Urashima, Tadasu; Odaka, Go; Uemura, Yusuke; Goto, Kohta; Senda, Akitsugu; Fukuda, Kenji] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 080, Japan. [Asakuma, Sadaki] Natl Agr Res Ctr Hokkaido Reg, Sapporo, Hokkaido, Japan. [Uemura, Yusuke] Kitasato Univ, Fac Sci, Sagamihara, Kanagawa 228, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Messer, Michael] Univ Sydney, Sch Mol & Microbial Biosci, Sydney, NSW 2006, Australia. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 080, Japan. EM urashima@obihiro.ac.jp FU Global COE Program "Frontier Program for Animal Global Health and Hygiene; Ministry of Education, Culture, Sports, Science, and Technology, Japan; Yotsuba Milk Products Co FX Global COE Program "Frontier Program for Animal Global Health and Hygiene"; Ministry of Education, Culture, Sports, Science, and Technology, Japan; and Yotsuba Milk Products Co. NR 38 TC 28 Z9 28 U1 0 U2 11 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0959-6658 J9 GLYCOBIOLOGY JI Glycobiology PD MAY PY 2009 VL 19 IS 5 BP 499 EP 508 DI 10.1093/glycob/cwp006 PG 10 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 431WR UT WOS:000265096000006 PM 19164487 ER PT J AU Silva, MF Domenech-Carbo, MT Fuster-Lopez, L Martin-Rey, S Mecklenburg, MF AF Silva, Miguel F. Teresa Domenech-Carbo, Maria Fuster-Lopez, Laura Martin-Rey, Susana Mecklenburg, Marion F. TI Determination of the plasticizer content in poly(vinyl acetate) paint medium by pyrolysis-silylation-gas chromatography-mass spectrometry SO JOURNAL OF ANALYTICAL AND APPLIED PYROLYSIS LA English DT Article; Proceedings Paper CT 18th International Symposium on Analytical and Applied Pyrolysis CY MAY 18-23, 2008 CL Lanzarote, SPAIN SP Spanish Minist Sci & Innovat, Spanish Council Sci Res, Univ Las Palmas de Gran Canaria DE Polyvinyl acetate; Plasticizer; Diethylphthalate; Dibutylphthalate; Py-GC-MS; 1,4-Dibromebenzene; Internal standard; Binding media; Quantification AB The use of plasticizers in emulsion paints is intended to provide optimal mechanical properties to polyvinyl acetate polymers (PVA), making them suitable as binding media for paintings. The loss of these properties with ageing is often related to the slow migration and evaporation of such plasticizers, resulting in severe embrittlement and potential damage to the paint film. A new method consisting of the quantification of the plasticizer content of PVAc samples with "online" silylation-pyrolysis with hexadimethyldisilazane (HMDS) as a derivatization agent in Py-GC-MS and using 1,4-dibromebenzene as an IS is proposed here. For this purpose, two series of specimens of Mowilith 50(th) (a pure PVAc resin) with the addition of two different plasticizers, diethylphthalate (DEP) and dibutylphthalate (DBP), were prepared as thin films and submitted to a multi-step UV-light artificial ageing program so that the plasticizer content was determined at each ageing stage. (C) 2009 Elsevier B.V. All rights reserved. C1 [Silva, Miguel F.; Teresa Domenech-Carbo, Maria; Fuster-Lopez, Laura; Martin-Rey, Susana] Univ Politecn Valencia, Inst Restauracio Patrimoni, Valencia 46022, Spain. [Mecklenburg, Marion F.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD USA. RP Domenech-Carbo, MT (reprint author), Univ Politecn Valencia, Inst Restauracio Patrimoni, Cami Vera S-N, Valencia 46022, Spain. EM tdomenec@upv.crbc.es RI FUSTER-LOPEZ, Laura/F-5503-2016 NR 23 TC 16 Z9 16 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-2370 J9 J ANAL APPL PYROL JI J. Anal. Appl. Pyrolysis PD MAY PY 2009 VL 85 IS 1-2 BP 487 EP 491 DI 10.1016/j.jaap.2008.11.020 PG 5 WC Chemistry, Analytical; Spectroscopy SC Chemistry; Spectroscopy GA 451HL UT WOS:000266461200066 ER PT J AU Crosier, AE Henghali, JN Howard, J Pukazhenthi, BS Terrell, KA Marker, LL Wildt, DE AF Crosier, Adrienne E. Henghali, Josephine N. Howard, Jogayle Pukazhenthi, Budhan S. Terrell, Kimberly A. Marker, Laurie L. Wildt, David E. TI Improved Quality of Cryopreserved Cheetah (Acinonyx jubatus) Spermatozoa After Centrifugation Through Accudenz SO JOURNAL OF ANDROLOGY LA English DT Article DE Felid; acrosome; cryopreservation; cryoprotectant; genome resource banking ID ARTIFICIAL-INSEMINATION; EJACULATE TRAITS; RESOURCE BANKS; DOMESTIC CAT; SPERM; GLYCEROL; CONSERVATION; TECHNOLOGIES; FERTILITY; INDUCTION AB Sperm cryopreservation, in combination with assisted reproductive techniques, is a valuable tool for the genetic management of endangered felids. However, the acrosome of the cheetah spermatozoon is especially sensitive to cryopreservation, with approximately 40% of spermatozoa experiencing acrosomal damage immediately after thawing and then another approximately 15% loss during the next 4 hours in vitro. Additionally, thawing causes a reduction in sperm motility by approximately 20% with another decrease of approximately 12% during subsequent incubation in vitro. We hypothesized that slow removal of glycerol from cryopreserved cheetah spermatozoa using an Accudenz gradient would improve acrosomal integrity, sperm motility longevity, and structural morphology. Accudenz was compared with traditional cheetah sperm processing methods for glycerol removal that involves washing, multistep resuspension, and swim-up processing. Electroejaculates (n = 21 total from 8 males) were washed in Ham F10 medium, and sperm pellets were resuspended in TEST-yolk buffer with 0% glycerol. Samples were cryopreserved in straws in 4% final glycerol, thawed, and assessed for percent intact acrosomes (% IA), percent motility (% M), and forward progressive status (FPS; scale, 0-5). Sperm motility index (SMI) was calculated as (% M + [FPS X 20]) divided by 2. In study 1, glycerol removal by centrifugation through an Accudenz gradient (4%, 10%) was compared with traditional sperm washing (control) and multistep resuspension protocols. At each time after centrifugation (hourly for 4 hours), % IA was improved (P < .05) for Accudenz (range, 36%-39%) compared with control (30%-33%) and multistep (29%-33%) treatments. In study 2, a modified Accudenz protocol was compared with traditional washing and was found to improve (P < .05) SMI (range, 52-64) compared with controls (range, 41-52) at each time postthaw after centrifugation. In study 3, swim-up processed sperm were compared with those treated by centrifugation through Accudenz and traditional sperm washing for improving sperm morphology. The percentage of structurally-normal sperm recovered postthawing increased (P < .05) for both the Accudenz (38%) and swim-up (33%) treatments compared with controls (21%). Percent IA and SMI also were improved (P < .05) for Accudenz (range, 39%-47% and 46-59, respectively) compared with controls (range, 26%-33% and 40-53, respectively). Results indicate that using Accudenz for glycerol removal from cryopreserved cheetah sperm mitigates the significant loss in sperm quality that occurs after freeze-thawing. This alleviation of cellular damage resulting from cryopreservation contributes to a more than 10% improvement in overall sperm motility and, more importantly, allows retention of 40% or more of sperm with intact acrosomes. C1 [Crosier, Adrienne E.; Howard, Jogayle; Pukazhenthi, Budhan S.; Terrell, Kimberly A.; Wildt, David E.] Smithsonians Natl Zool Pk, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. [Crosier, Adrienne E.; Henghali, Josephine N.; Marker, Laurie L.] Cheetah Conservat Fund, Otjiwarongo, Namibia. RP Crosier, AE (reprint author), Smithsonians Natl Zool Pk, Conservat & Res Ctr, Dept Reprod Sci, 1500 Remount Rd, Front Royal, VA 22630 USA. EM crosiera@si.edu FU Ohrstrom Family Foundation. Inc.; William H. Donner Foundation, Inc. FX Funding was provided by the Friends of the National Zoo, Smithsonian's Abbott Endownient Fund, Morris Annual Foundation, John Bull Zoo Society Wildlil'e Conservation Fund, Ohrstrom Family Foundation. Inc. and William H. Donner Foundation, Inc. International travel was supported by British Airways. NR 41 TC 10 Z9 10 U1 0 U2 17 PU AMER SOC ANDROLOGY, INC PI LAWRENCE PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA SN 0196-3635 EI 1939-4640 J9 J ANDROL JI J. Androl. PD MAY-JUN PY 2009 VL 30 IS 3 BP 298 EP 308 DI 10.2164/jandrol.108.006239 PG 11 WC Andrology SC Endocrinology & Metabolism GA 439IO UT WOS:000265621000012 PM 19023140 ER PT J AU Coddington, JA Agnarsson, I Miller, JA Kuntner, M Hormiga, G AF Coddington, Jonathan A. Agnarsson, Ingi Miller, Jeremy A. Kuntner, Matjaz Hormiga, Gustavo TI Undersampling bias: the null hypothesis for singleton species in tropical arthropod surveys SO JOURNAL OF ANIMAL ECOLOGY LA English DT Review DE Araneae; Guyana; neutral theory; sampling intensity; species richness estimation; spiders ID FRUIT-FEEDING BUTTERFLIES; RAIN-FOREST TREE; COMMUNITY STRUCTURE; BEETLE ASSEMBLAGES; ABUNDANCE DISTRIBUTIONS; TEMPORAL DIMENSIONS; RICHNESS ESTIMATION; RELATIVE ABUNDANCE; INSECT HERBIVORES; SAMPLING EFFORT AB Frequency of singletons - species represented by single individuals - is anomalously high in most large tropical arthropod surveys (average, 32%). We sampled 5965 adult spiders of 352 species (29% singletons) from 1 ha of lowland tropical moist forest in Guyana. Four common hypotheses (small body size, male-biased sex ratio, cryptic habits, clumped distributions) failed to explain singleton frequency. Singletons are larger than other species, not gender-biased, share no particular lifestyle, and are not clumped at 0.25-1 ha scales. Monte Carlo simulation of the best-fit lognormal community shows that the observed data fit a random sample from a community of similar to 700 species and 1-2 million individuals, implying approximately 4% true singleton frequency. Undersampling causes systematic negative bias of species richness, and should be the default null hypothesis for singleton frequencies. Drastically greater sampling intensity in tropical arthropod inventory studies is required to yield realistic species richness estimates. The lognormal distribution deserves greater consideration as a richness estimator when undersampling bias is severe. C1 [Coddington, Jonathan A.; Agnarsson, Ingi; Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Agnarsson, Ingi] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. [Kuntner, Matjaz] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, SI-1001 Ljubljana, Slovenia. [Miller, Jeremy A.] Natl Natuurhist Museum Nat, NL-2333 CR Leiden, Netherlands. [Hormiga, Gustavo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. RP Coddington, JA (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 105,POB 37012, Washington, DC 20013 USA. EM coddington@si.edu RI Hormiga, Gustavo/C-3874-2009; OI Miller, Jeremy/0000-0001-8918-9775 FU Smithsonian 'Biodiversity of the Guianas'; National Science Foundation [DEB 9712353] FX Thanks to Vicky Funk, Carol Kelloff, David Clarke, Tom Hollowell, and Romeo Williams for logistical support, and Rick West, Gita Bodner, G. B. Edwards, Martin Ramirez, Fernando Alvarez-Padilla, Scott Larcher, and Dana DeRoche for specimen work and identification. We are grateful for the hospitality of the WaiWai community of Southern Guyana. We thank Robert Colwell, Phil DeVries, Jack Longino, and Anne Magurran for comments on an earlier draft. Support for this research came from a Smithsonian 'Biodiversity of the Guianas' grant to J. A. Coddington, a Smithsonian Neotropical Lowlands grant to J. Coddington, and a National Science Foundation grant to G. Hormiga and J. Coddington (DEB 9712353). NR 120 TC 110 Z9 118 U1 4 U2 44 PU WILEY PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD MAY PY 2009 VL 78 IS 3 BP 573 EP 584 DI 10.1111/j.1365-2656.2009.01525.x PG 12 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 427NB UT WOS:000264784900011 PM 19245379 ER PT J AU Langin, KM Marra, PP Nemeth, Z Moore, FR Kyser, TK Ratcliffe, LM AF Langin, Kathryn M. Marra, Peter P. Nemeth, Zoltan Moore, Frank R. Kyser, T. Kurt Ratcliffe, Laurene M. TI Breeding latitude and timing of spring migration in songbirds crossing the Gulf of Mexico SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID HYDROGEN ISOTOPE RATIOS; WOOD-WARBLERS PARULINAE; STABLE-HYDROGEN; BIRD MIGRATION; GEOGRAPHIC ASSIGNMENT; ENERGETIC CONDITION; CATCHMENT AREAS; STOPOVER; MIGRANTS; PATTERNS AB Each spring, millions of songbirds migrate across the Gulf of Mexico on their way to breeding sites in North America. Data from radar and migration monitoring stations have revealed broad patterns in the spatial and temporal course of trans-Gulf migration. Unfortunately, we have limited information on where these birds have previously spent the winter and where they are migrating to breed. Here we measure stable-hydrogen isotopes in feathers (delta D(f)) to infer the breeding latitude of five species of songbirds - hooded warblers Wilsonia citrina, American redstarts Setophaga ruticilla, black-and-white warblers Mniotilta varia, ovenbirds Seiurus aurocapilla, and northern waterthrushes S. noveboracensis - that were captured at a stopover site along the coast of southwestern Louisiana in spring 2004. Values of delta D(f) across all species ranged from -163 to -35 parts per thousand (n=212), and within most species the range was consistent with the latitudinal extent of known breeding sites in central and eastern North America. Individuals that arrived first along the northern Gulf coast had delta D(f) values indicative of southerly breeding sites in hooded warblers, American redstarts, black-and-white warblers, and ovenbirds, but no relationship was found between passage timing and delta D(f) for northern waterthrushes. Our findings suggest that spring passage is often timed to coincide with the emergence of suitable conditions on breeding areas, with southern breeding birds migrating first. C1 [Marra, Peter P.] Smithsonian Migr Bird Ctr, Washington, DC 20008 USA. [Moore, Frank R.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Kyser, T. Kurt] Queens Univ, Dept Geol Sci & Geol Engin, Kingston, ON K7L 3N6, Canada. [Langin, Kathryn M.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. RP Langin, KM (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM langink@rams.colostate.edu RI Nemeth, Zoltan/B-6961-2013; OI Langin, Kathryn/0000-0002-1799-1942 FU National Science Foundation; PPM [0089565]; FRM [0078189]; Natural Sciences and Engineering Research Council of Canada (NSERC; LMR, TKK); Canadian Foundation for Innovation (TKK, LMR); Canada Graduate Scholarship (NSERC); Ontario Graduate Scholarship; Society of Canadian Ornithologists (Taverner award); Association of Field Ornithologists (Bergstrom award) FX Thanks to A. Sutton, J. Gore, E. Henry, and D. Rios for assistance in the field and K. Klassen, A. Vuletich, and K. Geale for help in the isotope lab. S. Lougheed, B. Frost, H. Schmaljohann, and two anonymous reviewers provided much appreciated comments on previous drafts. This research was funded by the National Science Foundation (0089565, PPM; 0078189, FRM), the Natural Sciences and Engineering Research Council of Canada (NSERC; LMR, TKK), and the Canadian Foundation for Innovation (TKK, LMR). KML was supported by a Canada Graduate Scholarship (NSERC), an Ontario Graduate Scholarship, and research grants from the Society of Canadian Ornithologists (Taverner award) and the Association of Field Ornithologists (Bergstrom award). NR 62 TC 12 Z9 12 U1 0 U2 22 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD MAY PY 2009 VL 40 IS 3 BP 309 EP 316 DI 10.1111/j.1600-048X.2008.04496.x PG 8 WC Ornithology SC Zoology GA 445CL UT WOS:000266027200011 ER PT J AU Liu, J Wang, B Ding, QH Kuang, XY Soon, WL Zorita, E AF Liu, Jian Wang, Bin Ding, Qinghua Kuang, Xueyuan Soon, Willie Zorita, Eduardo TI Centennial Variations of the Global Monsoon Precipitation in the Last Millennium: Results from ECHO-G Model SO JOURNAL OF CLIMATE LA English DT Article ID GENERAL-CIRCULATION MODEL; 1000-YR CONTROL SIMULATION; COUPLED CLIMATE MODEL; PROXY-BASED RECONSTRUCTIONS; SURFACE AIR-TEMPERATURE; HOLOCENE ASIAN MONSOON; PAST MILLENNIUM; ATMOSPHERIC CIRCULATION; SOUTHERN-OSCILLATION; INTERNAL VARIABILITY AB The authors investigate how the global monsoon (GM) precipitation responds to the external and anthropogenic forcing in the last millennium by analyzing a pair of control and forced millennium simulations with the ECHAM and the global Hamburg Ocean Primitive Equation (ECHO-G) coupled ocean-atmosphere model. The forced run, which includes the solar, volcanic, and greenhouse gas forcing, captures the major modes of precipitation climatology comparably well when contrasted with those captured by the NCEP reanalysis. The strength of the modeled GM precipitation in the forced run exhibits a significant quasi-bicentennial oscillation. Over the past 1000 yr, the simulated GM precipitation was weak during the Little Ice Age (1450-1850) with the three weakest periods occurring around 1460, 1685, and 1800, which fell in, respectively, the Sporer Minimum, Maunder Minimum, and Dalton Minimum periods of solar activity. Conversely, strong GM was simulated during the model Medieval Warm Period (ca. 1030-1240). Before the industrial period, the natural variations in the total amount of effective solar radiative forcing reinforce the thermal contrasts both between the ocean and continent and between the Northern and Southern Hemispheres resulting in the millennium-scale variation and the quasi-bicentennial oscillation in the GM index. The prominent upward trend in the GM precipitation occurring in the last century and the notable strengthening of the global monsoon in the last 30 yr (1961-90) appear unprecedented and are due possibly in part to the increase of atmospheric carbon dioxide concentration, though the authors' simulations of the effects from recent warming may be overestimated without considering the negative feedbacks from aerosols. The simulated change of GM in the last 30 yr has a spatial pattern that differs from that during the Medieval Warm Period, suggesting that global warming that arises from the increases of greenhouse gases and the input solar forcing may have different effects on the characteristics of GM precipitation. It is further noted that GM strength has good relational coherence with the temperature difference between the Northern and Southern Hemispheres, and that on centennial time scales the GM strength responds more directly to the effective solar forcing than the concurrent forced response in global-mean surface temperature. C1 [Liu, Jian; Kuang, Xueyuan] Chinese Acad Sci, Nanjing Inst Geog & Limnol, State Key Lab Lake Sci & Environm, Nanjing 210008, Peoples R China. [Wang, Bin; Ding, Qinghua] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. [Wang, Bin; Ding, Qinghua] Univ Hawaii Manoa, Internatl Pacific Res Ctr, Honolulu, HI 96822 USA. [Wang, Bin] Ocean Univ China, CPEO, Qingdao, Peoples R China. [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zorita, Eduardo] GKSS Forschungszentrum Geesthacht GmbH, Inst Coastal Res, Geesthacht, Germany. RP Liu, J (reprint author), Chinese Acad Sci, Nanjing Inst Geog & Limnol, State Key Lab Lake Sci & Environm, 73 E Beijing Rd, Nanjing 210008, Peoples R China. EM jianliu@niglas.ac.cn RI ding, qinghua/G-1186-2011 FU Chinese Academy of Sciences [KZCX2-YW315]; National Basic Research Program of China [2004CB720208]; National Natural Science Foundation of China [40672210]; National Science Foundation (NSF) [ATM06-29531]; NOAA/OGP FX Jian Liu and Bin Wang acknowledge the financial supports from the Innovation Project of Chinese Academy of Sciences (Grant KZCX2-YW315), the National Basic Research Program of China (Grant 2004CB720208), and the National Natural Science Foundation of China (Grant 40672210). Bin Wang and Qinghua Ding acknowledge the support received from the National Science Foundation (NSF) climate dynamics program (ATM06-29531) and NOAA/OGP. NR 74 TC 50 Z9 62 U1 3 U2 24 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 EI 1520-0442 J9 J CLIMATE JI J. Clim. PD MAY PY 2009 VL 22 IS 9 BP 2356 EP 2371 DI 10.1175/2008JCLI2353.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 448TT UT WOS:000266285600006 ER PT J AU Cardona, A Cordani, UG Ruiz, J Valencia, VA Armstrong, R Chew, D Nutman, A Sanchez, AW AF Cardona, A. Cordani, U. G. Ruiz, J. Valencia, V. A. Armstrong, R. Chew, D. Nutman, A. Sanchez, A. W. TI U-Pb Zircon Geochronology and Nd Isotopic Signatures of the Pre-Mesozoic Metamorphic Basement of the Eastern Peruvian Andes: Growth and Provenance of a Late Neoproterozoic to Carboniferous Accretionary Orogen on the Northwest Margin of Gondwana SO JOURNAL OF GEOLOGY LA English DT Review ID DETRITAL ZIRCONS; SOUTHERN MEXICO; NORTHERN CHILE; SM-ND; ARGENTINE PRECORDILLERA; TECTONIC IMPLICATIONS; ACTIVE MARGIN; PROTO-ANDES; MOBILE BELT; BREAK-UP AB This study integrates U-Pb zircon geochronology ( from LAM-ICP-MS, SHRIMP, and TIMS) with Nd isotopic data from orthogneisses and metasedimentary rocks of the pre-Mesozoic basement of the eastern Peruvian Andes to provide new information on the tectonic evolution and Neoproterozoic-Paleozoic paleogeography of this segment of the proto-Andean margin. A high-grade orthogneiss unit yields U-Pb zircon protolith crystallization ages of similar to 613 Ma. It was metamorphosed and intruded by an Early Ordovician granitoid. Subsequently, two different volcano-sedimentary sequences were laid down and metamorphosed, probably as a consequence of terrane accretion. The older sequence was deposited and metamorphosed between 450 and 420 Ma, and the younger one was deposited after 320 Ma and metamorphosed at 310 Ma. U-Pb detrital zircon age patterns from the two sequences are within the age intervals 315-480, 480-860, 960-1400, and 11400 Ma. These data strongly suggest geological and spatial links between the different units, implying the existence of active magmatism contemporaneous with the reworking of previously formed orogenic complexes. Mesoproterozoic and older ages suggest that the detrital sources are on the western margin of Gondwana, near the Amazonian Craton and/or other Grenvillian-type domains, such as those found within the Andean belt. Neoproterozoic to Ordovician zircons suggest that this crustal segment was formed on an active margin along the western side of the Amazonian Craton. Whole-rock Nd isotope data from metasedimentary rocks of the two younger units yield (epsilon)Nd (450 Ma, 310 Ma) values between similar to 6.3 and similar to 13.2 and Sm-Nd T(DM) model ages between 1.6 and 2.1 Ga. The comparison of the Nd isotope record with the U-Pb detrital zircon data suggests that recycling of older crust was an important factor in the growth of the central Peruvian segment of the proto-Andean margin during the Proterozoic and the Early Paleozoic. Different tectonic and paleogeographic models are discussed in light of the new data presented here. C1 [Cardona, A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Cordani, U. G.] Univ Sao Paulo, Inst Geociencias, BR-05508080 Sao Paulo, Brazil. [Ruiz, J.; Valencia, V. A.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Armstrong, R.] Australian Natl Univ, Res Sch Earth Sci, Acton, ACT 0200, Australia. [Chew, D.] Trinity Coll Dublin, Dept Geol, Dublin 2, Ireland. [Nutman, A.] Chinese Acad Geol Sci, Inst Geol, Beijing 100037, Peoples R China. [Sanchez, A. W.] Inst Geol Minero & Met, Lima 41, Peru. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM cardonaa@si.edu RI Chew, David/B-7828-2008; Cordani, Umberto/F-3686-2014 OI Chew, David/0000-0002-6940-1035; Cordani, Umberto/0000-0003-4425-5905 FU Sao Paulo State Research Agency (FAPESP) [02/072488-3] FX We wish to acknowledge the support received from the Sao Paulo State Research Agency (FAPESP), grant 02/072488-3. We thank the colleagues and the staff of the Geochronological Research Center of the University of Sao Paulo for technical help and fruitful discussions. J. Machare and O. Palacios of the Peruvian Geological Survey (INGEMMET) are acknowledged for their logistical support and help provided during several stages of this research. A. Zapata and J. Galdos of INGEMMET are acknowledged for discussions and help during field work. Thorough and clear reviews and suggestions by V. A. Ramos, J. Aleinikoff, and A. Anderson are acknowledged. The assistance of M. Marulanda during field work and other stages of this research is deeply appreciated. These results are part of A. Cardona's PhD thesis at the University of Sao Paulo. NR 112 TC 36 Z9 36 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0022-1376 J9 J GEOL JI J. Geol. PD MAY PY 2009 VL 117 IS 3 BP 285 EP 305 DI 10.1086/597472 PG 21 WC Geology SC Geology GA 423VU UT WOS:000264524600004 ER PT J AU Sarzetti, LC Labandeira, CC Muzon, J Wilf, P Cuneo, NR Johnson, KR Genise, JF AF Sarzetti, Laura C. Labandeira, Conrad C. Muzon, Javier Wilf, Peter Cuneo, N. Ruben Johnson, Kirk R. Genise, Jorge F. TI ODONATAN ENDOPHYTIC OVIPOSITION FROM THE EOCENE OF PATAGONIA: THE ICHNOGENUS PALEOOVOIDUS AND IMPLICATIONS FOR BEHAVIORAL STASIS SO JOURNAL OF PALEONTOLOGY LA English DT Article ID FOSSIL INSECT EGGS; ARGENTINA INSECTA; UPPER PALEOCENE; PHYLOGENETIC-RELATIONSHIPS; DRAGONFLY INSECTA; PLANT DIVERSITY; MIDDLE-EOCENE; SOUTH-AMERICA; ZYGOPTERA; FAMILY AB We document evidence of endophytic oviposition on fossil compression/impression leaves from the early Eocene Laguna del Hunco and middle Eocene Rio Pichileufu floras of Patagonia, Argentina. Based on distinctive morphologies and damage patterns of elongate, ovoid, lens-, or teardrop-shaped scars in the leaves, we assign this insect damage to the ichnogenus Paleoovoidus, consisting of an existing ichnospecies, P. rectus, and two new ichnospecies, P. arcuatum and P. bifurcatus. In P. rectus, the scars are characteristically arranged in linear rows along the midvein; in P. bifurcatus, scars are distributed in double rows along the midvein and parallel to secondary veins; and in P. arcuatum, scars are deployed in rectilinear and arcuate rows. In some cases, the narrow, angulate end of individual scars bear a darkened region encompassing a circular hole or similar feature indicating ovipositor tissue penetration. A comparison to the structure and surface pattern of modern ovipositional damage on dicotyledonous leaves suggests considerable similarity to certain zygopteran Odonata. Specifically, members of the Lestidae probably produced P. rectus and P. bifurcatus, whereas species of Coenagrionidae were responsible for P. arcuatum. Both Patagonian localities represent an elevated diversity of potential fern, gymnosperm, and especially angiosperm hosts, the targets of all observed oviposition. However, we did not detect targeting of particular plant families. Our results indicate behavioral stasis for the three ovipositional patterns for at least 50 million years. Nevertheless, synonymy of these oviposition patterns with mid-Mesozoic ichnospecies indicates older origins for these distinctive modes of oviposition. C1 [Sarzetti, Laura C.; Cuneo, N. Ruben; Genise, Jorge F.] Museo Paleontol Egidio Feruglio, CONICET, RA-9100 Trelew, Chubut, Argentina. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20213 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Muzon, Javier] Inst Limnol Dr Raul A Ringuelet, RA-1888 Buenos Aires, DF, Argentina. [Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Johnson, Kirk R.] Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA. RP Sarzetti, LC (reprint author), Museo Paleontol Egidio Feruglio, CONICET, Ave Fontana 140, RA-9100 Trelew, Chubut, Argentina. EM lsarzetti@mef.org.ar; labandec@si.edu; muzon@ilpla.edu.ar; pwilf@psu.edu; rcuneo@mef.org.ar; kirk.johnson@dmns.org; jgenise@mef.org.ar FU Proyecto de Investigacion Cientifica y Tecnologica (PICT) [13286]; National Science Foundation [DEB-0345750]; National Geographic Society [35229-G2]; Evolution of Terrestrial Ecosystems Consortium of the National Museum of Natural History FX We are grateful to Roberto Straneck for his excellent assistance with German translation. We thank Alejandra Molina for her help with field research in collecting extant odonatan oviposition, and to Alberto Slarm for his help with the plant identifications. For helpful reviews of the manuscript, we thank J. Petrulevicius and D. Vasilenko. In addition, we acknowledae M. Caffa, L. Canessa, B. Cariglino, I. Escapa, M. Gandolfo, C. Gonzalez, R. Horwitt, P Puerta, E. Ruigmez, H. Smekal. and S. Wing for invaluable assistance in the field and laboratory. This work was supported by the Proyecto de Investigacion Cientifica y Tecnologica (PICT) 13286 to J. E Genise; National Science Foundation Grant DEB-0345750 to PW. CCL, NRC, and KRJ, National Geographic Society grant 35229-G2 to PW and NRC; the Evolution of Terrestrial Ecosystems Consortium of the National Museum of Natural History to LCS; and the Smithsonian Institution Small Grants Fund to CCL. Thanks go to Finnegan Marsh for the final draft of the figures, and to the Nahueltripay family and INVAP (Instituto de Investigaciones Aplicadas) for land access. This is Contribution 163 of the Evolution of Terrestrial Ecosystems Consortium at the National Museum of Natural History, Washington, D.C. NR 119 TC 25 Z9 26 U1 0 U2 5 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 MAY PY 2009 VL 83 IS 3 BP 431 EP 447 DI 10.1666/08-121.1 PG 17 WC Paleontology SC Paleontology GA 449RT UT WOS:000266348400010 ER PT J AU Hershler, R Jayko, AS AF Hershler, Robert Jayko, Angela S. TI A MACTRID BIVALVE FROM PLEISTOCENE DEPOSITS OF LAKE RUSSELL, MONO BASIN, CALIFORNIA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID DEATH-VALLEY; RANGIA-CUNEATA; COLORADO RIVER; PLIOCENE C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Jayko, Angela S.] US Geol Survey, White Mt Res Stn, Bishop, CA 93514 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu; ajayko@usgs.gov NR 45 TC 0 Z9 0 U1 0 U2 2 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 MAY PY 2009 VL 83 IS 3 BP 496 EP 499 DI 10.1666/08-132.1 PG 4 WC Paleontology SC Paleontology GA 449RT UT WOS:000266348400017 ER PT J AU Riedlecker, EI Ashton, GV Ruiz, GM AF Riedlecker, Eva I. Ashton, Gail V. Ruiz, Gregory M. TI Geometric morphometric analysis discriminates native and non-native species of Caprellidae in western North America SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE allometry; amphipod; Caprella mutica; latitudinal variation; morphology; shape ID LIFE-HISTORY; AMPHIPODA; COAST; CRUSTACEA; CRAB; BRACHYURA; MUTICA; STOCKS AB Characteristics of the second gnathopod are traditionally used to distinguish between species of caprellid amphipods. However, these distinctions are Often subjective and can be variable within a species. Geometric morphometrics were used to quantitatively assess shape variation of the second gnathopod propodus of three species of caprellids in North America, including the non-native Caprella mutica. Gnathopod shapes of C. mutica specimens from different latitudes revealed distinct morphologies; the factors responsible for the shape variations are unknown. Allometric change of propodus shape was observed in C. mutica. Larger individuals showed a wide array of possible propodus morphologies. Despite this variability, there were clear differences between large specimens of C. mutica and two species native to North America: C. alaskana and C. kennerlyi. The use of geometric morphometrics and the thin-plate spline method can serve to both complement descriptions using traditional keys and aid in identification of non-native species in novel geographical regions. C1 [Riedlecker, Eva I.; Ashton, Gail V.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Riedlecker, Eva I.] Univ Vienna, Dept Theoret Biol & Morphol, A-1090 Vienna, Austria. RP Ashton, GV (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ashtong@si.edu OI Ruiz, Gregory/0000-0003-2499-441X FU National Sea Grant Program; Prince William Sound Regional Citizens' Advisory Council; Smithsonian Institution FX The authors are grateful to staff at the Smithsonian Environmental Research Center involved in specimen collection and Michael Stachowitsch for comments on the manuscript. This research was supported by the National Sea Grant Program, Prince William Sound Regional Citizens' Advisory Council, and Smithsonian Institution. NR 44 TC 2 Z9 3 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD MAY PY 2009 VL 89 IS 3 BP 535 EP 542 DI 10.1017/S0025315408002452 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 459TO UT WOS:000267133200011 ER PT J AU Zotz, G Reuter, N AF Zotz, Gerhard Reuter, Norman TI The effect of exposure to sea water on germination and vegetative growth of an epiphytic bromeliad SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Bromeliaceae; epiphytes; glycophyte; halophyte; heteroblasty; mangrove; nutrient limitation; Panama; RGR; seeds; Werauhia sanguinolenta ID WERAUHIA-SANGUINOLENTA; TILLANDSIA-CIRCINATA; SALT-TOLERANCE; SOUTH-FLORIDA; POPULATIONS; NUTRIENT; PLANT AB Vascular epiphytes call be quite abundant in vegetation close to the ocean surf. where they are exposed to a more or less Continuous input of salt spray. The ecophysiological basis of their Occurrence, i.e. salt tolerance or avoidance is Unresolved. because all previous Studies were observational and conclusions thus circumstantial. Here. the effect of varying concentrations of salt water on germination. and growth and survival of seedlings and established plants was investigated in a growth cabinet study under controlled conditions. Seeds (1500). seedlings (750) and small tank plants (336) were front four populations of Werauhia sanguinolenta that were growing either close to the sea or inland in Panama. Changes of Na(+) and K(+) concentrations in plant tissue were also determined. No differenccs in the sensitivity to salt were found among populations. nor among life stages. External concentrations (C(ext)) of up to 15% sea water (c. 0.5% Na(+)) allowed complete germination as well as positive growth and survival in both seedlings and established plants over short periods (8-10 wk). After longer exposure ( 12 wk) of established plants visible damage and increased mortality were observed at lower C(ext), but critical tissue Na(+) levels were similar: c. 50 mg gDW(-1). It is concluded that this Common epiphyte does not meet. the definition of a halophyte. but still possesses a rather high tolerance to sodium. C1 [Zotz, Gerhard; Reuter, Norman] Carl von Ossietzky Univ Oldenburg, Inst Environm & Biol Sci, AG Funct Ecol, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Zotz, G (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Environm & Biol Sci, AG Funct Ecol, Box 2503, D-26111 Oldenburg, Germany. EM gerhard.zotz@uni-oldenburg.de NR 23 TC 1 Z9 1 U1 1 U2 10 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 MAY PY 2009 VL 25 BP 311 EP 319 DI 10.1017/S0266467409006014 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 437RH UT WOS:000265504100008 ER PT J AU Duda, TF Lee, T AF Duda, Thomas Franklin, Jr. Lee, Taehwan TI Isolation and population divergence of a widespread Indo-West Pacific marine gastropod at Easter Island SO MARINE BIOLOGY LA English DT Article ID OYSTER PINCTADA-MARGARITIFERA; REEF FISHES; PHYLOGEOGRAPHY; PATTERNS; CONUS; EVOLUTION; DIFFERENTIATION; HAPLOTYPES; SPECIATION; HISTORY AB Oceanic islands represent excellent systems for studying the link between geographic isolation and population divergence. Easter Island is the world's most isolated island and exhibits a high level of endemicity in the nearshore marine environment. Yet few studies have examined the effect of such extreme isolation on the divergence of populations of widespread species that occur at Easter Island. Conus miliaris, a marine gastropod distributed throughout much of the Indo-West Pacific, occurs at Easter Island where the population is ecologically and morphologically distinct from other populations of the species. To determine whether these phenotypic differences are associated with genetic isolation of the Easter Island population, we investigated the phylogeography of this species by examining mitochondrial COI sequences obtained from 141 individuals from eight localities occurring predominantly in the western, central and southeastern Pacific. Results from our analyses show that C. miliaris at Easter Island differs genetically from other populations. We estimate that C. miliaris colonized Easter Island shortly after the origin of the island a parts per thousand currency sign0.7 million years ago and that since population founding, gene flow has occurred predominantly from Easter Island to the west and that little migration has occurred into Easter Island. C1 [Duda, Thomas Franklin, Jr.; Lee, Taehwan] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Duda, Thomas Franklin, Jr.; Lee, Taehwan] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Duda, Thomas Franklin, Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Duda, TF (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 1109 Geddes Ave, Ann Arbor, MI 48109 USA. EM tfduda@umich.edu FU National Geographic Society Committee for Research and Exploration [CRE 8228- 07]; NSF [IOS 0718370] FX We thank John Slapcinsky and Gustav Paulay of the Florida Museum of Natural History of the University of Florida at Gainesville and Jochen Gerber, Rudiger Bieler and Janet Voight of the Field Museum for loaned specimens. We also thank Chris Meyer from the National Museum of Natural History for sequences of some of the specimens analyzed in this work. We also gratefully acknowledge Javier Rivera Vergara from the Unidad de Recursos Bentonicos of the Subsecretaria de Pesca of Chile for permission to collect specimens at Easter Island, Brian Dyer from the Universidad del Mar in Vi a del Mar, Chile for assistance in obtaining the permission, and Dan Chang for Weld assistance at Easter Island. We appreciate comments from Diarmaid O Foighil, Alan Kohn and Haris Lessios on earlier drafts of this manuscript. This work was completed with support from the National Geographic Society Committee for Research and Exploration (CRE 8228- 07) and NSF ( IOS 0718370). NR 47 TC 9 Z9 9 U1 0 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAY PY 2009 VL 156 IS 6 BP 1193 EP 1202 DI 10.1007/s00227-009-1161-x PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 428TU UT WOS:000264873800009 ER PT J AU Janzen, DH Hallwachs, W Blandin, P Burns, JM Cadiou, JM Chacon, I Dapkey, T Deans, AR Epstein, ME Espinoza, B Franclemont, JG Haber, WA Hajibabaei, M Hall, JPW Hebert, PDN Gauld, ID Harvey, DJ Hausmann, A Kitching, IJ Lafontaine, D Landry, JF Lemaire, C Miller, JY Miller, JS Miller, L Miller, SE Montero, J Munroe, E Green, SR Ratnasingham, S Rawlins, JE Robbins, RK Rodriguez, JJ Rougerie, R Sharkey, MJ Smith, MA Solis, MA Sullivan, JB Thiaucourt, P Wahl, DB Weller, SJ Whitfield, JB Willmott, KR Wood, DM Woodley, NE Wilson, JJ AF Janzen, Daniel H. Hallwachs, Winnie Blandin, Patrick Burns, John M. Cadiou, Jean-Marie Chacon, Isidro Dapkey, Tanya Deans, Andrew R. Epstein, Marc E. Espinoza, Bernardo Franclemont, John G. Haber, William A. Hajibabaei, Mehrdad Hall, Jason P. W. Hebert, Paul D. N. Gauld, Ian D. Harvey, Donald J. Hausmann, Axel Kitching, Ian J. Lafontaine, Don Landry, Jean-Francois Lemaire, Claude Miller, Jacqueline Y. Miller, James S. Miller, Lee Miller, Scott E. Montero, Jose Munroe, Eugene Green, Suzanne Rab Ratnasingham, Sujeevan Rawlins, John E. Robbins, Robert K. Rodriguez, Josephine J. Rougerie, Rodolphe Sharkey, Michael J. Smith, M. Alex Solis, M. Alma Sullivan, J. Bolling Thiaucourt, Paul Wahl, David B. Weller, Susan J. Whitfield, James B. Willmott, Keith R. Wood, D. Monty Woodley, Norman E. Wilson, John J. TI Integration of DNA barcoding into an ongoing inventory of complex tropical biodiversity SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE Area de Conservacion Guanacaste; Braconidae; COI; Costa Rica; DNA barcoding; Lepidoptera; species identification; Tachinidae; taxonomy; tropical biodiversity inventory ID PARASITOID FLIES DIPTERA; SKIPPER BUTTERFLIES; GROUP HYMENOPTERA; LEPIDOPTERA; WASPS; GENUS; IDENTIFICATION; DIVERGENCE; TACHINIDAE; DIVERSITY AB Inventory of the caterpillars, their food plants and parasitoids began in 1978 for today's Area de Conservacion Guanacaste (ACG), in northwestern Costa Rica. This complex mosaic of 120 000 ha of conserved and regenerating dry, cloud and rain forest over 0-2000 m elevation contains at least 10 000 species of non-leaf-mining caterpillars used by more than 5000 species of parasitoids. Several hundred thousand specimens of ACG-reared adult Lepidoptera and parasitoids have been intensively and extensively studied morphologically by many taxonomists, including most of the co-authors. DNA barcoding - the use of a standardized short mitochondrial DNA sequence to identify specimens and flush out undisclosed species - was added to the taxonomic identification process in 2003. Barcoding has been found to be extremely accurate during the identification of about 100 000 specimens of about 3500 morphologically defined species of adult moths, butterflies, tachinid flies, and parasitoid wasps. Less than 1% of the species have such similar barcodes that a molecularly based taxonomic identification is impossible. No specimen with a full barcode was misidentified when its barcode was compared with the barcode library. Also as expected from early trials, barcoding a series from all morphologically defined species, and correlating the morphological, ecological and barcode traits, has revealed many hundreds of overlooked presumptive species. Many but not all of these cryptic species can now be distinguished by subtle morphological and/or ecological traits previously ascribed to 'variation' or thought to be insignificant for species-level recognition. Adding DNA barcoding to the inventory has substantially improved the quality and depth of the inventory, and greatly multiplied the number of situations requiring further taxonomic work for resolution. C1 [Janzen, Daniel H.; Hallwachs, Winnie; Dapkey, Tanya] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Blandin, Patrick] Museum Natl Hist Nat, F-75005 Paris, France. [Burns, John M.; Hall, Jason P. W.; Harvey, Donald J.; Miller, Scott E.; Robbins, Robert K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Chacon, Isidro; Espinoza, Bernardo; Montero, Jose] Inst Nacl Biodiversidad, Santo Domingo De Heredia, Costa Rica. [Deans, Andrew R.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Epstein, Marc E.] Calif Dept Food & Agr, Plant Pest Diagnost Branch, Sacramento, CA 95832 USA. [Haber, William A.] Missouri Bot Garden, St Louis, MO 63166 USA. [Hajibabaei, Mehrdad; Ratnasingham, Sujeevan; Rougerie, Rodolphe; Smith, M. Alex; Wilson, John J.] Univ Guelph, Canadian Ctr DNA Barcoding, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Hebert, Paul D. N.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Hausmann, Axel] Zool State Collect Munich, Sekt Lepidoptera, D-81247 Munich, Germany. [Kitching, Ian J.] Nat Hist Museum, Dept Entomol, London SW7 5BD, England. [Lafontaine, Don; Landry, Jean-Francois; Wood, D. Monty] Agr & Agri Food Canada, Canadian Natl Collect Insects, Ottawa, ON K1A 0C6, Canada. [Miller, Jacqueline Y.; Willmott, Keith R.] Univ Florida, McGuire Ctr Lepidoptera & Biodivers, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Green, Suzanne Rab] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. [Rawlins, John E.] Carnegie Museum Nat Hist, Sect Invertebrate Zool, Pittsburgh, PA 15213 USA. [Rodriguez, Josephine J.] Univ Illinois, Urbana, IL 61801 USA. [Sharkey, Michael J.] Univ Kentucky, Dept Entomol, Lexington, KY 40546 USA. [Solis, M. Alma; Woodley, Norman E.] Smithsonian Inst, SEL, USDA, Washington, DC 20013 USA. [Wahl, David B.] Amer Entomol Inst, Gainesville, FL 32608 USA. [Weller, Susan J.; Whitfield, James B.] Univ Minnesota, Bell Museum Nat Hist, Minneapolis, MN 55455 USA. RP Janzen, DH (reprint author), Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. EM djanzen@sas.upenn.edu RI Rougerie, Rodolphe/D-2930-2009; Wilson, John James/C-4656-2012; Smith, M Alex/B-4468-2013; Hebert, Paul/C-4161-2013; Ratnasingham, Sujeevan/G-9103-2014; Woodley, Norman/M-6160-2014; OI Miller, Scott/0000-0002-4138-1378; Rougerie, Rodolphe/0000-0003-0937-2815; Smith, M Alex/0000-0002-8650-2575; Hebert, Paul/0000-0002-3081-6700; Dapkey, Tanya/0000-0002-2050-7664; Deans, Andrew/0000-0002-2119-4663 FU Gordon and Betty Moore Foundation; NSERC; Genome Canada through the Ontario Genomics Institute; Canada Research Chairs program; US National Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; Guanacaste Dry Forest Conservation Fund; Wege Foundation; Science Connection; Jessie B. Cox Charitable Trust; INBio; Area de Conservacion Guanacaste FX This research was supported by grants from the Gordon and Betty Moore Foundation, NSERC, Genome Canada through the Ontario Genomics Institute, and the Canada Research Chairs program to PDNH, and by grants from the US National Science Foundation (BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730 and 0515699), Guanacaste Dry Forest Conservation Fund, Wege Foundation, Science Connection, Jessie B. Cox Charitable Trust, INBio, and Area de Conservacion Guanacaste to DHJ and WH. We thank our many colleagues at the Biodiversity Institute of Ontario for the diligent labour of DNA barcoding tens of thousands of specimens, and the 30 ACG parataxonomists for collecting, rearing, and databasing caterpillars and parasitoids. This study would never have occurred, nor could the analysis have been conducted, without the taxonomic and identification support of more than 150 taxonomists and their institutes that have identified plants, and Lepidoptera, wasps, and flies for the ACG caterpillar and parasitoid inventory during the past 30 years. Many of those supporting the taxonomy behind this barcoding study are co-authors, but we additionally wish to thank Andy Warren, Linda Pitkin, Malcolm Scoble, Robert Poole, Patricia Gentili-Poole, Phil DeVries, Mike Pogue, Vitor Becker, Jorge Corrales, Thierry Vaglia, Jean Haxaire, Manuel Balcazar and Espinita Porcupine for taxonomic and editing support. NR 60 TC 162 Z9 175 U1 4 U2 72 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAY PY 2009 VL 9 SU 1 BP 1 EP 26 DI 10.1111/j.1755-0998.2009.02628.x PG 26 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 433TC UT WOS:000265227700001 PM 21564960 ER PT J AU Gonzalez, S Maldonado, JE Ortega, J Talarico, AC Bidegaray-Batista, L Garcia, JE Duarte, JMB AF Gonzalez, Susana Maldonado, Jesus E. Ortega, Jorge Talarico, Angela Cristina Bidegaray-Batista, Leticia Garcia, Jose Eduardo Barbanti Duarte, Jose Mauricio TI Identification of the endangered small red brocket deer (Mazama bororo) using noninvasive genetic techniques (Mammalia; Cervidae) SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE cryptic species; Mazama; noninvasive sampling; small red brocket deer; species identification ID ELUSIVE ANIMALS; AMERICAN DEER; POPULATION; DNA; CONSERVATION AB The small red brocket deer Mazama bororo is one of the most endangered deer in the Neotropics. The great morphological similarities with three other sympatric brocket deer species, coupled with the fact that they inhabit densely forested habitats complicate detection and prevent the use of traditional methodologies for accurate identification of species. The ability to determine the presence of this endangered species in an area is crucial for estimating its distribution range, and is critical for establishing conservation management strategies. Here we describe a fast and reliable noninvasive genetic method for species identification of Mazama species from faeces. We designed a primer set that amplifies a short 224-bp fragment of the cytochrome b and demonstrate its effectiveness in successful amplification of DNA isolated from both tissue and faecal samples. This fragment contains a BSTNI/ECORII digestion site that is unique to the endangered M. bororo. The digested polymerase chain reaction products yielded a 160-bp fragment that is clearly visible in a 2% agarose gel. Two other diagnostic sites were identified to differentiate the other three sympatric species, SspI (M. gouazoubira) and AflIII (M. americana, and M. nana). C1 [Gonzalez, Susana; Bidegaray-Batista, Leticia] IIBCE, Dept Genet, Fac Ciencias UdelaR, Unidad Genet Conservac, Montevideo, Uruguay. [Maldonado, Jesus E.; Ortega, Jorge] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, NZP NMNH, Washington, DC 20008 USA. [Ortega, Jorge] Escuela Nacl Ciencias Biol, Lab Ictiol & Limnol, Inst Politecn Nacl, Col Santo Tomas 11340, Mexico. [Talarico, Angela Cristina; Barbanti Duarte, Jose Mauricio] Sao Paulo State Univ, NUPECCE, Dept Zootecnia, FCAV UNESP, BR-14884900 Jaboticabal, SP, Brazil. [Garcia, Jose Eduardo] Univ Fed Pernambuco, Ctr Acad Vitoria, BR-55608680 Vitoria De Santo Antao, PE, Brazil. RP Gonzalez, S (reprint author), IIBCE, Dept Genet, Fac Ciencias UdelaR, Unidad Genet Conservac, Montevideo, Uruguay. EM sugonza@iibce.edu.uy RI Barbanti Duarte, Jose Mauricio /C-6946-2013 OI Barbanti Duarte, Jose Mauricio /0000-0002-7805-0265 FU FAPESP; CNPq; PROBIO/MMA; CSIC-UdelaR; PEDECIBA; Smithsonian Center for Conservation and Evolutionary Genetics; Friends of the National Zoo and Wildlife Trust Alliance FX Our study was funded by FAPESP, CNPq, PROBIO/MMA, from Brazil, CSIC-UdelaR; PEDECIBA, from Uruguay, and the Smithsonian Center for Conservation and Evolutionary Genetics, Friends of the National Zoo and Wildlife Trust Alliance. We thank the 'Instituto Brazileiro do Meio Ambiente e dos Recursos Naturais Renovaveis' and Secretaria do Meio Ambiente do Parana for granting permits for sample collections. M. Cosse assisted in laboratory techniques and K. Maldonado provided comments that greatly enhanced the quality of this manuscript. NR 22 TC 11 Z9 11 U1 1 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAY PY 2009 VL 9 IS 3 BP 754 EP 758 DI 10.1111/j.1755-0998.2008.02390.x PG 5 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 443GC UT WOS:000265897200012 PM 21564736 ER PT J AU Peters, MB Hagen, C Snyder, B Glenn, TC Gowaty, PA AF Peters, Maureen B. Hagen, Cris Snyder, Brian Glenn, Travis C. Gowaty, Patricia Adair TI Microsatellite markers isolated from Drosophila hydei SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE anisogamy; Drosophila hydei; microsatellites; parentage analysis; PCR; sexual selection AB We isolated and characterized 10 polymorphic microsatellite loci in Drosophila hydei. The number of alleles per locus ranged from 3 to 8 (N = 23 individuals). Polymorphic information content ranged from 0.316 to 0.750 and observed heterozygosity from 0.261 to 0.913. These markers will be valuable in studies of sexual selection and parental investment in D. hydei. C1 [Peters, Maureen B.; Hagen, Cris; Glenn, Travis C.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA. [Snyder, Brian] Univ Georgia, Inst Ecol, Athens, GA 30602 USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Glenn, Travis C.] Univ Georgia, Coll Publ Hlth, Athens, GA 30602 USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. RP Peters, MB (reprint author), Univ Georgia, Savannah River Ecol Lab, PO Drawer E, Aiken, SC 29802 USA. EM mbpeters@uga.edu RI Glenn, Travis/A-2390-2008 FU US Department of Energy [DE-FC09-07SR22506]; University of Georgia Research Foundation; National Science Foundation [0545597] FX Disclaimer: 'This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not necessarily constitute or imply its endorsement, recommendation, or favouring by the United States Government or any agency thereof. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof.' NR 9 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAY PY 2009 VL 9 IS 3 BP 817 EP 819 DI 10.1111/j.1755-0998.2008.02266.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 443GC UT WOS:000265897200030 PM 21564754 ER PT J AU Buerki, S Forest, F Acevedo-Rodriguez, P Callmander, MW Nylander, JAA Harrington, M Sanmartin, I Kupfer, P Alvarez, N AF Buerki, Sven Forest, Felix Acevedo-Rodriguez, Pedro Callmander, Martin W. Nylander, Johan A. A. Harrington, Mark Sanmartin, Isabel Kuepfer, Philippe Alvarez, Nadir TI Plastid and nuclear DNA markers reveal intricate relationships at subfamilial and tribal levels in the soapberry family (Sapindaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Aceraceae; Classification; Hippocastanaceae; Molecular phylogeny; Paraphyly; Polyphyly; Sapindaceae; Xanthoceras ID MULTIPLE SEQUENCE ALIGNMENT; PHYLOGENETIC ANALYSIS; MISSING DATA; NONCODING REGIONS; UNIVERSAL PRIMERS; FLOWERING PLANTS; CHLOROPLAST DNA; INCOMPLETE TAXA; TREE; RBCL AB The economically important soapberry family (Sapindaceae) comprises about 1900 species mainly found in the tropical regions of the world, with only a few genera being restricted to temperate areas. The infra-familial classification of the Sapindaceae and its relationships to the closely related Aceraceae and Hippocastanaceae - which have now been included in an expanded definition of Sapindaceae (i.e., subfamily Hippocastanoideae) - have been debated for decades. Here we present a phylogenetic analysis of Sapindaceae based on eight DNA sequence regions from the plastid and nuclear genomes and including 85 of the 141 genera defined within the family. Our study comprises 997 new sequences of Sapindaceae from 152 specimens. Despite presenting 18.6% of missing data our complete data set produced a topology fully congruent with the one obtained from a subset without missing data, but including fewer markers. The use of additional information therefore led to a consistent result in the relative position of clades and allowed the definition of a new phylogenetic hypothesis. Our results confirm a high level of paraphyly and polyphyly at the subfamilial and tribal levels and even contest the monophyletic status of several genera. Our study confirms that the Chinese monotypic genus Xanthoceras is sister to the rest of the family, in which subfamily Hippocastanoideae is sister to a clade comprising subfamilies Dodonaeoideae and Sapindoideae. On the basis of the strong support demonstrated in Sapindoideae, Dodonaeoideae and Hippocastanoideae as well as in 14 subclades, we propose and discuss informal groupings as basis for a new classification of Sapindaceae. (C) 2009 Elsevier Inc. All rights reserved. C1 [Buerki, Sven; Kuepfer, Philippe; Alvarez, Nadir] Univ Neuchatel, Inst Biol, CH-2009 Neuchatel, Switzerland. [Forest, Felix] Royal Bot Gardens, Jodrell Lab, Mol Systemat Sect, Richmond TW9 3DS, Surrey, England. [Acevedo-Rodriguez, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Callmander, Martin W.] Missouri Bot Garden, St Louis, MO 63166 USA. [Callmander, Martin W.] Conservatoire & Jardin Bot Ville Geneve, CH-1292 Chambesy, Switzerland. [Nylander, Johan A. A.] Stockholm Univ, Dept Bot, SE-10691 Stockholm, Sweden. [Harrington, Mark] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4870, Australia. [Sanmartin, Isabel] Real Jardin Bot CSIC, Dept Biodivers & Conservat, Madrid 28014, Spain. RP Buerki, S (reprint author), Univ Neuchatel, Inst Biol, Rue Emile Argand 11, CH-2009 Neuchatel, Switzerland. EM sven.buerki@unine.ch RI Alvarez, Nadir/B-4318-2010; Buerki, Sven/A-8305-2012; Buerki, Sven/F-6008-2012; Sanmartin, Isabel/G-3131-2015 OI Alvarez, Nadir/0000-0002-0729-166X; Sanmartin, Isabel/0000-0001-6104-9658 FU University of Neuchatel (Switzerland) FX The first author would like to thank Professor Giorgina Bernasconi from the University of Neuchatel (Switzerland) for help and financial support. We are grateful to the following people and institutions for the supply of plant material: the Conservatoire et Jardin botaniques de la ville de Geneve (Switzerland); the Malagasy staff of the Missouri Botanical Garden in Antananarivo (Madagascar); Caroline Weckerle (University of Zurich, Switzerland); Laura Vary (University of California-Irvine; USA) and Jean-Noel Labat (Museum d'Histoire Naturelle, Paris, France). The first author thank Yong-Ming Yuan (University of Neuchatel, Switzerland) for providing laboratory support and plant material. We thank Nils Arrigo (University of Neuchatel; Switzerland), Ken Wurdack (Smithsonian Institution, Washington, USA), Jerome Munzinger (Laboratorie de Botanique, Centre IRD de Noumea, Noumea, New Caledonia), Peter Lowry II and Pete Phillipson (Missouri Botanical Garden, Saint-Louis; USA) for valuable comments on the manuscript and herbarium determinations. We thank the Associate Editor and two anonymous reviewers for numerous constructive comments that greatly improved the manuscript. NR 79 TC 63 Z9 68 U1 1 U2 32 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2009 VL 51 IS 2 BP 238 EP 258 DI 10.1016/j.ympev.2009.01.012 PG 21 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 442AL UT WOS:000265812000010 PM 19405193 ER PT J AU Keres, D Katz, N Fardal, M Dave, R Weinberg, DH AF Keres, Dusan Katz, Neal Fardal, Mark Dave, Romeel Weinberg, David H. TI Galaxies in a simulated Lambda CDM Universe - I. Cold mode and hot cores SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cooling flows; galaxies: evolution; galaxies: formation; galaxies: haloes; intergalactic medium ID SMOOTHED PARTICLE HYDRODYNAMICS; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; COSMOLOGICAL SPH SIMULATIONS; DARK-MATTER HALOES; COOLING FLOWS; STELLAR MASS; BLACK-HOLES; FORMATION HISTORY; DWARF GALAXIES AB We study the formation of galaxies in a large volume (50 h(-1) Mpc, 2 x 288(3) particles) cosmological simulation, evolved using the entropy and energy-conserving smoothed particle hydrodynamics (SPH) code GADGET-2. Most of the baryonic mass in galaxies of all masses is originally acquired through filamentary 'cold mode' accretion of gas that was never shock heated to its halo virial temperature, confirming the key feature of our earlier results obtained with a different SPH code. Atmospheres of hot, virialized gas develop in haloes above 2-3 x 10(11) M(circle dot), a transition mass that is nearly constant from z = 3 to 0. Cold accretion persists in haloes above the transition mass, especially at z >= 2. It dominates the growth of galaxies in low-mass haloes at all times, and it is the main driver of the cosmic star formation history. Our results suggest that the cooling of shock-heated virialized gas, which has been the focus of many analytic models of galaxy growth spanning more than three decades, might be a relatively minor element of galaxy formation. At high redshifts, satellite galaxies have gas accretion rates similar to central galaxies of the same baryonic mass, but at z < 1 the accretion rates of low-mass satellites are well below those of comparable central galaxies. Relative to our earlier simulations, the GADGET-2 simulations predict much lower rates of 'hot mode' accretion from the virialized gas component. Hot accretion rates compete with cold accretion rates near the transition mass, but only at z <= 1. Hot accretion is inefficient in haloes above similar to 5 x 10(12) M(circle dot), with typical rates lower than 1M(circle dot) yr(-1) at z <= 1, even though our simulation does not include active galactic nuclei (AGN) heating or other forms of 'preventive' feedback. Instead, the accretion rates are low because the inner density profiles of hot gas in these haloes are shallow, with long associated cooling times. The cooling recipes typically used in semi-analytic models can overestimate the accretion rates in these haloes by orders of magnitude, so these models may overemphasize the role of preventive feedback in producing observed galaxy masses and colours. A fraction of the massive haloes develop cuspy profiles and significant cooling rates between z = 1 and 0, a redshift trend similar to the observed trend in the frequency of cooling flow clusters. C1 [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Keres, Dusan; Katz, Neal; Fardal, Mark] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Dave, Romeel] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Keres, D (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM dkeres@cfa.harvard.edu; nsk@kaka.astro.umass.edu; fardal@astro.umass.edu; rad@astro.as.arizona.edu; dhw@astronomy.ohio-state.edu FU Institute for Theory and Computation at the Harvard College Observatory; NSF [AST-0205969]; NASA [NAGS-13308, NNG04GK68G] FX We thank V. Springel for making the GADGET-2 public and K. Finlator and B. Oppenheimer for help during the modification of the public version of the code. DK acknowledges the support from the ITC Fellowship at the Institute for Theory and Computation at the Harvard College Observatory. We also acknowledge support from NSF grant AST-0205969 and from NASA grants NAGS-13308 and NNG04GK68G. NR 90 TC 380 Z9 381 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP 160 EP 179 DI 10.1111/j.1365-2966.2009.14541.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700030 ER PT J AU Kumar, P Narayan, R AF Kumar, Pawan Narayan, Ramesh TI GRB 080319B: evidence for relativistic turbulence, not internal shocks SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; turbulence; gamma-rays: bursts ID GAMMA-RAY BURSTS; PROMPT EMISSION; AFTERGLOWS; MODEL; JETS AB We show that the excellent optical and gamma-ray data available for GRB 080319B rule out the internal shock model for the prompt emission. The data instead point to a model in which the observed radiation was produced close to the deceleration radius (similar to 10(17) cm) by a turbulent source with random Lorentz factors of similar to 10 in the comoving frame. The optical radiation was produced by synchrotron emission from relativistic electrons, and the gamma-rays by inverse-Compton scattering of the synchrotron photons. The gamma-ray emission originated both in eddies and in an inter-eddy medium, whereas the optical radiation was mostly from the latter. Therefore, the gamma-ray emission was highly variable whereas the optical was much less variable. The model explains all the observed features in the prompt optical and gamma-ray data of GRB 080319B. We are unable to determine with confidence whether the energy of the explosion was carried outwards primarily by particles (kinetic energy) or magnetic fields. Consequently, we cannot tell whether the turbulent medium was located in the reverse shock (we can rule out the forward shock) or in a Poynting-dominated jet. C1 [Kumar, Pawan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kumar, P (reprint author), Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. EM pk@astro.as.utexas.edu OI Narayan, Ramesh/0000-0002-1919-2730 NR 40 TC 61 Z9 62 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2009 VL 395 IS 1 BP 472 EP 489 DI 10.1111/j.1365-2966.2009.14539.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431QS UT WOS:000265078700060 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI Turanoceratops tardabilis-the first ceratopsid dinosaur from Asia SO NATURWISSENSCHAFTEN LA English DT Article DE Dinosauria; Ceratopsidae; Cretaceous; Asia ID HORNED DINOSAUR; NEOCERATOPSIA; EVOLUTION; SKULL AB Turanoceratops tardabilis from the Upper Cretaceous (Turonian) Bissekty Formation of Dzharakuduk, Uzbekistan, represents the first definite ceratopsid dinosaur recorded from Asia. Reexamination of the original and study of newly collected material indicate that Turanoceratops has well-developed supraorbital horns and apparently lacks a nasal horn. Turanoceratops is more derived than the more or less coeval Zuniceratops from the Moreno Hill Formation of New Mexico in the presence of double-rooted teeth and of two or three teeth in each vertical dental file. C1 [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Averianov, A (reprint author), Russian Acad Sci, Inst Zool, Univ Skaya Nab 1, St Petersburg 199034, Russia. EM suesh@si.edu; lepus@zin.ru RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, 0207004]; National Geographic Society [5901-97, 6281-98]; US Civilian Research and Development Foundation [RUB1-2860-ST-07] FX Fieldwork for this study was funded by grants from the National Science Foundation (EAR-9804771 and 0207004) and National Geographic Society (5901-97 and 6281-98) to J. D. Archibald and H.-D. S. and US Civilian Research and Development Foundation grant RUB1-2860-ST-07 to A. A. and J. D. Archibald. We thank the National Academy of Sciences of Uzbekistan, especially D. A. Azimov, director of the Institute of Zoology, for continued collaboration and assistance. M. J. Ryan and an anonymous reviewer provided helpful suggestions on a draft of the manuscript. NR 28 TC 20 Z9 21 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD MAY PY 2009 VL 96 IS 5 BP 645 EP 652 DI 10.1007/s00114-009-0518-9 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 430NA UT WOS:000264994600012 PM 19277598 ER PT J AU Paine, CET Harms, KE AF Paine, C. E. Timothy Harms, Kyle E. TI Quantifying the effects of seed arrival and environmental conditions on tropical seedling community structure SO OECOLOGIA LA English DT Article DE Community assembly; Dispersal; Niche differentiation; Seed addition; Variance partitioning ID RAIN-FOREST; RECRUITMENT LIMITATION; NEOTROPICAL FOREST; SPECIES ABUNDANCE; TREE SEEDLINGS; NEUTRAL THEORY; AMAZONIAN FORESTS; WOODY-PLANTS; DIVERSITY; BIODIVERSITY AB Though it is recognized that both stochastic and deterministic processes structure all communities, empirical assessments of their relative importance are rare, particularly within any single community. In this paper, we quantify the dynamic effects of dispersal assembly and niche assembly on the seedling layer in a diverse neotropical rain forest. The two theories make divergent predictions regarding the roles of seed arrival and environmental heterogeneity in generating community structure. Put simply, dispersal assembly posits that the stochasticity inherent to seed arrival structures communities, whereas niche assembly suggests that heterogeneity in post-dispersal environmental conditions is more important. We experimentally sowed 15,132 seeds of eight tree species at varying levels of density and diversity. Every six months we censused the seedlings that germinated and assessed the abiotic and biotic conditions of each plot. We assessed the density, diversity, and species composition of three nested subsets of the seedling layer: seedlings germinated from sown seeds, all seedlings germinated between July 2003 and 2004, and all woody seedlings. We partitioned the variance in density and diversity of each subset of the seedling layer into components representing seed-addition treatments and environmental conditions at 6- to 12-month intervals. Seed additions initially explained more variance in the density and diversity than did environmental heterogeneity for seven of eight sown species, but explained little variance in the density or diversity of the entire seedling layer. Species composition was better explained by seed-addition treatments than by environmental heterogeneity for all three subsets and in all time periods. Nevertheless, the variance in community structure explained by seed-addition treatments declined over the two years following germination, presaging shifts in the relative importance of dispersal assembly and niche assembly. Our study quantifies how dispersal assembly and niche assembly may vary among the components of an ecological community and shift dynamically through time. C1 [Paine, C. E. Timothy; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Panama. RP Paine, CET (reprint author), UMR EcoFoG, ENGREF, Campus Agron,BP 709, F-97379 Kourou, French Guiana. EM timothy.paine@ecofog.gf; kharms@lsu.edu RI Paine, C. E. Timothy/G-9961-2011 FU Organization of American States LASPAU; LSU Biology Graduate Student Association; LSU Board of Regents; National Science Foundation [DEB 0614044] FX We thank John Terborgh for his generosity in support of this project and in sharing unpublished data with us. Cecilia Carrasco, Christina Georghiou, Nataly Hidalgo, Armando Mendoza, Kristen Schmitt and Pamela Weisenhorn tagged and measured thousands of seedlings. Patricia Alvarez- Loayza identiWed endless seedlings and contributed to the reference collections. Discussions with Jane Carlson, Jonathan Myers and Adriana Bravo strengthened the manuscript. Peru's National Institute of Natural Resources ( INRENA) granted us permission to conduct research in Manu National Park. This research was supported through an Organization of American States LASPAU fellowship, the LSU Biology Graduate Student Association ( BioGrads), and a LSU Board of Regents Fellowship to CETP, as well as a National Science Foundation grant ( DEB 0614044) to KEH. The experiments performed in this study comply with the current laws of Peru, where they were performed. NR 61 TC 24 Z9 28 U1 1 U2 36 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAY PY 2009 VL 160 IS 1 BP 139 EP 150 DI 10.1007/s00442-008-1269-6 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 431YK UT WOS:000265100500014 PM 19142667 ER PT J AU Hetzinger, S Halfar, J Kronz, A Steneck, RS Adey, W Lebednik, PA Schone, BR AF Hetzinger, Steffen Halfar, Jochen Kronz, Andreas Steneck, Robert S. Adey, Walter Lebednik, Phillip A. Schoene, Bernd R. TI HIGH-RESOLUTION MG/CA RATIOS IN A CORALLINE RED ALGA AS A PROXY FOR BERING SEA TEMPERATURE VARIATIONS FROM 1902 TO 1967 SO PALAIOS LA English DT Article ID ELECTRON-MICROPROBE; CLIMATE; GROWTH; RECONSTRUCTION; CENTURIES AB We present the first continuous, high-resolution record of Mg/Ca variations within an encrusting coralline red alga, Clathromorphum nereostratum, from Amchitka Island, Aleutian Islands. Mg/Ca ratios of individual growth increments were analyzed by measuring a single-point, electron-microprobe transect, yielding a resolution of similar to 15 samples/year and a 65-year record (1902-1967) of variations. Results show that Mg/Ca ratios in the high-Mg calcite algal framework display pronounced annual cyclicity and archive late spring-late fall sea-surface temperatures (SST) corresponding to the main season of algal growth. Mg/Ca values correlate well to local SST, as well as to an air temperature record from the same region. High spatial correlation to large-scale SST variability in the subarctic North Pacific is observed, with patterns of strongest correlation following the direction of major oceanographic features that play a key role in the exchange of water masses between the North Pacific and the Bering Sea. Our data correlate well with a shorter Mg/Ca record from a second site, corroborating the ability of the alga to reliably record regional environmental signals. In addition, Mg/Ca ratios relate well to a 29-year delta(18)O time series measured on the same sample, providing additional support for the use of Mg in coralline red algae as a paleotemperature proxy that, unlike algal-delta(18)O, is not influenced by salinity fluctuations. Moreover, electron microprobe-based analysis enables higher sampling resolution and faster analysis, thus providing a promising approach for future studies of longer C. nereostratum records and applications to other coralline species. C1 [Hetzinger, Steffen; Halfar, Jochen] Univ Toronto, Dept Chem & Phys Sci, Mississauga, ON L5L 1C6, Canada. [Kronz, Andreas] Univ Gottingen, Geowissensch Zentrum, D-3400 Gottingen, Germany. [Steneck, Robert S.] Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. [Adey, Walter] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Lebednik, Phillip A.] LFR Inc, Ecosyst Serv Grp, Emeryville, CA USA. [Schoene, Bernd R.] Johannes Gutenberg Univ Mainz, Dept Appl & Analyt Paleontol, Inst Geosci, Mainz, Germany. RP Hetzinger, S (reprint author), Univ Toronto, Dept Chem & Phys Sci, Mississauga, ON L5L 1C6, Canada. EM steffen.hetzinger@utoronto.ca RI Schone, Bernd/B-6294-2011; Adey, Walter/G-2858-2011; Halfar, Jochen/C-7317-2014; Hetzinger, Steffen/B-5778-2016 FU Alexander von Humboldt Foundation; Deutsche Forschungsgemeinschaft [HA 3238/2-1. 2-2]; Natural Sciences and Engineering Research Council of Canada FX We thank Carolyn Winsborough for lab assistance and M. Joachimski for assistance with oxygen isotope analysis. The sample AM-KR-80 8-69-14B (Amchitka Island) was kindly provided by the U.S. National Herbarium of the Smithsonian Institution, Washington D.C. David W. Lea and Werner Piller provided very helpful comments that greatly improved the clarity of the manuscript. This research was funded by the Alexander von Humboldt Foundation (Feodor Lynen Fellowship to S.H.), the Deutsche Forschungsgemeinschaft (grant HA 3238/2-1. 2-2 to J.H. and A.K.), and a Natural Sciences and Engineering Research Council of Canada Discovery Grant to J.H. NR 40 TC 26 Z9 27 U1 4 U2 26 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 0883-1351 J9 PALAIOS JI Palaios PD MAY-JUN PY 2009 VL 24 IS 5-6 BP 406 EP 412 DI 10.2110/palo.2008.p08-116r PG 7 WC Geology; Paleontology SC Geology; Paleontology GA 454UE UT WOS:000266707400016 ER PT J AU Klein, M Hohensee, M Xiao, Y Kalra, R Phillips, DF Walsworth, RL AF Klein, M. Hohensee, M. Xiao, Y. Kalra, R. Phillips, D. F. Walsworth, R. L. TI Slow-light dynamics from electromagnetically-induced-transparency spectra SO PHYSICAL REVIEW A LA English DT Article DE optical pumping; self-induced transparency; slow light ID POLARITONS AB We show how slow-light pulse delays in realistic electromagnetically-induced-transparency (EIT) media can be determined directly from static transmission spectra. Using only the measured EIT linewidth and off-resonant transmission, the absolute delay of a slow-light pulse in an optically thick, power-broadened medium can be simply and accurately determined, while capturing more complex optical pumping behavior. C1 [Klein, M.; Hohensee, M.; Xiao, Y.; Kalra, R.; Phillips, D. F.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Klein, M.; Hohensee, M.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kalra, R.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Klein, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Hohensee, Michael/0000-0002-8106-4502 NR 27 TC 7 Z9 8 U1 3 U2 3 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 MAY PY 2009 VL 79 IS 5 AR 053833 DI 10.1103/PhysRevA.79.053833 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 451WF UT WOS:000266500900203 ER PT J AU Hohensee, MA Lehnert, R Phillips, DF Walsworth, RL AF Hohensee, Michael A. Lehnert, Ralf Phillips, David F. Walsworth, Ronald L. TI Particle-Accelerator Constraints on Isotropic Modifications of the Speed of Light SO PHYSICAL REVIEW LETTERS LA English DT Article ID LORENTZ VIOLATION; STANDARD MODEL; RADIATION; SPECTRUM; GRAVITY; RAYS; TEV; CPT AB The absence of vacuum Cherenkov radiation for 104.5 GeV electrons and positrons at the LEP collider at CERN combined with the observed stability of 300 GeV photons at the Tevatron constrains deviations of the speed of light relative to the maximal attainable speed of electrons. Within the standard-model extension, the limit -5.8 x 10(-12) <= (kappa) over tilde (tr) - 4/3c(e)(00) <= 1.2 x 10(-11) is extracted, which sharpens previous bounds by more than 3 orders of magnitude. The potential for further refinements of this limit with terrestrial experiments and astrophysical observations is discussed. C1 [Hohensee, Michael A.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lehnert, Ralf] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Lehnert, Ralf] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hohensee, MA (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. OI Hohensee, Michael/0000-0002-8106-4502 FU National Science Foundation; European Commission [MOIF-CT-2005-008687] FX The authors thank B. Altschul for helpful comments as this work developed, and F. R. Klinkhamer and M. Schreck for useful discussions. This work is supported in part by the National Science Foundation and by the European Commission under Grant No. MOIF-CT-2005-008687. NR 50 TC 63 Z9 63 U1 0 U2 1 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 MAY 1 PY 2009 VL 102 IS 17 AR 170402 DI 10.1103/PhysRevLett.102.170402 PG 4 WC Physics, Multidisciplinary SC Physics GA 443ZC UT WOS:000265948300002 PM 19518765 ER PT J AU Denevi, BW Robinson, MS Solomon, SC Murchie, SL Blewett, DT Domingue, DL McCoy, TJ Ernst, CM Head, JW Watters, TR Chabot, NL AF Denevi, Brett W. Robinson, Mark S. Solomon, Sean C. Murchie, Scott L. Blewett, David T. Domingue, Deborah L. McCoy, Timothy J. Ernst, Carolyn M. Head, James W. Watters, Thomas R. Chabot, Nancy L. TI The Evolution of Mercury's Crust: A Global Perspective from MESSENGER SO SCIENCE LA English DT Article ID CRATERING RECORD; VOLCANISM; FLYBY; MOON; REFLECTANCE; MARINER-10; REGOLITH; MAP AB Mapping the distribution and extent of major terrain types on a planet's surface helps to constrain the origin and evolution of its crust. Together, MESSENGER and Mariner 10 observations of Mercury now provide a near-global look at the planet, revealing lateral and vertical heterogeneities in the color and thus composition of Mercury's crust. Smooth plains cover approximately 40% of the surface, and evidence for the volcanic origin of large expanses of plains suggests that a substantial portion of the crust originated volcanically. A low-reflectance, relatively blue component affects at least 15% of the surface and is concentrated in crater and basin ejecta. Its spectral characteristics and likely origin at depth are consistent with its apparent excavation from a lower crust or upper mantle enriched in iron-and titanium-bearing oxides. C1 [Denevi, Brett W.; Robinson, Mark S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Murchie, Scott L.; Blewett, David T.; Domingue, Deborah L.; Ernst, Carolyn M.; Chabot, Nancy L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Denevi, BW (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. EM bdenevi@ser.asu.edu RI Ernst, Carolyn/I-4902-2012; Blewett, David/I-4904-2012; Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015; Chabot, Nancy/F-5384-2015 OI Blewett, David/0000-0002-9241-6358; Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751; Chabot, Nancy/0000-0001-8628-3176 FU Johns Hopkins University Applied Physics Laboratory [NAS5-97271]; Carnegie Institution of Washington [NASW-00002] FX We gratefully acknowledge the MESSENGER engineers and technical support team. N. Laslo, H. Kang, R. Vaughan, A. Harch, R. Shelton, and A. Berman designed the imaging sequences used here. S. Turner, K. Becker, and C. Hash contributed to data calibration and processing. The MESSENGER project is supported by the NASA Discovery Program under contracts NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 37 TC 117 Z9 117 U1 2 U2 18 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 MAY 1 PY 2009 VL 324 IS 5927 BP 613 EP 618 DI 10.1126/science.1172226 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 439DW UT WOS:000265608800036 PM 19407196 ER PT J AU Watters, TR Head, JW Solomon, SC Robinson, MS Chapman, CR Denevi, BW Fassett, CI Murchie, SL Strom, RG AF Watters, Thomas R. Head, James W. Solomon, Sean C. Robinson, Mark S. Chapman, Clark R. Denevi, Brett W. Fassett, Caleb I. Murchie, Scott L. Strom, Robert G. TI Evolution of the Rembrandt Impact Basin on Mercury SO SCIENCE LA English DT Article ID CRATERING RECORD; CALORIS BASIN; FLYBY; TECTONICS; VOLCANISM; MESSENGER; SLIP AB MESSENGER's second Mercury flyby revealed a similar to 715-kilometer-diameter impact basin, the second-largest well-preserved basin-scale impact structure known on the planet. The Rembrandt basin is comparable in age to the Caloris basin, is partially flooded by volcanic plains, and displays a unique wheel-and-spoke-like pattern of basin-radial and basin-concentric wrinkle ridges and graben. Stratigraphic relations indicate a multistaged infilling and deformational history involving successive or overlapping phases of contractional and extensional deformation. The youngest deformation of the basin involved the formation of a similar to 1000-kilometer-long lobate scarp, a product of the global cooling and contraction of Mercury. C1 [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Head, James W.; Fassett, Caleb I.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Robinson, Mark S.; Denevi, Brett W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85251 USA. [Chapman, Clark R.] SW Res Inst, Boulder, CO 80302 USA. [Murchie, Scott L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Strom, Robert G.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu RI Denevi, Brett/I-6502-2012; Murchie, Scott/E-8030-2015; OI Denevi, Brett/0000-0001-7837-6663; Murchie, Scott/0000-0002-1616-8751; Fassett, Caleb/0000-0001-9155-3804 FU Carnegie Institution of Washington [NASW-00002]; Johns Hopkins University Applied Physics Laboratory [NAS5-97271]; NASA [NNX07AR60G] FX We are grateful to the MESSENGER engineers and technical support personnel. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to Johns Hopkins University Applied Physics Laboratory. This work is also supported by NASA grant NNX07AR60G. NR 23 TC 26 Z9 26 U1 2 U2 3 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 MAY 1 PY 2009 VL 324 IS 5927 BP 618 EP 621 DI 10.1126/science.1172109 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 439DW UT WOS:000265608800037 PM 19407197 ER PT J AU Clough, GW AF Clough, G. Wayne TI Big Snakes 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 MAY PY 2009 VL 40 IS 2 BP 22 EP 22 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 437AX UT WOS:000265459100012 ER PT J AU David, J AF David, James TI What should nations reveal about their spying from space? An examination of the US experience SO SPACE POLICY LA English DT Article AB Revelation of the details of countries' space-based reconnaissance programs was unusual until the end of the Cold War, despite debates on the subject within the US government. Since then - and in contrast to Russia - the USA has been more open about its spying activities. This article charts the history of declassification in the USA from the Eisenhower Administration to that of G.W. Bush. It discusses issues such as the need to ensure freedom of space for the operation of spy satellites, gaining public acceptance of space-based reconnaissance by demonstrating the civil uses of such photography, and tradeoffs between revealing one's capabilities and letting others know how closely their actions can be observed. Published by Elsevier Ltd. C1 Smithsonian Inst, Natl Air & Space Museum DSH MRC 311, Washington, DC 20013 USA. RP David, J (reprint author), Smithsonian Inst, Natl Air & Space Museum DSH MRC 311, POB 37012, Washington, DC 20013 USA. EM davidj@si.edu NR 40 TC 0 Z9 0 U1 0 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 J9 SPACE POLICY JI Space Policy PD MAY PY 2009 VL 25 IS 2 BP 117 EP 127 DI 10.1016/j.spacepol.2009.02.009 PG 11 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA 465HO UT WOS:000267573600009 ER PT J AU Medeiros, MJ Davis, D Howarth, FG Gillespie, R AF Medeiros, Matthew J. Davis, Don Howarth, Francis G. Gillespie, Rosemary TI Evolution of cave living in Hawaiian Schrankia (Lepidoptera: Noctuidae) with description of a remarkable new cave species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE adaptive shift; biogeography; exaptation; flightless; speleology; synonymy; troglobite ID HYLAEUS BEES HYMENOPTERA; LAVA TUBES; PHYLOGENETIC INFERENCE; CANARY-ISLANDS; MIXED MODELS; SPECIATION; MITOCHONDRIAL; GENUS; NUCLEAR; ARTHROPODS AB Although temperate cave-adapted fauna may evolve as a result of climatic change, tropical cave dwellers probably colonize caves through adaptive shifts to exploit new resources. The founding populations may have traits that make colonization of underground spaces even more likely. To investigate the process of cave adaptation and the number of times that flightlessness has evolved in a group of reportedly flightless Hawaiian cave moths, we tested the flight ability of 54 Schrankia individuals from seven caves on two islands. Several caves on one island were sampled because separate caves could have been colonized by underground connections after flightlessness had already evolved. A phylogeny based on approximately 1500 bp of mtDNA and nDNA showed that Schrankia howarthi sp. nov. invaded caves on two islands, Maui and Hawaii. Cave-adapted adults are not consistently flightless but instead are polymorphic for flight ability. Although the new species appears well suited to underground living, some individuals were found living above ground as well. These individuals, which are capable of flight, suggest that this normally cave-limited species is able to colonize other, geographically separated caves via above-ground dispersal. This is the first example of an apparently cave-adapted species that occurs in caves on two separate Hawaiian islands. A revision of the other Hawaiian Schrankia is presented, revealing that Schrankia simplex, Schrankia oxygramma, Schrankia sarothrura, and Schrankia arrhecta are all junior synonyms of Schrankia altivolans. (C) 2009 The Linnean Society of London, Zoological Journal of the Linnean Society, 2009, 156, 114-139. C1 [Medeiros, Matthew J.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Davis, Don] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Howarth, Francis G.] Bernice P Bishop Museum, Dept Nat Sci, Honolulu, HI 96817 USA. [Gillespie, Rosemary] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Div Organisms & Environm, Berkeley, CA 94720 USA. RP Medeiros, MJ (reprint author), Univ Calif Berkeley, Dept Integrat Biol, 3060 Valley Life Sci Bldg, Berkeley, CA 94720 USA. EM m_j_m@berkeley.edu OI Howarth, Francis/0000-0002-6926-0455 FU Society for Integrative and Comparative Biology, Sigma Xi; Smithsonian Institution Research Opportunity Fund; University of California, Berkeley; Dept of Integrative Biology, University of California; Xerces Society; National Speleological Society; Cave Research Foundation; Margaret C. Walker Fund for teaching and research in systematic entomology FX We thank Jordana Anderson, Miguel Arnedo, Sam Aruch, Sara Backowski, Randy Bartlett, Kalena Blakemore, Jahkotta Burrell, Ring CardE, Idelle Cooper, Mignon Davis, Robert Dudley, Ric El;hard, Melody Euaparadorn, Scott Fay, Betsy GagnE and the Hawaii DOFAW, Jon Giffin, Will Haines, Ryan Hill, Martin Honey, Kevin Jenkins, Raina Kaholoa'a, Adam LeachE, David Medeiros, Steve Montgomery, Pete Oboyski, Kevin Padian, Bonnie Ploger, Jerry Powell, Kathlyn Richardson, Summer Roper, Harry A. Schick, Michal Shuldman, Wayne Souza and the staff at Kokee State Park, Fred Stone, Kevin Tuck, and the staffs of Haleakala National Park and Hawaii Volcanoes National Park for help with collecting, logistics, and advice. Photographic assistance was provided by John Steiner and the late Victor Kranz, Smithsonian Photographic Services, Susan Braden, formerly of the Smithsonian Scanning Electron Microscope Laboratory, H. Hoch, Museum fur Naturkunde, Berlin, (Fig. 2A); and William Mull, Volcano, Hawaii (Fig. 2B-D). We also thank Patricia Gentili-Poole, Department of Entomology, Smithsonian Institution, for her assistance with photographs and preparing the plates for publication. Line illustrations were by Young Sohn, Department of Entomology, Smithsonian Institution. This research was supported in part by: Society for Integrative and Comparative Biology, Sigma Xi, Smithsonian Institution Research Opportunity Fund, University of California, Berkeley, Dept of Integrative Biology, University of California Pacific Rim Research Project, Xerces Society, National Speleological Society, Cave Research Foundation, Margaret C. Walker Fund for teaching and research in systematic entomology. The work presented here represents a portion of M. J. Medeiros's PhD dissertation research at the University of California, Berkeley. NR 55 TC 10 Z9 11 U1 1 U2 8 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2009 VL 156 IS 1 BP 114 EP 139 DI 10.1111/j.1096-3642.2008.00477.x PG 26 WC Zoology SC Zoology GA 435YB UT WOS:000265378100004 ER PT J AU Revnivtsev, M Sazonov, S Churazov, E Forman, W Vikhlinin, A Sunyaev, R AF Revnivtsev, M. Sazonov, S. Churazov, E. Forman, W. Vikhlinin, A. Sunyaev, R. TI Discrete sources as the origin of the Galactic X-ray ridge emission SO NATURE LA English DT Article ID IRON LINE; CHANDRA; GALAXY; ASCA; EXTINCTION; PLANE; VIEW AB An unresolved X-ray glow (at energies above a few kiloelectron-volts) was discovered about 25 years ago and found to be coincident with the Galactic disk-the Galactic ridge X-ray emission(1,2). This emission(3-10) has a spectrum characteristic of a similar to 10(8) K optically thin thermal plasma, with a prominent iron emission line at 6.7 keV. The gravitational well of the Galactic disk, however, is far too shallow to confine such a hot interstellar medium; instead, it would flow away at a velocity of a few thousand kilometres per second, exceeding the speed of sound in the gas. To replenish the energy losses requires a source of 10(43) erg s(-1), exceeding by orders of magnitude all plausible energy sources in the Milky Way(11). An alternative is that the hot plasma is bound to a multitude of faint sources(12), which is supported by the recently observed similarities in the X-ray and near-infrared surface brightness distributions(13,14) (the latter traces the Galactic stellar distribution). Here we report that at energies of similar to 6-7 keV, more than 80 per cent of the seemingly diffuse X-ray emission is resolved into discrete sources, probably accreting white dwarfs and coronally active stars. C1 [Revnivtsev, M.] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Revnivtsev, M.; Sazonov, S.; Churazov, E.; Vikhlinin, A.; Sunyaev, R.] Space Res Inst, Moscow 117997, Russia. [Sazonov, S.; Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Forman, W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Revnivtsev, M (reprint author), Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. EM mikej@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013; OI Forman, William/0000-0002-9478-1682 FU DFG Cluster of Excellence; NASA Chandra [GO8-9132A]; Russian Academy of Sciences [OFH-17]; RFFI [07-02-01004, 07-02-00961] FX M. R. thanks M. Markevitch for his help with the Chandra instrumental background. This research was supported by the DFG Cluster of Excellence "Origin and Structure of the Universe'', by NASA Chandra grant GO8-9132A, by the OFH-17 programme of the Russian Academy of Sciences, and by grants RFFI 07-02-01004 and RFFI 07-02-00961. NR 28 TC 115 Z9 115 U1 1 U2 3 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 APR 30 PY 2009 VL 458 IS 7242 BP 1142 EP 1144 DI 10.1038/nature07946 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 441FL UT WOS:000265754600041 PM 19407795 ER PT J AU Solis, MA AF Solis, M. A. TI EUGENE G. MUNROE (8 SEPTEMBER 1919-31 MAY 2008) OBITUARY SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Biographical-Item C1 USDA, SEL, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Solis, MA (reprint author), USDA, SEL, Smithsonian Inst, Natl Museum Nat Hist, POB 37012,E-517,MRC 168, Washington, DC 20013 USA. EM alma.solis@ars.usda.gov NR 0 TC 0 Z9 0 U1 0 U2 0 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD APR 29 PY 2009 VL 63 IS 1 BP 52 EP 57 PG 6 WC Entomology SC Entomology GA 441XP UT WOS:000265804100008 ER PT J AU Lopatin, IK Konstantinov, AS AF Lopatin, I. K. Konstantinov, A. S. TI New genera and species of leaf beetles (Coleoptera: Chrysomelidae) from China and South Korea SO ZOOTAXA LA English DT Article DE Leaf beetles; Chrysomelidae; new species; new genera; skunk vine; China; South Korea AB Two new genera from China (Taumaceroides Lopatin and Yunnaniata Lopatin) and 11 new species (Smaragdina quadrimaculata Lopatin, S. oblongum Lopatin, Hyphaenia volkovitshi Lopatin, Arthrotus daliensis Lopatin, Taumaceroides sinicus Lopatin, Yunnaniata konstantinovi Lopatin, Calomicrus yunnanus Lopatin, C. minutissimus Lopatin, Hermaeophaga belkadavi Konstantinov, H. dali Konstantinov from China, and H. korotyaevi Konstantinov from South Korea) are described and illustrated. A key to Hermaeophaga species of Eurasia is presented. Since Hermaeophaga dali was collected feeding on Paederia foetida L. (Rubiaceae), which is an invasive noxious weed in the United States, this species has potential as a biological control agent of this weed. C1 [Lopatin, I. K.] Byelorussian State Univ, Dept Zool, Minsk, Byelarus. [Konstantinov, A. S.] ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,Natl Museum Nat Hist,MRC 16, Washington, DC 20013 USA. RP Lopatin, IK (reprint author), Byelorussian State Univ, Dept Zool, Minsk, Byelarus. EM lopatinik@gmail.com; alex.konstantinov@ars.usda.gov NR 14 TC 3 Z9 5 U1 2 U2 2 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 APR 27 PY 2009 IS 2083 BP 1 EP 18 PG 18 WC Zoology SC Zoology GA 438SM UT WOS:000265575700001 ER PT J AU Reding, DM Foster, JT James, HF Pratt, HD Fleischer, RC AF Reding, Dawn M. Foster, Jeffrey T. James, Helen F. Pratt, H. Douglas Fleischer, Robert C. TI Convergent evolution of 'creepers' in the Hawaiian honeycreeper radiation SO BIOLOGY LETTERS LA English DT Article DE ecological convergence; convergent evolution; Hawaiian honeycreepers; mitochondrial DNA introgression; hybridization; adaptive radiation AB Natural selection plays a fundamental role in the ecological theory of adaptive radiation. A prediction of this theory is the convergent evolution of traits in lineages experiencing similar environments. The Hawaiian honeycreepers are a spectacular example of adaptive radiation and may demonstrate convergence, but uncertainty about phylogenetic relationships within the group has made it difficult to assess such evolutionary patterns. We examine the phylogenetic relationships of the Hawaii creeper (Oreomystis mana), a bird that in a suite of morphological, ecological and behavioural traits closely resembles the Kauai creeper (Oreomystis bairdi), but whose mitochondrial DNA (mtDNA) and osteology suggest a relationship with the amakihis (Hemignathus in part) and akepas (Loxops). We analysed nuclear DNA sequence data from 11 relevant honeycreeper taxa and one outgroup to test whether the character contradiction results from historical hybridization and mtDNA introgression, or convergent evolution. We found no evidence of past hybridization, a phenomenon that remains undocumented in Hawaiian honeycreepers, and confirmed mtDNA and osteological evidence that the Hawaii creeper is most closely related to the amakihis and akepas. Thus, the morphological, ecological and behavioural similarities between the evolutionarily distant Hawaii and Kauai creepers represent an extreme example of convergent evolution and demonstrate how natural selection can lead to repeatable evolutionary outcomes. C1 [Pratt, H. Douglas] N Carolina State Museum Nat Sci, Raleigh, NC 27601 USA. [James, Helen F.] Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA. [Foster, Jeffrey T.] No Arizona Univ, Ctr Microbial Genet & Genom, Flagstaff, AZ 86011 USA. [Reding, Dawn M.] Univ Hawaii, Dept Zool, Honolulu, HI 96822 USA. [Reding, Dawn M.; Foster, Jeffrey T.; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Reding, Dawn M.; Foster, Jeffrey T.; Fleischer, Robert C.] Smithsonian Inst, Natl Museum Nat Hist, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Reding, DM (reprint author), Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. EM reding@iastate.edu OI Foster, Jeffrey/0000-0001-8235-8564 FU NSF [DEB-0083944, DEB-0643291]; Smithsonian Institution's Center for Conservation and Evolutionary Genetics FX We thank T. Pratt, C. Atkinson, S. Conant, A. McClung, P. Hart, D. Duffy and B. Woodworth for providing samples for analysis, and M. Haynie, C. McIntosh and the EEOB Department at Iowa State University for logistic support. NSF DEB-0083944, DEB-0643291 and the Smithsonian Institution's Center for Conservation and Evolutionary Genetics provided funding. NR 24 TC 13 Z9 14 U1 2 U2 52 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD APR 23 PY 2009 VL 5 IS 2 BP 221 EP 224 DI 10.1098/rsbl.2008.0589 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 421PX UT WOS:000264371900024 PM 19087923 ER PT J AU Johnson, GD Paxton, JR Sutton, TT Satoh, TP Sado, T Nishida, M Miya, M AF Johnson, G. David Paxton, John R. Sutton, Tracey T. Satoh, Takashi P. Sado, Tetsuya Nishida, Mutsumi Miya, Masaki TI Deep-sea mystery solved: astonishing larval transformations and extreme sexual dimorphism unite three fish families SO BIOLOGY LETTERS LA English DT Article DE Cetomimidae; Megalomycteridae; Mirapinnidae; ontogenetic transformation; sexual dimorphism; whalefishes AB The oceanic bathypelagic realm (1000-4000 m) is a nutrient-poor habitat. Most fishes living there have pelagic larvae using the rich waters of the upper 200 m. Morphological and behavioural specializations necessary to occupy such contrasting environments have resulted in remarkable developmental changes and life-history strategies. We resolve a long-standing biological and taxonomic conundrum by documenting the most extreme example of ontogenetic metamorphoses and sexual dimorphism in vertebrates. Based on morphology and mitogenomic sequence data, we show that fishes currently assigned to three families with greatly differing morphologies, Mirapinnidae (tapetails), Megalomycteridae (bignose fishes) and Cetomimidae (whalefishes), are larvae, males and females, respectively, of a single family Cetomimidae. Morphological transformations involve dramatic changes in the skeleton, most spectacularly in the head, and are correlated with distinctly different feeding mechanisms. Larvae have small, upturned mouths and gorge on copepods. Females have huge gapes with long, horizontal jaws and specialized gill arches allowing them to capture larger prey. Males cease feeding, lose their stomach and oesophagus, and apparently convert the energy from the bolus of copepods found in all transforming males to a massive liver that supports them throughout adult life. C1 [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. [Paxton, John R.] Australian Museum, Sydney, NSW 2010, Australia. [Sutton, Tracey T.] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Satoh, Takashi P.; Nishida, Mutsumi] Univ Tokyo, Ocean Res Inst, Nakano Ku, Tokyo 1648639, Japan. [Sado, Tetsuya; Miya, Masaki] Nat Hist Museum & Inst, Chuo Ku, Chiba 2668682, Japan. RP Johnson, GD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. EM johnsond@si.edu NR 13 TC 30 Z9 32 U1 0 U2 19 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD APR 23 PY 2009 VL 5 IS 2 BP 235 EP 239 DI 10.1098/rsbl.2008.0722 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 421PX UT WOS:000264371900028 PM 19158027 ER PT J AU Roy, K Hunt, G Jablonski, D Krug, AZ Valentine, JW AF Roy, Kaustuv Hunt, Gene Jablonski, David Krug, Andrew Z. Valentine, James W. TI A macroevolutionary perspective on species range limits SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE geographic range limits; macroevolution; biogeography ID LATITUDINAL DIVERSITY GRADIENTS; GEOGRAPHIC RANGE; PHYLOGENETIC STRUCTURE; ECOLOGICAL COMMUNITIES; CRETACEOUS MOLLUSKS; MARINE BIVALVES; PATTERNS; EVOLUTIONARY; HERITABILITY; SPECIATION AB Understanding the factors that determine the geographic range limits of species is important for many questions in ecology, evolution and conservation biology. These limits arise from complex interactions among ecology and dispersal ability of species and the physical environment, but many of the underlying traits can be conserved among related species and clades. Thus, the range limits of species are likely to be influenced by their macroevolutionary history. Using palaeontological and biogeographic data for marine bivalves, we find that the range limits of genera are significantly related to their constituent species richness, but the effects of age are weak and inconsistent. In addition, we find a significant phylogenetic signal in the range limits at both genus and family levels, although the strength of this effect shows interoceanic variation. This phylogenetic conservatism of range limits gives rise to an evolutionary pattern where wide-ranging lineages have clusters of species within the biogeographic provinces, with a few extending across major boundaries. C1 [Roy, Kaustuv] Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. [Hunt, Gene] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. [Jablonski, David; Krug, Andrew Z.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Valentine, James W.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Roy, K (reprint author), Univ Calif San Diego, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. EM kroy@ucsd.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 FU NASA FX We thank K. J. Gaston for the invitation to contribute to this special issue and two anonymous reviewers for their very insightful comments that improved the manuscript. This research was supported by a grant from the NASA. NR 88 TC 45 Z9 46 U1 3 U2 42 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD APR 22 PY 2009 VL 276 IS 1661 BP 1485 EP 1493 DI 10.1098/rspb.2008.1232 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 421IF UT WOS:000264351900013 PM 19324820 ER PT J AU Coe, MJ Schurch, M McBride, VA Corbet, RHD Townsend, LJ Udalski, A Galache, JL AF Coe, M. J. Schurch, M. McBride, V. A. Corbet, R. H. D. Townsend, L. J. Udalski, A. Galache, J. L. TI An X-ray and optical study of the new SMC X-ray binary pulsar system SXP7.92 and its probable optical counterpart, AzV285 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; X-rays: binaries ID SMALL-MAGELLANIC-CLOUD; SPACED DATA; CATALOG; LONG; SUPERGIANT; EMISSION AB Optical and X-ray observations are presented here of a newly reported X-ray transient system in the Small Magellanic Cloud (SMC) - SXP7.922. A detailed analysis of: the X-ray data reveal a coherent period of 7.9 s. A search through earlier X-ray observations of, the SMC reveal a previously Unknown earlier detection of this system. Follow-Up X-ray observations identified a new, transient source within the error circle of the previous observations. An optical counterpart. AzV285, is proposed which reveals clear evidence for a 36.8 d binary period. C1 [Coe, M. J.; Schurch, M.; McBride, V. A.; Townsend, L. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corbet, R. H. D.] Univ Maryland, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Coe, MJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM mjcoe@soton.ac.uk FU Polish MNiSW [N20303032/42-75] FX We are grateful to the referee for helpful comments and to file Swift team for scheduling, and supporting the follow-up observations. LJT acknowledges the support of a University of Southampton Mayflower Scholarship. The OGLE project is partially supported by the Polish MNiSW grant N20303032/42-75. NR 27 TC 4 Z9 4 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2009 VL 394 IS 4 BP 2191 EP 2196 DI 10.1111/j.1365-2966.2009.14501.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 452OD UT WOS:000266549600041 ER PT J AU Bryant, JJ Broderick, JW Johnston, HA Hunstead, RW Gaensler, BA De Breuck, C AF Bryant, J. J. Broderick, J. W. Johnston, H. A. Hunstead, R. W. Gaensler, B. A. De Breuck, C. TI A new search for distant radio galaxies in the Southern hemisphere - II. 2.2 mu m imaging SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies: active; galaxies: high-redshift; infrared: galaxies; radio continuum: galaxies ID K-Z RELATION; EIS-NVSS SURVEY; HIGH-REDSHIFT; ELLIPTIC GALAXIES; SKY SURVEY; SAMPLE DEFINITION; SPECTRUM; SUMSS; IMAGES; LUMINOSITY AB We have compiled a sample of 234 ultra-steep-spectrum (USS) selected radio sources in order to find high-redshift radio galaxies. The sample covers the declination range -40 degrees < delta < -30 degrees ill the overlap region between the 1400-MHz National Radio Astronomy Observatory (NRAO) Very Large Array (VLA) Sky Survey (NVSS), 408-MHz Revised Molonglo Reference Catalogue and the 843-MHz Sydney University Molonglo Sky survey (the MRCR-SUMSS sample). This is the second ill a;series of papers on the MRCR-SUMSS sample. and here we present the K-band (2.2 mu m) imaging off 73 of the sources primarily from the Magellan and the Analo-Australian Telescopes. We detect a counterpart to the radio source ill 93 per cent of the new K-band images which. along with previously published data. makes this the largest published sample of K-band counterparts to USS-selected radio galaxies. The location of the K-band identification has been compared to the features of the radio emission for (he double sources. We find that the identification is most likely to lie near the mid-point of the radio lobes rather than closer to the brighter lobe, making the centroid a less likely place to find the optical Counterpart. 79 per cent of the identifications are less than I arcsec from the radio lobe axis. These results differ front Studies of low-redshift radio samples where the environments are typically not nearly so dense and disturbed as those at high redshift. Ill contrast to some literature samples, we fired that the majority Of our sample shows no alignment between the near-infrared and radio axes. Several different morphologies of aligned structures are found and those that are aligned within 10 degrees are consistent with jet-induced still formation. The distribution and median value of the K-band magnitudes for the MRCR-SUMSS sample are found to be similar to several other USS-selected samples even through each sample has a very different median 1400MHz flux density. USS selection from a lower radio-frequency sample has not netted fainter K-band magnitudes, which may imply that the k-correction is not responsible for the effectiveness of USS selection. C1 [Bryant, J. J.; Broderick, J. W.; Johnston, H. A.; Hunstead, R. W.; Gaensler, B. A.] Univ Sydney, SifA, Sch Phys A29, Sydney, NSW 2006, Australia. [Gaensler, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. RP Bryant, JJ (reprint author), Univ Sydney, SifA, Sch Phys A29, Sydney, NSW 2006, Australia. EM jbryant@physics.usyd.edu.au RI Gaensler, Bryan/F-8655-2010 NR 59 TC 5 Z9 5 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 21 PY 2009 VL 394 IS 4 BP 2197 EP 2222 DI 10.1111/j.1365-2966.2009.14500.x PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 452OD UT WOS:000266549600042 ER PT J AU Smith, BD Yarnell, RA AF Smith, Bruce D. Yarnell, Richard A. TI Initial formation of an indigenous crop complex in eastern North America at 3800 BP SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE agriculture; archaeology; Chenopodium; domestication ID PLANT DOMESTICATION; CHENOPODIUM AB Although geneticists and archaeologists continue to make progress world-wide in documenting the time and place of the initial domestication of a growing number of plants and animals, far less is known regarding the critically important context of coalescence of various species into distinctive sets or complexes of domesticates in each of the world's 10 or more independent centers of agricultural origin. In this article, the initial emergence of a crop complex is described for one of the best-documented of these independent centers, eastern North America (ENA). Before 4000 B. P. there is no indication of a crop complex in ENA, only isolated evidence for single indigenous domesticate species. By 3800 B. P., however, at least 5 domesticated seed-bearing plants formed a coherent complex in the river valley corridors of ENA. Accelerator mass spectrometer radiocarbon dates and reanalysis of archaeobotanical assemblages from a short occupation of the Riverton Site in Illinois documents the contemporary cultivation at 3800 B. P. of domesticated bottle gourd (Lagenaria siceraria), marshelder (Iva annua var. macrocarpa), sunflower (Helianthus annuus var. macrocarpus), and 2 cultivated varieties of chenopod (Chenopodium berlandieri), as well as the possible cultivation of Cucurbita pepo squash and little barley (Hordeum pusillum). Rather than marking either an abrupt developmental break or a necessary response to population-packing or compressed resource catchments, the coalescence of an initial crop complex in ENA appears to reflect an integrated expansion and enhancement of preexisting hunting and gathering economies that took place within a context of stable long-term adaptation to resource-rich river valley settings. C1 [Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. [Yarnell, Richard A.] Univ N Carolina, Dept Anthropol, Chapel Hill, NC 27514 USA. [Yarnell, Richard A.] Univ N Carolina, Labs Archaeol, Chapel Hill, NC 27514 USA. RP Smith, BD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Archaeobiol Program, Washington, DC 20560 USA. EM smithb@si.edu NR 38 TC 43 Z9 44 U1 2 U2 21 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 APR 21 PY 2009 VL 106 IS 16 BP 6561 EP 6566 DI 10.1073/pnas.0901846106 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 437SI UT WOS:000265506800027 PM 19366669 ER PT J AU Posson-Brown, J Raychaudhury, S Forman, W Donnelly, RH Jones, C AF Posson-Brown, Jennifer Raychaudhury, Somak Forman, William Donnelly, R. Hank Jones, Christine TI CHANDRA OBSERVATIONS OF THE X-RAY POINT SOURCE POPULATION IN NGC 4636 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4636); X-rays: binaries; X-rays: galaxies ID EARLY-TYPE GALAXIES; GLOBULAR-CLUSTER SYSTEM; GROUP EVOLUTION MULTIWAVELENGTH; ACTIVE GALACTIC NUCLEUS; ELLIPTIC GALAXIES; DARK-MATTER; LUMINOSITY FUNCTION; CENTAURUS-A; BINARIES; NGC-4636 AB We present the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling similar to 193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, we detect 318 individual point sources. For our analysis, we use a subset of 277 detections with >= net 10 counts (a limiting luminosity of approximately 1.2 x 10(37) erg s(-1) in the 0.5-2 keV band, outside the central 1'.5 bright galaxy core). We present a radial distribution of the point sources. Between 1'.5 and 6' from the center, 25% of our sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% are low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6', background sources (AGN) will dominate the point sources. We explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, similar to 10% of the sources in each observation show significant short-term variability; we present an example light curve for a variable bright source. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope alpha = 1.14 +/- 0.03. We do not detect, but estimate an upper limit of similar to 4.5 x 10(37) erg s(-1) to the current X-ray luminosity of the historical supernova SN1939A. We find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1'.5 to 6' of the galaxy center, 48 of the 129 X-ray point sources (37%) with >= 10 net counts are matched with GC candidates. Since we expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, we find that similar to 70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. We do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10(37) erg s(-1) <= L(x) <= 1 x 10(38) erg s(-1). Finally, we present a color-color diagram based on ratios of X-ray flux rather than source counts, which yields a much tighter source distribution, and shows a large population of sources which are likely LMXBs and a small population of black hole candidates. C1 [Posson-Brown, Jennifer; Raychaudhury, Somak; Forman, William; Donnelly, R. Hank; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Donnelly, R. Hank] Ctr Naval Anal, Alexandria, VA 22311 USA. RP Posson-Brown, J (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM jpossonbrown@cfa.harvard.edu; somak@star.sr.bham.ac.uk; wforman@cfa.harvard.edu; cjones@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU NASA [NAS8-39073, NAS8-03060]; Chandra Science Center; Smithsonian Institution; University of Birmingham FX We thank Vinay Kashyap for helpful discussions on short-term source variability and the development of his extremely useful timevarvk IDL code. This work was supported by NASA contracts NAS8-39073 and NAS8-03060, the Chandra Science Center, the Smithsonian Institution, and the University of Birmingham. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. VizieR is a joint effort of CDS ( Centre de Donnees astronomiques de Strasbourg) and ESA-ESRIN ( Information Systems Division). NR 79 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1094 EP 1110 DI 10.1088/0004-637X/695/2/1094 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300029 ER PT J AU Kennedy, GM Kenyon, SJ AF Kennedy, Grant M. Kenyon, Scott J. TI STELLAR MASS DEPENDENT DISK DISPERSAL SO ASTROPHYSICAL JOURNAL LA English DT Review DE planetary systems: formation; planetary systems: protoplanetary disks; stars: formation; stars: pre-main sequence ID SCORPIUS OB ASSOCIATION; T-TAURI STARS; PRIMORDIAL BINARY POPULATION; SPITZER-SPACE-TELESCOPE; AURIGA MOLECULAR CLOUD; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DISKS; PLANET FORMATION; GIANT PLANETS AB We use published optical spectral and infrared (IR) excess data from nine young clusters and associations to study the stellar mass dependent dispersal of circumstellar disks. All clusters older than similar to 3 Myr show a decrease in disk fraction with increasing stellar mass for solar to higher mass stars. This result is significant at about the 1 sigma level in each cluster. For the complete set of clusters we reject the null hypothesis-that solar and intermediate-mass stars lose their disks at the same rate-with 95%-99.9% confidence. To interpret this behavior, we investigate the impact of grain growth, binary companions, and photoevaporation on the evolution of disk signatures. Changes in grain growth timescales at fixed disk temperature may explain why early-type stars with IR excesses appear to evolve faster than their later-type counterparts. Little evidence that binary companions affect disk evolution suggests that photoevaporation is the more likely mechanism for disk dispersal. A simple photoevaporation model provides a good fit to the observed disk fractions for solar and intermediate-mass stars. Although the current mass-dependent disk dispersal signal is not strong, larger and more complete samples of clusters with ages of 3-5 Myr can improve the significance and provide better tests of theoretical models. In addition, the orbits of extra-solar planets can constrain models of disk dispersal and migration. We suggest that the signature of stellar mass dependent disk dispersal due to photoevaporation may be present in the orbits of observed extra-solar planets. Planets orbiting hosts more massive than similar to 1.6 M-circle dot may have larger orbits because the disks in which they formed were dispersed before they could migrate. C1 [Kennedy, Grant M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kennedy, GM (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. EM grant@mso.anu.edu.au; kenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Kennedy, Grant/0000-0001-6831-7547 FU Australian Postgraduate Award; ANU Vice-Chancellor's Travel Grant; NASA [NAG5-13278]; TPF Foundation Science Program [NNG06GH25G] FX We thank Cathie Clarke, Charles Jenkins, and Eric Mamajek for helpful conversations, and the referee for a thorough review. G. K. thanks Mark Wyatt and the Cambridge IoA, and the Harvard-CfA, where a part of this study was carried out. This research was supported by an Australian Postgraduate Award and an ANU Vice-Chancellor's Travel Grant (GK), and the NASA Astrophysics Theory Program through grant NAG5-13278 and the TPF Foundation Science Program though grant NNG06GH25G (S. K.). This research has made use of the SIMBAD database and the VizieR catalog access tool, both operated at CDS, Strasbourg, France. It also makes use of data products from the Two Micron All Sky Survey (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 107 TC 47 Z9 47 U1 0 U2 1 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 APR 20 PY 2009 VL 695 IS 2 BP 1210 EP 1226 DI 10.1088/0004-637X/695/2/1210 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300039 ER PT J AU Novak, G Dotson, JL Li, H AF Novak, G. Dotson, J. L. Li, H. TI DISPERSION OF OBSERVED POSITION ANGLES OF SUBMILLIMETER POLARIZATION IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: magnetic fields; polarization; stars: formation; submillimeter ID MAGNETIC-FIELD STRENGTHS; FAR-INFRARED POLARIMETRY; STAR-FORMATION; DUST EMISSION; DARK CLOUDS; TURBULENCE; CORES; MODELS; SPARO; HERTZ AB One can estimate the characteristic magnetic field strength in Giant Molecular Clouds (GMCs) by comparing submillimeter polarimetric observations of these sources with simulated polarization maps developed using a range of different values for the assumed field strength. The point of comparison is the degree of order in the distribution of polarization position angles. In a recent paper by H. Li and collaborators, such a comparison was carried out using SPARO observations of two GMCs, and employing simulations by E. Ostriker and collaborators. Here, we re-examine this same question, using the same data set and the same simulations, but using an approach that differs in several respects. The most important difference is that we incorporate new, higher angular resolution observations for one of the clouds, obtained using the Hertz polarimeter. We conclude that the agreement between observations and simulations is best when the total magnetic energy (including both uniform and fluctuating field components) is at least as large as the turbulent kinetic energy. C1 [Novak, G.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Dotson, J. L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Li, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Novak, G (reprint author), Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. EM g-novak@northwestern.edu FU SPARO [OPP-01-30389]; Hertz [AST-02-04886]; Caltech Submillimeter Observatory [AST-05-40882] FX This work has benefited from illuminating discussions with R. Hildebrand and A. Lazarian. We are also grateful to E. Ostriker for providing the unpublished simulation, to P. Calisse for operating SPARO, and to the N. S. F. for supporting SPARO (Award OPP-01-30389 to Northwestern University), Hertz (Award AST-02-04886 to the University of Chicago), and the Caltech Submillimeter Observatory (Award AST-05-40882 to Caltech). NR 30 TC 16 Z9 16 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1362 EP 1369 DI 10.1088/0004-637X/695/2/1362 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300053 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, KL Celik, O Cesarini, A Ciupik, L Chow, YCK Cogan, P Colin, P Cui, W Daniel, MK Ergin, T Falcone, AD Fegan, SJ Finley, JP Fortin, P Fortson, LF Furniss, A Gillanders, GH Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, DB Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Moriarty, P Mukherjee, R Nagai, T Niemiec, J Ong, RA Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Toner, JA Valcarcel, L Vassiliev, VV Wagner, R Wakely, SP Ward, JE Weekes, TC Weinstein, A White, RJ Williams, DA Wissel, SA Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. L. Celik, O. Cesarini, A. Ciupik, L. Chow, Y. C. K. Cogan, P. Colin, P. Cui, W. Daniel, M. K. Ergin, T. Falcone, A. D. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. F. Furniss, A. Gillanders, G. H. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. B. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Nagai, T. Niemiec, J. Ong, R. A. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Toner, J. A. Valcarcel, L. Vassiliev, V. V. Wagner, R. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. White, R. J. Williams, D. A. Wissel, S. A. Wood, M. Zitzer, B. TI VERITAS OBSERVATIONS OF THE BL LAC OBJECT 1ES 1218+304 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (1ES 1218+304); galaxies: active; gamma rays: observations ID EXTRAGALACTIC BACKGROUND LIGHT; ENERGY GAMMA-RAYS; RADIATION-FIELDS; TEV BLAZARS; X-RAY; TELESCOPE; EMISSION; SPECTRA; DISCOVERY; HESS AB The VERITAS collaboration reports the detection of very-high-energy gamma-ray emission from the high-frequency-peaked BL Lac object 1ES 1218+304 located at a redshift of z = 0.182. A gamma-ray signal was detected with a statistical significance of 10.4 standard deviations (10.4 sigma) for the observations taken during the first three months of 2007, confirming the discovery of this object made by the MAGIC collaboration. The photon spectrum between similar to 160 GeV and similar to 1.8 TeV is well described by a power law with an index of Gamma = 3.08 +/- 0.34(stat) +/- 0.2(sys). The integral flux is Phi (E > 200 GeV) = (12.2 +/- 2.6) x 10(-12) cm(-2) s(-1), which corresponds to similar to 6% of that of the Crab Nebula. The light curve does not show any evidence for very high energy flux variability. Using lower limits on the density of the extragalactic background light in the near to mid-infrared, we are able to limit the range of intrinsic energy spectra for 1ES 1218+304. We show that the intrinsic photon spectrum has an index that is harder than Gamma = 2.32 +/- 0.37(stat). When including constraints from the spectra of 1ES 1101-232 and 1ES 0229+200, the spectrum of 1ES 1218+ 304 is likely to be harder than Gamma = 1.86 +/- 0.37(stat). C1 [Acciari, V. A.; Benbow, W.; Cesarini, A.; Hays, E.; Kildea, J.; Perkins, J. S.; Smith, A. W.; Toner, J. A.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Dept Phys & Astron, Newark, DE 19716 USA. [Arlen, T.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Arlen, T.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.; Smith, A. W.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Byrum, K. L.; Hays, E.; Horan, D.; Wagner, R.] Argonne Natl Lab, Argonne, IL 60439 USA. [Celik, O.; Chow, Y. C. K.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Dept Phys, Galway, Ireland. [Ciupik, L.; Fortson, L. F.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Valcarcel, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Colin, P.; Hui, C. M.; Kieda, D. B.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Cui, W.; Finley, J. P.; Konopelko, A.; Sembroski, G. H.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Ergin, T.] Univ Massachusetts, Dept Phys, Amherst, MA 01003 USA. [Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Grube, J.; Quinn, J.; Ward, J. E.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Humensky, T. B.; Reyes, L. C.; Swordy, S. P.; Wakely, S. P.; Wissel, S. A.] Univ Coll Dublin, Sch Phys, Dublin 2, Ireland. [Imran, A.; Krennrich, F.; Nagai, T.; Niemiec, J.; Pohl, M.; Schroedter, M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kaaret, P.; Pandel, D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Acciari, VA (reprint author), Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland. EM fortin@phys.columbia.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010; OI Daniel, Michael/0000-0002-8053-7910; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586 FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC; PPARC; Science Foundation Ireland FX This research is supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by PPARC in the UK, and Science Foundation Ireland. NR 41 TC 36 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1370 EP 1375 DI 10.1088/0004-637X/695/2/1370 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300054 ER PT J AU Tang, YW Ho, PTP Girart, JM Rao, R Koch, P Lai, SP AF Tang, Ya-Wen Ho, Paul T. P. Girart, Josep Miquel Rao, Ramprasad Koch, Patrick Lai, Shih-Ping TI EVOLUTION OF MAGNETIC FIELDS IN HIGH MASS STAR FORMATION: SUBMILLIMETER ARRAY DUST POLARIZATION IMAGE OF THE ULTRACOMPACT H II REGION G5.89-0.39 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (G5.89-0.39); ISM: magnetic fields; polarization; stars: formation ID MOLECULAR CLOUD CORES; FORMING-REGIONS; HII-REGIONS; RADIO FREQUENCIES; RADIATIVE TORQUES; OH MASERS; EMISSION; OUTFLOW; LINES; TURBULENCE AB We report high angular resolution (3 '') Submillimeter Array (SMA) observations of the molecular cloud associated with the Ultracompact H II region G5.89-0.39. Imaged dust continuum emission at 870 mu m reveals significant linear polarization. The position angles (P.A.s) of the polarization vary enormously but smoothly in a region of 2 x 10(4) AU. Based on the distribution of the P.A.s and the associated structures, the polarized emission can be separated roughly into two components. The component "x" is associated with a well-defined dust ridge at 870 mu m, and is likely tracing a compressed B field. The component "o" is located at the periphery of the dust ridge and is probably from the original B field associated with a pre-existing extended structure. The global B field morphology in G5.89, as inferred from the P.A.s, is clearly disturbed by the expansion of the H II region and the molecular outflows. Using the Chandrasekhar-Fermi method, we estimate from the smoothness of the field structures that the B field strength in the plane of sky can be no more than 2-3 mG. We then compare the energy densities in the radiation, the B field, and the mechanical motions as deduced from the C(17)O 3-2 line emission. We conclude that the B field structures are already overwhelmed and dominated by the radiation, outflows, and turbulence from the newly formed massive stars. C1 [Tang, Ya-Wen] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Tang, Ya-Wen; Ho, Paul T. P.; Rao, Ramprasad; Koch, Patrick; Lai, Shih-Ping] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Girart, Josep Miquel] CSIC, Fac Ciencies, IEEC, Inst Ciencies Espai, Bellaterra 08193, Catalunya, Spain. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 300, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 300, Taiwan. RP Tang, YW (reprint author), Natl Taiwan Univ, Dept Phys, 1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Tang, Ya-Wen/0000-0002-0675-276X NR 62 TC 35 Z9 35 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1399 EP 1412 DI 10.1088/0004-637X/695/2/1399 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300057 ER PT J AU Montero-Castano, M Herrnstein, RM Ho, PTP AF Montero-Castano, Maria Herrnstein, Robeson M. Ho, Paul T. P. TI GAS INFALL TOWARD Sgr A* FROM THE CLUMPY CIRCUMNUCLEAR DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: molecules; Galaxy: center; radio lines: ISM ID GALACTIC-CENTER; SAGITTARIUS-A; NEUTRAL-GAS; MOLECULAR CLOUDS; ROTATION CURVE; CENTRAL PARSEC; BLACK-HOLE; GALAXY; EMISSION; HCN AB We present the first large-scale mosaic performed with the Submillimeter Array in the Galactic center. We have produced a 25 pointing mosaic, covering a similar to 2' x 2' area around Sgr A*. We have detected emission from two high-density molecular tracers, HCN(4-3) and CS(7-6), the latter never before reported in this region. The data have an angular resolution of 4.'' 6 x 3.'' 1, and the spectral window coverage is from -180 km s(-1) to 1490 km s(-1) for HCN(4-3) and from - 1605 km s(-1) to 129 km s(-1) for CS(7-6). Both molecular tracers present a very clumpy distribution along the circumnuclear disk (CND), and are detected with a high signal-to-noise ratio in the southern part of the CND, while they are weaker toward the northern part. Assuming that the clumps are as close to the Galactic center as their projected distances, they are still dense enough to be gravitationally stable against the tidal shear produced by the supermassive black hole. Therefore, the CND is a nontransient structure. This geometrical distribution of both tracers suggests that the southern part of the CND is denser than the northern part. Also, by comparing the HCN(4-3) results with HCN(1-0) results we can see that the northern and the southern parts of the CND have different excitation levels, with the southern part warmer than the northern. Finally, we compare our results with those obtained with the detection of NH(3), which traces the warmer and less dense material detected in the inner cavity of the CND. We suggest that we are detecting the origin point where a portion of the CND becomes destabilized and approaches the dynamical center of the Milky Way, possibly being impacted by the southern streamer and heated on its way inward. C1 [Montero-Castano, Maria; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Montero-Castano, Maria] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain. [Montero-Castano, Maria; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Herrnstein, Robeson M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Montero-Castano, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmontero@cfa.harvard.edu; herrnstein@astro.columbia.edu; pho@cfa.harvard.edu FU Smithsonian Institution Visiting Student Grant; Academia Sinica Institute of Astronomy and Astrophysics Fellowship FX We thank M. Christopher for providing the HCN(1-0) data we have used for comparison. We also thank the referee, T. Wilson, for his helpful suggestions to improve the manuscript. During the development of this study, M. M.-C. has been supported by a Smithsonian Institution Visiting Student Grant and an Academia Sinica Institute of Astronomy and Astrophysics Fellowship. NR 36 TC 41 Z9 41 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1477 EP 1494 DI 10.1088/0004-637X/695/2/1477 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300063 ER PT J AU Fekel, FC Boden, AF Tomkin, J Torres, G AF Fekel, Francis C. Boden, Andrew F. Tomkin, Jocelyn Torres, Guillermo TI HR 8257: A THREE-DIMENSIONAL ORBIT AND BASIC PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: fundamental parameters; stars: individual (HR 8257) ID PALOMAR TESTBED INTERFEROMETER; ICCD SPECKLE OBSERVATIONS; CLOSE BINARY STARS; A-TYPE STARS; SPECTROSCOPIC BINARIES; 12 BOOTIS; SPECTRAL CLASSIFICATION; ROTATIONAL VELOCITIES; SOLAR NEIGHBORHOOD; TIDAL EVOLUTION AB We have used interferometric and spectroscopic observations of HR 8257 to determine a three-dimensional orbit of the system. The orbit has a period of 12.21345 days and an eccentricity of 0.2895. The masses of the F0 and F2 dwarf components are 1.56 and 1.38M(circle dot), respectively, with fractional errors of 1.4%. Our orbital parallax of 13.632 +/- 0.095 mas, corresponding to a distance of 73.4 +/- 0.6 pc, differs from the Hipparcos result by just 2% and has a significantly smaller uncertainty. From our spectroscopic observations and spectral energy distribution modeling we determine the component effective temperatures and luminosities to be T(eff)(A) = 7030 +/- 200K and T(eff)(B) = 6560 +/- 200K and L(A) = 9.4 +/- 0.3 L(circle dot) and L(B) = 4.7 +/- 0.2 L(circle dot). The primary rotates pseudosynchronously, while the secondary is not far from its pseudosynchronous rotational velocity. Although both early-F stars are slowly rotating, neither component of this close binary is an Am star. A comparison with evolutionary tracks indicates that the stars are slightly metal poor, and although the components have evolved away from the zero-age main sequence, they are both still dwarfs. C1 [Fekel, Francis C.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Boden, Andrew F.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Tomkin, Jocelyn] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Tomkin, Jocelyn] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fekel, FC (reprint author), Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. EM fekel@evans.tsuniv.edu; bode@astro.caltech.edu; jt@alexis.as.utexas.edu; gtorres@cfa.harvard.edu NR 47 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1527 EP 1536 DI 10.1088/0004-637X/695/2/1527 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300067 ER PT J AU Iono, D Wilson, CD Yun, MS Baker, AJ Petitpas, GR Peck, AB Krips, M Cox, TJ Matsushita, S Mihos, JC Pihlstrom, Y AF Iono, Daisuke Wilson, Christine D. Yun, Min S. Baker, Andrew J. Petitpas, Glen R. Peck, Alison B. Krips, Melanie Cox, T. J. Matsushita, Satoki Mihos, J. Christopher Pihlstrom, Ylva TI LUMINOUS INFRARED GALAXIES WITH THE SUBMILLIMETER ARRAY. II. COMPARING THE CO (3-2) SIZES AND LUMINOSITIES OF LOCAL AND HIGH-REDSHIFT LUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: observations; galaxies: formation; galaxies: high-redshift; galaxies: starburst; submillimeter ID DENSE MOLECULAR GAS; HUBBLE-SPACE-TELESCOPE; STAR-FORMING GALAXIES; LYMAN BREAK GALAXY; RADIO OBSERVATIONS; MAJOR MERGERS; HOST GALAXIES; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; Z-SIMILAR-TO-6 QUASARS AB We present a detailed comparison of the CO (3-2) emitting molecular gas between a local sample of luminous infrared galaxies (U/LIRGs) and a high-redshift sample that comprises submm selected galaxies (SMGs), quasars, and Lyman Break Galaxies (LBGs). The U/LIRG sample consists of our recent CO (3-2) survey using the Submillimeter Array while the CO (3-2) data for the high-redshift population are obtained from the literature. We find that the L'(CO(3-2)) and L(FIR) relation is correlated over five orders of magnitude, which suggests that the molecular gas traced in CO (3-2) emission is a robust tracer of dusty star formation activity. The near unity slope of 0.93 +/- 0.03 obtained from a fit to this relation suggests that the star formation efficiency is constant to within a factor of 2 across different types of galaxies residing in vastly different epochs. The CO (3-2) size measurements suggest that the molecular gas disks in local U/LIRGs (0.3-3.1 kpc) are much more compact than the SMGs (3-16 kpc), and that the size scales of SMGs are comparable to the nuclear separation (5-40 kpc) of the widely separated nuclei of U/LIRGs in our sample. We argue from these results that the SMGs studied here are predominantly intermediate stage mergers, and that the wider line widths arise from the violent merger of two massive gas-rich galaxies taking place deep in a massive halo potential. C1 [Iono, Daisuke] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Iono, Daisuke] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. [Wilson, Christine D.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Baker, Andrew J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Petitpas, Glen R.; Krips, Melanie; Cox, T. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peck, Alison B.] Joint ALMA Off, Santiago 7550108, Chile. [Matsushita, Satoki] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Mihos, J. Christopher] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Pihlstrom, Ylva] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Iono, D (reprint author), Univ Tokyo, Inst Astron, 2-21-1 Osawa, Tokyo 1810015, Japan. EM d.iono@nao.ac.jp OI Mihos, Chris/0000-0002-7089-8616 FU MEXT [15071202]; Natural Science and Engineering Research Council of Canada (NSERC); National Science Foundation [AST-0708653] FX We thank the referee for detailed comments that improved the focus of this paper. D. I. thanks Ryohei Kawabe, Kotaro Kohno, Koichiro Nakanishi, Yoichi Tamura, Akira Endo, Fumi Egusa, Bunyo Hatsukade, Masahiro Sameshima, Kazuyuki Muraoka, Shinya Komugi, Desika Narayanan for useful discussion, and Thomas Greve for kindly providing tabulated data for the SMGs. 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. 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. This study was financially supported by MEXT Grant-in-Aid for Scientific Research on Priority Areas No. 15071202. C.D.W. acknowledges support by the Natural Science and Engineering Research Council of Canada (NSERC). A.J.B. acknowledges support by National Science Foundation grant AST-0708653. NR 132 TC 90 Z9 91 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2009 VL 695 IS 2 BP 1537 EP 1549 DI 10.1088/0004-637X/695/2/1537 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300068 ER PT J AU Soria, R Risaliti, G Elvis, M Fabbiano, G Bianchi, S Kuncic, Z AF Soria, R. Risaliti, G. Elvis, M. Fabbiano, G. Bianchi, S. Kuncic, Z. TI THE XMM-NEWTON LONG LOOK OF NGC 1365: LACK OF A HIGH/SOFT STATE IN ITS ULTRALUMINOUS X-RAY SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: individual (NGC 1365) ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE BINARIES; ADVECTION-DOMINATED ACCRETION; CYGNUS X-1; SPECTRAL TRANSITIONS; SPIRAL GALAXIES; NEARBY GALAXIES; MASS; DISKS; EMISSION AB Based on our long (similar to 300 ks) 2007 XMM-Newton observation of the Seyfert galaxy NGC 1365, we report here on the spectral and timing behavior of two ultraluminous X-ray sources (ULXs), which had previously reached isotropic X-ray luminosities L-X approximate to 4 x 10(40) erg s(-1) (0.3- 10 keV band). In 2007, they were in a lower state ( L-X approximate to 5 x 10(39) and 1.5 x 10(39) erg s(-1) for X1 and X2, respectively). Their X-ray spectra were dominated by power laws with photon indices Gamma approximate to 1.8 and 1.2, respectively. Thus, their spectra were similar to those at their outburst peaks. Both sources have been seen to vary by a factor of 20 in luminosity over the years, but their spectra are always dominated by a hard power law; unlike most stellar-mass black holes, they have never been found in a canonical high/soft state dominated by a standard disk. The lack of a canonical high/soft state seems to be a common feature of ULXs. We speculate that the different kind of donor star and/or a persistently super-Eddington accretion rate during their outbursts may prevent accretion flows in ULXs from settling into steady standard disks. C1 [Soria, R.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Risaliti, G.; Elvis, M.; Fabbiano, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Arcetri, Florence, Italy. [Bianchi, S.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Kuncic, Z.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. RP Soria, R (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM roberto.soria@mssl.ucl.ac.uk RI Kuncic, Zdenka/B-4464-2008; Bianchi, Stefano/B-4804-2010; OI Bianchi, Stefano/0000-0002-4622-4240; Risaliti, Guido/0000-0002-3556-977X NR 65 TC 21 Z9 21 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 APR 20 PY 2009 VL 695 IS 2 BP 1614 EP 1622 DI 10.1088/0004-637X/695/2/1614 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 430VS UT WOS:000265018300075 ER PT J AU Paddack, MJ Reynolds, JD Aguilar, C Appeldoorn, RS Beets, J Burkett, EW Chittaro, PM Clarke, K Esteves, R Fonseca, AC Forrester, GE Friedlander, AM Garcia-Sais, J Gonzalez-Sanson, G Jordan, LKB McClellan, DB Miller, MW Molloy, PP Mumby, PJ Nagelkerken, I Nemeth, M Navas-Camacho, R Pitt, J Polunin, NVC Reyes-Nivia, MC Robertson, DR Rodriguez-Ramirez, A Salas, E Smith, SR Spieler, RE Steele, MA Williams, ID Wormald, CL Watkinson, AR Cote, IM AF Paddack, Michelle J. Reynolds, John D. Aguilar, Consuelo Appeldoorn, Richard S. Beets, Jim Burkett, Edward W. Chittaro, Paul M. Clarke, Kristen Esteves, Rene Fonseca, Ana C. Forrester, Graham E. Friedlander, Alan M. Garcia-Sais, Jorge Gonzalez-Sanson, Gaspar Jordan, Lance K. B. McClellan, David B. Miller, Margaret W. Molloy, Philip P. Mumby, Peter J. Nagelkerken, Ivan Nemeth, Michael Navas-Camacho, Raul Pitt, Joanna Polunin, Nicholas V. C. Reyes-Nivia, Maria Catalina Robertson, D. Ross Rodriguez-Ramirez, Alberto Salas, Eva Smith, Struan R. Spieler, Richard E. Steele, Mark A. Williams, Ivor D. Wormald, Clare L. Watkinson, Andrew R. Cote, Isabelle M. TI Recent Region-wide Declines in Caribbean Reef Fish Abundance SO CURRENT BIOLOGY LA English DT Article ID GREAT-BARRIER-REEF; MASS MORTALITY; CORAL-REEFS; DIADEMA-ANTILLARUM; TROPHIC CASCADES; MARINE RESERVES; PROTECTED AREAS; COMMUNITIES; POPULATIONS; ECOSYSTEMS AB Profound ecological changes are occurring on coral reefs throughout the tropics [1-3], with marked coral cover losses and concomitant algal increases, particularly in the Caribbean region [4]. Historical declines in the abundance of large Caribbean reef fishes likely reflect centuries of overexploitation [5-7]. However, effects of drastic recent degradation of reef habitats on reef fish assemblages have yet to be established. By using meta.-analysis, we analyzed time series of reef fish density obtained from 48 studies that include 318 reefs across the Caribbean and span the time period 1955-2007. Our analyses show that overall reef fish density has been declining significantly for more than a decade, at rates that are consistent across all subregions of the Caribbean basin (2.7% to 6.0% loss per year) and in three of six trophic groups. Changes in fish density over the past half-century are modest relative to concurrent changes in benthic cover on Caribbean reefs. However, the recent significant decline in overall fish abunclance and its consistency across several trophic groups. and among both fished and nonfished species indicate that Caribbean fishes have begun to respond negatively to habitat degradation. C1 [Paddack, Michelle J.; Reynolds, John D.; Molloy, Philip P.; Cote, Isabelle M.] Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. [Paddack, Michelle J.; Watkinson, Andrew R.] Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. [Aguilar, Consuelo; Gonzalez-Sanson, Gaspar] Univ La Habana, Ctr Invest Marinas, Havana, Cuba. [Appeldoorn, Richard S.; Esteves, Rene; Garcia-Sais, Jorge; Nemeth, Michael] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Beets, Jim] Univ Hawaii, Dept Marine Sci, Hilo, HI 96720 USA. [Burkett, Edward W.] Univ Wisconsin, Dept Biol & Earth Sci, Superior, WI 54880 USA. [Chittaro, Paul M.] Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Seattle, WA 98112 USA. [Clarke, Kristen] Univ W Indies, Ctr Marine Sci, Mona, Jamaica. [Fonseca, Ana C.; Salas, Eva] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Forrester, Graham E.] Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA. [Friedlander, Alan M.] Univ Hawaii, Dept Zool, Hawaii Cooperat Fishery Res Unit, Honolulu, HI 96822 USA. [Jordan, Lance K. B.; Spieler, Richard E.] Nova SE Univ, Oceanog Ctr, Dania, FL 33004 USA. [Jordan, Lance K. B.; Spieler, Richard E.] Nova SE Univ, Natl Coral Reef Inst, Dania, FL 33004 USA. [McClellan, David B.; Miller, Margaret W.] NOAA Fisheries, SE Fisheries Sci Ctr, Miami, FL 33149 USA. [Mumby, Peter J.] Univ Exeter, Marine Spatial Ecol Lab, Sch BioSci, Exeter EX4 4PS, Devon, England. [Nagelkerken, Ivan] Radboud Univ Nijmegen, Fac Sci, Inst Water & Wetland Res, Dept Anim Ecol & Ecophysiol, NL-6500 GL Nijmegen, Netherlands. [Navas-Camacho, Raul; Reyes-Nivia, Maria Catalina; Rodriguez-Ramirez, Alberto] Inst Invest Marinas & Costeras INVEMAR, Programa Biodiversidad & Ecosistemas Marinos, Santa Marta, Colombia. [Pitt, Joanna] Bermuda Govt, Environm Protect Dept, Marine Resources Sect, Coney Isl, Bermuda. [Polunin, Nicholas V. C.] Newcastle Univ, Sch Marine Sci & Technol, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Reyes-Nivia, Maria Catalina] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1090 GT Amsterdam, Netherlands. [Robertson, D. Ross] Smithsonian Trop Res Inst Panama, Unit 0948, Miami, FL 34002 USA. [Smith, Struan R.] Georgia State Univ, Dept Biol, Atlanta, GA 30302 USA. [Steele, Mark A.; Wormald, Clare L.] Calif State Univ Northridge, Dept Biol, Northridge, CA 91330 USA. [Williams, Ivor D.] Hawaii Cooperat Fishery Res Unit, Kailua Kona, HI 96740 USA. [Williams, Ivor D.] Hawaii Div Aquat Resources, Kailua Kona, HI 96740 USA. RP Paddack, MJ (reprint author), Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. EM michelle.paddack@gmail.com RI Mumby, Peter/F-9914-2010; Nagelkerken, Ivan/E-1093-2011; Watkinson, Andrew/N-1649-2013; Reynolds, John/L-6345-2015; OI Nagelkerken, Ivan/0000-0003-4499-3940; Reynolds, John/0000-0002-0459-0074; Salas De la Fuente, Eva Maria/0000-0002-6941-0548; Forrester, Graham/0000-0001-5253-773X; Gonzalez-Sanson, Gaspar/0000-0002-8555-2685 FU UK's Natural Environment Resource Council [NE/CO04442/1]; National Park Service, USGS; NOAA- Biogeography Branch; National Science and Engineering Research Council of Canada [OGP01 5284]; Puerto Rico National Coral Reef Monitoring Program; Department of Natural and Environmental Resources; Lianna Jarecki for logistical support; NOAA Coral Reef Conservation Program; BBSRC (Biotechnology and Biological Sciences Research Council) [01/Al/S/08113]; Netherlands Organisation for Scientific Research; MAVDT; COLCIENCIAS; UNEP-CAR/RCU; CORALINA; CEINER; UAESPNN; CARICOMP; UK DFID; The Smithsonian Tropical Research Institute; Government of the Republic of Panama; Kuna General Congress FX This project was funded by the UK's Natural Environment Resource Council, NE/CO04442/1. J.B. and A.M.F. acknowledge the National Park Service, USGS, and NOAA- Biogeography Branch. P.M.C. was supported by the National Science and Engineering Research Council of Canada (Grant # OGP01 5284). R.E. and J.G.-S. were supported by the Puerto Rico National Coral Reef Monitoring Program sponsored by NOAA and administered by the P.R. Department of Natural and Environmental Resources (PRIDNER). A.C.F. and E.S. thank CARICOMP and Jorge Cortes. G.E.F. acknowledges Falconwood Corporation for funding and Lianna Jarecki for logistical support. M.W.M. and D.B.M. were supported by NOAA Coral Reef Conservation Program. P.P.M. was supported by BBSRC (Biotechnology and Biological Sciences Research Council) studentship # 01/Al/S/08113 and the John and Pamela Salter Charitable Trust. I.N. was supported by a Vidi grant from the Netherlands Organisation for Scientific Research (NWO). M.G.G. Grol is thanked for help with the field work in Grand Cayman. R.N.-C., A.R.-R., and M.C.R.-N. were funded by MAVDT, COLCIENCIAS. and UNEP-CAR/RCU. CORALINA, CEINER, UAESPNN, and CARICOMP contributed with funds and logistical support. N.V.C.P. was supported by UK DFID. D.R.R. was supported by The Smithsonian Tropical Research Institute, the Government of the Republic of Panama, the Kuna General Congress. Field assistance to D.R.R.: E. Pena, A. Cedeno. M.A.S., C.L.W., and G.E.F. appreciate long-term financial support from the National Science Foundation; financial and logistical support from the NOAA National Undersea Research Program; and the help of numerous field assistants. I.M.C. was supported by the National Science and Engineering Research Council of Canada. NR 48 TC 121 Z9 124 U1 2 U2 72 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD APR 14 PY 2009 VL 19 IS 7 BP 590 EP 595 DI 10.1016/j.cub.2009.02.041 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 434HX UT WOS:000265266900029 PM 19303296 ER PT J AU Langley, JA Mckee, KL Cahoon, DR Cherry, JA Megonigal, JP AF Langley, J. Adam McKee, Karen L. Cahoon, Donald R. Cherry, Julia A. Megonigal, J. Patrick TI Elevated CO2 stimulates marsh elevation gain, counterbalancing sea-level rise SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE coastal wetlands; nitrogen pollution; tidal marsh loss; root productivity; salinity ID COASTAL WETLANDS; NITROGEN; BAY; RESPONSES; GROWTH; ENRICHMENT; SALINITY AB Tidal wetlands experiencing increased rates of sea-level rise (SLR) must increase rates of soil elevation gain to avoid permanent conversion to open water. The maximal rate of SLR that these ecosystems can tolerate depends partly on mineral sediment deposition, but the accumulation of organic matter is equally important for many wetlands. Plant productivity drives organic matter dynamics and is sensitive to global change factors, such as rising atmospheric CO2 concentration. It remains unknown how global change will influence organic mechanisms that determine future tidal wetland viability. Here, we present experimental evidence that plant response to elevated atmospheric [ CO2] stimulates biogenic mechanisms of elevation gain in a brackish marsh. Elevated CO2 (ambient + 340 ppm) accelerated soil elevation gain by 3.9 mm yr(-1) in this 2-year field study, an effect mediated by stimulation of below-ground plant productivity. Further, a companion greenhouse experiment revealed that the CO2 effect was enhanced under salinity and flooding conditions likely to accompany future SLR. Our results indicate that by stimulating biogenic contributions to marsh elevation, increases in the greenhouse gas, CO2, may paradoxically aid some coastal wetlands in counterbalancing rising seas. C1 [Langley, J. Adam; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Langley, J. Adam] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [McKee, Karen L.] US Geol Survey, Natl Wetland Res Ctr, Lafayette, LA 70506 USA. [Cahoon, Donald R.] US Geol Survey, Patuxent Wildlife Res Ctr, Beltsville, MD 20705 USA. [Cherry, Julia A.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Cherry, Julia A.] Univ Alabama, New Coll, Tuscaloosa, AL 35487 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM megonigalp@si.edu RI McKee, Karen/D-1365-2014 OI McKee, Karen/0000-0001-7042-670X NR 31 TC 97 Z9 102 U1 7 U2 61 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 APR 14 PY 2009 VL 106 IS 15 BP 6182 EP 6186 DI 10.1073/pnas.0807695106 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 433AB UT WOS:000265174600029 PM 19325121 ER PT J AU Miller-Jones, JCA Jonker, PG Nelemans, G Portegies Zwart, S Dhawan, V Brisken, W Gallo, E Rupen, MP AF Miller-Jones, J. C. A. Jonker, P. G. Nelemans, G. Portegies Zwart, S. Dhawan, V. Brisken, W. Gallo, E. Rupen, M. P. TI The formation of the black hole in the X-ray binary system V404 Cyg SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrometry; stars: individual: V404 Cyg; stars: kinematics; stars: supernovae: general; radio continuum: stars; X-rays: binaries ID SCORPIUS X-1; GALACTIC DISK; NEUTRON-STARS; GS 2023+338; VELOCITY; MASS; KICKS; KINEMATICS; EVOLUTION; ORIGIN AB Using new and archival radio data, we have measured the proper motion of the black hole X-ray binary V404 Cyg to be 9.2 +/- 0.3 mas yr(-1). Combined with the systemic radial velocity from the literature, we derive the full three-dimensional heliocentric space velocity of the system, which we use to calculate a peculiar velocity in the range 47-102 km s(-1), with a best-fitting value of 64 km s(-1). We consider possible explanations for the observed peculiar velocity and find that the black hole cannot have formed via direct collapse. A natal supernova is required, in which either significant mass (similar to 11 M(circle dot)) was lost, giving rise to a symmetric Blaauw kick of up to similar to 65 km s(-1), or, more probably, asymmetries in the supernova led to an additional kick out of the orbital plane of the binary system. In the case of a purely symmetric kick, the black hole must have been formed with a mass similar to 9 M(circle dot), since when it has accreted 0.5-1.5 M(circle dot) from its companion. C1 [Miller-Jones, J. C. A.] NRAO Headquarters, Charlottesville, VA 22903 USA. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. [Dhawan, V.; Brisken, W.; Rupen, M. P.] Array Operat Ctr, NRAO, Socorro, NM 87801 USA. [Gallo, E.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Portegies Zwart, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Portegies Zwart, S.] Univ Amsterdam, Sect Computat Sci, NL-1098 SJ Amsterdam, Netherlands. [Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. RP Miller-Jones, JCA (reprint author), NRAO Headquarters, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM jmiller@nrao.edu RI Miller-Jones, James/B-2411-2013; Nelemans, Gijs/D-3177-2012 OI Miller-Jones, James/0000-0003-3124-2814; Nelemans, Gijs/0000-0002-0752-2974 FU Chandra Postdoctoral Fellowship [PF5-60037]; NASA [NAS8-03060]; national research councils; European Community [R113CT 2003 5058187] FX JCAM-J is a Jansky Fellow of the National Radio Astronomy Observatory. EG is supported through Chandra Postdoctoral Fellowship grant number PF5-60037, issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. The VLA and VLBA are facilities of the National Radio Astronomy Observatory, which is operated by Associated Universities, Inc., under cooperative agreement with the National Science Foundation. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. ParselTongue was developed in the context of the ALBUS project, which has benefitted from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187. This research has made use of NASA's Astrophysics Data System. NR 52 TC 14 Z9 14 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2009 VL 394 IS 3 BP 1440 EP 1448 DI 10.1111/j.1365-2966.2009.14404.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428AP UT WOS:000264820500019 ER PT J AU Liu, A Tegmark, M Zaldarriaga, M AF Liu, Adrian Tegmark, Max Zaldarriaga, Matias TI Will point sources spoil 21-cm tomography? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: interferometric; early Universe; radio lines: general ID 21 CENTIMETER TOMOGRAPHY; HIGH-REDSHIFT; INTERGALACTIC MEDIUM; DARK-AGES; REIONIZATION; FOREGROUNDS; EPOCH; FLUCTUATIONS; EMISSION; RADIATION AB 21-cm tomography is emerging as a promising probe of the cosmological dark ages and the epoch of reionization, as well as a tool for observational cosmology in general. However, serious sources of foreground contamination must be subtracted for experimental efforts to be viable. In this paper, we focus on the removal of unresolved extragalactic point sources with smooth spectra, and evaluate how the residual foreground contamination after cleaning depends on instrumental and algorithmic parameters. A crucial but often ignored complication is that the synthesized beam of an interferometer array shrinks towards higher frequency, causing complicated frequency structure in each sky pixel as 'frizz' far from the beam centre contracts across unresolved radio sources. We find that current-generation experiments should none the less be able to clean out this point source contamination adequately, and quantify the instrumental and algorithmic design specifications required to meet this foreground challenge. C1 [Liu, Adrian; Tegmark, Max] MIT, Dept Phys, Cambridge, MA 02139 USA. [Zaldarriaga, Matias] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. [Liu, Adrian; Tegmark, Max] MIT, Kavli Inst, Cambridge, MA 02139 USA. RP Liu, A (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM acliu@mit.edu FU NSF [AST-0134999, AST-05-06556]; David and Lucile Packard Foundation; Research Corporation FX We wish to thank Judd Bowman, Jacqueline Hewitt and Miguel Morales for helpful discussions and comments, and for sharing an early version of their manuscript prior to publication. We also thank Mike Matejek and Christopher Williams for useful feedback, and Matthew McQuinn for sharing 21-cm simulation results. This work was supported by NSF grants AST-0134999 and AST-05-06556 as well as fellowships from the David and Lucile Packard Foundation and the Research Corporation. NR 28 TC 54 Z9 54 U1 0 U2 2 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2009 VL 394 IS 3 BP 1575 EP 1587 DI 10.1111/j.1365-2966.2009.14426.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428AP UT WOS:000264820500033 ER PT J AU Sobolewska, MA Gierlinski, M Siemiginowska, A AF Sobolewska, Malgorzata A. Gierlinski, Marek Siemiginowska, Aneta TI What can we learn about quasars from alpha(OX) measurements in Galactic black hole binaries? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; galaxies: active; quasars: general; X-ray: binaries; X-rays: galaxies ID X-RAY-EMISSION; RADIO-QUIET QUASARS; HIGH-REDSHIFT QUASARS; ENERGY-DISTRIBUTIONS; TIMING PROPERTIES; ACCRETION DISC; XTE J1550-564; AGN SAMPLES; GX 339-4; LUMINOSITY AB We draw a comparison between active galactic nuclei (AGN) and Galactic black hole binaries (GBHs) using a uniform description of spectral energy distribution of these two classes of X-ray sources. We parametrize spectra of GBHs with an alpha(GBH) parameter which we define as a slope of a nominal power-law function between 3 and 20 keV. We show that this parameter can be treated as an equivalent of the X-ray loudness, alpha(OX), used to describe AGN spectra. We do not find linear correlation between the alpha(GBH) and disc flux (similar to that between alpha(OX) and optical/UV luminosity found in AGN). Instead, we show that alpha(GBH) follows a well-defined pattern during a GBH outburst. We find that alpha(GBH) tend to cluster around 1, 1.5 and 2, which corresponds to the hard, very high/intermediate and soft spectral states, respectively. We conclude that majority of the observed Type 1 radio quiet AGN are in the spectral state corresponding to the very high/intermediate state of GBHs. The same conclusion is valid for radio-loud AGN. We also study variations of the spectral slopes (alpha(GBH) and the X-ray photon index, Gamma) as a function of disc and Comptonization fluxes. We discuss these dependencies in the light of correlations of alpha(OX) and Gamma with the optical/UV and X-ray 2 keV fluxes considered for AGN and quasars. C1 [Sobolewska, Malgorzata A.] Fdn Res & Technol Hellas IESL, Iraklion 71110, Crete, Greece. [Siemiginowska, Aneta] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Sobolewska, MA (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM malgosia@physics.uoc.gr OI Gierlinski, Marek/0000-0001-9149-3514 FU NASA [NAS8-39073]; Chandra awards [GO2-3148A, GO5-6113X]; EU [MTKD-CT-2006-039965]; Ministry of Science and Higher Education [N20301132/1518]; STFC; Polish grant [NN203065933] FX We thank Paul Green for valuable discussions about AGN surveys, and the anonymous referee for careful reading of the manuscript and comments on how to improve it. This research was funded in part by NASA contract NAS8-39073 and Chandra awards GO2-3148A and GO5-6113X. MS was supported by EU grant MTKD-CT-2006-039965 and by Polish grant N20301132/1518 from Ministry of Science and Higher Education. MG acknowledges support from STFC Fellowship and Polish grant NN203065933. NR 44 TC 16 Z9 16 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2009 VL 394 IS 3 BP 1640 EP 1648 DI 10.1111/j.1365-2966.2009.14436.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428AP UT WOS:000264820500039 ER PT J AU Younger, JD Omont, A Fiolet, N Huang, JS Fazio, GG Lai, K Polletta, M Rigopoulou, D Zylka, R AF Younger, J. D. Omont, A. Fiolet, N. Huang, J. -S. Fazio, G. G. Lai, K. Polletta, M. Rigopoulou, D. Zylka, R. TI A millimetre survey of starburst dominated ultraluminous infrared galaxies at z similar to 2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; radio continuum: galaxies; submillimetre ID SUPERMASSIVE BLACK-HOLES; SPITZER-SPACE-TELESCOPE; LUMINOUS SUBMILLIMETER GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; PROBE WMAP OBSERVATIONS; EXTENDED GROTH STRIP; LYMAN BREAK GALAXIES; STAR-FORMATION RATE; ARRAY CAMERA IRAC; MU-M OBSERVATIONS AB We present millimetre observations of a sample of 12 high-redshift ultraluminous infrared galaxies (ULIRGs) in the extended growth strip (EGS). These objects were initially selected on the basis of their observed mid-IR colours (0.0 < [3.6] - [4.5] < 0.4 and - 0.7 < [ 3.6] - [8.0] < 0.5) to lie at high redshift 1.5 less than or similar to z less than or similar to 3, and subsequent 20-38 mu m mid-IR spectroscopy confirms that they lie in a narrow redshift window centred on z approximate to 2. We detect 9/12 of the objects in our sample at high significance (>3 sigma) with a mean 1200 mu m flux of < F(1200 mu m)> = 1.6 +/- 0.1 mJy. Our millimetre photometry, combined with existing far-IR photometry from the Far-IR Deep Extragalactic Legacy Survey (FIDELS) and accurate spectroscopic redshifts, places constraints both sides of the thermal dust peak. This allows us to estimate the dust properties, including the far-IR luminosity, dust temperature and dust mass. We find that our sample is similar to other high-z and intermediate-z ULIRGs, and local systems, but has a different dust selection function than submillimeter-selected galaxies. Finally, we use existing 20-cm radio continuum imaging to test the far-IR/radio correlation at high redshift. We find that our sample is consistent with the local relation, implying little evolution. Furthermore, this suggests that our sample selection method is efficient at identifying ultraluminous, starburst-dominated systems within a very narrow redshift range centred at z similar to 2. C1 [Younger, J. D.; Huang, J. -S.; Fazio, G. G.; Lai, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Omont, A.; Fiolet, N.; Polletta, M.] Univ Paris 06, F-75014 Paris, France. [Polletta, M.] INAF IASF Milano, I-20133 Milan, Italy. [Zylka, R.] IRAM, F-38406 St Martin Dheres, France. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Rigopoulou, D.] CNRS, Inst Astrophys Paris, F-75014 Paris, France. RP Younger, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyounger@cfa.harvard.edu OI Polletta, Maria del Carmen/0000-0001-7411-5386 FU NASA throuth JPL/Caltech; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX Thanks to Lars Hernquist, Philip Hopkins, T. J. Cox, Dusan Keres, Chris Hayward and Stephanie Bush for helpful discussions, and to the referee, Stephen Serjeant, for his helpful suggestions for improving this manuscript. 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. This work includes observations made with IRAM, which is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). Thanks to the staff of IRAM Granada for their support in taking the MAMBO observations presented here. NR 113 TC 36 Z9 36 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2009 VL 394 IS 3 BP 1685 EP 1694 DI 10.1111/j.1365-2966.2009.14455.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 428AP UT WOS:000264820500043 ER PT J AU Espada, D Matsushita, S Peck, A Henkel, C Iono, D Israel, FP Muller, S Petitpas, G Pihlstrom, Y Taylor, GB Dinh-V-Trung AF Espada, D. Matsushita, S. Peck, A. Henkel, C. Iono, D. Israel, F. P. Muller, S. Petitpas, G. Pihlstroem, Y. Taylor, G. B. Dinh-V-Trung TI DISENTANGLING THE CIRCUMNUCLEAR ENVIRONS OF CENTAURUS A. I. HIGH-RESOLUTION MOLECULAR GAS IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 5128); galaxies: ISM; galaxies: structure ID RADIO GALAXY CENTAURUS; SUPERMASSIVE BLACK-HOLE; NEARBY SEYFERT-GALAXIES; NGC 5128; SCALE STRUCTURE; CENTRAL REGIONS; STAR-FORMATION; WARPED DISK; CO EMISSION; NUCLEUS AB We present high-resolution images of the (12)CO(2-1) emission in the central 1' (1 kpc) of NGC 5128 (Centaurus A), observed using the Submillimeter Array. We elucidate for the first time the distribution and kinematics of the molecular gas in this region with a resolution of 6.'' 0 x 2.'' 4 (100 pc x 40 pc). We spatially resolve the circumnuclear molecular gas in the inner 24 '' x 12 '' (400 pc x 200 pc), which is elongated along a position angle of P.A. similar or equal to 155 degrees and perpendicular to the radio/X-ray jet. The southeast (SE) and northwest (NW) components of the circumnuclear gas are connected to molecular gas found at larger radii. This gas appears as two parallel filaments at P.A. = 120 degrees, which are coextensive with the long sides of the 3 kpc parallelogram shape of the previously observed dust continuum, as well as ionized and pure rotational H(2) lines. Spatial and kinematical asymmetries are apparent in both the circumnuclear and outer gas, suggesting noncoplanar and/or noncircular motions. We extend to inner radii (r < 200 pc) previously studied warped disk models built to reproduce the central parallelogram-shaped structure. Adopting the warped disk model we would confirm a gap in emission between the radii r = 200-800 pc (12 ''-50 ''), as has been suggested previously. Although this model explains this prominent feature; however, our (12)CO(2-1) observations show relevant deviations from this model: namely, the physical connection between the circumnuclear gas and that at larger radii, brighter SE and NW sides on the parallelogram-shaped feature, and an outer curvature of its long sides. Overall, it resembles more closely an S-shaped morphology, a trend that is also found in other molecular species. Hence, we qualitatively explore the possible contribution of a weak bi-symmetric potential which would naturally explain these peculiarities. C1 [Espada, D.; Matsushita, S.; Muller, S.; Dinh-V-Trung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Espada, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espada, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Peck, A.] Joint ALMA Off, Santiago, Chile. [Peck, A.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Iono, D.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Israel, F. P.] Leiden Univ, NL-2300 CA Leiden, Netherlands. [Pihlstroem, Y.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Espada, D (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM despada@cfa.harvard.edu OI /0000-0002-9931-1313 FU National Aeronautics and Space Administration; Marie Curie International Fellowship; European Community FX We thank the SMA staff members who made the observations reported here possible. We especially acknowledge K. Sakamoto, P. T. P. Ho, and L. Verdes-Montenegro for useful comments on the manuscript. We also thank A. Quillen for kindly making available the mid-IR images from Spitzer/IRAC and IRS and A. Sarma for the 21 cm continuum data from VLA. This research has made use of NASA's Astrophysics Data System Bibliographic Services, and has also 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. This research was supported by a Marie Curie International Fellowship within the 6th European Community Framework Programme. NR 65 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 116 EP 134 DI 10.1088/0004-637X/695/1/116 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500010 ER PT J AU Silverman, JD Kovac, K Knobel, C Lilly, S Bolzonella, M Lamareille, F Mainieri, V Brusa, M Cappelluti, N Peng, Y Hasinger, G Zamorani, G Scodeggio, M Contini, T Carollo, CM Jahnke, K Kneib, JP Le Fevre, O Bardelli, S Bongiorno, A Brunner, H Caputi, K Civano, F Comastri, A Coppa, G Cucciati, O de la Torre, S de Ravel, L Elvis, M Finoguenov, A Fiore, F Franzetti, P Garilli, B Gilli, R Griffiths, R Iovino, A Kampczyk, P Koekemoer, A Le Borgne, JF Le Brun, V Maier, C Mignoli, M Pello, R Montero, EP Ricciardelli, E Tanaka, M Tasca, L Tresse, L Vergani, D Vignali, C Zucca, E Bottini, D Cappi, A Cassata, P Marinoni, C McCracken, HJ Memeo, P Meneux, B Oesch, P Porciani, C Salvato, M AF Silverman, J. D. Kovac, K. Knobel, C. Lilly, S. Bolzonella, M. Lamareille, F. Mainieri, V. Brusa, M. Cappelluti, N. Peng, Y. Hasinger, G. Zamorani, G. Scodeggio, M. Contini, T. Carollo, C. M. Jahnke, K. Kneib, J. -P. Le Fevre, O. Bardelli, S. Bongiorno, A. Brunner, H. Caputi, K. Civano, F. Comastri, A. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Elvis, M. Finoguenov, A. Fiore, F. Franzetti, P. Garilli, B. Gilli, R. Griffiths, R. Iovino, A. Kampczyk, P. Koekemoer, A. Le Borgne, J. -F. Le Brun, V. Maier, C. Mignoli, M. Pello, R. Montero, E. Perez Ricciardelli, E. Tanaka, M. Tasca, L. Tresse, L. Vergani, D. Vignali, C. Zucca, E. Bottini, D. Cappi, A. Cassata, P. Marinoni, C. McCracken, H. J. Memeo, P. Meneux, B. Oesch, P. Porciani, C. Salvato, M. TI THE ENVIRONMENTS OF ACTIVE GALACTIC NUCLEI WITHIN THE zCOSMOS DENSITY FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; quasars: general; X-rays: galaxies ID STAR-FORMING GALAXIES; DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES; RAY SELECTED AGN; COSMOS FIELD; REDSHIFT SURVEY; HOST GALAXIES; STELLAR MASS; EVOLUTION; CHANDRA AB The impact of environment on active galactic nucleus (AGN) activity up to z similar to 1 is assessed by utilizing a mass-selected sample of galaxies from the 10k catalog of the zCOSMOS spectroscopic redshift survey. We identify 147 AGN by their X-ray emission as detected by XMM-Newton from a parent sample of 7234 galaxies. We measure the fraction of galaxies with stellar mass M(*) > 2.5 x 10(10) M(circle dot) that host an AGN as a function of local overdensity using the 5th, 10th, and 20th nearest neighbors that cover a range of physical scales (similar to 1-4 Mpc). Overall, we find that AGNs prefer to reside in environments equivalent to massive galaxies with substantial levels of star formation. Specifically, AGNs with host masses between 0.25 and 1 x 10(11) M(circle dot) span the full range of environments (i.e., field to group) exhibited by galaxies of the same mass and rest-frame color or specific star formation rate. Host galaxies having M(*) > 1011 M(circle dot) clearly illustrate the association with star formation since they are predominantly bluer than the underlying galaxy population and exhibit a preference for lower-density regions analogous to Sloan Digital Sky Survey studies of narrow-line AGN. To probe the environment on smaller physical scales, we determine the fraction of galaxies (M(*) > 2.5 x 10(10) M(circle dot)) hosting AGNs inside optically selected groups, and find no significant difference with field galaxies. We interpret our results as evidence that AGN activity requires a sufficient fuel supply; the probability of a massive galaxy to have retained some sufficient amount of gas, as evidence by its ongoing star formation, is higher in underdense regions where disruptive processes (i.e., galaxy harassment, tidal stripping) are lessened. C1 [Silverman, J. D.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. Univ Toulouse, Lab Astrophys Toulouse Tarbes, CNRS, F-31400 Toulouse, France. European So Observ, D-85748 Garching, Germany. IASF Milano, INAF, Milan, Italy. Max Planck Inst Astron, D-69117 Heidelberg, Germany. Lab Astrophys Marseille, Marseille, France. Univ Sternwarte, D-81679 Munich, Germany. INAF Osservatorio Astron Brera, Milan, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. Ctr Phys Theor, Marseille, France. Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. CALTECH, Pasadena, CA 91125 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Silverman, JD (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. RI Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Zucca, Elena/O-9396-2015; Cappi, Alberto/O-9391-2015; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Bardelli, Sandro/O-9369-2015; OI Vergani, Daniela/0000-0003-0898-2216; Vignali, Cristian/0000-0002-8853-9611; Zucca, Elena/0000-0002-5845-8132; Cappi, Alberto/0000-0002-9200-7167; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; Bardelli, Sandro/0000-0002-8900-0298; Bongiorno, Angela/0000-0002-0101-6624; Scodeggio, Marco/0000-0002-2282-5850; Cappelluti, Nico/0000-0002-1697-186X; Jahnke, Knud/0000-0003-3804-2137; Oesch, Pascal/0000-0001-5851-6649; Garilli, Bianca/0000-0001-7455-8750; Koekemoer, Anton/0000-0002-6610-2048; Fiore, Fabrizio/0000-0002-4031-4157 FU European Southern Observatory (ESO) [175. A-0839] FX We thank the referee and Paul Martini for constructive comments that significantly improved the paper. This work is fully based on observations undertaken at the European Southern Observatory (ESO) Very Large Telescope (VLT) under the Large Program 175. A-0839 (P.I.: Simon Lilly). NR 72 TC 67 Z9 67 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 171 EP 182 DI 10.1088/0004-637X/695/1/171 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500014 ER PT J AU Landi, E Miralles, MP Curdt, W Hara, H AF Landi, E. Miralles, M. P. Curdt, W. Hara, H. TI PHYSICAL PROPERTIES OF COOLING PLASMA IN QUIESCENT ACTIVE REGION LOOPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: UV radiation ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; OPTICALLY THIN PLASMAS; IMAGING SPECTROMETER; ATOMIC DATABASE; EMISSION-LINES; SOLAR; PROMINENCES; CONDENSATION; DIAGNOSTICS; WAVELENGTHS AB In the present work, we use SOHO/SUMER, SOHO/UVCS, SOHO/EIT, SOHO/LASCO, STEREO/EUVI, and Hinode/EIS coordinated observations of an active region (AR 10989) at the west limb taken on 2008 April 8 to study the cooling of coronal loops. The cooling plasma is identified using the intensities of SUMER spectral lines emitted at temperatures in the 4.15 <= log T <= 5.45 range. EIS and SUMER spectral observations are used to measure the physical properties of the loops. We found that before cooling took place these loops were filled with coronal hole-like plasma, with temperatures in the 5.6 <= log T <= 5.9 range. SUMER spectra also allowed us to determine the plasma temperature, density, emission measure, element abundances, and dynamic status during the cooling process. The ability of EUVI to observe the emitting region from a different direction allowed us to measure the volume of the emitting region and estimate its emission measure. Comparison with values measured from line intensities provided us with an estimate of the filling factor. UVCS observations of the coronal emission above the active region showed no streamer structure associated with AR 10989 at position angles between 242 degrees and 253 degrees. EIT, LASCO, and EUVI-A narrowband images and UVCS spectral observations were used to discriminate between different scenarios and monitor the behavior of the active region in time. The present study provides the first detailed measurements of the physical properties of cooling loops, a very important benchmark for theoretical models of loop cooling and condensation. C1 [Landi, E.] USN, Res Lab, Artep Inc, Washington, DC 20375 USA. [Miralles, M. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Curdt, W.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Hara, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Landi, E (reprint author), USN, Res Lab, Artep Inc, 4555 Overlook Ave SW, Washington, DC 20375 USA. RI Landi, Enrico/H-4493-2011 FU NASA [NNG06EA14I, NNH06CD24C, NNX06AG95G, NNX08AQ96G]; DLR; CNES; ESA PRODEX programme (Swiss contribution) FX The work of E. L. is supported by the NNG06EA14I, NNH06CD24C and other NASA grants. The work of M. P. M. is supported by NASA grants NNX06AG95G and NNX08AQ96G to the Smithsonian Astrophysical Observatory. The ground-based polarization brightness images used here were produced by the High Altitude Observatory's Mauna Loa Observatory. The space-based images in Figures 1 and 2 are courtesy of the EIT and LASCO/SOHO consortia. The SUMER project is financially supported by DLR, CNES, NASA, and the ESA PRODEX programme (Swiss contribution). SUMER is part of SOHO of ESA and NASA. The authors thank S. R. Cranmer for valuable discussions, and the anonymous referee for his/her comments that helped improve the original manuscript. NR 40 TC 15 Z9 15 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 APR 10 PY 2009 VL 695 IS 1 BP 221 EP 237 DI 10.1088/0004-637X/695/1/221 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500018 ER PT J AU Reid, MJ Braatz, JA Condon, JJ Greenhill, LJ Henkel, C Lo, KY AF Reid, M. J. Braatz, J. A. Condon, J. J. Greenhill, L. J. Henkel, C. Lo, K. Y. TI THE MEGAMASER COSMOLOGY PROJECT. I. VERY LONG BASELINE INTERFEROMETRIC OBSERVATIONS OF UGC 3789 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; cosmology: observations; distance scale; galaxies: distances and redshifts; galaxies: individual (UGC 3789); masers ID ACTIVE GALACTIC NUCLEI; WATER MASER EMISSION; GEOMETRIC DISTANCE; GALAXY NGC-4258; CEPHEID DISTANCE; HUBBLE CONSTANT; DARK ENERGY; DISCOVERY; DISK; VELOCITIES AB The Megamaser Cosmology Project (MCP) seeks to measure the IIubble Constant (H(0)) in order to improve the extragalactic distance scale and constrain the nature of dark energy. We are searching for sources of H(2)O maser emission from active galactic nuclei with sub-pc accretion disks, as in NGC 4258, and following up these discoveries with very long baseline interferometric (VLBI) imaging and spectral monitoring. Here we present a VLBI map of the H(2)O masers toward UGC 3789, a galaxy well into the Hubble Flow. We have observed masers moving at rotational speeds up to 800 km s(-1) at radii as small as 0.08 pc. Our map reveals masers in a nearly edge-on disk in Keplerian rotation about a 107 M(circle dot) supermassive black hole. When combined with centripetal accelerations, obtained by observing spectral drifts of maser features (to be presented in Paper II), the UGC 3789 masers may provide an accurate determination of H(0), independent of luminosities and metallicity and extinction corrections. C1 [Reid, M. J.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Braatz, J. A.; Condon, J. J.; Lo, K. Y.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 29 TC 36 Z9 36 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 287 EP 291 DI 10.1088/0004-637X/695/1/287 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500024 ER PT J AU Berger, E Rutledge, RE Phan-Bao, N Basri, G Giampapa, MS Gizis, JE Liebert, J Martin, E Fleming, TA AF Berger, E. Rutledge, R. E. Phan-Bao, N. Basri, G. Giampapa, M. S. Gizis, J. E. Liebert, J. Martin, E. Fleming, T. A. TI PERIODIC RADIO AND H alpha EMISSION FROM THE L DWARF BINARY 2MASSW J0746425+200032: EXPLORING THE MAGNETIC FIELD TOPOLOGY AND RADIUS OF AN L DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: activity; stars: low-mass, brown dwarfs; stars: magnetic fields ID LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ELECTRON-CYCLOTRON MASER; ULTRACOOL DWARFS; BROWN DWARFS; X-RAY; TVLM-513-46546; ROTATION; ASTROMETRY; DISCOVERY AB We present an 8.5 hr simultaneous radio, X-ray, UV, and optical observation of the L dwarf binary 2MASSW J0746425+200032. We detect strong radio emission, dominated by short-duration periodic pulses at 4.86 GHz with P = 124.32 +/- 0.11 min. The stability of the pulse profiles and arrival times demonstrates that they are due to the rotational modulation of a B approximate to 1.7 kG magnetic field. A quiescent nonvariable component is also detected, likely due to emission from a uniform large-scale field. The Ha emission exhibits identical periodicity, but unlike the radio pulses it varies sinusoidally and is offset by exactly 1/4 of a phase. The sinusoidal variations require chromospheric emission from a large-scale field structure, with the radio pulses likely emanating from the magnetic poles. While both light curves can be explained by a rotating misaligned magnetic field, the 1/4 phase lag rules out a symmetric dipole topology since it would result in a phase lag of 1/2 (poloidal field) or zero (toroidal field). We therefore conclude that either (1) the field is dominated by a quadrupole configuration, which can naturally explain the 1/4 phase lag; or (2) the H alpha and/or radio emission regions are not trivially aligned with the field. Regardless of the field topology, we use the measured period along with the known rotation velocity (upsilon sin i approximate to 27 km s(-1)), and the binary orbital inclination (i approximate to 142 degrees), to derive a radius for the primary star of 0.078 +/- 0.010 R(circle dot). This is the first measurement of the radius of an L dwarf, and along with a mass of 0.085 +/- 0.010 M(circle dot) it provides a constraint on the mass-radius relation below 0.1 M(circle dot). We find that the radius is about 30% smaller than expected from theoretical models, even for an age of a few Gyr. The origin of this discrepancy is either a breakdown of the models at the bottom of the main sequence, or a significant misalignment between the rotational and orbital axes. C1 [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rutledge, R. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Phan-Bao, N.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Basri, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Giampapa, M. S.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Gizis, J. E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Liebert, J.; Fleming, T. A.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Liebert, J.; Fleming, T. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Martin, E.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Martin, E.] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration through Chandra [G08-9013A]; Chandra X-ray Observatory Center; National Aeronautics Space Administration [NAS8-03060] FX We thank the Chandra, Gemini, VLA, and Swift schedulers for their invaluable help in coordinating these observations. This work has made use of the SIMBAD database, operated at CDS, Strasbourg, France. It is based in part on 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 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), CNPq (Brazil) and CONICET (Argentina). Data from the UVOT instrument on Swift were used in this work. Swift is an international observatory developed and operated in the US, UK and Italy, and managed by NASA Goddard Space Flight Center with operations center at Penn State University. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G08-9013A 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. NR 35 TC 69 Z9 70 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 310 EP 316 DI 10.1088/0004-637X/695/1/310 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500026 ER PT J AU Hartman, JD Gaudi, BS Holman, MJ McLeod, BA Stanek, KZ Barranco, JA Pinsonneault, MH Meibom, S Kalirai, JS AF Hartman, J. D. Gaudi, B. S. Holman, M. J. McLeod, B. A. Stanek, K. Z. Barranco, J. A. Pinsonneault, M. H. Meibom, S. Kalirai, J. S. TI DEEP MMT* TRANSIT SURVEY OF THE OPEN CLUSTER M37 IV: LIMIT ON THE FRACTION OF STARS WITH PLANETS AS SMALL AS 0.3R(J) SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M37); planetary systems; surveys ID EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; HOT JUPITERS; DETERMINISTIC MODEL; PHOTOMETRIC SURVEYS; PERIOD DISTRIBUTION; STELLAR PHOTOMETRY; IMAGE SUBTRACTION; SPECTRAL-ANALYSIS; EXTENSIVE SEARCH AB We present the results of a deep (15 less than or similar to r less than or similar to 23), 20 night survey for transiting planets in the intermediate-age open cluster M37 (NGC 2099) using the Megacam wide-field mosaic CCD camera on the 6.5 m MMT. We do not detect any transiting planets among the similar to 1450 observed cluster members. We do, however, identify a similar to 1R(J) candidate planet transiting a 0.8 M-circle dot Galactic field star with a period of 0.77 days. The source is faint (V = 19.85 mag) and has an expected velocity semiamplitude of K similar to 220 m s(-1) (M/M-J). We conduct Monte Carlo transit injection and recovery simulations to calculate the 95% confidence upper limit on the fraction of cluster members and field stars with planets as a function of planetary radius and orbital period. Assuming a uniform logarithmic distribution in the orbital period, we find that < 1.1%, < 2.7%, and < 8.3% of cluster members have 1.0R(J) planets within extremely hot Jupiter (EHJ; 0.4 < P < 1.0 day), very hot Jupiter (VHJ; 1.0 < P < 3.0 day), and hot Jupiter (HJ; 3.0 < P < 5.0 day) period ranges, respectively. For 0.5R(J) planets, the limits are less than 3.2% and less than 21% for EHJ and VHJ period ranges, respectively, while for 0.35R(J) planets we can only place an upper limit of less than 25% on the EHJ period range. For a sample of 7814 Galactic field stars, consisting primarily of FGKM dwarfs, we place 95% upper limits of < 0.3%, < 0.8%, and < 2.7% on the fraction of stars with a 1.0R(J) EHJ, VHJ, and HJ, respectively, assuming that the candidate planet is not genuine. If the candidate is genuine, the frequency of similar to 1.0R(J) planets in the EHJ period range is 0.002% < f(EHJ) < 0.5% with 95% confidence. We place limits of < 1.4%, < 8.8%, and < 47% for 0.5R(J) planets, and a limit of < 16% on 0.3R(J) planets in the EHJ period range. This is the first transit survey to place limits on the fraction of stars with planets as small as Neptune. C1 [Hartman, J. D.; Holman, M. J.; McLeod, B. A.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaudi, B. S.; Stanek, K. Z.; Pinsonneault, M. H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Barranco, J. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Kalirai, J. S.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95060 USA. RP Hartman, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jhartman@cfa.harvard.edu; gaudi@astronomy.ohio-state.edu; mholman@cfa.harvard.edu; bmcleod@cfa.harvard.edu; kstanek@astronomy.ohio-state.edu; barranco@stars.sfsu.edu; pinsono@astronomy.ohio-state.edu; smeibom@cfa.harvard.edu; jkalirai@ucolick.org RI Gaudi, Bernard/I-7732-2012; OI Barranco, Joseph/0000-0003-2045-677X; Hartman, Joel/0000-0001-8732-6166 NR 94 TC 28 Z9 28 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 APR 10 PY 2009 VL 695 IS 1 BP 336 EP 356 DI 10.1088/0004-637X/695/1/336 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500029 ER PT J AU Park, S Kargaltsev, O Pavlov, GG Mori, K Slane, PO Hughes, JP Burrows, DN Garmire, GP AF Park, Sangwook Kargaltsev, Oleg Pavlov, George G. Mori, Koji Slane, Patrick O. Hughes, John P. Burrows, David N. Garmire, Gordon P. TI NONTHERMAL X-RAYS FROM SUPERNOVA REMNANT G330.2+1.0 AND THE CHARACTERISTICS OF ITS CENTRAL COMPACT OBJECT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual (SNR G330.2+1.0); stars: neutron; supernova remnants; X-rays: stars ID NEUTRON-STAR ATMOSPHERES; PARTICLE-ACCELERATION; SHOCK ACCELERATION; MAGNETIC-FIELD; EMISSION; SHELL; ENERGY; HESS; RX-J0852.0-4622; G347.3-0.5 AB We present results from our X-ray data analysis of the supernova remnant (SNR) G330.2+1.0 and its central compact object (CCO), CXOU J160103.1-513353 (J1601 hereafter). Using our XMM-Newton and Chandra observations, we find that the X-ray spectrum of J1601 can be described by neutron star atmosphere models (T(infinity) similar to 2.5-5.5MK). Assuming the distance of d similar to 5 kpc for J1601 as estimated for SNR G330.2+1.0, a small emission region of R similar to 0.4-2 km is implied. X-ray pulsations previously suggested by Chandra are not confirmed by the XMM-Newton data, and are likely not real. However, our timing analysis of the XMM-Newton data is limited by poor photon statistics, and thus pulsations with a relatively low amplitude (i.e., an intrinsic pulsed fraction less than 40%) cannot be ruled out. Our results indicate that J1601 is a CCO similar to that in the Cassiopeia A SNR. X-ray emission from SNR G330.2+1.0 is dominated by power-law continuum (Gamma similar to 2.1-2.5) which primarily originates from thin filaments along the boundary shell. This X-ray spectrum implies synchrotron radiation from shock-accelerated electrons with an exponential roll-off frequency nu(rolloff) similar to 2-3 x 10(17) Hz. For the measured widths of the X-ray filaments (D similar to 0.3 pc) and the estimated shock velocity (v(s) similar to a few x 10(3) km s(-1)), a downstream magnetic field B similar to 10-50 mu G is derived. The estimated maximum electron energy E(max) similar to 27-38 TeV suggests that G330.2+1.0 is a candidate TeV gamma-ray source. We detect faint thermal X-ray emission in G330.2+1.0. We estimate a low preshock density n(0) similar to 0.1 cm(-3), which suggests a dominant contribution from an inverse Compton mechanism (than the proton-proton collision) to the prospective gamma-ray emission. Follow-up deep radio, X-ray, and gamma-ray observations will be essential to reveal the details of the shock parameters and the nature of particle accelerations in this SNR. C1 [Park, Sangwook; Pavlov, George G.; Burrows, David N.; Garmire, Gordon P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kargaltsev, Oleg] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Mori, Koji] Miyazaki Univ, Dept Appl Phys, Nishi Ku, Miyazaki 8892192, Japan. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. RP Park, S (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM park@astro.psu.edu FU NASA [NNX08AW88G, NAS8-03060]; SAO [SV4-74018]; MEXT [18740108] FX The authors thank V. E. Zavlin for the helpful discussion on the hydrogen neutron star atmosphere models. This work was supported in parts by NASA grant NNX08AW88G and SAO grant SV4-74018. P. O. S. acknowledges partial support from NASA contract NAS8-03060. K. M. was partially supported by the Grant in-Aid for Young Scientists (B) of the MEXT (No. 18740108). This work makes use of the Supernova Remnant Catalog by the MOST which is operated by the University of Sydney with support from the Australian Research Council and the Science Foundation for Physics within the University of Sydney. NR 37 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 431 EP 441 DI 10.1088/0004-637X/695/1/431 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500036 ER PT J AU Horan, D Acciari, VA Bradbury, SM Buckley, JH Bugaev, V Byrum, KL Cannon, A Celik, O Cesarini, A Chow, YCK Ciupik, L Cogan, P Falcone, AD Fegan, SJ Finley, JP Fortin, P Fortson, LF Gall, D Gillanders, GH Grube, J Gyuk, G Hanna, D Hays, E Kertzman, M Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ Lee, K Moriarty, P Nagai, T Niemiec, J Ong, RA Perkins, JS Pohl, M Quinn, J Reynolds, PT Rose, HJ Sembroski, GH Smith, AW Steele, D Swordy, SP Toner, JA Vassiliev, VV Wakely, SP Weekes, TC White, RJ Williams, DA Wood, MD Zitzer, B Aller, HD Aller, MF Baker, M Barnaby, D Carini, MT Charlot, P Dumm, JP Fields, NE Hovatta, T Jordan, B Kovalev, YA Kovalev, YY Krimm, HA Kurtanidze, OM Lahteenmaki, A Le Campion, JF Maune, J Montaruli, T Sadun, AC Smith, S Tornikoski, M Turunen, M Walters, R AF Horan, D. Acciari, V. A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. L. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. K. Ciupik, L. Cogan, P. Falcone, A. D. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. F. Gall, D. Gillanders, G. H. Grube, J. Gyuk, G. Hanna, D. Hays, E. Kertzman, M. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Moriarty, P. Nagai, T. Niemiec, J. Ong, R. A. Perkins, J. S. Pohl, M. Quinn, J. Reynolds, P. T. Rose, H. J. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Toner, J. A. Vassiliev, V. V. Wakely, S. P. Weekes, T. C. White, R. J. Williams, D. A. Wood, M. D. Zitzer, B. Aller, H. D. Aller, M. F. Baker, M. Barnaby, D. Carini, M. T. Charlot, P. Dumm, J. P. Fields, N. E. Hovatta, T. Jordan, B. Kovalev, Y. A. Kovalev, Y. Y. Krimm, H. A. Kurtanidze, O. M. Lahteenmaki, A. Le Campion, J. F. Maune, J. Montaruli, T. Sadun, A. C. Smith, S. Tornikoski, M. Turunen, M. Walters, R. TI MULTIWAVELENGTH OBSERVATIONS OF MARKARIAN 421 IN 2005-2006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (Markarian 421); gamma rays: observations; X-rays: individual (Markarian 421) ID ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION; SPECTRAL SLOPE VARIABILITY; TEV BLAZAR MARKARIAN-421; X-RAY; LAC OBJECTS; CORRELATED VARIABILITY; TIMING EXPLORER; PROTON BLAZAR AB Since 2005 September, the Whipple 10 m Gamma-ray Telescope has been operated primarily as a blazar monitor. The five northern hemisphere blazars that have already been detected at the Whipple Observatory, Markarian 421 (Mrk 421), H1426+428, Mrk 501, 1ES 1959+650, and 1ES 2344+514, are monitored routinely each night that they are visible. We report on the Mrk 421 observations taken from 2005 November to 2006 June in the gamma-ray, X-ray, optical, and radio bands. During this time, Mrk 421 was found to be variable at all wavelengths probed. Both the variability and the correlations among different energy regimes are studied in detail here. A tentative correlation, with large spread, was measured between the X-ray and gamma-ray bands, while no clear correlation was evident among the other energy bands. In addition to this, the well-sampled spectral energy distribution of Mrk 421 (1101+384) is presented for three different activity levels. The observations of the other blazar targets will be reported separately. C1 [Horan, D.; Byrum, K. L.; Hays, E.; Smith, A. W.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Phys & Life Sci, Galway, Ireland. [Acciari, V. A.; Kildea, J.; Perkins, J. S.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.; White, R. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Cannon, A.; Grube, J.; Quinn, J.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Cannon, A.; Grube, J.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Celik, O.; Chow, Y. C. K.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Wood, M. D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L. F.; Gyuk, G.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Hanna, D.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Finley, J. P.; Gall, D.; Sembroski, G. H.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Fortin, P.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Hays, E.; Swordy, S. P.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Krennrich, F.; Nagai, T.; Niemiec, J.; Pohl, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Niemiec, J.] Inst Fizyki Hadrowej PAN, PL-31342 Krakow, Poland. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Baker, M.; Dumm, J. P.; Fields, N. E.; Montaruli, T.] Univ Wisconsin, Madison, WI 53706 USA. [Barnaby, D.; Carini, M. T.; Maune, J.; Smith, S.; Walters, R.] Western Kentucky Univ, Bowling Green, KY 42104 USA. [Charlot, P.; Le Campion, J. F.] Univ Bordeaux, Observ Aquitain Sci Univ, F-33271 Floirac, France. [Charlot, P.; Le Campion, J. F.] CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. [Hovatta, T.; Lahteenmaki, A.; Tornikoski, M.; Turunen, M.] Helsinki Univ Technol, Metsahovi Radio Observ, Kylmala 02540, Finland. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 4, Ireland. [Kovalev, Y. A.; Kovalev, Y. Y.] Ctr Astro Space, PN Lebedev Phys Inst, Moscow 117997, Russia. [Kovalev, Y. Y.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Krimm, H. A.] CRESST, Greenbelt, MD 20771 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Kurtanidze, O. M.] Abastumani Observ, Abastumani, GA USA. [Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80208 USA. RP Horan, D (reprint author), Argonne Natl Lab, Div High Energy Phys, 9700 S Cass Ave, Argonne, IL 60439 USA. EM deirdre.horan@gmail.com RI Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Kurtanidze, Omar/J-6237-2014; Kovalev, Yuri/N-1053-2015 OI Kovalev, Yuri/0000-0001-9303-3263; NR 61 TC 35 Z9 35 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 596 EP 618 DI 10.1088/0004-637X/695/1/596 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500050 ER PT J AU Meibom, S Mathieu, RD Stassun, KG AF Meibom, Soren Mathieu, Robert D. Stassun, Keivan G. TI STELLAR ROTATION IN M35: MASS-PERIOD RELATIONS, SPIN-DOWN RATES, AND GYROCHRONOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M35); stars: evolution; stars: late-type; stars: rotation ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; WIYN OPEN CLUSTER; ANGULAR-MOMENTUM EVOLUTION; ALPHA-PERSEI CLUSTER; INTERNAL-ROTATION; YOUNG STARS; RADIAL-VELOCITIES; PROPER MOTIONS; HYADES STARS AB We present the results of a five month photometric time-series survey for stellar rotation over a 40' x 40' field centered on the 150 Myr open cluster M35. We report rotation periods for 441 stars within this field and determine their cluster membership and binarity based on a decade-long radial velocity survey, proper-motion measurements, and multiband photometric observations. We find that 310 of the stars with measured rotation periods are late-type members of M35. The distribution of rotation periods for cluster members span more than 2 orders of magnitude from similar to 0.1 to 15 days, not constrained by the sampling frequency and the timespan of the survey. With an age between the zero-age main sequence and the Hyades, and with similar to 6 times more rotation periods than measured in the Pleiades, M35 permit detailed studies of early rotational evolution of late-type stars. Nearly 80% of the 310 rotators lie on two distinct sequences in the color-period plane, and define clear relations between stellar rotation period and color (mass). The M35 color-period diagram enables us to determine timescales for the transition between the two rotational states, of similar to 60 Myr and similar to 140 Myr for G and K dwarfs, respectively. These timescales are inversely related to the mass of the convective envelope, and offer constraints on the rates of internal and external angular momentum transport and of the evolution of stellar dynamos. A comparison to the Hyades, confirm the Skumanich spin-down dependence for G dwarfs on one rotational state, but suggest that K dwarfs spin down more slowly. The locations of the rotational sequences in the M35 color-period diagram support the use of rotational isochrones to determine ages for coeval stellar populations. We use such gyrochronology to determine "gyro-ages" for M35 from 134 Myr to 161 Myr. We use the M35 data to evaluate new color dependences for the rotational isochrones. C1 Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu FU NSF [AST-0406615]; Danish Research Academy; Kepler mission via NASA [NCC2-1390]; Research Corporation FX We thank the University of Wisconsin-Madison Astronomy Department and NOAO for the time granted on the WIYN 0.9 m and 3.5 m telescopes. We express our appreciation to the site managers and support staff at both telescopes for their exceptional and friendly support. We are thankful to all observers in the WIYN 0.9 m consortium who provided us with high-quality data through the queue-scheduled observing program. This work has been supported by NSF grant AST-0406615 to the UW-Madison, a PhD fellowship from the Danish Research Academy to S. M., partial support to S. M. from the Kepler mission via NASA Cooperative Agreement NCC2-1390, and by the Cottrell Scholarship from the Research Corporation to K. G. S. NR 63 TC 89 Z9 89 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 679 EP 694 DI 10.1088/0004-637X/695/1/679 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500056 ER PT J AU Godfrey, LEH Bicknell, GV Lovell, JEJ Jauncey, DL Gelbord, J Schwartz, DA Marshall, HL Birkinshaw, M Georganopoulos, M Murphy, DW Perlman, ES Worrall, DM AF Godfrey, L. E. H. Bicknell, G. V. Lovell, J. E. J. Jauncey, D. L. Gelbord, J. Schwartz, D. A. Marshall, H. L. Birkinshaw, M. Georganopoulos, M. Murphy, D. W. Perlman, E. S. Worrall, D. M. TI A MULTIWAVELENGTH STUDY OF THE HIGH SURFACE BRIGHTNESS HOT SPOT IN PKS 1421-490 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS 1421-490) ID X-RAY-EMISSION; MAGNETOSONIC SHOCK-WAVES; POWERFUL RADIO GALAXIES; ACTIVE GALACTIC NUCLEI; PARTICLE-ACCELERATION; CYGNUS-A; CHANDRA OBSERVATIONS; PHYSICAL CONDITIONS; RELATIVISTIC JETS; OPTICAL-EMISSION AB Long Baseline Array imaging of the z = 0.663 broadline radio galaxy PKS 1421-490 reveals a 400 pc diameter high surface brightness hot spot at a projected distance of similar to 40 kpc from the active galactic nucleus. The isotropic X-ray luminosity of the hot spot, L2-10 (keV) = 3 x 10(44) ergs s(-1), is comparable to the isotropic X-ray luminosity of the entire X-ray jet of PKS 0637-752, and the peak radio surface brightness is hundreds of times greater than that of the brightest hot spot in Cygnus A. We model the radio to X-ray spectral energy distribution using a one-zone synchrotron self-Compton model with a near equipartition magnetic field strength of 3 mG. There is a strong brightness asymmetry between the approaching and receding hotspots and the hot spot spectrum remains flat (alpha approximate to 0.5) well beyond the predicted cooling break for a 3 mG magnetic field, indicating that the hotspot emission may be Doppler beamed. A high plasma velocity beyond the terminal jet shock could be the result of a dynamically important magnetic field in the jet. There is a change in the slope of the hotspot radio spectrum at GHz frequencies, which we model by incorporating a cutoff in the electron energy distribution at gamma(min) approximate to 650, with higher values implied if the hotspot emission is Doppler beamed. We show that a sharp decrease in the electron number density below a Lorentz factor of 650 would arise from the dissipation of bulk kinetic energy in an electron/proton jet with a Lorentz factor Gamma(jet) greater than or similar to 5. C1 [Godfrey, L. E. H.; Bicknell, G. V.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Godfrey, L. E. H.; Lovell, J. E. J.; Jauncey, D. L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Lovell, J. E. J.] CSIRO, Sydney, NSW 2070, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Schwartz, D. A.; Birkinshaw, M.; Worrall, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Georganopoulos, M.; Perlman, E. S.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. [Georganopoulos, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Murphy, D. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Godfrey, LEH (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. EM lgodfrey@mso.anu.edu.au RI Godfrey, Leith/B-5283-2013 FU Commonwealth of Australia for operation as a National Facility managed by CSIRO; National Aeronautics and Space Administration; National Science Foundation FX L. E. H. G. thanks John Kirk for very helpful discussions on the topic of particle acceleration, and Emil Lenc for supplying the cordump patch for DIFMAP. L. E. H. G. also thanks the Grote Reber Foundation for financial support. The Australia Telescope Compact Array and Long Baseline Array are part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 66 TC 26 Z9 26 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 APR 10 PY 2009 VL 695 IS 1 BP 707 EP 723 DI 10.1088/0004-637X/695/1/707 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500058 ER PT J AU Haas, M Willner, SP Heymann, F Ashby, MLN Fazio, GG Wilkes, BJ Chini, R Siebenmorgen, R Stern, D AF Haas, Martin Willner, S. P. Heymann, Frank Ashby, M. L. N. Fazio, G. G. Wilkes, Belinda J. Chini, Rolf Siebenmorgen, Ralf Stern, Daniel TI CLUSTERING OF RED GALAXIES AROUND THE z=1.53 QUASAR 3C 270.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (3C270.1); infrared: galaxies; quasars: general ID SPITZER-SPACE-TELESCOPE; LYMAN-BREAK GALAXIES; RADIO GALAXIES; DISCOVERY; OBJECTS; IRAC; PROTOCLUSTER; OVERDENSITY; PHOTOMETRY; SOFTWARE AB In the paradigm of hierarchical galaxy formation, luminous radio galaxies mark mass assembly peaks that should contain clusters of galaxies. Observations of the z = 1.53 quasar 3C 270.1 with the Spitzer Space Telescope at 3.6-24 mu m and with the 6.5 m MMT in the z' and Y bands allow the detection of potential cluster members via photometric redshifts. Compared with nearby control fields, there is an excess of similar to 11 extremely red objects (EROs) at 1.33 <= z(phot) <= 1.73, consistent with a protocluster around the quasar. The spectral energy distributions of 3/4 of the EROs are better fitted with passive elliptical galaxies than with dust-reddened starbursts, and of four sources well detected on an archival Hubble Space Telescope (HST) snapshot image, all have undisturbed morphologies. However, one ERO, not covered by the HST image, is a double source with 0.'' 8 separation on the z' image and a marginal (2 sigma) 24 mu m detection indicating a dust-enshrouded starburst. The EROs are more luminous than L(star) (H = -23.6 AB mag at z approximate to 1.5). C1 [Haas, Martin; Heymann, Frank; Chini, Rolf] Ruhr Univ Bochum, Inst Astron, D-44801 Bochum, Germany. [Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.; Wilkes, Belinda J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heymann, Frank; Siebenmorgen, Ralf] European So Observ, D-85748 Garching, Germany. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Haas, M (reprint author), Ruhr Univ Bochum, Inst Astron, Univ Str 150, D-44801 Bochum, Germany. EM haas@astro.rub.de OI Wilkes, Belinda/0000-0003-1809-2364 FU NASA; Nordrhein-Westfalische Akademie der Wissenschaften FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The ground-based observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This research has made use of the NASA/IPAC Extragalactic Database (NED) and of the Sloan Digital Sky Survey (SDSS DR6). We thank Dominik Bomans and Hans Hippelein for valuable discussions and comments on the manuscript, and an anonymous referee for the constructive, critical report. M. H. is supported by the Nordrhein-Westfalische Akademie der Wissenschaften. NR 40 TC 4 Z9 4 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2009 VL 695 IS 1 BP 724 EP 731 DI 10.1088/0004-637X/695/1/724 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 427KZ UT WOS:000264779500059 ER PT J AU Aharonian, F Akhperjanian, AG Anton, G de Almeida, UB Bazer-Bachi, AR Becherini, Y Behera, B Benbow, W Bernlohr, K Boisson, C Bochow, A Borrel, V Brion, E Brucker, J Brun, P Buhler, R Bulik, T Busching, I Boutelier, T Chadwick, PM Charbonnier, A Chaves, RCG Cheesebrough, A Chounet, LM Clapson, AC Coignet, G Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C Dickinson, HJ Djannati-Atai, A Domainko, W Drury, LO Dubois, F Dubus, G Dyks, J Dyrda, M Egberts, K Emmanoulopoulos, D Espigat, P Farnier, C Feinstein, F Fiasson, A Forster, A Fontaine, G Fussling, M Gabici, S Gallant, YA Gerard, L Giebels, B Glicenstein, JF Gluck, B Goret, P Gohring, D Hauser, D Hauser, M Heinz, S Heinzelmann, G Henri, G Hermann, G Hinton, JA Hoffmann, A Hofmann, W Holleran, M Hoppe, S Horns, D Jacholkowska, A de Jager, OC Jahn, C Jung, I Katarzynsky, K Katz, U Kaufmann, S Kendziorra, E Kerschhaggl, M Khangulyan, D Khelifi, B Keogh, D Kluzniak, W Kneiske, T Komin, N Kosack, K Lamanna, G Latham, IJ Lenain, JP Lohse, T Marandon, V Martin, JM Martineau-Huynh, O Marcowith, A Maurin, D McComb, TJL Medina, MC Moderski, R Moulin, E Naumann-Godo, M de Naurois, M Nedbal, D Nekrassov, D Niemiec, J Nolan, SJ Ohm, S Olive, JF Wilhelmi, ED Orford, KJ Ostrowski, M Panter, M Arribas, MP Pedaletti, G Pelletier, G Petrucci, PO Pita, S Puhlhofer, G Punch, M Quirrenbach, A Raubenheimer, BC Raue, M Rayner, SM Renaud, M Rieger, F Ripken, J Rob, L Rosier-Lees, S Rowell, G Rudak, B Rulten, CB Ruppel, J Sahakian, V Santangelo, A Schlickeiser, R Schock, FM Schroder, R Schwanke, U Schwarzburg, S Schwemmer, S Shalchi, A Sikora, M Skilton, JL Sol, H Spangler, D Stawarz, L Steenkamp, R Stegmann, C Superina, G Szostek, A Tam, PH Tavernet, JP Terrier, R Tibolla, O Tluczykont, M van Eldik, C Vasileiadis, G Venter, C Venter, L Vialle, JP Vincent, P Vink, J Vivier, M Volk, HJ Volpe, F Wagner, SJ Ward, M Zdziarski, AA Zech, A AF Aharonian, F. Akhperjanian, A. G. Anton, G. de Almeida, U. Barres Bazer-Bachi, A. R. Becherini, Y. Behera, B. Benbow, W. Bernloehr, K. Boisson, C. Bochow, A. Borrel, V. Brion, E. Brucker, J. Brun, P. Buehler, R. Bulik, T. Buesching, I. Boutelier, T. Chadwick, P. M. Charbonnier, A. Chaves, R. C. G. Cheesebrough, A. Chounet, L. -M. Clapson, A. C. Coignet, G. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. Dickinson, H. J. Djannati-Atai, A. Domainko, W. Drury, L. O'C. Dubois, F. Dubus, G. Dyks, J. Dyrda, M. Egberts, K. Emmanoulopoulos, D. Espigat, P. Farnier, C. Feinstein, F. Fiasson, A. Foerster, A. Fontaine, G. Fuessling, M. Gabici, S. Gallant, Y. A. Gerard, L. Giebels, B. Glicenstein, J. -F. Glueck, B. Goret, P. Goehring, D. Hauser, D. Hauser, M. Heinz, S. Heinzelmann, G. Henri, G. Hermann, G. Hinton, J. A. Hoffmann, A. Hofmann, W. Holleran, M. Hoppe, S. Horns, D. Jacholkowska, A. de Jager, O. C. Jahn, C. Jung, I. Katarzynsky, K. Katz, U. Kaufmann, S. Kendziorra, E. Kerschhaggl, M. Khangulyan, D. Khelifi, B. Keogh, D. Kluzniak, W. Kneiske, T. Komin, Nu. Kosack, K. Lamanna, G. Latham, I. J. Lenain, J. -P. Lohse, T. Marandon, V. Martin, J. M. Martineau-Huynh, O. Marcowith, A. Maurin, D. McComb, T. J. L. Medina, M. C. Moderski, R. Moulin, E. Naumann-Godo, M. de Naurois, M. Nedbal, D. Nekrassov, D. Niemiec, J. Nolan, S. J. Ohm, S. Olive, J. -F. Wilhelmi, E. de Ona Orford, K. J. Ostrowski, M. Panter, M. Arribas, M. Paz Pedaletti, G. Pelletier, G. Petrucci, P. -O. Pita, S. Puehlhofer, G. Punch, M. Quirrenbach, A. Raubenheimer, B. C. Raue, M. Rayner, S. M. Renaud, M. Rieger, F. Ripken, J. Rob, L. Rosier-Lees, S. Rowell, G. Rudak, B. Rulten, C. B. Ruppel, J. Sahakian, V. Santangelo, A. Schlickeiser, R. Schoeck, F. M. Schroeder, R. Schwanke, U. Schwarzburg, S. Schwemmer, S. Shalchi, A. Sikora, M. Skilton, J. L. Sol, H. Spangler, D. Stawarz, L. Steenkamp, R. Stegmann, C. Superina, G. Szostek, A. Tam, P. H. Tavernet, J. -P. Terrier, R. Tibolla, O. Tluczykont, M. van Eldik, C. Vasileiadis, G. Venter, C. Venter, L. Vialle, J. P. Vincent, P. Vink, J. Vivier, M. Voelk, H. J. Volpe, F. Wagner, S. J. Ward, M. Zdziarski, A. A. Zech, A. TI DISCOVERY OF VERY HIGH ENERGY gamma-RAY EMISSION FROM CENTAURUS A WITH HESS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (Cen A); gamma rays: observations ID RADIO-GALAXY CENTAURUS; ACTIVE GALACTIC NUCLEI; COSMIC-RAYS; CHANDRA OBSERVATIONS; TEV EMISSION; M87; BLAZAR; REGION; JETS; RADIATION AB We report the discovery of faint very high energy (VHE; E > 100 GeV) gamma-ray emission from the radio galaxy Centaurus A in observations performed with the High Energy Stereoscopic System (H.E.S.S.) experiment, an imaging atmospheric Cherenkov telescope array consisting of four telescopes located in Namibia. Centaurus A has been observed for more than 120 hr. A signal with a statistical significance of 5.0 sigma is detected from the region including the radio core and the inner kpc jets. The integral flux above an energy threshold of similar to 250 GeV is measured to be 0.8% of the flux of the Crab Nebula (apparent luminosity: L(> 250 GeV) approximate to 2.6 x 1039 erg s(-1), adopting a distance of 3.8 Mpc). The spectrum can be described by a power law with a photon index of 2.7 +/- 0.5(stat) +/- 0.2(sys). No significant flux variability is detected in the data set. However, the low flux only allows detection of variability on the timescale of days to flux increments above a factor of similar to 15-20 (3 sigma and 4 sigma, respectively). The discovery of VHE gamma-ray emission from Centaurus A reveals particle acceleration in the source to > TeV energies and, together with M 87, establishes radio galaxies as a class of VHE emitters. C1 [Boisson, C.; Lenain, J. -P.; Martin, J. M.; Medina, M. C.; Sol, H.; Venter, L.; Zech, A.] Univ Paris, CNRS, Observ Paris, LUTH, F-92190 Meudon, France. [Aharonian, F.; Drury, L. O'C.; Gabici, S.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia. [Anton, G.; Brucker, J.; Glueck, B.; Goehring, D.; Heinz, S.; Jahn, C.; Jung, I.; Katz, U.; Schoeck, F. M.; Stegmann, C.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany. [de Almeida, U. Barres; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Dickinson, H. J.; Keogh, D.; Latham, I. J.; McComb, T. J. L.; Nolan, S. J.; Orford, K. J.; Rayner, S. M.; Rulten, C. B.; Spangler, D.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bazer-Bachi, A. R.; Borrel, V.; Olive, J. -F.] UPS 47, CNRS, Ctr Etud Spatiale Rayonnements, F-31029 Toulouse 4, France. [Becherini, Y.; Djannati-Atai, A.; Espigat, P.; Gerard, L.; Marandon, V.; Wilhelmi, E. de Ona; Pita, S.; Punch, M.; Renaud, M.; Terrier, R.] Univ Paris 07, CNRS, APC, F-75205 Paris 13, France. [Behera, B.; Emmanoulopoulos, D.; Hauser, D.; Hauser, M.; Kaufmann, S.; Pedaletti, G.; Puehlhofer, G.; Quirrenbach, A.; Schwemmer, S.; Tam, P. H.; Tibolla, O.; Wagner, S. J.] Univ Heidelberg, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Benbow, W.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bernloehr, K.; Dalton, M.; Fuessling, M.; Kerschhaggl, M.; Lohse, T.; Arribas, M. Paz; Schwanke, U.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Brion, E.; Brun, P.; Glicenstein, J. -F.; Goret, P.; Komin, Nu.; Moulin, E.; Vivier, M.] CE Saclay, CEA, DSM, IRFU, F-91191 Gif Sur Yvette, France. [Bulik, T.; Dyks, J.; Kluzniak, W.; Moderski, R.; Rudak, B.; Sikora, M.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Buesching, I.; Davids, I. D.; Holleran, M.; de Jager, O. C.; Raubenheimer, B. C.; Venter, C.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa. [Boutelier, T.; Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P. -O.; Szostek, A.] Univ Grenoble 1, CNRS, INSU, Astrophys Lab, F-38041 Grenoble 9, France. [Charbonnier, A.; Jacholkowska, A.; Martineau-Huynh, O.; Maurin, D.; de Naurois, M.; Tavernet, J. -P.; Vincent, P.] Univ Paris 07, Univ Paris 06, CNRS, LPNHE,IN2P3, F-75252 Paris 5, France. [Chounet, L. -M.; Degrange, B.; Fontaine, G.; Giebels, B.; Khelifi, B.; Naumann-Godo, M.; Superina, G.; Volpe, F.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France. [Coignet, G.; Dubois, F.; Lamanna, G.; Rosier-Lees, S.; Vialle, J. P.] CNRS, Lab Annecy Le Vieux Phys Particules, IN2P3, F-74941 Annecy Le Vieux, France. [Davids, I. D.; Steenkamp, R.] Univ Namibia, Windhoek, Namibia. [Dyrda, M.; Niemiec, J.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland. [Farnier, C.; Feinstein, F.; Fiasson, A.; Gallant, Y. A.; Marcowith, A.; Vasileiadis, G.] Univ Montpellier 2, CNRS, IN2P3, Lab Phys Theor Astroparticules,CC 70, F-34095 Montpellier 5, France. [Heinzelmann, G.; Horns, D.; Kneiske, T.; Ripken, J.; Tluczykont, M.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Hinton, J. A.; Skilton, J. L.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Hoffmann, A.; Kendziorra, E.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Katarzynsky, K.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Nedbal, D.; Rob, L.] Charles Univ Prague, Fac Math & Phys, Inst Particle & Nucl Phys, CR-18000 Prague, Czech Republic. [Ostrowski, M.; Stawarz, L.; Szostek, A.] Uniwersytet Jagiellonski, Obserwatorium Astron, Krakow, Poland. [Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Ruppel, J.; Schlickeiser, R.; Schroeder, R.; Shalchi, A.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany. [Vink, J.] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands. [Aharonian, F.; Bernloehr, K.; Bochow, A.; Buehler, R.; Chaves, R. C. G.; Clapson, A. C.; Deil, C.; Domainko, W.; Egberts, K.; Foerster, A.; Hermann, G.; Hofmann, W.; Hoppe, S.; Khangulyan, D.; Kosack, K.; Nekrassov, D.; Ohm, S.; Panter, M.; Raue, M.; Renaud, M.; Rieger, F.; Tibolla, O.; van Eldik, C.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. RP Lenain, JP (reprint author), Univ Paris, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France. EM jean-philippe.lenain@obspm.fr; martin.raue@mpi-hd.mpg.de RI Horns, Dieter/C-9727-2011; Venter, Christo/E-6884-2011; van Eldik, Christopher/C-3901-2013; Katz, Uli/E-1925-2013; Fontaine, Gerard/D-6420-2014; Daniel, Michael/A-2903-2010; Anton, Gisela/C-4840-2013; Drury, Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Komin, Nukri/J-6781-2015 OI Venter, Christo/0000-0002-2666-4812; van Eldik, Christopher/0000-0001-9669-645X; Katz, Uli/0000-0002-7063-4418; Kneiske, Tanja M./0000-0002-3210-6200; Daniel, Michael/0000-0002-8053-7910; Anton, Gisela/0000-0003-2039-4724; Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; Chadwick, Paula/0000-0002-1468-2685; Komin, Nukri/0000-0003-3280-0582 FU German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research [CNRS-IN2P3]; Astroparticle Interdisciplinary Programme of the CNRS; UK Science and Technology Facilities Council (STFC); IPNP of the Charles University; Polish Ministry of Science and Higher Education; South African Department of Science and Technology; National Research Foundation FX The support of the Namibian authorities and the University of Namibia in facilitating the construction and operation of H. E. S. S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and Namibia in the construction and operation of the equipment. 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, and NASA's Astrophysics Data System. NR 47 TC 119 Z9 120 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2009 VL 695 IS 1 BP L40 EP L44 DI 10.1088/0004-637X/695/1/L40 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424BE UT WOS:000264539700009 ER PT J AU Kilic, M Brown, WR Prieto, CA Swift, B Kenyon, SJ Liebert, J Agueros, MA AF Kilic, Mukremin Brown, Warren R. Prieto, Carlos Allende Swift, B. Kenyon, S. J. Liebert, J. Agueros, M. A. TI THE RUNAWAY WHITE DWARF LP400-22 HAS A COMPANION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; stars: individual (LP400-22); white dwarfs ID LOW-MASS; HYPERVELOCITY STARS; MILLISECOND PULSARS; GALACTIC-CENTER; PROPER MOTIONS; BINARY STARS; BLACK-HOLE; VELOCITY; SUPERNOVAE; EVOLUTION AB We report the detection of a radial velocity companion to the extremely low-mass white dwarf (WD) LP400-22. The radial velocity of the WD shows variations with a semiamplitude of 119 km s(-1) and a 0.98776 day period, which implies a companion mass of M >= 0.37 M(circle dot). The optical photometry rules out a main-sequence companion. Thus the invisible companion is another WD or a neutron star. Using proper-motion measurements and the radial velocity of the binary system, we find that it has an unusual Galactic orbit. LP400-22 is moving away from the Galactic center with a velocity of 396 +/- 43 km s(-1), which is very difficult to explain by supernova runaway ejection mechanisms. Dynamical interactions with a massive black hole like that in the Galactic center can in principle explain its peculiar velocity, if the progenitor was a triple star system comprised of a close binary and a distant tertiary companion. Until better proper motions become available, we consider LP400-22 to be most likely a halo star with a very unusual orbit. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Prieto, Carlos Allende] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Swift, B.; Liebert, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Agueros, M. A.] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Kenyon, Scott/0000-0003-0214-609X FU NASA through the Spitzer Space Telescope Fellowship Program; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST 06-02099] FX Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. M. A. Agueros is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST 06-02099. NR 38 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2009 VL 695 IS 1 BP L92 EP L96 DI 10.1088/0004-637X/695/1/L92 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424BE UT WOS:000264539700020 ER PT J AU Bernal, XE Rand, AS Ryan, MJ AF Bernal, Ximena E. Rand, A. Stanley Ryan, Michael J. TI Task differences confound sex differences in receiver permissiveness in tungara frogs SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE mating signals; Physalaemus pustulosus; receiver permissiveness; sexual differences; sexual selection; signal selectivity ID SPECIES SONG DISCRIMINATION; PHYSALAEMUS-PUSTULOSUS; SELECTIVE PHONOTAXIS; ADVERTISEMENT CALLS; FEMALE; BEHAVIOR; MALES; RECOGNITION; BLACKBIRDS; RESPONSES AB In many mating systems, both sexes respond to the same sexual signal. In frogs, males typically call in response to advertisement calls, while females approach male calls in choosing a mate. The costs of signal detection errors are expected to differ between the sexes. Missed opportunities are costly for males because ignoring a signal results in failing to compete with rivals for mates, while their cost for misidentification is lower (time and energy displaying to the incorrect target). By contrast, for females, the cost of misidentification is high (mating with incorrect species or low-quality partner), while their cost for missed opportunity is lower because the operational sex ratio puts females at a premium. Consequently, females should be more selective in their response to signal variation than males. We report that presumed sexual differences in selectivity in tungara frogs (Physalaemus pustulosus) are task-specific rather than sex-specific. As predicted, male tungara frogs are less selective in their vocal responses than are females in their phonotactic responses. Males exhibiting phonotaxis to the same calls, however, are as selective as females, and are significantly more selective than when they respond vocally to the same calls. Our study shows that apparent differences between the sexes emerge from differences in the behaviours themselves and are not intrinsic to each sex. Analogous behavioural differences might confound sex differences in other systems; thus, we suggest consideration of the behavioural plasticity of sex as well as its stereotypy. C1 [Bernal, Ximena E.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Rand, A. Stanley; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. RP Bernal, XE (reprint author), Texas Tech Univ, Dept Biol Sci, POB 43131, Lubbock, TX 79409 USA. EM xbernal@mail.utexas.edu FU National Science Foundation [IBN 0078150] FX We are grateful to the assistants who helped in the phonotaxis experiments. We are also thankful to D. Crews, K. Hoke, R. Page, W. Wilczynski and two anonymous reviewers for their comments on the manuscript. We are particularly grateful to W. Searcy, whose suggestions greatly improved this work. The Smithsonian Tropical Research Institute provided critical logistic support. The Autoridad Nacional del Ambiente, Panama, provided the required permits to perform this research. This work was funded by grant IBN 0078150 from the National Science Foundation. NR 34 TC 14 Z9 14 U1 2 U2 7 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 J9 P R SOC B JI Proc. R. Soc. B-Biol. Sci. PD APR 7 PY 2009 VL 276 IS 1660 BP 1323 EP 1329 DI 10.1098/rspb.2008.0935 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 421IE UT WOS:000264351800016 PM 19141428 ER PT J AU Ward, PS Brady, SG AF Ward, Philip S. Brady, Sean G. TI Rediscovery of the ant genus Amyrmex Kusnezov (Hymenoptera: Formicidae) and its transfer from Dolichoderinae to Leptanilloidinae SO ZOOTAXA LA English DT Article DE ant taxonomy; molecular phylogenetics; dorylomorphs; Leptanilloides; Asphinctanilloides; Neotropical region ID EVOLUTION; REVISION; PHYLOGENY AB The ant genus Amyrmex Kusnezov (1953), previously known only from several males collected more than fifty years ago in Tucuman, Argentina, is redescribed on the basis of more recent material from Argentina and Brazil. Using DNA sequence data from seven nuclear genes we investigate the phylogenetic position of Amyrmex and demonstrate that it is a member of the subfamily Leptanilloidinae, rather than the Dolichoderinae to which it had been previously assigned. This placement is also supported by a reevaluation of morphological traits. Amyrmex is possibly a senior synonym of the worker-based genus Asphinctanilloides Brandao, Diniz, Agosti & Delabie (1999), but additional study is needed to establish generic limits within the Leptanilloidinae and to reliably associate male and worker castes. C1 [Ward, Philip S.] Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. [Brady, Sean G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Ward, PS (reprint author), Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. EM psward@ucdavis.edu; bradys@si.edu FU Ant AToL (Assembling the Tree of Life); NSF [EF-0431330] FX We are grateful to Michael Branstetter for taking the Automontage images. Andrea Lucky and Bonnie Blaimer assisted with DNA sequencing work. Eric Fisher (California Department of Food and Agriculture) kindly answered our queries about habitat and methods of collection at Fazenda Rancho Grande. Brian Fisher and Christian Rabeling provided helpful comments on the manuscript. This research is part of the Ant AToL (Assembling the Tree of Life) Project, supported by NSF grant EF-0431330. NR 16 TC 10 Z9 10 U1 0 U2 0 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 APR 6 PY 2009 IS 2063 BP 46 EP 54 PG 9 WC Zoology SC Zoology GA 429WC UT WOS:000264949800002 ER PT J AU Dalling, JW Brown, TA AF Dalling, James W. Brown, Thomas A. TI Long-Term Persistence of Pioneer Species in Tropical Rain Forest Soil Seed Banks SO AMERICAN NATURALIST LA English DT Article DE carbon dating; pioneer species; seed survival; forest regeneration ID ACCELERATOR MASS-SPECTROMETRY; GAP-PHASE REGENERATION; BOMB C-14 DATA; RECRUITMENT LIMITATION; NEOTROPICAL PIONEERS; TREE DIVERSITY; DISPERSAL; DYNAMICS; SIZE; ENVIRONMENTS AB In tropical forests, pioneer tree species regenerate from seeds dispersed directly into canopy gaps and from seeds that persisted in soil seed banks before gap formation. Life-history models have suggested that selection for the long-term persistence of tree seeds in the soil should be weak because persistence potentially reduces population growth rate by extending generation time and because adult life spans may exceed the return interval of favorable recruitment sites. Here we use accelerator mass spectrometry to carbon-date seeds of three pioneer tree species extracted from undisturbed seed banks in seasonally moist lowland Neotropical forest. We show that seeds of Croton billbergianus, Trema micrantha, and Zanthoxylum ekmannii germinate successfully from surface soil microsites after 38, 31, and 18 years, respectively. Decades-long persistence may be common in large-seeded tropical pioneers and appears to be unrelated to specific regeneration requirements. C1 [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.] Smithsonian Trop Res Inst, Ancon, Panama. [Brown, Thomas A.] Lawrence Livermore Natl Lab, Ctr Accelerator Mass Spectrometry, Livermore, CA 94551 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM dallingj@life.uiuc.edu FU Center for Accelerator Mass Spectrometry; U. S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng48, DE-AC52-07NA27344] FX This research was supported in part by the Center for Accelerator Mass Spectrometry under the University Collaborative Research Program at Lawrence Livermore National Laboratory and was performed in part under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory ( contracts W-7405-Eng48 and DE-AC52-07NA27344). We thank A. Morris and E. Sanchez for assistance in the field and A. Davis, P. Grubb, and S. J. Wright for suggestions that greatly improved the manuscript. NR 42 TC 20 Z9 21 U1 1 U2 28 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 J9 AM NAT JI Am. Nat. PD APR PY 2009 VL 173 IS 4 BP 531 EP 535 DI 10.1086/597221 PG 5 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 415MG UT WOS:000263937300013 PM 19228112 ER PT J AU Ballentine, B AF Ballentine, Barbara TI The ability to perform physically challenging songs predicts age and size in male swamp sparrows, Melospiza georgiana SO ANIMAL BEHAVIOUR LA English DT Article DE female choice; male quality; Melospiza georgiana; reliable signal; sexual selection; song; swamp sparrow; vocal performance ID GREAT REED WARBLERS; REPRODUCTIVE SUCCESS; SEXUAL SELECTION; VOCAL-TRACT; DEVELOPMENTAL STRESS; BIRDSONG PRODUCTION; TERRITORY DEFENSE; FEMALE PREFERENCE; DARWINS FINCHES; EARLY NUTRITION AB Selection should favour female preferences for reliable signals of male quality when such preferences result in benefits to females. Research on bird song suggests that, because song is costly to produce or sustain, females are obtaining accurate information about male quality through song preferences. Females have been shown to express mating preferences for three general categories of costly song features: song output, song complexity and geographical variation. A novel mechanism for the reliability of song is suggested by constraints on the ability to produce rapid, broadband trills (i.e. 'vocal performance'). In several species of birds, females show a preference for superior vocal performance, supporting a key prediction of the hypothesis that vocal performance, like other features of song, may be a reliable indicator of male quality. In this study, I further test this hypothesis by investigating whether female swamp sparrows' preference for vocal performance is favoured by selection because it reliably reflects male quality. I found that vocal performance in male swamp sparrows was correlated with age and size, measured as mass. By preferring males with superior vocal performance, female swamp sparrows may obtain direct and indirect benefits by mating with older larger males. These results support the hypothesis that vocal performance in swamps sparrows is a reliable indicator of male quality. (C) 2009 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Ballentine, Barbara] Duke Univ, Dept Biol, Durham, NC USA. RP Ballentine, B (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM ballentineb@si.edu FU National Science Foundation Doctoral Dissertation Improvement [IBN-0407966] FX I thank Steve Nowicki, Susan Peters, Kimberly Rosvall and Jeremy Hyman for their help in the lab and in the field. I thank Steve Nowicki, Jeremy Hyman, Susan Alberts, Dan McShea, Haven Wiley, Will Wilson and three anonymous referees for their comments on the manuscript. I thank the Pennsylvania Game Commission for permission to conduct this study in Pennsylvania Gamelands. I thank Pymatuning Laboratory of Ecology for support in the field. This project was funded by a National Science Foundation Doctoral Dissertation Improvement Grant IBN-0407966 to S. Nowicki and B. Ballentine. NR 66 TC 51 Z9 51 U1 6 U2 35 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD APR PY 2009 VL 77 IS 4 BP 973 EP 978 DI 10.1016/j.anbehav.2008.12.027 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 420YO UT WOS:000264325300025 ER PT J AU Foley, RJ Matheson, T Blondin, S Chornock, R Silverman, JM Challis, P Clocchiatti, A Filippenko, AV Kirshner, RP Leibundgut, B Sollerman, J Spyromilio, J Tonry, JL Davis, TM Garnavich, PM Jha, SW Krisciunas, K Li, W Pignata, G Rest, A Riess, AG Schmidt, BP Smith, RC Stubbs, CW Tucker, BE Wood-Vasey, WM AF Foley, R. J. Matheson, T. Blondin, S. Chornock, R. Silverman, J. M. Challis, P. Clocchiatti, A. Filippenko, A. V. Kirshner, R. P. Leibundgut, B. Sollerman, J. Spyromilio, J. Tonry, J. L. Davis, T. M. Garnavich, P. M. Jha, S. W. Krisciunas, K. Li, W. Pignata, G. Rest, A. Riess, A. G. Schmidt, B. P. Smith, R. C. Stubbs, C. W. Tucker, B. E. Wood-Vasey, W. M. TI SPECTROSCOPY OF HIGH-REDSHIFT SUPERNOVAE FROM THE ESSENCE PROJECT: THE FIRST FOUR YEARS SO ASTRONOMICAL JOURNAL LA English DT Article DE distance scale; galaxies: distances and redshifts; supernovae: general ID LIGHT-CURVE SHAPES; IA SUPERNOVAE; LEGACY SURVEY; DARK ENERGY; SPECTRA; SPECTROGRAPH; TELESCOPE; CONSTRAINTS; CLASSIFICATION; PHOTOMETRY AB We present the results of spectroscopic observations from the ESSENCE high-redshift supernova (SN) survey during its first four years of operation. This sample includes spectra of all SNe Ia whose light curves were presented by Miknaitis et al. and used in the cosmological analyses of Davis et al. and Wood-Vasey et al. The sample represents 273 hr of spectroscopic observations with 6.5-10 m class telescopes of objects detected and selected for spectroscopy by the ESSENCE team. We present 184 spectra of 156 objects. Combining this sample with that of Matheson et al., we have a total sample of 329 spectra of 274 objects. From this, we are able to spectroscopically classify 118 Type Ia SNe. As the survey has matured, the efficiency of classifying SNe Ia has remained constant while we have observed both higher-redshift SNe Ia and SNe Ia farther from maximum brightness. Examining the subsample of SNe Ia with host-galaxy redshifts shows that redshifts derived from only the SN Ia spectra are consistent with redshifts found from host-galaxy spectra. Moreover, the phases derived from only the SN Ia spectra are consistent with those derived from light-curve fits. By comparing our spectra to local templates, we find that the rate of objects similar to the overluminous SN 1991T and the underluminous SN 1991bg in our sample are consistent with that of the local sample. We do note, however, that we detect no object spectroscopically or photometrically similar to SN 1991bg. Although systematic effects could reduce the high-redshift rate we expect based on the low-redshift surveys, it is possible that SN 1991bg-like SNe Ia are less prevalent at high redshift. C1 [Foley, R. J.; Chornock, R.; Silverman, J. M.; Filippenko, A. V.; Jha, S. W.; Li, W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, R. J.; Blondin, S.; Challis, P.; Kirshner, R. P.; Stubbs, C. W.; Wood-Vasey, W. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matheson, T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Blondin, S.; Leibundgut, B.; Spyromilio, J.] European So Observ, D-85748 Garching, Germany. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Sollerman, J.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Sollerman, J.; Davis, T. M.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Tonry, J. L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Davis, T. M.] Univ Queensland, Dept Phys, Brisbane, Qld 4072, Australia. [Garnavich, P. M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Jha, S. W.] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Krisciunas, K.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Pignata, G.] Univ Chile, Dept Astron, Santiago, Chile. [Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.; Smith, R. C.] Cerro Tololo Interamer Observ, Natl Opt Astron Observ, La Serena, Chile. [Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Riess, A. G.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Schmidt, B. P.; Tucker, B. E.] Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, PO 2611, Australia. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Foley, RJ (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM rfoley@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; Davis, Tamara/A-4280-2008 OI Stubbs, Christopher/0000-0003-0347-1724; Schmidt, Brian/0000-0001-6589-1287; Sollerman, Jesper/0000-0003-1546-6615; Davis, Tamara/0000-0002-4213-8783 FU US National Science Foundation [AST-0443378, AST-0507475]; Danish National Research Foundation; FONDECYT [1051061, 3070034]; FONDAP [15010003]; Bicentenario de Ciencia y Tecnologia de CONICYT and ICM de MIDEPLAN [P06-045-F]; NSF [AST-0307894, AST-0607485]; NASA Long-Term Astrophysics [NAG5-9364]; NASA/HST [GO-09860]; Stanford Linear Accelerator Center; Kavli Institute for Theoretical Physics [AST-0606772, PHY-9907949] FX The ESSENCE survey is supported by the US National Science Foundation through grants AST-0443378 and AST-0507475. The Dark Cosmology Centre is funded by the Danish National Research Foundation. A. C. acknowledges support from grants FONDECYT 1051061, FONDAP 15010003, and P06-045-F (Millennium Center for Supernova Science funded by programs Bicentenario de Ciencia y Tecnologia de CONICYT and ICM de MIDEPLAN). A. V. F.'s supernova group at U. C. Berkeley has been supported by many NSF grants over the past two decades, most recently AST-0307894 and AST-0607485. P. M. G. is supported in part by NASA Long-Term Astrophysics Grant NAG5-9364 and NASA/HST Grant GO-09860. S.J. thanks the Stanford Linear Accelerator Center for support via a Panofsky Fellowship. R. P. K. enjoys support from AST-0606772 and PHY-9907949 to the Kavli Institute for Theoretical Physics. G. P. acknowledges support by the Proyecto FONDECYT 3070034. A. R. thanks the NOAO Goldberg fellowship program for its support. NR 56 TC 24 Z9 24 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2009 VL 137 IS 4 BP 3731 EP 3742 DI 10.1088/0004-6256/137/4/3731 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417AF UT WOS:000264046100001 ER PT J AU Winn, JN Holman, MJ Carter, JA Torres, G Osip, DJ Beatty, T AF Winn, Joshua N. Holman, Matthew J. Carter, Joshua A. Torres, Guillermo Osip, David J. Beatty, Thomas TI THE TRANSIT LIGHT CURVE PROJECT. XI. SUBMILLIMAGNITUDE PHOTOMETRY OF TWO TRANSITS OF THE BLOATED PLANET WASP-4b SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (WASP-4=USNO-B1.0 0479-0948995) ID B-LIKE PLANETS; EXTRASOLAR PLANETS; Y-2 ISOCHRONES; GIANT PLANETS; MASS STARS; STELLAR; PARAMETERS; MAGNITUDE; MODELS; RADIUS AB We present photometry of two transits of the giant planet WASP-4b with a photometric precision of 400-800 parts per million and a time sampling of 25-40 s. The two midtransit times are determined to within 6 s. Together with previously published times, the data are consistent with a constant orbital period, giving no compelling evidence for period variations that would be produced by a satellite or additional planets. Analysis of the new photometry, in combination with stellar-evolutionary modeling, gives a planetary mass and radius of 1.237 +/- 0.064 M(Jup) and 1.365 +/- 0.021 R(Jup), respectively. The planet is 15% larger than expected based on previously published models of solar-composition giant planets. With data of the quality presented here, the detection of transits of a "super-Earth" of radius 1.75 R(circle plus) would have been possible. C1 [Winn, Joshua N.; Carter, Joshua A.; Beatty, Thomas] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.; Carter, Joshua A.; Beatty, Thomas] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Osip, David J.] Carnegie Observ, Campanas Observ, La Serena, Chile. RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Carter, Joshua/A-8280-2013 FU NASA Origins [NNG06GH69G, NNG04LG89G] FX We thank Paul Schechter and Adam Burgasser for observing on our behalf on several occasions, for this project and related projects, and for helpful discussions on observing techniques. Partial support for this work came from NASA Origins grants NNG06GH69G (to M.J.H.) and NNG04LG89G (to G. T.). NR 37 TC 49 Z9 49 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2009 VL 137 IS 4 BP 3826 EP 3833 DI 10.1088/0004-6256/137/4/3826 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 417AF UT WOS:000264046100009 ER PT J AU Brunthaler, A Castangia, P Tarchi, A Henkel, C Reid, MJ Falcke, H Menten, KM AF Brunthaler, A. Castangia, P. Tarchi, A. Henkel, C. Reid, M. J. Falcke, H. Menten, K. M. TI Evidence of a pure starburst nature of the nuclear region of NGC 253 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: interferometric; masers; galaxies: starburst; galaxies: individual: NGC 253 ID H2O MASER EMISSION; SAGITTARIUS-A-ASTERISK; GALAXY NGC-253; SUPERNOVA-REMNANTS; PROPER MOTION; WATER-VAPOR; LINE OBSERVATIONS; GALACTIC-CENTER; SEYFERT-GALAXY; RADIO-SOURCES AB We present high-resolution spectral line and continuum VLBI and VLA observations of the nuclear region of NGC 253 at 22 GHz. While the water vapor masers in this region were detected on arcsecond and milliarcsecond scales, we could not detect any compact continuum emission with a 5 sigma upper limit of similar to 1 mJy. The observations reveal that the water maser emission is not related to a possible low-luminosity active galactic nucleus but is almost certainly associated with star-formation activity. Not detecting any compact continuum source on milliarcsecond scales also questions the presence of a - previously assumed - active nucleus in NGC 253. C1 [Brunthaler, A.; Castangia, P.; Henkel, C.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Castangia, P.; Tarchi, A.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, CA, Italy. [Tarchi, A.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Falcke, H.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM brunthal@mpifr-bonn.mpg.de RI Falcke, Heino/H-5262-2012; OI Falcke, Heino/0000-0002-2526-6724; Tarchi, Andrea/0000-0001-8540-3500; Castangia, Paola/0000-0002-2318-8531 NR 50 TC 21 Z9 21 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 APR PY 2009 VL 497 IS 1 BP 103 EP 108 DI 10.1051/0004-6361/200911615 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 429AG UT WOS:000264892600013 ER PT J AU Winnberg, A Deguchi, S Reid, MJ Nakashima, J Olofsson, H Habing, HJ AF Winnberg, A. Deguchi, S. Reid, M. J. Nakashima, J. Olofsson, H. Habing, H. J. TI CO in OH/IR stars close to the Galactic centre SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: circumstellar matter; stars: mass-loss; Galaxy: bulge; radio lines: ISM; techniques: interferometric ID PRE-MAIN-SEQUENCE; HERBIG-AE STAR; SCUTI PULSATIONAL VARIABILITY; AE/BE STARS; ECLIPSING BINARIES; RS-CHAMAELEONTIS; NONRADIAL PULSATION; LIGHT VARIABILITY; INSTABILITY STRIP; MAGNETIC-FIELD AB Aims. A pilot project has been carried out to measure circumstellar CO emission from three OH/IR stars close to the Galactic centre. The intention was to find out whether it would be possible to conduct a large-scale survey for mass-loss rates using, for example, the Atacama large millimeter array (ALMA). Such a survey would increase our understanding of the evolution of the Galactic bulge. Methods. Two millimetre-wave instruments were used: the Nobeyama Millimeter Array at 115 GHz and the Submillimeter Array at 230 GHz. An interferometer is necessary as a "spatial filter" in this region of space because of the confusion with interstellar CO emission. Results. Towards two of the stars, CO emission was detected with positions and radial velocities coinciding within the statistical errors with the corresponding data of the associated OH sources. However, for one of the stars the line profile is not what one expects for an unresolved expanding circumstellar envelope. We believe that this CO envelope is partially resolved and that this star therefore is a foreground star not belonging to the bulge. Conclusions. The results of the observations have shown that it is possible to detect line profiles of circumstellar CO from late-type stars both within and in the direction of the Galactic bulge. ALMA will be able to detect CO emission in short integrations with sensitivity sufficient to estimate mass-loss rates from a large number of such stars. C1 [Winnberg, A.; Olofsson, H.] Onsala Space Observ, S-43992 Onsala, Sweden. [Deguchi, S.] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nakashima, J.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Nakashima, J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Habing, H. J.] Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. RP Winnberg, A (reprint author), Onsala Space Observ, S-43992 Onsala, Sweden. EM anders.winnberg@chalmers.se RI Nakashima, Jun-ichi/D-3113-2009 OI Nakashima, Jun-ichi/0000-0003-3324-9462 FU FP6 European Coordination Action HELAS; Research Council of the University of Leuven [GOA/2003/04] FX We want to thank the University of Canterbury, New Zealand, for providing us access to their Mt. John 1 m McLellan telescope, but also to the staff of the Mt. John observatory for supporting us during the observing run. W. Z. is supported by the FP6 European Coordination Action HELAS and by the Research Council of the University of Leuven under grant GOA/2003/04. NR 46 TC 1 Z9 1 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 APR PY 2009 VL 497 IS 1 BP 177 EP 194 DI 10.1051/0004-6361/200911655 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 429AG UT WOS:000264892600020 ER PT J AU Kainulainen, J Lada, CJ Rathborne, JM Alves, JF AF Kainulainen, J. Lada, C. J. Rathborne, J. M. Alves, J. F. TI The fidelity of the core mass functions derived from dust column density data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: clouds; ISM: structure; stars: formation; stars: luminosity function, mass function ID OPHIUCHI MOLECULAR CLOUD; 850 MU-M; STAR-FORMATION; CLUMP DISTRIBUTION; INITIAL CONDITIONS; INTERSTELLAR DUST; SCUBA SURVEY; PIPE NEBULA; ORION; POPULATION AB Aims. We examine the recoverability and completeness limits of the dense core mass functions (CMFs) derived for a molecular cloud using extinction data and a core identification scheme based on two-dimensional thresholding. We study how the selection of core extraction parameters affects the accuracy and completeness limit of the derived CMF and the core masses, and also how accurately the CMF can be derived in varying core crowding conditions. Methods. We performed simulations where a population of artificial cores was embedded in the variable background extinction field of the Pipe nebula. We extracted the cores from the simulated extinction maps, constructed the CMFs, and compared them to the input CMFs. The simulations were repeated using a variety of extraction parameters and several core populations with differing input mass functions and differing degrees of crowding. Results. The fidelity of the observed CMF depends on the parameters selected for the core extraction algorithm for our background. More importantly, it depends on how crowded the core population is. We find that the observed CMF recovers the true CMF reliably when the mean separation of cores is larger than the mean diameter of the cores (f > 1). If this condition holds, the derived CMF for the Pipe nebula background is accurate and complete above M greater than or similar to 0.8...1.5 M(circle dot), depending on the parameters used for the core extraction. In the simulations, the best fidelity was achieved with the detection threshold of 1 or 2 times the rms-noise of the extinction data, and with the contour level spacings of 3 times the rms-noise. Choosing a higher threshold and wider level spacings increases the limiting mass. The simulations also show that, when f greater than or similar to 1.5, the masses of individual cores are recovered with a typical uncertainty of 25...30%. When f approximate to 1, the uncertainty is similar to 60%. In very crowded cases where f < 1 the core identification algorithm is unable to recover the masses of the cores adequately, and the derived CMF is unlikely to represent the underlying CMF. For the cores of the Pipe nebula f approximate to 2.0 thereby justifying the use of the method in that region. C1 [Kainulainen, J.] TKK Metsahovi Radio Observ, Kylmala 02540, Finland. [Kainulainen, J.] Univ Helsinki, FIN-00014 Helsinki, Finland. [Lada, C. J.; Rathborne, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alves, J. F.] Ctr Astron Hispano, Calar Alto Observ, Almeria 04004, Spain. RP Kainulainen, J (reprint author), TKK Metsahovi Radio Observ, Metsahovintie 114, Kylmala 02540, Finland. EM jouni.kainulainen@helsinki.fi OI Alves, Joao/0000-0002-4355-0921 NR 27 TC 28 Z9 28 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 APR PY 2009 VL 497 IS 2 BP 399 EP 407 DI 10.1051/0004-6361/200810987 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431XE UT WOS:000265097300010 ER PT J AU Cappelluti, N Brusa, M Hasinger, G Comastri, A Zamorani, G Finoguenov, A Gilli, R Puccetti, S Miyaji, T Salvato, M Vignali, C Aldcroft, T Bohringer, H Brunner, H Civano, F Elvis, M Fiore, F Fruscione, A Griffiths, RE Guzzo, L Iovino, A Koekemoer, AM Mainieri, V Scoville, NZ Shopbell, P Silverman, J Urry, CM AF Cappelluti, N. Brusa, M. Hasinger, G. Comastri, A. Zamorani, G. Finoguenov, A. Gilli, R. Puccetti, S. Miyaji, T. Salvato, M. Vignali, C. Aldcroft, T. Boehringer, H. Brunner, H. Civano, F. Elvis, M. Fiore, F. Fruscione, A. Griffiths, R. E. Guzzo, L. Iovino, A. Koekemoer, A. M. Mainieri, V. Scoville, N. Z. Shopbell, P. Silverman, J. Urry, C. M. TI The XMM-Newton wide-field survey in the COSMOS field The point-like X-ray source catalogue SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; large-scale structure of Universe; X-rays: diffuse background; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; N-LOG S; BRIGHT SERENDIPITOUS SURVEY; HELLAS2XMM SURVEY; NUMBER-COUNTS; SPECTRAL PROPERTIES; OPTICAL IDENTIFICATIONS; LUMINOSITY FUNCTION; LOCKMAN HOLE; CHANDRA AB Context. The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey XMM-COSMOS a powerful tool to detect AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg(2) of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of similar to 1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg(2). Aims. We present the catalogue of point-like X-ray sources detected with the EPIC CCD cameras, the log N - log S relations and the X-ray colour-colour diagrams. Methods. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalogue as well as logN - logS and source density maps have been calibrated using Monte Carlo simulations. Results. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml > 10. The survey, which shows unprecedented homogeneity, has a flux limit of similar to 1.7 x 10(-15) erg cm(-2) s(-1), similar to 9.3 x 10(-15) erg cm(-2) s(-1) and similar to 1.3 x 10(-14) erg cm(-2) s(-1) over 90% of the area (1.92 deg(2)) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy band, respectively. Thanks to the rather homogeneous exposure over a large area, the derived logN - logS relations are very well determined over the flux range sampled by XMM-COSMOS. These relations have been compared with XRB synthesis models, which reproduce the observations with an agreement of similar to 10% in the 5-10 keV and 2-10 keV band, while in the 0.5-2 keV band the agreement is of the order of similar to 20%. The hard X-ray colors confirmed that the majority of the extragalactic sources in a bright subsample are actually type I or type II AGN. About 20% of the sources have a X-ray luminosity typical of AGN (L(X) > 10(42) erg/s) although they do not show any clear signature of nuclear activity in the optical spectrum. C1 [Cappelluti, N.; Brusa, M.; Hasinger, G.; Finoguenov, A.; Boehringer, H.; Brunner, H.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Cappelluti, N.; Brusa, M.; Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Comastri, A.; Zamorani, G.; Gilli, R.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico. [Salvato, M.; Scoville, N. Z.; Shopbell, P.] CALTECH, Pasadena, CA 91125 USA. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Aldcroft, T.; Civano, F.; Elvis, M.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fiore, F.] Osserv Astron Roma, INAF, I-00044 Monte Porzio Catone, Italy. [Griffiths, R. E.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Guzzo, L.; Iovino, A.] INAF Osservatorio Astron Brera, Milan, Italy. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Mainieri, V.] ESO, D-85748 Garching, Germany. [Silverman, J.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Urry, C. M.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. RP Cappelluti, N (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany. EM cappelluti@mpe.mpg.de RI Vignali, Cristian/J-4974-2012; Urry, Claudia/G-7381-2011; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Urry, Claudia/0000-0002-0745-9792; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Cappelluti, Nico/0000-0002-1697-186X; Koekemoer, Anton/0000-0002-6610-2048; Puccetti, Simonetta/0000-0002-2734-7835; Fiore, Fabrizio/0000-0002-4031-4157 FU German Deutsche Forschungsgemeinschaft [Ts 17/2-1]; Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt; Max-Planck society; NASA [NNX07AV03G]; PRIN/MIUR [2006-02-5203]; ASI-INAF [I/023/05/00, I/088/06]; German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize [FKZ HA 1850/28-1] FX Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2-1. In Germany the XMM-Newton project is supported by the Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt and the Max-Planck society. N.C. and A. F. were partially supported from a NASA grant NNX07AV03G to UMBC. In Italy, the XMM-COSMOS project is supported by PRIN/MIUR under grant 2006-02-5203 and ASI-INAF grants I/023/05/00, I/088/06. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). N.C. gratefully acknowledges Ezequiel Treister for providing his prediction of the XRB logN - logS. The entire COSMOS collaboration is gratefully acknowledged. N.C. acknowledges UNAM-Ensenada for the hospitality during his visit. NR 59 TC 158 Z9 158 U1 0 U2 1 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 APR PY 2009 VL 497 IS 2 BP 635 EP 648 DI 10.1051/0004-6361/200810794 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 431XE UT WOS:000265097300035 ER PT J AU Wang, JF Fabbiano, G Elvis, M Risaliti, G Mazzarella, JM Howell, JH Lord, S AF Wang, Junfeng Fabbiano, G. Elvis, M. Risaliti, G. Mazzarella, J. M. Howell, J. H. Lord, S. TI IMAGING THE CIRCUMNUCLEAR REGION OF NGC 1365 WITH CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: active; galaxies: individual (NGC 1365); galaxies: starburst; X-rays: galaxies; X-rays: ISM ID X-RAY-EMISSION; HUBBLE-SPACE-TELESCOPE; INTRACLUSTER MEDIUM ENRICHMENT; EXTRAGALACTIC DISTANCE SCALE; HOT INTERSTELLAR-MEDIUM; BARRED SPIRAL GALAXY; EXTENDED IONIZED-GAS; NARROW-LINE REGION; SEYFERT 2 GALAXIES; STAR-FORMATION AB We present the first Chandra/ACIS imaging study of the circumnuclear region of the nearby Seyfert galaxy NGC 1365. The X-ray emission is resolved into pointlike sources and complex, extended emission. The X-ray morphology of the extended emission shows a biconical soft X-ray-emission region extending similar to 5 kpc in projection from the nucleus, coincident with the high-excitation outflow cones seen in optical emission lines particularly to the northwest. Harder X-ray emission is detected from a kpc-diameter circumnuclear ring, coincident with the star-forming ring prominent in the Spitzer mid-infrared (IR) images; this X-ray emission is partially obscured by the central dust lane of NGC 1365. Spectral fitting of spatially separated components indicates a thermal plasma origin for the soft extended X-ray emission (kT = 0.57 keV). Only a small amount of this emission can be due to photoionization by the nuclear source. Detailed comparison with [O III]lambda 5007 observations shows that the hot interstellar medium (ISM) is spatially anticorrelated with the [O III]-emitting clouds and has thermal pressures comparable to those of the [O III] media, suggesting that the hot ISM acts as a confining medium for the cooler photoionized clouds. The abundance ratios of the hot ISM are fully consistent with the theoretical values for enrichment from Type II supernovae, suggesting that the hot ISM is a wind from the starburst circumnuclear ring. X-ray emission from a similar to 450 pc long nuclear radio jet is also detected to the southeast. C1 [Wang, Junfeng; Fabbiano, G.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzarella, J. M.; Howell, J. H.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM juwang@cfa.harvard.edu; pepi@cfa.harvard.edu; elvis@cfa.harvard.edu; risaliti@cfa.harvard.edu; mazz@ipac.caltech.edu; jhhowell@ipac.caltech.edu; lord@ipac.caltech.edu RI Wang, Junfeng/A-1476-2011; OI Risaliti, Guido/0000-0002-3556-977X; Mazzarella, Joseph/0000-0002-8204-8619 FU NASA [NAS8-39073]; Chandra GO [G06-7102X] FX We thank an anonymous referee for helpful comments that improved the clarity of the manuscript. We are grateful to S. Veilleux for providing us the [O III] images in Veilleux et al. (2003), and Tim Kallman for the helpful information about XSTAR. J.W. thanks A. Baldi for his help in the data analysis, H. Oti Floranes for providing the model results in Mas-Hesse et al. (2008), and A. Siemiginowska for helpful discussion on radio jets. G. F. and M. E. acknowledge stimulating discussions at the Aspen Center for Physics workshop on Active Galactic Nuclei. This work is supported by NASA Contract NAS8-39073 (CXC) and Chandra GO Grant G06-7102X (PI: Risaliti). NR 137 TC 36 Z9 36 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 APR 1 PY 2009 VL 694 IS 2 BP 718 EP 733 DI 10.1088/0004-637X/694/2/718 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900002 ER PT J AU McQuinn, M Lidz, A Zaldarriaga, M Hernquist, L Hopkins, PF Dutta, S Faucher-Giguere, CA AF McQuinn, Matthew Lidz, Adam Zaldarriaga, Matias Hernquist, Lars Hopkins, Philip F. Dutta, Suvendra Faucher-Giguere, Claude-Andre TI He II REIONIZATION AND ITS EFFECT ON THE INTERGALACTIC MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmology: theory; intergalactic medium ID LY-ALPHA FOREST; SUPERMASSIVE BLACK-HOLES; EQUATION-OF-STATE; PARTICLE HYDRODYNAMICS SIMULATIONS; IONIZING-RADIATION FLUCTUATIONS; TEMPERATURE-DENSITY RELATION; LARGE-SCALE STRUCTURE; SUBARU DEEP FIELD; METAL-LINE RATIOS; DARK-MATTER MODEL AB Observations of the intergalactic medium (IGM) suggest that quasars reionize He II in the IGM at z approximate to 3. We have run a set of 190 and 430 comoving Mpc simulations of He II being reionized by quasars to develop an understanding of the nature of He II reionization and its potential impact on observables. We find that He II reionization heats regions in the IGM by as much as 25,000 K above the temperature that is expected otherwise, with the volume-averaged temperature increasing by similar to 12,000 K and with large temperature fluctuations on similar to 50 Mpc scales. Much of this heating occurs far from quasars by photons with long mean free path. We find a temperature-density equation of state of gamma - 1 approximate to 0.3 during He II reionization, but with a wide dispersion in this relation having sigma(T) similar to 10(4) K. He II reionization by the observed population of quasars cannot produce an inverted relation (gamma - 1 < 0). Our simulations are consistent with the observed evolution in the mean transmission of the He II Ly alpha forest. We argue that the heat input from He II reionization is unable to cause the observed depression at z approximate to 3.2 in the H I Ly alpha forest opacity as has been suggested. We investigate how uncertainties in the properties of QSOs and of He II Lyman limit systems influence our predictions. C1 [McQuinn, Matthew; Lidz, Adam; Zaldarriaga, Matias; Hernquist, Lars; Hopkins, Philip F.; Dutta, Suvendra; Faucher-Giguere, Claude-Andre] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Lab Phys, Cambridge, MA 02138 USA. RP McQuinn, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmcquinn@cfa.harvard.edu FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690, AST 05-06556]; NASA ATP [NAG5-12140, NAG5-13292, NAG5-13381, NNG-05GJ40G]; David and Lucile Packard; Alfred P. Sloan; John D. and Catherine T. MacArthur Foundations FX Many thanks to Mark Dijkstra, Alexandre Tchekhovskoi, and Hy Trac for interesting discussions, and to James Bolton and Steven Furlanetto for providing useful comments on the manuscript. M. M. is supported by the NSF graduate student fellowship. This work was supported in part by NSF grants ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690, and AST 05-06556, and NASA ATP grants NAG5-12140, NAG5-13292, NAG5-13381, and NNG-05GJ40G. Further support was provide by the David and Lucile Packard, the Alfred P. Sloan, and the John D. and Catherine T. MacArthur Foundations. NR 102 TC 126 Z9 126 U1 1 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 APR 1 PY 2009 VL 694 IS 2 BP 842 EP 866 DI 10.1088/0004-637X/694/2/842 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900010 ER PT J AU Mroczkowski, T Bonamente, M Carlstrom, JE Culverhouse, TL Greer, C Hawkins, D Hennessy, R Joy, M Lamb, JW Leitch, EM Loh, M Maughan, B Marrone, DP Miller, A Muchovej, S Nagai, D Pryke, C Sharp, M Woody, D AF Mroczkowski, Tony Bonamente, Max Carlstrom, John E. Culverhouse, Thomas L. Greer, Christopher Hawkins, David Hennessy, Ryan Joy, Marshall Lamb, James W. Leitch, Erik M. Loh, Michael Maughan, Ben Marrone, Daniel P. Miller, Amber Muchovej, Stephen Nagai, Daisuke Pryke, Clem Sharp, Matthew Woody, David TI APPLICATION OF A SELF-SIMILAR PRESSURE PROFILE TO SUNYAEV-ZEL'DOVICH EFFECT DATA FROM GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: individual (Abell 1835, Abell 1914, CL J1226.9+3332); X-rays: galaxies: clusters ID RAY-IMAGING-SPECTROSCOPY; COSMIC DISTANCE SCALE; X-RAY; XMM-NEWTON; TEMPERATURE PROFILES; HOT PLASMA; MASS; GAS; CONSTRAINTS; SAMPLE AB We investigate the utility of a new, self-similar pressure profile for fitting Sunyaev-Zel'dovich (SZ) effect observations of galaxy clusters. Current SZ imaging instruments-such as the Sunyaev-Zel'dovich Array (SZA)-are capable of probing clusters over a large range in a physical scale. A model is therefore required that can accurately describe a cluster's pressure profile over a broad range of radii from the core of the cluster out to a significant fraction of the virial radius. In the analysis presented here, we fit a radial pressure profile derived from simulations and detailed X-ray analysis of relaxed clusters to SZA observations of three clusters with exceptionally high-quality X-ray data: A1835, A1914, and CL J1226.9+3332. From the joint analysis of the SZ and X-ray data, we derive physical properties such as gas mass, total mass, gas fraction and the intrinsic, integrated Compton y-parameter. We find that parameters derived from the joint fit to the SZ and X-ray data agree well with a detailed, independent X-ray-only analysis of the same clusters. In particular, we find that, when combined with X-ray imaging data, this new pressure profile yields an independent electron radial temperature profile that is in good agreement with spectroscopic X-ray measurements. C1 [Mroczkowski, Tony; Miller, Amber] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Mroczkowski, Tony; Muchovej, Stephen] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Mroczkowski, Tony] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bonamente, Max] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, Max; Joy, Marshall] NASA, Dept Space Sci, George C Marshall Space Flight Ctr, Huntsville, AL 35899 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Loh, Michael; Marrone, Daniel P.; Pryke, Clem; Sharp, Matthew] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Carlstrom, John E.; Culverhouse, Thomas L.; Greer, Christopher; Hennessy, Ryan; Leitch, Erik M.; Pryke, Clem] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, John E.; Marrone, Daniel P.; Pryke, Clem] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, John E.; Loh, Michael; Sharp, Matthew] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Hawkins, David; Lamb, James W.; Woody, David] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. [Maughan, Ben] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Maughan, Ben] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, Amber] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Nagai, Daisuke] Yale Univ, Yale Ctr Astron Astrophys, New Haven, CT 06520 USA. RP Mroczkowski, T (reprint author), Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski, Tony/0000-0003-3816-5372 FU James S. McDonnell Foundation; National Science Foundation [AST-0604982, PHY-0114422, AST-0507545, AST-05-07161]; University of Chicago; Sloan Fellowship; NRAO Jansky Fellowship; Chandra Fellowship FX We thank John Cartwright, Ben Reddall, and Marcus Runyan for their significant contributions to the construction and commissioning of the SZA instrument. We thank Esra Bulbul and Nicole Hasler for their insights, comments, and help with Chandra X-ray Observatory (CXO) data reduction and figure production. We thank the staff of the Owens Valley Radio Observatory and CARMA for their outstanding support. We thank Samuel LaRoque for his help with the modeling code. We gratefully acknowledge the James S. McDonnell Foundation, the National Science Foundation and the University of Chicago for funding to construct the SZA. The operation of the SZA is supported by NSF Division of Astronomical Sciences through grant AST-0604982. Partial support is provided by NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, and by NSF grants AST-0507545 and AST-05-07161 to Columbia University. A. M. acknowledges support from a Sloan Fellowship, D. P. M. from an NRAO Jansky Fellowship, B. M. from a Chandra Fellowship, and C. G., S. M., and M. S. from NSF Graduate Research Fellowships. NR 52 TC 49 Z9 49 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1034 EP 1044 DI 10.1088/0004-637X/694/2/1034 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900024 ER PT J AU Poznanski, D Butler, N Filippenko, AV Ganeshalingam, M Li, WD Bloom, JS Chornock, R Foley, RJ Nugent, PE Silverman, JM Cenko, SB Gates, EL Leonard, DC Miller, AA Modjaz, M Serduke, FJD Smith, N Swift, BJ Wong, DS AF Poznanski, Dovi Butler, Nathaniel Filippenko, Alexei V. Ganeshalingam, Mohan Li, Weidong Bloom, Joshua S. Chornock, Ryan Foley, Ryan J. Nugent, Peter E. Silverman, Jeffrey M. Cenko, S. Bradley Gates, Elinor L. Leonard, Douglas C. Miller, Adam A. Modjaz, Maryam Serduke, Frank J. D. Smith, Nathan Swift, Brandon J. Wong, Diane S. TI IMPROVED STANDARDIZATION OF TYPE II-P SUPERNOVAE: APPLICATION TO AN EXPANDED SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; distance scale; dust, extinction; supernovae: general ID QUANTITATIVE SPECTROSCOPIC ANALYSIS; IA SUPERNOVAE; PHOTOSPHERE METHOD; INFRARED OBSERVATIONS; LUMINOUS SUPERNOVA; OPTICAL PHOTOMETRY; DARK ENERGY; SN 2005CS; DISTANCE; GALAXY AB In the epoch of precise and accurate cosmology, cross-confirmation using a variety of cosmographic methods is paramount to circumvent systematic uncertainties. Owing to progenitor histories and explosion physics differing from those of Type Ia supernovae (SNe Ia), Type II-plateau supernovae (SNe II-P) are unlikely to be affected by evolution in the same way. Based on a new analysis of 17 SNe II-P, and on an improved methodology, we find that SNe II-P are good standardizable candles, almost comparable to SNe Ia. We derive a tight Hubble diagram with a dispersion of 10% in distance, using the simple correlation between luminosity and photospheric velocity introduced by Hamuy and Pinto. We show that the descendent method of Nugent et al. can be further simplified and that the correction for dust extinction has low statistical impact. We find that our SN sample favors, on average, a very steep dust law with total to selective extinction R(V) < 2. Such an extinction law has been recently inferred for many SNe Ia. Our results indicate that a distance measurement can be obtained with a single spectrum of a SN II-P during the plateau phase combined with sparse photometric measurements. C1 [Poznanski, Dovi; Butler, Nathaniel; Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong; Bloom, Joshua S.; Chornock, Ryan; Foley, Ryan J.; Silverman, Jeffrey M.; Cenko, S. Bradley; Miller, Adam A.; Modjaz, Maryam; Serduke, Frank J. D.; Smith, Nathan; Wong, Diane S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Gates, Elinor L.] Univ Calif Santa Cruz, Lick Observ, Mt Hamilton, CA 95140 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Swift, Brandon J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Poznanski, D (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM dovi@berkeley.edu NR 95 TC 75 Z9 75 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1067 EP 1079 DI 10.1088/0004-637X/694/2/1067 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900027 ER PT J AU Taylor, EN Franx, M van Dokkum, PG Bell, EF Brammer, GB Rudnick, G Wuyts, S Gawiser, E Lira, P Urry, CM Rix, HW AF Taylor, Edward N. Franx, Marijn van Dokkum, Pieter G. Bell, Eric F. Brammer, Gabriel B. Rudnick, Gregory Wuyts, Stijn Gawiser, Eric Lira, Paulina Urry, C. Megan Rix, Hans-Walter TI THE RISE OF MASSIVE RED GALAXIES: THE COLOR-MAGNITUDE AND COLOR-STELLAR MASS DIAGRAMS FOR z(phot) <= 2 FROM THE MULTIWAVELENGTH SURVEY BY YALE-CHILE SO ASTROPHYSICAL JOURNAL LA English DT Review DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: luminosity function, mass function; galaxies: stellar content ID DEEP FIELD-SOUTH; DIGITAL SKY SURVEY; STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; BAND OPTICAL-PROPERTIES; GOODS-MUSIC SAMPLE; LUMINOSITY FUNCTION; FORMING GALAXIES; PHOTOMETRIC REDSHIFTS; PHYSICAL-PROPERTIES AB We present the color-magnitude and color-stellar mass diagrams for galaxies with z(phot) <= 2, based on a K-(AB) < 22 catalog of the 1/2 x 1/2 square degrees. Extended Chandra Deep Field South from the MUltiwavelength Survey by Yale-Chile. Our main sample of 7840 galaxies contains 1297 M-* > 10(11)M circle dot galaxies in the range 0.2 < z(phot) < 1.8. We show empirically that this catalog is approximately complete for M-* > 10(11) M circle dot galaxies for z(phot) < 1.8. For this mass-limited sample, we show that the locus of the red sequence color-stellar mass relation evolves as Delta(u- r) alpha (-0.44 +/- 0.02) z(phot) for z(phot) less than or similar to 1.2. For z(phot) greater than or similar to 1.3, however, we are no longer able to reliably distinguish red and blue subpopulations from the observed color distribution; we show that this would require much deeper near-infrared data. At 1.5 < z(phot) < 1.8, the comoving number density of M-* > 10(11)M circle dot galaxies is approximate to 50% of the local value, with a red fraction of approximate to 33%. Making a parametric fit to the observed evolution, we find n(tot)(z) alpha (1 + z(phot))(-0.52 +/- 0.12(+/- 0.20)). We find stronger evolution in the red fraction: f(red)(z) alpha (1 + z(phot))(-1.17 +/- 0.18(+/- 0.21)). Through a series of sensitivity analyses, we show that the most important sources of systematic error are (1) systematic differences in the analysis of the z approximate to 0 and z >> 0 samples; (2) systematic effects associated with details of the photometric redshift calculation; and (3) uncertainties in the photometric calibration. With this in mind, we show that our results based on photometric redshifts are consistent with a completely independent analysis which does not require redshift information for individual galaxies. Our results suggest that, at most, 1/5 of local red sequence galaxies with M-* > 10(11) M circle dot were already in place at z similar to 2. C1 [Taylor, Edward N.; Franx, Marijn] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [van Dokkum, Pieter G.; Brammer, Gabriel B.; Urry, C. Megan] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bell, Eric F.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Rudnick, Gregory] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Wuyts, Stijn] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Lira, Paulina] Univ Chile, Dept Astron, Santiago, Chile. RP Taylor, EN (reprint author), Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. EM ent@strw.leidenuniv.nl RI Urry, Claudia/G-7381-2011; Taylor, Edward/C-6458-2015; Lira, Paulina/G-8536-2016 OI Urry, Claudia/0000-0002-0745-9792; Taylor, Edward/0000-0002-3958-0343; NR 108 TC 52 Z9 54 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 APR 1 PY 2009 VL 694 IS 2 BP 1171 EP 1199 DI 10.1088/0004-637X/694/2/1171 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900037 ER PT J AU Wolk, SJ Lisse, CM Bodewits, D Christian, DJ Dennerl, K AF Wolk, S. J. Lisse, C. M. Bodewits, D. Christian, D. J. Dennerl, K. TI CHANDRA'S CLOSE ENCOUNTER WITH THE DISINTEGRATING COMETS 73P/2006 (SCHWASSMANN-WACHMANN 3) FRAGMENT B AND C/1999 S4 (LINEAR) SO ASTROPHYSICAL JOURNAL LA English DT Article DE comets: individual (Schwassmann-Wachmann 3, Fragment B, Comet C/1999 S4); solar wind; techniques: spectroscopic ID X-RAY-EMISSION; EXTREME-ULTRAVIOLET EMISSION; SOLAR-WIND IONS; BOW SHOCK; PLASMA; HALLEY; GAS; 9P/TEMPEL-1; ATMOSPHERES; HYAKUTAKE AB On 2006 May 23, we used the ACIS-S instrument on Chandra to study the X-ray emission from the B fragment of comet 73P/2006 (Schwassmann-Wachmann 3) (73P/B). We obtained a total of 20 ks of Chandra observation time of Fragment B, and also investigated contemporaneous Advanced Composition Explorer and Solar and Heliospheric Observatory solar wind physical data. The Chandra data allow us to spatially resolve the detailed structure of the interaction zone between the solar wind and the fragment's coma at a resolution of similar to 1000 km, and to observe the X-ray emission due to multiple comet-like bodies. We detect a change in the spectral signature with the ratio of the C V/O VII line increasing with increasing collisional opacity as predicted by Bodewits et al. The line fluxes arise from a combination of solar wind speed, the species that populate the wind, and the gas density of the comet. We are able to understand some of the observed X-ray morphology in terms of nongravitational forces that act upon an actively outgassing comet's debris field. We have used the results of the Chandra observations on the highly fragmented 73P/B debris field to reanalyze and interpret the mysterious emission seen from comet C/1999 S4 (LINEAR) on 2000 August 1, after the comet had completely disrupted. We find the physical situations to be similar in both cases, with extended X-ray emission due to multiple, small outgassing bodies in the field of view. Nevertheless, the two comets interacted with completely different solar winds, resulting in distinctly different spectra. C1 [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Bodewits, D.] Univ Groningen, KVI Atom Phys, NL-9747 AA Groningen, Netherlands. [Christian, D. J.] Eureka Sci Inc, Oakland, CA 94602 USA. [Dennerl, K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. 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 CXC [DD6-7040X, GO4-5167X]; NASA [NAS8-03060]; Netherlands Organisation for Scientific Research (NWO); High Energy Astrophysics Division; Institute of Theoretical Atomic FX We thank H. Tananbaum for use of Director's Discretionary time for this unusual object. We thank D. Koutroumpa and V. Kharchenko for helpful discussions on the C v contamination issue. We are grateful for the cometary ephemerides of D. K. Yeomans published at the JPL/HorizonsWeb site. Proton velocities and ion measurements used here are courtesy of the SOHO/CELIAS/PM and ACE/SWICS teams, respectively. The CXC guest investigator program supported this work through grants DD6-7040X ( S. J. W.) and GO4-5167X ( C. M. L.). S. J. W. was supported by NASA contract NAS8-03060. D. B. wishes to acknowledge travel support from the Netherlands Organisation for Scientific Research (NWO), the High Energy Astrophysics Division at the Center of Astrophysics, and the Visiting Scholars Program of the Institute of Theoretical Atomic, Molecular and Optical Physics at the Center for Astrophysics. NR 59 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1293 EP 1308 DI 10.1088/0004-637X/694/2/1293 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900046 ER PT J AU Lee, CF Mao, YY Reipurth, B AF Lee, Chin-Fei Mao, Yao-Yuan Reipurth, Bo TI INFALL AND ROTATION MOTIONS IN THE HH 111 PROTOSTELLAR SYSTEM: A FLATTENED ENVELOPE IN TRANSITION TO A DISK? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: individual (HH 111); stars: formation ID HERBIG-HARO JETS; SUBMILLIMETER ARRAY; MAGNETIC BRAKING; STAR-FORMATION; ORION NEBULA; YOUNG STARS; COLLAPSE; OUTFLOWS; KINEMATICS; DISTANCE AB We have mapped the central region of the HH 111 protostellar system in 1.33 mm continuum, C(18)O (J = 2-1), (13)CO (J = 2-1), and SO (N(J) = 5(6)-4(5)) emissions at similar to 3 '' resolution with the Submillimeter Array. There are two sources, VLA 1 (= IRAS 05491+0247) and VLA 2, with the VLA 1 source driving the HH111 jet. Thermal emission is seen in 1.33 mm continuum tracing the dust in the envelope and the putative disks around the sources. A flattened, toruslike envelope is seen in C(18)O and (13)CO around the VLA 1 source surrounding the dust lane perpendicular to the jet axis, with an inner radius of similar to 400 AU (1 ''),an outer radius of similar to 3200 AU (8 ''), and a thickness of similar to 1000 AU (2 ''.5). It seems to be infalling toward the center with the conservation of specific angular momentum rather than with a Keplerian rotation as assumed by Yang et al. An inner envelope is seen in SO, with a radius of similar to 500 AU (1 ''.3). The inner part of this inner envelope, which is spatially coincident with the dust lane, seems to have a differential rotation and thus may have formed a rotationally supported disk. The outer part of this inner envelope, however, may have a rotation velocity decreasing toward the center and thus represent a region where an infalling envelope is in transition to a rotationally supported disk. A brief comparison with a collapsing model suggests that the flattened, toruslike envelope seen in C(18)O and (13)CO could result from a collapse of a magnetized rotating toroid. C1 [Lee, Chin-Fei] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lee, Chin-Fei] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Mao, Yao-Yuan] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Reipurth, Bo] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw OI Mao, Yao-Yuan/0000-0002-1200-0820 FU Smithsonian Institution; Academia Sinica 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. NR 33 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1395 EP 1401 DI 10.1088/0004-637X/694/2/1395 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900054 ER PT J AU Shporer, A Mazeh, T Pont, F Winn, JN Holman, MJ Latham, DW Esquerdo, GA AF Shporer, Avi Mazeh, Tsevi Pont, Frederic Winn, Joshua N. Holman, Matthew J. Latham, David W. Esquerdo, Gilbert A. TI PHOTOMETRIC FOLLOW-UP OBSERVATIONS OF THE TRANSITING NEPTUNE-MASS PLANET GJ 436b SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (GJ 436); planetary systems ID HUBBLE-SPACE-TELESCOPE; EXTRA-SOLAR PLANETS; STELLAR ATMOSPHERE MODELS; LIGHT-CURVE PROJECT; LIMB-DARKENING LAW; M-DWARF GJ-436; M-CIRCLE-PLUS; 16 CYGNI B; HARPS SEARCH; IMPROVED PARAMETERS AB This paper presents multiband photometric follow-up observations of the Neptune-mass transiting planet GJ 436b, consisting of five new ground-based transit light curves obtained in 2007 May. Together with one already published light curve, we have at hand a total of six light curves, spanning 29 days. The analysis of the data yields an orbital period P = 2.64386 +/- 0.00003 days, midtransit time T(c) [HJD] = 2454235.8355 +/- 0.0001, planet mass M (p) = 23.1 +/- 0.9 M(circle dot) = 0.073 +/- 0.003 M (Jup), planet radius R(p) = 4.2 +/- 0.2 R(circle plus) = 0.37 +/- 0.01 R(Jup), and stellar radius R(s) = 0.45 +/- 0.02 R(circle dot). Our typical precision for the midtransit timing for each transit is about 30 s. We searched the data for a possible signature of a second planet in the system through transit timing variations (TTV) and variation of the impact parameter. The analysis could not rule out a small, of the order of a minute, TTV and a long-term modulation of the impact parameter, of the order of +0.2 yr(-1). C1 [Shporer, Avi; Mazeh, Tsevi] Tel Aviv Univ, Wise Observ, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel. [Pont, Frederic] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Latham, David W.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Esquerdo, Gilbert A.] Planetary Sci Inst, Tucson, AZ 85705 USA. RP Shporer, A (reprint author), Tel Aviv Univ, Wise Observ, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel. FU United States-Israel Binational Science Foundation [2006234]; Kepler Mission under NASA Cooperative Agreement [NCC 2-1390]; Smithsonian Astrophysical Observatory; NASA Origins grant [NNG06GH69G] FX We are deeply thankful to Michael Gillon for his photometric processing of the data obtained on 2007 May 4 and May 25. We thank the anonymous referee for his thorough reading of the paper and his useful comments which helped improve the paper. T. Mazeh and A. Shporer thank Elia Leibowitz and Liliana Formiggini for allowing the use of their telescope time at the Wise Observatory 1 m telescope on 2007 May 4. This work was partly supported by Grant No. 2006234 from the United States-Israel Binational Science Foundation ( F), by the Kepler Mission under NASA Cooperative Agreement NCC 2-1390 with the Smithsonian Astrophysical Observatory, and by NASA Origins grant NNG06GH69G ( to M. J. H.). NR 49 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1559 EP 1565 DI 10.1088/0004-637X/694/2/1559 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900068 ER PT J AU Ho, PTP Altamirano, P Chang, CH Chang, SH Chang, SW Chen, CC Chen, KJ Chen, MT Han, CC Ho, WM Huang, YD Hwang, YJ Ibanez-Romano, F Jiang, HM Koch, PM Kubo, DY Li, CT Lim, J Lin, KY Liu, GC Lo, KY Ma, CJ Martin, RN Martin-Cocher, P Molnar, SM Ng, KW Nishioka, H O'Connell, KE Oshiro, P Patt, F Raffin, P Umetsu, K Wei, TS Wu, JHP Chiueh, TD Chiueh, T Chu, TH Huang, CWL Hwang, WYP Liao, YW Lien, CH Wang, FC Wang, HE Wei, RM Yang, CH Kesteven, M Kingsley, J Sinclair, MM Wilson, W Birkinshaw, M Liang, H Lancaster, K Park, CG Pen, UL Peterson, JB AF Ho, Paul T. P. Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Chung-Cheng Chen, Ke-Jung Chen, Ming-Tang Han, Chih-Chiang Ho, West M. Huang, Yau-De Hwang, Yuh-Jing Ibanez-Romano, Fabiola Jiang, Homin Koch, Patrick M. Kubo, Derek Y. Li, Chao-Te Lim, Jeremy Lin, Kai-Yang Liu, Guo-Chin Lo, Kwok-Yung Ma, Cheng-Jiun Martin, Robert N. Martin-Cocher, Pierre Molnar, Sandor M. Ng, Kin-Wang Nishioka, Hiroaki O'Connell, Kevin E. Oshiro, Peter Patt, Ferdinand Raffin, Philippe Umetsu, Keiichi Wei, Tashun Wu, Jiun-Huei Proty Chiueh, Tzi-Dar Chiueh, Tzihong Chu, Tah-Hsiung Huang, Chih-Wei Locutus Hwang, W. Y. Pauchy Liao, Yu-Wei Lien, Chun-Hsien Wang, Fu-Cheng Wang, Huei Wei, Ray-Ming Yang, Chia-Hsiang Kesteven, Michael Kingsley, Jeff Sinclair, Malcolm M. Wilson, Warwick Birkinshaw, Mark Liang, Haida Lancaster, Katy Park, Chan-Gyung Pen, Ue-Li Peterson, Jeffrey B. TI THE YUAN-TSEH LEE ARRAY FOR MICROWAVE BACKGROUND ANISOTROPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; instrumentation: interferometers; telescopes ID PROBE WMAP OBSERVATIONS; LENSING ANALYSIS; POWER SPECTRA; POLARIZATION; AMIBA; TEMPERATURE; IMAGER; CLUSTERS; MASS; COSMOLOGY AB The Yuan-Tseh Lee Array for microwave background anisotropy is the first interferometer dedicated to study the cosmic microwave background radiation at 3 mm wavelength. The choice of 3 mm is to minimize the contributions from foreground synchrotron radiation and Galactic dust emission. The initial configuration of seven 0.6 m telescopes mounted on a 6 m hexapod platform was dedicated in 2006 October on Mauna Loa, Hawaii. Scientific operations began with the detection of a number of clusters of galaxies via the thermal Sunyaev-Zel'dovich effect. We compare our data with Subaru weak-lensing data to study the structure of dark matter. We also compare our data with X-ray data to derive the Hubble constant. C1 [Ho, Paul T. P.; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Chung-Cheng; Chen, Ke-Jung; Chen, Ming-Tang; Han, Chih-Chiang; Ho, West M.; Huang, Yau-De; Hwang, Yuh-Jing; Ibanez-Romano, Fabiola; Jiang, Homin; Koch, Patrick M.; Kubo, Derek Y.; Li, Chao-Te; Lim, Jeremy; Lin, Kai-Yang; Liu, Guo-Chin; Lo, Kwok-Yung; Ma, Cheng-Jiun; Martin, Robert N.; Martin-Cocher, Pierre; Molnar, Sandor M.; Ng, Kin-Wang; Nishioka, Hiroaki; O'Connell, Kevin E.; Oshiro, Peter; Patt, Ferdinand; Raffin, Philippe; Umetsu, Keiichi; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Tamsui 251, Taipei County, Taiwan. [Lo, Kwok-Yung] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ma, Cheng-Jiun] Univ Hawaii Manoa, IfA, Honolulu, HI 96822 USA. [Martin, Robert N.; Wei, Ray-Ming] Composite Mirror Applicat, Tucson, AZ 85710 USA. [Umetsu, Keiichi; Wu, Jiun-Huei Proty; Chiueh, Tzihong; Huang, Chih-Wei Locutus; Hwang, W. Y. Pauchy; Liao, Yu-Wei; Wang, Fu-Cheng] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Kesteven, Michael; Sinclair, Malcolm M.; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Kingsley, Jeff] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Birkinshaw, Mark; Liang, Haida; Lancaster, Katy] Univ Bristol, Bristol BS8 1TL, Avon, England. [Liang, Haida] Nottingham Trent Univ, Nottingham NG11 8NS, England. [Park, Chan-Gyung] Sejong Univ, Seoul 143747, South Korea. [Pen, Ue-Li] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Peterson, Jeffrey B.] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP Ho, PTP (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM pho@asiaa.sinica.edu.tw; ho@cfa.harvard.edu RI Peterson, Jeffrey/O-4794-2014; Liang, Haida/C-7830-2016; OI Peterson, Jeffrey/0000-0003-1340-818X; Liang, Haida/0000-0001-9496-406X; HWANG, W-Y/0000-0003-1563-8683; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822; YANG, CHIA-HSIANG/0000-0003-1163-321X; CHIUEH, TZI-DAR/0000-0003-0851-6629 FU Ministry of Education, the National Science Council; Academia Sinica FX We thank the Ministry of Education, the National Science Council, and the Academia Sinica for their support to this project. We thank the Smithsonian Astrophysical Observatory for hosting the AMiBA project staff at the SMA Hilo Base Facility. We thank the NOAA for locating the AMiBA project on their site on Mauna Loa. We also thank the Hawaiian people for allowing astronomers to work on their mountains in order to study the universe. NR 56 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 APR 1 PY 2009 VL 694 IS 2 BP 1610 EP 1618 DI 10.1088/0004-637X/694/2/1610 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900073 ER PT J AU Wu, JHP Ho, PTP Huang, CWL Koch, PM Liao, YW Lin, KY Liu, GC Molnar, SM Nishioka, H Umetsu, K Wang, FC Altamirano, P Birkinshaw, M Chang, CH Chang, SH Chang, SW Chen, MT Chiueh, T Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, DY Lancaster, K Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wilson, W AF Wu, Jiun-Huei Proty Ho, Paul T. P. Huang, Chih-Wei Locutus Koch, Patrick M. Liao, Yu-Wei Lin, Kai-Yang Liu, Guo-Chin Molnar, Sandor M. Nishioka, Hiroaki Umetsu, Keiichi Wang, Fu-Cheng Altamirano, Pablo Birkinshaw, Mark Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Chiueh, Tzihong Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Y. Lancaster, Katy Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI ARRAY FOR MICROWAVE BACKGROUND ANISOTROPY: OBSERVATIONS, DATA ANALYSIS, AND RESULTS FOR SUNYAEV-ZEL'DOVICH EFFECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations; galaxies: clusters: general; methods: data analysis ID GALAXY CLUSTERS; X-RAY; SCALING RELATIONS; AMIBA; CONSTRAINTS; TELESCOPE; COSMOLOGY; PROJECT; IMAGER AB We present observations, analysis, and results for the first-year operation of Array for Microwave Background Anisotropy (AMiBA), an interferometric experiment designed to study cosmology via the measurement of cosmic microwave background (CMB). AMiBA is the first CMB interferometer operating at 3 mm to have reported successful results, currently with seven close-packed antennas of 60 cm diameter giving a synthesized resolution of around 6'. During 2007, AMiBA detected the Sunyaev-Zel'dovich effects (SZEs) of six galaxy clusters at redshift 0.091 <= z <= 0.322. An observing strategy with on-off-source switching is used to minimize the effects from electronic offset and ground pickup. Planets were used to test the observational capability of AMiBA and to calibrate the conversion from correlator time-lag data to visibilities. The detailed formalism for data analysis is given. We summarize our early tests including observations of planets and quasars, and present images, visibility profiles, the estimated central coordinates, sizes, and SZE amplitudes of the galaxy clusters. Scientific implications are summarized. We also discuss possible systematic effects in the results. C1 [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Umetsu, Keiichi; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan. [Ho, Paul T. P.; Koch, Patrick M.; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek Y.; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Birkinshaw, Mark; Lancaster, Katy] Univ Bristol, Bristol BS8 1TL, Avon, England. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Wu, JHP (reprint author), Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822 FU Ministry of Education, the National Science Council; Academia Sinica; National Taiwan University; National Center for Theoretical Science; Center for Theoretical Sciences, National Taiwan University; National Center for High-Performance Computing, Taiwan; STFC FX We thank the Ministry of Education, the National Science Council, the Academia Sinica, and National Taiwan University for their support of this project. We thank the Smithsonian Astrophysical Observatory for hosting the AMiBA project staff at the SMAHilo Base Facility. We thank the NOAA for locating the AMiBA project on their site on Mauna Loa. We thank the Hawaiian people for allowing astronomers to work on their mountains in order to study the universe. This work is also supported by National Center for Theoretical Science, and Center for Theoretical Sciences, National Taiwan University for J. H. P. W. We are grateful for computing support from the National Center for High-Performance Computing, Taiwan. Support from the STFC for M. B. and K. L. is also acknowledged. NR 38 TC 21 Z9 21 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1619 EP 1628 DI 10.1088/0004-637X/694/2/1619 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900074 ER PT J AU Lin, KY Li, CT Ho, PTP Huang, CWL Liao, YW Liu, GC Koch, PM Molnar, SM Nishioka, H Umetsu, K Wang, FC Wu, JHP Kestevan, M Birkinshaw, M Altamirano, P Chang, CH Chang, SH Chang, SW Chen, MT Martin-Cocher, P Han, CC Huang, YD Hwang, YJ Ibanez-Roman, F Jiang, HM Kubo, DY Oshiro, P Raffin, P Wei, TS Wilson, W Chen, KJ Chiueh, T AF Lin, Kai-Yang Li, Chao-Te Ho, Paul T. P. Huang, Chih-Wei Locutus Liao, Yu-Wei Liu, Guo-Chin Koch, Patrick M. Molnar, Sandor M. Nishioka, Hiroaki Umetsu, Keiichi Wang, Fu-Cheng Wu, Jiun-Huei Proty Kestevan, Michael Birkinshaw, Mark Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Martin-Cocher, Pierre Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Ibanez-Roman, Fabiola Jiang, Homin Kubo, Derek Y. Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick Chen, Ke-Jung Chiueh, Tzihong TI AMiBA: SYSTEM PERFORMANCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; galaxies: clusters: general; instrumentation: interferometers ID COSMIC BACKGROUND IMAGER; POWER SPECTRUM; ANISOTROPY; ACBAR AB The Y.T. Lee Array for Microwave Background Anisotropy started scientific operation in early 2007. This work describes the optimization of the system performance for the measurements of the Sunyaev-Zel'dovich effect for six massive galaxy clusters at redshifts 0.09-0.32. We achieved a point-source sensitivity of 63 +/- 7 mJy with the seven 0.6 m dishes in 1 hr of on-source integration in two-patch differencing observations. We measured and compensated for the delays between the antennas of our platform-mounted interferometer. Beam switching was used to cancel instrumental instabilities and ground pick up. Total power and phase stability were good on timescales of hours, and the system was shown to integrate down on equivalent timescales of 300 hr per baseline/correlation, or about 10 hr for the entire array. While the broadband correlator leads to good sensitivity, the small number of lags in the correlator resulted in poorly measured bandpass response. We corrected for this by using external calibrators (Jupiter and Saturn). Using Jupiter as the flux standard, we measured the disk brightness temperature of Saturn to be 149(-12)(+5) K. C1 [Lin, Kai-Yang; Li, Chao-Te; Ho, Paul T. P.; Liu, Guo-Chin; Koch, Patrick M.; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Martin-Cocher, Pierre; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Ibanez-Roman, Fabiola; Jiang, Homin; Kubo, Derek Y.; Oshiro, Peter; Raffin, Philippe; Wei, Tashun; Chen, Ke-Jung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Lin, Kai-Yang; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Chiueh, Tzihong] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huang, Chih-Wei Locutus; Liao, Yu-Wei; Umetsu, Keiichi; Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Chiueh, Tzihong] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 106, Taiwan. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Kestevan, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Birkinshaw, Mark] Univ Bristol, Bristol BS8 1TL, Avon, England. RP Lin, KY (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822 FU Academia Sinica Key Project; STFC FX Capital and operational funding for AMiBA came from the MoE and the NSC as part of the Cosmology and Particle Astrophysics (CosPA) initiative. Additional funding also came in the form of an Academia Sinica Key Project. Support from the STFC for M. B. is also acknowledged. NR 22 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1629 EP 1636 DI 10.1088/0004-637X/694/2/1629 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900075 ER PT J AU Nishioka, H Wang, FC Wu, JHP Ho, PTP Huang, CWL Koch, PM Liao, YW Lin, KY Liu, GC Molnar, SM Umetsu, K Birkinshaw, M Altamirano, P Chang, CH Chang, SH Chang, SW Chen, MT Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, DY Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wilson, W AF Nishioka, Hiroaki Wang, Fu-Cheng Wu, Jiun-Huei Proty Ho, Paul T. P. Huang, Chih-Wei Locutus Koch, Patrick M. Liao, Yu-Wei Lin, Kai-Yang Liu, Guo-Chin Molnar, Sandor M. Umetsu, Keiichi Birkinshaw, Mark Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Y. Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI TESTS OF AMiBA DATA INTEGRITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations; methods: data analysis ID BACKGROUND POWER SPECTRUM; SYSTEMATIC-ERROR LIMITS; SMALL ARRAY DATA; NON-GAUSSIANITY; MICROWAVE; MAPS AB We describe methods used to validate data from the Y.T. Lee Array for Microwave Background Anisotropy (AMiBA), an interferometric array designed to measure the Sunyaev-Zel'dovich effect and the anisotropy of the cosmic microwave background. We perform several statistical tests on data from pointed observations of galaxy clusters taken in 2007 and noise data from long-term blank-sky observations and measurements with the feeds covered by the absorbers. We apply power-spectrum analysis, cross-power-spectrum analysis among different outputs with different time lags in our analog correlator, and sample-variance law tests to noise data. We find that (1) there is no time variation of electronic offsets on the timescale of our two-patch observations (similar to 10 minutes); (2) noise is correlated by less than 10% between different lags; and (3) the variance of noise scales with the inverse of time. To test the Gaussianity of the data, we apply Kolmogorov-Smirnov tests to cluster data and find that a 5% significance level efficiently detects data sets with known hardware problems without rejecting an excess of acceptable data. We also calculate third- and fourth-order moments and cumulants for the noise residual visibilities and find that about 95% of our data are within the 99% confidence regions of Gaussianity. C1 [Nishioka, Hiroaki; Ho, Paul T. P.; Koch, Patrick M.; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Umetsu, Keiichi; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek Y.; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Umetsu, Keiichi] Natl Taiwan Univ, LeCosPA, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Taipei, Taiwan. [Birkinshaw, Mark] Univ Bristol, Bristol BS8 1TL, Avon, England. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Nishioka, H (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM nishioka@asiaa.sinica.edu.tw OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822 FU STFC FX We thank all the members of the AMiBA team for their hard work. We thank Katy Lancaster and Tzihong Chiueh for useful comments and discussions. We thank an anonymous referee for useful suggestions to improve the original manuscript. Support from the STFC for M. B. is also acknowledged. NR 21 TC 13 Z9 13 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1637 EP 1642 DI 10.1088/0004-637X/694/2/1637 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900076 ER PT J AU Umetsu, K Birkinshaw, M Liu, GC Wu, JHP Medezinski, E Broadhurst, T Lemze, D Zitrin, A Ho, PTP Huang, CWL Koch, PM Liao, YW Lin, KY Molnar, SM Nishioka, H Wang, FC Altamirano, P Chang, CH Chang, SH Chang, SW Chen, MT Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, DY Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wilson, W AF Umetsu, Keiichi Birkinshaw, Mark Liu, Guo-Chin Wu, Jiun-Huei Proty Medezinski, Elinor Broadhurst, Tom Lemze, Doron Zitrin, Adi Ho, Paul T. P. Huang, Chih-Wei Locutus Koch, Patrick M. Liao, Yu-Wei Lin, Kai-Yang Molnar, Sandor M. Nishioka, Hiroaki Wang, Fu-Cheng Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Y. Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI MASS AND HOT BARYONS IN MASSIVE GALAXY CLUSTERS FROM SUBARU WEAK-LENSING AND AMiBA SUNYAEV-ZEL'DOVICH EFFECT OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Review DE cosmic microwave background; cosmology: observations; galaxies: clusters: individual (A1689, A2142, A2261, A2390); gravitational lensing ID COSMIC BACKGROUND IMAGER; HUBBLE-SPACE-TELESCOPE; N-BODY SIMULATIONS; DARK-MATTER; X-RAY; NEARBY CLUSTERS; RELATIVISTIC CORRECTIONS; COSMOLOGICAL PARAMETERS; ANISOTROPY OBSERVATIONS; INTRACLUSTER MEDIUM AB We present a multiwavelength analysis of a sample of four hot (T-X > 8 keV) X-ray galaxy clusters (A1689, A2261, A2142, and A2390) using joint AMiBA Sunyaev-Zel'dovich effect (SZE) and Subaru weak-lensing observations, combined with published X-ray temperatures, to examine the distribution of mass and the intracluster medium (ICM) in massive cluster environments. Our observations show that A2261 is very similar to A1689 in terms of lensing properties. Many tangential arcs are visible around A2261, with an effective Einstein radius similar to 40" (at z similar to 1.5), which when combined with our weak-lensing measurements implies a mass profile well fitted by a Navarro- Frenk-White model with a high concentration c(vir) similar to 10, similar to A1689 and to other massive clusters. The cluster A2142 shows complex mass substructure, and displays a shallower profile (c(vir) similar to 5), consistent with detailed X-ray observations which imply recent interaction. The AMiBA map of A2142 exhibits an SZE feature associated with mass substructure lying ahead of the sharp northwest edge of the X-ray core suggesting a pressure increase in the ICM. For A2390 we obtain highly elliptical mass and ICM distributions at all radii, consistent with other X-ray and strong-lensing work. Our cluster gas fraction measurements, free from the hydrostatic equilibrium assumption, are overall in good agreement with published X-ray and SZE observations, with the sample-averaged gas fraction of (f(gas)(< r(200))> = 0.133 +/- 0.027, for our sample with < M-vir > = ( 1.2 +/- 0.1) x 10(15) M circle dot h(-1). When compared to the cosmic baryon fraction f(b) = ohm(b)/ohm(m) constrained by the WMAP five-year data, this indicates < f(gas),200 >/f(b) = 0.78 +/- 0.16, i. e., (22 +/- 16)% of the baryons are missing from the hot phase of clusters. C1 [Umetsu, Keiichi; Liu, Guo-Chin; Ho, Paul T. P.; Koch, Patrick M.; Lin, Kai-Yang; Molnar, Sandor M.; Nishioka, Hiroaki; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek Y.; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Umetsu, Keiichi; Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Wang, Fu-Cheng] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Birkinshaw, Mark] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Taipei, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng] Natl Taiwan Univ, Dept Phys, Taipei 10617, Taiwan. [Medezinski, Elinor; Broadhurst, Tom; Lemze, Doron; Zitrin, Adi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Umetsu, K (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822 NR 117 TC 79 Z9 79 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 APR 1 PY 2009 VL 694 IS 2 BP 1643 EP 1663 DI 10.1088/0004-637X/694/2/1643 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900077 ER PT J AU Chen, MT Li, CT Hwang, YJ Jiang, HM Altamirano, P Chang, CH Chang, SH Chang, SW Chiueh, TD Chu, TH Han, CC Huang, YD Kesteven, M Kubo, D Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wang, H Wilson, W Ho, PTP Huang, CW Koch, P Liao, YW Lin, KY Liu, GC Molnar, SM Nishioka, H Umetsu, K Wang, FC Wu, JHP AF Chen, Ming-Tang Li, Chao-Te Hwang, Yuh-Jing Jiang, Homin Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chiueh, Tzi-Dar Chu, Tah-Hsiung Han, Chih-Chiang Huang, Yau-De Kesteven, Michael Kubo, Derek Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wang, Huei Wilson, Warwick Ho, Paul T. P. Huang, Chih-Wei Koch, Patrick Liao, Yu-Wei Lin, Kai-Yang Liu, Guo-Chin Molnar, Sandor M. Nishioka, Hiroaki Umetsu, Keiichi Wang, Fu-Cheng Wu, Jiun-Huei Proty TI AMiBA: BROADBAND HETERODYNE COSMIC MICROWAVE BACKGROUND INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology: observations; instrumentation: interferometers ID ARRAY; CORRELATOR; ANISOTROPY; DESIGN AB The Y. T. Lee Array for Microwave Background (AMiBA) has reported the first results on the detection of galaxy clusters via the Sunyaev-Zel'dovich effect. The objectives required small reflectors in order to sample large-scale structures (20'), while interferometry provided modest resolutions (2'). With these constraints, we designed for the best sensitivity by utilizing the maximum possible continuum bandwidth matched to the atmospheric window at 86-102 GHz, with dual polarizations. A novel wide-band analog correlator was designed that is easily expandable for more interferometer elements. Monolithic millimeter-wave integrated circuit technology was used throughout as much as possible in order to miniaturize the components and to enhance mass production. These designs will find application in other upcoming astronomy projects. AMiBA is now in operation since 2006, and we are in the process to expand the array from seven to 13 elements. C1 [Chen, Ming-Tang; Li, Chao-Te; Hwang, Yuh-Jing; Jiang, Homin; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Han, Chih-Chiang; Huang, Yau-De; Kubo, Derek; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun; Ho, Paul T. P.; Koch, Patrick; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Chiueh, Tzi-Dar; Chu, Tah-Hsiung; Wang, Huei; Huang, Chih-Wei; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng; Wu, Jiun-Huei Proty] Natl Taiwan Univ, Taipei 106, Taiwan. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, MT (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM mchen@asiaa.sinica.edu.tw OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822; CHIUEH, TZI-DAR/0000-0003-0851-6629 FU Ministry of Education, the National Science Council FX We thank the Ministry of Education, the National Science Council, and the Academia Sinica for their support of this project. We thank the Smithsonian Astrophysical Observatory for hosting the AMiBA project staff at the SMA Hilo Base Facility. We thank the NOAA for locating the AMiBA project at their site on Mauna Loa. We thank the Hawaiian people for allowing astronomers to work on their mountains in order to study the universe. NR 33 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1664 EP 1669 DI 10.1088/0004-637X/694/2/1664 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900078 ER PT J AU Koch, PM Kesteven, M Nishioka, H Jiang, HM Lin, KY Umetsu, K Huang, YD Raffin, P Chen, KJ Ibanez-Romano, F Chereau, G Huang, CWL Chen, MT Ho, PTP Pausch, K Willmeroth, K Altamirano, P Chang, CH Chang, SH Chang, SW Han, CC Kubo, D Li, CT Liao, YW Liu, GC Martin-Cocher, P Oshiro, P Wang, FC Wei, TS Wu, JHP Birkinshaw, M Chiueh, T Lancaster, K Lo, KY Martin, RN Molnar, SM Patt, F Romeo, B AF Koch, Patrick M. Kesteven, Michael Nishioka, Hiroaki Jiang, Homin Lin, Kai-Yang Umetsu, Keiichi Huang, Yau-De Raffin, Philippe Chen, Ke-Jung Ibanez-Romano, Fabiola Chereau, Guillaume Huang, Chih-Wei Locutus Chen, Ming-Tang Ho, Paul T. P. Pausch, Konrad Willmeroth, Klaus Altamirano, Pablo Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Han, Chih-Chiang Kubo, Derek Li, Chao-Te Liao, Yu-Wei Liu, Guo-Chin Martin-Cocher, Pierre Oshiro, Peter Wang, Fu-Cheng Wei, Ta-Shun Wu, Jiun-Huei Proty Birkinshaw, Mark Chiueh, Tzihong Lancaster, Katy Lo, Kwok Yung Martin, Robert N. Molnar, Sandor M. Patt, Ferdinand Romeo, Bob TI THE AMiBA HEXAPOD TELESCOPE MOUNT SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: interferometers AB The Array for Microwave Background Anisotropy (AMiBA) is the largest hexapod astronomical telescope in current operation. We present a description of this novel hexapod mount with its main mechanical components-the support cone, universal joints, jack screws, and platform-and outline the control system with the pointing model and the operating modes that are supported. The AMiBA hexapod mount performance is verified based on optical pointing tests and platform photogrammetry measurements. The photogrammetry results show that the deformations in the inner part of the platform are less than 120 mu m rms. This is negligible for optical pointing corrections, radio alignment, and radio phase errors for the currently operational seven-element compact configuration. The optical pointing error in azimuth and elevation is successively reduced by a series of corrections to about 0.'4 rms which meets our goal for the seven-element target specifications. C1 [Koch, Patrick M.; Nishioka, Hiroaki; Jiang, Homin; Lin, Kai-Yang; Umetsu, Keiichi; Huang, Yau-De; Raffin, Philippe; Chen, Ke-Jung; Ibanez-Romano, Fabiola; Chereau, Guillaume; Chen, Ming-Tang; Ho, Paul T. P.; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Han, Chih-Chiang; Kubo, Derek; Li, Chao-Te; Liu, Guo-Chin; Martin-Cocher, Pierre; Oshiro, Peter; Wei, Ta-Shun; Molnar, Sandor M.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kesteven, Michael] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Lin, Kai-Yang; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Chiueh, Tzihong] Natl Taiwan Univ, Inst Astrophys, Dept Phys, Taipei 10617, Taiwan. [Lin, Kai-Yang; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty; Chiueh, Tzihong] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Umetsu, Keiichi; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Wang, Fu-Cheng; Wu, Jiun-Huei Proty] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pausch, Konrad; Willmeroth, Klaus] Vertex Antennentech GmbH, Duisburg, Germany. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Taipei, Taiwan. [Birkinshaw, Mark; Lancaster, Katy] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Lo, Kwok Yung] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Martin, Robert N.; Romeo, Bob] Composite Mirror Applicat Inc, Tucson, AZ 85710 USA. [Patt, Ferdinand] ESO Headquarters, Garching, Germany. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI WU, JIUN-HUEI/0000-0001-9608-7662; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822 NR 22 TC 23 Z9 23 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2009 VL 694 IS 2 BP 1670 EP 1684 DI 10.1088/0004-637X/694/2/1670 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 424AW UT WOS:000264538900079 ER PT J AU Currie, T AF Currie, Thayne TI ON THE SEMIMAJOR AXIS DISTRIBUTION OF EXTRASOLAR GAS GIANT PLANETS: WHY HOT JUPITERS ARE RARE AROUND HIGH-MASS STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems: formation ID CHI-PERSEI; ACCRETION; COMPANIONS; EVOLUTION; EXOPLANETS; MIGRATION; DISKS AB Based on a suite of Monte Carlo simulations, I show that a stellar-mass-dependent lifetime of the gas disks from which planets form can explain the lack of hot Jupiters/close-in giant planets around high-mass stars and other key features of the observed semimajor axis distribution of radial velocity-detected giant planets. Using reasonable parameters for the Type II migration rate, regions of planet formation, and timescales for gas giant core formation, I construct synthetic distributions of Jovian planets. A planet formation/migration model assuming a stellar-mass-dependent gas disk lifetime reproduces key features in the observed distribution by preferentially stranding planets around high-mass stars at large semimajor axes. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02140 USA. RP Currie, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. EM tcurrie@cfa.harvard.edu FU NASA Astrophysics Theory [NAG5-13278]; NASA [NNG06GH25G] FX I thank John A. Johnson and Jason Wright for discussions on exoplanet data and for encouraging the writing of this paper; Geoff Marcy, Scott Kenyon, Dan Fabrycky, Ruth Murray- Clay, Brad Hansen, and Jonathan Irwin for valuable comments, and the referee for a rapid and insightful report. This work is supported by NASA Astrophysics Theory Grant NAG5-13278 and NASA Grant NNG06GH25G. NR 24 TC 42 Z9 42 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 1 PY 2009 VL 694 IS 2 BP L171 EP L176 DI 10.1088/0004-637X/694/2/L171 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 419CL UT WOS:000264196600019 ER PT J AU Evans, NJ Dunham, MM Jorgensen, JK Enoch, ML Merin, B van Dishoeck, EF Alcala, JM Myers, PC Stapelfeldt, KR Huard, TL Allen, LE Harvey, PM van Kempen, T Blake, GA Koerner, DW Mundy, LG Padgett, DL Sargent, AI AF Evans, Neal J., II Dunham, Michael M. Jorgensen, Jes K. Enoch, Melissa L. Merin, Bruno van Dishoeck, Ewine F. Alcala, Juan M. Myers, Philip C. Stapelfeldt, Karl R. Huard, Tracy L. Allen, Lori E. Harvey, Paul M. van Kempen, Tim Blake, Geoffrey A. Koerner, David W. Mundy, Lee G. Padgett, Deborah L. Sargent, Anneila I. TI THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE dust, extinction; infrared: stars; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; AURIGA MOLECULAR CLOUD; II DARK CLOUD; T-TAURI STARS; SPACE-TELESCOPE OBSERVATIONS; DUST CONTINUUM EMISSION; RHO-OPHIUCHI CLOUD AB The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. Three of the clouds were also mapped in dust continuum emission at 1.1 mm, and optical spectroscopy has been obtained for some clouds. This paper combines information drawn from studies of individual clouds into a combined and updated statistical analysis of star-formation rates and efficiencies, numbers and lifetimes for spectral energy distribution (SED) classes, and clustering properties. Current star-formation efficiencies range from 3% to 6%; if star formation continues at current rates for 10 Myr, efficiencies could reach 15-30%. Star-formation rates and rates per unit area vary from cloud to cloud; taken together, the five clouds are producing about 260 M(circle dot) of stars per Myr. The star-formation surface density is more than an order of magnitude larger than would be predicted from the Kennicutt relation used in extragalactic studies, reflecting the fact that those relations apply to larger scales, where more diffuse matter is included in the gas surface density. Measured against the dense gas probed by the maps of dust continuum emission, the efficiencies are much higher, with stellar masses similar to masses of dense gas, and the current stock of dense cores would be exhausted in 1.8 Myr on average. Nonetheless, star formation is still slow compared to that expected in a free-fall time, even in the dense cores. The derived lifetime for the Class I phase is 0.54 Myr, considerably longer than some estimates. Similarly, the lifetime for the Class 0 SED class, 0.16 Myr, with the notable exception of the Ophiuchus cloud, is longer than early estimates. If photometry is corrected for estimated extinction before calculating class indicators, the lifetimes drop to 0.44 Myr for Class I and to 0.10 for Class 0. These lifetimes assume a continuous flow through the Class II phase and should be considered median lifetimes or half-lives. Star formation is highly concentrated to regions of high extinction, and the youngest objects are very strongly associated with dense cores. The great majority (90%) of young stars lie within loose clusters with at least 35 members and a stellar density of 1 M(circle dot) pc(-3). Accretion at the sound speed from an isothermal sphere over the lifetime derived for the Class I phase could build a star of about 0.25 M(circle dot), given an efficiency of 0.3. Building larger mass stars by using higher mass accretion rates could be problematic, as our data confirm and aggravate the "luminosity problem" for protostars. At a given T(bol), the values for L(bol) are mostly less than predicted by standard infall models and scatter over several orders of magnitude. These results strongly suggest that accretion is time variable, with prolonged periods of very low accretion. Based on a very simple model and this sample of sources, half the mass of a star would be accreted during only 7% of the Class I lifetime, as represented by the eight most luminous objects. C1 [Evans, Neal J., II; Dunham, Michael M.; Harvey, Paul M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Jorgensen, Jes K.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Enoch, Melissa L.; Sargent, Anneila I.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Enoch, Melissa L.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Merin, Bruno; van Dishoeck, Ewine F.; van Kempen, Tim] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Merin, Bruno] European Space Technol Ctr, European Space Agcy, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Alcala, Juan M.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Myers, Philip C.; Huard, Tracy L.; Allen, Lori E.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stapelfeldt, Karl R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Huard, Tracy L.; Mundy, Lee G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Koerner, David W.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Padgett, Deborah L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Evans, NJ (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM nje@astro.as.utexas.edu; mdunham@astro.as.utexas.edu; jes@astro.uni-bonn.de; bmerin@rssd.esa.int; ewine@strw.LeidenUniv.nl; alcala@oacn.inaf.it; pmyers@cfa.harvard.edu; krs@exoplanet.jpl.nasa.gov; thuard@astro.umd.edu; leallen@cfa.harvard.edu; pmh@astro.as.utexas.edu; gab@gps.caltech.edu; david.koerner@nau.edu; lgm@astro.umd.edu; dlp@ipac.caltech.edu; afs@astro.caltech.edu RI Stapelfeldt, Karl/D-2721-2012; OI Alcala, Juan Manuel/0000-0001-8657-095X; Merin, Bruno/0000-0002-8555-3012 FU NASA [1224608, 1230779, 1288658, 1288664, 1230782, 1407, NNG04GG24G, NNX07AJ72G]; NSF [NSF PHY05-51164]; NWO Spinoza; NOVA FX We thank the referee, Charles Lada, for a very thought-provoking report, which helped us to improve the clarity of the paper. We thank the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. Part of the work was done while in residence at the Kavli Institute for Theoretical Physics in Santa Barbara, California. We thank M. Krumholz for enlightening discussions and derivations of the speed of star formation in dense gas and F. Comeron for drawing our attention to biases caused by low-mass objects dropping out of the sample as they age. We are also grateful to D. Ward-Thompson for helpful suggestions. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230779, 1288658, 1288664, and 1230782 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. Additional support came from NASA Origins grants NNG04GG24G and NNX07AJ72G to N.J.E. While several coauthors were at the Kavli Institute, the research was supported in part by the NSF under Grant No. NSF PHY05-51164. M. L. E. acknowledges support of an NSF Graduate Research Fellowship and a Spitzer Space Telescope Postdoctoral Fellowship. Astrochemistry in Leiden is supported by a NWO Spinoza grant and a NOVA grant. NR 179 TC 649 Z9 651 U1 3 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 321 EP 350 DI 10.1088/0067-0049/181/2/321 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700001 ER PT J AU Chambers, ET Jackson, JM Rathborne, JM Simon, R AF Chambers, E. T. Jackson, J. M. Rathborne, J. M. Simon, R. TI STAR FORMATION ACTIVITY OF CORES WITHIN INFRARED DARK CLOUDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE dust, extinction; ISM: clouds; masers; stars: formation ID SUBMILLIMETER CONTINUUM SURVEY; MOLECULAR CLOUDS; MASSIVE STARS; INTERSTELLAR EXTINCTION; METHANOL MASERS; GALACTIC PLANE; DENSE CORES; SPITZER; PROTOSTARS; CLUSTERS AB Infrared Dark Clouds (IRDCs) contain compact cores which probably host the early stages of high-mass star formation. Many of these cores contain regions of extended, enhanced 4.5 mu m emission, the so-called "green fuzzies," which indicate shocked gas. Many cores also contain 24 mu m emission, presumably from heated dust which indicates embedded protostars. Because "green fuzzies" and 24 mu m point sources both indicate star formation, we have developed an algorithm to identify star-forming cores within IRDCs by searching for the simultaneous presence of these two distinct indicators. We employ this algorithm on a sample of 190 cores found toward IRDCs, and classify the cores as "active" if they contain a green fuzzy coincident with an embedded 24 mu m source, and as "quiescent" if they contain neither IR signature. We hypothesize that the "quiescent" cores represent the earliest "preprotostellar" ( starless) core phase, before the development of a warm protostar, and that the "active" cores represent a later phase, after the development of a protostar. We test this idea by comparing the sizes, densities, and maser activity of the "active" and "quiescent" cores. We find that, on average, "active" cores have smaller sizes, higher densities, and more pronounced water and methanol maser activity than the "quiescent" cores. This is expected if the "quiescent" cores are in an earlier evolutionary state than the "active" cores. The masses of "active" cores suggest that they may be forming high-mass stars. The highest mass "quiescent" cores are excellent candidates for the elusive high-mass starless cores. C1 [Chambers, E. T.; Jackson, J. M.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Rathborne, J. M.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Simon, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Chambers, ET (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. EM etc1@bu.edu; jackson@bu.edu; jrathborne@cfa.harvard.edu; simonr@ph1.uni-koeln.de FU NSF [AST-0098562]; NASA [1407, 1264028, 1289760]; NRAO [GSSP06-0007] FX The authors gratefully acknowledge funding support through NSF grant AST-0098562. 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 NASA contract 1407. Support for this work was provided by NASA through contracts 1264028 and 1289760 issued by JPL/Caltech, as well as through GSSP06-0007 from the NRAO. The GBT is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities Inc. This works makes use of data from the GLIMPSE and MIPSGAL surveys. We thank the GLIMSPE and MIPSGAL teams for their help and support. The authors also thank the anonymous referee, whose comments and suggestions resulted in a much improved paper. NR 45 TC 124 Z9 124 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 360 EP 390 DI 10.1088/0067-0049/181/2/360 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700003 ER PT J AU Agueros, MA Anderson, SF Covey, KR Hawley, SL Margon, B Newsom, ER Posselt, B Silvestri, NM Szkody, P Voges, W AF Agueros, Marcel A. Anderson, Scott F. Covey, Kevin R. Hawley, Suzanne L. Margon, Bruce Newsom, Emily R. Posselt, Bettina Silvestri, Nicole M. Szkody, Paula Voges, Wolfgang TI X-RAY-EMITTING STARS IDENTIFIED FROM THE ROSAT ALL-SKY SURVEY AND THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE surveys; X-rays: stars ID MEDIUM-SENSITIVITY SURVEY; RS CANUM-VENATICORUM; BRIGHT SOURCE CATALOG; 1ST DATA RELEASE; A-TYPE STARS; CATACLYSMIC VARIABLES; OPTICAL IDENTIFICATIONS; WHITE-DWARFS; COMPLETE SAMPLE; BINARY-SYSTEMS AB The ROSAT All-Sky Survey (RASS) was the first imaging X-ray survey of the entire sky. Combining the RASS Bright and Faint Source Catalogs yields an average of about three X-ray sources per square degree. However, while X-ray source counterparts are known to range from distant quasars to nearby M dwarfs, the RASS data alone are often insufficient to determine the nature of an X-ray source. As a result, large-scale follow-up programs are required to construct samples of known X-ray emitters. We use optical data produced by the Sloan Digital Sky Survey (SDSS) to identify 709 stellar X-ray emitters cataloged in the RASS and falling within the SDSS Data Release 1 footprint. Most of these are bright stars with coronal X-ray emission unsuitable for SDSS spectroscopy, which is designed for fainter objects (g > 15 [mag]). Instead, we use SDSS photometry, correlations with the Two Micron All Sky Survey and other catalogs, and spectroscopy from the Apache Point Observatory 3.5 m telescope to identify these stellar Xray counterparts. Our sample of 707 X-ray-emitting F, G, K, and M stars is one of the largest X-ray-selected samples of such stars. We derive distances to these stars using photometric parallax relations appropriate for dwarfs on the main sequence, and use these distances to calculate L-X. We also identify a previously unknown cataclysmic variable (CV) as a RASS counterpart. Separately, we use correlations of the RASS and the SDSS spectroscopic catalogs of CVs and white dwarfs (WDs) to study the properties of these rarer X-ray-emitting stars. We examine the relationship between (f(X)/f(g)) and the equivalent width of the H beta emission line for 46 X-ray-emitting CVs and discuss tentative classifications for a subset based on these quantities. We identify 17 new X-ray-emitting DA (hydrogen) WDs, of which three are newly identified WDs. We report on follow-up observations of three candidate cool X-ray-emitting WDs (one DA and two DB (helium) WDs); we have not confirmed X-ray emission from these WDs. C1 [Agueros, Marcel A.; Newsom, Emily R.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Anderson, Scott F.; Hawley, Suzanne L.; Silvestri, Nicole M.; Szkody, Paula] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Covey, Kevin R.; Posselt, Bettina] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Margon, Bruce] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Voges, Wolfgang] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Agueros, MA (reprint author), Columbia Univ, Columbia Astrophys Lab, 550 W 120th St, New York, NY 10027 USA. EM marcel@astro.columbia.edu RI Margon, Bruce/B-5913-2012; Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Posselt, Bettina/0000-0003-2317-9747; Covey, Kevin/0000-0001-6914-7797 FU NSF [AST-0602099]; NASA; ESA Member States; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; [GO6-7058X]; [GO8-9012X] FX We thank the referee for comments that improved the paper. We are grateful to the APO time allocation committee at the University of Washington for providing us with the nights needed to complete our spectroscopic program. We thank the telescope operators at the observatory for their assistance with our observations. We also thank Michelle Cash, Nick Cowan, Lee Mannikko, Anil Seth, and Kristine Washburn for using some of their APO observing time to obtain data for this program. Finally, we thank Beth Willman for sharing her matching code. M. Agueros is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602099; much of the work described here was made possible by a NASA Harriett G. Jenkins Predoctoral Fellowship. Further NASA support was provided to K. Covey through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We gratefully acknowledge Chandra grants GO6-7058X and GO8-9012X for support of portions of our program.; This research has made use of data obtained from the Chandra Archive and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. Some of 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.; 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.; 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 123 TC 24 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 444 EP 465 DI 10.1088/0067-0049/181/2/444 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700010 ER PT J AU Hopkins, PF Lauer, TR Cox, TJ Hernquist, L Kormendy, J AF Hopkins, Philip F. Lauer, Tod R. Cox, Thomas J. Hernquist, Lars Kormendy, John TI DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. III. "CORE" ELLIPTICALS AND "MISSING" LIGHT SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE cosmology: theory; galaxies: active; galaxies: evolution; quasars: general ID EARLY-TYPE GALAXIES; SUPERMASSIVE BLACK-HOLES; HUBBLE-SPACE-TELESCOPE; CCD SURFACE PHOTOMETRY; DIGITAL SKY SURVEY; PARTICLE HYDRODYNAMICS SIMULATIONS; SPATIALLY-RESOLVED SPECTROSCOPY; PLANETARY CAMERA OBSERVATIONS; BRIGHTEST CLUSTER GALAXIES; QUASAR LUMINOSITY FUNCTION AB We investigate how "extra" or "excess" central light in the surface brightness profiles of cusp or power-law elliptical galaxies relates to the profiles of ellipticals with cores. The envelopes of cusp ellipticals are established by violent relaxation in mergers acting on stars present in gas-rich progenitor disks, while their centers are structured by the relics of dissipational, compact starbursts. Ellipticals with cores are formed by the subsequent merging of the now gas-poor cusp ellipticals, with the fossil starburst components combining to preserve a dense, compact component in these galaxies as well ( although mixing of stars smooths the transition from the outer to inner components in the profiles). By comparing extensive hydrodynamical simulations to observed profiles spanning a broad mass range, we show how to observationally isolate and characterize the relic starburst component in core ellipticals. Our method recovers the younger starburst population, demonstrating that these dense concentrations survive spheroid-spheroid mergers and reflect the degree of dissipation in the initial mergers that formed the penultimate galaxy progenitors. The degree of dissipation in the mergers that produced the cusp ellipticals is a strong function of stellar mass, roughly tracing the observed gas fractions of disks of the same mass over redshifts z similar to 0-2. The strength of this component strongly correlates with effective radius at fixed mass: systems with more dissipation are more compact, sufficient to explain the discrepancy in the maximum phase-space densities of ellipticals and their progenitor spirals. The survival of this component together with scattering of stars into the envelope in re-mergers naturally explain the high-Sersic index profile shapes characteristic of very massive core ellipticals. This is also closely related to the kinematics and isophotal shapes: only systems with matched starburst components from their profile fits also reproduce the observed kinematics of boxy/core ellipticals. The final "core-scouring" phase of core formation occurs when a black hole binary formed in the merger scatters stars out of the innermost regions of the extra-light component. It is therefore critical to adopt a physically motivated profile decomposition that accounts for the fossil starburst component when attempting to quantify scouring. We show that estimates of the scoured mass that employ single-component forms fitted to the entire galaxy profile can be strongly biased. C1 [Hopkins, Philip F.; Cox, Thomas J.; Hernquist, Lars] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lauer, Tod R.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Kormendy, John] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Hopkins, PF (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [ACI 96-19019, AST 00-71019, AST 02-06299, AST 03-07690, AST 06-07490]; NASA [NAG5-12140, NAG5-13292, NAG5-13381]; W.M. Keck Foundation FX We thank Marijn Franx, Josh Younger, and Barry Rothberg for helpful discussions and contributed data sets used in this paper. We also thank the anonymous referee for helpful advice on the content herein. This work was supported in part by NSF grants ACI 96-19019, AST 00-71019, AST 02-06299, and AST 03-07690, and NASA ATP grants NAG5-12140, NAG5-13292, and NAG5-13381. Support for T.J.C. was provided by the W.M. Keck Foundation. J.K.'s work was supported in part by NSF grant AST 06-07490. NR 195 TC 98 Z9 99 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 486 EP 532 DI 10.1088/0067-0049/181/2/486 PG 47 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700013 ER PT J AU Cheung, CC Healey, SE Landt, H Kleijn, GV Jordan, A AF Cheung, C. C. Healey, Stephen E. Landt, Hermine Kleijn, Gijs Verdoes Jordan, Andres TI FIRST "WINGED" AND X-SHAPED RADIO SOURCE CANDIDATES. II. NEW REDSHIFTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; galaxies: distances and redshifts; quasars: general ID BL LACERTAE OBJECTS; REVISED 3C CATALOG; ABELL CLUSTERS; BLACK-HOLE; OPTICAL SPECTROSCOPY; SURFACE PHOTOMETRY; GALAXY NGC-326; SKY SURVEY; VLA SURVEY; EMISSION AB We report optical spectroscopic observations of X-shaped radio sources with the Hobby-Eberly Telescope and Multiple-Mirror Telescope, focused on the sample of candidates from the FIRST survey presented in a previous paper. A total of 27 redshifts were successfully obtained, 21 of which are new, including a newly identified candidate source of this type which is presented here. With these observations, the sample of candidates from the previous paper is over 50% spectroscopically identified. Two new broad emission-lined X-shaped radio sources are revealed, while no emission lines were detected in about one-third of the observed sources; a detailed study of the line properties is deferred to a future paper. Finally, to explore their relation to the Fanaroff Riley division, the radio luminosities and host galaxy absolute magnitudes of a spectroscopically identified sample of 50 X-shaped radio galaxies are calculated to determine their placement in the Owen-Ledlow plane. C1 [Cheung, C. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cheung, C. C.; Healey, Stephen E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Healey, Stephen E.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Landt, Hermine; Jordan, Andres] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kleijn, Gijs Verdoes] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Jordan, Andres] European So Observ, D-85748 Garching, Germany. RP Cheung, CC (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM Teddy.Cheung@nasa.gov OI Jordan, Andres/0000-0002-5389-3944 FU National Science Foundation; NASA; DOE DE-AC03-76SF00515; University of Texas at Austin; Pennsylvania State University; Stanford University; Ludwig-Maximillians-Universitat Munchen; Georg-August-Universitat Gottingen; HET; Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico FX C. C. C. was supported by the National Radio Astronomy Observatory (2004-2007), which is operated by Associated Universities, Inc. under a cooperative agreement with the National Science Foundation, and currently by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. S. E. H. is supported by the Stanford Linear Accelerator Center under DOE contract DE-AC03-76SF00515. C. C. C. is grateful to the MMT staff, particularly Mike Alegria and Grant Williams for their assistance during the observing run, and Alessondra Springmann for her assistance during a clouded out MMT run in July 2006. The MMT is a facility operated jointly by the University of Arizona and the Smithsonian Institution.; The Hobby-Eberly Telescope is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximillians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario Low-Resolution Spectrograph is named for Mike Marcario of High Lonesome Optics, who fabricated several optics for the instrument but died before its completion; it is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. This paper includes data taken with the Harlan J. Smith Telescope at the McDonald Observatory of the University of Texas at Austin.; This research has made use of NASA's Astrophysics Data System Abstract Service 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 48 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 548 EP 556 DI 10.1088/0067-0049/181/2/548 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700016 ER PT J AU Brassington, NJ Fabbiano, G Kim, DW Zezas, A Zepf, S Kundu, A Angelini, L Davies, RL Gallagher, J Kalogera, V Fragos, T King, AR Pellegrini, S Trinchieri, G AF Brassington, N. J. Fabbiano, G. Kim, D. -W. Zezas, A. Zepf, S. Kundu, A. Angelini, L. Davies, R. L. Gallagher, J. Kalogera, V. Fragos, T. King, A. R. Pellegrini, S. Trinchieri, G. TI DEEP CHANDRA MONITORING OBSERVATIONS OF NGC 4278: CATALOG OF SOURCE PROPERTIES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: individual (NGC 4278); X-rays: binaries; X-rays: galaxies ID X-RAY BINARIES; GLOBULAR-CLUSTER SYSTEMS; MULTIWAVELENGTH PROJECT; ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; SOURCE POPULATION; NEARBY GALAXIES; POINT SOURCES; CENTAURUS-A; DISTANCES AB We present the properties of the discrete X-ray sources detected in our monitoring program of the globular cluster ( GC) rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D(25) ellipse of the galaxy. These 236 sources range in L(X) from 3.5 x 10(36) erg s(-1) ( with 3 sigma upper limit <= 1 x 10(37) erg s(-1)) to similar to 2 x 10(40) erg s(-1), including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L(X) > 1 x 10(38) erg s(-1). From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of these sources expected to be background objects from the log N - log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. C1 [Brassington, N. J.; Fabbiano, G.; Kim, D. -W.; Zezas, A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zepf, S.; Kundu, A.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Angelini, L.] NASA, Goddard Space Flight Ctr, Lab Xray Astrophys, Greenbelt, MD 20771 USA. [Davies, R. L.] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Gallagher, J.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Kalogera, V.; Fragos, T.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] Osserv Astron Brera, INAF, I-20121 Milan, Italy. RP Brassington, NJ (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nbrassington@head.cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523 FU Chandra G0 [G06-7079A, G06-7079B]; NASA [NAS8-3907, NAG5-13056]; Italian Space Agency ASI (Agenzia Spaziale Italiana) [ASI-INAF I/023/05/0] FX We thank the CXC DS and SDS teams for their efforts in reducing the data and developing the software used for the reduction (SDP) and analysis (CIAO). We also thank the referee, Jimmy Irwin, for his helpful comments which have improved this paper. This work was supported by Chandra G0 grant G06-7079A (PI: Fabbiano) and subcontract G06-7079B (PI: Kalogera). We acknowledge partial support from NASA contract NAS8-39073 (CXC). A. Zezas acknowledges support from NASA LTSA grant NAG5-13056. S. Pellegrini acknowledges partial financial support from the Italian Space Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAF I/023/05/0. NR 40 TC 29 Z9 29 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2009 VL 181 IS 2 BP 605 EP 626 DI 10.1088/0067-0049/181/2/605 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 426ZF UT WOS:000264746700019 ER PT J AU Bell, JA Geismar, H AF Bell, Joshua A. Geismar, Haidy TI Materialising Oceania: New ethnographies of things in Melanesia and Polynesia SO AUSTRALIAN JOURNAL OF ANTHROPOLOGY LA English DT Review ID OBJECTS; RETHINKING; PACIFIC; CONTEXT AB Oceania Occupies an intriguing place within anthropology's genealogy. In the introduction to this collection of essays, we examine the role of the ethnography of Oceania in the development of our anthropological perspectives oil materialisation, the dynamic process by which persons and things are inter-related. Building upon the recent resurgence of theoretical interests in things we use the term materialisation (rather than material Culture or materiality) to capture the vitality of the lived processes by which ideas of objectivity and subjectivity, persons and things, minds and bodies are entangled. Taking a processual view, we advocate for an Oceanic anthropology that continues to engage with things on the ground; that asks what strategies communities use to materialistic their social relations, desires and values; and that recognises how these processes remain important tools for understanding historical and contemporary Oceanic societies. Examining these locally articulated processes and forms contributes to a material (re)turn for anthropology that clarifies how we, as scholars, think about things more widely. C1 [Bell, Joshua A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Geismar, Haidy] NYU, New York, NY 10003 USA. RP Bell, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 152 TC 7 Z9 8 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1035-8811 EI 1757-6547 J9 AUST J ANTHROPOL JI Aust. J. Anthropol. PD APR PY 2009 VL 20 IS 1 BP 3 EP 27 DI 10.1111/j.1757-6547.2009.00001.x PG 25 WC Anthropology SC Anthropology GA 443FI UT WOS:000265895200002 ER PT J AU Bell, JA AF Bell, Joshua A. TI Documenting discontent: Struggles for recognition in the Purari Delta of Papua New Guinea SO AUSTRALIAN JOURNAL OF ANTHROPOLOGY LA English DT Article ID STORIES AB Within the context of the Purari Delta's transforming materialities of resource extraction, and the legacy of the Torn Kabu iconoclastic modernist movement (1946-69), 1 examine the processes of materialisation bound LIP With two related but different things: heirlooms (eve uku) and documents (Incorporated Land Group (ILG) forms). Eve uku ('hand head') lie within a continuum of things (names, relations, totemic ancestral spirit-beings and sites in the environment) through which ancestral actions are shown to have happened, and descent groups' identities manifest. However, given the ambiguous status of the traditional past among the I'ai, the power of these forms is circumscribed to the village thus making them ineffectual tokens in the bid to secure royalties from resource extraction. Instead, highly coveted documents known as ILG certificates have emerged as efficacious things by which royalties can be secured. Examining these certificates as objects, I investigate how these documents help materialise anew descent groups, communities' relations to their environment and thus their aspirations for development with its attending materialities. The problem for the I'ai, however, remains how to obtain these documents and, as with eve uku, how to control them. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Bell, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. NR 67 TC 11 Z9 11 U1 1 U2 3 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1035-8811 J9 AUST J ANTHROPOL JI Aust. J. Anthropol. PD APR PY 2009 VL 20 IS 1 BP 28 EP 47 DI 10.1111/j.1757-6547.2009.00002.x PG 20 WC Anthropology SC Anthropology GA 443FI UT WOS:000265895200003 ER PT J AU Perotto-Baldivieso, HL Melendez-Ackerman, E Garcia, MA Leimgruber, P Cooper, SM Martinez, A Calle, P Ramos Gonzales, OM Quinones, M Christen, CA Pons, G AF Perotto-Baldivieso, Humberto L. Melendez-Ackerman, Elvia Garcia, Miguel A. Leimgruber, Peter Cooper, Susan M. Martinez, Alma Calle, Paulina Ramos Gonzales, Olga M. Quinones, Maya Christen, Catherine A. Pons, Gaspar TI Spatial distribution, connectivity, and the influence of scale: habitat availability for the endangered Mona Island rock iguana SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Connectivity; Cyclura cornuta stejnegeri; Habitat spatial distribution; Landscape structure; Mona Island; Mona rock iguana; Scale ID CYCLURA-CORNUTA-STEJNEGERI; LANDSCAPE CONNECTIVITY; CONSERVATION; DISPERSAL; PATCHES; INDEXES AB The Caribbean region is one of the five leading biodiversity hotspots in the world. Analysis of the spatial structure of critical habitats and how it affects endemic species in this region is essential baseline information for biodiversity monitoring and management. We quantified and evaluated the spatial structure and connectivity of depression forests on Mona Island and their potential impact on Mona Island rock iguana habitat, as a framework to assess spatial distribution, connectivity, and the issue of scale in small and widely dispersed habitats. Using IKONOS imagery, we mapped and delineated depression forests at four different scales (minimum mapping units: < 100, 100, 500, and 1,000 m), and calculated landscape metrics describing their spatial structure, and connectivity, for each map resolution. Our approach resulted in a more detailed map than previously described maps, providing better information on habitat connectivity for iguanas. The comparison of the island landscape mapped at different scales provided evidence on how changing scales affect the output of spatial metrics and may have a significant impact when planning decisions and assigning conservation priorities. It also highlighted the importance of adequate ecological scales when addressing landscape management and conservation priorities. The analysis of landscapes at multiple scales provided a mechanism to evaluate the role of patch detection and its effect on the interpretation of connectivity and spatial structure of suitable areas for species with small and widely dispersed habitats. These methodologies can be applied other species, in different environments, with similar limitations related to connectivity and habitat availability. C1 [Perotto-Baldivieso, Humberto L.; Cooper, Susan M.] Texas AgriLife Res, Uvalde, TX 78801 USA. [Melendez-Ackerman, Elvia; Martinez, Alma; Calle, Paulina] Univ Puerto Rico, ITES, San Juan, PR 00931 USA. [Melendez-Ackerman, Elvia; Garcia, Miguel A.; Martinez, Alma; Calle, Paulina; Pons, Gaspar] Univ Puerto Rico, CATEC, CREST, San Juan, PR 00931 USA. [Ramos Gonzales, Olga M.; Quinones, Maya] USDA Forest Serv, IITF, Jardin Bot Sur, San Juan, PR 00926 USA. [Leimgruber, Peter; Christen, Catherine A.] Smithsonian Inst, Natl Zool Pk, Front Royal, VA 22630 USA. [Garcia, Miguel A.; Pons, Gaspar] Natl Pk Serv, Dept Nat & Environm Resources, San Juan, PR 00936 USA. [Perotto-Baldivieso, Humberto L.] Casilla, La Paz, Bolivia. RP Perotto-Baldivieso, HL (reprint author), Texas AgriLife Res, 1619 Garner Field Rd, Uvalde, TX 78801 USA. EM hperotto@tamu.edu RI Perotto-Baldivieso, Humberto/C-5886-2011; Leimgruber, Peter/O-1304-2015 OI Perotto-Baldivieso, Humberto/0000-0001-7700-7110; Leimgruber, Peter/0000-0002-3682-0153 FU NSF-CREST CATEC [HRD-0206200] FX We would like to thank G. Olivieri, H. Lopez, and J. Sustache for their valuable help during the Weld work in Mona Island, M. Jimnez and S. Martinuzzi for the comments and suggestions for the image analysis, M. Figueroa and J. N. Romo for their help during the data analysis, and E. Hollister, X. Ben Wu, H. Hood, and the two anonymous reviewers for their review comments that helped improve this manuscript. This project was funded by NSF-CREST CATEC HRD-0206200, federal support from the Smithsonian Latino Center, the Wildlife Restoration Program ( Project W14, US Fish and Wildlife Service), the Department of Natural and Environmental Resources of the Commonwealth of Puerto Rico, and the Environmental Science Program of the University of Puerto Rico at R o Piedras. NR 37 TC 10 Z9 12 U1 2 U2 18 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2009 VL 18 IS 4 BP 905 EP 917 DI 10.1007/s10531-008-9520-3 PG 13 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 424DT UT WOS:000264546400009 ER PT J AU Songer, M Aung, M Senior, B DeFries, R Leimgruber, P AF Songer, Melissa Aung, Myint Senior, Briony DeFries, Ruth Leimgruber, Peter TI Spatial and temporal deforestation dynamics in protected and unprotected dry forests: a case study from Myanmar (Burma) SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Tropical dry forests; Biodiversity; Change detection; Deforestation rates; Fragmentation; Protected areas; Forest dynamics; Land use change; Remote sensing; Landsat; ASTER ID DEER CERVUS-ELDI; MANAGEMENT EFFECTIVENESS; SOUTHEAST-ASIA; RAIN-FORESTS; COVER CHANGE; AREA SYSTEM; CONSERVATION; BIODIVERSITY; PATTERNS; PARKS AB Tropical dry forests are more threatened, less protected and especially susceptible to deforestation. However, most deforestation research focuses on tropical rain forests. We analyzed spatial and temporal changes in land cover from 1972 through 2005 at Chatthin Wildlife Sanctuary (CWS), a tropical dry forest in Myanmar (Burma). CWS is one of the largest protected patches of tropical dry forest in Southeast Asia and supports over half the remaining wild population of the endangered Eld's deer. Between 1973 and 2005, 62% of forest was lost at an annual rate of 1.86% in the area, while forest loss inside CWS was only 16% (0.45% annually). Based on trends found during our study period, dry forests outside CWS would not persist beyond 2019, while forests inside CWS would persist for at least another 100 years. Analysis of temporal deforestation patterns indicates the highest rate of loss occurred between 1992 and 2001. Conversion to agriculture, shifting agriculture, and flooding from a hydro-electric development were the main deforestation drivers. Fragmentation was also severe, halving the area of suitable Eld's deer habitat between 1973 and 2001, and increasing its isolation. CWS protection efforts were effective in reducing deforestation rates, although deforestation effects extended up to 2 km into the sanctuary. Establishing new protected areas for dry forests and finding ways to mitigate human impacts on existing forests are both needed to protect remaining dry forests and the species they support. C1 [Songer, Melissa; Senior, Briony; Leimgruber, Peter] Smithsonian Inst, Natl Zool Pk, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Aung, Myint] SICAS Off, Kamayut Township, Yangon, Myanmar. [DeFries, Ruth] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. RP Songer, M (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM songerm@si.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU NASA FX We thank the staff of Chatthin Wildlife Sanctuary for their assistance in collection of field data and Dan Kelly and Melanie Delion for assistance in data management in the laboratory. This project was primarily funded by a grant awarded by NASA to the Conservation Non- Governmental Working Group. NR 59 TC 14 Z9 15 U1 9 U2 62 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD APR PY 2009 VL 18 IS 4 BP 1001 EP 1018 DI 10.1007/s10531-008-9490-5 PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 424DT UT WOS:000264546400015 ER PT J AU Miglietta, MP Lessios, HA AF Miglietta, Maria Pia Lessios, Harilaos A. TI A silent invasion SO BIOLOGICAL INVASIONS LA English DT Article DE Invasive species; Morphological response; Hydrozoa; Turritopsis; Medusa ID MOLECULAR EVIDENCE; BIOLOGICAL INVASIONS; MULTIPLE INVASIONS; SEQUENCE ALIGNMENT; RAPID EVOLUTION; CNIDARIA; MARINE; HYDROZOA; PHYLOGEOGRAPHY; INCREASES AB Invasions mediated by humans have been reported from around the world, and ships' ballast water has been recognized as the main source of marine invaders worldwide. Some invasions have dramatic economic and ecological consequences. On the other hand, many invasions especially in the marine realm, can go unnoticed. Here we identify a human mediated, worldwide introduction of the hydrozoan species Turritopsis dohrnii. The normal life cycle of hydrozoans involves the asexual budding of medusae from colonial polyps. Medusae of Turritopsis, however, when starved or damaged, are able to revert their life cycle, going back to the polyp stage through a process called transdifferentiation. They can thus easily survive through long journeys in cargo ships and ballast waters. We have identified a clade of the mitochondrial 16S gene in Turritopsis which contains individuals collected from Japan, the Pacific and Atlantic coasts of Panama, Florida, Spain, and Italy differing from each other in only an average of 0.31% of their base-pairs. Fifteen individuals from Japan, Atlantic Panama, Spain, and Italy shared the same haplotype. Turritopsis dohrnii medusae, despite the lack of genetic differences, are morphologically different between the tropical and temperate locations we sampled, attesting to a process of phenotypic response to local conditions that contributes to making this grand scale invasion a silent one. C1 [Miglietta, Maria Pia; Lessios, Harilaos A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Miglietta, MP (reprint author), Penn State Univ, Dept Biol, University Pk, PA 16802 USA. EM mp.miglietta@psu.edu FU Smithsonian Marine Science Network FX We thank the staff of the Smithsonian Marine Stations of Naos, Bocas del Toro, Galeta and Fort Pierce for logistical support. We also thank S. Piraino for sharing information, A. Faucci and M. Rossi for discussion and suggestions on the manuscript, A. Driskell for DNA extraction and sequencing of some of the specimens, and C. S. Dugas for collecting some of the specimens from Bocas del Toro. This work was funded by a Smithsonian Marine Science Network postdoctoral fellowship to M. P. M. NR 38 TC 24 Z9 25 U1 9 U2 72 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD APR PY 2009 VL 11 IS 4 BP 825 EP 834 DI 10.1007/s10530-008-9296-0 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 413IB UT WOS:000263785700005 ER PT J AU Wyckhuys, KAG Koch, RL Kula, RR Heimpel, GE AF Wyckhuys, Kris A. G. Koch, Robert L. Kula, Robert R. Heimpel, George E. TI Potential exposure of a classical biological control agent of the soybean aphid, Aphis glycines, on non-target aphids in North America SO BIOLOGICAL INVASIONS LA English DT Article DE Biological control; Ecological risk assessment; Aphids; Parasitoids; Binodoxys; Prairie habitats; Community-assemblage studies; Spatial modeling; CLIMEX; GARP ID PARASITOID BINODOXYS-COMMUNIS; ARTHROPOD PESTS; ATTENDING ANTS; TRICHOGRAMMA-BRASSICAE; NATURAL ENEMIES; RISK; INTRODUCTIONS; HOMOPTERA; INVASION; HYMENOPTERA AB In summer 2007, the Asian parasitoid Binodoxys communis (Hymenoptera: Braconidae) was released in North America for control of the exotic soybean aphid, Aphis glycines (Hemiptera: Aphididae). Despite its comparatively narrow host range, releases of B. communis may still constitute a risk to native aphid species. To estimate the risk of exposure of non-target aphids to B. communis, we merged assessments of temporal co-occurrence with projections of spatial overlap between B. communis and three native aphid species, and in-field measurements of the incidence of ecological filters that may protect these aphids from parasitism. Temporal co-occurrence was assessed between A. glycines and native aphids (Aphis asclepiadis, Aphis oestlundi, and Aphis monardae) at four different locations in Minnesota, USA. The degree of temporal overlap depended greatly on location and aphid species, ranging between 0 and 100%. All of the native aphids were tended by multiple species of ants, with overall ant-attendance ranging from 26.1 to 89.6%. During temporal overlap with A. glycines, 53 +/- 11% of A. monardae colonies were partly found in flower heads of their host plant, with flowers acting as a physical refuge for this aphid. The extent of geographic overlap between B. communis and native aphids based upon Climex modeling was 17-28% for A. monardae, 13-22% for A. oestlundi, 46-55% for A. asclepiadis and 12-24% for the A. asclepiadis species complex. The estimated overall probability of potential exposure of B. communis on native aphids was relatively low (P = 0.115) for A. oestlundi and high (P = 0.550) for A. asclepiades. Physical and ant-mediated refuges considerably lowered probability of population-level impact on A. monardae, and could lead to substantial reduction of exposure for the other native aphids. These findings are used to make broader statements regarding the ecological safety of current B. communis releases and their potential impact on native aphid species in North America. C1 [Wyckhuys, Kris A. G.] Univ Jorge Tadeo Lozano, Hort Res Ctr CIAA, Chia Cundinamarca 140196, Colombia. [Koch, Robert L.] Minnesota Dept Agr, Div Plant Protect, St Paul, MN USA. [Kula, Robert R.] Smithsonian Inst, Systemat Entomol Lab, Washington, DC 20560 USA. [Heimpel, George E.] Univ Minnesota, Dept Entomol, St Paul, MN 55108 USA. RP Wyckhuys, KAG (reprint author), Univ Jorge Tadeo Lozano, Hort Res Ctr CIAA, Carretera Cent Norte,3 Kms Adelante Caro, Chia Cundinamarca 140196, Colombia. EM kwyckhuys@hotmail.com FU USDA-RAMP; North Central Soybean Research Council; Minnesota Agricultural Experiment Station FX This paper is dedicated to Robert J. O'Neil, a pioneer in the field of biological control and source of inspiration to many, who passed away in Feb. 2008. We would like to thank Norbert Brotz and Jeremy Chacon for help with field research. We are grateful to Susana Acheampong, Nicolas Desneux and Wang LiMin for providing unpublished data. This work benefited greatly from technical assistance by Robert Venette ( US Forest Service). The help of David Voegtlin and James C. Trager in identifying the respective aphid and ant species was invaluable. We are also grateful to Bob Djupstrom, Ellen Fuge and the Minnesota DNR, Scientific and Natural Areas Program for their granting permission to conduct research in Minnesota prairie sites. Lastly, we would like to thank Jeffrey Corney and John Haarstad at the Cedar Creek Natural History Area for their assistance in selecting appropriate field sites. This work was funded in part by the multi-state USDA-RAMP project, in part by the North Central Soybean Research Council, and in part by the Minnesota Agricultural Experiment Station. NR 84 TC 19 Z9 19 U1 4 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD APR PY 2009 VL 11 IS 4 BP 857 EP 871 DI 10.1007/s10530-008-9299-x PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 413IB UT WOS:000263785700008 ER PT J AU Roche, DG Torchin, ME Leung, B Binning, SA AF Roche, Dominique G. Torchin, Mark E. Leung, Brian Binning, Sandra A. TI Localized invasion of the North American Harris mud crab, Rhithropanopeus harrisii, in the Panama Canal: implications for eradication and spread SO BIOLOGICAL INVASIONS LA English DT Article DE Introduced species; Biological invasions; Shipping; Global invader; Salinity tolerance ID BIOLOGICAL INVASIONS; POPULATION-STRUCTURE; PROPAGULE PRESSURE; UNITED-STATES; MARINE; CONSEQUENCES; INVASIBILITY; TEMPERATURE; SALINITY; TRANSPORT AB As the rate of biological invasions continues to increase, a growing number of aquatic introduced species are becoming globally widespread. Despite this ubiquitous phenomenon, rarely do we discover aquatic invaders early enough to allow the possibility of eradication. Recently, the North American Harris mud crab (Rhithropanopeus harrisii) was found in the waters adjacent to the Panama Canal and herein we provide an assessment of the crab's distribution in Panama to evaluate the possibility of eradication. Using salinity tolerance experiments, we also evaluate the potential for further spread of this crab within the Canal. Our results suggest that populations of R. harrisii are currently limited to two manmade lagoons which are adjacent to the Panama Canal. Our experiments suggest that both juvenile and adult R. harrisii can survive in salinities found outside its current range in Panama. Although it is difficult to predict the potential for future spread and impacts in Panama, current management strategies could reduce the probability for spread locally as well as elsewhere in the world given the intensity of shipping in this region. The current containment of this invader suggests that a localized eradication may be possible. C1 [Roche, Dominique G.; Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Roche, Dominique G.; Leung, Brian; Binning, Sandra A.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM torchinm@si.edu RI Roche, Dominique/K-7426-2012; OI Roche, Dominique/0000-0002-3326-864X; Binning, Sandra/0000-0002-2804-9979 FU Smithsonian Tropical Research Institute; Secretaria Nacional de Ciencia; Tecnologia e Innovacion de Panama; Natural Sciences and Engineering Research Council of Canada; Fonds Quebecois de Recherche sur la Nature et les Technologies; Office Quebec Amerique pour la Jeunesse; McGill-STRI NEO FX We thank Y. Kam and C. Schloeder who provided immense assistance with field and laboratory work. We are also grateful to the ACP for granting access to restricted sites and to M. Calderon, F. O. Guardia, H. Broce and D. Muschett for providing information, assistance in the field and suggestions throughout the study. We acknowledge the Smithsonian Tropical Research Institute and the Secretaria Nacional de Ciencia, Tecnologia e Innovacion de Panama for financial support and grants from the Natural Sciences and Engineering Research Council of Canada, the Fonds Quebecois de Recherche sur la Nature et les Technologies, the Office Quebec Amerique pour la Jeunesse, and McGill-STRI NEO to DGR. NR 47 TC 8 Z9 11 U1 2 U2 27 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 EI 1573-1464 J9 BIOL INVASIONS JI Biol. Invasions PD APR PY 2009 VL 11 IS 4 BP 983 EP 993 DI 10.1007/s10530-008-9310-6 PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 413IB UT WOS:000263785700019 ER PT J AU Barse, WP AF Barse, William P. TI The Early Ronquin Paleosol and the Orinocan Ceramic Sequence SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article CT 72nd Annual Meeting of the Society-for-American-Archaeology CY 2007 CL Chicago, IL SP Soc Amer Archaeol DE Ronquin; Barrancas; Saladero; paleosols AB In their 1958 monograph, Cruxent and Rouse suggested that the lower levels of the Ronquin site could be subdivided into more than one period, possibly a developmental change from Saladeroto Barrancas-style ceramics. This paper examines evidence for this suggested revision based on reanalysis of the existing Ronquin collection, as well other available information. Evidence from new radiocarbon dates and additional archaeological sites with paleosol horizons containing related ceramic complexes suggest that Cruxent and Rouse's observation is inaccurate; the lower levels of the Ronquin site, termed Early Ronquin by Howard, is best seen as a single occupation dating to the middle of the first millennium AD. It is part of a widespread stylistic interaction sphere extending from the Lower Orinoco up to the Atures Rapids. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20013 USA. RP Barse, WP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM bbarse89@yahoo.com NR 23 TC 1 Z9 1 U1 0 U2 0 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118, AFGHANISTAN SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2009 VL 50 IS 1 BP 85 EP 98 PG 14 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 471AK UT WOS:000268023900007 ER PT J AU Descantes, C Speakman, RJ Glascock, MD AF Descantes, Christophe Speakman, Robert J. Glascock, Michael D. TI Neutron Activation Analysis of Ceramics from Five Archaeological Sites in Antigua, West Indies SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article CT 72nd Annual Meeting of the Society-for-American-Archaeology CY 2007 CL Chicago, IL SP Soc Amer Archaeol DE Caribbean; provenance studies; Antigua; ceramics; NAA ID POTTERY AB Ceramics of multiple styles from five archaeological sites on Antigua were analyzed at the University of Missouri Research Reactor Center to obtain a better understanding of ceramic compositional variability within Antigua. Bulk chemical characterizations of pottery were determined by neutron activation analysis. Findings suggest that all of the ceramics in our sample were made from locally available, naturally tempered clays, and that there is compositional continuity through time despite the different stylistic and locational attributes of the sherds. C1 [Descantes, Christophe] Univ Calif Berkeley, Archaeol Res Facil, Berkeley, CA 94720 USA. [Speakman, Robert J.] Museum Support Ctr, Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Glascock, Michael D.] Univ Missouri, Res Reactor Ctr, Archaeometry Lab, Columbia, MO 65211 USA. RP Descantes, C (reprint author), Univ Calif Berkeley, Archaeol Res Facil, 2251 Coll Bldg, Berkeley, CA 94720 USA. EM cdescantes@berkeley.edu NR 19 TC 1 Z9 1 U1 0 U2 2 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118, AFGHANISTAN SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD APR PY 2009 VL 50 IS 1 BP 147 EP 155 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 471AK UT WOS:000268023900010 ER PT J AU Mueller, T Selva, N Pugacewicz, E Prins, E AF Mueller, Thomas Selva, Nuria Pugacewicz, Eugeniuz Prins, Erik TI Scale-sensitive landscape complementation determines habitat suitability for a territorial generalist SO ECOGRAPHY LA English DT Article ID BIALOWIEZA PRIMEVAL FOREST; RAVENS CORVUS-CORAX; SELECTION; QUALITY; BIRDS; POPULATIONS; PREDATION; DENSITY; MODELS; CONSEQUENCES AB Evaluating habitat suitability is often complex, as habitat effects may be scale-dependent, critical resources may be spatially segregated, and resource availability may also depend on intra- and inter-specific interactions. Using analyses that spanned multiple years and spatial scales, we investigated habitat requirements of a territorial generalist, the common raven Corvus corax, in a relatively pristine woodland, Bialowieza Forest (E Poland). We compiled data from multiple raven surveys conducted between 1985 and 2001. Ravens were regularly distributed over the entire study area but declined in density over 50% within the 16 yr interval. In the same period game and forest management significantly reduced ungulate densities and likely diminished the habitat quality with regard to food supply, especially carrion. To better understand habitat requirements of ravens we studied breeding performance in relation to three different habitat types across multiple scales: open areas, coniferous-dominated forest, and deciduous-dominated forest. We found a prominent dissimilarity between raven nesting and foraging habitats highlighting the importance of resource complementation for ravens. On a fine scale, large old pines were exclusively selected as nesting trees and nesting areas were generally coniferous-dominated. However, at increasingly broader scales, coniferous habitats were negatively associated with raven reproductive success as those habitats likely provide a lower food supply. Only where the coniferous nesting areas at smaller scales were complemented with high percentages of deciduous forests and open areas at broader scales did the breeding performance increase. In addition to habitat composition, intra-specific interactions were important determinants of reproductive performance and very successful neighbors decreased reproductive performance of a focal pair. Most of previous studies have investigated resource complementation in terms of habitat edges or proximity of complementing resource patches. Our study demonstrates that the concept of landscape complementation also applies to gradients in landscape composition and emphasizes the importance of scales and intraspecific interactions in habitat analyses. C1 [Mueller, Thomas] Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Mueller, Thomas] Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA 22630 USA. [Mueller, Thomas] Univ Marburg, Dept Anim Ecol, DE-35032 Marburg, Germany. [Selva, Nuria] Polish Acad Sci, Inst Nat Conservat, PL-31120 Krakow, Poland. [Prins, Erik] PRINS, DK-2970 Horsholm, Denmark. RP Mueller, T (reprint author), Univ Maryland, Grad Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. EM muellert@gmail.com RI Selva, Nuria/J-6970-2013; Mueller, Thomas/A-1740-2014 OI Selva, Nuria/0000-0003-3389-201X; Mueller, Thomas/0000-0001-9305-7716 NR 58 TC 9 Z9 10 U1 2 U2 18 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0906-7590 J9 ECOGRAPHY JI Ecography PD APR PY 2009 VL 32 IS 2 BP 345 EP 353 DI 10.1111/j.1600-0587.2008.05694.x PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 444YA UT WOS:000266015600016 ER PT J AU Newsome, SD Tinker, MT Monson, DH Oftedal, OT Ralls, K Staedler, MM Fogel, ML Estes, JA AF Newsome, Seth D. Tinker, M. Tim Monson, Daniel H. Oftedal, Olav T. Ralls, Katherine Staedler, Michelle M. Fogel, Marilyn L. Estes, James A. TI Using stable isotopes to investigate individual diet specialization in California sea otters (Enhydra lutris nereis) SO ECOLOGY LA English DT Article DE dietary specialization; Enhydra lutris nereis; isotopic niche; southern sea otter; stable isotopes; vibrissae ID LIONS EUMETOPIAS-JUBATUS; FORAGING STRATEGIES; PHOCA-VITULINA; NITROGEN; CARBON; DELTA-N-15; VIBRISSAE; PATTERNS; GROWTH; FRACTIONATION AB Differences in diet composition among conspecifics (dietary specialization) have been documented across a broad range of taxonomic groups and habitats, and such variation at the individual level is increasingly recognized as an important component of diversity in trophic interactions. Accurate identification of individual dietary specialization, however, requires longitudinal dietary records that are labor-intensive and cost-prohibitive to obtain for many species. Here we explore the use of stable isotopes (delta(13)C and delta(15)N) as a promising technique for detecting and quantifying patterns of individual dietary specialization. Southern sea otters (Enhydra lutris nereis) offer a unique opportunity for testing this approach because (1) they consume a wide variety of prey that span multiple trophic levels, habitats, and ecologically defined functional groups; and (2) individual diet specialization can be validated with existing observational data. We analyzed the isotopic composition of sea otter vibrissae (n = 31) in order to characterize inter- and intra-individual variation in sea otter diets at Monterey Bay, California, USA. At the population level, sea otters showed substantial variation in both delta(13)C and delta(15)N values, occupying nearly all of the "isotopic space'' created by the diversity of isotopic signatures of potential prey taxa. Most of the variation in sea otter vibrissae was accounted for by differences between individuals, with much less contributed by within-individual variation. A majority of sea otters (similar to 80%) showed relatively little temporal variability in isotopic composition, suggesting that the proportional composition of most individuals' diets is relatively constant over time; a few individuals (similar to 20%) exhibited a high degree of intra-vibrissa isotopic variability, suggesting seasonal shifts in diet composition. These results and our interpretation of them were supported by long-term observational data on the diets of radio-tagged sea otters from the same population (n = 23). Our results demonstrate that stable isotopes can provide an efficient tool for measuring individual-and population-level dietary breadth and may be useful for studying populations where longitudinal data on individuals would otherwise be impossible to acquire. This will be critical for examining the causes and consequences of dietary variation within and among consumer populations, thereby improving our understanding of these important ecological and evolutionary processes at the community level. C1 [Newsome, Seth D.; Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Tinker, M. Tim] US Geol Survey, Western Ecol Res Ctr, Long Marine Lab, Santa Cruz, CA 95060 USA. [Monson, Daniel H.] USGS Alaska Sci Ctr, Anchorage, AK 99503 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ralls, Katherine] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Staedler, Michelle M.] Monterey Bay Aquarium, Sea Otter Res & Conservat, Monterey, CA 93940 USA. [Estes, James A.] Univ Calif Santa Cruz, Long Marine Lab, Ctr Ocean Hlth, Santa Cruz, CA 95060 USA. RP Newsome, SD (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA. EM snewsome@ciw.edu RI Tinker, Martin/F-1277-2011; Monson, Daniel/N-4469-2013 OI Monson, Daniel/0000-0002-4593-5673 FU National Science Foundation [OCE-0345943]; Carnegie Institution of Washington; Mia J. Tegner Memorial Student Research Grant Program in Historical Ecology; Myers Oceanographic and Marine Biology Trust; UCSC Long Marine Laboratory; PADI Foundation FX Thanks to the Monterey Bay National Marine Sanctuary Foundation and the Marine Mammal Commission for funding collection of the prey samples. We thank E. Snyder, C. Mancuso, and W. Wurzel for laboratory assistance and C. Martinez del Rio, G. Bentall, A. Kage, and P. Koch for informative discussions. We thank T. Gelatt, M. Etnier, and A. C. Jakle for constructive reviews. S. D. Newsome was partially funded by a National Science Foundation grant (OCE-0345943), Carnegie Institution of Washington, and through generous support from the Mia J. Tegner Memorial Student Research Grant Program in Historical Ecology, Myers Oceanographic and Marine Biology Trust, UCSC Long Marine Laboratory, and the PADI Foundation. Any use of trade, product, or firm names in this publication is for descriptive purposes only and does not imply endorsement by the U.S. government, the Carnegie Institution of Washington, the University of California, or the Monterey Bay Aquarium. NR 45 TC 126 Z9 127 U1 9 U2 93 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 APR PY 2009 VL 90 IS 4 BP 961 EP 974 DI 10.1890/07-1812.1 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 427AY UT WOS:000264753400014 PM 19449691 ER PT J AU Egeland, GM Ponce, R Bloom, NS Knecht, R Loring, S Middaugh, JP AF Egeland, G. M. Ponce, Rafael Bloom, Nicolas S. Knecht, Rick Loring, Stephen Middaugh, John P. TI Hair methylmercury levels of mummies of the Aleutian Islands, Alaska SO ENVIRONMENTAL RESEARCH LA English DT Article DE Indigenous Peoples; Hair; Mercury; Pre-historic ID ATMOSPHERIC MERCURY DEPOSITION; FISH; ETHYLATION; EXPOSURE; AGE AB Ancient human hair specimens can shed light on the extent of pre-historic exposures to methylmercury and provide valuable comparison data with current-day exposures, particularly for Indigenous Peoples who continue to rely upon local traditional food resources. Human hair from ancient Aleutian Island Native remains were tested for total and methylmercury (Hg, MeHg) and were radiocarbon dated. The remains were approximately 500 years old (1450 A.D.). For four adults, the mean and median total hair mercury concentration was 5.8 ppm (SD = 0.9). In contrast, MeHg concentrations were lower with a mean of 1.2 ppm (SD = 1.8) and a median of 0.54 ppm (0.12-3.86). For the five infants, the mean and median MeHg level was 1.2 ppm (SD = 1.8) and 0.20 ppm (0.007-4.61), respectively. Segmental analyses showed variations in MeHg concentrations in 1-cm segments, consistent with fluctuations in naturally occurring exposure to mercury through dietary sources. The levels are comparable to or lower than those found in fish and marine mammal-eating populations today who rely far less on subsistence food than pre-historic humans. The findings are, therefore, compatible with increased anthropogenic release of trace metals during the past several centuries. (C) 2008 Elsevier Inc. All rights reserved. C1 [Egeland, G. M.] McGill Univ, Ctr Indigenous Peoples Nutr & Environm CINE, Ste Anne De Bellevue, PQ H9X 3V9, Canada. [Ponce, Rafael] Amgen WA, Toxicology, Seattle, WA USA. [Bloom, Nicolas S.] Studio Geochim, Seattle, WA 98105 USA. [Knecht, Rick] Univ Alaska, Dept Alaska Native & Rural Dev, Anchorage, AK 99508 USA. [Loring, Stephen] Natl Museum Nat Hist, Smithsonian Inst, Arct Studies Ctr, Washington, DC 20013 USA. [Middaugh, John P.] Nevada Dept Hlth & Human Serv, Carson City, NV 89706 USA. RP Egeland, GM (reprint author), McGill Univ, Ctr Indigenous Peoples Nutr & Environm CINE, 21,111 Lakeshore Rd, Ste Anne De Bellevue, PQ H9X 3V9, Canada. EM grace.egeland@mcgill.ca; rponce@amgen.com; nicolasb@nickslab.org; Knecht@palaunet.com; lorings@si.edu; middaugh@SNHDMAIL.ORG NR 32 TC 10 Z9 10 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 J9 ENVIRON RES JI Environ. Res. PD APR PY 2009 VL 109 IS 3 BP 281 EP 286 DI 10.1016/j.envres.2008.11.004 PG 6 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA 426JT UT WOS:000264704800011 PM 19195649 ER PT J AU Courtenay, WR Collette, BB Essington, TE Hilborn, R Orr, JW Pauly, D Randall, JE Smith-Vaniz, WF AF Courtenay, Walter R., Jr. Collette, Bruce B. Essington, Timothy E. Hilborn, Ray Orr, James W. Pauly, Daniel Randall, John E. Smith-Vaniz, William F. TI Risks of Introductions of Marine Fishes: Reply to Briggs SO FISHERIES LA English DT Editorial Material ID LIONFISH PTEROIS-VOLITANS; NORTH-ATLANTIC; MANAGEMENT; SCORPAENIDAE; INVASION; ISLANDS; SEAS AB This is a rebuttal to a publication by John C. Briggs in the April 2008 issue of Fisheries in Which be suggested introducing fishes and invertebrates from the North Pacific into the North Atlantic to increase diversity toward improving fisheries ill the latter. We argue otherwise for reasons that Briggs downplayed or never considered. Using examples of introductions within the Pacific bind the Atlantic, and movements of species from the Pacific to the Atlantic, we provide a record of failures and damage or dangers to native species from the few introductions that became successful. We argue that a lack of diversity of fishes and invertebrates in the North Atlantic versus that of the North Pacific is not the problem to be corrected by introductions is Briggs suggested. A record of overfishing and management policies is the problem in the North Atlantic. Introductions from the North Pacific to the North Atlantic are not worth the costs or the environmental risks involved C1 [Courtenay, Walter R., Jr.] Florida Atlantic Univ, Gainesville, FL USA. [Collette, Bruce B.] Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20560 USA. [Essington, Timothy E.; Hilborn, Ray] Univ Washington, Coll Aquat & Fisheries Sci, Seattle, WA 98195 USA. [Orr, James W.] NOAA, Natl Marine Fisheries Serv, Alaska Fisheries Sci Ctr, Seattle, WA 98115 USA. [Pauly, Daniel] Univ British Columbia, Fisheries Ctr, Vancouver, BC V5Z 1M9, Canada. [Randall, John E.] Bernice P Bishop Museum, Honolulu, HI USA. [Smith-Vaniz, William F.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Courtenay, WR (reprint author), Florida Atlantic Univ, Gainesville, FL USA. EM courtenayw@yahoo.com RI Hilborn, Ray/D-6332-2013 NR 43 TC 3 Z9 3 U1 0 U2 11 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0363-2415 J9 FISHERIES JI Fisheries PD APR PY 2009 VL 34 IS 4 BP 181 EP 186 DI 10.1577/1548-8446-34.4.181 PG 6 WC Fisheries SC Fisheries GA 477NC UT WOS:000268524800003 ER PT J AU Helson, JE Capson, TL Johns, T Aiello, A Windsor, DM AF Helson, Julie E. Capson, Todd L. Johns, Timothy Aiello, Annette Windsor, Donald M. TI Ecological and evolutionary bioprospecting: using aposematic insects as guides to rainforest plants active against disease SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Article ID DRUG DISCOVERY; SEQUESTRATION; COEVOLUTION; CONSERVATION; COLLECTION; ALKALOIDS AB We examined Coleoptera and Lepidoptera assemblages feeding on two different groups of plants: one in which plants were active against cancer cell lines and/or protozoan parasites responsible for tropical parasitic diseases, and a second group that was inactive in the same bioassays. Aposematic species were found on nine of the ten active plant species, but on only four of the ten inactive plant species. Non-aposematic insects did not show a significant difference in their association with active versus inactive plants. Our results suggest that the presence of aposematic, herbivorous insects can be used to facilitate the identification of plants with compounds active against important human diseases. C1 [Helson, Julie E.; Capson, Todd L.; Johns, Timothy] McGill Univ, Dept Plant Sci, Ste Anne De Bellevue, PQ, Canada. [Capson, Todd L.; Aiello, Annette; Windsor, Donald M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Helson, JE (reprint author), Univ Toronto, Scarborough, ON M1C 1A4, Canada. EM capsont@si.edu FU US National Institutes of Health; US National Science Foundation; US Department of Agriculture through the International Cooperative Biodiversity Groups Program [1U01 TW01021-01, 1U01 TW006634-01]; Engineering Research Council of Canada (NSERC) PGS-A Fellowship; Levinson Fellowship FX The authors thank E Ortega, L Romero, and their colleagues for performing the bioassays reported in this study, R Aizpr a for confirming plant identifications, H Stock-well for helping with insect identifications, the Panamanian National Authority of the Environment for plant and insect collection permits (permit numbers for plants: SC/P-17-03, SC/P-22-03, SC/P-23-03, SC/P-2403, SC/P-25-03, SC/P-26-03, SC/P-27-03, and SC/P-2803; permit numbers for insects: SC/AP-1-05), ICBG participants P Coley, T Kursar, and M Heller for the use of laboratory facilities, and J Bede for input and support. We gratefully acknowledge financial support from the US National Institutes of Health, the US National Science Foundation, and the US Department of Agriculture through the International Cooperative Biodiversity Groups Program (grant numbers 1U01 TW01021-01 and 1U01 TW006634-01), an Engineering Research Council of Canada (NSERC) PGS-A Fellowship, and the Levinson Fellowship from the STRI-McGill NEO program. NR 28 TC 11 Z9 11 U1 0 U2 12 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 APR PY 2009 VL 7 IS 3 BP 130 EP 134 DI 10.1890/070189 PG 5 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 430GT UT WOS:000264977600018 ER PT J AU King, DA Davies, SJ Tan, S Noor, NSM AF King, David A. Davies, Stuart J. Tan, Sylvester Noor, Nur Supardi Md. TI Trees approach gravitational limits to height in tall lowland forests of Malaysia SO FUNCTIONAL ECOLOGY LA English DT Article DE mechanical limits to height; tree allometry; tree architecture; tropical forest ID TROPICAL RAIN-FOREST; MIXED DIPTEROCARP FOREST; PSEUDOTSUGA-TSUGA FOREST; WOOD DENSITY; ASYMPTOTIC HEIGHT; MAXIMUM HEIGHT; ADULT STATURE; LIFE-HISTORY; GROWTH; ALLOMETRY AB 1. In the absence of wind, tree height is limited by elastic instability, which occurs when a tree becomes too spindly to erect itself when bent from the vertical. To assess the extent to which trees approach this limit and characterize species stature in diverse tropical forests, we measured tree dimensions in tall, dense forests at Lambir Hills, National Park, Sarawak, Malaysia and Pasoh Forest Reserve, Peninsular Malaysia. From these measurements we determined characteristic adult heights and trunk diameters for 91 species. 2. Across all species, adult height scaled with adult diameter to the 2/3 power, as predicted for a column at its buckling limit. These heights were, on average, 65% of the buckling limit calculated for a cylindrical column with typical wood properties. 3. At a given diameter, the species of Lambir were 9% taller than those of Pasoh, a pattern related to the greater rainfall and density of trees at Lambir. 4. On the topographically rugged Lambir plot, large emergent trees were shorter on ridges than in hollows, whereas small, sheltered trees showed no relation between allometry and elevation. 5. Thus, trees may approach gravitational limits to height in favourable environments for growth where there are large advantages of height for light interception and trees are sheltered from wind. C1 [King, David A.; Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum, Cambridge, MA 02138 USA. [Davies, Stuart J.] Smithsonian Trop Res Inst, Balboa, Panama. [Tan, Sylvester] Sarawak Forestry Corp, Kuching, Sarawak, Malaysia. [Noor, Nur Supardi Md.] Forest Res Inst Malaysia, Forest Management & Conservat Div, Kuala Lumpur 52109, Malaysia. RP King, DA (reprint author), 610 NW 18th St, Corvallis, OR 97330 USA. EM dkingaz@yahoo.com FU Smithsonian Tropical Research Institute; Harvard University, USA [DEB-9107247, DEB-9629601]; Osaka City University, Japan [06041094, 08NP0901, 09NP0901]; CTFS-AA [INT-84-12201]; Conservation, Food and Health Foundation, Inc., USA; United Nations UNESCO-MAB [217.651.5, 217.652.5, 243.027.6, 213.164.4]; UNESCO-ROSTSEA [243.170.6]; National Institute for Environmental Studies, Japan FX The 52-ha long-term Ecological Research project at Lambir is a collaborative project of the Sarawak Forestry Corporation, Malaysia, the Center for Tropical Forest Science-Arnold Arboretum Asia Program (CTFS-AA) of the Smithsonian Tropical Research Institute and Harvard University, USA ( under NSF awards DEB-9107247 and DEB-9629601 to P. S. Ashton), and Osaka City University, Japan ( under Monbusho grant 06041094 to T. Yamakura, 08NP0901 to S. Tamura and 09NP0901 to S.Sasaki). The 50-ha forest plot at Pasoh is a collaborative project of the Forest Research Institute Malaysia (FRIM), under the leadership of Dr A. Rahim Nik, CTFS-AA (under NSF award INT-84-12201 to P.S. Ashton and S. Hubbell, and grants from Conservation, Food and Health Foundation, Inc., USA, and the United Nations UNESCO-MAB Numbers 217.651.5, 217.652.5, 243.027.6, 213.164.4, and UNESCO-ROSTSEA No. 243.170.6), and the National Institute for Environmental Studies, Japan. Authors thank Xysctus Tan and Ahmad Bin Awang for field assistance, CTFS for a grant to King for field expenses and Katherine McCulloh and Egbert Leigh Jr for helpful reviews of the article. NR 62 TC 30 Z9 30 U1 3 U2 28 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD APR PY 2009 VL 23 IS 2 BP 284 EP 291 DI 10.1111/j.1365-2435.2008.01514.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 418YH UT WOS:000264185500008 ER EF