FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Goddi, C
Greenhill, LJ
Humphreys, EML
Chandler, CJ
Matthews, LD
AF Goddi, C.
Greenhill, L. J.
Humphreys, E. M. L.
Chandler, C. J.
Matthews, L. D.
TI UNVEILING SOURCES OF HEATING IN THE VICINITY OF THE ORION BN/KL HOT CORE
AS TRACED BY HIGHLY EXCITED INVERSION TRANSITIONS OF AMMONIA
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: abundances; ISM: individual objects (Orion BN/KL); ISM: molecules
ID STAR-FORMING REGIONS; SOURCE I; SUBMILLIMETER ARRAY; L1157 OUTFLOW; BOW
SHOCKS; EMISSION; KL; RESOLUTION; EVOLUTION; NEBULA
AB Using the Expanded Very Large Array, we have mapped the vicinity of the Orion BN/KL Hot Core with subarcsecond angular resolution in seven metastable inversion transitions of ammonia (NH3): (J, K) = (6,6) to (12,12). This emission comes from levels up to 1500 K above the ground state, enabling identification of source(s) responsible for heating the region. We used this multi-transition data set to produce images of the rotational/kinetic temperature (T-rot/T-kin) and the column density N-col of NH3 for ortho and para species separately and on a position-by-position basis. We find T-rot and N-col in the range 160-490 K and (1-4) x 10(17) cm(-2), respectively. Our spatially resolved images show that the highest (column) density and hottest gas is found in a northeast-southwest elongated ridge to the southeast of Source I. We have also measured the ortho-para ratio of ammonia, estimated to vary in the range 0.9-1.6. Enhancement of ortho with respect to para and the offset of hot NH3 emission peaks from known (proto) stellar sources provide evidence that the NH3 molecules have been released from dust grains into the gas phase through the passage of shocks and not by stellar radiation. We propose that the combined effect of Source I's proper motion and its low-velocity outflow impinging on a pre-existing dense medium is responsible for the excitation of NH3 and the Orion Hot Core. Finally, we found for the first time evidence of a slow (similar to 5 km s(-1)) and compact (similar to 1000 AU) outflow toward IRc7.
C1 [Goddi, C.; Humphreys, E. M. L.] European So Observ, D-85748 Garching, Germany.
[Greenhill, L. J.; Humphreys, E. M. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chandler, C. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA.
RP Goddi, C (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.
EM cgoddi@eso.org
FU National Science Foundation [AST 0507478]
FX We thank Malcolm Walmsley and Steve Longmore for useful discussions, and
the anonymous referee for a constructive report. These data were
obtained under EVLA OSRO program 10B-225, and the work was supported by
the National Science Foundation (AST 0507478).
NR 35
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L13
DI 10.1088/2041-8205/739/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900013
ER
PT J
AU Kepley, AA
Chomiuk, L
Johnson, KE
Goss, WM
Balser, DS
Pisano, DJ
AF Kepley, Amanda A.
Chomiuk, Laura
Johnson, Kelsey E.
Goss, W. M.
Balser, Dana S.
Pisano, D. J.
TI UNVEILING EXTRAGALACTIC STAR FORMATION USING RADIO RECOMBINATION LINES:
AN EXPANDED VERY LARGE ARRAY PILOT STUDY WITH NGC 253
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: individual (NGC 253); galaxies: ISM; galaxies: star formation;
radio continuum: galaxies; radio lines: galaxies
ID H II REGIONS; STARBURST GALAXIES; VLA OBSERVATIONS; H92-ALPHA LINE;
IONIZED-GAS; NGC-253; H53-ALPHA; RESOLUTION; CLUSTERS; NUCLEUS
AB Radio recombination lines (RRLs) are powerful, extinction-free diagnostics of the ionized gas in young, star-forming regions. Unfortunately, these lines are difficult to detect in external galaxies. We present the results of Expanded Very Large Array (EVLA) observations of the RRL and radio continuum emission at 33 GHz from NGC 253, a nearby nuclear starburst galaxy. We detect the previously unobserved H58 alpha and H59 alpha RRLs and make simultaneous sensitive measurements of the continuum. We measure integrated line fluxes of 44.3 +/- 0.7 W m(-2) and 39.9 +/- 0.8 W m(-2) for the H58 alpha and H59 alpha lines, respectively. The thermal gas in NGC 253 is kinematically complex with multiple velocity components. We constrain the density of the thermal gas to (1.4-4) x 10(4) cm(-3) and estimate an ionizing photon flux of 1 x 10(53) s(-1). We use the RRL kinematics and the derived ionizing photon flux to show that the nuclear region of NGC 253 is not gravitationally bound, which is consistent with the outflow of gas inferred from the X-ray and H alpha measurements. The line profiles, fluxes, and kinematics of the H58 alpha and H59 alpha lines agree with those of RRLs at different frequencies confirming the accuracy of the previous, more difficult, high-frequency observations. We find that the EVLA is an order of magnitude more efficient for extragalactic RRL observations than the Very Large Array. These observations demonstrate both the power of the EVLA and the future potential of extragalactic RRL studies with the EVLA.
C1 [Kepley, Amanda A.; Johnson, Kelsey E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Chomiuk, Laura; Balser, Dana S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Pisano, D. J.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA.
[Chomiuk, Laura; Johnson, Kelsey E.; Pisano, D. J.] Natl Radio Astron Observ, Charlottesville, VA USA.
RP Kepley, AA (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA.
EM kepley@virginia.edu; lchomiuk@cfa.harvard.edu; kej7a@virginia.edu;
mgoss@nrao.edu; dbalser@nrao.edu; DJPisano@mail.wvu.edu
FU NSF [0548103]; David and Lucile Packard Foundation
FX The authors acknowledge the hard work and dedication of the EVLA
commissioning team. K.E.J. acknowledges support provided by NSF through
CAREER award 0548103 and the David and Lucile Packard Foundation through
a Packard Fellowship.
NR 35
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L24
DI 10.1088/2041-8205/739/1/L24
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900024
ER
PT J
AU Melis, C
Duchene, G
Chomiuk, L
Palmer, P
Perrin, MD
Maddison, ST
Menard, F
Stapelfeldt, K
Pinte, C
Duvert, G
AF Melis, Carl
Duchene, G.
Chomiuk, Laura
Palmer, Patrick
Perrin, M. D.
Maddison, S. T.
Menard, F.
Stapelfeldt, K.
Pinte, C.
Duvert, G.
TI MICROWAVE OBSERVATIONS OF EDGE-ON PROTOPLANETARY DISKS: PROGRAM OVERVIEW
AND FIRST RESULTS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; planets and
satellites: formation; protoplanetary disks; stars: individual (IRAS
04368+2557); stars: variables: T Tauri, Herbig Ae/Be
ID YOUNG STELLAR OBJECTS; T-TAURI STARS; CIRCUMSTELLAR DISKS; DUST
DISTRIBUTION; CORONET CLUSTER; IRAS 18059-3211; GRAIN-GROWTH; DARK
CLOUD; X-RAY; AURIGA
AB We are undertaking a multi-frequency Expanded Very Large Array (EVLA) survey of edge-on protoplanetary disks to probe the growth of solids in each disk, sedimentation of such material into the disk midplane, and the connection of these phenomena to the planet formation process. The projection of edge-on disk systems along our line of sight enables a study of the vertical stratification of large grains with fewer model dependencies than would be required for disks that are more face-on. Robust studies of the spatial distribution of grains up to approximate to 1 cm in size are possible with the wavelength range and sensitivity of the EVLA. In this contribution, we describe target selection and observational strategies. First results concerning the Class 0 source IRAS 04368+2557 (L1527 IRS) are presented, including a study of this source's 8.46 GHz continuum variability over short and long time baselines and an indication that its protoplanetary disk may have a dearth of pebble-sized grains.
C1 [Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
[Duchene, G.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Duchene, G.; Menard, F.; Pinte, C.; Duvert, G.] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG, UMR 5274, F-38041 Grenoble 9, France.
[Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Palmer, Patrick] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Perrin, M. D.] Space Telescope Sci Inst, Baltimore, MD 21231 USA.
[Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Stapelfeldt, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Melis, C (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92093 USA.
EM cmelis@ucsd.edu
RI Stapelfeldt, Karl/D-2721-2012
FU National Science Foundation (NSF) [AST-1003318, AST-0702933]; PNPS of
CNRS/INSU; ANR of France [ANR-07-BLAN-0221]; European Commission
[PIEF-GA-2008-220891]; ANR [ANR-2010-JCJC-0504-01]
FX We thank the anonymous referee for comments that helped improve this
work. C.M. acknowledges support from the National Science Foundation
under award No. AST-1003318. M.D.P. was supported by NSF Postdoctoral
Fellowship No. AST-0702933. F. M., C. P., and G. D. acknowledge PNPS of
CNRS/INSU, and ANR (contract ANR-07-BLAN-0221) of France for financial
support. C. P. acknowledges funding from the European Commission's 7th
Framework Program (contract PIEF-GA-2008-220891) and from ANR under
contract ANR-2010-JCJC-0504-01.
NR 50
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L7
DI 10.1088/2041-8205/739/1/L7
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900007
ER
PT J
AU Miller-Jones, JCA
Jonker, PG
Maccarone, TJ
Nelemans, G
Calvelo, DE
AF Miller-Jones, J. C. A.
Jonker, P. G.
Maccarone, T. J.
Nelemans, G.
Calvelo, D. E.
TI A DEEP RADIO SURVEY OF HARD STATE AND QUIESCENT BLACK HOLE X-RAY
BINARIES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; ISM: jets and outflows; radio continuum: stars;
X-rays: binaries
ID ADVECTION-DOMINATED ACCRETION; FUNDAMENTAL PLANE; LOW/HARD STATE;
OUTBURST DECAY; EVENT HORIZONS; XTE J1550-564; V404 CYG; CHANDRA;
TRANSIENTS; EMISSION
AB We have conducted a deep radio survey of a sample of black hole X-ray binaries in the hard and quiescent states to determine whether any systems were sufficiently bright for astrometric follow-up with high-sensitivity very long baseline interferometric arrays. The one hard-state system, Swift J1753.5-0127, was detected at a level of 0.5 mJy beam(-1). All 11 quiescent systems were not detected. In the three cases with the highest predicted quiescent radio brightnesses (GRO J0422+32, XTE J1118+480, and GRO J1655-40), the new capabilities of the Expanded Very Large Array were used to reach noise levels as low as 2.6 mu Jy beam (1). None of the three sources were detected to 3 sigma upper limits of 8.3, 7.8, and 14.2 mu Jy beam(-1), respectively. These observations represent the most stringent constraints to date on quiescent radio emission from black hole X-ray binaries. The uncertainties in the source distances, quiescent X-ray luminosities at the times of the observations, and the power-law index of the empirical correlation between radio and X-ray luminosities make it impossible to determine whether these three sources are significantly less luminous in the radio band than expected. Thus it is not clear whether that correlation holds all the way down to quiescence for all black hole X-ray binaries.
C1 [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
[Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Highfield SO17 IBJ, England.
[Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands.
[Calvelo, D. E.] Univ Southampton, Sch Phys & Astron, Highfield SO17 IBJ, England.
[Miller-Jones, J. C. A.] NRAO Headquarters, Charlottesville, VA 22903 USA.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Miller-Jones, JCA (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
EM james.miller-jones@curtin.edu.au
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
NR 44
TC 24
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U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L18
DI 10.1088/2041-8205/739/1/L18
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900018
ER
PT J
AU Pineda, JE
Goodman, AA
Arce, HG
Caselli, P
Longmore, S
Corder, S
AF Pineda, Jaime E.
Goodman, Alyssa A.
Arce, Hector G.
Caselli, Paola
Longmore, Steven
Corder, Stuartt
TI EXPANDED VERY LARGE ARRAY OBSERVATIONS OF THE BARNARD 5 STAR-FORMING
CORE: EMBEDDED FILAMENTS REVEALED
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE ISM: clouds; ISM: individual objects (B5, Perseus Molecular Complex);
ISM: molecules; stars: formation
ID DENSE CORES; INITIAL CONDITIONS; MAIN CLOUD; TRANSITION; COHERENCE;
OPHIUCHUS; NGC-2264; PERSEUS
AB We present similar to 6'.5 x 8' Expanded Very Large Array (EVLA) mosaic observations of the NH3 (1,1) emission in the Barnard 5 region in Perseus, with an angular resolution of 6 ''. This map covers the coherent region, where the dense gas presents subsonic non-thermal motions (as seen from single dish observations with the Green Bank Telescope, GBT). The combined EVLA and GBT observations reveal, for the first time, a striking filamentary structure (20 '' wide or 5000 AU at the distance of Perseus) in this low-mass star-forming region. The integrated intensity profile of this structure is consistent with models of an isothermal filament in hydrostatic equilibrium. The observed separation between the B5-IRS1 young stellar object (YSO), in the central region of the core, and the northern starless condensation matches the Jeans length of the dense gas. This suggests that the dense gas in the coherent region is fragmenting. The observed region displays a narrow velocity dispersion, where most of the gas shows evidence for subsonic turbulence and where little spatial variations are present. It is only close to the YSO where an increase in the velocity dispersion is found, but still displaying subsonic non-thermal motions.
C1 [Pineda, Jaime E.; Longmore, Steven] ESO, D-85748 Garching, Germany.
[Pineda, Jaime E.] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England.
[Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Corder, Stuartt] N Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA.
[Corder, Stuartt] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Pineda, JE (reprint author), ESO, Karl Schwarzschild St 2, D-85748 Garching, Germany.
EM jaime.pineda@manchester.ac.uk
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 [AST-0908159, AST-0845619]
FX We thank Alvaro Hacar for discussions regarding the properties of
filaments. The Expanded Very Large Array 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. This material is
based upon work supported by the National Science Foundation under Grant
AST-0908159 to AAG and AST-0845619 to HGA.
NR 23
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L2
DI 10.1088/2041-8205/739/1/L2
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900002
ER
PT J
AU Umana, G
Buemi, CS
Trigilio, C
Leto, P
Agliozzo, C
Ingallinera, A
Noriega-Crespo, A
Hora, JL
AF Umana, G.
Buemi, C. S.
Trigilio, C.
Leto, P.
Agliozzo, C.
Ingallinera, A.
Noriega-Crespo, A.
Hora, J. L.
TI EXPANDED VERY LARGE ARRAY OBSERVATIONS OF THE NEBULA AROUND G79.29+0.46
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: early-type; stars:
individual (G79.29+0.46); stars: winds, outflows
ID SPITZER-SPACE-TELESCOPE; INNER GALACTIC PLANE; CAMERA IRAC; CYGNUS-X;
MIPSGAL; STARS; SPECTROSCOPY; SUPERNOVAE
AB We have observed the radio nebula surrounding the Galactic luminous blue variable candidate G79.29+0.46 with the Expanded Very Large Array (EVLA) at 6 cm. These new radio observations allow a morphological comparison between the radio emission, which traces the ionized gas component, and the mid-IR emission, a tracer of the dust component. The InfraRed Array Camera (8 mu m) and the Multiband Imaging Photometer for Spitzer (24 mu m and 70 mu m) images have been reprocessed and compared with the EVLA map. We confirm the presence of a second shell at 24 mu m and also provide evidence for its detection at 70 mu m. The differences between the spatial morphology of the radio and mid-IR maps indicate the existence of two dust populations, the cooler one emitting mostly at longer wavelengths. Analysis of the two dusty, nested shells have provided us with an estimate of the characteristic timescales for shell ejection, providing important constraints for stellar evolutionary models. Finer details of the ionized gas distribution can be appreciated thanks to the improved quality of the new 6 cm image, most notably the highly structured texture of the nebula. Evidence of interaction between the nebula and the surrounding interstellar medium can be seen in the radio map, including brighter features that delineate regions where the shell structure is locally modified. In particular, the brighter filaments in the southwest region appear to frame the shocked southwestern clump reported from CO observations.
C1 [Umana, G.; Buemi, C. S.; Trigilio, C.; Leto, P.; Agliozzo, C.; Ingallinera, A.] INAF Osservatorio Astrofisico Catania, I-95123 Catania, Italy.
[Agliozzo, C.; Ingallinera, A.] Univ Catania, Dept Phys & Astron, I-95123 Catania, Italy.
[Noriega-Crespo, A.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Umana, G (reprint author), INAF Osservatorio Astrofisico Catania, I-95123 Catania, Italy.
EM Grazia.Umana@oact.inaf.it
OI Umana, Grazia/0000-0002-6972-8388; Buemi, Carla
Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Hora,
Joseph/0000-0002-5599-4650
FU NASA through JPL/Caltech
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 27
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U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 20
PY 2011
VL 739
IS 1
AR L11
DI 10.1088/2041-8205/739/1/L11
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818OQ
UT WOS:000294762900011
ER
PT J
AU Jones, FA
Erickson, DL
Bernal, MA
Bermingham, E
Kress, WJ
Herre, EA
Muller-Landau, HC
Turner, BL
AF Jones, F. Andrew
Erickson, David L.
Bernal, Moises A.
Bermingham, Eldredge
Kress, W. John
Herre, Edward Allen
Muller-Landau, Helene C.
Turner, Benjamin L.
TI The Roots of Diversity: Below Ground Species Richness and Rooting
Distributions in a Tropical Forest Revealed by DNA Barcodes and Inverse
Modeling
SO PLOS ONE
LA English
DT Article
ID SEED DISPERSAL; LAND PLANTS; DENSITY-DEPENDENCE; COEXISTENCE; PANAMA;
IDENTIFICATION; NEIGHBORHOOD; RECRUITMENT; COMMUNITY; ABUNDANCE
AB Background: Plants interact with each other, nutrients, and microbial communities in soils through extensive root networks. Understanding these below ground interactions has been difficult in natural systems, particularly those with high plant species diversity where morphological identification of fine roots is difficult. We combine DNA-based root identification with a DNA barcode database and above ground stem locations in a floristically diverse lowland tropical wet forest on Barro Colorado Island, Panama, where all trees and lianas >1 cm diameter have been mapped to investigate richness patterns below ground and model rooting distributions.
Methodology/Principal Findings: DNA barcode loci, particularly the cpDNA locus trnH-psba, can be used to identify fine and small coarse roots to species. We recovered 33 species of roots from 117 fragments sequenced from 12 soil cores. Despite limited sampling, we recovered a high proportion of the known species in the focal hectare, representing approximately 14% of the measured woody plant richness. This high value is emphasized by the fact that we would need to sample on average 13 m(2) at the seedling layer and 45 m(2) for woody plants >1 cm diameter to obtain the same number of species above ground. Results from inverse models parameterized with the locations and sizes of adults and the species identifications of roots and sampling locations indicates a high potential for distal underground interactions among plants.
Conclusions: DNA barcoding techniques coupled with modeling approaches should be broadly applicable to studying root distributions in any mapped vegetation plot. We discuss the implications of our results and outline how second-generation sequencing technology and environmental sampling can be combined to increase our understanding of how root distributions influence the potential for plant interactions in natural ecosystems.
C1 [Jones, F. Andrew; Bernal, Moises A.; Bermingham, Eldredge; Herre, Edward Allen; Muller-Landau, Helene C.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Bernal, Moises A.] Univ Texas Austin, Dept Marine Sci, Inst Marine Sci, Port Aransas, TX USA.
RP Jones, FA (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Biol, Silwood Pk, Ascot SL5 7PY, Berks, England.
EM f.jones@imperial.ac.uk
RI Turner, Benjamin/E-5940-2011; Bernal , Moises /D-9006-2012; Bernal,
Moises /B-9490-2013
OI Turner, Benjamin/0000-0002-6585-0722;
FU Tupper postdoctoral fellowship in tropical biology; National Science
Foundation [DEB 0453665]; Smithsonian Institution Global Earth
Observatory; Smithsonian Tropical Research Institute/Center for Tropical
Forest Sciences; Smithsonian Tropical Research Institute
FX FAJ acknowledges the support of a Tupper postdoctoral fellowship in
tropical biology and the National Science Foundation (DEB 0453665).
Funding was provided by the Smithsonian Institution Global Earth
Observatory, the Smithsonian Tropical Research Institute/Center for
Tropical Forest Sciences endowment fund, and the Smithsonian Tropical
Research Institute/Frank Levinson fund. We would like to thank Autoridad
Nacional del Ambiente and the Smithsonian Tropical Research Institute
for processing research permits. We thank S. Hubbell and R. Condit for
access to plot data, S. Schnitzer for liana census data (NSF DEB
0613666), and L. Comita and S. Hubbell for access to seedling data (NSF
DEB 0075102 and DEB 0823728). The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 56
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U1 4
U2 70
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD SEP 19
PY 2011
VL 6
IS 9
AR e24506
DI 10.1371/journal.pone.0024506
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825FZ
UT WOS:000295257900019
PM 21949723
ER
PT J
AU Wallace, LE
Culley, TM
Weller, SG
Sakai, AK
Kuenzi, A
Roy, T
Wagner, WL
Nepokroeff, M
AF Wallace, Lisa E.
Culley, Theresa M.
Weller, Stephen G.
Sakai, Ann K.
Kuenzi, Ashley
Roy, Tilottama
Wagner, Warren L.
Nepokroeff, Molly
TI Asymmetrical Gene Flow in a Hybrid Zone of Hawaiian Schiedea
(Caryophyllaceae) Species with Contrasting Mating Systems
SO PLOS ONE
LA English
DT Article
ID ADAPTIVE RADIATION; SALICARIA CARYOPHYLLACEAE; INBREEDING DEPRESSION;
PHYLOGENETIC ANALYSIS; SILVERSWORD ALLIANCE; WIND POLLINATION;
INTERSPECIFIC HYBRIDIZATION; NATURAL-POPULATIONS; GYNODIOECIOUS PLANT;
MITOCHONDRIAL-DNA
AB Asymmetrical gene flow, which has frequently been documented in naturally occurring hybrid zones, can result from various genetic and demographic factors. Understanding these factors is important for determining the ecological conditions that permitted hybridization and the evolutionary potential inherent in hybrids. Here, we characterized morphological, nuclear, and chloroplast variation in a putative hybrid zone between Schiedea menziesii and S. salicaria, endemic Hawaiian species with contrasting breeding systems. Schiedea menziesii is hermaphroditic with moderate selfing; S. salicaria is gynodioecious and wind-pollinated, with partially selfing hermaphrodites and largely outcrossed females. We tested three hypotheses: 1) putative hybrids were derived from natural crosses between S. menziesii and S. salicaria, 2) gene flow via pollen is unidirectional from S. salicaria to S. menziesii and 3) in the hybrid zone, traits associated with wind pollination would be favored as a result of pollen-swamping by S. salicaria. Schiedea menziesii and S. salicaria have distinct morphologies and chloroplast genomes but are less differentiated at the nuclear loci. Hybrids are most similar to S. menziesii at chloroplast loci, exhibit nuclear allele frequencies in common with both parental species, and resemble S. salicaria in pollen production and pollen size, traits important to wind pollination. Additionally, unlike S. menziesii, the hybrid zone contains many females, suggesting that the nuclear gene responsible for male sterility in S. salicaria has been transferred to hybrid plants. Continued selection of nuclear genes in the hybrid zone may result in a population that resembles S. salicaria, but retains chloroplast lineage(s) of S. menziesii.
C1 [Wallace, Lisa E.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA.
[Culley, Theresa M.; Kuenzi, Ashley] Univ Cincinnati, Dept Biol Sci, Cincinnati, OH 45221 USA.
[Weller, Stephen G.; Sakai, Ann K.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92717 USA.
[Roy, Tilottama] SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA.
[Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20560 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 NSF [DEB-0445410, DEB-9207724]; National Tropical Botanical Garden
FX The authors acknowledge support from NSF grants DEB-0445410 to MN and LW
and DEB-9207724 to AKS and SGW as well as the McBryde endowment of
National Tropical Botanical Garden to MN and WLW. The funders had no
role in study design, data collection and analysis, decision to publish,
or preparation of the manuscript.
NR 84
TC 9
Z9 9
U1 0
U2 17
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 SEP 19
PY 2011
VL 6
IS 9
AR e24845
DI 10.1371/journal.pone.0024845
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825FZ
UT WOS:000295257900030
PM 21949765
ER
PT J
AU Nowlan, CR
Liu, X
Chance, K
Cai, Z
Kurosu, TP
Lee, C
Martin, RV
AF Nowlan, C. R.
Liu, X.
Chance, K.
Cai, Z.
Kurosu, T. P.
Lee, C.
Martin, R. V.
TI Retrievals of sulfur dioxide from the Global Ozone Monitoring Experiment
2 (GOME-2) using an optimal estimation approach: Algorithm and initial
validation
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID ROTATIONAL RAMAN-SCATTERING; ABSORPTION CROSS-SECTIONS;
TEMPERATURE-DEPENDENCE; SATELLITE-OBSERVATIONS; PROFILE RETRIEVALS;
WAVELENGTH RANGE; VOLCANIC SO2; 000 CM(-1); NM REGION; INSTRUMENT
AB We apply an optimal estimation algorithm originally developed for retrieving ozone profiles from the Global Ozone Monitoring Experiment (GOME) and the Ozone Monitoring Instrument (OMI) to make global observations of sulfur dioxide from the Global Ozone Monitoring Experiment 2 (GOME-2) on the MetOp-A satellite. Our approach combines a full radiative transfer calculation, retrieval algorithm, and trace gas climatologies to implicitly include the effects of albedo, clouds, ozone, and SO2 profiles in the retrieval. Under volcanic conditions, the algorithm may also be used to directly retrieve SO2 plume altitude. Retrieved SO2 columns over heavy anthropogenic pollution typically agree with those calculated using a two-step slant column and air mass factor approach to within 10%. Retrieval uncertainties are quantified for GOME-2 SO2 amounts; these are dominated by uncertainty contributions from noise, surface albedo, profile shape, correlations with other retrieved parameters, atmospheric temperature, choice of wavelength fitting window, and aerosols. When plume altitudes are also simultaneously retrieved, additional significant uncertainties result from uncertainties in the a priori altitude, the model's vertical layer resolution, and instrument calibration. Retrieved plume height information content is examined using the Mount Kasatochi volcanic plume on 9 August 2008. An a priori altitude of 10 km and uncertainty of 2 km produce degrees of freedom for signal of at least 0.9 for columns >30 Dobson units. GOME-2 estimates of surface SO2 are compared with in situ annual means over North America in 2008 from the Clear Air Status and Trends Network (CASTNET; r = 0.85, N = 65) and Air Quality System (AQS) and National Air Pollution Surveillance (NAPS; r = 0.40, N = 438) networks.
C1 [Nowlan, C. R.; Liu, X.; Chance, K.; Kurosu, T. P.; Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Cai, Z.] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China.
[Lee, C.] Korea Meteorol Adm, Natl Inst Meteorol Res, Seoul 156720, South Korea.
[Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
RP Nowlan, CR (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St,MS-50, Cambridge, MA 02138 USA.
EM cnowlan@cfa.harvard.edu
RI Martin, Randall/C-1205-2014; 杨, 宇栋/F-6250-2012; Liu, Xiong/P-7186-2014;
OI Martin, Randall/0000-0003-2632-8402; Liu, Xiong/0000-0003-2939-574X;
Nowlan, Caroline/0000-0002-8718-9752; Chance, Kelly/0000-0002-7339-7577
FU NASA; Smithsonian Institution; NIMR/KMA
FX The authors wish to thank the GOME-2 team at EUMETSAT for helpful
discussions and data access, and the European Space Agency for their
ongoing cooperation in the GOME program. CASTNET and AQS data are
provided by the EPA. NAPS data are provided by the Analysis and Air
Quality Division of Environment Canada. Research at the Smithsonian
Astrophysical Observatory was funded by NASA and the Smithsonian
Institution. This work was also partially supported by the NIMR/KMA
project 'Development of meteorological resources for green growth'.
NR 62
TC 27
Z9 27
U1 2
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD SEP 16
PY 2011
VL 116
AR D18301
DI 10.1029/2011JD015808
PG 20
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 823OJ
UT WOS:000295131500002
ER
PT J
AU Doyle, LR
Carter, JA
Fabrycky, DC
Slawson, RW
Howell, SB
Winn, JN
Orosz, JA
Prsa, A
Welsh, WF
Quinn, SN
Latham, D
Torres, G
Buchhave, LA
Marcy, GW
Fortney, JJ
Shporer, A
Ford, EB
Lissauer, JJ
Ragozzine, D
Rucker, M
Batalha, N
Jenkins, JM
Borucki, WJ
Koch, D
Middour, CK
Hall, JR
McCauliff, S
Fanelli, MN
Quintana, EV
Holman, MJ
Caldwell, DA
Still, M
Stefanik, RP
Brown, WR
Esquerdo, GA
Tang, SM
Furesz, G
Geary, JC
Berlind, P
Calkins, ML
Short, DR
Steffen, JH
Sasselov, D
Dunham, EW
Cochran, WD
Boss, A
Haas, MR
Buzasi, D
Fischer, D
AF Doyle, Laurance R.
Carter, Joshua A.
Fabrycky, Daniel C.
Slawson, Robert W.
Howell, Steve B.
Winn, Joshua N.
Orosz, Jerome A.
Prsa, Andrej
Welsh, William F.
Quinn, Samuel N.
Latham, David
Torres, Guillermo
Buchhave, Lars A.
Marcy, Geoffrey W.
Fortney, Jonathan J.
Shporer, Avi
Ford, Eric B.
Lissauer, Jack J.
Ragozzine, Darin
Rucker, Michael
Batalha, Natalie
Jenkins, Jon M.
Borucki, William J.
Koch, David
Middour, Christopher K.
Hall, Jennifer R.
McCauliff, Sean
Fanelli, Michael N.
Quintana, Elisa V.
Holman, Matthew J.
Caldwell, Douglas A.
Still, Martin
Stefanik, Robert P.
Brown, Warren R.
Esquerdo, Gilbert A.
Tang, Sumin
Furesz, Gabor
Geary, John C.
Berlind, Perry
Calkins, Michael L.
Short, Donald R.
Steffen, Jason H.
Sasselov, Dimitar
Dunham, Edward W.
Cochran, William D.
Boss, Alan
Haas, Michael R.
Buzasi, Derek
Fischer, Debra
TI Kepler-16: A Transiting Circumbinary Planet
SO SCIENCE
LA English
DT Article
ID CM DRACONIS; BINARY-SYSTEMS; GIANT PLANETS; STARS; PERFORMANCE;
ALGORITHM; SCIENCE; RADII; MASS
AB We report the detection of a planet whose orbit surrounds a pair of low-mass stars. Data from the Kepler spacecraft reveal transits of the planet across both stars, in addition to the mutual eclipses of the stars, giving precise constraints on the absolute dimensions of all three bodies. The planet is comparable to Saturn in mass and size and is on a nearly circular 229-day orbit around its two parent stars. The eclipsing stars are 20 and 69% as massive as the Sun and have an eccentric 41-day orbit. The motions of all three bodies are confined to within 0.5 degrees of a single plane, suggesting that the planet formed within a circumbinary disk.
C1 [Doyle, Laurance R.; Slawson, Robert W.; Jenkins, Jon M.; Quintana, Elisa V.; Caldwell, Douglas A.] SETI Inst, Carl Sagan Ctr Study Life Universe, Mountain View, CA 94043 USA.
[Carter, Joshua A.; Quinn, Samuel N.; Latham, David; Torres, Guillermo; Ragozzine, Darin; Holman, Matthew J.; Stefanik, Robert P.; Brown, Warren R.; Esquerdo, Gilbert A.; Tang, Sumin; Furesz, Gabor; Geary, John C.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Middour, Christopher K.; Hall, Jennifer R.; McCauliff, Sean] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
[Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Orosz, Jerome A.; Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA.
[Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Furesz, Gabor] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark.
[Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Shporer, Avi] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Ford, Eric B.] 211 Bryant Space Sci Ctr, Gainesville, FL 32611 USA.
[Rucker, Michael; Batalha, Natalie] San Jose State Univ, Dept Phys, San Jose, CA 95192 USA.
[Fanelli, Michael N.; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA.
[Buchhave, Lars A.] Konkoly Observ Budapest, H-1121 Budapest, Hungary.
[Berlind, Perry; Calkins, Michael L.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Short, Donald R.] San Diego State Univ, Dept Math, San Diego, CA 92182 USA.
[Steffen, Jason H.] FermiLab Ctr Particle Astrophys, Batavia, IL 60510 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA.
[Buzasi, Derek] Eureka Sci, Oakland, CA 94602 USA.
[Fischer, Debra] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
RP Doyle, LR (reprint author), SETI Inst, Carl Sagan Ctr Study Life Universe, 189 Bernardo Ave, Mountain View, CA 94043 USA.
EM ldoyle@seti.org
RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Ragozzine,
Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014;
OI Caldwell, Douglas/0000-0003-1963-9616; Fortney,
Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666;
Fabrycky, Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; NASA [NNX08AR15G, HF-51267.01-A,
HF-51272.01-A, NAS 5-26555, NNX09AB33G]; Space Telescope Science
Institute
FX NASA's Science Mission Directorate provided funding for the Kepler
Discovery mission. L. R. D. acknowledges the NASA Kepler Participating
Scientist Program (grant no. NNX08AR15G) and helpful discussions with
the Kepler Science Team. J.A.C. and D. C. F. acknowledge support for
this work provided by NASA through Hubble Fellowship grants
HF-51267.01-A and HF-51272.01-A awarded by the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy for NASA, under contract NAS 5-26555. J.N.W. is
grateful for support from the NASA Origins program (grant NNX09AB33G).
The Kepler data used in this analysis can be downloaded from
http://archive.stsci.edu/prepds/kepler_hlsp.
NR 29
TC 285
Z9 286
U1 0
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 SEP 16
PY 2011
VL 333
IS 6049
BP 1602
EP 1606
DI 10.1126/science.1210923
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 820JE
UT WOS:000294900900035
PM 21921192
ER
PT J
AU Knornschild, M
Ueberschaer, K
Helbig, M
Kalko, EKV
AF Knoernschild, Mirjam
Ueberschaer, Katja
Helbig, Maria
Kalko, Elisabeth K. V.
TI Sexually Selected Infanticide in a Polygynous Bat
SO PLOS ONE
LA English
DT Article
ID LANGURS PRESBYTIS-ENTELLUS; ACTIVE TERMITE NESTS; ROUND-EARED BAT;
LOPHOSTOMA-SILVICOLUM; FOOD-DEPRIVATION; RED DEER; ROOST;
PHYLLOSTOMIDAE; BEHAVIOR; STRATEGIES
AB Background: Adult individuals of many species kill unrelated conspecific infants for several adaptive reasons ranging from predation or resource competition to the prevention of misdirected parental care. Moreover, infanticide can increase the reproductive success of the aggressor by killing the offspring of competitors and thereafter mating with the victimized females. This sexually selected infanticide predominantly occurs in polygynous species, with convincing evidence for primates, carnivores, equids, and rodents. Evidence for bats was predicted but lacking.
Methodology/Principal Findings: Here we report the first case, to our knowledge, of sexually selected infanticide in a bat, the polygynous white-throated round-eared bat, Lophostoma silvicolum. Behavioral studies in a free-living population revealed that an adult male repeatedly attacked and injured the pups of two females belonging to his harem, ultimately causing the death of one pup. The infanticidal male subsequently mated with the mother of the victimized pup and this copulation occurred earlier than any other in his harem.
Conclusions/Significance: Our findings indicate that sexually selected infanticide is more widespread than previously thought, adding bats as a new taxon performing this strategy. Future work on other bats, especially polygynous species in the tropics, has great potential to investigate the selective pressures influencing the evolution of sexually selected infanticide and to study how infanticide impacts reproductive strategies and social structures of different species.
C1 [Knoernschild, Mirjam; Ueberschaer, Katja; Helbig, Maria; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany.
[Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Knornschild, M (reprint author), Univ Ulm, Inst Expt Ecol, Ulm, Germany.
EM mirjam.knoernschild@uni-ulm.de
RI Knornschild, Mirjam/C-9401-2011
FU National Museum of Natural History, Washington, DC; Smithsonian Tropical
Research Institution
FX The National Museum of Natural History, Washington, DC, and the
Smithsonian Tropical Research Institution funded this study. The funders
had no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 73
TC 0
Z9 0
U1 4
U2 23
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD SEP 16
PY 2011
VL 6
IS 9
AR e25001
DI 10.1371/journal.pone.0025001
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 824BI
UT WOS:000295173800056
PM 21949829
ER
PT J
AU Poorani, J
Vandenberg, NJ
Booth, RG
AF Poorani, J.
Vandenberg, Natalia J.
Booth, R. G.
TI A revision of the genus Stictobura Crotch and description of a new
species of Sticholotis Crotch (Coleoptera: Coccinellidae:
Sticholotidinae)
SO ZOOTAXA
LA English
DT Article
DE Stictobura; Sticholotis; Coccinellidae; Sticholotidinae; revision; new
synonym; new combination; new species
AB The species of Stictobura Crotch (1874) (Coccinellidae: Sticholotidinae) are revised. Stictobura gibbula (Weise, 1908) indeed belongs to Sticholotis Crotch (1874) under which it was originally described (stat. rev.) and is removed from Stictobura. Stictobura buruensis Korschefsky (1944) is transferred to Sticholotis (new combination). Lectotypes are designated for Sticholotis (Apterolotis) andrewesi Weise (1908), Sticholotis (Apterolotis) gibbula Weise (1908), Stictobura semipolita Sicard (1911), and Stictobura rubroguttata Sicard (1925). The species of Stictobura are keyed and notes on biology are provided wherever available. Sticholotis magnostriata sp. n., which is externally similar to the species of Stictobura, is described from India (Assam).
C1 [Poorani, J.] Natl Bur Agr Important Insects, Bangalore 560024, Karnataka, India.
[Vandenberg, Natalia J.] ARS, SEL, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Booth, R. G.] Nat Hist Museum, Dept Entomol, London SW7 5BD, England.
RP Poorani, J (reprint author), Natl Bur Agr Important Insects, PB 2491,HA Farm Post,Bellary Rd, Bangalore 560024, Karnataka, India.
EM pooranij@gmail.com; Natalia.Vandenberg@ars.usda.gov; r.booth@nhm.ac.uk
NR 23
TC 0
Z9 0
U1 1
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 SEP 16
PY 2011
IS 3031
BP 1
EP 13
PG 13
WC Zoology
SC Zoology
GA 820EZ
UT WOS:000294889700001
ER
PT J
AU Serrano, L
Ferrari, L
Martinez, ML
Petrone, CM
Jaramillo, C
AF Serrano, Lina
Ferrari, Luca
Lopez Martinez, Margarita
Maria Petrone, Chiara
Jaramillo, Carlos
TI An integrative geologic, geochronologic and geochemical study of Gorgona
Island, Colombia: Implications for the formation of the Caribbean Large
Igneous Province
SO EARTH AND PLANETARY SCIENCE LETTERS
LA English
DT Article
DE Gorgona Island; Caribbean Large Igneous Province; geochronology;
Galapagos hotspot; slab window
ID MANTLE REFERENCE FRAME; GULF-OF-MEXICO; OCEANIC PLATEAU; MELTING
EXPERIMENTS; TECTONIC EVOLUTION; TERRANE ACCRETION; SOUTH-AMERICA;
FORE-ARC; HETEROGENEITY; CONSTRAINTS
AB The genesis of the Caribbean Large Igneous Province (CLIP) has been associated to the melting of the Galapagos plume head at similar to 90 Ma or to the interaction between the plume and the Caribbean slab window. Gorgona Island, offshore western Colombia, is an accreted fragment of the CLIP and its highly heterogeneous igneous suite, ranging from enriched basalts to depleted komatiites and picrites, was assumed to have formed at similar to 89 Ma from different part of the plume. Here we present new geologic. geochronologic and geochemical data of Gorgona with significant implications for the formation of the CLIP. A new set of Ar-40-Ar-39 ages documents a magmatic activity spanning the whole Late Cretaceous (98.7 +/- 7.7 to 64.4 +/- 5 Ma) followed by a shallower, picritic pyroclastic eruption in the Paleocene. Trace element and isotope geochemistry confirm the existence of an enriched (EDMM: La/Sm-N >= and epsilon Nd-i of 5.7 to 7.8) and a depleted (DMM: La/Sm-N<1 and epsilon Nd-i of 9.5 to 11.3) mantle sources. A progressive increase in the degree of melting and melt extraction with time occurred in both groups. Petrologic modeling indicates that low but variable degrees of wet melting (<5%) of an EDMM can produce the LREE-enriched rocks. Higher degree of melting (>10%) of a mixed DMM + EDMM (40 to 60%) may reproduce the more depleted rocks with temperatures in the range of ambient mantle in absence of plumes. Our results contradict the notion that the CLIP formed by melting of a plume head at similar to 90 Ma. Multiple magmatic pulses over several tens of Ma in small areas like Gorgona, also recognized in other CUP areas, suggest a long period of diffuse magmatism without a clear pattern of migration. The age span of this magmatism is broadly concurrent with the Caribbean slab window. During this time span the Farallon oceanic lithosphere (later becoming the Caribbean plate) advanced eastward similar to 1500 km, overriding the astenosphere feeding the proto-Caribbean spreading ridge. This hotter mantle flowed westward into, and mixed with, the opening mantle wedge, promoting increasing melting with time. The fortuitous occurrence of a plume passing through the slab gap area cannot be excluded but not required to produce the observed composition and degree of melting. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Serrano, Lina; Ferrari, Luca] Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76230, Qro, Mexico.
[Lopez Martinez, Margarita] Ctr Invest Cient & Educ Super Ensenada, Lab Geocronol, Ensenada 22860, Baja California, Mexico.
[Maria Petrone, Chiara] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England.
[Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Ferrari, L (reprint author), Univ Nacl Autonoma Mexico, Ctr Geociencias, Campus Juriquilla,Blvd Juriquilla 3001, Queretaro 76230, Qro, Mexico.
EM linaserranod@hotmail.com; luca@geociencias.unam.mx; marlopez@cicese.mx;
cmp57@cam.ac.uk; jaramilloC@si.edu
RI Ferrari, Luca/G-2659-2013; Petrone, Chiara Maria/B-6103-2015
OI Ferrari, Luca/0000-0002-4847-6337; Petrone, Chiara
Maria/0000-0002-4492-9183
FU UNAM-PAPIIT [IN114508]; CICESE Geochronology Laboratory; Instituto
Panamericano de Geografia e Historia
FX The research was funded by grant UNAM-PAPIIT IN114508 (to IF) and by the
CICESE Geochronology Laboratory (MLM). LSD was supported by a M.Sc.
scholarship from Instituto Panamericano de Geografia e Historia. V.
Kamenetsky, EPSL editor R. Carlson and an anonymous reviewer provided
important criticism and suggestions that greatly improve the final
manuscript. We thank J. Pindell for useful discussions and the review of
an earlier version of the manuscript. We also thank M. A. Garcia and A.
S. Rosas for assistence with the 40Ar-39Ar
experiments, A. Gomez-Tuena and O. Perez for supervising ICP-MS
geochemistry, S. Tommasini and E. Braschi for help in measuring Sr and
Nd isotopes. G. Serrano, P. de Greiff, R. Lopez and the Gorgona Natural
Park guides are greatly acknowledged for their assistance during the
fieldwork. We acknowledge Parques Nacionales Naturales de Colombia for
granting the access to Gorgona island and collecting samples between
2006 and 2009.
NR 71
TC 12
Z9 12
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 SEP 15
PY 2011
VL 309
IS 3-4
BP 324
EP 336
DI 10.1016/j.epsl.2011.07.011
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 831CZ
UT WOS:000295707600015
ER
PT J
AU Hong, T
AF Hong, Terry
TI 1Q84
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA.
RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 3
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 SEP 15
PY 2011
VL 136
IS 15
BP 69
EP 69
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 821LP
UT WOS:000294976800077
ER
PT J
AU Riley, S
AF Riley, Sheila
TI It's Classified
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 SEP 15
PY 2011
VL 136
IS 15
BP 73
EP 73
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 821LP
UT WOS:000294976800096
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI A More Perfect Heaven: How Copernicus Revolutionized the Cosmos
SO NATURE
LA English
DT Book Review
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ginger@cfa.harvard.edu
NR 1
TC 0
Z9 0
U1 1
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 15
PY 2011
VL 477
IS 7364
BP 276
EP 277
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 819TD
UT WOS:000294852400012
ER
PT J
AU Gharaibeh, MF
Bizau, JM
Cubaynes, D
Guilbaud, S
El Hassan, N
Al Shorman, MM
Miron, C
Nicolas, C
Robert, E
Blancard, C
McLaughlin, BM
AF Gharaibeh, M. F.
Bizau, J. M.
Cubaynes, D.
Guilbaud, S.
El Hassan, N.
Al Shorman, M. M.
Miron, C.
Nicolas, C.
Robert, E.
Blancard, C.
McLaughlin, B. M.
TI K-shell photoionization of singly ionized atomic nitrogen: experiment
and theory
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID ELECTRON-IMPACT; CROSS-SECTIONS; RESONANCES; IONS; PHOTOABSORPTION;
SPECTROSCOPY; TRANSITIONS; IONIZATION; ENERGIES; EMISSION
AB Absolute cross sections for the K-shell photoionization of C-like nitrogen ions were measured by employing the ion-photon merged-beam technique at the SOLEIL synchrotron radiation facility in Saint-Aubin, France. High-resolution spectroscopy with E/Delta E approximate to 7000 was achieved with the photon energy from 388 to 430 eV scanned with a band pass of 300 meV, and the 399.4-402 eV range with 60 meV. Experimental results are compared with theoretical predictions made from the multi-configuration Dirac-Fock and R-matrix methods. The interplay between experiment and theory enabled the identification and characterization of the strong 1s -> 2p resonances observed in the spectra.
C1 [Gharaibeh, M. F.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan.
[Bizau, J. M.; Cubaynes, D.; Guilbaud, S.; El Hassan, N.; Al Shorman, M. M.] Univ Paris 11, CNRS, ISMO, UMR 8214, F-91405 Orsay, France.
[Bizau, J. M.; Cubaynes, D.; Miron, C.; Nicolas, C.; Robert, E.] Synchrotron SOLEIL, F-91192 Gif Sur Yvette, France.
[Blancard, C.] CEA DAM DIF, F-91297 Arpajon, France.
[McLaughlin, B. M.] Queens Univ Belfast, CTAMOP, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Gharaibeh, MF (reprint author), Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan.
EM mfg@just.edu.jo; b.mclaughlin@qub.ac.uk
OI MIRON, Catalin/0000-0002-8302-7158
FU Triangle de le Physique [2007-001T]; US National Science Foundation
FX Data collection was performed on the PLEIADES beam line, at the SOLEIL
Synchrotron Radiation Facility in Saint-Aubin, France. The authors would
like to thank the staff of SOLEIL and, in particular, the staff of the
PLEIADES beam line for their helpful assistance. The experimental
research work described here has been supported by Triangle de le
Physique contract 2007-001T. BMM acknowledges support by the US National
Science Foundation through a grant to ITAMP at the Harvard-Smithsonian
Center for Astrophysics. The computational work was carried out at the
National Energy Research Scientific Computing Center in Oakland, CA,
USA, and on the Tera-grid at the National Institute for Computational
Sciences (NICS) in Knoxville, TN, USA, which is supported in part by the
US National Science Foundation.
NR 44
TC 29
Z9 29
U1 0
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 14
PY 2011
VL 44
IS 17
AR 175208
DI 10.1088/0953-4075/44/17/175208
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 820FR
UT WOS:000294891500016
ER
PT J
AU McLaughlin, BM
Lee, TG
Ludlow, JA
Landi, E
Loch, SD
Pindzola, MS
Ballance, CP
AF McLaughlin, B. M.
Lee, Teck-Ghee
Ludlow, J. A.
Landi, E.
Loch, S. D.
Pindzola, M. S.
Ballance, C. P.
TI A large-scale R-matrix calculation for electron-impact excitation of the
Ne2+, O-like ion
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Article
ID CROSS-SECTIONS; TRANSITION-PROBABILITIES; COLLISIONAL EXCITATION;
FORBIDDEN LINES; ENERGY-LEVELS; ORION NEBULA; NEIII; STRENGTHS; PROGRAM;
NEON
AB The five J Pi levels within an np(2) or np(4) ground-state complex provide an excellent testing ground for the comparison of theoretical line ratios with astrophysically observed values, in addition to providing valuable electron temperature and density diagnostics. The low-temperature nature of the line ratios ensures that the theoretically derived values are sensitive to the underlying atomic structure and electron-impact excitation rates. Previous R-matrix calculations for the O-like Ne ion, Ne2+, exhibit spurious structure in the cross sections at higher electron energies, which may affect Maxwellian averaged rates even at low temperatures. Furthermore, there is an absence of comprehensive excitation data between the excited states that may provide newer diagnostics to complement the more established lines discussed in this paper. To resolve these issues, we present both a small-scale 56-level Breit-Pauli calculation and a large-scale 554-level R-matrix intermediate coupling frame transformation calculation that extends the scope and validity of earlier JAJOM calculations both in terms of the atomic structure and scattering cross sections. Our results provide a comprehensive electron-impact excitation data set for all transitions to higher n-shells. The fundamental atomic data for this O-like ion are subsequently used within a collisional radiative framework to provide the intensity line ratios across a range of electron temperatures and densities of interest in astrophysical observations.
C1 [McLaughlin, B. M.] Queens Univ Belfast, CTAMOP, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Lee, Teck-Ghee; Ludlow, J. A.; Loch, S. D.; Pindzola, M. S.; Ballance, C. P.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA.
[Landi, E.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA.
RP McLaughlin, BM (reprint author), Queens Univ Belfast, CTAMOP, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland.
EM b.mclaughlin@qub.ac.uk; ballance@physics.auburn.edu
RI Landi, Enrico/H-4493-2011; Lee, Teck Ghee/D-5037-2012
OI Lee, Teck Ghee/0000-0001-9472-3194
FU US Department of Energy (DoE) through Auburn University; NASA
[NNX10AM17G, NNX11AC20G]; US National Science Foundation
FX It is a pleasure to thank Professor A Dalgarno FRS for drawing our
attention to this problem and the need for accurate atomic data required
for the modelling of planetary nebulae. T-GL, CPB and JAL were supported
by US Department of Energy (DoE) grants through Auburn University. EL
acknowledges support from NASA grants NNX10AM17G and NNX11AC20G. BMM
acknowledges support by the US National Science Foundation through a
grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. The
computational work was carried out at the National Energy Research
Scientific Computing Center in Oakland, CA, USA, and on the Tera-grid at
the National Institute for Computational Sciences (NICS) in Knoxville,
TN, USA, which is supported in part by the US National Science
Foundation.
NR 34
TC 5
Z9 5
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 14
PY 2011
VL 44
IS 17
AR 175206
DI 10.1088/0953-4075/44/17/175206
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 820FR
UT WOS:000294891500014
ER
PT J
AU Rittenhouse, ST
von Stecher, J
D'Incao, JP
Mehta, NP
Greene, CH
AF Rittenhouse, S. T.
von Stecher, J.
D'Incao, J. P.
Mehta, N. P.
Greene, C. H.
TI The hyperspherical four-fermion problem
SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS
LA English
DT Review
ID STOCHASTIC VARIATIONAL METHOD; TRIPLY EXCITED-STATES; CORRELATED FERMI
GAS; QUANTUM REACTIVE SCATTERING; GENERAL-ORDER COLLISIONS; FEW-BODY
PROBLEMS; ELECTRON CORRELATIONS; ENERGY-LEVELS; INTERACTING PARTICLES;
3-BODY COLLISIONS
AB The problem of a few interacting fermions in quantum physics has sparked intense interest, particularly in recent years owing to connections with the behaviour of superconductors, fermionic superfluids and finite nuclei. This review addresses recent developments in the theoretical description of four fermions having finite-range interactions, stressing insights that have emerged from a hyperspherical coordinate perspective. The subject is complicated, so we have included many detailed formulae that will hopefully make these methods accessible to others interested in using them. The universality regime, where the dominant length scale in the problem is the two-body scattering length, is particularly stressed, including its implications for the famous BCS-BEC crossover problem. Derivations and relevant formulae are also included for the calculation of challenging few-body processes such as recombination.
C1 [Rittenhouse, S. T.; von Stecher, J.; D'Incao, J. P.; Mehta, N. P.; Greene, C. H.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Rittenhouse, S. T.; von Stecher, J.; D'Incao, J. P.; Mehta, N. P.; Greene, C. H.] Univ Colorado, JILA, Boulder, CO 80309 USA.
[Rittenhouse, S. T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Mehta, N. P.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
RP Rittenhouse, ST (reprint author), Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
EM chris.greene@colorado.edu
RI Greene, Chris/C-3821-2011
OI Greene, Chris/0000-0002-2096-6385
FU NSF
FX Many of the results described in this review were developed in close
collaboration with Doerte Blume, and we deeply appreciate her
contributions and insights. In particular, we thank D Blume and K M
Daily for providing the results presented in figure 27. We also thank
Brett Esry for numerous informative discussions and for access to some
of his results prior to publication. This project was supported by the
NSF.
NR 144
TC 18
Z9 18
U1 1
U2 32
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0953-4075
J9 J PHYS B-AT MOL OPT
JI J. Phys. B-At. Mol. Opt. Phys.
PD SEP 14
PY 2011
VL 44
IS 17
AR 172001
DI 10.1088/0953-4075/44/17/172001
PG 43
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 820FR
UT WOS:000294891500001
ER
PT J
AU Redmond, NE
Raleigh, J
van Soest, RWM
Kelly, M
Travers, SAA
Bradshaw, B
Vartia, S
Stephens, KM
McCormack, GP
AF Redmond, Niamh E.
Raleigh, Jean
van Soest, Rob W. M.
Kelly, Michelle
Travers, Simon A. A.
Bradshaw, Brian
Vartia, Salla
Stephens, Kelly M.
McCormack, Grace P.
TI Phylogenetic Relationships of the Marine Haplosclerida (Phylum Porifera)
Employing Ribosomal (28S rRNA) and Mitochondrial (cox1, nad1) Gene
Sequence Data
SO PLOS ONE
LA English
DT Article
ID OXIDASE SUBUNIT-I; CLASS DEMOSPONGIAE; ORDER HAPLOSCLERIDA;
MAXIMUM-LIKELIHOOD; MIXED MODELS; CLASSIFICATION; INFERENCE; SUPPORTS;
RDNA; AMPLIFICATION
AB The systematics of the poriferan Order Haplosclerida (Class Demospongiae) has been under scrutiny for a number of years without resolution. Molecular data suggests that the order needs revision at all taxonomic levels. Here, we provide a comprehensive view of the phylogenetic relationships of the marine Haplosclerida using many species from across the order, and three gene regions. Gene trees generated using 28S rRNA, nad1 and cox1 gene data, under maximum likelihood and Bayesian approaches, are highly congruent and suggest the presence of four clades. Clade A is comprised primarily of species of Haliclona and Callyspongia, and clade B is comprised of H. simulans and H. vansoesti (Family Chalinidae), Amphimedon queenslandica (Family Niphatidae) and Tabulocalyx (Family Phloeodictyidae), Clade C is comprised primarily of members of the Families Petrosiidae and Niphatidae, while Clade D is comprised of Aka species. The polyphletic nature of the suborders, families and genera described in other studies is also found here.
C1 [Redmond, Niamh E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Redmond, Niamh E.; Raleigh, Jean; Bradshaw, Brian; Vartia, Salla; Stephens, Kelly M.; McCormack, Grace P.] Natl Univ Ireland, Galway, Ireland.
[van Soest, Rob W. M.] Univ Amsterdam, Zool Museum, Amsterdam, Netherlands.
[Kelly, Michelle] Natl Inst Water & Atmospher Res, Natl Ctr Aquat Biodivers & Biosecur, Auckland, New Zealand.
[Travers, Simon A. A.] Univ Western Cape, S African Natl Bioinformat Inst, ZA-7535 Bellville, South Africa.
RP Redmond, NE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
EM grace.mccormack@nuigalway.ie
FU Irish Research Council for Science, Engineering and Technology
[EI/SC/2003432/Y]; U.S. National Science Foundation [0829986]
FX The Irish Research Council for Science, Engineering and Technology
(http://www.ircset.ie/) primarily funded this work, Grant No.
EI/SC/2003432/Y. The Porifera Tree of Life Project, which is funded by
the U.S. National Science Foundation (http://www.nsf.gov/) Grant No.
0829986, to Robert W. Thacker and Allen G. Collins, provided sequences
from specimens. The funders had no role in study design, data collection
and analysis, decision to publish, or preparation of the manuscript.
NR 60
TC 20
Z9 20
U1 3
U2 15
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 SEP 13
PY 2011
VL 6
IS 9
AR e24344
DI 10.1371/journal.pone.0024344
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 825ZV
UT WOS:000295321800024
PM 21931685
ER
PT J
AU Pringle, JM
Blakeslee, AMH
Byers, JE
Roman, J
AF Pringle, James M.
Blakeslee, April M. H.
Byers, James E.
Roman, Joe
TI Asymmetric dispersal allows an upstream region to control population
structure throughout a species' range
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE invasive species; marine genetics; phylogeography; physical oceanography
ID LONG-DISTANCE DISPERSAL; CRAB; LARVAE; SHELF; GULF; FLOW; VARIABILITY;
CIRCULATION; PATHOGENS; RETENTION
AB In a single well-mixed population, equally abundant neutral alleles are equally likely to persist. However, in spatially complex populations structured by an asymmetric dispersal mechanism, such as a coastal population where larvae are predominantly moved downstream by currents, the eventual frequency of neutral haplotypes will depend on their initial spatial location. In our study of the progression of two spatially separate, genetically distinct introductions of the European green crab (Carcinus maenas) along the coast of eastern North America, we captured this process in action. We documented the shift of the genetic cline in this species over 8 y, and here we detail how the upstream haplotypes are beginning to dominate the system. This quantification of an evolving genetic boundary in a coastal system demonstrates that novel genetic alleles or haplotypes that arise or are introduced into upstream retention zones (regions whose export of larvae is not balanced by import from elsewhere) will increase in frequency in the entire system. This phenomenon should be widespread when there is asymmetrical dispersal, in the oceans or on land, suggesting that the upstream edge of a species' range can influence genetic diversity throughout its distribution. Efforts to protect the upstream edge of an asymmetrically dispersing species' range are vital to conserving genetic diversity in the species.
C1 [Pringle, James M.] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
[Blakeslee, April M. H.] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA.
[Byers, James E.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA.
[Roman, Joe] Univ Vermont, Gund Inst Ecol Econ, Burlington, VT 05405 USA.
RP Pringle, JM (reprint author), Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA.
EM jpringle@unh.edu
FU Greg Ruiz Invasion laboratory; Whitman Miller Invasion laboratory; Plant
Ecology laboratory at the Smithsonian Environmental Research Center;
Sloan Foundation's Census of Marine Life; National Science Foundation
[OCE0961344]
FX The original data collection and preliminary analyses were performed by
J.R. in the laboratory of S. Palumbi, who was essential in catalyzing
this research. We thank Carrie Keogh for help with data collection,
Caitlin Hamer for field and laboratory assistance, and Michael Lesser
for use of equipment and facilities. A.M.H.B. thanks Greg Ruiz, Whitman
Miller, the Invasions laboratory, and the Plant Ecology laboratory at
the Smithsonian Environmental Research Center for support and use of
facilities. The 2007 data collection was supported by the Sloan
Foundation's Census of Marine Life. J.M.P. and J.E.B. were supported by
National Science Foundation Grant OCE0961344.
NR 35
TC 47
Z9 47
U1 0
U2 26
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 SEP 13
PY 2011
VL 108
IS 37
BP 15288
EP 15293
DI 10.1073/pnas.1100473108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 819DF
UT WOS:000294804900061
PM 21876126
ER
PT J
AU Taylor, PJ
Lavrenchenko, LA
Carleton, MD
Verheyen, E
Bennett, NC
Oosthuizen, CJ
Maree, S
AF Taylor, Peter J.
Lavrenchenko, Leonid A.
Carleton, Michael D.
Verheyen, Erik
Bennett, Nigel C.
Oosthuizen, Carel J.
Maree, Sarita
TI Specific limits and emerging diversity patterns in East African
populations of laminate-toothed rats, genus Otomys (Muridae: Murinae:
Otomyini): Revision of the Otomys typus complex
SO ZOOTAXA
LA English
DT Article
DE Otomys; geometric morphometrics; cytochrome b; 12S rRNA; microendemism;
speciation; Afromontane
ID 12S RIBOSOMAL-RNA; NUCLEOTIDE SUBSTITUTION; GEOMETRIC MORPHOMETRICS;
PHYLOGENETIC TREES; ENDEMIC RODENTS; ARC MOUNTAINS; SEQUENCE; DNA;
TANZANIA; CLIMATE
AB We combined evidence from biogeography, craniodental traits, linear and geometric morphometrics (233 skulls), cytogenetics (karyotypes of 18 individuals) and mitochondrial DNA sequences (44 cytochrome b and 21 12S rRNA sequences) to test species limits within Otomys typus s.l. (Muridae: Murinae: Otomyini), a complex that is patchily distributed across alpine zones of Ethiopia and East Africa. Our results confirm the specific validity of O. dartmouthi, O. jacksoni, O. orestes, and O. uzungwensis, forms recently removed from synonymy under typus s.l.; support elevation of four other alpine forms to species (O. fortior, O. helleri, O. thomasi, and O. zinki); identify three additional new species (O. cheesmani sp. nov., O. simiensis sp. nov., O. yaldeni sp. nov.); and enable redefinition of O. typus s.s. as a species restricted to certain mountains west of the Great Rift Valley in Ethiopia (Simien and Guna Mountains in the north, extending to the highlands of the western rim of the Rift Valley). Phylogenetic interpretation of the cytochrome b data clearly demonstrates that the alpine morphotype once united under O. typus s.l. has originated independently at high elevations on several mountain ranges in eastern and northeastern Africa; although generally adapted to high-elevation vegetation, such alpine species are ecologically segregated from one another. Patterns of morphometric, genetic, and ecological differentiation among populations once misassigned to nominal O. tropicalis and O. typus more parsimoniously reflect regional cladogenesis along elevational gradients, rather than multiple, successive colonization by different ancestral forms from southern Africa as earlier supposed. Although incomplete and preliminary, information gathered for O. tropicalis indicates that it too is a species composite; several lines of research are discussed to redress its polyphyletic content. Our results, together with other recent taxonomic studies of Otomys, appreciably elevate the level of endemism within eastern Africa and underscore the significance of Africa's eastern highlands to the continental diversification of Otomyini.
C1 [Taylor, Peter J.] Durban Nat Sci Museum, ZA-4000 Durban, South Africa.
[Taylor, Peter J.] Univ Venda, Dept Ecol & Resource Management, Thohoyandou, South Africa.
[Taylor, Peter J.] Univ KwaZulu Natal, Sch Biol & Conservat Sci, Durban, South Africa.
[Lavrenchenko, Leonid A.] Russian Acad Sci, Severtsov Inst Ecol & Evolut, Moscow 119071, Russia.
[Carleton, Michael D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Verheyen, Erik] Royal Belgian Inst Nat Sci, Vertebrate Dept, B-1000 Brussels, Belgium.
[Oosthuizen, Carel J.; Maree, Sarita] Univ Pretoria, Dept Zool & Entomol, Mammal Res Inst, ZA-0002 Pretoria, South Africa.
[Oosthuizen, Carel J.; Maree, Sarita] Univ Pretoria, Dept Genet, Molecular Ecol & Evolut Programme, ZA-0002 Pretoria, South Africa.
RP Taylor, PJ (reprint author), Durban Nat Sci Museum, POB 4085, ZA-4000 Durban, South Africa.
EM Peter.Taylor@univen.ac.za; lavrenchenko@sevin.ru; carletonm@si.edu;
erik.verheyen@naturalsciences.be; smaree@zoology.up.ac.za
RI Taylor, Peter/E-8655-2011;
OI Taylor, Peter/0000-0001-9048-7366; Bennett, Nigel/0000-0001-9748-2947
FU Smithsonian Institution; South African National Research Foundation
FX We are indebted to the many curators who facilitated access to museum
collections of Otomys: John Phelps, William T. Stanley, and Lawrence
Heaney from the Field Museum of Natural History (FMNH); Farish Jenkins
and Judith Chapasko from the Museum of Comparative Zoology, Harvard
(MCZ); Wim Van Neer and Wim Wendelin from the Royal Museum for Central
Africa, Tervuren, Belgium (RMCA); Linda Gordon and Michael Carleton from
the Smithsonian Museum of Natural History, Washington DC (USNM); Fritz
Dieterlen from the Museum fur Naturkunde, Stuttgart, Germany (SM); Paula
Jenkins from the Natural History Museum, London (BM); and Teresa Kearney
from the Transvaal Museum, Northern Flagship Institute, Pretoria (TM).
We are grateful to Paulina Jenkins and additional staff of the Natural
History Museum, London for arranging and granting permission for the use
of high quality photographs of the holotype of Otomys cheesmani sp. nov.
Vladimir M. Aniskin and Nina Sh.c (Severtsov Institute of Ecology and
Evolution, RAS) made an inestimable contribution to the karyological
part of this study. We gratefully acknowledge the financial assistance
of the Smithsonian Institution Short Term Visitor Award (in 2006), and a
South African National Research Foundation Grant (between 2005 and
2007), which allowed P.J.T. to visit and study important North American
and European museum collections of Otomys. We thank Julian Kerbis,
Christiane Denys, Ann Laudisoit and L.J. McLellan for donating tissues
for molecular analysis. We are grateful to two anonymous reviewers whose
comments immeasurably improved this paper.
NR 123
TC 13
Z9 14
U1 1
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 SEP 13
PY 2011
IS 3024
BP 1
EP 66
PG 66
WC Zoology
SC Zoology
GA 818MJ
UT WOS:000294755500001
ER
PT J
AU Megill, ND
Fresl, K
Waegell, M
Aravind, PK
Pavicic, M
AF Megill, Norman D.
Fresl, Kresimir
Waegell, Mordecai
Aravind, P. K.
Pavicic, Mladen
TI Probabilistic generation of quantum contextual sets
SO PHYSICS LETTERS A
LA English
DT Article
DE Kochen-Specker sets; MMP hypergraphs; 600-cell
ID STATE
AB We give a method for exhaustive generation of a huge number of Kochen-Specker contextual sets, based on the 600-cell, for possible experiments and quantum gates. The method is complementary to our previous parity proof generation of these sets, and it gives all sets while the parity proof method gives only sets with an odd number of edges in their hypergraph representation. Thus we obtain 35 new kinds of critical KS sets with an even number of edges. We also give a statistical estimate of the number of sets that might be obtained in an eventual exhaustive enumeration. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 41000, Croatia.
[Pavicic, Mladen] Harvard Univ, Dept Phys, ITAMP, Cambridge, MA 02138 USA.
[Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Waegell, Mordecai; Aravind, P. K.] Worcester Polytech Inst, Dept Phys, Worcester, MA 01609 USA.
[Fresl, Kresimir] Univ Zagreb, Fac Civil Engn, Dept Mech, Zagreb 41000, Croatia.
[Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA.
RP Pavicic, M (reprint author), Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 41000, Croatia.
EM pavicic@grad.hr
FU Ministry of Science, Education, and Sport of Croatia [082-0982562-3160];
US Nat. Sci. Found.
FX One of us (M.P.) thanks his host Hossein Sadeghpour for a support at
ITAMP. Supported by the US Nat. Sci. Found. through a grant for Inst.
for Theor., Atom., Molec., and Opt. Phys. (ITAMP) at Harvard Univ. and
Smithsonian Astrophys. Obs. and by the Ministry of Science, Education,
and Sport of Croatia (project 082-0982562-3160). Computational support
was provided by the Zagreb Univ. Computing Centre and Croatian Nat. Grid
Infrastructure.
NR 26
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U1 2
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0375-9601
J9 PHYS LETT A
JI Phys. Lett. A
PD SEP 12
PY 2011
VL 375
IS 39
BP 3419
EP 3424
DI 10.1016/j.physleta.2011.07.050
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 828KV
UT WOS:000295500800007
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Boltuch, D
Bugaev, V
Cannon, A
Ciupik, L
Cogan, P
Colin, P
Dickherber, R
Falcone, A
Fegan, SJ
Finley, JP
Fortin, P
Fortson, LF
Furniss, A
Gall, D
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
Maier, G
Moriarty, P
Mukherjee, R
Ong, RA
Otte, AN
Pandel, D
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reynolds, PT
Rose, HJ
Schroedter, M
Sembroski, GH
Smith, AW
Steele, D
Swordy, SP
Theiling, M
Toner, JA
Varlotta, A
Vassiliev, VV
Vincent, S
Wagner, R
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.
Beilicke, M.
Benbow, W.
Boltuch, D.
Bugaev, V.
Cannon, A.
Ciupik, L.
Cogan, P.
Colin, P.
Dickherber, R.
Falcone, A.
Fegan, S. J.
Finley, J. P.
Fortin, P.
Fortson, L. F.
Furniss, A.
Gall, D.
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.
Maier, G.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Otte, A. N.
Pandel, D.
Perkins, J. S.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reynolds, P. T.
Rose, H. J.
Schroedter, M.
Sembroski, G. H.
Smith, A. W.
Steele, D.
Swordy, S. P.
Theiling, M.
Toner, J. A.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Wagner, R.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Wissel, S.
Wood, M.
Zitzer, B.
TI MULTIWAVELENGTH OBSERVATIONS OF THE VERY HIGH ENERGY BLAZAR 1ES 2344+514
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (IES 2344+514)
ID BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION; EINSTEIN SLEW SURVEY;
CORRELATED VARIABILITY; CHERENKOV TELESCOPES; SPECTRAL VARIABILITY;
STRONG FLARES; MARKARIAN 501; RADIATION; VERITAS
AB Multiwavelength observations of the high-frequency-peaked blazar 1ES 2344+514 were performed from 2007 October to 2008 January. The campaign represents the first contemporaneous data on the object at very high energy (VHE, E > 100 GeV) gamma-ray, X-ray, and UV energies. Observations with VERITAS in VHE gamma-rays yield a strong detection of 20s with 633 excess events in a total exposure of 18.1 hr live time. A strong VHE gamma-ray flare on 2007 December 7 is measured at F(> 300 GeV) = (6.76 +/- 0.62) x 10(-11) photons cm(-2) s(-1), corresponding to 48% of the Crab Nebula flux. Excluding this flaring episode, nightly variability at lower fluxes is observed with a time-averaged mean of F(> 300 GeV) = (1.06 +/- 0.09) x 10(-11) photons cm(-2) s(-1) (7.6% of the Crab Nebula flux). The differential photon spectrum between 390 GeV and 8.3 TeV for the time-averaged observations excluding 2007 December 7 is well described by a power law with a photon index of G = 2.78 +/- 0.09(stat) +/- 0.15(syst). On the flaring night of 2007 December 7 the measured VHE gamma-ray photon index was Gamma = 2.43 +/- 0.22(stat) +/- 0.15(syst). Over the full period of VERITAS observations contemporaneous X-ray and UV data were taken with Swift and RXTE. The measured 2-10 keV flux ranged by a factor of similar to 7 during the campaign. On 2007 December 8 the highest ever observed X-ray flux from 1ES 2344+514 was measured by Swift X-ray Telescope at a flux of F(2-10 keV) = (6.28 +/- 0.31) x 10(-11) erg cm(-2) s(-1). Evidence for a correlation between the X-ray flux and VHE. -ray flux on nightly timescales is indicated with a Pearson correlation coefficient of r = 0.60 +/- 0.11. Contemporaneous spectral energy distributions (SEDs) of 1ES 2344+514 are presented for two distinct flux states. A one-zone synchrotron self-Compton (SSC) model describes both SEDs using parameters consistent with previous SSC modeling of 1ES 2344+514 from non-contemporaneous observations.
C1 [Acciari, V. A.; Benbow, W.; 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.; 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, Dept Phys, Santa Cruz, CA 95064 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.
[Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Ciupik, L.; Fortson, L. F.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Colin, P.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Fortin, P.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland.
[Horan, D.] Ecole Polytech, Lab Leprince Ringuet, CNRS, IN2P3, F-91128 Palaiseau, France.
[Humensky, T. B.; Swordy, S. P.; 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.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pichel, A.] Inst Astron & Fis Espacio, Buenos Aires, DF, Argentina.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Smith, A. W.; Wagner, R.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
EM jgrube@adlerplanetarium.org
OI 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; STFC in the UK; 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 STFC in the UK and by Science Foundation Ireland.
Special acknowledgment to the Swift and RXTE teams for the support of
these observations.
NR 49
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 169
DI 10.1088/0004-637X/738/2/169
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200051
ER
PT J
AU Cerrigone, L
Hora, JL
Umana, G
Trigilio, C
Hart, A
Fazio, G
AF Cerrigone, Luciano
Hora, Joseph L.
Umana, Grazia
Trigilio, Corrado
Hart, Alexa
Fazio, Giovanni
TI IDENTIFICATION OF THREE NEW PROTOPLANETARY NEBULAE EXHIBITING THE
UNIDENTIFIED FEATURE AT 21 mu m
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared: stars; stars: AGB and post-AGB
ID SPITZER-SPACE-TELESCOPE; POST-AGB STARS; YOUNG PLANETARY-NEBULAE;
OBSERVATORY SPECTROSCOPY; INFRARED SPECTROGRAPH; M EMISSION;
INTERSTELLAR; GALAXIES; CATALOG; DUST
AB Among its great findings, the Infrared Astronomical Satellite mission showed the existence of an unidentified mid-IR feature around 21 mu m. Since its discovery, this feature has been detected in all C-rich protoplanetary nebulae (PPNe) of intermediate spectral type (F-G) and-weakly-in a few PNe and asymptotic giant branch (AGB) stars, but the nature of its carriers remains unknown. In this paper, we show the detection of this feature in the spectra of three new stars transiting from the AGB to the PN stage obtained with the Spitzer Space Telescope. Following a recent suggestion, we try to model the spectral energy distributions of our targets with amorphous carbon and FeO, which might be responsible for the unidentified feature. The fit thus obtained is not completely satisfactory, since the shape of the feature is not well matched. In an attempt to relate the unidentified feature to other dust features, we retrieved mid-IR spectra of all 21 mu m sources currently known from Infrared Space Observatory and Spitzer online archives and noticed a correlation between the flux emitted in the 21 mu m feature and that emitted at 7 and 11 mu m (polycyclic aromatic hydrocarbon bands and hydrogenated amorphous carbon broad emission). Such a correlation may point to a common nature of the carriers.
C1 [Cerrigone, Luciano] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Hora, Joseph L.; Hart, Alexa; Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Umana, Grazia; Trigilio, Corrado] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
RP Cerrigone, L (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM lcerrigone@mpifr.de; jhora@cfa.harvard.edu; grazia.umana@oact.inaf.it;
corrado.trigilio@oact.inaf.it; ahart@cfa.harvard.edu;
gfazio@cfa.harvard.edu
OI Umana, Grazia/0000-0002-6972-8388
FU NASA; National Aeronautics and Space Administration [NAS5-26555];
Italian Council for Research in Astronomy; European Southern
Observatory; Space Telescope European Coordinating Facility;
International GEMINI project; European Space Agency Astrophysics
Division; European Commission [CT920791, CT940627]; INSU; MEN; CNRS in
France; State of Baden-Wurttemberg in Germany; DGICYT in Spain; CNR in
Italy; FFwFBWF in Austria; FAPESP in Brazil; OTKA in Hungary [F-4239,
F-013990]; ESO CEE [A-04-046]
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. The Guide Star Catalogue-II is a joint project of the Space
Telescope Science Institute and the Osservatorio Astronomico di Torino.
Space Telescope Science Institute is operated by the Association of
Universities for Research in Astronomy, for the National Aeronautics and
Space Administration under contract NAS5-26555. The participation of the
Osservatorio Astronomico di Torino is supported by the Italian Council
for Research in Astronomy. Additional support is provided by European
Southern Observatory, Space Telescope European Coordinating Facility,
the International GEMINI project, and the European Space Agency
Astrophysics Division. The DENIS project has been partly funded by the
SCIENCE and the HCM plans of the European Commission under grants
CT920791 and CT940627. It is supported by INSU, MEN, and CNRS in France,
by the State of Baden-Wurttemberg in Germany, by DGICYT in Spain, by CNR
in Italy, by FFwFBWF in Austria, by FAPESP in Brazil, by OTKA grants
F-4239 and F-013990 in Hungary, and by the ESO C&EE grant A-04-046. Jean
Claude Renault from IAP was the Project manager. Observations were
carried out thanks to the contribution of numerous students and young
scientists from all involved institutes, under the supervision of P.
Fouque, survey astronomer resident in 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. This research is based in part on observations with AKARI, a
JAXA project with the participation of ESA.
NR 32
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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 SEP 10
PY 2011
VL 738
IS 2
AR 121
DI 10.1088/0004-637X/738/2/121
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200003
ER
PT J
AU Cohen, O
Kashyap, VL
Drake, JJ
Sokolov, IV
Gombosi, TI
AF Cohen, O.
Kashyap, V. L.
Drake, J. J.
Sokolov, I. V.
Gombosi, T. I.
TI THE DYNAMICS OF STELLAR CORONAE HARBORING HOT JUPITERS. II. A SPACE
WEATHER EVENT ON A HOT JUPITER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planet; star interactions; stars: coronae; Sun: coronal mass ejections
(CMEs)
ID EXTRASOLAR GIANT PLANETS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY;
IN HABITABLE ZONES; MASS M-STARS; X-RAY; TERRESTRIAL EXOPLANETS;
CHROMOSPHERIC ACTIVITY; ANGULAR-MOMENTUM; MAGNETIC-FIELDS
AB We carry out a numerical simulation depicting the effects of a coronal mass ejection (CME) event on a close-in giant planet in an extrasolar system. We drive the CME in a similar manner as in simulations of space weather events on Earth. The simulation includes the planetary orbital motion, which leads to the forming of a comet-like planetary magnetotail which is oriented almost perpendicular to the direction of propagation of the CME. The combination of this feature and the fact that the CME does not expand much by the time it reaches the planet leads to a unique CME-magnetosphere interaction, where the CME itself is highly affected by the presence of the planetary magnetosphere. This change in the CME properties throughout the event cannot be estimated by simple, analytic calculations. We find that the planet is well-shielded from CME penetration, even for a relatively weak intrinsic magnetic field. The planetary angular momentum loss associated with such an event is negligible compared to the total planetary angular momentum. We also find that the energy which is deposited in the magnetosphere is much higher than in the case of the Earth, and our simulation suggests there is a large-scale change in the orientation of the magnetosphere-ionosphere current system during the CME event.
C1 [Cohen, O.; Kashyap, V. L.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sokolov, I. V.; 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; Sokolov, Igor/H-9860-2013;
OI Gombosi, Tamas/0000-0001-9360-4951; Sokolov, Igor/0000-0002-6118-0469;
Cohen, Ofer/0000-0003-3721-0215
FU SHINE through NSF [ATM-0823592]; NASA-LWSTRT [NNG05GM44G]; NASA
[NAS8-39073]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI
FX We thank an unknown referee for her/his many useful comments. We also
thank KC Hansen, Alex Glocer, and Aaron Ridley for their useful comments
on the magnetospheric response to the CME. O.C. is supported by SHINE
through NSF ATM-0823592 grant, and by NASA-LWSTRT Grant NNG05GM44G.
J.J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the
Chandra X-ray Center. Simulation results were obtained using the Space
Weather Modeling Framework, developed by the Center for Space
Environment Modeling, at the University of Michigan with funding support
from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI.
NR 69
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 166
DI 10.1088/0004-637X/738/2/166
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200048
ER
PT J
AU Gavazzi, R
Cooray, A
Conley, A
Aguirre, JE
Amblard, A
Auld, R
Beelen, A
Blain, A
Blundell, R
Bock, J
Bradford, CM
Bridge, C
Brisbin, D
Burgarella, D
Chanial, P
Chapin, E
Christopher, N
Clements, DL
Cox, P
Djorgovski, SG
Dowell, CD
Eales, S
Earle, L
Ellsworth-Bowers, TP
Farrah, D
Franceschini, A
Fu, H
Glenn, J
Solares, EAG
Griffin, M
Gurwell, MA
Halpern, M
Ibar, E
Ivison, RJ
Jarvis, M
Kamenetzky, J
Kim, S
Krips, M
Levenson, L
Lupu, R
Mahabal, A
Maloney, PD
Maraston, C
Marchetti, L
Marsden, G
Matsuhara, H
Mortier, AMJ
Murphy, E
Naylor, BJ
Neri, R
Nguyen, HT
Oliver, SJ
Omont, A
Page, MJ
Papageorgiou, A
Pearson, CP
Perez-Fournon, I
Pohlen, M
Rangwala, N
Rawlings, JI
Raymond, G
Riechers, D
Rodighiero, G
Roseboom, IG
Rowan-Robinson, M
Schulz, B
Scott, D
Scott, KS
Serra, P
Seymour, N
Shupe, DL
Smith, AJ
Symeonidis, M
Tugwell, KE
Vaccari, M
Valiante, E
Valtchanov, I
Verma, A
Vieira, JD
Vigroux, L
Wang, L
Wardlow, J
Wiebe, D
Wright, G
Xu, CK
Zeimann, G
Zemcov, M
Zmuidzinas, J
AF Gavazzi, R.
Cooray, A.
Conley, A.
Aguirre, J. E.
Amblard, A.
Auld, R.
Beelen, A.
Blain, A.
Blundell, R.
Bock, J.
Bradford, C. M.
Bridge, C.
Brisbin, D.
Burgarella, D.
Chanial, P.
Chapin, E.
Christopher, N.
Clements, D. L.
Cox, P.
Djorgovski, S. G.
Dowell, C. D.
Eales, S.
Earle, L.
Ellsworth-Bowers, T. P.
Farrah, D.
Franceschini, A.
Fu, H.
Glenn, J.
Solares, E. A. Gonzalez
Griffin, M.
Gurwell, M. A.
Halpern, M.
Ibar, E.
Ivison, R. J.
Jarvis, M.
Kamenetzky, J.
Kim, S.
Krips, M.
Levenson, L.
Lupu, R.
Mahabal, A.
Maloney, P. D.
Maraston, C.
Marchetti, L.
Marsden, G.
Matsuhara, H.
Mortier, A. M. J.
Murphy, E.
Naylor, B. J.
Neri, R.
Nguyen, H. T.
Oliver, S. J.
Omont, A.
Page, M. J.
Papageorgiou, A.
Pearson, C. P.
Perez-Fournon, I.
Pohlen, M.
Rangwala, N.
Rawlings, J. I.
Raymond, G.
Riechers, D.
Rodighiero, G.
Roseboom, I. G.
Rowan-Robinson, M.
Schulz, B.
Scott, Douglas
Scott, K. S.
Serra, P.
Seymour, N.
Shupe, D. L.
Smith, A. J.
Symeonidis, M.
Tugwell, K. E.
Vaccari, M.
Valiante, E.
Valtchanov, I.
Verma, A.
Vieira, J. D.
Vigroux, L.
Wang, L.
Wardlow, J.
Wiebe, D.
Wright, G.
Xu, C. K.
Zeimann, G.
Zemcov, M.
Zmuidzinas, J.
TI MODELING OF THE HERMES SUBMILLIMETER SOURCE LENSED BY A DARK MATTER
DOMINATED FOREGROUND GROUP OF GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: groups: general;
galaxies: halos; gravitational lensing: strong; submillimeter: galaxies
ID HIGH-DENSITY ENVIRONMENTS; ELLIPTIC GALAXIES; HIGH-REDSHIFT; ACS SURVEY;
STAR-FORMATION; NUMBER COUNTS; MASS PROFILE; HALOS; FIELD; EVOLUTION
AB We present the results of a gravitational lensing analysis of the bright z(s) = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be mu = 10.9 +/- 0.7. We measure the half-light radius R-eff of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R-eff,R-* = [2.0 +/- 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (R-eff,R-gas = [1.1 +/- 0.5] kpc) by mapping back in the source plane the CO (J = 5 -> 4) transition line emission. The lens modeling yields a relatively large Einstein radius R-Ein = 4 ''.10 +/- 0 ''.02, corresponding to a deflector velocity dispersion of [483 +/- 16] km s(-1). This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z(l) similar to 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f(dm)(= 100 GeV) range at a flux level detectable by the current generation of ground-based Cherenkov telescopes. This enables us to place constraints on models of extragalactic background light within LAT energies and features the source as a promising candidate for VHE studies of the universe at an unprecedented redshift of z = 0.896.
C1 [McConville, W.; Donato, D.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[McConville, W.; Donato, D.; McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA.
[McConville, W.; Donato, D.; McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Ostorero, L.] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Ostorero, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Ostorero, L.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Ostorero, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Moderski, R.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Kanagawa 2525210, Japan.
[Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
[Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA.
[Ajello, M.; Monzani, M. E.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Ajello, M.; Monzani, M. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Bouvier, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Bregeon, J.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Donato, D.] CRESST, Greenbelt, MD 20771 USA.
[Finke, J.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Orienti, M.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Orienti, M.; Rossetti, A.] Ist Radioastron INAF, I-40129 Bologna, Italy.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
RP McConville, W (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA.
EM wmcconvi@umd.edu; stawarz@astro.isas.jaxa.jp;
Teddy.Cheung.ctr@nrl.navy.mil
RI McEnery, Julie/D-6612-2012;
OI Ostorero, Luisa/0000-0003-3983-5980; orienti, monica/0000-0003-4470-7094
FU INFN [PD51]; ASI [I/016/07/0]; MNiSW [N-N203-301635]
FX L.O. acknowledges support by a 2009 National Fellowship "L'OREAL Italia
Per le Donne e la Scienza" of the L'OREAL-UNESCO program "ForWomen in
Science," and partial support from the INFN grant PD51 and the ASI
Contract No. I/016/07/0 COFIS. L. S. is grateful for the support from
Polish MNiSW through the grant N-N203-380336. R. M. was supported by the
MNiSW grant no. N-N203-301635
NR 114
TC 21
Z9 21
U1 0
U2 9
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 148
DI 10.1088/0004-637X/738/2/148
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200030
ER
PT J
AU Saul, M
Cunningham, M
Rathborne, J
Walsh, W
Butner, HM
AF Saul, M.
Cunningham, M.
Rathborne, J.
Walsh, W.
Butner, H. M.
TI PRESTELLAR CORES IN THE COALSACK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; ISM: molecules; ISM: structure; radio lines: ISM; stars:
formation; stars: protostars
ID SOUTHERN COALSACK; STAR-FORMATION; MOLECULAR CLOUDS; BETA-PHOTOMETRY;
DARK CLOUDS; DENSE CORES; NANTEN OBSERVATIONS; BOK GLOBULE; MILKY-WAY;
CO SURVEY
AB We present high spectral resolution millimeter mapped observations of seven prestellar cores in the Coalsack, including imaging in five optically thin molecular species of the kinematic structure of two of the densest cores, C2 and C4. Various collapse-critical indices are calculated; critical masses needed for collapse are consistently greater than those observed, the latter ranging from 0.4 to 2.4 M-circle dot. The molecular emission in several of the cores shows line profiles with infall characteristics as well as elongated areas of increased line widths and reversals of center velocity gradients, implying that accretion disks may be forming.
C1 [Saul, M.; Cunningham, M.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Rathborne, J.] Las Condes, Dept Astron, Santiago, Chile.
[Walsh, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA.
RP Saul, M (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM msaul@phys.unsw.edu.au; mariac@phys.unsw.edu.au; rathborn@das.uchile.cl;
wwalsh@cfa.harvard.edu; butnerhm@jmu.edu
OI Butner, Harold/0000-0003-4899-2064; Cunningham,
Maria/0000-0001-7020-6176
NR 48
TC 3
Z9 3
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 SEP 10
PY 2011
VL 738
IS 2
AR 152
DI 10.1088/0004-637X/738/2/152
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200034
ER
PT J
AU Schmelz, JT
Rightmire, LA
Saar, SH
Kimble, JA
Worley, BT
Pathak, S
AF Schmelz, J. T.
Rightmire, L. A.
Saar, S. H.
Kimble, J. A.
Worley, B. T.
Pathak, S.
TI WARM AND FUZZY: TEMPERATURE AND DENSITY ANALYSIS OF AN Fe xv EUV IMAGING
SPECTROMETER LOOP
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: UV radiation; Sun: X-rays; gamma rays
ID ACTIVE-REGION LOOPS; CORONAL LOOPS; RAY TELESCOPE; MULTITHERMAL
ANALYSIS; ATOMIC DATABASE; EMISSION-LINES; HINODE; DISTRIBUTIONS;
WAVELENGTHS; ANGSTROM
AB The Hinode EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) were designed in part to work together. They have the same spatial resolution and cover different but overlapping coronal temperature ranges. These properties make a combined data set ideal for multithermal analysis, where EIS provides the best information on the cooler corona (log T < 6.5) and XRT provides the best information on the hotter corona (log T > 6.5). Here, we analyze a warm non-flaring loop detected in images made in a strong EIS Fe xv emission line with a wavelength of 284.16 angstrom and peak formation temperature of log T = 6.3. We perform differential emission measure (DEM) analysis in three pixels at different heights above the footpoint and find multithermal results with the bulk of the emission measure in the range 6.0 < log T < 6.6. Analysis with the EIS lines alone gave a DEM with huge amounts of emission measure at very high temperatures (log T > 7.2); analysis with XRT data alone resulted in a DEM that was missing most of the cooler emission measure required to produce many of the EIS lines. Thus, both results were misleading and unphysical. It was only by combining the EIS and XRT data that we were able to produce a reasonable result, one without ad hoc assumptions on the shape and range of the DEM itself.
C1 [Schmelz, J. T.; Rightmire, L. A.; Kimble, J. A.; Worley, B. T.; Pathak, S.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
[Schmelz, J. T.; Saar, S. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Rightmire, L. A.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA.
EM jschmelz@memphis.edu
FU NASA/SAO; NSF [ATM-0402729]; NASA [NNM07AB07C]
FX Hinode is a Japanese mission developed and launched by ISAS/JAXA, with
NAOJ as domestic partner and NASA and STFC (UK) as international
partners. It is operated by these agencies in co-operation with ESA and
the NSC (Norway). CHIANTI is a collaborative project involving the NRL
(USA), the Universities of Florence (Italy) and Cambridge (UK), and
George Mason University (USA). Solar physics research at the University
of Memphis is supported by a Hinode subcontract from NASA/SAO as well as
NSF ATM-0402729. S. H. S. is supported by contract NNM07AB07C to NASA.
We benefited greatly from discussions at four workshops on solar coronal
loops: Paris (2002 November), Palermo (2004 September), Santorini (2007
June), and Florence (2009 June).
NR 29
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 146
DI 10.1088/0004-637X/738/2/146
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200028
ER
PT J
AU Williamson, R
Benson, BA
High, FW
Vanderlinde, K
Ade, PAR
Aird, KA
Andersson, K
Armstrong, R
Ashby, MLN
Bautz, M
Bazin, G
Bertin, E
Bleem, LE
Bonamente, M
Brodwin, M
Carlstrom, JE
Chang, CL
Chapman, SC
Clocchiatti, A
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Fazio, GG
Foley, RJ
Forman, WR
Garmire, G
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Murray, SS
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Saliwanchik, BR
Saro, A
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Stanford, SA
Staniszewski, Z
Stark, AA
Story, K
Stubbs, CW
Vieira, JD
Vikhlinin, A
Zenteno, A
AF Williamson, R.
Benson, B. A.
High, F. W.
Vanderlinde, K.
Ade, P. A. R.
Aird, K. A.
Andersson, K.
Armstrong, R.
Ashby, M. L. N.
Bautz, M.
Bazin, G.
Bertin, E.
Bleem, L. E.
Bonamente, M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Chapman, S. C.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Fazio, G. G.
Foley, R. J.
Forman, W. R.
Garmire, G.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Stanford, S. A.
Staniszewski, Z.
Stark, A. A.
Story, K.
Stubbs, C. W.
Vieira, J. D.
Vikhlinin, A.
Zenteno, A.
TI A SUNYAEV-ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS
IN THE 2500 deg(2) SOUTH POLE TELESCOPE SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general
ID ATACAMA COSMOLOGY TELESCOPE; GREATER-THAN 1; ALL-SKY SURVEY; PHOTOMETRIC
REDSHIFTS; SCALING RELATIONS; STELLAR LOCUS; POWER SPECTRA; DARK-MATTER;
CATALOG; CONSTRAINTS
AB The South Pole Telescope (SPT) is currently surveying 2500 deg(2) of the southern sky to detect massive galaxy clusters out to the epoch of their formation using the Sunyaev-Zel'dovich (SZ) effect. This paper presents a catalog of the 26 most significant SZ cluster detections in the full survey region. The catalog includes 14 clusters which have been previously identified and 12 that are new discoveries. These clusters were identified in fields observed to two differing noise depths: 1500 deg2 at the final SPT survey depth of 18 mu K arcmin at 150 GHz and 1000 deg2 at a depth of 54 mu K arcmin. Clusters were selected on the basis of their SZ signal-to-noise ratio (S/N) in SPT maps, a quantity which has been demonstrated to correlate tightly with cluster mass. The S/N thresholds were chosen to achieve a comparablemass selection across survey fields of both depths. Cluster redshifts were obtained with optical and infrared imaging and spectroscopy from a variety of ground-and space-based facilities. The redshifts range from 0.098 <= z <= 1.132 with a median of z(med) = 0.40. The measured SZ S/N and redshifts lead to unbiased mass estimates ranging from 9.8 x 10(14) M-circle dot h(70)(-1) <= M-200(rho(mean)) <= 3.1 x 10(15) M-circle dot h(-1). Based on the SZ mass estimates, we find that none of the clusters are individually in significant tension with the Lambda CDM cosmological model. We also test for evidence of non-Gaussianity based on the cluster sample and find the data show no preference for non-Gaussian perturbations.
C1 [Williamson, R.; Benson, B. A.; High, F. W.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hoover, S.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Vieira, J. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Williamson, R.; High, F. W.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Vanderlinde, K.; de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Ashby, M. L. N.; Brodwin, M.; Fazio, G. G.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Bertin, E.] Univ Paris 06, CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Bonamente, M.; Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Clocchiatti, A.] Dept Astron & Astrophys, Santiago 22, Chile.
[Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Garmire, G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Rest, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Williamson, R (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM rw247@kicp.uchicago.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996
FU National Science Foundation (NSF) [ANT-0638937, AST-1009012,
AST-1009649, MRI-0723073, NAS 8-03060]; NSF Physics Frontier Center
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation;
JPL/Caltech; NASA [12800071, 12800088, NAS8-03060]; NASA Office of Space
Science; National Sciences and Engineering Research Council of Canada,
Canad; Canadian Institute for Advanced Research; Excellence Cluster
Universe; DFG [TR33]; Clay Fellowship; KICP Fellowship; Pennsylvania
State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research
Fellowship; Smithsonian Institution; Brinson Foundation
FX The South Pole Telescope program is supported by the National Science
Foundation through grant ANT-0638937. Partial support is also provided
by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli
Institute of Cosmological Physics at the University of Chicago, the
Kavli Foundation, and the Gordon and Betty Moore Foundation. This work
is based in part on observations obtained with the Spitzer Space
Telescope (PID 60099), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. Additional data were obtained with the 6.5 m Magellan
Telescopes located at the Las Campanas Observatory, Chile. Support for
X-ray analysis was provided by NASA through Chandra Award Numbers
12800071 and 12800088 issued by the Chandra X-ray Observatory Center,
which is operated by the Smithsonian Astrophysical Observatory for and
on behalf of NASA under contract NAS8-03060. Optical imaging data from
the Blanco 4 m at Cerro Tololo Inter-American Observatories (programs
2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598) and spectroscopic
observations from VLT programs 086.A-0741 and 286.A-5021 and Gemini
program GS-2009B-Q-16 were included in this work. We acknowledge the use
of the Legacy Archive for Microwave Background Data Analysis (LAMBDA).
Support for LAMBDA is provided by the NASA Office of Space Science.
Galaxy cluster research at Harvard is supported by NSF grant
AST-1009012. Galaxy cluster research at SAO is supported in part by NSF
grants AST-1009649 and MRI-0723073. The McGill group acknowledges
funding from the National Sciences and Engineering Research Council of
Canada, Canada Research Chairs program, and the Canadian Institute for
Advanced Research. X-ray research at the CfA is supported through NASA
Contract NAS 8-03060. The Munich group acknowledges support from the
Excellence Cluster Universe and the DFG research program TR33. R.J.F. is
supported by a Clay Fellowship. B.A.B. is supported by a KICP
Fellowship, support for M. Brodwin was provided by the W. M. Keck
Foundation, M. Bautz acknowledges support from contract
2834-MIT-SAO-4018 from the Pennsylvania State University to the
Massachusetts Institute of Technology. M.D. acknowledges support from an
Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support
from the Smithsonian Institution, and B. S. acknowledges support from
the Brinson Foundation.
NR 68
TC 145
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U1 1
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 10
PY 2011
VL 738
IS 2
AR 139
DI 10.1088/0004-637X/738/2/139
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821DE
UT WOS:000294954200021
ER
PT J
AU Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bottcher, M
Bouvier, A
Bradbury, SM
Buckley, JH
Bugaev, V
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Errando, M
Falcone, A
Finley, JP
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Gyuk, G
Hanna, D
Holder, J
Huan, H
Hughes, G
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Madhavan, AS
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pichel, A
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Skole, C
Smith, AW
Staszak, D
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Tyler, J
Varlotta, A
Vincent, S
Vivier, M
Wakely, SP
Ward, JE
Weinstein, A
Weisgarber, T
Williams, DA
AF Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boettcher, M.
Bouvier, A.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Errando, M.
Falcone, A.
Finley, J. P.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Gyuk, G.
Hanna, D.
Holder, J.
Huan, H.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Madhavan, A. S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pichel, A.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Skole, C.
Smith, A. W.
Staszak, D.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Tyler, J.
Varlotta, A.
Vincent, S.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
TI VERITAS OBSERVATIONS OF THE UNUSUAL EXTRAGALACTIC TRANSIENT SWIFT
J164449.3+573451
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; galaxies: active; gamma rays: galaxies;
radiation mechanisms: non-thermal
ID GAMMA-RAY ASTRONOMY; CHERENKOV TELESCOPES; LIGHT
AB We report on very high energy (>100 GeV) gamma-ray observations of Swift J164449.3+573451, an unusual transient object first detected by the Swift Observatory and later detected by multiple radio, optical, and X-ray observatories. A total exposure of 28 hr was obtained on Swift J164449.3+573451 with the Very Energetic Radiation Imaging Telescope Array System ( VERITAS) during 2011 March 28-April 15. We do not detect the source and place a differential upper limit on the emission at 500 GeV during these observations of 1.4 x 10(-12) erg cm(-2) s(-1) (99% confidence level). We also present time-resolved upper limits and use a flux limit averaged over the X-ray flaring period to constrain various emission scenarios that can accommodate both the radio-through-X-ray emission detected from the source and the lack of detection by VERITAS.
C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Arlen, T.; Majumdar, P.; Ong, R. A.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA.
[Aune, T.; Bouvier, A.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Schroedter, M.; Theiling, M.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Cannon, A.; Collins-Hughes, E.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Huan, H.; Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Skole, C.] DESY, D-15738 Zeuthen, Germany.
[Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Madhavan, A. S.; Orr, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
[Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Smith, A. W.] Argonne Natl Lab, Argonne, IL 60439 USA.
RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
EM apbouvie@ucsc.edu; boettchm@ohio.edu; daniel-d-gall@uiowa.edu
OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610;
Ward, John E/0000-0003-1973-0794
FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian
Institution; NSERC in Canada; Science Foundation Ireland (SFI)
[10/RFP/AST2748]; STFC in the UK
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 (SFI 10/RFP/AST2748), and
by STFC in the UK. We acknowledge the excellent work of the technical
support staff at the Fred Lawrence Whipple Observatory and the
collaborating institutions in the construction and operation of the
instrument. This work made use of data supplied by the UK Swift Science
Data Centre at the University of Leicester.
NR 28
TC 5
Z9 5
U1 0
U2 10
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 10
PY 2011
VL 738
IS 2
AR L30
DI 10.1088/2041-8205/738/2/L30
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818NY
UT WOS:000294760700014
ER
PT J
AU Joron, M
Frezal, L
Jones, RT
Chamberlain, NL
Lee, SF
Haag, CR
Whibley, A
Becuwe, M
Baxter, SW
Ferguson, L
Wilkinson, PA
Salazar, C
Davidson, C
Clark, R
Quail, MA
Beasley, H
Glithero, R
Lloyd, C
Sims, S
Jones, MC
Rogers, J
Jiggins, CD
Ffrench-Constant, RH
AF Joron, Mathieu
Frezal, Lise
Jones, Robert T.
Chamberlain, Nicola L.
Lee, Siu F.
Haag, Christoph R.
Whibley, Annabel
Becuwe, Michel
Baxter, Simon W.
Ferguson, Laura
Wilkinson, Paul A.
Salazar, Camilo
Davidson, Claire
Clark, Richard
Quail, Michael A.
Beasley, Helen
Glithero, Rebecca
Lloyd, Christine
Sims, Sarah
Jones, Matthew C.
Rogers, Jane
Jiggins, Chris D.
Ffrench-Constant, Richard H.
TI Chromosomal rearrangements maintain a polymorphic supergene controlling
butterfly mimicry
SO NATURE
LA English
DT Article
ID GENE FLOW; HELICONIUS BUTTERFLIES; PAPILIO-DARDANUS; LOCUS; EVOLUTION;
INVERSIONS; SPECIATION; SEQUENCE; SELECTION; LINKAGE
AB Supergenes are tight clusters of loci that facilitate the co-segregation of adaptive variation, providing integrated control of complex adaptive phenotypes(1). Polymorphic supergenes, in which specific combinations of traits are maintained within a single population, were first described for 'pin' and 'thrum' floral types in Primula(1) and Fagopyrum(2), but classic examples are also found in insect mimicry(3-5) and snail morphology(6). Understanding the evolutionary mechanisms that generate these co-adapted gene sets, as well as the mode of limiting the production of unfit recombinant forms, remains a substantial challenge(7-10). Here we show that individual wing-pattern morphs in the polymorphic mimetic butterfly Heliconius numata are associated with different genomic rearrangements at the supergene locus P. These rearrangements tighten the genetic linkage between at least two colour-pattern loci that are known to recombine in closely related species(9-11), with complete suppression of recombination being observed in experimental crosses across a 400-kilobase interval containing at least 18 genes. In natural populations, notable patterns of linkage disequilibrium (LD) are observed across the entire P region. The resulting divergent haplotype clades and inversion breakpoints are found in complete association with wing-pattern morphs. Our results indicate that allelic combinations at known wing-patterning loci have become locked together in a polymorphic rearrangement at the P locus, forming a supergene that acts as a simple switch between complex adaptive phenotypes found in sympatry. These findings highlight how genomic rearrangements can have a central role in the coexistence of adaptive phenotypes involving several genes acting in concert, by locally limiting recombination and gene flow.
C1 [Joron, Mathieu; Frezal, Lise; Whibley, Annabel] CNRS, Museum Natl Hist Nat, UMR 7205, F-75005 Paris, France.
[Joron, Mathieu; Becuwe, Michel] Univ Edinburgh, Inst Evolutionary Biol, Ashworth Labs, Edinburgh EH9 3JT, Midlothian, Scotland.
[Joron, Mathieu] Leiden Univ, Inst Biol, NL-2300 RA Leiden, Netherlands.
[Jones, Robert T.; Chamberlain, Nicola L.; Wilkinson, Paul A.; Ffrench-Constant, Richard H.] Univ Exeter, Sch Biosci, Ctr Ecol & Conservat, Penryn TR10 9EZ, Cornwall, England.
[Lee, Siu F.] Univ Melbourne, Inst Bio21, Dept Genet, Parkville, Vic 3010, Australia.
[Haag, Christoph R.] Univ Fribourg, Dept Ecol & Evolut Biol, CH-1700 Fribourg, Switzerland.
[Baxter, Simon W.; Ferguson, Laura; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Salazar, Camilo] NAOS Isl, Smithsonian Trop Res Inst, Panama City, Panama.
[Davidson, Claire; Clark, Richard; Quail, Michael A.; Beasley, Helen; Glithero, Rebecca; Lloyd, Christine; Sims, Sarah; Jones, Matthew C.; Rogers, Jane] Wellcome Trust Sanger Inst, Cambridge CB10 1HH, England.
RP Joron, M (reprint author), CNRS, Museum Natl Hist Nat, UMR 7205, CP50,45 Rue Buffon, F-75005 Paris, France.
EM joron@mnhn.fr
RI Haag, Christoph/B-6488-2009; Whibley, Annabel/G-2836-2011; Jiggins,
Chris/B-9960-2008; Joron, Mathieu/C-9178-2009; Salazar,
camilo/A-1647-2010; GenePool, The/D-8812-2012;
OI Haag, Christoph/0000-0002-8817-1431; Jiggins, Chris/0000-0002-7809-062X;
Joron, Mathieu/0000-0003-1043-4147; Salazar, camilo/0000-0001-9217-6588;
ffrench-Constant, Richard/0000-0001-5385-9888; Davidson,
Claire/0000-0002-4910-8202
FU CNRS; EMBO [ALTF-431-2004]; Royal Society [516002.K5917/ROG]; European
Research Council; BBSRC [BBE0118451]; Leverhulme Trust [F/00144AY)];
Leverhulme Research Leadership grant
FX We thank M. Blaxter and D. Charlesworth for advice throughout the study;
The GenePool and S. Humphray for DNA sequencing; S. Kumar and A.
Papanicolaou for bioinformatics support; M. Beltran, A. Bulski, M.
Veuille and the Botanique-Entomologie-Mycologie molecular facility
(BoEM) for laboratory support; S. Johnston for genome-size estimates in
H. numata; D. Obbard for providing R scripts; M. Abanto, S. Gallusser,
C. Ramirez, L. de Silva, J. Barbut, B. Gilles and G. Lamas for help with
butterfly rearing, fieldwork and collecting permits; and the Peruvian
National Institute of Natural Resources (INRENA) for granting collecting
and export permits (076-2007-INRENA-IFFS-DCB). Fieldwork in French
Guiana was supported by a CNRS 'Nouragues Research Grant'. This work was
supported by an EMBO long-term fellowship (ALTF-431-2004), EMBO-matching
funds from NWO (Netherlands), a Royal Society University Research
Fellowship (516002.K5917/ROG), a CNRS grant (ATIP Biodiversite 2008,
France) and a European Research Council Starting Grant (ERC-Stg
'MimEvol') to M. J., a BBSRC grant (BBE0118451) to C. D. J. and
R.H.ff.-C., a Leverhulme Trust grant (F/00144AY) to R.H.ff.-C., and a
Royal Society University Research Fellowship and a Leverhulme Research
Leadership grant to C. D. J.
NR 42
TC 162
Z9 163
U1 13
U2 153
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD SEP 8
PY 2011
VL 477
IS 7363
BP 203
EP U102
DI 10.1038/nature10341
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 816MC
UT WOS:000294603900034
PM 21841803
ER
PT J
AU Zhao, L
Duan, WH
Yelin, SF
AF Zhao, L.
Duan, Wenhui
Yelin, S. F.
TI Generation of tunable-volume transmission-holographic gratings at low
light levels
SO PHYSICAL REVIEW A
LA English
DT Article
ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; QUANTUM COHERENCE; REFRACTION;
OPTICS; INDEX; MEDIA
AB By utilizing giant Kerr nonlinearity obtained by electromagnetically induced transparency (EIT), tunable volume transmission holographic gratings for a weak probe field can be generated by means of a standing-wave signal field at low light levels in a four-level N-type ultracold atomic ensemble. The induced grating can be characterized as a mixed volume holographic grating with a strong phase modulation accompanied by a weak amplitude modulation. Based on Kogelnik's coupled-wave theory in optical holography, we find that high diffraction efficiency (up to 85%) and sensitive angular selectivity (up to +/- 0.000149 rad) can be achieved for the induced grating in the Bragg diffraction regime. And, both of them can be dynamically controlled by tuning the weak standing-wave signal field and the coupling field. Our study not only develops a fundamental understanding of volume diffraction effects in EIT media, but also provides a practical prototype of EIT-based holographic devices for all-optical classical and quantum information processing.
C1 [Zhao, L.; Duan, Wenhui] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
[Zhao, L.; Duan, Wenhui] Tsinghua Univ, State Key Lab Low Dimens Quantum Phys, Beijing 100084, Peoples R China.
[Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
[Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Zhao, L (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China.
EM zhaol@phys.tsinghua.edu.cn
RI Duan, Wenhui /H-4992-2011
OI Duan, Wenhui /0000-0001-9685-2547
FU Ministry of Science and Technology of China [2011CB921901,
2011CB606405]; National Natural Science Foundation of China; NSF
FX L.Z. thanks F. Peng for helpful discussions. L.Z. and W. D. acknowledge
the financial support from the Ministry of Science and Technology of
China (Grant Nos. 2011CB921901 and 2011CB606405) and the National
Natural Science Foundation of China. S.F.Y. wants to thank the NSF for
funding.
NR 31
TC 7
Z9 7
U1 2
U2 13
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 SEP 7
PY 2011
VL 84
IS 3
AR 033806
DI 10.1103/PhysRevA.84.033806
PG 9
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 816YG
UT WOS:000294637400003
ER
PT J
AU Smith, DR
AF Smith, David R.
TI The Nearctic Oak-Feeding Sawflies of Periclista Subgenus Neocharactus
(Hymenoptera: Tenthredinidae
SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Blennocampinae; eastern North America; California; oaks; Quercus
ID HYMENOPTERA; SYMPHYTA
AB Eleven species of Periclista subg. Neocharactus MacGillivray are recognized in North America. Six species occur in eastern North America: P. (N.) absens, n. sp., P. (N.) asper, n. sp., P. (N.) inaequidens (Norton), P. (N.) major, n. sp., P. (N.) subtnmcata Dyar, and P. (N.) varia, n. sp. Five species are found only in California: P. (N.) bakeri (MacGillivray), P. (N.) curva, n. sp., P. (N.) pallipes (Provancher), P. (N.) parva, n. sp., and P. (N.) schiffi, n. sp. Known host plants are various species of oaks, Quercus spp. A key to species is provided, as well as descriptions and illustrations of each species.
C1 ARS, Systemat Entomol Lab, PSI, US Dept Agr,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, US Dept Agr,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM sawfly2@aol.com
NR 38
TC 1
Z9 1
U1 0
U2 1
PU AMER ENTOMOL SOC
PI PHILADELPHIA
PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA
SN 0002-8320
EI 2162-3139
J9 T AM ENTOMOL SOC
JI Trans. Am. Entomol. Soc.
PD SEP-DEC
PY 2011
VL 137
IS 3-4
BP 225
EP 250
PG 26
WC Entomology
SC Entomology
GA 978SB
UT WOS:000306765000001
ER
PT J
AU Nifong, JC
Frick, MG
AF Nifong, James C.
Frick, Michael G.
TI First Record of the American Alligator (Alligator mississippiensis) as a
Host to the Sea Turtle Barnacle (Chelonibia testudinaria)
SO SOUTHEASTERN NATURALIST
LA English
DT Article
ID MORELETS CROCODILE; PARASITES
AB Chelonibia testudinaria (Sea Turtle Barnacle) and other closely related barnacle species of the genus Chelonibia are known to utilize a variety of organisms for their attachment substrate. These include the calcified exoskeleton of marine crustaceans and chelicerids, the epidermis of manatees, and the carapace regions of all extant sea turtle species. Here, we present the first records of an Alligator mississippiensis (American Alligator; Alligatoridae) as a host for C. testudinaria.
C1 [Nifong, James C.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA.
RP Nifong, JC (reprint author), Univ Florida, Dept Biol, POB 118525, Gainesville, FL 32611 USA.
EM ncboy@ufl.edu
RI Nifong, James/D-4137-2015
OI Nifong, James/0000-0003-3607-0441
FU Estuarine Reserves Division, Office of Ocean and Coastal Resource
Management, National Ocean Service, National Oceanic and Atmospheric
Administration at the Guana Tolomato Matanzas Estuarine Research Reserve
Ponte Vedra, FL
FX These findings were produced while conducting research under an award
from the Estuarine Reserves Division, Office of Ocean and Coastal
Resource Management, National Ocean Service, National Oceanic and
Atmospheric Administration at the Guana Tolomato Matanzas Estuarine
Research Reserve Ponte Vedra, FL. Additionally, we thank Justin
Ellenberger, Tyler Mosteller (Guana River Wildlife Management Area), and
Kevin Torregrosa (St. Augustine Alligator Farm Zoological Park) for
assistance during alligator captures. All captures were performed under
FWC Special Use Permit # SPGS-10-43 and University of Florida IACUC
Permit # 201005071. Special thanks are due to two anonymous reviewers
and John D. Zardus for comments on this manuscript.
NR 7
TC 8
Z9 8
U1 0
U2 7
PU HUMBOLDT FIELD RESEARCH INST
PI STEUBEN
PA PO BOX 9, STEUBEN, ME 04680-0009 USA
SN 1528-7092
J9 SOUTHEAST NAT
JI Southeast. Nat.
PD SEP
PY 2011
VL 10
IS 3
BP 557
EP 560
DI 10.1656/058.010.0316
PG 4
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 976SY
UT WOS:000306606300016
ER
PT J
AU Cohen, CS
McCann, L
Davis, T
Shaw, L
Ruiz, G
AF Cohen, C. Sarah
McCann, Linda
Davis, Tammy
Shaw, Linda
Ruiz, Gregory
TI Discovery and significance of the colonial tunicate Didemnum vexillum in
Alaska
SO AQUATIC INVASIONS
LA English
DT Article
DE Didemnum vexillum; ascidian; nonindigenous species; genetic species
identification; citizen science; aquaculture; multilocus
ID HABITAT; CALIFORNIA; INVASIONS
AB The colonial tunicate, Didemnum vexillum Kott, 2002, has a history of invading and overgrowing marine communities in temperate waters worldwide. The species can colonize and dominate remarkably large areas of benthic habitat, including coastal bays and outer coastal areas, causing concerns about potential long-term effects on community structure, critical habitats, and fisheries resources. We report here the confirmed occurrence of D. vexillum in Alaska, representing a dramatic 1000 km northward extension of this non-native species along the western coast of North America. The species was detected as part of a " bioblitz", engaging citizen scientists to survey local biota and detect non-native marine species incursions. Following detection, the identity of D. vexillum was confirmed with robust genetic methods, and morphological characters were also consistent with previous species descriptions. Although invasions have been relatively rare in Alaskan waters to date, it is now clear that D. vexillum is established in at least one site (Whiting Harbor) near Sitka, Alaska. Given the explosive growth and spread of this species in other global regions, and its potential for significant impacts across diverse habitats in Alaska, current efforts are underway to evaluate its distribution and options to eradicate or control the species.
C1 [Cohen, C. Sarah] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA.
[Cohen, C. Sarah] San Francisco State Univ, Dept Biol, Tiburon, CA 94920 USA.
[McCann, Linda] Smithsonian Environm Res Ctr, Romberg Tiburon Ctr, Tiburon, CA 94920 USA.
[Davis, Tammy] Invas Species Program, Alaska Dept Fish & Game, Juneau, AK 99811 USA.
[Shaw, Linda] Natl Marine Fisheries Serv, Habitat Conservat Div, Juneau, AK 99802 USA.
[Ruiz, Gregory] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Cohen, CS (reprint author), San Francisco State Univ, Romberg Tiburon Ctr, 3150 Paradise Dr, Tiburon, CA 94920 USA.
EM sarahcoh@rtc.sfsu.edu; mccannl@si.edu; tammy.davis@alaska.gov;
Linda.Shaw@noaa.gov; ruizg@si.edu
OI Ruiz, Gregory/0000-0003-2499-441X
FU Alaska Department of Fish and Game, San Francisco State University, and
the Smithsonian Institution
FX We thank many people who helped in this research. Marnie Chapman and
Heather Woody assisted tirelessly in all aspects of this research.
Heather Woody also inspired us to undertake the bioblitz. Richard
Coleman and David Lake obtained genetic data at the SFSU RTC molecular
facility (NSF FSML award 0435033). John Stein provided lab space at the
Sitka Science Center, and Grant Miller provided access to Whiting
Harbor. Carolyn Bergstrom, Krissy Dunker, Jon Martin, Katharine Miller,
Ken Rear, David Tallmon, Sherry Tamone, and many others assisted in the
field surveys. Larry Harris and Benjamin Becker provided additional
samples from non-Alaskan regions for genetic analyses. Gretchen Lambert
examined morphological characters of Alaskan samples. This research was
supported by funding from Alaska Department of Fish and Game, San
Francisco State University, and the Smithsonian Institution.
NR 28
TC 12
Z9 13
U1 3
U2 27
PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC
PI HELSINKI
PA PL 3, HELSINKI, 00981, FINLAND
SN 1798-6540
EI 1818-5487
J9 AQUAT INVASIONS
JI Aquat. Invasions
PD SEP
PY 2011
VL 6
IS 3
BP 263
EP 271
DI 10.3391/ai.2011.6.3.03
PG 9
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 972LA
UT WOS:000306277400003
ER
PT J
AU Kam, Y
Schloder, C
Roche, DG
Torchin, ME
AF Kam, Yulang
Schloeder, Carmen
Roche, Dominique G.
Torchin, Mark E.
TI The Iraqi crab, Elamenopsis kempi in the Panama Canal: distribution,
abundance and interactions with the exotic North American crab,
Rhithropanopeus harrisii
SO AQUATIC INVASIONS
LA English
DT Article
DE Elamenopsis kempi; Rhithropanopeus harrisii; Panama Canal; introduced
species; biological invasions; predation
ID BIOLOGY
AB We report on the distribution and abundance of the Iraqi crab Elamenopsis kempi in the Panama Canal and investigate possible interactions of this species with another invader, the North American mud crab, Rhithropanopeus harrisii. While more widespread than R. harrisii, E. kempi is currently limited to four locations within the Canal area: the Miraflores Lake, the Miraflores Spillway, the Southern Lagoon and the Northern Lagoon. Crabs reached peak abundances November through February. Where the two crab species overlap, the abundance of E. kempi was negatively associated with that of R. harrisii. Average E. kempi densities were significantly higher in cores with vegetation than those without vegetation. Laboratory experiments indicated that R. harrisii readily eats E. kempi, but that the presence of aquatic vegetation reduces predation rates. After four days, all E. kempi in treatments without vegetation were eaten, whereas only 53% of crabs were eaten in treatments with vegetation. Elamenopsis kempi is a small cryptic crab that can be easily overlooked even when abundant, suggesting that it may be more widespread than is currently reported.
C1 [Kam, Yulang; Schloeder, Carmen; Roche, Dominique G.; Torchin, Mark E.] Smithsonian Trop Res Inst, Panama City, Panama.
[Roche, Dominique G.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM yulang_0184k@hotmail.com; schloederc@si.edu; dominique.roche@anu.edu.au;
torchinm@si.edu
RI Roche, Dominique/K-7426-2012;
OI Roche, Dominique/0000-0002-3326-864X
FU Secretaria Nacional de Ciencia, Tecnologia y Innovacion de Panama
(SENACYT); Smithsonian Tropical Research Institute; Smithsonian Marine
Science Network
FX We are grateful to the Autoridad del Canal de Panama for granting access
to restricted sites in the Canal and to M. Calderon, F. O. Guardia, H.
Broce and D. Muschett for providing comments on the manuscript,
assistance in the field as well as information on the Panama Canal. We
thank O. Miura, C. Mabin and M. Strader for help in the field and M.
Sytsma for plant species identification. J. Carlton and two anonymous
reviewers provided useful comments on the manuscript. We acknowledge the
Secretaria Nacional de Ciencia, Tecnologia y Innovacion de Panama
(SENACYT), Smithsonian Tropical Research Institute and Smithsonian
Marine Science Network for financial support. We acknowledge the
Autoridad Nacional del Ambiente de Panama and the Autoridad de Recursos
Acuaticos de Panama for providing applicable permits in Panama.
NR 13
TC 0
Z9 0
U1 2
U2 16
PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC
PI HELSINKI
PA PL 3, HELSINKI, 00981, FINLAND
SN 1798-6540
EI 1818-5487
J9 AQUAT INVASIONS
JI Aquat. Invasions
PD SEP
PY 2011
VL 6
IS 3
BP 339
EP 345
DI 10.3391/ai.2011.6.3.10
PG 7
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 972LA
UT WOS:000306277400010
ER
PT J
AU Crouch, TD
AF Crouch, Tom D.
TI The Aeronautic Society of New York and the Birth of American Aviation,
1908-1918
SO NEW YORK HISTORY
LA English
DT Article
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 27
TC 0
Z9 0
U1 0
U2 1
PU NEW YORK STATE HIST ASSOC
PI COOPERSTOWN
PA PO BOX 800, COOPERSTOWN, NY 13326-0800 USA
SN 0146-437X
J9 NEW YORK HIST
JI N. Y. Hist.
PD FAL
PY 2011
VL 92
IS 4
BP 269
EP 289
PG 21
WC History
SC History
GA 959HZ
UT WOS:000305304800003
ER
PT J
AU Goddard, I
AF Goddard, Ives
TI First Manhattans: A Brief History of the Munsee Indians
SO NEW YORK HISTORY
LA English
DT Book Review
C1 [Goddard, Ives] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
RP Goddard, I (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
NR 27
TC 1
Z9 1
U1 0
U2 1
PU NEW YORK STATE HIST ASSOC
PI COOPERSTOWN
PA PO BOX 800, COOPERSTOWN, NY 13326-0800 USA
SN 0146-437X
J9 NEW YORK HIST
JI N. Y. Hist.
PD FAL
PY 2011
VL 92
IS 4
BP 290
EP 302
PG 13
WC History
SC History
GA 959HZ
UT WOS:000305304800004
ER
PT J
AU Zatwarnicki, T
Mathis, WN
AF Zatwarnicki, Tadeusz
Mathis, Wayne N.
TI Heterogeneity in shore flies - the case of Glenanthe Haliday (Diptera:
Ephydridae) in the Old World
SO ANNALES DE LA SOCIETE ENTOMOLOGIQUE DE FRANCE
LA English
DT Article
DE Systematic; revision; new species; male terminalia
ID COQUILLETT DIPTERA; GENUS; FLY; REVISION
AB Old World species of the genus Glenanthe are treated comprehensively with an emphasis on the unusually diverse morphological heterogeneity discovered in structures of the male terminalia. As perspective for this treatment, the tribe Lipochaetini, in which Glenanthe is placed, is characterized and discussed, and an annotated key to the four included genera is provided to facilitate their identification. Glenanthe is demonstrated to be a monophyletic lineage within Lipochaetini. Seven Old World species of Glenanthe are now known, including two new Afrotropical species as follows (type locality in parenthesis): G. namibia n. sp. (Namibia. Mukwe: Divuju: Okavango River [18 degrees 04'04 '' S, 21 degrees 28'51 '' E] and G. danielssoni n. sp. (Republic of South Africa. Cape Province: De Hoop Nature Reserve [34 degrees 27'S, 28 degrees 25'E]. The identity of G. fuscinervis Becker, revised status (raised from synonymy with G. ripicola (Haliday)), is clarified, and found to be conspecific with Hydrina ochracea Oldenberg, which is recognized as a junior synonym. Papp's synonymy of Glenanthe fasciventris Becker with Hydretlia (Glenanthe) ripicola Haliday is confirmed, and herein we relegate G. iranica Canzoneri & Rampini also as junior synonym of G. ripicola, The remarkable diverse structures of the male terminalia of all included species are described and illustrated and distribution maps are also provided.
C1 [Zatwarnicki, Tadeusz] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland.
[Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, MRC 169, Washington, DC 20013 USA.
RP Zatwarnicki, T (reprint author), Opole Univ, Dept Biosystemat, Ul Oleska 22, PL-45052 Opole, Poland.
EM zatwar@uni.opole.pl; mathisw@si.edu
OI Zatwarnicki, Tadeusz/0000-0003-2163-0143
FU Research Opportunity Fund; National Museum of Natural History; European
Commission [HU TAF 4730]
FX Typical of comprehensive studies, the assistance of many people and
institutions has contributed significantly to the final production and
publication of this study, and we gratefully acknowledge and thank all
who have assisted. In particular we thank the following institutions and
their respective curators for the loan of specimens: Daniel J. Bickel
and David K. McAlpine (AM), Jon K. Gelhaus and Jason D. Weintraub
(ANSP), Brian Pitkin, John E. Chainey, and Nigel Wyatt (BMNH), Frank
Menzel (DEI), Laszlo Papp (HNHM), Patrick Grootaert (IRSN), Lorenzo
Munari, Enrico Ratti, and Marco Uliana (MCV), Bernhard Merz (MHNG),
Christophe Daugeron (MNHN), James P. O'Connor (NMI), Eliane De Coninck
(MRAC), Luca Picciau (MRSN), Peter Sehnal (NMW), Bert Vicklund and Kevin
C. Holston (NRS), Hans-Peter Tschorsnig (SMN), Amnon Freidberg (TAU),
Thomas Pape (NRS and UZMC), Rudolf Meier (UZMC), Pekka Vilkamaa (UZMH),
Roy Danielsson (ZIL), Hans Mejlon (ZIU), Ben Bruge and Hermann de Jong
(ZMA), Joachim Ziegler (ZMHU), and Venelin L. Beschovski (ZMS). The late
H.B. Williams initially prepared the distribution maps, which were
augmented and finalized by Karolyn Darrow and Joaquin Mengual. We thank
them both. Lorenzo Munari kindly provided geographic coordinates for
Italian localities and Nigel Wyatt for localities in the United Kingdom.
For reviewing an early draft of this paper, we thank Allen L. Norrbom
and Anthony G. Irwin. We are also grateful to David Challinor
(deceased), former Assistant Secretary for Research, Smithsonian
Institution, and Stanwyn G. Shetler, former Deputy Director of the
National Museum of Natural History, for financial support to conduct
field work and study primary types through grants from the Research
Opportunity Fund. Our work in several museums of Europe in 2005 was
supported by the Small Grants Program (Biological Surveys and
Inventories, BSI), National Museum of Natural History. We also
acknowledge the financial support of the European Commission's Research
Infrastructure Action (the SYNTHESYS Project No. HU TAF 4730).
NR 47
TC 0
Z9 1
U1 0
U2 1
PU SOC ENTOMOLOGIQUE FRANCE
PI PARIS
PA 45 RUE BUFFON, 75005 PARIS, FRANCE
SN 0037-9271
EI 2168-6351
J9 ANN SOC ENTOMOL FR
JI Ann. Soc. Entomol. Fr.
PD SEP-DEC
PY 2011
VL 47
IS 3-4
BP 418
EP 443
PG 26
WC Entomology
SC Entomology
GA 922AP
UT WOS:000302519500016
ER
PT J
AU Knee, KL
Garcia-Solsona, E
Garcia-Orellana, J
Boehm, AB
Paytan, A
AF Knee, Karen L.
Garcia-Solsona, Ester
Garcia-Orellana, Jordi
Boehm, Alexandria B.
Paytan, Adina
TI Using radium isotopes to characterize water ages and coastal mixing
rates: A sensitivity analysis
SO LIMNOLOGY AND OCEANOGRAPHY-METHODS
LA English
DT Article
ID SUBMARINE GROUNDWATER DISCHARGE; NATURAL GEOCHEMICAL TRACERS; FECAL
INDICATOR BACTERIA; RESIDENCE TIME; SURF ZONE; NEW-YORK; CONTAMINATED
GROUNDWATER; SUBTERRANEAN ESTUARY; NUTRIENT DISCHARGE; DIFFUSION
DIAGRAMS
AB Numerous studies have used naturally occurring Ra isotopes (Ra-223, Ra-224, Ra-226, and Ra-228, with half-lives of 11.4 d, 3.7 d, 1600 y, and 5.8 y, respectively) to quantify water mass ages, coastal ocean mixing rates, and submarine groundwater discharge (SGD). Using Monte Carlo models, this study investigated how uncertainties in Ra isotope activities and the derived activity ratios (AR) arising from analytical uncertainty and natural variability affect the uncertainty associated with Ra-derived water ages and eddy diffusion coefficients, both of which can be used to calculate SGD. Analytical uncertainties associated with Ra-224, Ra-226, and Ra-228 activities were reported in most published studies to be less than 10% of sample activity; those reported for Ra-223 ranged from 7% to 40%. Relative uncertainty related to natural variability-estimated from the variability in Ra-223 and Ra-224 activities of replicate field samples-ranged from 15% to 50% and was similar for Ra-223 activity, Ra-224 activity, and the Ra-224/Ra-223 AR. Our analysis revealed that AR-based water ages shorter than 3-5 d often have relative uncertainties greater than 100%, potentially limiting their utility. Uncertainties in eddy diffusion coefficients estimated based on cross-shore gradients in short-lived Ra isotope activity were greater when fewer points were used to determine the linear trend, when the coefficient of determination (R-2) was low, and when Ra-224, rather than Ra-223, was used. By exploring the uncertainties associated with Ra-derived water ages and eddy diffusion coefficients, this study will enable researchers to apply these methods more effectively and to reduce uncertainty.
C1 [Knee, Karen L.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA.
[Garcia-Solsona, Ester] Lab Etud Geophys & Oceanog Spatiales LEGOS OMP, Toulouse, France.
[Garcia-Solsona, Ester; Garcia-Orellana, Jordi] Univ Autonoma Barcelona, Dept Fis, Inst Ciencia & Tecnol Ambientals, E-08193 Barcelona, Spain.
[Boehm, Alexandria B.] Stanford Univ, Dept Civil & Environm Engn, Stanford, CA 94305 USA.
[Paytan, Adina] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA.
RP Knee, KL (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM kneek@si.edu
RI Garcia-Solsona, Ester/C-7029-2008; Garcia-Orellana, Jordi/L-7758-2014
OI Garcia-Solsona, Ester/0000-0003-4136-9165; Garcia-Orellana,
Jordi/0000-0002-0543-2641
NR 78
TC 8
Z9 8
U1 2
U2 19
PU AMER SOC LIMNOLOGY OCEANOGRAPHY
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA
SN 1541-5856
J9 LIMNOL OCEANOGR-METH
JI Limnol. Oceanogr. Meth.
PD SEP
PY 2011
VL 9
BP 380
EP 395
DI 10.4319/lom.2011.9.380
PG 16
WC Limnology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 893TE
UT WOS:000300377600003
ER
PT J
AU Nielsen, M
Buffington, M
AF Nielsen, M.
Buffington, M.
TI Redescription of Stentorceps Quinlan, 1984 (Hymenoptera: Figitidae),
with a description of five new species
SO AFRICAN ENTOMOLOGY
LA English
DT Article
DE revision; parasitoid; Trichoplastini; Afrotropical
ID EUCOILINAE HYMENOPTERA; CYNIPOIDEA; GENUS; REVISION; PHYLOGENY; DIPTERA;
GENERA
AB The Afrotropical eucoiline genus Stentorceps, described in 1984, has remained monotypic until now. Stentorceps is herein redescribed using recent field collections from Kenya and Madagascar. Stentorceps tubicen Quinlan is redescribed, and the new species S. abbotti, S. heimdalli, S. vuvuzela, S. weedlei and S. zuparkoi are described. Stentorceps heimdalli, S. weedlei and S. zuparkoi extend the range of Stentorceps to Nigeria, Madagascar, Rwanda, Somalia and South Africa. The descriptions and keys provide a foundation for future taxonomic and biological investigations.
C1 [Buffington, M.] Smithsonian Inst, Systemat Entomol Lab, ARS USDA, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Nielsen, M.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
RP Buffington, M (reprint author), Smithsonian Inst, Systemat Entomol Lab, ARS USDA, Natl Museum Nat Hist, 10th & Constitut Ave, Washington, DC 20560 USA.
EM matt.buffington@ars.usda.gov
FU National Science Foundation [DEB-0072713, DEB-0344731]; SEM Lab,
National Museum of Natural History, Washington, D.C; National Museum of
Natural History
FX We thank R. Bagine, Director of Research, Kenya Wildlife Service for
granting R.S. Copeland permission to sample in Kenyan National Parks and
Reserves. H. Oyieke, Head of Collections and Research, National Museums
of Kenya, was instrumental in granting permission to loan insects for
study. This work was partially supported by the National Science
Foundation under Grant No. DEB-0072713 to B.L. Fisher and C.E. Griswold
and DEB-0344731 to B.L. Fisher and P.S. Ward. Fieldwork in Madagascar
that provided the basis for part of this work could not have been
completed without the gracious support of the Malagasy people. R.
Zuparko and B. Fisher (CAS) provided specimens from Madagascar. At The
Natural History Museum (London), D. Notton provided loans of S. tubicen
type specimens from the collection, and A. Polaszek assisted M.
Buffington with conducting research. L. Masner and J. Read (CNCI)
generously loaned specimens that greatly expanded the known range of
Stentorceps. S. Whittaker (SEM Lab, National Museum of Natural History,
Washington, D.C.) provided SEM training and support for M. Nielsen. M.
Pogue, T. Henry (Systematic Entomology Laboratory, ARS/USDA, Washington,
D.C.), L. Masner (Canadian National Collection of Insects, Ottawa,
Canada), M. Forshage (Department of Entomology, Swedish Museum of
Natural History, Stockholm, Sweden) and S. van Noort (Iziko South
African Museum, Cape Town, South Africa) provided extremely useful
comments on earlier drafts of this manuscript. We would also like to
thank E. Cottrell, G. Hunt and V. Power (programme coordinators, Natural
History Research Experience Program, National Museum of Natural History)
for running the 2010 NHRE program, and C. Samper (National Museum of
Natural History) for providing funding.
NR 27
TC 6
Z9 6
U1 0
U2 2
PU ENTOMOLOGICAL SOC SOUTHERN AFRICA
PI HATFIELD
PA PO BOX 13162, HATFIELD 0028, SOUTH AFRICA
SN 1021-3589
EI 1026-4914
J9 AFR ENTOMOL
JI Afr. Entomol.
PD SEP
PY 2011
VL 19
IS 3
BP 597
EP 613
PG 17
WC Entomology
SC Entomology
GA 881CV
UT WOS:000299459000005
ER
PT J
AU McClintock, JB
Amsler, MO
Angus, RA
Challener, RC
Schram, JB
Amsler, CD
Mah, CL
Cuce, J
Baker, BJ
AF McClintock, James B.
Amsler, Margaret O.
Angus, Robert A.
Challener, Roberta C.
Schram, Julie B.
Amsler, Charles D.
Mah, Christopher L.
Cuce, Jason
Baker, Bill J.
TI The Mg-Calcite Composition of Antarctic Echinoderms: Important
Implications for Predicting the Impacts of Ocean Acidification
SO JOURNAL OF GEOLOGY
LA English
DT Article
ID MAGNESIAN CALCITE; CLIMATE-CHANGE; SEA-FLOOR; WATER; PH; PERMEABILITY;
TEMPERATURE; ECHINOIDEA; CARBON; LIFE
AB The Southern Ocean is considered to be the canary in the coal mine with respect to the first effects of ocean acidification (OA). This vulnerability is due to naturally low carbonate ion concentrations that result from the effect of low temperature on acid-base dissociation coefficients, from the high solubility of CO 2 at low temperature, and from ocean mixing. Consequently, the two calcium carbonate polymorphs, aragonite and calcite, are expected to become undersaturated in the Southern Ocean within 50 and 100 years, respectively. Marine invertebrates such as echinoderms, whose skeletons are classified as high-magnesium carbonate (>4% mol MgCO3), are even more vulnerable to OA than organisms whose skeletons consist primarily of aragonite or calcite, with respect to both increased susceptibility to skeletal dissolution and further challenge to their production of skeletal elements. Currently, despite their critical importance to predicting the effects of OA, there is almost no information on the Mg-calcite composition of Antarctic echinoderms, a group known to be a major contributor to the global marine carbon cycle. Here we report the Mg-calcite compositions of 26 species of Antarctic echinoderms, representing four classes. As seen in tropical and temperate echinoderms, Mg-calcite levels varied with taxonomic class, with sea stars generally having the highest levels. When combined with published data for echinoderms from primarily temperate and tropical latitudes, our findings support the hypothesis that Mg-calcite level varies inversely with latitude. Sea stars and brittle stars, key players in Antarctic benthic communities, are likely to be the first echinoderms to be challenged by near-term OA.
C1 [McClintock, James B.; Amsler, Margaret O.; Angus, Robert A.; Challener, Roberta C.; Schram, Julie B.; Amsler, Charles D.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA.
[Mah, Christopher L.] Smithsonian Inst, Museum Nat Hist, Washington, DC 20013 USA.
[Cuce, Jason; Baker, Bill J.] Univ S Florida, Dept Chem, Tampa, FL 33620 USA.
RP McClintock, JB (reprint author), Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA.
EM mcclinto@uab.edu
OI Amsler, Charles/0000-0002-4843-3759
FU National Science Foundation [ANT-0838773, ANT-0838776]; University of
Alabama at Birmingham
FX We wish to acknowledge the outstanding assistance provided by Raytheon
Polar Service support staff at Palmer Station, Antarctica. We also thank
H. W. Dietrich for so generously facilitating access to his ship-based
trawling operations along the western Antarctic Peninsula. C. Mooi and
M. O'Laughlin generously provided assistance with taxonomy. E. Hofmann
of Actlabs kindly provided valuable input on assay protocols. This work
was supported by National Science Foundation awards ANT-0838773 to C. D.
Amsler and J. B. McClintock and ANT-0838776 to B. J. Baker. J. B.
McClintock acknowledges the support of an Endowed Professorship in Polar
and Marine Biology provided by the University of Alabama at Birmingham.
We appreciate the helpful editorial comments and insights of two
anonymous reviewers.
NR 42
TC 30
Z9 30
U1 2
U2 43
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 SEP
PY 2011
VL 119
IS 5
BP 457
EP 466
DI 10.1086/660890
PG 10
WC Geology
SC Geology
GA 878PP
UT WOS:000299269300002
ER
PT J
AU Siler, CD
Crombie, RI
Diesmos, AC
Brown, RM
AF Siler, Cameron D.
Crombie, Ronald I.
Diesmos, Arvin C.
Brown, Rafe M.
TI Redescriptions of Two Poorly Known Slender Skinks, Brachymeles bicolor
and Brachymeles pathfinderi (Reptilia: Squamata: Scincidae), from the
Philippines
SO JOURNAL OF HERPETOLOGY
LA English
DT Article
ID LOAM-SWIMMING SKINK; LUZON ISLAND; BODY-FORM; PHYLOGENY; EVOLUTION;
PATTERNS
AB Brachymeles bicolor (Gray 1845), from the Sierra Madre Mountain Range of Luzon Island, and Brachymeles pathfinderi Taylor 1925, from southern Mindanao Island, are among the most distinctive species in the genus, representing the largest species and one of only two known nonpentadactyl species with unequal digit numbers respectively. However, both species are inadequately diagnosed, based on a total of only five specimens. Here we provide brief taxonomic histories, discuss and clarify type localities, and redescribe each species using larger sample sizes and specimens well documented and collected during our recent biodiversity surveys. We include new information on morphological variation, distribution, ecology, and microhabitat.
C1 [Siler, Cameron D.; Brown, Rafe M.] Univ Kansas, Dept Ecol & Evolutionary Biol, Nat Hist Museum, Lawrence, KS 66045 USA.
[Siler, Cameron D.; Brown, Rafe M.] Univ Kansas, Dept Ecol & Evolutionary Biol, Biodivers Inst, Lawrence, KS 66045 USA.
[Crombie, Ronald I.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
[Diesmos, Arvin C.] Natl Museum Philippines, Div Zool, Herpetol Sect, Manila, Philippines.
RP Siler, CD (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Nat Hist Museum, Lawrence, KS 66045 USA.
EM camsiler@ku.edu; rafe@ku.edu
FU University of Kansas Biodiversity Institute; University of Kansas;
Fulbright-Hayes Fellowship; NSF [DEB 0804115, EF-0334952, DEB 0743491];
CAS; MCZ
FX We thank the Protected Areas and Wildlife Bureau (PAWB) of the
Philippine Department of Environment and Natural Resources (DENR) for
facilitating collecting and export permits necessary for this and
related studies, wherein we are particularly grateful to M. Lim, C.
Custodio, J. L. De Leon, and A. Tagtag. Financial support for fieldwork
for CDS was provided by a Panorama Fund grant from the University of
Kansas Biodiversity Institute, a Madison and Lila Self Fellowship from
the University of Kansas, a Fulbright-Hayes Fellowship, and NSF DEB
0804115. Financial support for RMB and ACD provided by NSF EF-0334952
and DEB 0743491 funds to RMB. For the loans of specimens, we thank J.
Vindum, R. Drewes, and A. Leviton (CAS); V. Papallatoc and C. Alvina
(PNM); J. Ferner (CMNH); A. Resetar and H. Voris (FMNH); K. de Queiroz
(USNM); and T. LaDuc (TNHC). Critical reviews of the manuscript were
provided by J. Esselstyn and two anonymous reviewers. CDS gratefully
acknowledges CAS's Stearns Fellowship and the MCZ Ernst Mayr's
Fellowship for funding recent visits to examine comparative material.
NR 43
TC 8
Z9 9
U1 1
U2 3
PU SOC STUDY AMPHIBIANS REPTILES
PI ST LOUIS
PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST
LOUIS, MO 63103 USA
SN 0022-1511
EI 1937-2418
J9 J HERPETOL
JI J. Herpetol.
PD SEP
PY 2011
VL 45
IS 3
BP 355
EP 369
PG 15
WC Zoology
SC Zoology
GA 853TG
UT WOS:000297448000018
ER
PT J
AU LaDeau, SL
Calder, CA
Doran, PJ
Marra, PP
AF LaDeau, Shannon L.
Calder, Catherine A.
Doran, Patrick J.
Marra, Peter P.
TI West Nile virus impacts in American crow populations are associated with
human land use and climate
SO ECOLOGICAL RESEARCH
LA English
DT Article
DE Anthropogenic; Avian; Land use; Pathogen; West Nile virus
ID NORTHEASTERN UNITED-STATES; TRANSMISSION DYNAMICS;
CORVUS-BRACHYRHYNCHOS; HUMAN FOOTPRINT; RISK-FACTORS; NEW-YORK; ECOLOGY;
DISEASE; EPIDEMIOLOGY; PREVALENCE
AB West Nile virus (WNV) was first detected in the western hemisphere during the summer of 1999, reawakening US public awareness of the potential severity of vector-borne pathogens. Since its New World introduction, WNV has caused disease in human, avian, and mammalian communities across the continent. American crows (Corvus brachyrhynchos) are a highly susceptible WNV host and when modeled appropriately, changes in crow abundances can serve as a proxy for the spatio-temporal presence of WNV. We use the dramatic declines in abundance of this avian host to examine spatio-temporal heterogeneity in WNV intensity across the northeastern US, where WNV was first detected. Using data from the Breeding Bird Survey, we identify significant declines in crow abundance after WNV emergence that are associated with lower forest cover, more urban land use, and warmer winter temperatures. Importantly, we document continued declines as WNV was present in an area over consecutive years. Our findings support the urban-pathogen link that human WNV incidence studies have shown. For each 1% increase in urban land cover we expect an additional 5% decline in the log crow abundance beyond the decline attributed to WNV in undeveloped areas. We also demonstrate a significant relationship between above-average winter temperatures and WNV-related declines in crow abundance. The mechanisms behind these patterns remain uncertain and hypotheses requiring further research are suggested. In particular, a strong positive relationship between urban land cover and winter temperatures may confound mechanistic understanding, especially when a temperature-sensitive vector is involved.
C1 [LaDeau, Shannon L.] Cary Inst Ecosyst Studies, Millbrook, NY 12545 USA.
[LaDeau, Shannon L.; Marra, Peter P.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[Calder, Catherine A.] Ohio State Univ, Dept Stat, Columbus, OH 43228 USA.
[Doran, Patrick J.] Nature Conservancy, Lansing, MI 48906 USA.
RP LaDeau, SL (reprint author), Cary Inst Ecosyst Studies, Millbrook, NY 12545 USA.
EM ladeaus@ecostudies.org
OI Calder, Catherine/0000-0002-4459-1418; LaDeau,
Shannon/0000-0003-4825-5435
FU National Science Foundation (NSF); Nature Conservancy
FX The authors wish to thank the dedicated volunteers that keep the
Breeding Bird Survey active in North America. SLL thanks Dr. Zen
Kawabata for the opportunity to present at the 2008 Kyoto symposium on
'Environmental Change, Pathogens and Human Linkages'. PJD was supported
by The Nature Conservancy's Great Lakes Fund for Partnership in
Conservation Science and Economics. SLL was supported by the National
Science Foundation (NSF) Program in Bioinformatics for part of this
research. This paper is a contribution to the program of the Cary
Institute of Ecosystem Studies.
NR 58
TC 12
Z9 12
U1 4
U2 56
PU SPRINGER TOKYO
PI TOKYO
PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN
SN 0912-3814
J9 ECOL RES
JI Ecol. Res.
PD SEP
PY 2011
VL 26
IS 5
SI SI
BP 909
EP 916
DI 10.1007/s11284-010-0725-z
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 850OD
UT WOS:000297204000007
ER
PT J
AU Solis, MA
Metz, MA
AF Solis, M. Alma
Metz, M. A.
TI Male genital homology based on musculature originating from the tegumen
in snout moths (Lepidoptera: Pyraloidea)
SO ARTHROPOD STRUCTURE & DEVELOPMENT
LA English
DT Article
DE Genitalia; Gnathos; Uncus; Comparative morphology; Pyralidae; Crambidae
ID PYRALIDAE
AB The homology and terminology of the sclerotized structures, specifically the uncus and gnathos, formed by the fused segments caudal to the ninth abdominal segment in males of Lepidoptera, specifically in the Pyraloidea, have been confused in the literature. Based on comparative morphology of sclerotized structures and musculature, the uncus, scaphium, gnathos, and subscaphium are defined and described for stabilization in future systematic studies. Muscles IX-X (ex) and IX-X (int) are associated with these sclerotized structures and attached to the tegumen anteriorly. They are present in most of the species examined and are consistently topologically constrained in their origins and insertions; no differences were observed at the familial level. Muscle IX-X (int) is lacking in Pyralinae (Pyralidae) and this condition is hypothesized to be derived independently and an autapomorphy for this subfamily. The unique subteguminal processes of the Schoenobiinae are structures independent of the gnathos contrary to previous thought, and are instead associated with the valvae. Published by Elsevier Ltd.
C1 [Solis, M. Alma; Metz, M. A.] ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst,SEL, Washington, DC 20013 USA.
RP Solis, MA (reprint author), ARS, Systemat Entomol Lab, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst,SEL, POB 37012,E-517,MRC 168, Washington, DC 20013 USA.
EM alma.solis@ars.usda.gov; mark.metz@ars.usda.gov
NR 40
TC 4
Z9 4
U1 0
U2 2
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1467-8039
J9 ARTHROPOD STRUCT DEV
JI Arthropod Struct. Dev.
PD SEP
PY 2011
VL 40
IS 5
BP 435
EP 448
DI 10.1016/j.asd.2011.03.005
PG 14
WC Entomology
SC Entomology
GA 832OQ
UT WOS:000295814700006
ER
PT J
AU Falcon-Lang, HJ
Heckel, PH
Dimichele, WA
Blake, BM
Easterday, CR
Eble, CF
Elrick, S
Gastaldo, RA
Greb, SF
Martino, RL
Nelson, WJ
Pfefferkorn, HW
Phillips, TL
Rosscoe, SJ
AF Falcon-Lang, Howard J.
Heckel, Philip H.
Dimichele, William A.
Blake, Bascombe M., Jr.
Easterday, Cary R.
Eble, Cortland F.
Elrick, Scott
Gastaldo, Robert A.
Greb, Stephen F.
Martino, Ronald L.
Nelson, W. John
Pfefferkorn, Hermann W.
Phillips, Tom L.
Rosscoe, Steven J.
TI NO MAJOR STRATIGRAPHIC GAP EXISTS NEAR THE MIDDLE-UPPER PENNSYLVANIAN
(DESMOINESIAN-MISSOURIAN) BOUNDARY IN NORTH AMERICA: PALAIOS, v. 26, no.
3, p. 125-139, 2011 REPLY
SO PALAIOS
LA English
DT Editorial Material
C1 [Falcon-Lang, Howard J.] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England.
[Heckel, Philip H.] Univ Iowa, Dept Geosci, Iowa City, IA 52242 USA.
[Dimichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Blake, Bascombe M., Jr.] W Virginia Geol Survey, Morgantown, WV 26508 USA.
[Easterday, Cary R.] NE Illinois Univ, Dept Earth Sci, Chicago, IL 60625 USA.
[Eble, Cortland F.; Greb, Stephen F.] Univ Kentucky, Kentucky Geol Survey, Lexington, KY 40506 USA.
[Elrick, Scott; Nelson, W. John] Illinois State Geol Survey, Champaign, IL 61820 USA.
[Gastaldo, Robert A.] Colby Coll, Dept Geol, Waterville, ME 04901 USA.
[Martino, Ronald L.] Marshall Univ, Dept Geol, Huntington, WV 25701 USA.
[Pfefferkorn, Hermann W.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
[Phillips, Tom L.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
[Rosscoe, Steven J.] Hardin Simmons Univ, Dept Geol Sci, Abilene, TX 79698 USA.
RP Falcon-Lang, HJ (reprint author), Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England.
EM h.falcon-lang@es.rhul.ac.uk; philip-heckel@uiowa.edu; dimichel@si.edu;
blake@geosrv.wvnet.edu; c-easterday@neiu.edu; eble@uky.edu;
elrick@isgs.illinois.edu; ragastal@colby.edu; stephen.greb@uky.edu;
jnelson@isgs.illinois.edu; hpfeffer@sas.upenn.edu;
tlphilli@life.uiuc.edu; srosscoe@hsutx.edu
RI DiMichele, William/K-4301-2012
NR 0
TC 0
Z9 0
U1 0
U2 3
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 SEP-OCT
PY 2011
VL 26
IS 9-10
BP 671
EP 671
DI 10.2110/palo.2011.p11-055r
PG 1
WC Geology; Paleontology
SC Geology; Paleontology
GA 835NL
UT WOS:000296043000015
ER
PT J
AU Fletcher, L
Dennis, BR
Hudson, HS
Krucker, S
Phillips, K
Veronig, A
Battaglia, M
Bone, L
Caspi, A
Chen, Q
Gallagher, P
Grigis, PT
Ji, H
Liu, W
Milligan, RO
Temmer, M
AF Fletcher, L.
Dennis, B. R.
Hudson, H. S.
Krucker, S.
Phillips, K.
Veronig, A.
Battaglia, M.
Bone, L.
Caspi, A.
Chen, Q.
Gallagher, P.
Grigis, P. T.
Ji, H.
Liu, W.
Milligan, R. O.
Temmer, M.
TI An Observational Overview of Solar Flares
SO SPACE SCIENCE REVIEWS
LA English
DT Review
DE Sun
ID HARD X-RAY; CORONAL MASS EJECTION; WHITE-LIGHT FLARES; PHOTOSPHERIC
MAGNETIC-FIELD; HIGH TIME RESOLUTION; LOOP RADIATIVE HYDRODYNAMICS;
QUIET ACTIVE REGIONS; 2003 OCTOBER 29; GENTLE CHROMOSPHERIC EVAPORATION;
ENERGETIC PARTICLE EVENTS
AB We present an overview of solar flares and associated phenomena, drawing upon a wide range of observational data primarily from the RHESSI era. Following an introductory discussion and overview of the status of observational capabilities, the article is split into topical sections which deal with different areas of flare phenomena (footpoints and ribbons, coronal sources, relationship to coronal mass ejections) and their interconnections. We also discuss flare soft X-ray spectroscopy and the energetics of the process. The emphasis is to describe the observations from multiple points of view, while bearing in mind the models that link them to each other and to theory. The present theoretical and observational understanding of solar flares is far from complete, so we conclude with a brief discussion of models, and a list of missing but important observations.
C1 [Fletcher, L.; Battaglia, M.] Univ Glasgow, Sch Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland.
[Dennis, B. R.; Liu, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Milligan, R. O.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland.
[Hudson, H. S.; Krucker, S.; Caspi, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
[Phillips, K.; Bone, L.] Mullard Space Sci Lab, Dorking RH5 CNT, Surrey, England.
[Veronig, A.] Graz Univ, Inst Geophys Astrophys & Meteorol, A-8010 Graz, Austria.
[Temmer, M.] Graz Univ, Inst Phys, A-8010 Graz, Austria.
[Chen, Q.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Gallagher, P.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland.
[Grigis, P. T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ji, H.] Purple Mt Observ, Nanjing 210008, Peoples R China.
[Ji, H.] New Jersey Inst Technol, Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Liu, W.] Stanford Lockheed Inst Space Res, Stanford, CA 94305 USA.
RP Fletcher, L (reprint author), Univ Glasgow, Sch Phys & Astron, Astron & Astrophys Grp, Glasgow G12 8QQ, Lanark, Scotland.
EM lyndsay.fletcher@glasgow.ac.uk
RI Dennis, Brian/C-9511-2012; Veronig, Astrid/B-8422-2009; Gallagher,
Peter/C-7717-2011;
OI Gallagher, Peter/0000-0001-9745-0400; Battaglia,
Marina/0000-0003-1438-9099; Caspi, Amir/0000-0001-8702-8273; Temmer,
Manuela/0000-0003-4867-7558
FU UK STFC [ST/F0026371]; EU [MTRN-CT-2006-035484]; Leverhulme Foundation
[F/00 179/AY]; NSFC [10833007W]; NASA at Goddard Space Flight Center;
Hinode SOT [NNM07AA01C]; NASA [NAS5-98033, NAG5-12878, NNX08AJ18G];
Austrian Science Fund (FWF) [P20867-N16, P20145-N16]
FX The authors would collectively like to acknowledge the work by the many
instrument teams and software teams, whose sustained efforts over the
years have made this kind of multiwavelength analysis possible. The
chief architects of and major contributors to the Solarsoft library
deserve particular thanks (Sam Freeland, Richard Schwartz, William
Thompson, Kim Tolbert and Dominic Zarro). L. F. would like to
acknowledge financial support from the UK STFC (Rolling grant
ST/F0026371), the EU's SOLAIRE Research and Training Network
(MTRN-CT-2006-035484) and L. F. and M. B. also acknowledge the support
of the Leverhulme Foundation (Grant F/00 179/AY). The work of H. Ji was
supported by NSFC 10833007W. W. Liu was partly supported by an
appointment to the NASA Postdoctoral Program at Goddard Space Flight
Center, administered by Oak Ridge Associated Universities through a
contract with NASA. Partial support to W. Liu's work was also provided
by Hinode SOT contract NNM07AA01C. A. Caspi, H. Hudson, and S. Krucker
were supported by NASA under contract NAS5-98033 and grants NAG5-12878
and NNX08AJ18G. A. V. and M. T. acknowledge the Austrian Science Fund
(FWF) projects no. P20867-N16 and P20145-N16. We are grateful to several
insitutions for granting permission for the use of previously published
figures. In addition to those noted in figure captions, we also
acknowledge the following figures from A&A, reproduced with permission
(c) ESO: Fig. 12 (Mandrini et al. 1995, 303, 927); Fig. 18 (Miklenic et
al. 2007, 461, 697); Fig. 34 (Mann et al. 2003, 400, 329). The following
figures are reproduced with kind permission from Springer
Science+Business Media: Fig. 19 (Lindsey and Donea 2008); Fig. 27
(Krucker et al. 2008a); and Fig. 29 (Gallagher et al. 2002).
NR 491
TC 170
Z9 171
U1 1
U2 20
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-6308
EI 1572-9672
J9 SPACE SCI REV
JI Space Sci. Rev.
PD SEP
PY 2011
VL 159
IS 1-4
BP 19
EP 106
DI 10.1007/s11214-010-9701-8
PG 88
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 831NM
UT WOS:000295738400003
ER
PT J
AU Hendrickx, ME
Mah, C
Zarate-Montes, CM
AF Hendrickx, Michel E.
Mah, Christopher
Magno Zarate-Montes, Carlo
TI Deep-water Asteroidea (Echinodermata) collected during the TALUD cruises
in the Gulf of California, Mexico
SO REVISTA MEXICANA DE BIODIVERSIDAD
LA English
DT Article
DE Asteroidea; continental slope; western Mexico
ID SEA STARS ASTEROIDEA; SPECIES-DIVERSITY; OXYGEN; PACIFIC; FORCIPULATIDA;
BIODIVERSITY; COMMUNITIES; MACROFAUNA; GASTROPODS; PHYLOGENY
AB During a series of cruises aboard the RN "El Puma" aimed at collecting the deep-water benthic and pelagic fauna off the Pacific coast of Mexico, in the eastern Pacific, samples of Asteroidea were collected below 500 m depth (587-1 526 m). A total of 335 specimens were collected, belonging to 18 species, 14 identified to species, 3 to genus, and 1 previously undescribed species. New records are provided for Dipsacaster laetmophilus Fisher, 1910, Myxoderma sacculatum '(Fisher, 1905), Peribolaster biserialis Fisher, 1905, Ampheraster chirophts Fisher, 1928, Ampheraster hyperoncus (H. L. Clark, 1913), Anteliaster coscinactis Fisher, 1923, Nearchaster aciculosus (Fisher, 1910), Ceramaster leptoceramus (Fisher, 1905), Mediaster transfuga Ludwig, 1905, and Lophaster furcilliger Fisher, 1905. All species were collected below the oxygen minimum zone that extends throughout the central and southern Gulf of California, or within the threshold zone where severe to mild hypoxic conditions prevail. Epibenthic dissolved oxygen concentrations associated with the capture tithe specimens show support for strong tolerance to severe hypoxia (<1.0 ml O(2)/1) for most species, but only mild hypoxia for Ctenodiscus crispatus (Retzius, 1805), and Nymphaster diomedeae Ludwig, 1905. A checklist of all species of Asteroidea occurring below 500 m depth off the Pacific coast of Mexico is included.
C1 [Hendrickx, Michel E.; Magno Zarate-Montes, Carlo] Univ Nacl Autonoma Mexico, Lab Invertebrados Benton, Unidad Acad Mazatlan, Inst Ciencias Mar & Limnol, Mazatlan 82000, Sinaloa, Mexico.
[Mah, Christopher] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA.
[Magno Zarate-Montes, Carlo] Univ Nacl Autonoma Mexico, Posgrad Program, Inst Ciencias Mar & Limnol, Mexico City 04510, DF, Mexico.
RP Hendrickx, ME (reprint author), Univ Nacl Autonoma Mexico, Lab Invertebrados Benton, Unidad Acad Mazatlan, Inst Ciencias Mar & Limnol, Apartado Postal 811, Mazatlan 82000, Sinaloa, Mexico.
EM michel@ola.icmyl.unam.mx
FU DGAPA [IN-217306-3]; PASPA; UNAM, Mexico; CONACyT [216056]; CONACyT,
Mexico [31805-N]
FX The authors thank the scientists, students and crew members who
participated in the TALUD cruises aboard the R/V "El Puma". One of us
(MEH) is grateful to the Royal Belgian Institute of Natural Sciences
(RBINS) and the Free University of Brussels (ULB) for their hospitality
during his sabbatical leave. Special thanks to Thierry Backeljau
(RBINS), Michel Jangoux (ULB) for their invitation and to Frank Fiers,
Claude Massin, Philippe Willenz (RBINS), and Chantal De Ridder (ULB),
for the facilities provided. Permanent access to literature available in
the Laboratoire de Biologic Marine, ULB, was particularly helpful. The
DGAPA, PASPA, UNAM, Mexico, is acknowledged for providing support during
MEH sabbatical stay. CMZ was supported with a CONACyT Master Degree
grant (216056). We thank Gordon Hendler for providing data related to
the Allan Hancock expeditions material, the 2 anonymous reviewers for
their helpful suggestions, and Mercedes Cordero for preparation of maps
and final edition of the manuscript. This project was partly supported
by CONACyT, Mexico (project 31805-N) and DGAPA (project IN-217306-3),
UNAM, Mexico.
NR 69
TC 6
Z9 6
U1 2
U2 12
PU INST BIOLOGIA, UNIV NACIONAL AUTONOMA MEXICO
PI MEXICO
PA APARTADO POSTAL 70-233, MEXICO, D F 00000, MEXICO
SN 1870-3453
J9 REV MEX BIODIVERS
JI Rev. Mex. Biodivers.
PD SEP
PY 2011
VL 82
IS 3
BP 798
EP 824
PG 27
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA 833VP
UT WOS:000295913300008
ER
PT J
AU Wilson, JK
AF Wilson, J. Keith
TI Chinese Art Now at the Freer and Sackler INTRODUCTION
SO ARTS OF ASIA
LA English
DT Editorial Material
C1 [Wilson, J. Keith] Smithsonian Inst, Washington, DC 20560 USA.
[Wilson, J. Keith] Cleveland Museum Art, Cleveland, OH USA.
[Wilson, J. Keith] Los Angeles Cty Museum Art, Los Angeles, CA USA.
RP Wilson, JK (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 3
TC 0
Z9 0
U1 0
U2 0
PU ARTS ASIA PUBLICATIONS LTD
PI KOWLOON
PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG
SN 0004-4083
J9 ART ASIA
JI Arts Asia
PD SEP-OCT
PY 2011
VL 41
IS 5
BP 100
EP 103
PG 4
WC Art; Asian Studies
SC Art; Asian Studies
GA 831BN
UT WOS:000295703800003
ER
PT J
AU Douglas, JG
AF Douglas, Janet G.
TI Reconsidering the Configuration of a Jade and Gold Assemblage from
Jincun: A Technical Study
SO ARTS OF ASIA
LA English
DT Article
C1 Smithsonian Inst, Dept Conservat & Sci Res, Washington, DC 20560 USA.
RP Douglas, JG (reprint author), Smithsonian Inst, Dept Conservat & Sci Res, Washington, DC 20560 USA.
NR 10
TC 0
Z9 0
U1 1
U2 1
PU ARTS ASIA PUBLICATIONS LTD
PI KOWLOON
PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG
SN 0004-4083
J9 ART ASIA
JI Arts Asia
PD SEP-OCT
PY 2011
VL 41
IS 5
BP 117
EP 121
PG 5
WC Art; Asian Studies
SC Art; Asian Studies
GA 831BN
UT WOS:000295703800005
ER
PT J
AU Wilson, JK
AF Wilson, J. Keith
TI THEN AND NOW Displaying Chinese Art at the Freer Gallery
SO ARTS OF ASIA
LA English
DT Article
C1 [Wilson, J. Keith] Smithsonian Inst, Freer Gallery Art, Washington, DC 20560 USA.
[Wilson, J. Keith] Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA.
RP Wilson, JK (reprint author), Smithsonian Inst, Freer Gallery Art, Washington, DC 20560 USA.
NR 15
TC 0
Z9 0
U1 0
U2 0
PU ARTS ASIA PUBLICATIONS LTD
PI KOWLOON
PA KOWLOON CENTER-SUITE 1309 29-39 ASHLEY RD, KOWLOON, HONG KONG
SN 0004-4083
J9 ART ASIA
JI Arts Asia
PD SEP-OCT
PY 2011
VL 41
IS 5
BP 135
EP 147
PG 13
WC Art; Asian Studies
SC Art; Asian Studies
GA 831BN
UT WOS:000295703800007
ER
PT J
AU Harlow, GE
Sisson, VB
Sorensen, SS
AF Harlow, G. E.
Sisson, V. B.
Sorensen, S. S.
TI Jadeitite from Guatemala: new observations and distinctions among
multiple occurrences
SO GEOLOGICA ACTA
LA English
DT Article
DE Jadeitite; Serpentinite; Melange; HP-LT rock; Subduction processes
ID MOTAGUA FAULT ZONE; TEMPERATURE MELANGE; LAWSONITE ECLOGITE;
SUBDUCTION-ZONE; OCEANIC-CRUST; SERPENTINITE; OMPHACITE; GREECE;
METAMORPHISM; BLUESCHIST
AB In Guatemala, jadeitite occurs as blocks in serpentinite melange in distinct settings on opposite sides of the Motagua fault. Jadeitites north of the Motagua fault are associated with eclogites, blueschists, and garnet amphibolites and distributed over a 200km E-W area. Omphacitite, omphacite - taramite metabasite, albitite, and phengite rock are found with jadeitite. The assemblages indicate formation at 6-12kbar and 300-400 degrees C, however jadeite - omphacite pairs yield T from similar to 200 to >500 degrees C for jadeite crystallization. Jadeitites south of the Motagua fault are sourced from three separate fault slices of serpentinite in Jalapa and Zacapa departments and are distinctive:
1) Jadeitite near Carrizal Grande is found in serpentinite with lawsonite eclogites, variably altered to blueschist, and rarely in schists. A large jadeite - omphacite gap and lawsonite suggests T=300-400 degrees C, but at high P as indicated by the presence of quartz: P>12-20kbar. Lawsonite eclogites (P=20-25kbar, T=350-450 degrees C) occur with these jadeitites.
2) At La Ceiba, jadeitites coexist with omphacite blueschists and contain late-stage veins of quartz, diopside, cymrite, actinolite, titanite and vesuvianite. A large jadeite - omphacite gap suggests 300-400 degrees C, but at lower P as indicated by quartz + albite: P=10-14kbar.
3) At La Ensenada jade i tites occur with lawsonite-glaucophane blueschists and chloritite. It is a fine-grained jadeite-pumpellyite rock, intensely deformed and veined with grossular, omphacite, albite and titanite, but no quartz. A large jadeite-omphacite gap and pumpellyite suggest similar to 200-similar to 300 degrees C at lower P consistent with primary albite: P=6-9kbar. The silicates contain little iron.
C1 [Harlow, G. E.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
[Sisson, V. B.] Univ Houston, Dept Earth & Atmospher Sci, Houston, TX USA.
[Sorensen, S. S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
RP Harlow, GE (reprint author), Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA.
EM gharlow@amnh.org; j_sisson@netzero.net; sorensen@si.edu
FU IGCP Project [546]; [EAR0309320]; [EAR0309116]
FX We want to thank Carlos Gonzales for field assistance and Eric Sahm and
Jamie Newman for analytical and sample processing assistance and John
Cleary for sharing geological observations from mapping observations on
the jade deposits near Carrizal Grande. This work was funded by
EAR0309320 to GEH, and EAR0309116 to VBS. This project is part of IGCP
Project 546 on Subduction Zones of the Caribbean. We appreciate
constructive reviews by Walter Maresch and Tatsuki Tsujimori.
NR 67
TC 28
Z9 31
U1 0
U2 14
PU UNIV BARCELONA
PI BARCELONA
PA INST CIENCIES TERRA JAUME ALMERA-CSIC, LLUIS SOLE I SABARIS S-N,
BARCELONA, E-08028, SPAIN
SN 1695-6133
J9 GEOL ACTA
JI Geol. Acta
PD SEP-DEC
PY 2011
VL 9
IS 3-4
BP 363
EP +
DI 10.1344/105.000001694
PG 30
WC Geology
SC Geology
GA 835FU
UT WOS:000296021900010
ER
PT J
AU Weber, M
Cardona, A
Valencia, V
Altenberger, U
Lopez-Martinez, M
Tobon, M
Zapata, S
Zapata, G
Concha, AE
AF Weber, M.
Cardona, A.
Valencia, V.
Altenberger, U.
Lopez-Martinez, M.
Tobon, M.
Zapata, S.
Zapata, G.
Concha, A. E.
TI Geochemistry and Geochronology of the Guajira Eclogites, northern
Colombia: evidence of a metamorphosed primitive Cretaceous Caribbean
Island-arc
SO GEOLOGICA ACTA
LA English
DT Article
DE Eclogites; Primitive island-arc; Geochronology; Guajira Peninsula;
Colombia; Caribbean
ID HIGH-PRESSURE METAMORPHISM; CURA BLUESCHIST BELT; SOUTH-AMERICA;
TECTONIC HISTORY; BASIN DEVELOPMENT; MARGARITA ISLAND; SUBDUCTION ZONES;
GREATER ANTILLES; VENEZUELA; PLATE
AB The chemical composition of eclogites, found as boulders in a Tertiary conglomerate from the Guajira Peninsula, Colombia suggests that these rocks are mainly metamorphosed basaltic andesites. They are depleted in LILE elements compared to MORB, have a negative Nb-anomaly and flat to enriched REE patterns, suggesting that their protoliths evolved in a subduction related tectonic setting. They show island-arc affinities and are similar to primitive island-arc rocks described in the Caribbean. The geochemical characteristics are comparable to low-grade greenschists from the nearby Etpana Terrane, which are interpreted as part of a Cretaceous intra-oceanic arc. These data support evidence that the eclogites and the Etpana terrane rocks formed from the same volcano-sedimentary sequence. Part of this sequence was accreted onto the margin and another was incorporated into the subduction channel and metamorphosed at eclogite facies conditions. Ar-40-Ar-39 ages of 79.2 +/- 1.1Ma and 82.2 +/- 2.5Ma determined on white micas, separated from two eclogite samples, are interpreted to be related to the cooling of the main metamorphic event. The formation of a common volcano-sedimentary protolith and subsequent metamorphism of these units record the ongoing Late Cretaceous continental subduction of the South American margin within the Caribbean intra-oceanic arc subduction zone. This gave way to an arc-continent collision between the Caribbean and the South American plates, where this sequence was exhumed after the Campanian.
C1 [Weber, M.; Tobon, M.; Zapata, S.; Zapata, G.; Concha, A. E.] Univ Nacl Colombia, Medellin, Colombia.
[Cardona, A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Cardona, A.] Corp Geol Ares, Bogota, Colombia.
[Valencia, V.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Altenberger, U.] Univ Potsdam, D-14476 Potsdam, Germany.
[Lopez-Martinez, M.] CICESE, Dept Geol, Ensenada 22860, Baja California, Mexico.
RP Weber, M (reprint author), Univ Nacl Colombia, Carrera 80 65-223, Medellin, Colombia.
EM mweber@unal.edu.com; CardonaA@si.edu; victorv@email.arizona.edu;
uwe@geo.uni-potsdam.de; marlopez@cicese.mx
FU Universidad Nacional de Colombia through DIME [30805975]
FX Oscar Talavera is acknowledged for discussions and encouragement during
field work. Continuous help from Oscar Jaramillo at the Petrography
Laboratory, Universidad Nacional de Colombia is greatly appreciated.
This research was supported by the Universidad Nacional de Colombia
through DIME grant 30805975. This is a contribution to Project 546 of
the International Geological Correlation Program "Subduction zones of
the Caribbean". We are grateful to Antje Musiol (Potsdam) and Nora
Groshopf (Mainz), for their assistance with the chemical analyses. M.
Garcia Garcia assisted with the argon experiments. We would like to
thank J. Lewis and J. Wright, whose careful reviews considerably
improved this paper.
NR 70
TC 4
Z9 5
U1 0
U2 8
PU UNIV BARCELONA
PI BARCELONA
PA INST CIENCIES TERRA JAUME ALMERA-CSIC, LLUIS SOLE I SABARIS S-N,
BARCELONA, E-08028, SPAIN
SN 1695-6133
J9 GEOL ACTA
JI Geol. Acta
PD SEP-DEC
PY 2011
VL 9
IS 3-4
BP 425
EP 443
DI 10.1344/105.000001740
PG 19
WC Geology
SC Geology
GA 835FU
UT WOS:000296021900013
ER
PT J
AU Cardona, A
Valencia, V
Weber, M
Duque, J
Montes, C
Ojeda, G
Reiners, P
Domanik, K
Nicolescu, S
Villagomez, D
AF Cardona, A.
Valencia, V.
Weber, M.
Duque, J.
Montes, C.
Ojeda, G.
Reiners, P.
Domanik, K.
Nicolescu, S.
Villagomez, D.
TI Transient Cenozoic tectonic stages in the southern margin of the
Caribbean plate: U-Th/He thermochronological constraints from Eocene
plutonic rocks in the Santa Marta massif and Serrania de Jarara,
northern Colombia
SO GEOLOGICA ACTA
LA English
DT Article
DE U-Th/He thermochronology; Exhumation; Oblique convergence; Caribbean
subduction
ID HETEROGENEOUS OCEANIC-CRUST; FISSION-TRACK ANALYSIS; AMERICAN PLATE;
APATITE (U-TH)/HE; TERRANE ACCRETION; CONTINENTAL-MARGIN; CONVERGENT
MARGINS; WESTERN VENEZUELA; HELIUM DIFFUSION; RIDGE SUBDUCTION
AB We use U-Th/(He) zircon and apatite thermochronology and Al in hornblende geobarometry from Eocene granitoids of the Sierra Nevada de Santa Marta and Guajira uplifted massifs in northern Colombia to elucidate the exhumation history of the northern South America continental margin and its bearing to Cenozoic Caribbean-South American plate interactions. Aluminium in hornblende geobarometry from the Eocene Santa Marta batholith yields pressures between 4.9 +/- 0.6kbar and 6.4 +/- 0.6kbar, which indicate that at least, 14.7-19.2km of unroofing took place since 56-50Ma in the northwestern Sierra Nevada de Santa Marta. In the Guajira Peninsula, calculated pressures for the Eocene Parashi stock are 2.3 +/- 0.6kbar and 3 +/- 0.6kbar. Stratigraphic considerations pertaining to Oligocene conglomerates from the Guajira area suggest that 6.9-9km of crust was lost between 50Ma and ca. 26Ma. U-Th/He zircon and apatite thermochronology from granitoids in the Sierra Nevada de Santa Marta shows the existence of major exhumation events in the Late Eocene (ca. 45-40Ma), Late Oligocene (ca. 25Ma) and Miocene (ca. 15Ma). The Guajira region records the Late Eocene to Early Oligocene (35-25Ma) event, but it lacks evidence for the Miocene exhumation phase. These differences reflect isolation of the Guajira region from the Sierra Nevada de Santa Marta and the Andean chain due to extensive block rotation and transtensional tectonics that affected the region during post-Eocene times.
The post-Eocene events correlate in time with an increased convergence rate and the frontal approach of North and South America. It is suggested that the two major tectonic mechanisms that govern exhumation in these Caribbean massifs are: 1) subduction of the Caribbean plate, and 2) post Eocene changes in plate convergence obliquity and rates that caused the South American continental margin blocks to override the Caribbean plate. Temporal correlation with other Caribbean and Northern Andean events allows to resolve the regional Cenozoic plate tectonic reorganizations experienced by the South American, Caribbean and Pacific plates at a regional scale.
C1 [Cardona, A.; Montes, C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Valencia, V.] Washington State Univ, Earth & Environm Sci Dept, Pullman, WA 99164 USA.
[Weber, M.] Univ Nacl Colombia, Escuela Geociencias & Med Ambiente, Medellin, Colombia.
[Duque, J.] Univ Autonoma Mexico, Ctr Geociencias, Queretaro, Mexico.
[Cardona, A.; Montes, C.] Corp Geol Ares, Bogota, Colombia.
[Ojeda, G.] Inst Colombiano Petroleoecopetrol, Piedecuesta, Colombia.
[Reiners, P.; Nicolescu, S.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA.
[Domanik, K.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA.
[Villagomez, D.] Univ Geneva, Dept Earth Sci, CH-1211 Geneva 4, Switzerland.
RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
OI Montes, Camilo/0000-0002-3553-0787
FU ECOPETROL-ICP; INGEOMINAS; INVEMAR; Fundacion para el Apoyo de la
Investigacion y la Cultura del Banco de la Republica de Colombia [2289];
Universidad Nacional de Colombia DIME [30805975]; NSF [EAR-0443387]
FX ECOPETROL-ICP, INGEOMINAS and INVEMAR are acknowledged for the support
given to A. Cardona during his participation in the Sierra Nevada de
Santa Marta geological project, including access to sample collections.
Diego Morata and an anonymous reviewer are acknowledged for their
suggestions and reviews that enormously improved the manuscript. Sergio
Restrepo is acknowledged for his valuable suggestions. Field work in the
Guajira Region and U-Th/He analyses received support from the Fundacion
para el Apoyo de la Investigacion y la Cultura del Banco de la Republica
de Colombia (project 2289), and the Universidad Nacional de Colombia
DIME Grant 30805975. Funding for the LaserChron Center was provided by
the NSF EAR-0443387. Scientific support by C. Jaramillo is enormously
appreciated. C. Bustamante and S. Zapata are acknowledged for helping
with the data organization and sample collection. A. Garcia-Casco is
acknowledged for continuous discussions and encouragement. This is a
contribution to the IGCP 546: "Subduction zones of the Caribbean".
NR 138
TC 6
Z9 6
U1 0
U2 9
PU UNIV BARCELONA
PI BARCELONA
PA INST CIENCIES TERRA JAUME ALMERA-CSIC, LLUIS SOLE I SABARIS S-N,
BARCELONA, E-08028, SPAIN
SN 1695-6133
EI 1696-5728
J9 GEOL ACTA
JI Geol. Acta
PD SEP-DEC
PY 2011
VL 9
IS 3-4
BP 445
EP +
DI 10.1344/105.000001739
PG 25
WC Geology
SC Geology
GA 835FU
UT WOS:000296021900014
ER
PT J
AU Santos-Granero, F
AF Santos-Granero, Fernando
TI Strange Enemies: Indigenous Agency and Scenes of Encounters in Amazonia
SO JOURNAL OF ANTHROPOLOGICAL RESEARCH
LA English
DT Book Review
C1 [Santos-Granero, Fernando] Smithsonian Trop Res Inst, Balboa, Panama.
RP Santos-Granero, F (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV NEW MEXICO, DEPT ANTHROPOL
PI ALBUQUERQUE
PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA
SN 0091-7710
J9 J ANTHROPOL RES
JI J. Anthropol. Res.
PD FAL
PY 2011
VL 67
IS 3
BP 455
EP 456
PG 2
WC Anthropology
SC Anthropology
GA 834GC
UT WOS:000295946800011
ER
PT J
AU Kelly, BC
AF Kelly, Brandon C.
TI Data Augmentation, Internal Representation, and Unsupervised Learning
Comment
SO JOURNAL OF COMPUTATIONAL AND GRAPHICAL STATISTICS
LA English
DT Editorial Material
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kelly, BC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bckelly@cfa.harvard.edu
NR 5
TC 2
Z9 2
U1 0
U2 0
PU AMER STATISTICAL ASSOC
PI ALEXANDRIA
PA 732 N WASHINGTON ST, ALEXANDRIA, VA 22314-1943 USA
SN 1061-8600
J9 J COMPUT GRAPH STAT
JI J. Comput. Graph. Stat.
PD SEP
PY 2011
VL 20
IS 3
BP 584
EP 591
DI 10.1198/jcgs.2011.203c
PG 8
WC Statistics & Probability
SC Mathematics
GA 835YP
UT WOS:000296073500004
ER
PT J
AU Arcand, KK
Watzke, M
AF Arcand, Kimberly K.
Watzke, Megan
TI Creating Public Science With the From Earth to the Universe Project
SO SCIENCE COMMUNICATION
LA English
DT Article
DE public science; astronomy; science outreach; science communication
ID ASTRONOMY
AB The authors propose formalizing an entity for the sciences and science communication that is akin to public art in the humanities: public science. Public science might be able to play a role in enhancing and supporting society's relationship with science by embedding science content into everyday experiences. The authors examine one project and its potential impact in public science. From Earth to the Universe has placed astronomy images in "nontraditional" science communication venues such as parks and airports. From Earth to the Universe could serve as a model for a type of public science, an attempt to make science accessible to nonexperts in public spaces.
C1 [Arcand, Kimberly K.; Watzke, Megan] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Arcand, KK (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
EM kkowal@cfa.harvard.edu
NR 14
TC 2
Z9 2
U1 1
U2 7
PU SAGE PUBLICATIONS INC
PI THOUSAND OAKS
PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA
SN 1075-5470
EI 1552-8545
J9 SCI COMMUN
JI Sci. Commun.
PD SEP
PY 2011
VL 33
IS 3
BP 398
EP 407
DI 10.1177/1075547011417895
PG 10
WC Communication
SC Communication
GA 828XQ
UT WOS:000295538400005
ER
PT J
AU Walsh, AJ
Breen, SL
Britton, T
Brooks, KJ
Burton, MG
Cunningham, MR
Green, JA
Harvey-Smith, L
Hindson, L
Hoare, MG
Indermuehle, B
Jones, PA
Lo, N
Longmore, SN
Lowe, V
Phillips, CJ
Purcell, CR
Thompson, MA
Urquhart, JS
Voronkov, MA
White, GL
Whiting, MT
AF Walsh, A. J.
Breen, S. L.
Britton, T.
Brooks, K. J.
Burton, M. G.
Cunningham, M. R.
Green, J. A.
Harvey-Smith, L.
Hindson, L.
Hoare, M. G.
Indermuehle, B.
Jones, P. A.
Lo, N.
Longmore, S. N.
Lowe, V.
Phillips, C. J.
Purcell, C. R.
Thompson, M. A.
Urquhart, J. S.
Voronkov, M. A.
White, G. L.
Whiting, M. T.
TI The H2O Southern Galactic Plane Survey (HOPS) - I. Techniques and H2O
maser data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE masers; surveys; stars: formation; ISM: molecules; Galaxy: structure;
radio lines: ISM
ID H-II-REGIONS; STAR-FORMING REGIONS; ULTRACOMPACT HII-REGIONS;
GIANT-BRANCH STAR; WATER MASERS; METHANOL MASERS; MOLECULAR CLOUDS;
HYPERFINE STRUCTURE; IRAS SOURCES; SIO MASER
AB We present first results of the H2O Southern Galactic Plane Survey (HOPS), using the Mopra Radio Telescope with a broad-band backend and a beam size of about 2 arcmin. We have observed 100 deg(2) of the southern Galactic plane at 12 mm (19.5-27.5 GHz), including spectral line emission from H2O masers, multiple metastable transitions of ammonia, cyanoacetylene, methanol and radio recombination lines. In this paper, we report on the characteristics of the survey and H2O maser emission. We find 540 H2O masers, of which 334 are new detections. The strongest maser is 3933 Jy and the weakest is 0.7 Jy, with 62 masers over 100 Jy. In 14 maser sites, the spread in the velocity of the H2O maser emission exceeds 100 km s(-1). In one region, the H2O maser velocities are separated by 351.3 km s(-1). The rms noise levels are typically between 1 and 2 Jy, with 95 per cent of the survey under 2 Jy. We estimate completeness limits of 98 per cent at around 8.4 Jy and 50 per cent at around 5.5 Jy. We estimate that there are between 800 and 1500 H2O masers in the Galaxy that are detectable in a survey with similar completeness limits to HOPS. We report possible masers in NH3 (11,9) and (8,6) emission towards G19.61-0.23 and in the NH3 (3,3) line towards G23.33-0.30.
C1 [Walsh, A. J.; White, G. L.] James Cook Univ, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia.
[Breen, S. L.; Britton, T.; Brooks, K. J.; Green, J. A.; Harvey-Smith, L.; Hindson, L.; Indermuehle, B.; Jones, P. A.; Lowe, V.; Phillips, C. J.; Urquhart, J. S.; Voronkov, M. A.; Whiting, M. T.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia.
[Burton, M. G.; Cunningham, M. R.; Lowe, V.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Hindson, L.; Voronkov, M. A.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Hoare, M. G.; Purcell, C. R.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Jones, P. A.; Lo, N.] Univ Chile, Dept Astron, Santiago, Chile.
[Lo, N.] Uni Paris Diderot, Lab AIM Paris Saclay, CEA Irfu, CNRS,INSU, F-91191 Gif Sur Yvette, France.
[Longmore, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Longmore, S. N.] European So Observ, D-85748 Garching, Germany.
RP Walsh, AJ (reprint author), James Cook Univ, Sch Engn & Phys Sci, Townsville, Qld 4811, Australia.
EM andrew.walsh@jcu.edu.au
RI Walsh, Andrew/B-5627-2013;
OI Walsh, Andrew/0000-0001-9506-0855; Purcell, Cormac/0000-0002-7491-7386;
Cunningham, Maria/0000-0001-7020-6176; Burton,
Michael/0000-0001-7289-1998
FU GEMINI-CONICYT FUND; Ile-de-France Region; Australian Research Council;
CSIRO; University of New South Wales; Monash University; University of
Sydney; Commonwealth of Australia
FX The HOPS team would like to thank the dedicated work of CSIRO Narrabri
staff who supported the observations beyond the call of duty. PAJ
acknowledges partial support from Centro de Astrofisica FONDAP 15010003
and the GEMINI-CONICYT FUND. NL acknowledges partial support from the
Center of Excellence in Astrophysics and Associated Technologies (PFB
06) and Centro de Astrofisica FONDAP 15010003. NL's postdoctoral
position at CEA/Irfu was funded by the Ile-de-France Region. The
University of New South Wales Digital Filter Bank used for the
observations (MOPS) with the Mopra Telescope was provided with support
from the Australian Research Council, CSIRO, The University of New South
Wales, Monash University and The University of Sydney. The Mopra Radio
Telescope is part of the Australia Telescope National Facility which is
funded by the Commonwealth of Australia for operation as a National
Facility managed by CSIRO.
NR 114
TC 73
Z9 73
U1 0
U2 2
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 SEP
PY 2011
VL 416
IS 3
BP 1764
EP 1821
DI 10.1111/j.1365-2966.2011.19115.x
PG 58
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 826TQ
UT WOS:000295378100013
ER
PT J
AU Narayan, R
Kumar, P
Tchekhovskoy, A
AF Narayan, Ramesh
Kumar, Pawan
Tchekhovskoy, Alexander
TI Constraints on cold magnetized shocks in gamma-ray bursts
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE acceleration of particles; MHD; radiation mechanisms: non-thermal;
relativistic processes; shock waves; gamma-ray burst: general
ID DOUBLE RADIO-SOURCES; KINETIC-ENERGY; FERMI OBSERVATIONS; RELATIVISTIC
JETS; EARLY AFTERGLOWS; REVERSE SHOCK; LIGHT CURVES; GRB 080916C; SWIFT
ERA; MODEL
AB We consider a model in which the ultrarelativistic jet in a gamma-ray burst (GRB) is cold and magnetically accelerated. We assume that the energy flux in the outflowing material is partially thermalized via internal shocks or a reverse shock, and we estimate the maximum amount of radiation that could be produced in such magnetized shocks. We compare this estimate with the available observational data on prompt gamma-ray emission in GRBs. We find that, even with highly optimistic assumptions, the magnetized jet model is radiatively too inefficient to be consistent with observations. One way out is to assume that much of the magnetic energy in the post-shock, or even pre-shock, jet material is converted to particle thermal energy by some unspecified process, and then radiated. This can increase the radiative efficiency sufficiently to fit observations. Alternatively, jet acceleration may be driven by thermal pressure rather than magnetic fields. In this case, which corresponds to the traditional fireball model, sufficient prompt GRB emission could be produced either from shocks at a large radius or from the jet photosphere closer to the centre.
C1 [Narayan, Ramesh] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kumar, Pawan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Tchekhovskoy, Alexander] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA.
RP Narayan, R (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rnarayan@cfa.harvard.edu; pk@astro.as.utexas.edu; atchekho@princeton.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA [NNX11AE16G]; NSF [AST-1041590, AST-0909110]; NSF through QueenBee
of the Louisiana Optical Network Initiative; National Institute for
Computational Sciences [TG-AST080026N, TG-AST100040]; Princeton Center
FX RN and AT were supported in part by NASA grant NNX11AE16G and NSF grant
AST-1041590, and by NSF through TeraGrid resources provided by QueenBee
of the Louisiana Optical Network Initiative (http://www.loni.org) and
Kraken of the National Institute for Computational Sciences
(http://www.nics.tennessee.edu) under grant number TG-AST080026N (RN and
AT) and TG-AST100040 (AT). AT was supported in part by a Princeton
Center for Theoretical Science Fellowship. PK was supported in part by
NSF grant AST-0909110.
NR 60
TC 22
Z9 22
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 SEP
PY 2011
VL 416
IS 3
BP 2193
EP 2201
DI 10.1111/j.1365-2966.2011.19197.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 826TQ
UT WOS:000295378100045
ER
PT J
AU Kauffmann, J
Bertoldi, F
Bourke, TL
Myers, PC
Lee, CW
Huard, TL
AF Kauffmann, J.
Bertoldi, F.
Bourke, T. L.
Myers, P. C.
Lee, C. W.
Huard, T. L.
TI Confirmation of the VeLLO L1148-IRS: star formation at very low (column)
density
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE brown dwarfs; stars: formation; stars: low-mass; ISM: individual
objects: L1148; ISM: jets and outflows; infrared: stars
ID SPITZER C2D SURVEY; YOUNG STELLAR OBJECTS; BIPOLAR MOLECULAR OUTFLOW;
LOW-LUMINOSITY OBJECT; 1ST HYDROSTATIC CORE; PRE-MAIN-SEQUENCE; LOW-MASS
STARS; INFALL MOTIONS; EVOLUTIONARY MODELS; SMALL CLOUDS
AB We report the detection of a compact (similar to 5 arcsec; about 1800 au projected size) CO outflow from L1148-IRS. This confirms that this Spitzer source is physically associated with the nearby (approximate to 325 pc) L1148 dense core. Radiative transfer modelling suggests an internal luminosity of 0.08 to 0.13 L-circle dot. This validates L1148-IRS as a Very Low Luminosity Object (VeLLO; L = 0.1 L-circle dot). The L1148 dense core has unusually low densities and column densities for a star-forming core. It is difficult to understand how L1148-IRS might have formed under these conditions. Independent of the exact final mass of this VeLLO (which is likely <0.24 M-circle dot), L1148-IRS and similar VeLLOs might hold some clues about the isolated formation of brown dwarfs.
C1 [Kauffmann, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Bourke, T. L.; Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lee, C. W.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea.
[Huard, T. L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
RP Kauffmann, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM jens.kauffmann@jpl.nasa.gov
FU NASA [1279198, 1288806, 1407]; National Research Foundation of Korea;
Ministry of Education, Science and Technology [2010-0011605]
FX We are indebted to our local IRAM contacts, Arancha Castro-Carrizo and
Frederic Gueth, who changed their busy schedule to simplify our travel
arrangements for a data reduction visit. We thank Endrik Krugel for
providing us with a custom-modified dust radiative transfer code. Mike
Dunham was so kind to check our VeLLO catalogue (Table 2, Section 5.2)
against his notes. JK is deeply indebted to FB, Karl Menten, Malcolm
Walmsley, Johannes Schmid-Burgk and TP. This work would have been
impossible without their continuous and unconditional support. He also
thanks Di Li and Paul Goldsmith, his hosts at JPL, for making this
research possible. This project was supported by an appointment of JK to
the NASA Postdoctoral Program at the Jet Propulsion Laboratory,
administered by Oak Ridge Associated Universities through a contract
with NASA. His research was executed at the Jet Propulsion Laboratory,
California Institute of Technology, under a contract with the National
Air and Space Administration. Partial support for TLB was provided by
NASA through contracts 1279198 and 1288806 issued by the Jet Propulsion
Laboratory, California Institute of Technology, under NASA contract
1407. CWL acknowledges the support by Basic Science Research Program
through the National Research Foundation of Korea funded by the Ministry
of Education, Science and Technology (2010-0011605).
NR 86
TC 19
Z9 19
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 SEP
PY 2011
VL 416
IS 3
BP 2341
EP 2358
DI 10.1111/j.1365-2966.2011.19205.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 826TQ
UT WOS:000295378100055
ER
PT J
AU Sayer, EJ
Heard, MS
Grant, HK
Marthews, TR
Tanner, EVJ
AF Sayer, Emma J.
Heard, Matthew S.
Grant, Helen K.
Marthews, Toby R.
Tanner, Edmund V. J.
TI Soil carbon release enhanced by increased tropical forest litterfall
SO NATURE CLIMATE CHANGE
LA English
DT Article
ID ORGANIC-CARBON; RHIZOSPHERE RESPIRATION; ATMOSPHERIC CO2; CLIMATE;
VEGETATION; FEEDBACKS; STORAGE; EFFLUX; PLOTS
AB Tropical forests are a critical component of the global carbon cycle(1) and their response to environmental change will play a key role in determining future concentrations of atmospheric carbon dioxide (CO2)(1,2). Increasing primary productivity in tropical forests over recent decades has been attributed to CO2 fertilization(3), and greater biomass in tropical forests could represent a substantial sink for carbon in the future(3,4). However, the carbon sequestration capacity of tropical forest soils is uncertain and feedbacks between increased plant productivity and soil carbon dynamics remain unexplored(5,6). Here, we show that experimentally increasing litterfall in a lowland tropical forest enhanced carbon release from the soil. Using a large-scale litter manipulation experiment combined with carbon isotope measurements, we found that the efflux of CO2 derived from soil organic carbon was significantly increased by litter addition. Furthermore, this effect was sustained over several years. We predict that a future increase in litterfall of 30% with an increase in atmospheric CO2 concentrations of 150 ppm could release about 0.6 t C ha(-1) yr(-1) from the soil, partially offsetting predicted net gains in carbon storage. Thus, it is essential that plant-soil feedbacks are taken into account in predictions of the carbon sequestration potential of tropical forests.
C1 [Sayer, Emma J.; Heard, Matthew S.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Sayer, Emma J.; Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England.
[Sayer, Emma J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Marthews, Toby R.] Lancaster Environm Ctr, Ctr Ecol Hydrol, Life Sci Mass Spectrometry Facil, Lancaster LA1 4AP, England.
[Marthews, Toby R.] Environm Change Inst, Sch Geog & Environm, Oxford OX1 3QY, England.
RP Sayer, EJ (reprint author), Ctr Ecol & Hydrol, Maclean Bldg,Benson Lane, Wallingford OX10 8BB, Oxon, England.
EM emsa@ceh.ac.uk
RI Sayer, Emma/B-2514-2010; Heard, Matthew/E-6743-2012; MARTHEWS,
TOBY/H-6264-2014
OI Sayer, Emma/0000-0002-3322-4487; MARTHEWS, TOBY/0000-0003-3727-6468
FU FP6 Marie-Curie Outgoing International Fellowship; Smithsonian Tropical
Research Institute; Department of Plant Sciences, Cambridge
FX We thank F. Valdez, D. Urena and A. Worrell for field assistance, S. J.
Wright and the Smithsonian Tropical Research Institute for hosting our
fieldwork, A. Stott for help with isotope analyses, N. Isaac and S.
Freeman for advice on statistics and N. Ostle for helpful discussions.
Soil water content data were provided by the Terrestrial-Environmental
Sciences Program of the Smithsonian Tropical Research Institute. This
research was funded by an FP6 Marie-Curie Outgoing International
Fellowship to E.J.S, the Smithsonian Tropical Research Institute and the
Department of Plant Sciences, Cambridge.
NR 30
TC 64
Z9 71
U1 14
U2 145
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1758-678X
J9 NAT CLIM CHANGE
JI Nat. Clim. Chang.
PD SEP
PY 2011
VL 1
IS 6
BP 304
EP 307
DI 10.1038/NCLIMATE1190
PG 4
WC Environmental Sciences; Environmental Studies; Meteorology & Atmospheric
Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 832JD
UT WOS:000295799900016
ER
PT J
AU Ashby, MLN
Mahajan, S
Smith, HA
Willner, SP
Fazio, GG
Raychaudhury, S
Zezas, A
Barmby, P
Bonfini, P
Cao, C
Gonzalez-Alfonso, E
Ishihara, D
Kaneda, H
Lyttle, V
Madden, S
Papovich, C
Sturm, E
Surace, J
Wu, H
Zhu, YN
AF Ashby, M. L. N.
Mahajan, S.
Smith, H. A.
Willner, S. P.
Fazio, G. G.
Raychaudhury, S.
Zezas, A.
Barmby, P.
Bonfini, P.
Cao, C.
Gonzalez-Alfonso, E.
Ishihara, D.
Kaneda, H.
Lyttle, V.
Madden, S.
Papovich, C.
Sturm, E.
Surace, J.
Wu, H.
Zhu, Y. -N.
TI The Star Formation Reference Survey. I. Survey Description and Basic
Data
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; TELESCOPE KEY
PROJECT; DIGITAL SKY SURVEY; FORMATION HISTORY; SPACE-TELESCOPE; NEARBY
GALAXIES; FORMATION RATES; INFRARED PROPERTIES; STARBURST GALAXIES
AB Star formation is arguably the most important physical process in the cosmos. It is a fundamental driver of galaxy evolution and the ultimate source of most of the energy emitted by galaxies in the local universe. A correct interpretation of star formation rate (SFR) measures is therefore essential to our understanding of galaxy formation and evolution. Unfortunately, however, no single SFR estimator is universally available or even applicable in all circumstances: the numerous galaxies found in deep surveys are often too faint (or too distant) to yield significant detections with most standard SFR measures, and until now there have been no global multiband observations of nearby galaxies that span all the conditions under which star formation is taking place. To address this need in a systematic way, we have undertaken a multiband survey of all types of star-forming galaxies in the local universe. This project, the Star Formation Reference Survey (SFRS), is based on a statistically valid sample of 369 nearby galaxies that span all existing combinations of dust temperature, SFR, and specific SFR. Furthermore, because the SFRS is blind with respect to AGN fraction and environment, it serves as a means to assess the influence of these factors on SFR. Our panchromatic global flux measurements (including GALEX FUV + NUV, SDSS ugriz, 2MASS JHK(s), Spitzer 3-8 mu m, and others) furnish uniform SFR measures and the context in which their reliability can be assessed. This article describes the SFRS survey strategy, defines the sample, and presents the multiband photometry collected to date.
C1 [Ashby, M. L. N.; Mahajan, S.; Smith, H. A.; Willner, S. P.; Fazio, G. G.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mahajan, S.; Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Zezas, A.; Bonfini, P.] Univ Crete, Dept Phys, Iraklion, Greece.
[Barmby, P.; Lyttle, V.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada.
[Cao, C.] Shandong Univ, Sch Space Sci & Phys, Weihai 264209, Shandong, Peoples R China.
[Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, E-28871 Madrid, Spain.
[Ishihara, D.; Kaneda, H.] Nagoya Univ, Grad Sch Sci, Chikusa Ku, Aichi 4648602, Japan.
[Madden, S.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Papovich, C.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Sturm, E.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany.
[Surace, J.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Wu, H.; Zhu, Y. -N.] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China.
RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mashby@cfa.harvard.edu
RI Mahajan, Smriti/D-8902-2013; Barmby, Pauline/I-7194-2016; Zezas,
Andreas/C-7543-2011
OI Barmby, Pauline/0000-0003-2767-0090; Zezas, Andreas/0000-0001-8952-676X
FU National Aeronautics and Space Administration [NNX07AH49G, NNX10AD83G];
National Science Foundation of China [10833006, 10773014]; 973 Program
[2007CB815406]; Natural Sciences and Engineering Research Council of
Canada; Smithsonian Institution; Marie-Curie International Reintegration
Grant [224878]; European Union [206469]
FX The authors gratefully acknowledge the assistance of R. Brent Tully, who
generously supplied quality distances for many of our sample galaxies.
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 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 this work was provided by NASA. The VLA is operated by the National
Radio Astronomy Observatory, which is a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. H. Wu is supported by National Science Foundation of
China grants 10833006 and 10773014 and the 973 Program grant
2007CB815406. P. Barmby acknowledges research support through a
Discovery Grant from the Natural Sciences and Engineering Research
Council of Canada. S. Mahajan acknowledges support from a Smithsonian
Institution Endowment Grant. A. Zezas and P. Bonfini acknowledge support
by Marie-Curie International Reintegration Grant 224878 and European
Union grant 206469. H. Smith acknowledges support from NASA grants
NNX07AH49G and NNX10AD83G.
NR 80
TC 3
Z9 3
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD SEP
PY 2011
VL 123
IS 907
BP 1011
EP 1029
DI 10.1086/661920
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 829ON
UT WOS:000295593300001
ER
PT J
AU Bulbul, GE
Hasler, N
Bonamente, M
Joy, M
Marrone, D
Miller, A
Mroczkowski, T
AF Bulbul, G. E.
Hasler, N.
Bonamente, M.
Joy, M.
Marrone, D.
Miller, A.
Mroczkowski, T.
TI The effect of helium sedimentation on galaxy cluster masses and scaling
relations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: clusters: general
ID X-RAY MEASUREMENTS; BREMSSTRAHLUNG GAUNT FACTOR; HUBBLE CONSTANT; CL
0016+16; CONSTRAINTS; DIFFUSION; ELEMENTS; PLASMA; GAS
AB Context. Recent theoretical studies predict that the inner regions of galaxy clusters may have an enhanced helium abundance due to sedimentation over the cluster lifetime. If sedimentation is not suppressed (e.g., by tangled magnetic fields), this may significantly affect the cluster mass estimates.
Aims. We use Chandra X-ray observations of eight relaxed galaxy clusters to investigate the upper limits to the effect of helium sedimentation on the measurement of cluster masses and the best-fit slopes of the Y(X) - M(500) and Y(X) -M(2500) scaling relations.
Methods. We calculated gas mass and total mass in two limiting cases: a uniform, unenhanced abundance distribution and a radial distribution from numerical simulations of helium sedimentation on a timescale of 11 Gyr.
Results. The assumed helium sedimentation model, on average, produces a negligible increase in the gas mass inferred within large radii (r < r(500)) (1.3 +/- 1.2%) and a 10.2 +/- 5.5% mean decrease in the total mass inferred within r < r(500). Significantly stronger effects in the gas mass (10.5 +/- 0.8%) and total mass (25.1 +/- 1.1%) are seen at small radii owing to a larger variance in helium abundance in the inner region, r <= 0.1 r(500).
Conclusions. We find that the slope of the Y(X) - M(500) scaling relation is not significantly affected by helium sedimentation.
C1 [Bulbul, G. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bulbul, G. E.; Hasler, N.; Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA.
[Bonamente, M.; Joy, M.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA.
[Marrone, D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Miller, A.] Columbia Univ, Dept Phys, New York, NY 10027 USA.
[Mroczkowski, T.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
RP Bulbul, GE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bonamem@email.uah.edu
OI Marrone, Daniel/0000-0002-2367-1080; Mroczkowski,
Tony/0000-0003-3816-5372
NR 31
TC 5
Z9 5
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 SEP
PY 2011
VL 533
AR A6
DI 10.1051/0004-6361/201016407
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100006
ER
PT J
AU Cesaroni, R
Beltran, MT
Zhang, Q
Beuther, H
Fallscheer, C
AF Cesaroni, R.
Beltran, M. T.
Zhang, Q.
Beuther, H.
Fallscheer, C.
TI Dissecting a hot molecular core: the case of G31.41+0.31
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: formation; ISM: individual objects: G31.41+0.31; ISM: molecules;
ISM: jets and outflows; accretion, accretion disks
ID YOUNG STELLAR OBJECTS; MASSIVE STARS; ROTATING TOROIDS; HII-REGIONS;
ACCRETION; OUTFLOWS; DISKS; SUBMILLIMETER; EMISSION; AMMONIA
AB Context. The role of disks in the formation of high-mass stars is still a matter of debate but the detection of circumstellar disks around O-type stars would have a profound impact on high-mass star formation theories.
Aims. We made a detailed observational analysis of a well known hot molecular core lying in the high-mass star-forming region G31.41+0.31. This core is believed to contain deeply embedded massive stars and presents a velocity gradient that has been interpreted either as rotation or as expansion, depending on the authors. Our aim was to shed light on this question and possibly prepare the ground for higher resolution ALMA observations, which could directly detect circumstellar disks around the embedded massive stars.
Methods. Observations at sub-arcsecond resolution were performed with the Submillimeter Array in methyl cyanide, a typical hot molecular core tracer, and (CO)-C-12 and (CO)-C-13, well known outflow tracers. We also obtained sensitive continuum maps at 1.3 mm.
Results. Our findings confirm the existence of a sharp velocity gradient across the core, but cannot confirm the existence of a bipolar outflow perpendicular to it. The improved angular resolution and sampling of the uv plane allow us to attain higher quality channel maps of the CH3CN lines with respect to previous studies and thus significantly improve our knowledge of the structure and kinematics of the hot molecular core.
Conclusions. While no conclusive argument can rule out any of the two interpretations (rotation or expansion) proposed to explain the velocity gradient observed in the core, in our opinion the observational evidence collected so far indicates the rotating toroid as the most likely scenario. The outflow hypothesis appears less plausible, because the dynamical time scale is too short compared to that needed to form species such as CH3CN, and the mass loss and momentum rates estimated from our measurements appear too high.
C1 [Cesaroni, R.; Beltran, M. T.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Beuther, H.; Fallscheer, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Fallscheer, C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
RP Cesaroni, R (reprint author), INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
EM cesa@arcetri.astro.it; qzhang@cfa.harvard.edu; beuther@mpia-hd.mpg.de;
cassandra.fallscheer@nrc-cnrc.gc.ca
OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Cesaroni,
Riccardo/0000-0002-2430-5103; Zhang, Qizhou/0000-0003-2384-6589
NR 35
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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 SEP
PY 2011
VL 533
AR A73
DI 10.1051/0004-6361/201117206
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100073
ER
PT J
AU Curran, SJ
Tanna, A
Koch, FE
Berengut, JC
Webb, JK
Stark, AA
Flambaum, VV
AF Curran, S. J.
Tanna, A.
Koch, F. E.
Berengut, J. C.
Webb, J. K.
Stark, A. A.
Flambaum, V. V.
TI Measuring space-time variation of the fundamental constants with
redshifted submillimetre transitions of neutral carbon
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE submillimeter: galaxies; cosmology: observations; cosmology: theory;
quasars: emission lines; galaxies: ISM; techniques: spectroscopic
ID QUASAR HOST GALAXY; STAR-FORMATION LAW; Z RADIO GALAXIES; SIMILAR-TO 2;
MOLECULAR GAS; ATOMIC CARBON; CO EMISSION; LABORATORY OBSERVATION;
PHYSICAL CONSTANTS; STARBURST GALAXY
AB We compare the redshifts of neutral carbon and carbon monoxide in the redshifted sources in which the P-3(1) -> P-3(0) fine structure transition of neutral carbon, [C I], has been detected, in order to measure space-time variation of the fundamental constants. Comparison with the CO rotational lines measures F = alpha(2)/mu, where alpha is the fine structure constant and mu is the electron-proton mass ratio, which is the same combination of constants obtained from the comparison P-2(3/2) -> P-2(1/2) fine structure line of singly ionised carbon, [C II]. However, neutral carbon has the distinct advantage that it may be spatially coincident with the carbon monoxide, whereas [C II] could be located in the diffuse medium between molecular clouds, and so any comparison with CO could be dominated by intrinsic velocity differences. Using [C I], we obtain a mean variation of = (-3.6 +/- 8.5) x 10(-5), over z = 2.3-4.1, for the eight [C I] systems, which degrades to (-1.5 +/- 11) x 10(-5), over z = 2.3-6.4 when the two [C II] systems are included. That is, zero variation over look-back times of 10.8-12.8 Gyr. However, the latest optical results indicate a spatial variation in alpha, where Delta alpha/alpha describes a dipole and we see the same direction in Delta F/F. This trend is, however, due to a single source for which the [C I] spectrum is of poor quality. This also applies to one of the two [C II] spectra previously used to find a zero variation in alpha(2)/mu. Quantifying this, we find an anti-correlation between |Delta F/F| and the quality of the carbon detection, as measured by the spectral resolution, indicating that the typical values of greater than or similar to 50 km s (1), used to obtain a detection, are too coarse to reliably measure changes in the constants. From the fluxes of the known z greater than or similar to 1 CO systems, we predict that current instruments are incapable of the sensitivities required to measure changes in the constants through the comparison of CO and carbon lines. We therefore discuss in detail the use of ALMA for such an undertaking and find that, based upon the current CO detections only, the Full Array configuration is expected to detect similar to 100 galaxies in [C I] at better than 10 km s(-1) spectral resolution, while potentially resolving the individual molecular cloud complexes at redshifts of z greater than or similar to 3. This could provide greater than or similar to 1000 individual systems with which to obtain accurate measurements of space-time variation of the constants at look-back times in excess of 11 Gyr.
C1 [Curran, S. J.; Tanna, A.; Koch, F. E.; Berengut, J. C.; Webb, J. K.; Flambaum, V. V.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Stark, A. A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Curran, SJ (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
EM sjc@phys.unsw.edu.au
RI Berengut, Julian/A-1764-2010;
OI Stark, Antony/0000-0002-2718-9996
FU National Aeronautics and Space Administration
FX We would like to thank the referee Paolo Molaro for his prompt and
helpful comments as well as Stephen Lo for facilitating the enjoyable
seafood lunch overlooking Coogee Bay, during which the ideas for this
paper were developed. Also, Nick Tothill who came for coffee afterwards
and threw in his two cents worth. 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
research has also made use of NASA's Astrophysics Data System
Bibliographic Service.
NR 84
TC 8
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U1 0
U2 10
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 SEP
PY 2011
VL 533
AR A55
DI 10.1051/0004-6361/201117457
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100055
ER
PT J
AU Lattanzi, V
Gottlieb, CA
Thaddeus, P
Thorwirth, S
McCarthy, MC
AF Lattanzi, V.
Gottlieb, C. A.
Thaddeus, P.
Thorwirth, S.
McCarthy, M. C.
TI The rotational spectrum of protonated sulfur dioxide, HOSO+
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: molecules; radio lines: ISM; molecular processes; molecular data;
line: identification
ID LINE SURVEY; ORION-KL; GHZ; CHEMISTRY; STATES; SO2
AB Aims. We report on the millimeter-wave rotational spectrum of protonated sulfur dioxide, HOSO+.
Methods. Ten rotational transitions between 186 and 347 GHz have been measured to high accuracy in a negative glow discharge.
Results. The present measurements improve the accuracy of the previously reported centimeter-wave spectrum by two orders of magnitude, allowing a frequency calculation of the principal transitions to about 4 km s(-1) in equivalent radial velocity near 650 GHz, or one linewidth in hot cores and corinos.
Conclusions. Owing to the high abundance of sulfur-bearing molecules in many galactic molecular sources, the HOSO+ ion is an excellent candidate for detection, especially in hot cores and corinos in which SO2 and several positive ions are prominent.
C1 [Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Lattanzi, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM vlattanzi@cfa.harvard.edu
RI Thorwirth, Sven/C-6217-2011;
OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy,
Michael/0000-0001-9142-0008
FU NASA [NNX08AE05G]; Deutsche Forschungsgemainschaft (DFG) [TH 1301/3-1]
FX The authors wish to thank N. Adams and V. Bierbaum for helpful
discussions on ion chemistry; and E. Palmer, D. Kokkin, and O. Martinez
for assistance with the ion cell. This work was supported in part by
NASA Grant NNX08AE05G. S.T. gratefully acknowledges support by the
Deutsche Forschungsgemainschaft (DFG) through grant TH 1301/3-1.
NR 25
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U2 9
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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 SEP
PY 2011
VL 533
AR L11
DI 10.1051/0004-6361/201117753
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100158
ER
PT J
AU Migliori, G
Grandi, P
Torresi, E
Dermer, C
Finke, J
Celotti, A
Mukherjee, R
Errando, M
Gargano, F
Giordano, F
Giroletti, M
AF Migliori, G.
Grandi, P.
Torresi, E.
Dermer, C.
Finke, J.
Celotti, A.
Mukherjee, R.
Errando, M.
Gargano, F.
Giordano, F.
Giroletti, M.
TI Implications for the structure of the relativistic jet from
multiwavelength observations of NGC 6251
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: jets; galaxies: active; gamma rays: galaxies; galaxies:
individual: NGC 6251
ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; RADIO GALAXY NGC-6251;
GAMMA-RAY EMISSION; SPECTRAL ENERGY-DISTRIBUTION; FAST TEV VARIABILITY;
BL-LACERTAE OBJECTS; MASSIVE BLACK-HOLES; XMM-NEWTON VIEW; FR-I
AB NGC 6251 is a luminous radio galaxy approximate to 104 Mpc away that was detected significantly with the Fermi Gamma-ray Space Telescope, and before that with EGRET (onboard the Compton Gamma-ray Observatory). Different observational constraints favor a nuclear origin for the gamma-ray emission. Here we present a study of the spectral energy distribution of the core of NGC 6251, and give results of modeling in the one-zone synchrotron/SSC framework. The SSC model provides a good description of the radio to gamma-ray emission but, as for other misaligned sources, predicts a lower Lorentz factor (Gamma similar to 2.4) than typically found when modeling blazars. If the blazar unification scenario is correct, this seems to point to the presence of at least two emitting regions in these objects, one with a higher and one with a lower Lorentz factor. The solution of a structured jet, with a fast moving spine surrounded by a slow layer, is explored and the consequences of the two models for the jet energetics and evolution are discussed.
C1 [Migliori, G.; Celotti, A.] SISSA Int Sch Adv Studies, I-34136 Trieste, Italy.
[Migliori, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Grandi, P.; Torresi, E.] INAF, Ist Astrofis & Fis Cosm Bologna, I-40129 Bologna, Italy.
[Torresi, E.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Dermer, C.; Finke, J.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA.
[Mukherjee, R.; Errando, M.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Gargano, F.; Giordano, F.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
[Giordano, F.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Giroletti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy.
RP Migliori, G (reprint author), SISSA Int Sch Adv Studies, Via Bonomea 265, I-34136 Trieste, Italy.
EM migliori@head.cfa.harvard.edu
RI Gargano, Fabio/O-8934-2015;
OI Gargano, Fabio/0000-0002-5055-6395; Grandi, Paola/0000-0003-1848-6013;
Errando, Manel/0000-0002-1853-863X; Giroletti,
Marcello/0000-0002-8657-8852; TORRESI, ELEONORA/0000-0002-5201-010X
FU [GO0-11133X]
FX 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. The authors would like to thanks the ASI Science Data
Center (ASDC) for providing on-line facilities for the Swift/XRT data
analysis. G.M. research is supported by Chandra grant GO0-11133X.
NR 84
TC 9
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U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A72
DI 10.1051/0004-6361/201116808
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100072
ER
PT J
AU Osborne, JP
Page, KL
Henden, AA
Ness, JU
Bode, MF
Schwarz, GJ
Starrfield, S
Drake, JJ
Kuulkers, E
Beardmore, AP
AF Osborne, J. P.
Page, K. L.
Henden, A. A.
Ness, J. -U.
Bode, M. F.
Schwarz, G. J.
Starrfield, S.
Drake, J. J.
Kuulkers, E.
Beardmore, A. P.
TI Swift observations of the March 2011 outburst of the cataclysmic
variable NSV 1436: a probable dwarf nova (Research Note)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; binaries: general; stars: dwarf novae;
novae, cataclysmic variables; stars: individual: NSV 1436
ID X-RAY OBSERVATIONS; TELESCOPE
AB Aims. The March 2011 outburst of the poorly-studied cataclysmic variable NSV 1436 offered an opportunity to decide between dwarf nova and recurrent nova classifications.
Methods. We use seven daily observations in the X-ray and UV by the Swift satellite, together with AAVSO V photometry, to characterise the outburst and decline behaviour.
Results. The short optical outburst coincided with a faint and relatively soft X-ray state, whereas in decline to fainter optical magnitudes the X-ray source was harder and brighter. These attributes, and the modest optical outburst amplitude, indicate that this was a dwarf nova outburst and not a recurrent nova. The rapid optical fading suggests an orbital period below 2 h.
C1 [Osborne, J. P.; Page, K. L.; Beardmore, A. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Henden, A. A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA.
[Ness, J. -U.] ESAC, XMM Newton Sci Operat Ctr, Madrid 28691, Spain.
[Bode, M. F.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LDS, Merseyside, England.
[Schwarz, G. J.] Amer Astron Soc, Austin, TX USA.
[Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kuulkers, E.] ESAC, INTEGRAL Sci Operat Ctr, Madrid 28691, Spain.
RP Osborne, JP (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
EM julo@star.le.ac.uk
FU UK Space Agency; NSF; NASA
FX We thank the Swift operations team and PI for their support of these
observations. J.P.O., K.L.P. and A.P.B. acknowledge financial support
from the UK Space Agency. S.S. is grateful to the NSF and to NASA for
partial support. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester.
NR 17
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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 SEP
PY 2011
VL 533
AR A41
DI 10.1051/0004-6361/201117088
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100041
ER
PT J
AU Singh, V
Shastri, P
Risaliti, G
AF Singh, V.
Shastri, P.
Risaliti, G.
TI Measuring the level of nuclear activity in Seyfert galaxies and the
unification scheme
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: Seyfert; X-rays: galaxies; galaxies: active
ID HARD X-RAY; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES;
BRIGHT QUASAR SURVEY; GALACTIC NUCLEI; UNIFIED MODEL; NEARBY GALAXIES;
EMISSION-LINE; ACCRETION; SAMPLE
AB Context. The unification scheme of Seyfert galaxies hypothesizes that Seyfert type 1s and type 2s are intrinsically similar and the observed differences between the two subtypes are solely due to the differing orientations of toroidal-shaped obscuring material around the AGN. In the framework of the unification scheme, both the Seyfert subtypes are expected to show similar intrinsic nuclear properties such as the absorption-corrected AGN X-ray luminosity, bolometric luminosity, accretion rate and the mass of the supermassive black hole.
Aims. To test the predictions of the Seyfert unification scheme, we make statistical comparison of the distributions of: (i) the absorption-corrected 2.0-10 keV X-ray luminosities; (ii) the bolometric luminosities; (iii) the black hole masses and; (iv) the Eddington ratios, of Seyfert type 1s and type 2s.
Methods. We use an optically selected Seyfert sample in which type 1s and type 2s are matched in properties that are independent to the orientation of the obscuring torus, the AGN axis and the host galaxy.
Results. The distributions of the absorption-corrected 2.0-10 keV X-ray luminosities (L2.0-10 (c)(keV)), the bolometric luminosities (L-Bol), the black masses (M-BH) and, the Eddington ratios (lambda) are statistically similar for the two Seyfert subtypes, consistent with the orientation and obscuration based Seyfert unification scheme. The Eddington ratio distributions suggest that both the Seyfert subtypes are accreting at sub-Eddington level with wide span of Eddington ratios i. e., 10(-4)- 10(-1).
C1 [Singh, V.; Shastri, P.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Singh, V.] Univ Calicut, Dept Phys, Calicut 673635, Kerala, India.
[Risaliti, G.] INAF Osservatorio Arcetri, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Singh, V (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
EM veeresh@iiap.res.in
OI Risaliti, Guido/0000-0002-3556-977X
NR 68
TC 8
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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 SEP
PY 2011
VL 533
AR A128
DI 10.1051/0004-6361/201117422
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100128
ER
PT J
AU Straub, O
Bursa, M
Sadowski, A
Steiner, JF
Abramowicz, MA
Kluzniak, W
McClintock, JE
Narayan, R
Remillard, RA
AF Straub, O.
Bursa, M.
Sadowski, A.
Steiner, J. F.
Abramowicz, M. A.
Kluzniak, W.
McClintock, J. E.
Narayan, R.
Remillard, R. A.
TI Testing slim-disk models on the thermal spectra of LMC X-3
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries
ID BLACK-HOLE BINARIES; X-RAY BINARIES; ACCRETION DISK; VERTICAL STRUCTURE;
SPIN; OUTFLOW; THIN
AB Slim-disk models describe advective accretion flows at high luminosities, while reducing to the standard thin disk form in the low luminosity limit. We have developed a new spectral model, slimbb, within the framework of XSPEC, which describes fully relativistic slim-disk accretion and includes photon ray-tracing that starts from the disk photosphere, rather than the equatorial plane. We demonstrate the features of this model by applying it to RXTE spectra of the persistent black-hole X-ray binary LMC X-3. LMC X-3 has the virtues of exhibiting large intensity variations while maintaining itself in soft spectral states which are well described using accretion-disk models, making it an ideal candidate to test the aptness of slimbb. Our results demonstrate consistency between the low-luminosity (thin-disk) and high luminosity (slim-disk) regimes. The results also illustrate that advection alone does not solve the problem of the origin of the surprisingly soft high-luminosity spectra in LMC X-3. We show that X-ray continuum-fitting in the high accretion rate regime can powerfully test black-hole accretion disk models.
C1 [Straub, O.; Sadowski, A.; Abramowicz, M. A.; Kluzniak, W.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Bursa, M.] Acad Sci Czech Republic, Inst Astron, Prague 14131, Czech Republic.
[Steiner, J. F.; McClintock, J. E.; Narayan, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Abramowicz, M. A.] Gothenburg Univ, Dept Phys, S-41296 Gothenburg, Sweden.
[Remillard, R. A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Straub, O (reprint author), Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland.
EM odele@camk.edu.pl
RI Bursa, Michal/G-9004-2014;
OI Narayan, Ramesh/0000-0002-1919-2730
FU Polish Ministry of Science [NN203 383136, NN203 381436]; Czech MSMT
[LC06014, ME09036]; Swedish VR
FX We gratefully acknowledge the Polish Ministry of Science grants NN203
383136 (O.S.) and NN203 381436 (W.K.), the Czech MSMT grants LC06014 and
ME09036 (M.B.) and the Swedish VR grant (M.A.).
NR 34
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U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR A67
DI 10.1051/0004-6361/201117385
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100067
ER
PT J
AU Vidal-Madjar, A
Huitson, CM
des Etangs, AL
Sing, DK
Ferlet, R
Desert, JM
Hebrard, G
Boisse, I
Ehrenreich, D
Moutou, C
AF Vidal-Madjar, A.
Huitson, C. M.
des Etangs, A. Lecavelier
Sing, D. K.
Ferlet, R.
Desert, J. -M.
Hebrard, G.
Boisse, I.
Ehrenreich, D.
Moutou, C.
TI The upper atmosphere of the exoplanet HD209458b revealed by the sodium D
lines: temperature-pressure profile, ionization layer and thermosphere
(vol 527, pg A110, 2011)
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Correction
DE methods: observational; techniques: spectroscopic; planets and
satellites: atmospheres; methods: data analysis; Errata, addenda; stars:
individual: HD209458
C1 [Vidal-Madjar, A.; des Etangs, A. Lecavelier; Ferlet, R.; Hebrard, G.; Boisse, I.] Inst Astrophys Paris, CNRS, UPMC, UMR 7095, F-75014 Paris, France.
[Huitson, C. M.; Sing, D. K.] Univ Exeter, Astrophys Grp, Sch Phys, Exeter EX4 4QL, Devon, England.
[Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Ehrenreich, D.] Univ Grenoble 1, Lab Astrophys Grenoble, CNRS, UMR 5571, F-38041 Grenoble 9, France.
[Moutou, C.] Lab Astrophys Marseille, F-13013 Marseille, France.
RP Vidal-Madjar, A (reprint author), Inst Astrophys Paris, CNRS, UPMC, UMR 7095, 98Bis Blvd Arago, F-75014 Paris, France.
EM alfred@iap.fr
NR 5
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U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
AR C4
DI 10.1051/0004-6361/201015698e
PG 2
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100147
ER
PT J
AU Zhang, Z
Gilfanov, M
Voss, R
Sivakoff, GR
Kraft, RP
Brassington, NJ
Kundu, A
Jordan, A
Sarazin, C
AF Zhang, Z.
Gilfanov, M.
Voss, R.
Sivakoff, G. R.
Kraft, R. P.
Brassington, N. J.
Kundu, A.
Jordan, A.
Sarazin, C.
TI Luminosity functions of LMXBs in different stellar environments
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays: binaries; globular clusters: general
ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; EARLY-TYPE GALAXIES; CHANDRA
MONITORING OBSERVATIONS; GLOBULAR-CLUSTER CONNECTION; ELLIPTIC GALAXIES;
POINT SOURCES; DEEP CHANDRA; CENTAURUS-A; FIELD
AB Aims. Based on the archival data from the Chandra observations of nearby galaxies, we study different sub populations of low-mass X-ray binaries (LMXBs) - dynamically formed systems in globular clusters (GCs) and in the nucleus of M 31 and (presumably primordial) X-ray binaries in the fields of galaxies. Our aim is to produce accurate luminosity distributions of X-ray binaries in different environments, suitable for quantitative comparison with each other and with the output of population synthesis calculations.
Methods. Our sample includes seven nearby galaxies (M 31, Maffei 1, Centaurus A, M 81, NGC 3379, NGC 4697, and NGC 4278) and the Milky Way, which together provide relatively uniform coverage down to the luminosity limit of 10(35) erg s(-1). In total we have detected 185 LMXBs associated with GCs, 35 X-ray sources in the nucleus of M 31, and 998 field sources of which similar to 365 are expected to be background AGN. We combine these data, taking special care to accurately account for X-ray and optical incompleteness corrections and the removal of the contamination from the cosmic X-ray background sources, to produce luminosity distributions of X-ray binaries in different environments to far greater accuracy than has been obtained previously.
Results. We found that luminosity distributions of GC and field LMXBs differ throughout the entire luminosity range, the fraction of faint (log(L-X) < 37) sources among the former being similar to 4 times less than in the field population. The X-ray luminosity function (XLF) of sources in the nucleus of M 31 is similar to that of GC sources at the faint end but differs at the bright end, with the M 31 nucleus hosting significantly fewer bright sources. We discuss the possible origin and potential implications of these results.
C1 [Zhang, Z.; Gilfanov, M.] Max Planck Inst Astrophys, D-85740 Garching, Germany.
[Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
[Voss, R.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Sivakoff, G. R.; Sarazin, C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[Kraft, R. P.; Brassington, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brassington, N. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Kundu, A.] Eureka Sci, Oakland, CA 94602 USA.
[Jordan, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile.
RP Zhang, Z (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany.
EM zzhang@mpa-garching.mpg.de; gilfanov@mpa-garching.mpg.de
RI Sivakoff, Gregory/G-9602-2011;
OI Sivakoff, Gregory/0000-0001-6682-916X; Jordan,
Andres/0000-0002-5389-3944
FU BASAL CATA [PFB-06]; FONDAP [CFA 15010003]; MIDEPLAN ICM Nucleus
[P07-021-F]; Anillo [ACT-086]
FX We thank Mark B. Peacock for the help with the GC catalog in M 31 and
Akos Bogdan for helpful discussions. This research made use of Chandra
archival data provided by Chandra X-ray Center, 2MASS Large Galaxy Atlas
data provided by NASA/IPAC infrared science archive, and ASM RXTE data
from HEASARC online service. Andres Jordan acknowledges support from
BASAL CATA PFB-06, FONDAP CFA 15010003, MIDEPLAN ICM Nucleus P07-021-F
and Anillo ACT-086. We thank the referee for helpful remarks on this
paper.
NR 49
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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 SEP
PY 2011
VL 533
AR A33
DI 10.1051/0004-6361/201116936
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100033
ER
PT J
AU Zwintz, K
Lenz, P
Breger, M
Pamyatnykh, AA
Zdravkov, T
Kuschnig, R
Matthews, JM
Guenther, DB
Moffat, AFJ
Rowe, JF
Rucinski, SM
Sasselov, D
Weiss, WW
AF Zwintz, K.
Lenz, P.
Breger, M.
Pamyatnykh, A. A.
Zdravkov, T.
Kuschnig, R.
Matthews, J. M.
Guenther, D. B.
Moffat, A. F. J.
Rowe, J. F.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI Regular frequency patterns in the classical delta Scuti star HD 144277
observed by the MOST satellite
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: oscillations; techniques: photometric; asteroseismology; stars:
variables: delta Scuti; stars: individual: HD 144277
ID RAPIDLY ROTATING STARS; SPACE; OPACITIES; PHOTOMETRY; PULSATION;
VARIABLES; SPECTRA; CLUSTER; MODES
AB Context. We present high-precision time-series photometry of the classical delta Scuti star HD 144277 obtained with the MOST (Microvariability and Oscillations of STars) satellite in two consecutive years. The observed regular frequency patterns are investigated asteroseismologically.
Aims. HD 144277 is a hot A-type star that is located on the blue border of the classical instability strip. While we mostly observe low radial order modes in classical delta Scuti stars, HD 144277 presents a different case. Its high observed frequencies, i.e., between 59.9 d(-1) (693.9 mu Hz) and 71.1 d(-1) (822.8 mu Hz), suggest higher radial orders. We examine the progression of the regular frequency spacings from the low radial order to the asymptotic frequency region.
Methods. Frequency analysis was performed using Period04 and SigSpec. The results from the MOST observing runs in 2009 and 2010 were compared to each other. The resulting frequencies were submitted to asteroseismic analysis.
Results. HD 144277 was discovered to be a delta Scuti star using the time-series photometry observed by the MOST satellite. Twelve independent pulsation frequencies lying in four distinct groups were identified. Two additional frequencies were found to be combination frequencies. The typical spacing of 3.6 d(-1) corresponds to the spacing between subsequent radial and dipole modes, therefore the spacing between radial modes is twice this value, 7.2 d(-1). Based on the assumption of slow rotation, we find evidence that the two radial modes are the sixth and seventh overtones, and the frequency with the highest amplitude can be identified as a dipole mode.
Conclusions. The models required to fit the observed instability range need slightly less metallicity and a moderate enhancement of the helium abundance compared to the standard chemical composition. Our asteroseismic models suggest that HD 144277 is a delta Scuti star close to the ZAMS with a mass of 1.66 M(circle dot).
C1 [Zwintz, K.; Breger, M.; Pamyatnykh, A. A.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Lenz, P.; Pamyatnykh, A. A.; Zdravkov, T.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
[Breger, M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Pamyatnykh, A. A.] Russian Acad Sci, Inst Astron, Moscow 109017, Russia.
[Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[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.
[Rowe, J. F.] NASA, Moffett Field, CA 94035 USA.
[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 konstanze.zwintz@univie.ac.at
OI Zwintz, Konstanze/0000-0001-9229-8315
FU Polish MNiSW [N N203 379 636]; Austrian Fonds zur Forderung der
wissenschaftlichen Forschung [P21830-N16, P22691-N16]; Austrian Academy
of Sciences at the Institute of Astronomy of the University of Vienna
FX We are grateful to Gerald Handler, who obtained the Stroemgren
photometry for HD 144277 for us at the SAAO 50 cm telescope. K.Z. is
recipient of an APART fellowship of the Austrian Academy of Sciences at
the Institute of Astronomy of the University of Vienna. P.L.,A.A.P., and
T.Z. acknowledge partial financial support from the Polish MNiSW grant
No. N N203 379 636. M.B. and W.W.W. acknowledge support by the Austrian
Fonds zur Forderung der wissenschaftlichen Forschung (MB: project
P21830-N16; WWW: project P22691-N16).
NR 27
TC 5
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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 SEP
PY 2011
VL 533
AR A133
DI 10.1051/0004-6361/201117272
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100133
ER
PT J
AU Bolin, JF
Bray, RD
Musselman, LJ
AF Bolin, Jay F.
Bray, Rebecca D.
Musselman, Lytton John
TI A New Species of Diploid Quillwort (Isoetes, Isoetaceae, Lycophyta) from
Lebanon
SO NOVON
LA English
DT Article
DE Isoetaceae; Isoetes; IUCN Red List; Lebanon; Lycophyta
AB A new species, Isoetes libanotica Musselman, Bolin & B. D. Bray (Isoetaceae, Lycophyta), is described from Akkar District of northern Lebanon. It is a seasonal terrestrial species of basaltic soils, diploid (2n = 22), with complete velum coverage. Megaspore diameter ranges from 338 to 477 mu m with remote, low tuberculate ornamentation and a low to obsolete equatorial girdle; microspore length ranges from 25 to 30 mu m, with echinate ornamentation. At the type locality of I. libanotica, two other Isoetes L. species occur sympatrically. These superficially similar Isoetes species can be differentiated from I. libanotica using megaspore characters; I. duriei Bory has larger alveolate megaspores and I. olympica A. Braun has a prominent equatorial girdle.
C1 [Bolin, Jay F.; Bray, Rebecca D.; Musselman, Lytton John] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
[Bolin, Jay F.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
RP Musselman, LJ (reprint author), Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA.
EM bolinj@si.edu; rbray@odu.edu; lmusselm@odu.edu
NR 6
TC 5
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U1 1
U2 1
PU MISSOURI BOTANICAL GARDEN
PI ST LOUIS
PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA
SN 1055-3177
J9 NOVON
JI Novon
PD SEP
PY 2011
VL 21
IS 3
BP 295
EP 298
DI 10.3417/2010028
PG 4
WC Plant Sciences
SC Plant Sciences
GA 824NK
UT WOS:000295208400001
ER
PT J
AU Allali, HA
Collin, R
Lopez-Bautista, JM
AF Allali, H. A.
Collin, R.
Lopez-Bautista, J. M.
TI DIVERSITY AND DISTRIBUTION OF EPIPHYTIC SUBAERIAL ALGAE IN A PANAMANIAN
FOREST
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Allali, H. A.; Lopez-Bautista, J. M.] Univ Alabama, Tuscaloosa, AL 35487 USA.
[Collin, R.] Smithsonian Trop Res Inst, Panama City, Panama.
EM allal001@crimson.ua.edu; collinr@si.edu; jlopez@ua.edu
NR 0
TC 0
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U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S76
EP S77
PG 2
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200231
ER
PT J
AU Bachvaroff, TR
Kim, S
Delwiche, CF
Coats, DW
AF Bachvaroff, T. R.
Kim, S.
Delwiche, C. F.
Coats, D. W.
TI DIVERSITY OF THE SYNDINIAN GENUS DUBOSCQUELLA
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Bachvaroff, T. R.; Coats, D. W.] Smithsonian Environm Res Ctr, Edgewater, MD USA.
[Kim, S.] Kongju Natl Univ, Gonju, South Korea.
[Delwiche, C. F.] Univ Maryland, College Pk, MD 20742 USA.
EM bachvarofft@si.edu; sunjukim75@gmail.com; delwiche@umd.edu;
coatsw@si.edu
NR 0
TC 0
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U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S29
EP S29
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200088
ER
PT J
AU Coats, DW
Bachvaroff, TR
AF Coats, D. W.
Bachvaroff, T. R.
TI SYNDINIAN SEX
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Coats, D. W.; Bachvaroff, T. R.] Smithsonian Environm Res Ctr, Edgewater, MD USA.
EM coatsw@si.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S23
EP S23
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200068
ER
PT J
AU Fredericq, S
Krayesky, D
Gabriel, D
Norris, JN
Schmidt, WE
AF Fredericq, S.
Krayesky, D.
Gabriel, D.
Norris, J. N.
Schmidt, W. E.
TI NEW TAXONOMIC CONCEPTS IN THE GENERA OF THE PEYSSONNELIACEAE
(PEYSSONNELIALES, RHODOPHYTA) WITH FOCUS ON TAXA FROM THE GULF OF MEXICO
AND PANAMA
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Fredericq, S.; Schmidt, W. E.] Univ Louisiana, Lafayette, LA 70504 USA.
[Krayesky, D.] Slippery Rock Univ, Slippery Rock, PA 16057 USA.
[Gabriel, D.] Univ Acores, Azores, Portugal.
[Norris, J. N.] Smithsonian Inst, NMNH, Washington, DC 20560 USA.
EM slf9209@louisiana.edu; david.krayesky@sru.edu;
danielalgabriel@gmail.com; norrisj@si.edu; weschmidt01@yahoo.com
NR 0
TC 0
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U1 1
U2 2
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S43
EP S43
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200129
ER
PT J
AU Kim, M
Nam, SW
Shin, W
Coats, DW
Park, MG
AF Kim, M.
Nam, S. W.
Shin, W.
Coats, D. W.
Park, M. G.
TI THE MARINE DINOFLAGELLATE GENUS DINOPHYSIS IS ON THE WAY TO GAINING
PLASTIDS
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Kim, M.; Park, M. G.] Chonnam Natl Univ, Kwangju, South Korea.
[Nam, S. W.; Shin, W.] Chungnam Natl Univ, Taejon, South Korea.
[Coats, D. W.] Smithsonian Environm Res Ctr, Edgewater, MD USA.
EM kmr1230@hanmail.net
NR 0
TC 1
Z9 1
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S27
EP S27
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200081
ER
PT J
AU Krayesky, DM
Norris, JN
West, JA
Fredericq, SL
AF Krayesky, D. M.
Norris, J. N.
West, J. A.
Fredericq, S. L.
TI A NEW SPECIES OF CALOGLOSSA (DELESSERIACEAE, RHODOPHYTA) FROM THE
COASTLINE OF THE WESTERN ATLANTIC
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Krayesky, D. M.] Slippery Rock Univ, Slippery Rock, PA 16057 USA.
[Norris, J. N.] Smithsonian Inst, Washington, DC 20560 USA.
[West, J. A.] Univ Melbourne, Melbourne, Vic 3010, Australia.
[Fredericq, S. L.] Univ Louisiana Lafayette, Lafayette, LA USA.
EM david.krayesky@sru.edu; NORRISJ@si.edu; jwest@unimelb.edu.au;
slf9209@louisiana.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S74
EP S74
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200223
ER
PT J
AU Laughinghouse, HD
Adey, WH
Miller, J
AF Laughinghouse, H. D.
Adey, W. H.
Miller, J.
TI ALGAL TURF PRODUCTION ON THE GREAT WICOMICO RIVER, VA, USA: DIVERSITY
AND BIOCHEMISTRY OF AN ALGAL TURF SCRUBBER (ATS)
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Laughinghouse, H. D.] Univ Maryland, NMNH, Smithsonian Inst, College Pk, MD 20742 USA.
[Laughinghouse, H. D.] Univ Maryland, MEES Program, CMNS, College Pk, MD 20742 USA.
[Miller, J.] Western Michigan Univ, Kalamazoo, MI 49008 USA.
[Adey, W. H.] Smithsonian Inst, NMNH, Washington, DC 20560 USA.
EM hdliv@hotmail.com
RI Adey, Walter/G-2858-2011
NR 0
TC 0
Z9 0
U1 0
U2 12
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S66
EP S67
PG 2
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200201
ER
PT J
AU Litaker, RW
Holland, WC
Kibler, SR
Vandersea, MW
Faust, MA
Tester, PA
AF Litaker, R. W.
Holland, W. C.
Kibler, S. R.
Vandersea, M. W.
Faust, M. A.
Tester, P. A.
TI PROROCENTRUM MEXICANUM VS. PROROCENTRUM RHATHYMUM: COMPARATIVE TAXONOMY,
ECOLOGY AND TOXICOLOGY
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Litaker, R. W.; Holland, W. C.; Kibler, S. R.; Vandersea, M. W.; Tester, P. A.] NOAA, Silver Spring, MD USA.
[Faust, M. A.] Smithsonian Inst, Washington, DC 20560 USA.
EM wayne.litaker@noaa.gov
NR 0
TC 0
Z9 0
U1 1
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S69
EP S69
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200209
ER
PT J
AU Werner, VR
Laughinghouse, HD
Fiore, MF
Sant'Anna, CL
Hoff, C
Santos, KR
Neuhaus, EB
Molica, RJ
Honda, RY
Echenique, RO
AF Werner, V. R.
Laughinghouse, H. D.
Fiore, M. F.
Sant'Anna, C. L.
Hoff, C.
Santos, K. R.
Neuhaus, E. B.
Molica, R. J.
Honda, R. Y.
Echenique, R. O.
TI SPHAEROSPERMOPSIS TORQUES-REGINAE (CYANOBACTERIA, NOSTOCALES) COMB. NOV
FROM SOUTH AMERICAN WATER BLOOMS
SO JOURNAL OF PHYCOLOGY
LA English
DT Meeting Abstract
C1 [Werner, V. R.; Neuhaus, E. B.] FCNyM Univ Nac La Plata, La Plata, Buenos Aires, Argentina.
[Laughinghouse, H. D.] Univ Maryland, NMNH, Smithsonian Inst, College Pk, MD 20742 USA.
[Laughinghouse, H. D.] Univ Maryland, MEES Program, CMNS, College Pk, MD 20742 USA.
[Fiore, M. F.; Hoff, C.; Honda, R. Y.] Univ Sao Paulo, CENA, BR-05508 Sao Paulo, Brazil.
[Sant'Anna, C. L.; Santos, K. R.] Inst Bot Sao Paulo, Phycol Sect, Sao Paulo, Brazil.
[Molica, R. J.] Univ Fed Rural Pernambuco, Recife, PE, Brazil.
EM vera-werner@fzb.rs.gov.br; hdliv@hotmail.com
RI SantAnna, Celia/G-2420-2012; Molica, Renato /J-2630-2012; Sant' Anna,
Celia/D-3735-2015
NR 0
TC 1
Z9 1
U1 0
U2 3
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD SEP
PY 2011
VL 47
SU 2
SI SI
BP S77
EP S77
PG 1
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 822ZO
UT WOS:000295090200232
ER
PT J
AU Gordon, IE
Rothman, LS
Toon, GC
AF Gordon, Iouli E.
Rothman, Laurence S.
Toon, Geoffrey C.
TI Revision of spectral parameters for the B- and gamma-bands of oxygen and
their validation against atmospheric spectra
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE HITRAN; Oxygen spectroscopy; B-band; gamma-Band
ID MOLECULAR SPECTROSCOPIC DATABASE; O-2 A-BAND; SELF-BROADENING
COEFFICIENTS; RING-DOWN SPECTROSCOPY; ABSORPTION-SPECTROSCOPY; INTENSITY
MEASUREMENTS; LINE PARAMETERS; RESOLUTION; PRESSURE; O-16(2)
AB Until recently the B (b(1)Sigma(+)(g) (nu=1)-X-3 Sigma(-)(g) (nu=0)) and gamma (b(1)Sigma(+)(g) (nu=2)-X-3 Sigma(-)(g) (nu=0)) bands of oxygen in the visible region had not been used extensively in satellite remote sensing of the atmosphere. These bands roughly cover the regions around 14,527 and 15,904 cm(-1), respectively (0.69 and 0.63 mu m). However, these bands (in particular the B-band) are now being increasingly considered for future satellite missions. In this light, it is important to make sure that the reference spectroscopic parameters allow accurate retrieval of important physical characteristics from the atmospheric spectra. The spectroscopic parameters currently given for these bands in the HITRAN2008 spectroscopic database were tested against high-resolution atmospheric spectra measured with solar-pointing Fourier transform spectrometers at Park Falls, Wisconsin (B-band) and Kitt Peak, Arizona (gamma-band). It was found that the current HITRAN parameters cannot produce satisfactory fits of the observed spectra. In order to improve the database we have collected the best available measured line positions that involve the b(1)E(g)(+) (nu=1 and nu=2) states for the three most abundant isotopologues of oxygen and performed a combined fit to obtain a consistent set of spectroscopic constants. These constants were then used to calculate the line positions. A careful review of the available intensity and line-shape measurements was also carried out, and new parameters were derived based on that review. In particular, line shift parameters, that were not previously available, were introduced. The new data have been validated using the high-resolution atmospheric spectra measured with the Fourier transform spectrometers at Park Falls, Wisconsin (B-band) and Kitt Peak, Arizona (gamma-band) and have yielded substantial improvement. In addition, we report the first direct observation and analysis of the (OO)-O-16-O-18 lines in the gamma-band. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM igordon@cfa.harvard.edu
OI Gordon, Iouli/0000-0003-4763-2841
FU NASA [NAG5-13534]
FX We would like to thank Joseph Hodges and Daniel Lisak for providing us
with unpublished line position measurements of five transitions in the
B-band. Helpful discussions with Linda Brown and Caroline Nowlan are
much appreciated. The work carried out at the Harvard-Smithsonian Center
for Astrophysics was supported by NASA through the Earth Observing
System (EOS) under grant NAG5-13534. Part of this work was performed at
the Jet Propulsion Laboratory, California Institute of Technology, under
contract with NASA We thank the Kitt Peak National Observatory, and the
Total Column Carbon Observing Network (TCCON) for providing the
atmospheric spectra used to validate the new line lists.
NR 44
TC 20
Z9 20
U1 0
U2 11
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 SEP
PY 2011
VL 112
IS 14
BP 2310
EP 2322
DI 10.1016/j.jqsrt.2011.05.007
PG 13
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 823FW
UT WOS:000295108900007
ER
PT J
AU Yang, J
Goldstein, JI
Scott, ERD
Michael, JR
Kotula, PG
Pham, T
McCoy, TJ
AF Yang, J.
Goldstein, J. I.
Scott, E. R. D.
Michael, J. R.
Kotula, P. G.
Pham, T.
McCoy, T. J.
TI Thermal and impact histories of reheated group IVA, IVB, and ungrouped
iron meteorites and their parent asteroids
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID FE-NI-P; METALLOGRAPHIC COOLING RATES; CHEMICAL CLASSIFICATION; GE
CONCENTRATIONS; PHASE-DIAGRAM; MICROSTRUCTURE; SYSTEM; IIIAB; METAL;
PLANETESIMALS
AB The microstructures of six reheated iron meteoritesotwo IVA irons, Maria Elena (1935), Fuzzy Creek; one IVB iron, Ternera; and three ungrouped irons, Hammond, Babb's Mill (Blake's Iron), and Babb's Mill (Troost's Iron)owere characterized using scanning and transmission electron microscopy, electron-probe microanalysis, and electron backscatter diffraction techniques to determine their thermal and shock history and that of their parent asteroids. Maria Elena and Hammond were heated below approximately 700-750 degrees C, so that kamacite was recrystallized and taenite was exsolved in kamacite and was spheroidized in plessite. Both meteorites retained a record of the original Widmanstitten pattern. The other four, which show no trace of their original microstructure, were heated above 600-700 degrees C and recrystallized to form 10-20 mu m wide homogeneous taenite grains. On cooling, kamacite formed on taenite grain boundaries with their close-packed planes aligned. Formation of homogeneous 20 mu m wide taenite grains with diverse orientations would have required as long as approximately 800 yr at 600 degrees C or approximately 1 h at 1300 degrees C. All six irons contain approximately 5-10 mu m wide taenite grains with internal microprecipitates of kamacite and nanometer-scale M-shaped Ni profiles that reach approximately 40% Ni indicating cooling over 100-10,000 yr. Un-decomposed high-Ni martensite (alpha(2)) in taeniteothe first occurrence in ironsoappears to be a characteristic of strongly reheated irons. From our studies and published work, we identified four progressive stages of shock and reheating in IVA irons using these criteria: cloudy taenite, M-shaped Ni profiles in taenite, Neumann twin lamellae, martensite, shock-hatched kamacite, recrystallization, microprecipitates of taenite, and shock-melted troilite. Maria Elena and Fuzzy Creek represent stages 3 and 4, respectively. Although not all reheated irons contain evidence for shock, it was probably the main cause of reheating. Cooling over years rather than hours precludes shock during the impacts that exposed the irons to cosmic rays. If the reheated irons that we studied are representative, the IVA irons may have been shocked soon after they cooled below 200 degrees C at 4.5 Gyr in an impact that created a rubblepile asteroid with fragments from diverse depths. The primary cooling rates of the IVA irons and the proposed early history are remarkably consistent with the Pb-Pb ages of troilite inclusions in two IVA irons including the oldest known differentiated meteorite (Blichert-Toft et al. 2010).
C1 [Yang, J.; Goldstein, J. I.; Pham, T.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA.
[Yang, J.] Carl Zeiss NTS LLC, Peabody, MA 01960 USA.
[Scott, E. R. D.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 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.
EM jiyang@ecs.umass.edu
RI Kotula, Paul/A-7657-2011
OI Kotula, Paul/0000-0002-7521-2759
FU NASA [NNX08AG53G, NNG06GF56G, NNX08AI43G]
FX Financial support from NASA through grants NNX08AG53G (J. I. Goldstein,
P. I.), NNG06GF56G (T. J. McCoy), and NNX08AI43G (E. R. D. Scott, P. I.)
is acknowledged. We thank Laurence Garvie (Arizona State University),
Joseph Boesenberg and Denton Ebel (American Museum of Natural History),
and Valerie Reynolds (Colby College) for helpful discussions and
assistance with the source(s) of the Babb's Mill specimens. We thank
Alice Kilgo (Sandia) for metallographic preparation, and Michael Rye and
Garry Bryant (both from Sandia) for FIB preparation. Our research was
aided considerably by Vagn Buchwald's Handbook of Iron Meteorites, as it
contributed enormously to our understanding of cosmically and
terrestrially reheated iron meteorites. We thank Henning Haack, Alan
Rubin, and an anonymous referee for their helpful and detailed reviews.
NR 66
TC 13
Z9 13
U1 3
U2 17
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 SEP
PY 2011
VL 46
IS 9
BP 1227
EP 1252
DI 10.1111/j.1945-5100.2011.01210.x
PG 26
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 822MY
UT WOS:000295053300001
ER
PT J
AU Steiner, JF
Reis, RC
McClintock, JE
Narayan, R
Remillard, RA
Orosz, JA
Gou, LJ
Fabian, AC
Torres, MAP
AF Steiner, James F.
Reis, Rubens C.
McClintock, Jeffrey E.
Narayan, Ramesh
Remillard, Ronald A.
Orosz, Jerome A.
Gou, Lijun
Fabian, Andrew C.
Torres, Manuel A. P.
TI The spin of the black hole microquasar XTE J1550-564 via the
continuum-fitting and Fe-line methods
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; stars: individual: XTE
J1550-564; X-rays: binaries
ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; QUASI-PERIODIC OSCILLATIONS;
ACCRETION DISK MODELS; NOVA-MUSCAE 1991; ENERGY-SPECTRA; HIGH-STATE;
INTERSTELLAR-MEDIUM; 2000 OUTBURST; GRS 1915+105
AB We measure the spin of XTE J1550-564 using the two leading methods: (i) modelling the thermal continuum spectrum of the accretion disc; and (ii) modelling the broad red wing of the reflection fluorescence Fe K alpha line. We find that these two independent measurements of spin are in agreement. For the continuum-fitting analysis, we use a data sample consisting of several dozen Rossi X-ray Timing Explorer spectra, and for the Fe K alpha analysis, we use a pair of ASCA spectra from a single epoch. Our spin estimate for the black hole primary using the continuum-fitting method is -0.11 < a* < 0.71 (90 per cent confidence), with a most likely spin of a* = 0.34. In obtaining this result, we have thoroughly explored the dependence of the spin value on a wide range of model-dependent systematic errors and observational errors; our precision is limited by uncertainties in the distance and orbital inclination of the system. For the Fe-line method, our estimate of spin is a* = 0.55(-0.22)(+0.15). Combining these results, we conclude that the spin of this black hole is moderate, a* = 0.49(-0.20)(+0.13), which suggests that the jet activity of this microquasar is powered largely by its accretion disc rather than by the spin energy of the black hole.
C1 [Steiner, James F.; McClintock, Jeffrey E.; Narayan, Ramesh; Gou, Lijun; Torres, Manuel A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Reis, Rubens C.; Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Torres, Manuel A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands.
RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jsteiner@cfa.harvard.edu; rcr36@ast.cam.ac.uk
OI reis, rubens/0000-0002-6618-2412; Narayan, Ramesh/0000-0002-1919-2730
FU Smithsonian Institution; NASA [NNX08AJ55G, NNX08AH32G]; NSF
[AST-0805832]; Science and Technology Research Council; Smithsonian
Astrophysical Observatory
FX JFS was supported by the Smithsonian Institution Endowment Funds and JEM
acknowledges support from NASA grant NNX08AJ55G. RN acknowledges support
from NASA grant NNX08AH32G and NSF grant AST-0805832. RCR would like to
thank the Science and Technology Research Council and the Smithsonian
Astrophysical Observatory for financial support. JFS thanks Bob Penna
and Sasha Tchekhovskoy for helpful discussions, and the FAS Sciences
Division Research Computing Group for their technical support with
analyses performed on the Odyssey cluster.
NR 109
TC 71
Z9 73
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 2
BP 941
EP 958
DI 10.1111/j.1365-2966.2011.19089.x
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900011
ER
PT J
AU Galvan-Madrid, R
Peters, T
Keto, ER
Mac Low, MM
Banerjee, R
Klessen, RS
AF Galvan-Madrid, Roberto
Peters, Thomas
Keto, Eric R.
Mac Low, Mordecai-Mark
Banerjee, Robi
Klessen, Ralf S.
TI Time variability in simulated ultracompact and hypercompact H II regions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; stars: massive; H II regions
ID MASSIVE STAR-FORMATION; COMPACT HII-REGIONS; G24.78+0.08 A1; ACCRETION;
GAS; G10.6-0.4; EVOLUTION; RADIATION; COLLAPSE; FEEDBACK
AB Ultracompact and hypercompact H II regions appear when a star with a mass larger than about 15 M-circle dot starts to ionize its own environment. Recent observations of time variability in these objects are one of the pieces of evidence that suggest that at least some of them harbour stars that are still accreting from an infalling neutral accretion flow that becomes ionized in its innermost part. We present an analysis of the properties of the H II regions formed in the three-dimensional radiation-hydrodynamic simulations presented by Peters et al. as a function of time. Flickering of the H II regions is a natural outcome of this model. The radio-continuum fluxes of the simulated H II regions as well as their flux and size variations are in agreement with the available observations. From the simulations, we estimate that a small but non-negligible fraction (similar to 10 per cent) of observed H II regions should have detectable flux variations (larger than 10 per cent) on time-scales of similar to 10 yr, with positive variations being more likely to happen than negative variations. A novel result of these simulations is that negative flux changes do happen, in contrast to the simple expectation of ever growing H II regions. We also explore the temporal correlations between properties that are directly observed (flux and size) and other quantities like density and ionization rates.
C1 [Galvan-Madrid, Roberto; Peters, Thomas; Keto, Eric R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Galvan-Madrid, Roberto] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Galvan-Madrid, Roberto] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Peters, Thomas; Banerjee, Robi; Klessen, Ralf S.] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany.
[Mac Low, Mordecai-Mark] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA.
RP Galvan-Madrid, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rgalvan@cfa.harvard.edu; thomas.peters@ita.uni-heidelberg.de
OI Mac Low, Mordecai-Mark/0000-0003-0064-4060
FU SAO; ASIAA; Annette Kade; Baden-Wurttemberg Stiftung [grant
P-LS-SPII/18]; German Bundesministerium fur Bildung und Forschung via
the ASTRONET [05A09VHA]; Deutsche Forschungsgemeinschaft (DFG) [KL
1358/1, KL 1358/4, KL 1359/5, KL 1358/10, KL 1358/11]; Heidelberg
University; German Excellence Initiative; NSF [AST 08-35734]; DFG via
the Emmy-Noether [BA 3706/1-1]
FX The authors acknowledge the referee for a report that helped to clarify
the main aspects of this paper. RG-M thanks Luis F. Rodriguez for
comments on a draft of the paper. RG-M acknowledges support from the SAO
and ASIAA through an SMA pre-doctoral fellowship. TP is a fellow of the
Baden-Wurttemberg Stiftung funded by their program International
Collaboration II (grant P-LS-SPII/18). TP also acknowledges support from
an Annette Kade Fellowship for his visit to the AMNH and a Visiting
Scientist Award of the SAO. RSK acknowledges financial support from the
Baden-Wurttemberg Stiftung via their programme International
Collaboration II (grant P-LS-SPII/18) and from the German
Bundesministerium fur Bildung und Forschung via the ASTRONET project
STAR FORMAT (grant 05A09VHA). RSK furthermore gives thanks for subsidies
from the Deutsche Forschungsgemeinschaft (DFG) under grants nos KL
1358/1, KL 1358/4, KL 1359/5, KL 1358/10 and KL 1358/11, as well as from
a Frontier grant of Heidelberg University sponsored by the German
Excellence Initiative. M-MML was partly supported by NSF grant AST
08-35734. RB is funded by the DFG via the Emmy-Noether grant BA
3706/1-1. We acknowledge computing time at the Leibniz-Rechenzentrum in
Garching (Germany), the NSF-supported Texas Advanced Computing Center
(USA) and Julich Supercomputing Centre (Germany). The FLASH code was in
part developed by the DOE-supported Alliances Center for Astrophysical
Thermonuclear Flashes (ASCI) at the University of Chicago.
NR 60
TC 20
Z9 20
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 SEP
PY 2011
VL 416
IS 2
BP 1033
EP 1044
DI 10.1111/j.1365-2966.2011.19101.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900017
ER
PT J
AU Vera-Ciro, CA
Sales, LV
Helmi, A
Frenk, CS
Navarro, JF
Springel, V
Vogelsberger, M
White, SDM
AF Vera-Ciro, Carlos A.
Sales, Laura V.
Helmi, Amina
Frenk, Carlos S.
Navarro, Julio F.
Springel, Volker
Vogelsberger, Mark
White, Simon D. M.
TI The shape of dark matter haloes in the Aquarius simulations: evolution
and memory
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: haloes; dark matter
ID SAGITTARIUS DWARF GALAXY; LARGE-SCALE STRUCTURE; SKY SURVEY VIEW;
SATELLITE GALAXIES; MILKY-WAY; ANGULAR-MOMENTUM; GALACTIC HALO;
HYDRODYNAMIC SIMULATIONS; ANISOTROPIC DISTRIBUTION; MILLENNIUM
SIMULATION
AB We use the high-resolution cosmological N-body simulations from the Aquarius project to investigate in detail the mechanisms that determine the shape of Milky Way type dark matter haloes. We find that, when measured at the instantaneous virial radius, the shape of individual haloes changes with time, evolving from a typically prolate configuration at early stages to a more triaxial/oblate geometry at the present day. This evolution in halo shape correlates well with the distribution of the infalling material: prolate configurations arise when haloes are fed through narrow filaments, which characterizes the early epochs of halo assembly, whereas triaxial/oblate configurations result as the accretion turns more isotropic at later times. Interestingly, at redshift z = 0, clear imprints of the past history of each halo are recorded in their shapes at different radii, which also exhibit a variation from prolate in the inner regions to triaxial/oblate in the outskirts. Provided that the Aquarius haloes are fair representatives of Milky Way like 10(12) M-circle dot objects, we conclude that the shape of such dark matter haloes is a complex, time-dependent property, with each radial shell retaining memory of the conditions at the time of collapse.
C1 [Vera-Ciro, Carlos A.; Sales, Laura V.; Helmi, Amina] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Sales, Laura V.; White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany.
[Frenk, Carlos S.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
[Navarro, Julio F.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
[Springel, Volker] Univ Heidelberg, Zentrum Astron, Astron Recheninst, D-69120 Heidelberg, Germany.
[Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Vera-Ciro, CA (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands.
EM cavera@astro.rug.nl
OI Vera-Ciro, Carlos/0000-0002-5727-8025
FU NWO; European Research Council [GALACTICA-240271]; Royal Society; STFC
FX LVS and AH gratefully acknowledge financial support from NWO and from
the European Research Council under ERC-Starting Grant GALACTICA-240271.
CSF acknowledges a Royal Society Wolfson Research Merit Award. This work
was supported in part by an STFC rolling grant to the Institute for
Computational Cosmology at Durham. We thank the anonymous referee for
useful suggestions and comments.
NR 114
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U1 0
U2 1
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 SEP
PY 2011
VL 416
IS 2
BP 1377
EP 1391
DI 10.1111/j.1365-2966.2011.19134.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900043
ER
PT J
AU Angus, GW
Diaferio, A
Kroupa, P
AF Angus, G. W.
Diaferio, Antonaldo
Kroupa, Pavel
TI Using dwarf satellite proper motions to determine their origin
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitation; galaxies: dwarf; galaxies: evolution; Local Group; dark
matter
ID MILKY-WAY; LOCAL-GROUP; SPHEROIDAL GALAXIES; DARK-MATTER; GALACTIC
SATELLITES; CIRCULAR VELOCITY; STAR-FORMATION; LAMBDA-CDM; MASS; MOND
AB The highly organized distribution of satellite galaxies surrounding the Milky Way is a serious challenge to the concordance cosmological model. Perhaps the only remaining solution, in this framework, is that the dwarf satellite galaxies fall into the Milky Way's potential along one or two filaments, which may or may not plausibly reproduce the observed distribution. Here we test this scenario by making use of the proper motions of the Fornax, Sculptor, Ursa Minor and Carina dwarf spheroidals, and trace their orbits back through several variations of the Milky Way's potential and account for dynamical friction. The key parameters are the proper motions and total masses of the dwarf galaxies. Using a simple model, we find no tenable set of parameters that can allow Fornax to be consistent with filamentary infall, mainly because the 1 sigma error on its proper motion is relatively small. The other three must walk a tightrope between requiring a small pericentre (less than 20 kpc) to lose enough orbital energy to dynamical friction and avoiding being tidally disrupted. We then employed a more realistic model with host halo mass accretion and found that the four dwarf galaxies must have fallen in at least 5 Gyr ago. This time-interval is longer than organized distribution is expected to last before being erased by the randomization of the satellite orbits.
C1 [Angus, G. W.] Univ Cape Town, Astrophys Cosmol & Grav Ctr, ZA-7700 Rondebosch, South Africa.
[Angus, G. W.; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Angus, G. W.; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kroupa, Pavel] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
RP Angus, GW (reprint author), Univ Cape Town, Astrophys Cosmol & Grav Ctr, Private Bag X3, ZA-7700 Rondebosch, South Africa.
EM angus.gz@gmail.com
FU University of Torino, Regione Piemonte; INFN [PD51]; MIUR
FX We sincerely thank the referee for his/her careful reading of the
manuscript and for suggesting the additional test with the mass
accretion of the host halo. GWA's and AD's research is supported by the
University of Torino, Regione Piemonte, by the INFN grant PD51 and the
PRIN-MIUR-2008 grant 'Matter-antimatter asymmetry, dark matter and dark
energy in the LHC Era'.
NR 59
TC 19
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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 SEP
PY 2011
VL 416
IS 2
BP 1401
EP 1409
DI 10.1111/j.1365-2966.2011.19138.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900045
ER
PT J
AU Sing, DK
Pont, F
Aigrain, S
Charbonneau, D
Desert, JM
Gibson, N
Gilliland, R
Hayek, W
Henry, G
Knutson, H
des Etangs, AL
Mazeh, T
Shporer, A
AF Sing, D. K.
Pont, F.
Aigrain, S.
Charbonneau, D.
Desert, J. -M.
Gibson, N.
Gilliland, R.
Hayek, W.
Henry, G.
Knutson, H.
des Etangs, A. Lecavelier
Mazeh, T.
Shporer, A.
TI Hubble Space Telescope transmission spectroscopy of the exoplanet HD
189733b: high-altitude atmospheric haze in the optical and
near-ultraviolet with STIS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: spectroscopic; stars: individual: HD 189733; planetary
systems
ID EXTRASOLAR PLANET; CHEMICAL-COMPOSITION; EMISSION-SPECTRUM; HOT
JUPITERS; TEMPERATURE INVERSION; RAYLEIGH-SCATTERING; MODEL ATMOSPHERES;
MU-M; 209458B; TRANSIT
AB We present Hubble Space Telescope (HST) optical and near-ultraviolet transmission spectra of the transiting hot Jupiter HD 189733b, taken with the repaired Space Telescope Imaging Spectrograph (STIS) instrument. The resulting spectra cover the range 2900-5700 angstrom and reach per exposure signal-to-noise ratio levels greater than 11 000 within a 500-angstrom bandwidth. We used time series spectra obtained during two transit events to determine the wavelength dependence of the planetary radius and measure the exoplanet's atmospheric transmission spectrum for the first time over this wavelength range. Our measurements, in conjunction with existing HST spectra, now provide a broad-band transmission spectrum covering the full optical regime. The STIS data also show unambiguous evidence of a large occulted stellar spot during one of our transit events, which we use to place constraints on the characteristics of the K dwarf's stellar spots, estimating spot temperatures around T-eff similar to 4250 K. With contemporaneous ground-based photometric monitoring of the stellar variability, we also measure the correlation between the stellar activity level and transit-measured planet-to-star radius contrast, which is in good agreement with predictions. We find a planetary transmission spectrum in good agreement with that of Rayleigh scattering from a high-altitude atmospheric haze as previously found from HST Advanced Camera for Surveys. The high-altitude haze is now found to cover the entire optical regime and is well characterized by Rayleigh scattering. These findings suggest that haze may be a globally dominant atmospheric feature of the planet which would result in a high optical albedo at shorter optical wavelengths.
C1 [Sing, D. K.; Pont, F.; Hayek, W.] Univ Exeter, Astrophys Grp, Sch Phys, Exeter EX4 4QL, Devon, England.
[Aigrain, S.; Gibson, N.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Charbonneau, D.; Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gilliland, R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Henry, G.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Knutson, H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[des Etangs, A. Lecavelier] Univ Paris 06, Inst Astrophys Paris, CNRS, F-75014 Paris, France.
[Mazeh, T.] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel.
[Shporer, A.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
RP Sing, DK (reprint author), Univ Exeter, Astrophys Grp, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England.
EM sing@astro.ex.ac.uk
OI Gibson, Neale/0000-0002-9308-2353; Sing, David /0000-0001-6050-7645
FU NASA, STScI [GO-11740.01-A]; STFC; European Research Council under the
European Community [FP7/2007-2013, 247060]
FX We would like to thank the astronauts for their courageous work during
the HST Servicing Mission 4. We also thank Jonathan Fortney for
providing his model atmospheres, Gilda Ballester for helpful detailed
comments and our reviewer Ignas Snellen for constructive commentary.
This work is based on observations with the NASA/ESA Hubble Space
Telescope, obtained at the STScI operated by AURA, Inc. Support for this
work was provided by NASA through the GO-11740.01-A grant from the
STScI. We wish to acknowledge the support of a STFC Advanced Fellowship
(FP). WH acknowledges support by the European Research Council under the
European Community's 7th Framework Programme (FP7/2007-2013 Grant
Agreement no. 247060).
NR 58
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U2 9
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 SEP
PY 2011
VL 416
IS 2
BP 1443
EP 1455
DI 10.1111/j.1365-2966.2011.19142.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900050
ER
PT J
AU Rea, N
Torres, DF
Caliandro, GA
Hadasch, D
van der Klis, M
Jonker, PG
Mendez, M
Sierpowska-Bartosik, A
AF Rea, N.
Torres, D. F.
Caliandro, G. A.
Hadasch, D.
van der Klis, M.
Jonker, P. G.
Mendez, M.
Sierpowska-Bartosik, A.
TI Deep Chandra observations of TeV binaries - II. LS 5039
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE binaries: general; X-rays: binaries
ID X-RAY-EMISSION; PULSAR WIND NEBULA; YOUNG PULSAR; I+61 303; MILLISECOND
PULSARS; TIMING OBSERVATIONS; PSR J0218+4232; NEUTRON-STARS; DISCOVERY;
I+61-DEGREES-303
AB We report on Chandra observations of the TeV-emitting high-mass X-ray binary LS 5039, for a total exposure of similar to 70 ks, using the ACIS-S camera in continuous clocking mode to search for a possible X-ray pulsar in this system. We did not find any periodic or quasi-periodic signal in the 0.3-0.4 and 0.75-0.9 orbital phases, and in a frequency range of 0.005-175 Hz. We derived an average pulsed fraction 3 sigma upper limit for the presence of a periodic signal of less than or similar to 15 per cent (depending on the frequency and the energy band), the deepest limit ever reached for this object. If the X-ray emission of LS 5039 is due (at least in part) to a rotational powered pulsar, the latter is either spinning faster than similar to 5.6 ms, or having a beam pointing away from our line of sight, or contributing to less than or similar to 15 per cent of the total X-ray emission of the system in the orbital phases we observed.
C1 [Rea, N.; Torres, D. F.; Caliandro, G. A.; Hadasch, D.] Fac Ciencies, Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Torres, D. F.] ICREA, Barcelona, Spain.
[van der Klis, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands.
[Mendez, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Sierpowska-Bartosik, A.] Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
RP Rea, N (reprint author), Fac Ciencies, Inst Ciencies Espai IEEC CSIC, Campus UAB,Torre C5 Parell,2A Planta, Barcelona 08193, Spain.
EM rea@ieec.uab.es
RI Mendez, Mariano/C-8011-2012; Rea, Nanda/I-2853-2015; Torres,
Diego/O-9422-2016
OI Mendez, Mariano/0000-0003-2187-2708; Rea, Nanda/0000-0003-2177-6388;
Torres, Diego/0000-0002-1522-9065
FU Ramon y Cajal Research Fellowship; [AYA2009-07391]; [SGR2009-811];
[TW2010005]
FX This research has made use of data from the Chandra X-ray Observatory
and software provided by the Chandra X-ray Center. We thank G. L. Israel
for useful suggestions, and for allowing the use of his DPS software. We
thank S. Zhang, J. Li and Y. Chen for discussion, and the anonymous
referee for valuable suggestions. NR is supported by a Ramon y Cajal
Research Fellowship to CSIC. This work has been supported by grants
AYA2009-07391, SGR2009-811 and TW2010005.
NR 71
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U1 0
U2 3
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 2
BP 1514
EP 1521
DI 10.1111/j.1365-2966.2011.19148.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823KA
UT WOS:000295119900056
ER
PT J
AU Adams, JS
Kraus, MJ
Wing, SL
AF Adams, Jason S.
Kraus, Mary J.
Wing, Scott L.
TI Evaluating the use of weathering indices for determining mean annual
precipitation in the ancient stratigraphic record
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Paleosol; Weathering index; Paleoclimate; Vertisol; Paleocene-Eocene
Thermal Maximum; Global warming
ID EOCENE THERMAL MAXIMUM; BIGHORN BASIN; EBRO BASIN; SOIL DEVELOPMENT;
TROPICAL AFRICA; OXYGEN-ISOTOPE; NORTH-AMERICA; FOSSIL LEAVES;
PALEOSOLS; PALEOPRECIPITATION
AB Different quantitative methods have been developed to determine paleo-rainfall using paleosols. Of particular interest are methods that use bulk geochemistry to calculate a weathering index and, from that, mean annual precipitation. Twenty-three paleosols that formed during a time of significant climate change-the Paleocene-Eocene Thermal Maximum (PETM)-were analyzed to evaluate the relative merits of two geochemical proxies that have been developed for estimating paleoprecipitation: one depends on the chemical index of alteration without potash (CIA-K) and the other uses the CALMAG weathering index, which depends on CaO and MgO. The paleosols are located in the Paleogene Fort Union and Willwood formations in the Bighorn Basin, WY. Morphologic differences among the paleosols indicate that they formed under varied soil moisture conditions. A morphology index was developed from pedogenic features that are sensitive to soil drainage, and thus to rainfall, to assess that variability. Quantitative mean annual precipitation (MAP) values were calculated for each paleosol using the CIA-K index and the CALMAG index, which was developed specifically for Vertisols. Those results were compared to the morphology index for 23 paleosols.
The results indicate that increases and decreases in MAP calculated from both methods correlate relatively well to changes in the soil morphology index; however, the results from the CALMAG weathering index show a stronger correlation. The results suggest that the CALMAG proxy provides a more robust MAP estimate for Vertisols. In addition to comparing MAP estimates to the soil morphology index, we compared the MAP values to paleorainfall estimates determined from paleofloras at the same stratigraphic levels as three of the paleosols. That comparison confirms that the CALMAG method is reliable for reconstructing MAP from ancient Vertisols. The results also show that, in the Bighorn Basin, Vertisols with a B horizon <1 m thick should not be used to determine MAP. Thinner paleosols have had less time for weathering and may not have cation distributions representative of precipitation. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Adams, Jason S.; Kraus, Mary J.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA.
[Wing, Scott L.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
RP Kraus, MJ (reprint author), Univ Colorado, Dept Geol Sci, UCB 399,2200 Colorado Ave, Boulder, CO 80309 USA.
EM mary.kraus@colorado.edu
RI Kraus, Mary/C-3323-2008;
OI Kraus, Mary/0000-0002-1721-2566; Wing, Scott/0000-0002-2954-8905
FU NSF [EAR0718740, EAR0717892]; Smithsonian Institution; Geological
Society of America; Shell Oil/University of Colorado; American
Association of Petroleum Geologists; Rocky Mountain Association of
Geologists; Rocky Mountain Section of Society of Economic
Paleontologists and Mineralogists
FX This research was supported by NSF Award EAR0718740 to MJK, NSF Award
EAR0717892 to SLW, the Roland W. Brown Fund of the Smithsonian
Institution, and research grants provided by Geological Society of
America, Shell Oil/University of Colorado, American Association of
Petroleum Geologists, Rocky Mountain Association of Geologists, and the
Rocky Mountain Section of Society of Economic Paleontologists and
Mineralogists to JSA.
NR 56
TC 26
Z9 26
U1 2
U2 31
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD SEP 1
PY 2011
VL 309
IS 3-4
BP 358
EP 366
DI 10.1016/j.palaeo.2011.07.004
PG 9
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 822TM
UT WOS:000295072500019
ER
PT J
AU Wilson, JA
Barrett, PM
Carrano, MT
AF Wilson, Jeffrey A.
Barrett, Paul M.
Carrano, Matthew T.
TI AN ASSOCIATED PARTIAL SKELETON OF JAINOSAURUS CF. SEPTENTRIONALIS
(DINOSAURIA: SAUROPODA) FROM THE LATE CRETACEOUS OF CHHOTA SIMLA,
CENTRAL INDIA
SO PALAEONTOLOGY
LA English
DT Article
DE Dinosauria; Sauropoda; Cretaceous; Gondwana; India; palaeobiogeography
ID SAURISCHIA; PHYLOGENY; THEROPODA; ARGENTINA; DISTRICT; NEUQUEN; GUJARAT;
AGE
AB The Cretaceous dinosaur fauna of Indo-Pakistan has remained poorly understood because of a lack of associated and articulated remains, proliferation of named species, and an incomplete understanding of the dinosaur clades present (e. g. abelisaurid theropods; titanosaur sauropods). Continued work on existing collections, and new discoveries of dinosaur material from India, Pakistan and elsewhere in Gondwana, has begun to resolve the composition and affinities of Indo-Pakistani dinosaurs. Here, we provide archival evidence that documents associations between postcranial remains of a sauropod collected from Chhota Simla, India by C. A. Matley in the 1930s and later described as 'Titanosaurus sp.' This partial skeleton, which represents only the fifth such documented association from Indo-Pakistan, is referable to Jainosaurus cf. septentrionalis and provides a fuller understanding of its anatomy and phylogenetic affinities.
C1 [Wilson, Jeffrey A.] Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA.
[Wilson, Jeffrey A.] Univ Michigan, Dept Geol Sci, Ann Arbor, MI 48109 USA.
[Barrett, Paul M.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England.
[Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA.
RP Wilson, JA (reprint author), Univ Michigan, Museum Paleontol, 1109 Geddes Ave, Ann Arbor, MI 48109 USA.
EM wilsonja@umich.edu; p.barrett@nhm.ac.uk; carranom@si.edu
RI Barrett, Paul/A-2648-2010; Carrano, Matthew/C-7601-2011
OI Barrett, Paul/0000-0003-0412-3000; Carrano, Matthew/0000-0003-2129-1612
FU NHMUK; National Science Foundation (NSF) [DEB 0640434]
FX Our research was supported by a grant from the Special Funds of the
NHMUK (to PMB) and the National Science Foundation (NSF DEB 0640434 to
JAW). Access to NHMUK archival material was granted by P. Parry and J.
Hatton. Photographs of the Chhota Simla specimen were provided by P.
Crabb and P. Hurst (NHMUK Image Resources); stereo-pairs in Text-figures
9 and 11 were taken by JAW and M. D'Emic. S. Walsh and R. J. Butler are
thanked for their help in moving these large bones. All plates were put
together by B. Miljour. We thank D. Gillette and P. Upchurch for their
reviews of this paper, and K. Angielczyk for editorial guidance. Field
reconnaissance was performed by J. A. Wilson, D. Mohabey and M. D'Emic;
logistical support was provided by the Geological Survey of India
(Central Region).
NR 55
TC 16
Z9 16
U1 0
U2 1
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 SEP
PY 2011
VL 54
BP 981
EP 998
DI 10.1111/j.1475-4983.2011.01087.x
PN 5
PG 18
WC Paleontology
SC Paleontology
GA 823AT
UT WOS:000295094100003
ER
PT J
AU Hastings, AK
Bloch, JI
Jaramillo, CA
AF Hastings, Alexander K.
Bloch, Jonathan I.
Jaramillo, Carlos A.
TI A NEW LONGIROSTRINE DYROSAURID (CROCODYLOMORPHA, MESOEUCROCODYLIA) FROM
THE PALEOCENE OF NORTH-EASTERN COLOMBIA: BIOGEOGRAPHIC AND BEHAVIOURAL
IMPLICATIONS FOR NEW-WORLD DYROSAURIDAE
SO PALAEONTOLOGY
LA English
DT Article
DE Cerrejon; Colombia; Crocodylomorpha; Dyrosauridae; Acherontisuchus;
Paleocene; South America
ID NEOTROPICAL RAIN-FOREST; CERREJON FORMATION; NORTHEASTERN COLOMBIA;
SOUTH-AMERICA; WEST-AFRICA; CROCODYLIFORMES; MOROCCO; PHYLOGENY;
BOUNDARY; ORIGIN
AB Fossils of dyrosaurid crocodyliforms are limited in South America, with only three previously diagnosed taxa including the short-snouted Cerrejonisuchus improcerus from the Paleocene Cerrejon Formation of north-eastern Colombia. Here we describe a second dyrosaurid from the Cerrejon Formation, Acherontisuchus guajiraensis gen. et sp. nov., based on three partial mandibles, maxillary fragments, teeth, and referred postcrania. The mandible has a reduced seventh alveolus and laterally depressed retroarticular process, both diagnostic characteristics of Dyrosauridae. Acherontisuchus guajiraensis is distinct among known dyrosaurids in having a unique combination of craniomandibular characteristics, and postcranial morphology that suggests it may have occupied a more placid, fluvial habitat than most known Old-World dyrosaurids. Results from a cladistic analysis of Dyrosauridae, using 82 primarily cranial and mandibular characters, support an unresolved relationship between A. guajiraensis and a combination of New-and Old-World dyrosaurids including Hyposaurus rogersii, Congosaurus bequaerti, Atlantosuchus coupatezi, Guarinisuchus munizi, Rhabdognathus keiniensis and Rhabdognathus aslerensis. Our results are consistent with an African origin for Dyrosauridae with multiple dispersals into the New World during the Late Cretaceous and a transition from marine habitats in ancestral taxa to more fluvial habitats in more derived taxa.
C1 [Hastings, Alexander K.; Bloch, Jonathan I.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Hastings, AK (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
EM akh@ufl.edu; jbloch@flmnh.ufl.edu; jaramilloc@si.edu
OI Bloch, Jonathan/0000-0003-1484-6931
FU National Science Foundation [DEB-0733725, DSGC 640179]; Florida Museum
of Natural History; Smithsonian Tropical Research Institute; Geological
Society of America; Gary S. Morgan Student Research Award; Cerrejon Coal
mine
FX Funding for research and fieldwork was made possible by the National
Science Foundation Grant DEB-0733725 and DSGC 640179, funds from the
Florida Museum of Natural History, the Smithsonian Tropical Research
Institute Paleobiology Fund, the Geological Society of America Graduate
Student Research Grant, the R. Jerry Britt, Jr. Paleobiology Award
(Florida Museum of Natural History), Gary S. Morgan Student Research
Award, and the Cerrejon Coal mine. Many thanks to L. Teicher, F. Chavez,
G. Hernandez, C. Montes, and the rest of the crew at the Cerrejon coal
mine for access to the site and housing during field work. Thanks to
Ecopetrol S.A.-ICP for logistic support. Thanks to H. Garcia, A. Rincon,
E. Cadena, F. Herrera, S. Wing, and M. Ramirez for help collecting
fossils at Cerrejon. J. Bourque provided useful guidance for specimen
preparation and conservation. Thanks to J. Nestler and K. and N.
Hastings for their assistance in research and literature translation.
Thanks to D. Brinkman for access and assistance with the YPM
collections. Thanks to C. Mehling for access to the AMNH collections.
Thanks to L. Steel for access and assistance with the collections at the
Museum of Natural History, London. Thanks to E. Martin and D. Foster for
helpful discussions about paleocurrents and tectonics, respectively.
Thanks also to the reviewers and editor for helpful comments and
suggestions. Lastly, thanks to the Colombian Geological and Mining
Institute (INGEOMINAS) in Bogota, Colombia, for access to specimens and
facilitating ongoing research of the remarkable vertebrate fossils of
the Paleocene-Eocene of Colombia.
NR 79
TC 11
Z9 12
U1 0
U2 5
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0031-0239
J9 PALAEONTOLOGY
JI Paleontology
PD SEP
PY 2011
VL 54
BP 1095
EP 1116
DI 10.1111/j.1475-4983.2011.01092.x
PN 5
PG 22
WC Paleontology
SC Paleontology
GA 823AT
UT WOS:000295094100008
ER
PT J
AU Grant, JA
Golombek, MP
Grotzinger, JP
Wilson, SA
Watkins, MM
Vasavada, AR
Griffes, JL
Parker, TJ
AF Grant, John A.
Golombek, Matthew P.
Grotzinger, John P.
Wilson, Sharon A.
Watkins, Michael M.
Vasavada, Ashwin R.
Griffes, Jennifer L.
Parker, Timothy J.
TI The science process for selecting the landing site for the 2011 Mars
Science Laboratory
SO PLANETARY AND SPACE SCIENCE
LA English
DT Article
DE Mars; Landing sites
ID MERIDIANI-PLANUM; VALLES-MARINERIS; LAYERED DEPOSITS; TERRA MERIDIANI;
MAWRTH-VALLIS; CLAY-MINERALS; HOLDEN CRATER; MELAS-CHASMA; ART.;
EVOLUTION
AB The process of identifying the landing site for NASA's 2011 Mars Science Laboratory (MSL) began in 2005 by defining science objectives, related to evaluating the potential habitability of a location on Mars, and engineering parameters, such as elevation, latitude, winds, and rock abundance, to determine acceptable surface and atmospheric characteristics. Nearly 60 candidate sites were considered at a series of open workshops in the years leading up to the launch. During that period, iteration between evolving engineering constraints and the relative science potential of candidate sites led to consensus on four final sites. The final site will be selected in the Spring of 2011 by NASA's Associate Administrator for the Science Mission Directorate. This paper serves as a record of landing site selection activities related primarily to science, an inventory of the number and variety of sites proposed, and a summary of the science potential of the highest ranking sites. Published by Elsevier Ltd.
C1 [Grant, John A.; Wilson, Sharon A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
[Golombek, Matthew P.; Watkins, Michael M.; Vasavada, Ashwin R.; Parker, Timothy J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Grotzinger, John P.; Griffes, Jennifer L.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Grant, JA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 6th & Independence SW, Washington, DC 20560 USA.
EM grantj@si.edu
FU NASA MDAP [NNX09AI65G]
FX Reviews by Nicolas Mangold and an anonymous reviewer improved the
manuscript. Work supported by NASA MDAP Grant NNX09AI65G.
NR 75
TC 26
Z9 27
U1 2
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0032-0633
J9 PLANET SPACE SCI
JI Planet Space Sci.
PD SEP
PY 2011
VL 59
IS 11-12
SI SI
BP 1114
EP 1127
DI 10.1016/j.pss.2010.06.016
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 822TS
UT WOS:000295073100002
ER
PT J
AU Wang, HQ
Toigo, AD
Richardson, MI
AF Wang, Huiqun
Toigo, Anthony D.
Richardson, Mark I.
TI Curvilinear features in the southern hemisphere observed by Mars Global
Surveyor Mars Orbiter Camera
SO ICARUS
LA English
DT Article
DE Atmospheres, Dynamics; Atmospheres, Structure; Mars, Atmosphere
ID THERMAL EMISSION SPECTROMETER; GENERAL-CIRCULATION MODEL; TES NADIR
DATA; DUST STORMS; MARTIAN ATMOSPHERE; MGS TES; NORTHERN-HEMISPHERE;
MAPPING YEAR; CLOUDS; TEMPERATURES
AB We have used the complete set of Mars Global Surveyor (MGS) Mars Daily Global Maps (MDGMs) to study martian weather in the southern hemisphere, focusing on curvilinear features, including frontal events and streaks. "Frontal events" refer to visible events that are morphologically analogous to terrestrial baroclinic storms. MDGMs show that visible frontal events were mainly concentrated in the 210-300 degrees E (60-150 degrees W) sector and the 0-60 degrees E sector around the southern polar cap during L-s = 140-250 degrees and L-s = 340-60 degrees. The non-uniform spatial and temporal distributions of activity were also shown by MGS Thermal Emission Spectrometer transient temperature variations near the surface. "Streaks" refer to long curvilinear features in the polar hood or over the polar cap. They are an indicator of the shape of the polar vortex. Streaks in late winter usually show wavy segments between the 180 degrees meridian and Argyre. Model results suggest that the zonal wave number m = 3 eastward traveling waves are important for their formation. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Wang, Huiqun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Toigo, Anthony D.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA.
[Richardson, Mark I.] Ashima Res, Pasadena, CA 91106 USA.
RP Wang, HQ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM hwang@cfa.harvard.edu
FU NASA
FX We would like to thank two anonymous reviewers for comments. H. Wang
would like to thank the NASA Mars Data Analysis Program and the NASA
Planetary Atmosphere program for supporting this effort.
NR 39
TC 3
Z9 3
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 SEP
PY 2011
VL 215
IS 1
BP 242
EP 252
DI 10.1016/j.icarus.2011.06.029
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400020
ER
PT J
AU Laraia, AL
Gamache, RR
Lamouroux, J
Gordon, IE
Rothman, LS
AF Laraia, Anne L.
Gamache, Robert R.
Lamouroux, Julien
Gordon, Iouli E.
Rothman, Laurence S.
TI Total internal partition sums to support planetary remote sensing
SO ICARUS
LA English
DT Article
DE Abundances, Atmospheres; Atmospheres, Composition; Radiative transfer;
Spectroscopy
ID HIGH-RESOLUTION FOURIER; MOLECULAR SPECTROSCOPIC DATABASE; ASTROPHYSICAL
INTEREST; INFRARED-SPECTRUM; FUNDAMENTAL-BAND; GROUND-STATE; MU-M;
ROTATIONAL ANALYSIS; LINEAR-MOLECULES; INTEGRATED BAND
AB Total internal partition sums are determined from 65 to 3010 K for (13)C(18)O(2), (13)C(18)O(17)O, (12)CH(3)D, (13)CH(3)D, H(12)C(12)CD, (13)C(12)CH(6), (12)CH(3)(79)Br, (12)CH(3)(81)Br, (12)CF(4), H(12)C(12)C(12)C(12)CH, H(12)C(12)C(12)C(14)N, H(12)C(12)C(13)C(14)N, H(12)C(13)C(12)C(14)N, H(13)C(12)C(12)C(14)N, H(12)C(12)C(12)C(15)N, D(12)C(12)C(12)C(14)N, (14)N(12)C(12)C(14)N, (15)N(12)C(12)C(15)N, (12)C(32)S, (12)C(33)S, (12)C(34)S, (13)C(32)S, H(2), HD, (32)S(16)O, (32)S(18)O, (34)S(16)O, (12)C(3)H(4), (12)CH(3), (12)C(32)S(2), (32)S(12)C(34)S, (13)C(32)S(2), and (32)S(12)C(33)S. These calculations complete the partition sum data needed for additional isotopologues in HITRAN2008 and also extend the partition sums to molecules of astrophysical interest. These data, at 25 K steps, are incorporated into a FORTRAN code (TIPS_2011.for) that can be used to rapidly generate the data at any temperature in the range 70-3000 K. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Laraia, Anne L.; Gamache, Robert R.; Lamouroux, Julien] Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA.
[Laraia, Anne L.; Gamache, Robert R.; Lamouroux, Julien] Univ Massachusetts, Sch Marine Sci, Lowell, MA 01854 USA.
[Gordon, Iouli E.; Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
RP Gamache, RR (reprint author), Univ Massachusetts, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA.
EM Robert_Gamache@uml.edu
OI Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847
FU National Science Foundation [ATM-0803135]; NASA [NNX10AB94G]; Earth
Observing System (EOS) [NAG5-13534]
FX A.L.L., R.R.G., and J.L. would like to acknowledge the support of this
research by the National Science Foundation through Grant Number
ATM-0803135. Any opinions, findings, and conclusions or recommendations
expressed in this material are those of the author(s) and do not
necessarily reflect the views of the National Science Foundation. The
effort at the Harvard-Smithsonian Center for Astrophysics has been
supported by NASA through the Planetary Atmospheres Grant NNX10AB94G and
the Earth Observing System (EOS) under Grant NAG5-13534.
NR 65
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Z9 36
U1 0
U2 17
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 SEP
PY 2011
VL 215
IS 1
BP 391
EP 400
DI 10.1016/j.icarus.2011.06.004
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 821NJ
UT WOS:000294981400031
ER
PT J
AU Hardesty, BD
AF Hardesty, Britta Denise
TI Effectiveness of seed dispersal by ants in a Neotropical tree
SO INTEGRATIVE ZOOLOGY
LA English
DT Article
DE Atta colombica; Barro Colorado Island; seed dispersal effectiveness;
Simarouba amara
ID ATTA-CEPHALOTES; GENETIC-STRUCTURE; RAIN-FOREST; COSTA-RICA; NESTS;
COLOMBICA; VEGETATION; GAPS
AB Seed dispersal and subsequent recruitment is the template on which forest regeneration takes place. Hence, considering the scale over which ecological processes occur is key for understanding the overall impact of various dispersal agents. To explore leafcutter ant (Atta colombica) dispersal effectiveness in space and time, seed movement and subsequent recruitment of a large-seeded predominately vertebrate-dispersed tree, Simarouba amara (Aubl. Simaroubaceae), was investigated on Barro Colorado Island, Panama. At each of 218 reproductive-sized adults (>= 20 cm diameter at breast height), presence or absence of a leafcutter ant colony was noted, with extensive checks for Atta activity taking place at or in close proximity to seed and seedling transects, which extended 4 cardinal directions for 30 m from each reproductive female tree (n = 74). Only at 2 S. amara trees were nests observed, and in these areas a dense S. amara seedling carpet was observed. Although nearby nest and dump sites might increase local S. amara recruitment in the short term, mortality at these sites is complete or nearly so. Hence, the seed dispersal effectiveness by leafcutter ants appears to be ephemeral and likely contributes inconsequentially to the long-term recruitment and distribution patterns of the species. This finding highlights the importance of evaluating disperser effectiveness at ecologically relevant spatiotemporal scales.
C1 [Hardesty, Britta Denise] CSIRO, Atherton, Qld 4883, Australia.
[Hardesty, Britta Denise] Univ Georgia, Dept Plant Biol, Athens, GA 30602 USA.
[Hardesty, Britta Denise] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Hardesty, BD (reprint author), CSIRO, Atherton, Qld 4883, Australia.
EM denise.hardesty@csiro.au
RI Hardesty, Britta Denise/A-3189-2011
OI Hardesty, Britta Denise/0000-0003-1948-5098
FU Smithsonian Tropical Research Institute; Center for Tropical Forest
Science; University of Georgia; Garden Club of America; Mellon
Foundation
FX I thank the Smithsonian Tropical Research Institute, the Center for
Tropical Forest Science, the University of Georgia, the Garden Club of
America, and the Mellon Foundation for financial and logistical support
during the time this research was conducted, and Pablo Ramos for his
untiring efforts in the field. This work could not have been completed
without the support of SP Hubbell and E Bermingham.
NR 33
TC 3
Z9 3
U1 1
U2 13
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1749-4877
EI 1749-4869
J9 INTEGR ZOOL
JI Integr. Zool.
PD SEP
PY 2011
VL 6
IS 3
BP 222
EP 226
DI 10.1111/j.1749-4877.2011.00246.x
PG 5
WC Zoology
SC Zoology
GA 822AY
UT WOS:000295016900006
PM 21910841
ER
PT J
AU Swaisgood, RR
Wei, FW
Mcshea, WJ
Wildt, DE
Kouba, AJ
Zhang, ZJ
AF Swaisgood, Ronald R.
Wei, Fuwen
Mcshea, William J.
Wildt, David E.
Kouba, Andrew J.
Zhang, Zejun
TI Can science save the giant panda (Ailuropoda melanoleuca)? Unifying
science and policy in an adaptive management paradigm
SO INTEGRATIVE ZOOLOGY
LA English
DT Article
DE adaptive management; conservation policy; endangered species; giant
panda; strategic conservation plan
ID CARRYING-CAPACITY; HABITAT USE; RED PANDAS; CONSERVATION; BAMBOO; CHINA;
POPULATIONS; DYNAMICS; BEHAVIOR; FOREST
AB The giant panda (Ailuropoda melanoleuca David, 1869) is an iconic species for global conservation, yet field research has only recently advanced to the point where adaptive management is possible. Here, we review recent developments in giant panda conservation science and propose a strategic plan for moving panda conservation forward. Because of scientific, funding, political, and logistical hurdles, few endangered species management programs have embraced adaptive management, wherein management decisions are shaped iteratively by targeted scientific research. Specific threats, such as habitat destruction, anthropogenic disturbance and fragmented nonviable populations, need to be addressed simultaneously by researchers, managers and policy-makers working in concert to understand and overcome these obstacles to species recovery. With the backing of the Chinese Government and the conservation community, the giant panda can become a high-profile test species for this much touted, but rarely implemented, approach to conservation management.
C1 [Swaisgood, Ronald R.; Zhang, Zejun] San Diego Zoo Inst Conservat Res, Escondido, CA 92027 USA.
[Wei, Fuwen; Zhang, Zejun] Chinese Acad Sci, Inst Zool, Beijing, Peoples R China.
[Mcshea, William J.; Wildt, David E.] Smithsonians Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA.
[Kouba, Andrew J.] Memphis Zoo, Memphis, TN USA.
[Zhang, Zejun] China W Normal Univ, Inst Rare Anim & Plants, Nanchong, Sichuan, Peoples R China.
RP Swaisgood, RR (reprint author), San Diego Zoo Inst Conservat Res, 15600 San Pasqual Valley Rd, Escondido, CA 92027 USA.
EM rswaisgood@sandiegozoo.org
NR 37
TC 14
Z9 16
U1 5
U2 88
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1749-4877
J9 INTEGR ZOOL
JI Integr. Zool.
PD SEP
PY 2011
VL 6
IS 3
BP 290
EP 296
DI 10.1111/j.1749-4877.2011.00250.x
PG 7
WC Zoology
SC Zoology
GA 822AY
UT WOS:000295016900013
PM 21910848
ER
PT J
AU Cadena, EA
AF Cadena, Edwin A.
TI POTENTIAL EARLIEST RECORD OF PODOCNEMIDOID TURTLES FROM THE EARLY
CRETACEOUS (VALANGINIAN) OF COLOMBIA
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID TESTUDINES PLEURODIRA; BOTHREMYDIDAE
AB A costal and a peripheral bone from the Early Cretaceous (Valanginian, ca. 135 Ma) Rosablanca Formation, Zapatoca town, Colombia are described. These specimens represent the earliest record of podocnemidoid turtles. Evolutionary and paleogeographical implications are also discussed.
C1 [Cadena, Edwin A.] Ctr Trop Paleoecol & Archeol, Smithsonian Trop Res Inst, Balboa, Panama.
[Cadena, Edwin A.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
RP Cadena, EA (reprint author), Ctr Trop Paleoecol & Archeol, Smithsonian Trop Res Inst, Balboa, Panama.
EM eacadena@ncsu.edu
FU Smithsonian Paleobiology Endowment Fund
FX Funding for fieldwork came from the Smithsonian Paleobiology Endowment
Fund. I would like to thank D. Ksepka and C. Jaramillo for reviewing the
preliminary draft and providing valuable comments. Thanks are also
extended to A. Rincon, collector of IPN 16 EAC-14012003-1B. F. Lapparent
de Broin and P. Romano provided useful reviews. For access to
collections I thank J. Arenas (Museo Geologico Jose Royo y
Gomez-Instituto Colombiano de Geologia y Mineria-Ingeominas), C. Mehling
(American Museum of Natural History), and P. Pritchard (Chelonian
Research Institute). Special thanks to M. Gonzalez and R. Rueda, for
their continuous support and motivation to write this paper, as well as
for Zapatoca's citizens for their special kindness.
NR 42
TC 2
Z9 3
U1 0
U2 1
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 SEP
PY 2011
VL 85
IS 5
BP 877
EP 881
PG 5
WC Paleontology
SC Paleontology
GA 820DG
UT WOS:000294885100005
ER
PT J
AU Dove, CJ
Olson, SL
AF Dove, Carla J.
Olson, Storrs L.
TI FOSSIL FEATHERS FROM THE HAWAIIAN FLIGHTLESS IBIS (APTERIBIS SP.):
PLUMAGE COLORATION AND SYSTEMATICS OF A PREHISTORICALLY EXTINCT BIRD
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID ISLANDS
AB A nearly complete skeleton of an adult Hawaiian flightless ibis (Apteribis sp.) was recovered from a vaulted dry lava tube in association with remains of contour feathers. This is the first documentation of the genus Apteribis from the island of Lanai and provides the only record of the nature of the plumage in any of the prehistorically extinct species of birds known from the Hawaiian Islands. Light and scanning electron microscope analyses of structure of the pennaceous and plumulaceous (downy) portions of these feathers confirmed their placement with the ibises (Threskiornithidae). Within that family, the microscopic structure of the downy feathers is most similar to that of the New World ibises of the genus Eudocimus, thus corroborating molecular evidence of the derivation of Apteribis from Eudocimus. Plumage color was a combination of brown-black and ivory-beige/light brown suggestive of that of juveniles of Eudocimus. Plumage coloration in Apteribis may thus have evolved through the same processes of paedomorphosis that gave rise to flightlessness.
C1 [Dove, Carla J.; Olson, Storrs L.] Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Dove, CJ (reprint author), Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
EM dovec@si.edu; olsons@si.edu
FU FAA; US Air Force; US Navy
FX For discovering the importance of the lava tube on Lanai and for
assistance in the field we are indebted to R. M. Severns and especially
P. Fiene-Severns, without whose patience in carefully retrieving the
feathered Apteribis from its nearly inaccessible crevice this paper
would never have been written. We thank J. Post and R. Fiske, Dept. of
Mineral Sciences, Smithsonian Institution, for mineral analysis. For
additional assistance in the museum we are grateful to H. F. James, M.
Spitzer, and M. Florence. We thank H. F. James and J. Kushlan for
information and comments. D. Deedrick assisted with microslide
preparation and S. Whittaker assisted with SEM. C. Dove is supported by
interagency agreements with FAA, US Air Force and US Navy. Figure 1 is
by B. Schmidt.
NR 35
TC 2
Z9 2
U1 1
U2 10
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-3360
EI 1937-2337
J9 J PALEONTOL
JI J. Paleontol.
PD SEP
PY 2011
VL 85
IS 5
BP 892
EP 897
PG 6
WC Paleontology
SC Paleontology
GA 820DG
UT WOS:000294885100007
ER
PT J
AU Uhen, MD
Pyenson, ND
Devries, TJ
Urbina, M
Renne, PR
AF Uhen, Mark D.
Pyenson, Nicholas D.
Devries, Thomas J.
Urbina, Mario
Renne, Paul R.
TI NEW MIDDLE EOCENE WHALES FROM THE PISCO BASIN OF PERU
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID AR-40/AR-39 GEOCHRONOLOGY; ARCHAEOCETE WHALE; DECAY CONSTANTS; CETACEAN
BRAIN; NORTH-CAROLINA; FOSSIL RECORD; SOUTHERN PERU; ORIGIN; EVOLUTION;
MAMMALIA
AB Three new specimens of middle Eocene cetaceans are reported from the Pisco Basin of southern Peru. All three specimens originate from the Paracas Formation and their minimum age is constrained to about 37 Ma using Ar-40/Ar-39 dating of ash collected similar to 100 m up section from the source localities. Two new genera of archaeocete cetaceans are described along with additional material of another distinctive protocetid, which is not named pending the discovery of more complete material. Phylogenetic analysis resolves the two new genera within Basilosauridae, while the unnamed protocetid is closely related to Eocetus. The discovery of crownward protocetids in South America demonstrates that early cetaceans may have dispersed into both hemispheres prior to evolving a fully aquatic lifestyle. Geochronologic constraints on the age of new Peruvian archaeocetes establish them as the oldest whales from South America and among the oldest known from the Southern Hemisphere, which highlights the need for better sampling of marginal marine rocks from this part of the world.
C1 [Uhen, Mark D.] George Mason Univ, Dept Atmospher Ocean & Space Sci, Fairfax, VA 22030 USA.
[Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Pyenson, Nicholas D.; Devries, Thomas J.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA.
[Urbina, Mario] Museo Hist Nat San Marcos, Dept Paleontol Vertebrados, Lima 14, Peru.
[Renne, Paul R.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA.
[Renne, Paul R.] Berkeley Geochronol Ctr, Berkeley, CA 94709 USA.
RP Uhen, MD (reprint author), George Mason Univ, Dept Atmospher Ocean & Space Sci, Fairfax, VA 22030 USA.
EM muhen@gmu.edu; pyensonn@si.edu
OI Urbina, Mario/0000-0002-1898-9051
FU National Science Foundation; Natural Sciences and Engineering Research
Council of Canada; Smithsonian Institution
FX We warmly acknowledge the assistance of R. Salas-Gismondi, D. Omura, J.
Tejada, W. Aguirre, J. F. Parham, S. Rieboldt, M. D. Lewin, D. T.
Ksepka, and J. A. Clarke with both field and museum work in Peru.
Additionally, we wish to recognize L.M. Berg, who also assisted with
fossil preparation and photography in Lima. For comments on earlier
drafts of this manuscript, we thank P. A. Holroyd, R. B. Irmis, and J.
F. Parham. We also thank insightful and constructive comments from R. E.
Fordyce and three anonymous reviewers on this and earlier drafts.
Generous assistance from the University of California Museum of
Paleontology Remington Kellogg Fund (to NDP) and the Smithsonian
Institution Remington Kellogg Fund (to MDU) supported field and museum
work in Peru. During the course of this study, NDP was supported by a
National Science Foundation Graduate Research Fellowship, a postdoctoral
research fellowship from the Natural Sciences and Engineering Research
Council of Canada and by funding from the Smithsonian Institution.
NR 89
TC 13
Z9 15
U1 0
U2 13
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA
SN 0022-3360
EI 1937-2337
J9 J PALEONTOL
JI J. Paleontol.
PD SEP
PY 2011
VL 85
IS 5
BP 955
EP 969
PG 15
WC Paleontology
SC Paleontology
GA 820DG
UT WOS:000294885100014
ER
PT J
AU Hallworth, MT
Reitsma, LR
Parent, K
AF Hallworth, Michael T.
Reitsma, Leonard R.
Parent, Kyle
TI HABITAT USE OF THE LOUISIANA WATERTHRUSH DURING THE NON-BREEDING SEASON
IN PUERTO RICO
SO WILSON JOURNAL OF ORNITHOLOGY
LA English
DT Article
ID MIXED-SPECIES FLOCKS; AMERICAN REDSTARTS; NEOTROPICAL MIGRANT; MIGRATORY
SONGBIRD; NONBREEDING SEASON; FORAGING BEHAVIOR; SEIURUS-MOTACILLA; BODY
CONDITION; SITE FIDELITY; WINTER
AB We used radiotelemetry to quantify habitat and spatial use patterns of neighboring Louisiana Waterthrush (Parkesia motacilla) along two streams in the Caribbean National Forest in Puerto Rico during 2005-2007. Home range sizes varied with younger birds having larger home ranges and core areas than older birds. All birds occupied some length of stream but a wide range of off-stream habitats were also used. Off-stream habitats included a range of disturbance from residential areas to small saturated pastures. Neighbors exhibited a wide range of overlap in home ranges ((x) over bar = 20%) and older birds had more overlap than younger birds. The greatest percent of foraging time was along streams (64.4%) followed by muddy substrate (26.5%), housing developments (7.4%), and roads (1.7%). The greater proportion of time foraging along streams indicates this is the preferred habitat for this species. Use of off-stream habitat indicates a strategy of exploiting food-rich ground substrates, and in particular those with high moisture. Received 28 September 2010. Accepted 5 February 2011.
C1 [Hallworth, Michael T.; Reitsma, Leonard R.; Parent, Kyle] Plymouth State Univ, Plymouth, NH 03264 USA.
RP Hallworth, MT (reprint author), Smithsonian Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
EM mhallwor@gmu.edu
FU New England Institute for Landscape Ecology
FX We thank J. M. Wunderle and J. E. Mercado for support and assistance as
well as the staff at Sabana Field Station, Sabana, Puerto Rico. The
authors also thank P. M. Benham, A. J. Leppold, R. S. Mulvihill, F. L.
Newell, and Carly Reitsma for help in the field. This study was
supported by the New England Institute for Landscape Ecology. We thank
C. E. Braun and two anonymous reviewers who made comments that improved
this paper.
NR 44
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U1 2
U2 18
PU WILSON ORNITHOLOGICAL SOC
PI WACO
PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA
SN 1559-4491
EI 1938-5447
J9 WILSON J ORNITHOL
JI Wilson J. Ornithol.
PD SEP
PY 2011
VL 123
IS 3
BP 567
EP 574
PG 8
WC Ornithology
SC Zoology
GA 818ZO
UT WOS:000294795400017
ER
PT J
AU Pearlstein, P
AF Pearlstein, Philip
TI BEING THERE
SO ART IN AMERICA
LA English
DT Editorial Material
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Pearlstein, P (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
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U1 0
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PU BRANT PUBL, INC
PI NEW YORK
PA 575 BROADWAY, NEW YORK, NY 10012 USA
SN 0004-3214
J9 ART AM
JI Art Am.
PD SEP
PY 2011
VL 99
IS 8
BP 57
EP 57
PG 1
WC Art
SC Art
GA 815IX
UT WOS:000294520400013
ER
PT J
AU Evans, NR
Berdnikov, L
Gorynya, N
Rastorguev, A
Eaton, J
AF Evans, Nancy Remage
Berdnikov, Leonid
Gorynya, Natalia
Rastorguev, Alexey
Eaton, Joel
TI THE ORBIT OF THE CEPHEID V350 Sgr REVISITED
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries: spectroscopic; stars: massive; stars: variables: Cepheids
ID PERIOD SOUTHERN CEPHEIDS; INTERMEDIATE-MASS STARS;
HUBBLE-SPACE-TELESCOPE; RADIAL-VELOCITIES; CLASSICAL CEPHEID;
CORRELATION SPECTROMETER; VARIABLE-STARS; PHOTOELECTRIC OBSERVATIONS;
BOLOMETRIC CORRECTIONS; EVOLUTIONARY MODELS
AB "The Cepheid Mass Problem" is one of the fundamental tests of the understanding of stellar evolution. One of the foundations of measured masses for Cepheids for this question is binary orbits. V350 Sgr is a classical Cepheid in a binary system. New radial velocity data for the system have been obtained over the last several years, and are used to update the orbit. The secondary in the system has previously had its orbital velocity amplitude measured in the ultraviolet with the Hubble Space Telescope. This amplitude has been combined with the new orbit and the adopted mass of the secondary resulting in a Cepheid mass of 5.0 +/- 0.8 M-circle dot.
C1 [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Berdnikov, Leonid; Gorynya, Natalia; Rastorguev, Alexey] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Berdnikov, Leonid] Isaac Newton Inst Chile, Moscow Branch, Moscow 119992, Russia.
[Gorynya, Natalia] Russian Acad Sci, Inst Astron, Moscow V71, Russia.
RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA.
EM nevans@cfa.harvard.edu; nevans@cfa.harvard.edu
RI Rastorguev, Alexey/P-7956-2015
OI Rastorguev, Alexey/0000-0003-3525-6869
FU Chandra X-ray Center NASA [NAS8-03060]; Russian Foundation of Basic
Research [10-02-00489]; KBN [2-P03D-011-14, 5-P03D-011-30]; MNiSV
(Poland) [1-P03D-011-30]; Russian Foundation for Basic Research
[05-02-16526, 08-02-00738]
FX It is a pleasure to acknowledge comments from Frank Fekel on the draft
of this paper. We also thank the referee for constructive comments
leading to an improved version. N. R. E. acknowledges support from the
Chandra X-ray Center NASA Contract NAS8-03060. The present study was
supported by research funding awarded through the Russian Foundation of
Basic Research (grant 10-02-00489) to L. N. B. N. G. is grateful to Dr.
P. Moskalik (Copernicus Astronomical Centre, Warsaw, Poland) for his
advice, helpful discussions, and permanent support of radial velocity
measurements. Her work was also partly supported by KBN grants
2-P03D-011-14, 5-P03D-011-30 and MNiSV grant 1-P03D-011-30 (Poland). A.
R. and N. G. are grateful to Russian Foundation for Basic Research
(grants 05-02-16526, 08-02-00738) for permanent support of observations.
NR 68
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 87
DI 10.1088/0004-6256/142/3/87
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700021
ER
PT J
AU Fulton, BJ
Shporer, A
Winn, JN
Holman, MJ
Pal, A
Gazak, JZ
AF Fulton, Benjamin J.
Shporer, Avi
Winn, Joshua N.
Holman, Matthew J.
Pal, Andras
Gazak, J. Zachary
TI LONG-TERM TRANSIT TIMING MONITORING AND REFINED LIGHT CURVE PARAMETERS
OF HAT-P-13b
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-13)
ID STELLAR ATMOSPHERE MODELS; LIMB-DARKENING LAW; EXTRASOLAR PLANETS;
SURFACE GRAVITIES; HOT JUPITER; SPACED DATA; SYSTEM; COMPANION; DETECT;
ORBITS
AB We present 10 new transit light curves of the transiting hot Jupiter HAT-P-13b, obtained during two observational seasons by three different telescopes. When combined with 12 previously published light curves, we have a sample consisting of 22 transit light curves, spanning 1041 days across four observational seasons. We use this sample to examine the recently observed large-amplitude transit timing variations (TTVs) by Pal et al. and give refined system parameters. We find that the transit times are consistent with a linear ephemeris, with the exception of a single transit time, from UT 2009 November 5, for which the measured mid-transit time significantly deviates from our linear ephemeris. The nature of this deviation is not clear, and the rest of the data do not show any significant TTVs.
C1 [Fulton, Benjamin J.; Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
[Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[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.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pal, Andras] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Pal, Andras] Eotvos Lorand Univ, Dept Astron, H-1117 Budapest, Hungary.
[Gazak, J. Zachary] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Fulton, BJ (reprint author), Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA.
EM bjfulton@lcogt.net
FU NASA [NNX10AG02A, NNX09AB33G]; ESA [PECS 98073]; HAS
FX A. S. acknowledges support from NASA Grant Number NNX10AG02A. M. H. and
J. W. gratefully acknowledge support from the NASA Origins program
through award NNX09AB33G. A. P. is thankful for the support of the ESA
grant PECS 98073, and the Janos Bolyai Research Scholarship of the HAS.
This paper uses observations obtained with facilities of the Las Cumbres
Observatory Global Telescope. The Byrne Observatory at Sedgwick (BOS) is
operated by the Las Cumbres Observatory Global Telescope Network and is
located at the Sedgwick Reserve, a part of the University of California
Natural Reserve System. PyRAF is a product of the Space Telescope
Science Institute, which is operated by AURA for NASA.
NR 25
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 84
DI 10.1088/0004-6256/142/3/84
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700018
ER
PT J
AU Kipping, DM
Hartman, J
Bakos, GA
Torres, G
Latham, DW
Bayliss, D
Kiss, LL
Sato, B
Beky, B
Kovacs, G
Quinn, SN
Buchhave, LA
Andersen, J
Marcy, GW
Howard, AW
Fischer, DA
Johnson, JA
Noyes, RW
Sasselov, DD
Stefanik, RP
Lazar, J
Papp, I
Sari, P
Furesz, G
AF Kipping, D. M.
Hartman, J.
Bakos, G. A.
Torres, G.
Latham, D. W.
Bayliss, D.
Kiss, L. L.
Sato, B.
Beky, B.
Kovacs, Geza
Quinn, S. N.
Buchhave, L. A.
Andersen, J.
Marcy, G. W.
Howard, A. W.
Fischer, D. A.
Johnson, J. A.
Noyes, R. W.
Sasselov, D. D.
Stefanik, R. P.
Lazar, J.
Papp, I.
Sari, P.
Furesz, G.
TI HAT-P-31b,c: A TRANSITING, ECCENTRIC, HOT JUPITER AND A LONG-PERIOD,
MASSIVE THIRD BODY
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-31, GSC 2099-00908);
techniques: photometric; techniques: spectroscopic
ID EXTRASOLAR PLANET; TERRESTRIAL PLANETS; FIELD; STAR; SEARCH; ORBIT;
ATMOSPHERE; PRECISION; ALGORITHM; EXOMOON
AB We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17 M-J, 1.1 R-J planet has a period of P-b = 5.0054 days and maintains an unusually high eccentricity of e(b) = 0.2450 +/- 0.0045, determined through Keck, FIbr-fed Echelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4 M-J and period >= 2.8 years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.
C1 [Kipping, D. M.; Hartman, J.; Bakos, G. A.; Torres, G.; Latham, D. W.; Beky, B.; Quinn, S. N.; Noyes, R. W.; Sasselov, D. D.; Stefanik, R. P.; Furesz, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kipping, D. M.] UCL, Dept Phys & Astron, London, England.
[Bayliss, D.; Kiss, L. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT, Australia.
[Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Buchhave, L. A.; Andersen, J.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
RI Bayliss, Daniel/I-4635-2012; Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars
A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166; Fischer,
Debra/0000-0003-2221-0861
FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390, N167Hr];
Smithsonian Institution Restricted Endowment Funds; SAO IRD grants; NSF
[AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation
(OTKA) [K-60750, K76816, K83790, MB08C 81013]; Hungarian Academy of
Sciences
FX HATNet operations have been funded by NASA grants NNG04GN74G,
NNX08AF23G, and SAO IR&D grants. D. M. K. has been supported by
Smithsonian Institution Restricted Endowment Funds. Work of G.A.B. and
J. Johnson were supported by the Postdoctoral Fellowship of the NSF
Astronomy and Astrophysics Program (AST-0702843 and AST-0702821,
respectively). G. T. acknowledges partial support from NASA grant
NNX09AF59G. We acknowledge partial support also from the Kepler Mission
under NASA Cooperative Agreement NCC2-1390 (D. W. L., PI). G. K. thanks
the Hungarian Scientific Research Foundation (OTKA) for support through
grant K-60750. L. L. K. is supported by the "Lendulet" Young Researchers
Program of the Hungarian Academy of Sciences and the Hungarian OTKA
grants K76816, K83790, and MB08C 81013. Tamas Szalai (University of
Szeged) is acknowledged for his assistance during the ANU 2.3 m
observations. This research has made use of Keck telescope time granted
through NASA (N167Hr). This work is based in part on data collected at
Subaru Telescope, which is operated by the National Astronomical
Observatory of Japan, and in part on observations made with the Nordic
Optical Telescope, operated on the island of La Palma jointly by
Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica
de Canarias. Thanks to G. Laughlin for useful advise on the Systemic
Console, Dan Fabrycky and Rene Heller for useful comments, and special
thanks to the anonymous referee for their helpful suggestions.
NR 48
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 95
DI 10.1088/0004-6256/142/3/95
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700029
ER
PT J
AU Krisciunas, K
Li, WD
Matheson, T
Howell, DA
Stritzinger, M
Aldering, G
Berlind, PL
Calkins, M
Challis, P
Chornock, R
Conley, A
Filippenko, AV
Ganeshalingam, M
Germany, L
Gonzalez, S
Gooding, SD
Hsiao, E
Kasen, D
Kirshner, RP
Marion, GHH
Muena, C
Nugent, PE
Phelps, M
Phillips, MM
Qiu, YL
Quimby, R
Rines, K
Silverman, JM
Suntzeff, NB
Thomas, RC
Wang, LF
AF Krisciunas, Kevin
Li, Weidong
Matheson, Thomas
Howell, D. Andrew
Stritzinger, Maximilian
Aldering, Greg
Berlind, Perry L.
Calkins, M.
Challis, Peter
Chornock, Ryan
Conley, Alexander
Filippenko, Alexei V.
Ganeshalingam, Mohan
Germany, Lisa
Gonzalez, Sergio
Gooding, Samuel D.
Hsiao, Eric
Kasen, Daniel
Kirshner, Robert P.
Marion, G. H. Howie
Muena, Cesar
Nugent, Peter E.
Phelps, M.
Phillips, Mark M.
Qiu, Yulei
Quimby, Robert
Rines, K.
Silverman, Jeffrey M.
Suntzeff, Nicholas B.
Thomas, Rollin C.
Wang, Lifan
TI THE MOST SLOWLY DECLINING TYPE Ia SUPERNOVA 2001ay
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE supernovae: individual (SN 2001ay); techniques: photometric; techniques:
spectroscopic
ID MASS WHITE-DWARF; LIGHT CURVES; STANDARD STARS; MAXIMUM LIGHT;
K-CORRECTIONS; FACTORY OBSERVATIONS; INFRARED PHOTOMETRY; ABSOLUTE
MAGNITUDES; HUBBLE CONSTANT; LUMINOSITY
AB We present optical and near-infrared photometry, as well as ground-based optical spectra and Hubble Space Telescope ultraviolet spectra, of the Type Ia supernova (SN) 2001ay. At maximum light the Si II and Mg II lines indicated expansion velocities of 14,000 km s-(1), while Si III and S II showed velocities of 9000 km s(-1). There is also evidence for some unburned carbon at 12,000 km s(-1). SN 2001ay exhibited a decline-rate parameter of Delta m(15)(B) = 0.68 +/- 0.05 mag; this and the B-band photometry at t greater than or similar to + 25 day past maximum make it the most slowly declining Type Ia SN yet discovered. Three of the four super-Chandrasekhar-mass candidates have decline rates almost as slow as this. After correction for Galactic and host-galaxy extinction, SN 2001ay had M-B = -19.19 and M-V = -19.17 mag at maximum light; thus, it was not overluminous in optical bands. In near-infrared bands it was overluminous only at the 2 sigma level at most. For a rise time of 18 days (explosion to bolometric maximum) the implied Ni-56 yield was (0.58 +/- 0.15)/alpha M-circle dot, with alpha = L-max/E-Ni probably in the range 1.0-1.2. The Ni-56 yield is comparable to that of many Type Ia SNe. The "normal" Ni-56 yield and the typical peak optical brightness suggest that the very broad optical light curve is explained by the trapping of gamma rays in the inner regions.
C1 [Krisciunas, Kevin; Gooding, Samuel D.; Suntzeff, Nicholas B.; Wang, Lifan] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
[Li, Weidong; Filippenko, Alexei V.; Ganeshalingam, Mohan; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Howell, D. Andrew] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA.
[Howell, D. Andrew] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA.
[Stritzinger, Maximilian] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Aldering, Greg; Hsiao, Eric; Nugent, Peter E.; Thomas, Rollin C.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Berlind, Perry L.; Calkins, M.; Phelps, M.; Rines, K.] Fred L Whipple Observ, Amado, AZ 85645 USA.
[Challis, Peter; Chornock, Ryan; Kirshner, Robert P.; Marion, G. H. Howie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Conley, Alexander] Univ Colorado, Dept Astron, Boulder, CO 80309 USA.
[Germany, Lisa] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Gonzalez, Sergio; Muena, Cesar; Phillips, Mark M.] Las Campanas Observ, La Serena, Chile.
[Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Qiu, Yulei] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China.
[Quimby, Robert] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
RP Krisciunas, K (reprint author), Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA.
EM krisciunas@physics.tamu.edu; weidong@astro.berkeley.edu;
matheson@noao.edu; ahowell@lcogt.net; max.stritzinger@astro.su.se;
galdering@lbl.gov; berlind@cfa.harvard.edu; pchallis@cfa.harvard.edu;
rchornock@cfa.harvard.edu; alexander.conley@colorado.edu;
alex@astro.berkeley.edu; mganesh@astro.berkeley.edu;
lgermany@swin.edu.au; sam.gooding86@gmail.com; ehsiao@lbl.gov;
kasen@berkeley.edu; kirshner@cfa.harvard.edu; hman@astro.as.utexas.edu;
penugent@lbl.gov; mmp@lco.cl; qiuyl@bao.ac.cn; quimby@astro.caltech.edu;
jsilverman@astro.berkeley.edu; suntzeff@physics.tamu.edu;
rcthomas@lbl.gov; wang@physics.tamu.edu
OI stritzinger, maximilian/0000-0002-5571-1833
FU NASA [NAS5-26555, NAS 5-26555]; NSF; W. M. Keck Foundation; NSF
[AST-0908886, AST-0709181, AST-0907903]; TABASGO Foundation; NASA from
the Space Telescope Science Institute [AR-11248, AR-12126]; Office of
Science, Office of High Energy Physics, of the U.S. Department of Energy
[DE-AC02-05CH11231]
FX The work presented here is based in part on observations made with the
NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555; the Cerro
Tololo Inter-American Observatory and the Kitt Peak National Observatory
of the National Optical Astronomy Observatory, which is operated by the
Association of Universities for Research in Astronomy (AURA), Inc.,
under cooperative agreement with the NSF; the MMTObservatory, a joint
facility of the Smithsonian Institution and the University of Arizona;
the Fred L. Whipple Observatory; the Lick Observatory of the University
of California; the Las Campanas Observatory; the Beijing Astronomical
Observatory; and the W. M. Keck Observatory, which was generously funded
by the W. M. Keck Foundation and is operated as a scientific partnership
among the California Institute of Technology, the University of
California, and NASA. We thank the staffs at these observatories for
their efficient assistance, Don Groom for taking some of the Nickel 1 m
images, and Rachel Gibbons, Maryam Modjaz, Isobel Hook, and Saul
Perlmutter for other observational assistance. We are grateful to Peter
Hoflich, Alexei Khokhlov, and Eddie Baron for comments on Section 4.3.;
The supernova research of A.V.F.'s group at U. C. Berkeley is supported
by NSF grant AST-0908886 and by the TABASGO Foundation, as well as by
NASA through grants AR-11248 and AR-12126 from the Space Telescope
Science Institute, which is operated by Associated Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. KAIT and
its ongoing operation were made possible by donations from Sun
Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation,
Lick Observatory, the NSF, the University of California, the Sylvia &
Jim Katzman Foundation, and the TABASGO Foundation. J. M. S. is grateful
to Marc J. Staley for a Graduate Fellowship. K. K., L. W., and N. B. S.
are supported in part by NSF grant AST-0709181. Supernova research at
Harvard is supported by NSF grant AST-0907903. This work was also
supported by the Director, Office of Science, Office of High Energy
Physics, of the U.S. Department of Energy under Contract No.
DE-AC02-05CH11231.
NR 91
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 74
DI 10.1088/0004-6256/142/3/74
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700008
ER
PT J
AU Thomas, CA
Trilling, DE
Emery, JP
Mueller, M
Hora, JL
Benner, LAM
Bhattacharya, B
Bottke, WF
Chesley, S
Delbo, M
Fazio, G
Harris, AW
Mainzer, A
Mommert, M
Morbidelli, A
Penprase, B
Smith, HA
Spahr, TB
Stansberry, JA
AF Thomas, C. A.
Trilling, D. E.
Emery, J. P.
Mueller, M.
Hora, J. L.
Benner, L. A. M.
Bhattacharya, B.
Bottke, W. F.
Chesley, S.
Delbo, M.
Fazio, G.
Harris, A. W.
Mainzer, A.
Mommert, M.
Morbidelli, A.
Penprase, B.
Smith, H. A.
Spahr, T. B.
Stansberry, J. A.
TI ExploreNEOs. V. AVERAGE ALBEDO BY TAXONOMIC COMPLEX IN THE NEAR-EARTH
ASTEROID POPULATION
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids: general; surveys
ID THERMAL INFRARED SPECTROPHOTOMETRY; SPITZER-SPACE-TELESCOPE; 10302 1989
ML; SPECTROSCOPIC SURVEY; MAIN-BELT; PHYSICAL-CHARACTERIZATION; SPECTRAL
PROPERTIES; OPTICAL-PROPERTIES; OBJECT SURVEY; PHASE-II
AB Examining the albedo distribution of the near-Earth object (NEO) population allows for a better understanding of the relationship between absolute (H) magnitude and size, which impacts calculations of the size frequency distribution and impact hazards. Examining NEO albedos also sheds light on the differences between the NEO and Main Belt populations. We combine albedo results from the ExploreNEOs Warm Spitzer Exploration Science program with taxonomic classifications from the literature, publicly available data sets, and new observations from our concurrent spectral survey to derive the average albedos for C-, D-, Q-, S-, V-, and X-complex NEOs. Using a sample size of 118 NEOs, we calculate average albedos of 0.29(-0.04)(+0.05), 0.26(-0.03)(+0.04), and 0.42(-0.11)(+0.13) for the Q-, S-, and V-complexes, respectively. The averages for the C-and D-complexes are 0.13(-0.05)(+0.06) and 0.02(-0.01)(+0.02), but these averages are based on a small number of objects (five and two, respectively) and will improve with additional observations. We use albedos to assign X-complex asteroids to one of the E-, M-, or P-types. Our results demonstrate that the average albedos for the C-, S-, V-, and X-complexes are higher for NEOs than the corresponding averages observed in the Main Belt.
C1 [Thomas, C. A.; Trilling, D. E.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
[Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mueller, M.; Delbo, M.; Morbidelli, A.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France.
[Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Benner, L. A. M.; Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bhattacharya, B.] Claremont Mckenna Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bhattacharya, B.] Pitzer Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bhattacharya, B.] Scripps Coll, Joint Sci Dept, Claremont, CA 91711 USA.
[Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA.
[Harris, A. W.; Mommert, M.] DLR Inst Planetary Res, D-12489 Berlin, Germany.
[Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Thomas, CA (reprint author), No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA.
EM cristina.thomas@nau.edu
OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650;
Thomas, Cristina/0000-0003-3091-5757
FU NASA; National Aeronautics and Space Administration, Office of Space
Science, Planetary Astronomy Program [NCC 5-538, NNX-08AE38A]; National
Science Foundation [0506716]
FX This work is based in part on observations made with the Spitzer Space
Telescope, which is operated by JPL/Caltech under a contract with NASA.
Support for this work was provided by NASA through an award issued by
JPL/Caltech.; Some of this work was performed at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration (NASA). This material is
based in part upon work supported by NASA under the Science Mission
Directorate Research and Analysis Programs.; Part of the data utilized
in this publication were obtained and made available by the MIT-UH-IRTF
Joint Campaign for NEO Reconnaissance. The IRTF is operated by the
University of Hawaii under Cooperative Agreement no. NCC 5-538 with the
National Aeronautics and Space Administration, Office of Space Science,
Planetary Astronomy Program. The MIT component of this work is supported
by the National Science Foundation under Grant 0506716.; Visiting
Astronomer at the Infrared Telescope Facility, which is operated by the
University of Hawaii under Cooperative Agreement no. NNX-08AE38A with
the National Aeronautics and Space Administration, Science Mission
Directorate, Planetary Astronomy Program.
NR 53
TC 27
Z9 27
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD SEP
PY 2011
VL 142
IS 3
AR 85
DI 10.1088/0004-6256/142/3/85
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 817JY
UT WOS:000294669700019
ER
PT J
AU Levine, AM
Bradt, HV
Chakrabarty, D
Corbet, RHD
Harris, RJ
AF Levine, Alan M.
Bradt, Hale V.
Chakrabarty, Deepto
Corbet, Robin H. D.
Harris, Robert J.
TI AN EXTENDED AND MORE SENSITIVE SEARCH FOR PERIODICITIES IN ROSSI X-RAY
TIMING EXPLORER/ALL-SKY MONITOR X-RAY LIGHT CURVES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE binaries: general; X-rays: stars
ID ORBITAL PERIOD; BLACK-HOLE; NEUTRON-STAR; INTEGRAL OBSERVATIONS; PULSAR
EXO-1722-363; COMPACT OBJECT; GRO J1008-57; TIME-SERIES; 4TH EDITION; 4U
1746-371
AB We present the results of a systematic search in similar to 14 years of Rossi X-ray Timing Explorer All-Sky Monitor (ASM) data for evidence of periodicities. Two variations of the commonly used Fourier analysis search method have been employed to significantly improve upon the sensitivity achieved by Wen et al. in 2006, who also searched for periodicities in ASM data. In addition, the present search is comprehensive in terms of sources studied and frequency range covered, and has yielded the detection of the signatures of the orbital periods of eight low-mass X-ray binary systems and of ten high-mass X-ray binaries not listed in the tables of Wen et al. Orbital periods, epochs, signal amplitudes, modulation fractions, and folded light curves are given for each of these systems. Seven of the orbital periods are the most precise reported to date. In the course of this work, the 18.545 day orbital period of IGR J18483-0311 was co-discovered, and the first detections in X-rays were made of the similar to 3.9 day orbital period of LMC X-1 and the similar to 3.79 hr orbital period of 4U 1636-536. The results inform future searches for orbital and other periodicities in X-ray binaries.
C1 [Levine, Alan M.; Bradt, Hale V.; Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bradt, Hale V.; Chakrabarty, Deepto] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Corbet, Robin H. D.] Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA.
[Corbet, Robin H. D.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Harris, Robert J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Levine, AM (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM aml@space.mit.edu; hale@space.mit.edu; deepto@mit.edu;
robin.corbet@nasa.gov; rjharris@cfa.harvard.edu
FU NASA [NAS 5-30612 (MIT)]
FX We gratefully acknowledge the efforts of the RXTE/ASM science teams at
MIT and NASA/GSFC, and the RXTE mission support groups at GSFC. We thank
Alex Camacho for computing the upper limits presented in Table 3. We
also want to acknowledge an anonymous referee for helpful comments. This
work was supported by NASA through Contract NAS 5-30612 (MIT).
NR 81
TC 26
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD SEP
PY 2011
VL 196
IS 1
AR UNSP 6
DI 10.1088/0067-0049/196/1/6
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400006
ER
PT J
AU Otto, E
Green, PJ
Gray, RO
AF Otto, Elizabeth
Green, Paul J.
Gray, Richard O.
TI GALACTIC S STARS: INVESTIGATIONS OF COLOR, MOTION, AND SPECTRAL FEATURES
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars: abundances; stars: AGB and post-AGB; stars: carbon
ID DIGITAL SKY SURVEY; LATITUDE CARBON STARS; BRANCH STARS; SYSTEM;
EVOLUTION; CATALOG; 2MASS; TECHNETIUM
AB Known bright S stars, recognized as such by their enhanced s-process abundances and C/O ratio, are typically members of the asymptotic giant branch (AGB) or the red giant branch. Few modern digital spectra for these objects have been published, from which intermediate resolution spectral indices and classifications could be derived. For published S stars, we find accurate positions using the Two-Micron All Sky Survey (2MASS), and use the FAST spectrograph of the Tillinghast reflector on Mt. Hopkins to obtain the spectra of 57 objects. We make available a digital S star spectral atlas consisting of 14 spectra of S stars with diverse spectral features. We define and derive basic spectral indices that can help distinguish S stars from late-type (M) giants and carbon stars. We convolve all our spectra with the Sloan Digital Sky Survey bandpasses, and employ the resulting gri magnitudes together with 2MASS JHK(s) mags to investigate S star colors. These objects have colors similar to carbon and M stars, and are therefore difficult to distinguish by color alone. Using near-and mid-infrared colors from IRAS and Akari, we identify some of the stars as intrinsic (AGB) or extrinsic (with abundances enhanced by past mass transfer). We also use V band and 2MASS magnitudes to calculate a temperature index for stars in the sample. We analyze the proper motions and parallaxes of our sample stars to determine upper and lower limit absolute magnitudes and distances, and confirm that most are probably giants.
C1 [Otto, Elizabeth] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Green, Paul J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gray, Richard O.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA.
RP Otto, E (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA.
EM otto.65@buckeyemail.osu.edu
FU National Science Foundation Research Experiences for Undergraduates
(REU); Department of Defense [0754568]; Smithsonian Institution
FX Many thanks to the referee for a thorough reading. We are grateful to
Kevin Covey for the use of the high-quality sample of SDSS/2MASS
matches. Also, thanks to Warren Brown and Mukremin Kilic, who provided
many helpful discussions and hints on color selection and the SDSS
photometry. Many thanks to Doug Mink for all his invaluable help with
rvsao and SDSS correlations, and to Bill Wyatt for his help with
accessing SDSS DR-7 spectra, all of which we hope to use in upcoming
publications. We gratefully acknowledge Bob Kurucz, Andrew Vanture, and
George Wallerstein for illuminating discussions. Thanks also to Verne
Smith and G. W. for compiling an initial list of Li 6707 angstrom
detections in S stars. We are grateful to the SAO REU program
organizers-Marie Machacek, Christine Jones, and Jonathan McDowell-for
all their support. Finally, this work is supported in part by the
National Science Foundation Research Experiences for Undergraduates
(REU) and Department of Defense Awards to Stimulate and Support
Undergraduate Research Experiences (ASSURE) programs under Grant No.
0754568 and by the Smithsonian Institution.
NR 37
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U1 0
U2 3
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 SEP
PY 2011
VL 196
IS 1
AR UNSP 5
DI 10.1088/0067-0049/196/1/5
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RT
UT WOS:000294773400005
ER
PT J
AU Vaslet, A
France, C
Phillips, DL
Feller, IC
Baldwin, CC
AF Vaslet, A.
France, C.
Phillips, D. L.
Feller, I. C.
Baldwin, C. C.
TI Stable-isotope analyses reveal the importance of seagrass beds as
feeding areas for juveniles of the speckled worm eel Myrophis punctatus
(Teleostei: Ophichthidae) in Florida
SO JOURNAL OF FISH BIOLOGY
LA English
DT Article
DE Anguilliformes; mangroves; resource partitioning; SIAR; stomach contents
ID INCORPORATING CONCENTRATION-DEPENDENCE; INDIAN-RIVER LAGOON; MIXING
MODELS; ANGUILLIFORMES OPHICHTHIDAE; MANGROVE CARBON; NITROGEN; FISH;
LEPTOCEPHALI; ECOSYSTEMS; MARINE
AB The feeding habits and habitats of the speckled worm eel Myrophis punctatus were studied on the mangrove edge of the Indian River Lagoon (IRL, Florida) using gut-content and stable-isotope analyses of carbon (delta C-13) and nitrogen (delta N-15). Four taxa were identified through analyses of gut contents, and the index of relative importance suggested that amphipods, microphytobenthos and annelids are the most important food sources in the fish's diet. To assess the feeding habits of the fish after their recruitment to the IRL, these food sources were collected from mangroves and nearby seagrass beds for isotope analyses. Stable isotopes constituted a powerful tool for discriminating fish prey items from mangroves (mean +/- S.D. delta C-13 = -20.5 +/- 0.6%) and those from seagrass beds (mean +/- S.D. delta C-13 = -16.9 +/- 0.6%), thus providing good evidence of food source origins. The 56 M. punctatus collected [10.0 < total length (L-T) < 16.2 cm] had average isotopic signatures of delta C-13 = -16.7 +/- 0.2% and delta N-15 = 8.2 +/- 0.1%. A significant depletion in C-13 was observed for larger juveniles (15.0 < L-T < 16.2 cm), suggesting that they found a portion of their food in mangroves. Estimation of the trophic level from stable isotopes (T-Liso) was similar among different size groups of juvenile fish (T-Liso = 3.2-3.5); therefore, M. punctatus was considered a secondary consumer, which is consistent with its zoobenthic diet. The concentration-dependent mixing Stable Isotope Analysis in R (SIAR) model revealed the importance of food sources from seagrass beds as carbon sources for all the fish collected, with a significant increase in mangrove prey contributions, such as annelids, in the diet of larger juveniles. This study highlights the importance of seagrass beds as feeding habitats for juveniles of M. punctatus after their recruitment to coastal waters. (C) 2011 The Authors Journal of Fish Biology (C) 2011 The Fisheries Society of the British Isles
C1 [Vaslet, A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
[France, C.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA.
[Phillips, D. L.] US EPA, Natl Hlth & Environm Effects Res Lab, Western Ecol Div, Corvallis, OR 97333 USA.
[Feller, I. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Baldwin, C. C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Vaslet, A (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.
EM amandine.vaslet@gmail.com
OI Feller, Ilka/0000-0002-6391-1608
FU SMSFP
FX The authors thank Z. Foltz, W. Lee from Smithsonian Marine Station at
Fort Pierce (SMSFP) for their help in field collections and all the
staff of the SMSFP for their assistance and the access of the laboratory
facilities. We are grateful to A. Jackson and A. Parnell for their help
on SIAR mixing model and to R. M. Connolly for his comments and
suggestions on the manuscript. The authors thank four anonymous referees
for their comments that substantially improved this manuscript. This
research was funded by SMSFP Postdoctoral Fellowship. Collecting in
Florida was conducted pursuant to SAL #09-1024-SR to C. C. B. D.L.P.'s
time was provided by the U. S. Environmental Protection Agency. The
manuscript has been subjected to the Agency's peer and administrative
review, and it has been approved for publication as an EPA document.
Mention of trade names or commercial products does not constitute
endorsement or recommendation for use. This is contribution number 851
from the Smithsonian Marine Station at Fort Pierce.
NR 44
TC 5
Z9 6
U1 1
U2 27
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-1112
EI 1095-8649
J9 J FISH BIOL
JI J. Fish Biol.
PD SEP
PY 2011
VL 79
IS 3
BP 692
EP 706
DI 10.1111/j.1095-8649.2011.03052.x
PG 15
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 816KO
UT WOS:000294598300008
PM 21884107
ER
PT J
AU Ubelaker, DH
AF Ubelaker, Douglas H.
TI The Forensic Sciences: International Perspectives, Global Vision
SO JOURNAL OF FORENSIC SCIENCES
LA English
DT Editorial Material
C1 Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA.
RP Ubelaker, DH (reprint author), Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, MRC 112, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-1198
J9 J FORENSIC SCI
JI J. Forensic Sci.
PD SEP
PY 2011
VL 56
IS 5
BP 1091
EP 1093
DI 10.1111/j.1556-4029.2011.01876.x
PG 3
WC Medicine, Legal
SC Legal Medicine
GA 816OT
UT WOS:000294612600001
PM 21884118
ER
PT J
AU Dutton, AA
Conroy, C
van den Bosch, FC
Simard, L
Mendel, JT
Courteau, S
Dekel, A
More, S
Prada, F
AF Dutton, Aaron A.
Conroy, Charlie
van den Bosch, Frank C.
Simard, Luc
Mendel, J. Trevor
Courteau, Stephane
Dekel, Avishai
More, Surhud
Prada, Francisco
TI Dark halo response and the stellar initial mass function in early-type
and late-type galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: fundamental
parameters; galaxies: haloes; galaxies: spiral; galaxies: structure;
dark matter
ID DIGITAL SKY SURVEY; TULLY-FISHER RELATION; TO-LIGHT RATIOS; LENS ACS
SURVEY; DISPERSION-SUPPORTED GALAXIES; URSA-MAJOR CLUSTER; MATTER
HALOES; ELLIPTIC GALAXIES; STAR-FORMATION; FUNDAMENTAL PLANE
AB We investigate the origin of the relations between stellar mass and optical circular velocity for early-type galaxies (ETGs) and late-type galaxies (LTGs) - the Faber-Jackson (FJ) and Tully-Fisher (TF) relations. We combine measurements of dark halo masses (from satellite kinematics and weak lensing), and the distribution of baryons in galaxies (from a new compilation of galaxy scaling relations), with constraints on dark halo structure from cosmological simulations. The principal unknowns are the halo response to galaxy formation and the stellar initial mass function (IMF). The slopes of the TF and FJ relations are naturally reproduced for a wide range of halo response and IMFs. However, models with a universal IMF and universal halo response cannot simultaneously reproduce the zero-points of both the TF and FJ relations. For a model with a universal Chabrier IMF, LTGs require halo expansion, while ETGs require halo contraction. A Salpeter IMF is permitted for high-mass (sigma greater than or similar to 180 km s(-1)) ETGs, but is inconsistent for intermediate masses, unless V-circ(R-e)/sigma(e) greater than or similar to 1.6. If the IMF is universal and close to Chabrier, we speculate that the presence of a major merger may be responsible for the contraction in ETGs while clumpy accreting streams and/or feedback leads to expansion in LTGs. Alternatively, a recently proposed variation in the IMF disfavours halo contraction in both types of galaxies. Finally we show that our models naturally reproduce flat and featureless circular velocity profiles within the optical regions of galaxies without fine-tuning.
C1 [Dutton, Aaron A.; Mendel, J. Trevor] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van den Bosch, Frank C.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Courteau, Stephane] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada.
[Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[More, Surhud] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain.
RP Dutton, AA (reprint author), Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
EM dutton@uvic.ca
RI More, Surhud/A-5049-2013
OI More, Surhud/0000-0002-2986-2371
FU Canadian Institute for Theoretical Astrophysics (CITA); Natural Science
and Engineering Research Council of Canada; ISF [6/08]; GIF
[G-1052-104.7/2009]; DIP; Einstein Center at HU; NSF at USA [1010033];
Alfred P. Sloan Foundation; National Aeronautics and Space
Administration; National Science Foundation; US Department of Energy;
Japanese Monbukagakusho; Max Planck Society; University of Chicago;
Fermilab; Institute for Advanced Study; Japan Participation Group; Johns
Hopkins University; Los Alamos National Laboratory; Max-Planck-Institute
for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New
Mexico State University; University of Pittsburgh; Princeton University;
United States Naval Observatory; University of Washington
FX AAD acknowledges financial support from the Canadian Institute for
Theoretical Astrophysics (CITA) National Fellows programme. SC
acknowledges the support of a Discovery grant by the Natural Science and
Engineering Research Council of Canada. The work of AD was partly
supported by ISF grant 6/08, GIF grant G-1052-104.7/2009, a DIP grant,
the Einstein Center at HU and NSF grant 1010033 at USA. This research
has made use of NASA's Astrophysics Data System Bibliographic Services.;
Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Aeronautics and Space Administration, the National Science Foundation,
the US Department of Energy, the Japanese Monbukagakusho and the Max
Planck Society. The SDSS web site is http://www.sdss.org/.; The SDSS is
managed by the Astrophysical Research Consortium (ARC) for the
Participating Institutions. The Participating Institutions are The
University of Chicago, Fermilab, the Institute for Advanced Study, the
Japan Participation Group, The Johns Hopkins University, Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, University of Pittsburgh, Princeton University, the United
States Naval Observatory and the University of Washington.
NR 166
TC 89
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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 SEP
PY 2011
VL 416
IS 1
BP 322
EP 345
DI 10.1111/j.1365-2966.2011.19038.x
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000028
ER
PT J
AU Lin, MK
Krumholz, MR
Kratter, KM
AF Lin, Min-Kai
Krumholz, Mark R.
Kratter, Kaitlin M.
TI Spin-down of protostars through gravitational torques
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; hydrodynamics; methods: numerical; stars:
protostars; stars: rotation
ID ANGULAR-MOMENTUM EVOLUTION; ADAPTIVE MESH REFINEMENT; GAMMA-RAY BURSTS;
STAR-FORMATION; ACCRETION DISC; MASSIVE STARS; YOUNG STARS; 1ST STARS;
FRAGMENTATION; COLLAPSE
AB Young protostars embedded in circumstellar discs accrete from an angular momentum rich mass reservoir. Without some braking mechanism, all stars should be spinning at or near breakup velocity. In this paper, we perform simulations of the self-gravitational collapse of an isothermal cloud using the ORION adaptive-mesh refinement code and investigate the role that gravitational torques might play in the spin-down of the dense central object. While magnetic effects likely dominate for low-mass stars, high-mass and Population III stars might be less well magnetized. We find that gravitational torques alone prevent the central object from spinning up to more than half of its breakup velocity, because higher rotation rates lead to bar-like deformations that enable efficient angular momentum transfer to the surrounding medium. We also find that the long-term spin evolution of the central object is dictated by the properties of the surrounding disc. In particular, spiral modes with the azimuthal wavenumber m = 2 couple more effectively to its spin than the lopsided m = 1 mode, which was found to inhibit spin evolution. We suggest that even in the absence of magnetic fields, gravitational torques may provide an upper limit on stellar spin, and that moderately massive circumstellar discs can cause long-term spin-down.
C1 [Lin, Min-Kai; Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
[Lin, Min-Kai] Univ Cambridge, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England.
[Kratter, Kaitlin M.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Lin, MK (reprint author), Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA.
EM mk123@cam.ac.uk; krumholz@ucolick.org; kkratter@cfa.harvard.edu
OI Krumholz, Mark/0000-0003-3893-854X
FU NSF [0847477, AST-0807739, CAREER-0955300]; France-Berkeley fund;
Institute for Geophysics and Planetary Physics; Center for Origin,
Dynamics and Evolution of Planets; Isaac Newton Trust; St. John's
College, Cambridge; Alfred P. Sloan Fellowship; NASA [NNX09AK31G];
Spitzer Space Telescope Theoretical Research Program grant
FX This project was initiated during the ISIMA 2010 summer programme,
funded by the NSF CAREER grant 0847477, the France-Berkeley fund, the
Institute for Geophysics and Planetary Physics and the Center for
Origin, Dynamics and Evolution of Planets. We thank them for their
support. M-KL acknowledges support from the Isaac Newton Trust and St.
John's College, Cambridge. MRK acknowledges support from an Alfred P.
Sloan Fellowship, NSF grants AST-0807739 and CAREER-0955300, and NASA
through Astro-physics Theory and Fundamental Physics grant NNX09AK31G
and a Spitzer Space Telescope Theoretical Research Program grant. KMK is
supported by an Institute for Theory and Computation Postdoctoral
Fellowship at Harvard College Observatory.
NR 45
TC 13
Z9 13
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 1
BP 580
EP 590
DI 10.1111/j.1365-2966.2011.19074.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000053
ER
PT J
AU Lu, Y
Keres, D
Katz, N
Mo, HJ
Fardal, M
Weinberg, MD
AF Lu, Yu
Keres, Dusan
Katz, Neal
Mo, H. J.
Fardal, Mark
Weinberg, Martin D.
TI On the algorithms of radiative cooling in semi-analytic models
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; galaxies: evolution; galaxies: formation
ID DARK-MATTER HALOES; PARTICLE HYDRODYNAMICS SIMULATIONS; DISSIPATIONAL
GALAXY FORMATION; LAMBDA-CDM UNIVERSE; COSMOLOGICAL SIMULATIONS;
STAR-FORMATION; GAS ACCRETION; MASS FUNCTION; COLD FLOWS; EVOLUTION
AB We study the behaviour of multiple radiative-cooling algorithms implemented in seven semi-analytic models (SAMs) of galaxy formation, including a new model we propose in this paper. We use versions of the models without feedback and apply them to dark matter haloes growing in a cosmological context, which have final virial masses that range from 1011 to 10(14)M(circle dot). First, using simplified smoothly growing halo models, we demonstrate that the different algorithms predict cooling rates and final cold gas masses that differ by a factor of similar to 5 for massive haloes (>= 10(12)M(circle dot)). The algorithms are in better agreement for less massive haloes because they cool efficiently and, therefore, their cooling rates are largely limited by the halo accretion rate. However, for less massive haloes, all the SAMs predict less cooling than corresponding 1D hydrodynamic models. Secondly, we study the gas-accretion history of the central galaxies of dark matter haloes using merger trees. The inclusion of mergers alters the cooling history of haloes by locking up gas in galaxies within small haloes at early times. For realistic halo models, the dispersion in the cold gas mass predicted by the algorithms is 0.5 dex for high-mass haloes and 0.1 dex for low-mass haloes, while the dispersion in the accretion rate is about two times larger. Comparing to cosmological smoothed particle hydrodynamic simulations, we find that most SAMs systematically underpredict the gas-accretion rates for low-mass haloes but overpredict the gas-accretion rates for massive haloes. Although the models all include both 'rapid'-and 'slow'-mode accretion, the transition between the two accretion modes varies between models and also differs from the simulations. Finally, we construct a new phenomenological model that explicitly incorporates cold halo gas and a gradual transition between the cold and hot modes of gas accretion to illustrate that such a class ofmodels can bettermatch the results from cosmological hydrodynamic simulations. The large dispersion in cooling rates between different SAMs influences parameter choices for other galaxy physics, including star formation and feedback. Therefore, careful parametrizations of the multimode gas cooling and accretion mechanisms in simulations are necessary to ensure that the predictions from SAMs are reliable.
C1 [Lu, Yu; Katz, Neal; Mo, H. J.; Fardal, Mark; Weinberg, Martin D.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Lu, Yu] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA.
[Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA.
RP Lu, Y (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
EM luyu@stanford.edu
RI Mo, Houjun/P-7811-2015;
OI Weinberg, Martin/0000-0003-2660-2889
FU Harvard University; NASA [HSTHF-51276.01-A]; NSF [0611948, 0908334];
NASA AISR [NNG06GF25G]
FX We thank Andrew Benson, Darren Croton and Martin White for useful
discussion. DK acknowledges support from Harvard University funds and
from NASA through Hubble Fellowship grant HSTHF-51276.01-A. This work
was supported in part by NSF IIS Program through award 0611948 and by
NASA AISR Program through award NNG06GF25G. HJM acknowledges the support
of NSF 0908334.
NR 70
TC 23
Z9 23
U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 1
BP 660
EP 679
DI 10.1111/j.1365-2966.2011.19072.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000061
ER
PT J
AU Kipping, DM
AF Kipping, David M.
TI LUNA: an algorithm for generating dynamic planet-moon transits
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: analytical; techniques: photometric; eclipses; planets and
satellites: general; planetary systems
ID EXTRASOLAR PLANETS; LIGHT CURVES; SATELLITES; PHOTOMETRY; EXOMOON;
HD-189733; ORBITS; MODEL
AB It has been previously shown that moons of extrasolar planets may be detectable with the Kepler Mission, for moon masses above similar to 0.2M(circle dot). Transit timing effects have been formerly identified as a potent tool to this end, exploiting the dynamics of the system. In this work, we explore the simulation of transit light curves of a planet plus a single moon including not only the transit timing effects, but also the light-curve signal of the moon itself. We introduce our new algorithm, LUNA, which produces transit light curves for both bodies, analytically accounting for shadow overlaps, stellar limb darkening and planet-moon dynamical motion. By building the dynamics into the core of LUNA, the routine automatically accounts for transittiming/duration variations and ingress/egress asymmetries for not only the planet, but also the moon.
We then generate some artificial data for two feasibly detectable hypothetical systems of interest: (i) prograde and (ii) retrograde Earth-like moons around a habitable-zone Neptune for an M dwarf system. We fit the hypothetical systems using LUNA and demonstrate the feasibility of detecting these cases with Kepler photometry.
C1 [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kipping, David M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dkipping@cfa.harvard.edu
FU Smithsonian Institution; NASA [NNX08AF23G]; UCL through the Science
Technology and Facilities Council (STFC)
FX DMK has been supported by Smithsonian Institution Restricted Endowment
Funds, NASA grant NNX08AF23G and UCL through the Science Technology and
Facilities Council (STFC) studentships. Special thanks to the anonymous
referee for highly useful advices and suggestions.
NR 37
TC 31
Z9 31
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 1
BP 689
EP 709
DI 10.1111/j.1365-2966.2011.19086.x
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000063
ER
PT J
AU Field, GB
Blackman, EG
Keto, ER
AF Field, George B.
Blackman, Eric G.
Keto, Eric R.
TI Does external pressure explain recent results for molecular clouds?
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM: clouds; ISM: evolution; ISM: structure
ID MASS; TURBULENCE
AB The recent paper by Heyer et al. indicates that observations of size, linewidth and column density of interstellar clouds do not agree with simple virial equilibrium (SVE) as a balance between gravitational and kinetic energies in the sense that the clouds either have too much kinetic energy or too little mass to be bound. This may be explained by violation of SVE as suggested by Dobbs et al., by observational underestimation of the masses as suggested by Heyer et al. or by an external pressure acting as an additional confining force as suggested earlier by Heyer et al. The data of Heyer et al. cannot be explained with a single value for the external pressure, but if different clouds in the sample have different external pressures in the range of P-e/k = 10(4)-10(7) cm(-3) K, then most of the clouds could be in pressure-bounded virial equilibrium. In this paper we discuss two consequences of the external pressure. First, we show that the observational data are consistent with the hypothesis that most clouds are at a critical mass for dynamical stability determined solely by the pressure. Above this mass a cloud is unstable to gravitational collapse or fragmentation. Secondly, we show that the external pressure modifies the well-known size-linewidth relationship first proposed by Larson so that the proportionality is no longer constant but depends on the external pressure.
C1 [Field, George B.; Keto, Eric R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Blackman, Eric G.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
RP Field, GB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM keto@cfa.harvard.edu
NR 25
TC 22
Z9 22
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD SEP
PY 2011
VL 416
IS 1
BP 710
EP 714
DI 10.1111/j.1365-2966.2011.19091.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808YD
UT WOS:000294017000064
ER
PT J
AU Harasewych, MG
Petit, RE
AF Harasewych, M. G.
Petit, Richard E.
TI Two new species of Admetinae (Gastropoda: Cancellariidae) from the
northeastern Pacific Ocean
SO NAUTILUS
LA English
DT Article
DE Mollusca; Neogastropoda; Admete; Neadmete; Bathyal; hydrothermal vents;
egg capsules
ID EGG CAPSULES
AB Two new species of the cancellariid subfamily Admetinae are described from bathyal depths of the northeastern Pacific Ocean. Admete verenae is presently known only from the hydrothermal vents of the Juan de Fuca Ridge, at depths of 2192 to 2415 in. It differs from other Admete in having a large shell with a high spire, strong spiral sculpture, and anteriorly tapering aperture with a deflected siphonal canal and a distinctive siphonal fasciole. Egg capsules, each containing 5-8 embryos, are broadly oval, V-shaped in end view, and raised on a short, broad stalk. Neadmete allot, from off northern California and Washington State at depths of 276 to 732 m, may be recognized by its distinctive tabulate spire profile and broad, strongly channeled sutural ramp, as well by its anteriorly tapered aperture.
C1 [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.
RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 7012, Washington, DC 20013 USA.
EM Harasewych@si.edu; r.e.petit@att.net
NR 14
TC 0
Z9 1
U1 0
U2 3
PU BAILEY-MATTHEWS SHELL MUSEUM
PI SANIBEL
PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD,
SANIBEL, FL 33957 USA
SN 0028-1344
J9 NAUTILUS
JI Nautilus
PD SEP 1
PY 2011
VL 125
IS 3
BP 159
EP 163
PG 5
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 817BW
UT WOS:000294646800006
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI The great Martian catastrophe and how Kepler fixed it
SO PHYSICS TODAY
LA English
DT Article
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 6
TC 2
Z9 2
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD SEP
PY 2011
VL 64
IS 9
BP 50
EP 54
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 818LF
UT WOS:000294752500018
ER
PT J
AU Panzer, M
AF Panzer, Mary
TI "This is the Photo League"
SO APERTURE
LA English
DT Article
C1 [Panzer, Mary] NYU, Dept Media Culture & Commun, Steinhardt Sch Culture Educ & Human Dev, New York, NY 10003 USA.
[Panzer, Mary] Natl Portrait Gallery, Smithsonian Inst, Washington, DC USA.
RP Panzer, M (reprint author), NYU, Dept Media Culture & Commun, Steinhardt Sch Culture Educ & Human Dev, New York, NY 10003 USA.
NR 0
TC 1
Z9 1
U1 0
U2 0
PU APERTURE
PI NEW YORK
PA 20 EAST 23RD ST, NEW YORK, NY 10010 USA
SN 0003-6420
J9 APERTURE
JI Aperture
PD FAL
PY 2011
IS 204
BP 32
EP +
PG 4
WC Art
SC Art
GA 812UQ
UT WOS:000294318800008
ER
PT J
AU Di Stefano, R
Voss, R
Claeys, JSW
AF Di Stefano, R.
Voss, R.
Claeys, J. S. W.
TI SPIN-UP/SPIN-DOWN MODELS FOR TYPE Ia SUPERNOVAE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE accretion, accretion disks; cosmological parameters; dark energy;
supernovae: general; white dwarfs
ID ACCRETING WHITE-DWARFS; RAPIDLY ROTATING STARS; X-RAY SOURCES;
CATACLYSMIC VARIABLES; SUPERSOFT SOURCES; AE-AQUARII; EXTERNAL GALAXIES;
SOFT SOURCES; QUASI-SOFT; EVOLUTION
AB In the single-degenerate scenario for Type Ia supernovae (SNe Ia), a white dwarf (WD) must gain a significant amount of matter from a companion star. Because the accreted mass carries angular momentum, the WD is likely to achieve fast spin periods, which can increase the critical mass, M-crit, needed for explosion. When M-crit is higher than the maximum mass achieved by the WD, the central regions of the WD must spin down before it can explode. This introduces super-Chandrasekhar single-degenerate explosions, and a delay between the completion of mass gain and the time of the explosion. Matter ejected from the binary during mass transfer therefore has a chance to become diffuse, and the explosion occurs in a medium with a density similar to that of typical regions of the interstellar medium. Also, either by the end of the WD's mass increase or else by the time of explosion, the donor may exhaust its stellar envelope and become a WD. This alters, generally diminishing, explosion signatures related to the donor star. Nevertheless, the spin-up/spin-down model is highly predictive. Prior to explosion, progenitors can be super-M-Ch WDs in either wide binaries with WD companions or cataclysmic variables. These systems can be discovered and studied through wide-field surveys. Post-explosion, the spin-up/spin-down model predicts a population of fast-moving WDs, low-mass stars, and even brown dwarfs. In addition, the spin-up/spin-down model provides a paradigm which may be able to explain both the similarities and the diversity observed among SNe Ia.
C1 [Di Stefano, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Voss, R.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands.
[Claeys, J. S. W.] Univ Utrecht, Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands.
RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NSF [AST-0908878]; Smithsonian Astrophysical Observatory
FX We thank Ryan Chornock, Ryan Foley, Boris Gaensicke, Robert P. Kirshner,
and Andrew MacFadyen for comments. This work was supported in part by
NSF through AST-0908878 and by a development award from the Smithsonian
Astrophysical Observatory. The authors thank the Lorentz Center for its
hospitality during the workshop "Observational signatures of Type Ia
supernova progenitors," where this work was started.
NR 47
TC 60
Z9 60
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD SEP 1
PY 2011
VL 738
IS 1
AR L1
DI 10.1088/2041-8205/738/1/L1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808FA
UT WOS:000293961400001
ER
PT J
AU Stouffer, PC
Cockle, KL
Aleixo, A
Areta, JI
Barnett, JM
Bodrati, A
Cadena, CD
Di Giacomo, AS
Herzog, SK
Hosner, P
Johnson, EI
Naka, LN
Sanchez, C
AF Stouffer, Philip C.
Cockle, Kristina L.
Aleixo, Alexandre
Areta, Juan I.
Mazar Barnett, Juan
Bodrati, Alejandro
Daniel Cadena, Carlos
Di Giacomo, Adrian S.
Herzog, Sebastian K.
Hosner, Peter
Johnson, Erik I.
Naka, Luciano N.
Sanchez, Cesar
TI No evidence for widespread bird declines in protected South American
forests
SO CLIMATIC CHANGE
LA English
DT Article
ID ATLANTIC FOREST; CLIMATE-CHANGE; SPECIES RICHNESS; FRAGMENTS;
EXTINCTIONS; COMMUNITY; CONSERVATION; ABUNDANCE
C1 [Stouffer, Philip C.; Johnson, Erik I.] Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
[Stouffer, Philip C.; Johnson, Erik I.] Smithsonian Trop Res Inst, BR-69060 Manaus, Amazonas, Brazil.
[Stouffer, Philip C.; Johnson, Erik I.] Inst Nacl de Pesquisas da Amazonia, Projeto Dinam Biol Fragmentos Florestais, BR-69060 Manaus, Amazonas, Brazil.
[Cockle, Kristina L.] Univ British Columbia, Dept Forest Sci, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada.
[Aleixo, Alexandre] MCT Museu Paraense Emilio Goeldi, Belem, Para, Brazil.
[Areta, Juan I.] CICyTTP CONICET, RA-3105 Diamante, Entre Rios, Argentina.
[Bodrati, Alejandro] Proyecto Selva Pino Parana, San Pedro, Misiones, Argentina.
[Daniel Cadena, Carlos] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia.
[Di Giacomo, Adrian S.] FCEN Univ Buenos Aires, Dept Ecol Genet & Evoluc, Buenos Aires, DF, Argentina.
[Herzog, Sebastian K.] Asociac Armonia BirdLife Int, Santa Cruz, Bolivia.
[Hosner, Peter] Univ Kansas, Nat Hist Museum, Lawrence, KS 66044 USA.
[Hosner, Peter] Univ Kansas, Biodivers Res Ctr, Lawrence, KS 66044 USA.
[Naka, Luciano N.; Sanchez, Cesar] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Naka, Luciano N.; Sanchez, Cesar] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
RP Stouffer, PC (reprint author), Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
EM pstouffer@lsu.edu
RI Naka, Luciano/G-7485-2014; Aleixo, Alexandre/L-3135-2013;
OI Cockle, Kristina/0000-0002-6502-923X; Areta, Juan
Ignacio/0000-0001-8588-3030
FU US National Science Foundation [LTREB-0545491]
FX Funding for the research in Manaus was provided by the US National
Science Foundation (LTREB-0545491). This is publication 574 of the BDFFP
INPA/STRI Technical Series and 21 of the Amazonian Ornithology Technical
Series of the INPA Collections Program. The manuscript was approved by
the Director of the Louisiana State University Agricultural Center as
manuscript number 2011-241-6154.
NR 27
TC 1
Z9 1
U1 1
U2 15
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0165-0009
EI 1573-1480
J9 CLIMATIC CHANGE
JI Clim. Change
PD SEP
PY 2011
VL 108
IS 1-2
BP 383
EP 386
DI 10.1007/s10584-011-0162-1
PG 4
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 814NV
UT WOS:000294464000019
ER
PT J
AU Campbell, BA
Putzig, NE
Carter, LM
Phillips, RJ
AF Campbell, Bruce A.
Putzig, Nathaniel E.
Carter, Lynn M.
Phillips, Roger J.
TI Autofocus Correction of Phase Distortion Effects on SHARAD Echoes
SO IEEE GEOSCIENCE AND REMOTE SENSING LETTERS
LA English
DT Article
DE Mars; radar signal processing; spaceborne radar
ID MAGNETIC-FIELD; MARS; IONOSPHERE; SHARPNESS
AB SHARAD is a frequency-modulated (15-25 MHz) radar sounder that probes the upper few kilometers of the Martian crust and polar layered deposits. At solar zenith angles less than about 100 degrees, the ionosphere of Mars can induce phase distortion in surface and subsurface radar echoes that substantially degrades the signal-to-noise ratio and vertical resolution of the range-compressed data. We present a range-compression autofocus approach that estimates the phase distortion of SHARAD data along ground-track segments of about 100 km, using a power-law image-sharpness metric and an empirically derived scaling between the phase correction and radar frequency. This method is rapid, yields a greatly improved subsurface image, and provides a means to track regional and temporal changes in the Martian ionosphere.
C1 [Campbell, Bruce A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
[Putzig, Nathaniel E.; Phillips, Roger J.] SW Res Inst, Boulder, CO 80302 USA.
[Carter, Lynn M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20706 USA.
RP Campbell, BA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA.
EM campbellb@si.edu; nathaniel@putzig.com; lynn.m.carter@nasa.gov;
roger@boulder.swri.edu
RI Carter, Lynn/D-2937-2012
NR 23
TC 9
Z9 10
U1 0
U2 6
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA
SN 1545-598X
EI 1558-0571
J9 IEEE GEOSCI REMOTE S
JI IEEE Geosci. Remote Sens. Lett.
PD SEP
PY 2011
VL 8
IS 5
BP 939
EP 942
DI 10.1109/LGRS.2011.2143692
PG 4
WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote
Sensing; Imaging Science & Photographic Technology
SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science
& Photographic Technology
GA 815RY
UT WOS:000294546900021
ER
PT J
AU Stoop, J
Mishchenko, MI
Menguc, MP
Rothman, LS
AF Stoop, Jose
Mishchenko, Michael I.
Menguc, M. Pinar
Rothman, Laurence S.
TI SPECIAL ISSUE POLARIMETRIC DETECTION, CHARACTERIZATION, AND REMOTE
SENSING
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Editorial Material
C1 [Stoop, Jose] Elsevier, NL-1043 NX Amsterdam, Netherlands.
[Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
[Menguc, M. Pinar] Ozyegin Univ, Ctr Energy Environm & Econ, TR-34662 Istanbul, Turkey.
[Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
RP Stoop, J (reprint author), Elsevier, Radarweg 29, NL-1043 NX Amsterdam, Netherlands.
EM J.Stoop@elsevier.com; mmishchenko@giss.nasa.gov;
pinar.menguc@ozyegin.edu.tr; lrothman@cfa.harvard.edu
RI Menguc, Pinar/O-3114-2013; Mishchenko, Michael/D-4426-2012
NR 1
TC 2
Z9 2
U1 0
U2 4
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 SEP
PY 2011
VL 112
IS 13
SI SI
BP 2041
EP 2041
DI 10.1016/j.jqsrt.2011.06.020
PG 1
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 815IC
UT WOS:000294518300001
ER
PT J
AU Grinolds, MS
Maletinsky, P
Hong, S
Lukin, MD
Walsworth, RL
Yacoby, A
AF Grinolds, M. S.
Maletinsky, P.
Hong, S.
Lukin, M. D.
Walsworth, R. L.
Yacoby, A.
TI Quantum control of proximal spins using nanoscale magnetic resonance
imaging
SO NATURE PHYSICS
LA English
DT Article
ID SINGLE SPIN; DIAMOND; RESOLUTION; MICROSCOPY; CENTERS; SPECTROSCOPY;
FABRICATION
AB Quantum control of individual spins in condensed-matter systems is an emerging field with wide-ranging applications in spintronics(1), quantum computation(2) and sensitive magnetometry(3). Recent experiments have demonstrated the ability to address and manipulate single electron spins through either optical(4,5) or electrical techniques(6-8). However, it is a challenge to extend individual-spin control to nanometre-scale multi-electron systems, as individual spins are often irre-solvable with existing methods. Here we demonstrate that coherent individual-spin control can be achieved with few-nanometre resolution for proximal electron spins by carrying out single-spin magnetic resonance imaging (MRI), which is realized using a scanning-magnetic-field gradient that is both strong enough to achieve nanometre spatial resolution and sufficiently stable for coherent spin manipulations. We apply this scanning-field-gradient MRI technique to electronic spins in nitrogen-vacancy (NV) centres in diamond and achieve nanometre resolution in imaging, characterization and manipulation of individual spins. For NV centres, our results in individual-spin control demonstrate an improvement of nearly two orders of magnitude in spatial resolution when compared with conventional optical diffraction-limited techniques. This scanning-field-gradient microscope enables a wide range of applications including materials characterization, spin entanglement and nanoscale magnetometry.
C1 [Grinolds, M. S.; Maletinsky, P.; Lukin, M. D.; Walsworth, R. L.; Yacoby, A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Hong, S.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
EM yacoby@physics.harvard.edu
RI Maletinsky, Patrick/L-1851-2015; Hong, Sungkun/D-3282-2014
OI Maletinsky, Patrick/0000-0003-1699-388X; Hong,
Sungkun/0000-0003-0985-6641
FU Department of Defense; NSF; Swiss National Science Foundation; Kwanjeong
Scholarship Foundation; NIST; DARPA
FX We gratefully acknowledge G. Balasubramanian and P. R. Hemmer for
fruitful technical discussions, as well as B. Hausmann and M. Loncar for
instruction in the fabrication of NV-centre-containing nanostructures.
M.S.G. is supported through fellowships from the Department of Defense
(NDSEG program) and the NSF. P.M. acknowledges support from the Swiss
National Science Foundation, and S.H. thanks the Kwanjeong Scholarship
Foundation for fellowship funding. This work was supported by NIST and
DARPA.
NR 31
TC 71
Z9 73
U1 2
U2 51
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1745-2473
J9 NAT PHYS
JI Nat. Phys.
PD SEP
PY 2011
VL 7
IS 9
BP 687
EP 692
DI 10.1038/NPHYS1999
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 814VN
UT WOS:000294485400013
ER
PT J
AU Cernusak, LA
Winter, K
Martinez, C
Correa, E
Aranda, J
Garcia, M
Jaramillo, C
Turner, BL
AF Cernusak, Lucas A.
Winter, Klaus
Martinez, Carlos
Correa, Edwin
Aranda, Jorge
Garcia, Milton
Jaramillo, Carlos
Turner, Benjamin L.
TI Responses of Legume Versus Nonlegume Tropical Tree Seedlings to Elevated
CO2 Concentration
SO PLANT PHYSIOLOGY
LA English
DT Article
ID WATER-USE EFFICIENCY; CARBON-DIOXIDE CONCENTRATION; WHOLE-PLANT WATER;
ATMOSPHERIC CO2; TRANSPIRATION EFFICIENCY; STOMATAL CONDUCTANCE; N-2
FIXATION; RAIN-FOREST; RISING CO2; ISOTOPE COMPOSITION
AB We investigated responses of growth, leaf gas exchange, carbon-isotope discrimination, and whole-plant water-use efficiency (W-P) to elevated CO2 concentration ([CO2]) in seedlings of five leguminous and five nonleguminous tropical tree species. Plants were grown at CO2 partial pressures of 40 and 70 Pa. As a group, legumes did not differ from nonlegumes in growth response to elevated [CO2]. The mean ratio of final plant dry mass at elevated to ambient [CO2] (M-E/M-A) was 1.32 and 1.24 for legumes and nonlegumes, respectively. However, there was large variation in M-E/M-A among legume species (0.92-2.35), whereas nonlegumes varied much less (1.21-1.29). Variation among legume species in M-E/M-A was closely correlated with their capacity for nodule formation, as expressed by nodule mass ratio, the dry mass of nodules for a given plant dry mass. W-P increased markedly in response to elevated [CO2] in all species. The ratio of intercellular to ambient CO2 partial pressures during photosynthesis remained approximately constant at ambient and elevated [CO2], as did carbon isotope discrimination, suggesting that W-P should increase proportionally for a given increase in atmospheric [CO2]. These results suggest that tree legumes with a strong capacity for nodule formation could have a competitive advantage in tropical forests as atmospheric [CO2] rises and that the water-use efficiency of tropical tree species will increase under elevated [CO2].
C1 [Cernusak, Lucas A.] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia.
[Winter, Klaus; Martinez, Carlos; Correa, Edwin; Aranda, Jorge; Garcia, Milton; Jaramillo, Carlos; Turner, Benjamin L.] Smithsonian Trop Res Inst Balboa, Ancon, Panama.
RP Cernusak, LA (reprint author), Australian Natl Univ, Res Sch Biol, GPO Box 4, Canberra, ACT 0200, Australia.
EM lucas.cernusak@anu.edu.au
RI Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011
OI Turner, Benjamin/0000-0002-6585-0722; Cernusak,
Lucas/0000-0002-7575-5526
FU Smithsonian Tropical Research Institute; Australian Research Council
[DP0771427, FT100100329]
FX This work was supported by a Tupper postdoctoral fellowship from the
Smithsonian Tropical Research Institute, by a postdoctoral fellowship
and Discovery Grant from the Australian Research Council (grant no.
DP0771427), and by a Future Fellowship from the Australian Research
Council (grant no. FT100100329), all to L.A.C.
NR 70
TC 19
Z9 20
U1 0
U2 25
PU AMER SOC PLANT BIOLOGISTS
PI ROCKVILLE
PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA
SN 0032-0889
EI 1532-2548
J9 PLANT PHYSIOL
JI Plant Physiol.
PD SEP
PY 2011
VL 157
IS 1
BP 372
EP 385
DI 10.1104/pp.111.182436
PG 14
WC Plant Sciences
SC Plant Sciences
GA 814XZ
UT WOS:000294491800029
PM 21788363
ER
PT J
AU Ortner, DJ
AF Ortner, Donald J.
TI What skeletons tell us. The story of human paleopathology
SO VIRCHOWS ARCHIV
LA English
DT Review
DE Paleopathology; Skeletal disease; Ancient health
ID IDENTIFICATION
AB Human skeletal paleopathology provides important insight regarding the antiquity of some diseases and their distribution in past human groups. The history of human skeletal paleopathology extends back more than 150 years. Rudolf Virchow published reports on the subject, and research on paleopathology has provided critical data on important topics such as the origin of syphilis. With the development of powerful new research tools, human paleopathology will continue to be a source of data on the development of disease and its effect on human biological and cultural development.
C1 [Ortner, Donald J.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Ortner, Donald J.] Univ Bradford, Dept Archaeol Sci, Bradford BD7 1DP, W Yorkshire, England.
RP Ortner, DJ (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM ortner@si.edu
NR 33
TC 10
Z9 10
U1 2
U2 33
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0945-6317
J9 VIRCHOWS ARCH
JI Virchows Arch.
PD SEP
PY 2011
VL 459
IS 3
BP 247
EP 254
DI 10.1007/s00428-011-1122-x
PG 8
WC Pathology
SC Pathology
GA 813GZ
UT WOS:000294356100001
PM 21779895
ER
PT J
AU Terrell, KA
Wildt, DE
Anthony, NM
Bavister, BD
Leibo, SP
Penfold, LM
Marker, LL
Crosier, AE
AF Terrell, Kimberly A.
Wildt, David E.
Anthony, Nicola M.
Bavister, Barry D.
Leibo, S. P.
Penfold, Linda M.
Marker, Laurie L.
Crosier, Adrienne E.
TI Oxidative Phosphorylation Is Essential for Felid Sperm Function, but Is
Substantially Lower in Cheetah (Acinonyx jubatus) Compared to Domestic
Cat (Felis catus) Ejaculate
SO BIOLOGY OF REPRODUCTION
LA English
DT Article
DE cat; gamete biology; lipid; mitochondria; myxothiazol; spermatozoa;
sperm metabolism; sperm motility and transport; teratospermia;
teratozoospermia
ID IN-VITRO FERTILIZATION; CYTOPLASMIC DROPLETS; HUMAN-SPERMATOZOA;
ARTIFICIAL CRYPTORCHIDISM; MITOCHONDRIAL ACTIVITY; SEMINAL QUALITY; BOAR
SEMEN; SWIM-UP; MOTILITY; TRAITS
AB Compared with the normospermic domestic cat, sperm metabolic function is compromised in the teratospermic cat and cheetah, but the pathway(s) involved in this deficiency are unknown. Glycolysis is essential for sperm motility, yet it appears to function normally in spermatozoa of either species regardless of structural morphology. We conducted a comparative study to further understand the mechanisms of energy production in felid spermatozoa, with the hypothesis that oxidative phosphorylation is required for normal sperm function and is impaired in teratospermic ejaculates. Electroejaculates from both species were stained with MitoTracker to quantify mitochondrial membrane potential (MMP) or were incubated to assess changes in sperm function (motility, acrosomal integrity, and lactate production) after mitochondrial inhibition with myxothiazol. Sperm midpiece dimensions also were quantified. Sperm mitochondrial fluorescence (directly proportional to MMP) was similar to 95% lower in the cheetah compared with the normospermic and teratospermic cat, despite the cheetah having a 10% longer midpiece. In both species, MMP was increased 5-fold in spermatozoa with retained cytoplasm compared with structurally normal cells. Inhibition of oxidative phosphorylation impaired sperm function in both species, but a 100-fold higher inhibitor concentration was required in the cat compared with the cheetah. Collectively, findings revealed that oxidative phosphorylation was required for sperm function in the domestic cat and cheetah. This pathway of energy production appeared markedly less active in the cheetah, indicating a species-specific vulnerability to mitochondrial dysfunction. The unexpected, cross-species linkage between retained cytoplasmic droplets and elevated MMP may reflect increased concentrations of metabolic enzymes or substrates in these structures.
C1 [Terrell, Kimberly A.; Wildt, David E.; Crosier, Adrienne E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Terrell, Kimberly A.; Anthony, Nicola M.; Leibo, S. P.] Univ New Orleans, Dept Biol Sci, New Orleans, LA 70148 USA.
[Bavister, Barry D.] Univ Puerto Rico, San Juan, PR 00936 USA.
[Leibo, S. P.] Audubon Ctr Res Endangered Species, New Orleans, LA USA.
[Penfold, Linda M.] White Oak Conservat Ctr, Yulee, FL USA.
[Marker, Laurie L.] Cheetah Conservat Fund, Otjiwarongo, Namibia.
RP Crosier, AE (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM crosiera@si.edu
FU National Science Foundation; Ohrstrom Family Foundation; William H.
Donner Foundation Inc.; CCF-USA; Smithsonian Predoctoral Research
Fellowship Program
FX Supported by the National Science Foundation Graduate Research
Fellowship Program, the Ohrstrom Family Foundation, the William H.
Donner Foundation Inc., CCF-USA, and the Smithsonian Predoctoral
Research Fellowship Program.
NR 85
TC 4
Z9 4
U1 2
U2 28
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1603 MONROE ST, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD SEP
PY 2011
VL 85
IS 3
BP 473
EP 481
DI 10.1095/biolreprod.111.092106
PG 9
WC Reproductive Biology
SC Reproductive Biology
GA 810FH
UT WOS:000294110400007
PM 21593479
ER
PT J
AU Rawlinson, KA
Gillis, JA
Billings, RE
Borneman, EH
AF Rawlinson, K. A.
Gillis, J. A.
Billings, R. E., Jr.
Borneman, E. H.
TI Taxonomy and life history of the Acropora-eating flatworm Amakusaplana
acroporae nov sp (Polycladida: Prosthiostomidae)
SO CORAL REEFS
LA English
DT Article
DE Coral predator; Acropora-eating flatworm; Polyclad; Amakusaplana
acroporae; Intracapsular larva; 28S rDNA phylogeny
ID MARITIGRELLA-CROZIERI; COTYLEA; PLATYHELMINTHES; TURBELLARIA;
MORPHOLOGY; PREDATOR; BIOLOGY; MODELS; WATERS
AB Efforts to culture and conserve acroporid corals in aquaria have led to the discovery of a corallivorous polyclad flatworm (known as AEFW - Acropora-eating flatworm), which, if not removed, can eat entire colonies. Live observations of the AEFW, whole mounts, serial histological sections and comparison of 28S rDNA sequences with other polyclads reveal that this is a new species belonging to the family Prosthiostomidae Lang, 1884 and previously monospecific genus Amakusaplana (Kato 1938). Amakusaplana acroporae is distinguished from Amakusaplana ohshimai by a different arrangement and number of eyes, a large seminal vesicle and dorsoventrally compressed shell gland pouch. Typical of the genus, A. acroporae, lacks a ventral sucker and has a small notch at the midline of the anterior margin. Nematocysts and a Symbiodinium sp. of dinoflagellate from the coral are abundantly distributed in the gut and parenchyma. Individual adults lay multiple egg batches on the coral skeleton, each egg batch has 20-26 egg capsules, and each capsule contains between 3-7 embryos. Embryonic development takes approximately 21 days, during which time characteristics of a pelagic life stage (lobes and ciliary tufts) develop but are lost before hatching. The hatchling is capable of swimming but settles to the benthos quickly, and no zooxanthellae were observed in the animal at this stage. We suggest that intracapsular metamorphosis limits the dispersal potential of hatchlings and promotes recruitment of offspring into the natal habitat. The evolutionary and ecological significance of retaining lobes and ciliary tufts in the embryo are discussed. Camouflage, high fecundity and possible dispersal dimorphisms probably explain how Amakusaplana acroporae can cause Acropora sp. mortality in aquaria where natural predators may be absent.
C1 [Rawlinson, K. A.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
[Gillis, J. A.] Univ Cambridge, Dept Physiol Dev & Neurosci, Cambridge CB2 3DY, England.
[Borneman, E. H.] Univ Houston, Dept Biol, Houston, TX 77204 USA.
RP Rawlinson, KA (reprint author), UCL, Dept Genet Evolut & Environm, Gower St, London WC1E 6BT, England.
EM k.rawlinson@ucl.ac.uk
FU Smithsonian Marine Science Network; Smithsonian Link Foundation
FX We thank Greg Rouse, Fernando Nosratpour, Bruce Wilfong, Alan Flojo and
Randy Donowitz for providing additional AEFW specimens. We thank
Bernhard Egger and Peter Ladurner for providing samples of
Prosthiostomum siphunculus and Macrostomum lignano, respectively. We
thank John Chuk for help with collection and identification of
Australian polyclad species, Nicolette Craig of Practical Fish Keeping
magazine and Mary Hagerdorn for helpful discussion. This work was funded
by a Smithsonian Marine Science Network fellowship to KAR and a
Smithsonian Link Foundation Fellowship to JAG. Smithsonian Marine
Station contribution number 842.
NR 41
TC 14
Z9 14
U1 0
U2 18
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0722-4028
J9 CORAL REEFS
JI Coral Reefs
PD SEP
PY 2011
VL 30
IS 3
BP 693
EP 705
DI 10.1007/s00338-011-0745-3
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 802UN
UT WOS:000293536600018
ER
PT J
AU Wilson, S
LaDeau, SL
Tottrup, AP
Marra, PP
AF Wilson, Scott
LaDeau, Shannon L.
Tottrup, Anders P.
Marra, Peter P.
TI Range-wide effects of breeding- and nonbreeding-season climate on the
abundance of a Neotropical migrant songbird
SO ECOLOGY
LA English
DT Article
DE American Redstart; Breeding Bird Survey; climate; hierarchical models;
migratory connectivity; Neotropical migrant; population dynamics;
Setophaga ruticilla
ID DISTANCE MIGRATORY BIRD; NORTH-AMERICAN; POPULATION-DYNAMICS;
MELOSPIZA-MELODIA; HABITAT QUALITY; RAINFALL; WARBLERS; SUCCESS; NDVI;
FOOD
AB Geographic variation in the population dynamics of a species can result from regional variability in climate and how it affects reproduction and survival. Identifying such effects for migratory birds requires the integration of population models with knowledge of migratory connectivity between breeding and nonbreeding areas. We used Bayesian hierarchical models with 26 years of Breeding Bird Survey data (1982-2007) to investigate the impacts of breeding-and nonbreeding-season climate on abundance of American Redstarts (Setophaga ruticilla) across the species range. We focused on 15 populations defined by Bird Conservation Regions, and we included variation across routes and observers as well as temporal trends and climate effects. American Redstart populations that breed in eastern North America showed increased abundance following winters with higher plant productivity in the Caribbean where they are expected to overwinter. In contrast, western breeding populations showed little response to conditions in their expected wintering areas in west Mexico, perhaps reflecting lower migratory connectivity or differential effects of winter rainfall on individuals across the species range. Unlike the case with winter climate, we found few effects of temperature prior to arrival in spring (March-April) or during the nesting period (May-June) on abundance the following year. Eight populations showed significant changes in abundance, with the steepest declines in the Atlantic Northern Forest (-3.4%/ yr) and the greatest increases in the Prairie Hardwood Transition (4%/yr). This study emphasizes how the effects of climate on populations of migratory birds are context dependent and can vary depending on geographic location and the period of the annual cycle. Such knowledge is essential for predicting regional variation in how populations of a species might vary in their response to climate change.
C1 [Wilson, Scott; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA.
[LaDeau, Shannon L.] Cary Inst Ecosyst Studies, Millbrook, NY 12545 USA.
[Tottrup, Anders P.] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen, Denmark.
RP Wilson, S (reprint author), Environm Canada, Canadian Wildlife Serv, 115 Perimeter Rd, Saskatoon, SK S7N 0X4, Canada.
EM scottd.wilson@ec.gc.ca
RI Tottrup, Anders/N-3836-2013; publist, CMEC/C-3010-2012; publicationpage,
cmec/B-4405-2017;
OI Tottrup, Anders/0000-0001-8776-9629; LaDeau, Shannon/0000-0003-4825-5435
FU Smithsonian Institution Office of Fellowships; Natural Sciences and
Engineering Research Council of Canada; National Science Foundation
[0717243]; Danish National Research Foundation
FX We very much appreciate the work of C. Robbins and the U.S. Geological
Survey for creating and maintaining the Breeding Bird Survey. We are
grateful for financial support in the form of fellowships from the
Smithsonian Institution Office of Fellowships and the Natural Sciences
and Engineering Research Council of Canada to S. Wilson, National
Science Foundation grant number 0717243 to P. P. Marra, and funding from
the Danish National Research Foundation to A. P. Tottrup in the Center
for Macroecology, Evolution and Climate. This article greatly benefited
from comments from two anonymous reviewers.
NR 52
TC 41
Z9 41
U1 5
U2 83
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0012-9658
EI 1939-9170
J9 ECOLOGY
JI Ecology
PD SEP
PY 2011
VL 92
IS 9
BP 1789
EP 1798
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 810UK
UT WOS:000294152800010
PM 21939075
ER
PT J
AU Stine, JK
AF Stine, Jeffrey K.
TI Ditch of Dreams: The Cross Florida Barge Canal and the Struggle for
Florida's Future
SO ENTERPRISE & SOCIETY
LA English
DT Book Review
C1 [Stine, Jeffrey K.] Smithsonian Inst, Washington, DC 20560 USA.
RP Stine, JK (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1467-2227
J9 ENTERP SOC
JI Enterp. Soc
PD SEP
PY 2011
VL 12
IS 3
BP 628
EP U154
DI 10.1093/es/khq150
PG 3
WC Business; History Of Social Sciences
SC Business & Economics; Social Sciences - Other Topics
GA 809QZ
UT WOS:000294073100005
ER
PT J
AU Kersey, DC
Wildt, DE
Brown, JL
Snyder, RJ
Huang, Y
Monfort, SL
AF Kersey, David C.
Wildt, David E.
Brown, Janine L.
Snyder, Rebecca J.
Huang, Yan
Monfort, Steven L.
TI Rising fecal glucocorticoid concentrations track reproductive activity
in the female giant panda (Ailuropoda melanoleuca)
SO GENERAL AND COMPARATIVE ENDOCRINOLOGY
LA English
DT Article
DE Giant panda; Fecal glucocorticoids; Adrenal physiology; Seasonality;
Reproductive acyclicity
ID PITUITARY-ADRENAL AXIS; SEASONAL-CHANGES; CORTISOL-LEVELS; STRESS;
PREGNANCY; HORMONES; BEHAVIOR; ESTRUS; ENDOCRINOLOGY; CONSERVATION
AB To better understand the adaptive significance of adrenal glucocorticoid (GC) variation in the giant panda, we assessed patterns of fecal GC excretion over time as well as during estrus, parturient and non-parturient luteal phases, lactation and acyclicity in 17 adult females. Fecal estrogen and GC patterns were positively correlated (P < 0.05) in four of five periestrual females (r = 0.57-0.92). Among all reproductive states, fecal GC was highest (P < 0.05) during periestrus (non-parturient, 495.9 +/- 100.7 ng/g [mean +/- SE]; parturient, 654.1 +/- 106.5 ng/g: P > 0.05). Concentrations of GC metabolites were lower (P < 0.05) during the later stage of the luteal phase in non-parturient (334.8 +/- 24.8 ng/g) compared to parturient (470.4 +/- 54.0 ng/g) females. Although fecal GC concentrations in cyclic, non-parturient females did not differ (P > 0.05) across all seasons, there were seasonal variations (P < 0.05) in females that were acyclic and non-lactational. However, the overall lack of difference (P > 0.05) in GC values between reproductively cyclic and acyclic females did not support the hypothesis that ovarian acyclicity is due to increased adrenal activity (related or unrelated to physiological stress). Furthermore, GCs may play an important role in the normal endocrine milieu associated with sexual receptivity and late pregnancy. These data demonstrate that both reproductive status and seasonal factors are important modulators of adrenal function in this endangered species. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Kersey, David C.; Wildt, David E.; Brown, Janine L.; Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Snyder, Rebecca J.] Zoo Atlanta, Atlanta, GA 30315 USA.
[Huang, Yan] China Conservat & Res Ctr Giant Panda, Wolong Nat Reserve, Wenchuan 623006, Sichuan Prov, Peoples R China.
RP Kersey, DC (reprint author), Western Univ Hlth Sci, Coll Vet Med, Pomona, CA USA.
EM dkersey@westernu.edu
FU Friends of the National Zoo
FX The authors thank Nicole Parker, Copper Aitken-Palmer. Adrienne Crosier,
Nicole Presley, Karen Steinman, Rosemary Stewart and Susan Walker for
providing logistical support. We are especially indebted for the
dedicated laboratory assistance of Corinna Bazlett, Jessica Beckman,
Serena Enloe, Luo Li, Valerie Parkman, Nicole Savageau and Bridgette von
Holdt. Keeper and curatorial staffs at the Smithsonian National
Zoological Park, Zoo Atlanta and the China Conservation and Research
Center for the Giant Panda were invaluable in their dedication to the
frequent and accurate collection of samples. This study was supported by
Friends of the National Zoo.
NR 59
TC 4
Z9 5
U1 1
U2 22
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 SEP 1
PY 2011
VL 173
IS 2
BP 364
EP 370
DI 10.1016/j.ygcen.2011.06.013
PG 7
WC Endocrinology & Metabolism
SC Endocrinology & Metabolism
GA 810DR
UT WOS:000294106100015
PM 21726558
ER
PT J
AU Makana, JR
Ewango, CN
McMahon, SM
Thomas, SC
Hart, TB
Condit, R
AF Makana, Jean-Remy
Ewango, Corneille N.
McMahon, Sean M.
Thomas, Sean C.
Hart, Terese B.
Condit, Richard
TI Demography and biomass change in monodominant and mixed old-growth
forest of the Congo
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE Africa; Congo; mortality; biomass; population dynamics; tree growth;
tropical rain forest
ID TROPICAL FORESTS; LATE QUATERNARY; RAIN-FOREST; TREE; AFRICAN; TURNOVER;
DYNAMICS; IMPACT; AMAZON; PLOTS
AB Mbau forest covers much of the Congo, and shifts in its composition could have a large impact on the African tropics. The Ituri forest in east Congo is near a boundary between the monodominant mbau type and non-mbau mixed forest, and two 20-ha censuses of trees >= 1 cm diameter were carried out over 12 y to monitor forest change. Based on published diameter allometry, mbau forest had 535 Mg ha(-1) biomass above ground and gained 1.1 Mg ha(-1) y(-1). Mixed forest had 399 Mg ha(-1) and gained 3 Mg ha(-1) y(-1). The mbau tree (Gilbertiodendron dewevrei) increased its share of biomass from 4.1% to 4.4% in mixed forest; other common species also increased. Sapling density declined at both sites, likely because increased biomass meant shadier understorey, but the mbau tree increased in sapling density, suggesting it will become more important in the future. Tree mortality and growth rates were low relative to other tropical forests, especially in the mbau plots. Shifting toward G. dewevrei would represent a large gain in carbon in the mixed forest, but mbau is presently more important as a high-carbon stock: biomass lost during forest harvest could not recuperate for centuries due to slow community dynamics.
C1 [Makana, Jean-Remy] Wildlife Conservat Soc, DRC Program, Kinshasa, Zaire.
[Ewango, Corneille N.] Wildlife Conservat Soc, Ctr Format & Rech Conservat Forestiere CEFRECOF, Kinshasa, Zaire.
[McMahon, Sean M.] Smithsonian Trop Res Inst, Edgewater, MD USA.
[McMahon, Sean M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Thomas, Sean C.] Univ Toronto, Fac Forestry, Toronto, ON, Canada.
[Hart, Terese B.] Project TL2, Kinshasa, Zaire.
[Condit, Richard] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Dpo, AA 34002 USA.
RP Makana, JR (reprint author), Wildlife Conservat Soc, DRC Program, Kinshasa, Zaire.
EM conditr@gmail.com
FU Wildlife Conservation Society; Peninsula Foundation; Smithsonian
Scholarly Studies Program; National Science Foundation [DEB-0090311,
DEB-9806828]
FX Civil war reached the Okapi Reserve several times between censuses, and
our thanks need to be amplified in this light: one of us - C. N. E. -
was captured by rebels while at the research site. He was later awarded
the Goldman Environmental Prize for his efforts to maintain botanical
research during war. Many other individuals and organizations maintained
support despite the difficulties imposed: the Wildlife Conservation
Society through its conservation project in the Okapi Faunal Reserve; J.
Madidi, P. Umunay, F. Bujo, and J. Mukinzi through their field work;
M.N. Ndiu and P. Umunay by maintaining the database. The Institut
Congolais pour la Conservation de la Nature graciously provided the
research permit, while S. Davies, E. Bermingham, and I. Rubinoff
provided direction and financial support for the international plot
network via the Smithsonian Tropical Research Institute and the Arnold
Arboretum at Harvard University. The Ituri plots were supported by
funding from the Wildlife Conservation Society, the Peninsula
Foundation, and the Smithsonian Scholarly Studies Program. Analyses
reported here were developed during workshops sponsored by the National
Science Foundation (grants DEB-0090311 and DEB-9806828) and the
Peninsula Foundation.
NR 41
TC 13
Z9 13
U1 3
U2 28
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 SEP
PY 2011
VL 27
BP 447
EP 461
DI 10.1017/S0266467411000265
PN 5
PG 15
WC Ecology
SC Environmental Sciences & Ecology
GA 811LP
UT WOS:000294212300001
ER
PT J
AU Turmel, MS
Turner, BL
Whalen, JK
AF Turmel, Marie-Soleil
Turner, Benjamin L.
Whalen, Joann K.
TI Soil fertility and the yield response to the System of Rice
Intensification
SO RENEWABLE AGRICULTURE AND FOOD SYSTEMS
LA English
DT Article
DE System of Rice Intensification; highly weathered soils; marginal soils;
low-input rice production
ID SRI; PHOSPHORUS; MANAGEMENT
AB The System of Rice Intensification (SRI) is a low-input rice (Oryza sativa L.) production system that differs from conventional systems in several ways: seedlings are transplanted earlier and are more widely spaced, organic fertilizer is often used in addition to mineral fertilizer, and soils are irrigated intermittently rather than flooded for long periods. The yield benefits of SRI compared to conventional systems can be substantial, and yet are regionally variable and have been the subject of considerable debate, due partly to a lack of mechanistic understanding. Here we show that soil properties may in part explain the variability in yield response to SRI. A meta-analysis of data from 72 field studies where SRI was compared with conventional systems indicates that yields increased significantly (P < 0.0001) when SRI was implemented on highly weathered infertile soils rich in iron and aluminum oxides (Acrisols and Ferralsols), but there was no difference in yield between SRI and conventional systems in more fertile favorable soils for rice production (Gleysols, Luvisols and Fluvisols). The yield difference between SRI and conventional rice production therefore appears to be related in part to soil properties linked to weathering. This should help resolve the debate about the value of SRI and allow research to be targeted toward understanding the biological and chemical processes in soils under SRI management.
C1 [Turmel, Marie-Soleil; Whalen, Joann K.] McGill Univ, Dept Nat Resource Sci, Ste Anne De Bellevue, PQ H9X 3V9, Canada.
[Turmel, Marie-Soleil; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Whalen, JK (reprint author), McGill Univ, Dept Nat Resource Sci, Macdonald Campus,21 111 Lakeshore Rd, Ste Anne De Bellevue, PQ H9X 3V9, Canada.
EM joann.whalen@mcgill.ca
RI Turner, Benjamin/E-5940-2011
OI Turner, Benjamin/0000-0002-6585-0722
FU Natural Sciences and Engineering Research Council of Canada
FX We thank individuals who provided data for the meta-analysis, Rosa
Orlandini and Joanna Hobbins (Walter Hitschfeld Geographic Information
Centre) for their help with GIS, Rick Condit (STRI) for statistical
advice, and anonymous reviewers for comments on the manuscript.
Financial support for this work was from the Natural Sciences and
Engineering Research Council of Canada.
NR 48
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U2 15
PU CAMBRIDGE UNIV PRESS
PI CAMBRIDGE
PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND
SN 1742-1705
J9 RENEW AGR FOOD SYST
JI Renew. Agr. Food Syst.
PD SEP
PY 2011
VL 26
IS 3
BP 185
EP 192
DI 10.1017/S174217051100007X
PG 8
WC Agriculture, Multidisciplinary
SC Agriculture
GA 810JF
UT WOS:000294120900002
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI Sound Scholarship
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
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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 SEP
PY 2011
VL 42
IS 5
BP 34
EP 34
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 811FW
UT WOS:000294192300010
ER
PT J
AU Leurini, S
Pillai, T
Stanke, T
Wyrowski, F
Testi, L
Schuller, F
Menten, KM
Thorwirth, S
AF Leurini, S.
Pillai, T.
Stanke, T.
Wyrowski, F.
Testi, L.
Schuller, F.
Menten, K. M.
Thorwirth, S.
TI The molecular distribution of the IRDC G351.77-0.51
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: clouds; stars: formation; stars: protostars; ISM: individual
objects: G351.77-0.51
ID INFRARED-DARK CLOUDS; MASSIVE-STAR-FORMATION; HERBIG AE/BE STARS; H-II
REGIONS; HII-REGIONS; PROTOSTELLAR CORES; INITIAL CONDITIONS; LINE
OBSERVATIONS; FORMING REGIONS; IRAS 17233-3606
AB Context. Infrared dark clouds are massive, dense clouds seen in extinction against the IR Galactic background. Many of these objects appear to be on the verge of star and star cluster formation.
Aims. Our aim is to understand the physical properties of IRDCs in very early evolutionary phases. We selected the filamentary IRDC G351.77-0.51, which is remarkably IR quiet at 8 mu m.
Methods. As a first step, we observed mm dust continuum emission and rotational lines of moderate and dense gas tracers to characterise different condensations along the IRDC and study the velocity field of the filament.
Results. Our initial study confirms coherent velocity distribution along the infrared dark cloud ruling out any coincidental projection effects. Excellent correlation between MIR extinction, mm continumm emission and gas distribution is found. Large-scale turbulence and line profiles throughout the filament is indicative of a shock in this cloud. Excellent correlation between line width and MIR brightness indicates turbulence driven by local star formation.
C1 [Leurini, S.; Wyrowski, F.; Schuller, F.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Pillai, T.] CALTECH, Pasadena, CA 91125 USA.
[Pillai, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stanke, T.; Testi, L.] ESO, D-85748 Garching, Germany.
[Testi, L.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
[Thorwirth, S.] Univ Cologne, Physikal Inst 1, D-50937 Cologne, Germany.
RP Leurini, S (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM sleurini@mpifr.de
RI Thorwirth, Sven/C-6217-2011
OI Thorwirth, Sven/0000-0001-8200-6710
FU Deutsche Forschungsgemeinschaft [TH1301/3-1]; Combined Array for
Research in Millimeter-wave Astronomy (CARMA); National Science
Foundation [AST 05-40399]
FX The authors would like to thank J. Kauffmann for fruitful discussions.
S.T. is grateful to the Deutsche Forschungsgemeinschaft for a research
grant (TH1301/3-1). T.P. acknowledges support from the Combined Array
for Research in Millimeter-wave Astronomy (CARMA), which is supported by
the National Science Foundation through grant AST 05-40399.
NR 82
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD SEP
PY 2011
VL 533
DI 10.1051/0004-6361/201016380
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 823ZN
UT WOS:000295168100085
ER
PT J
AU Neufeld, MJ
AF Neufeld, Michael J.
TI Dark Side of the Moon: Wernher von Braun, the Third Reich, and the Space
Race
SO JOURNAL OF COLD WAR STUDIES
LA English
DT Book Review
C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 5
PU MIT PRESS
PI CAMBRIDGE
PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA
SN 1520-3972
J9 J COLD WAR STUD
JI J. Cold War Stud.
PD FAL
PY 2011
VL 13
IS 4
BP 223
EP 224
PG 2
WC History; International Relations; Political Science
SC History; International Relations; Government & Law
GA 011YV
UT WOS:000309203100013
ER
PT J
AU Sturm, G
AF Sturm, Gary
TI THE CONSERVATION, RESTORATION, AND REPAIR OF STRINGED INSTRUMENTS AND
THEIR BOWS
SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION
LA English
DT Book Review
C1 [Sturm, Gary] Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
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 FAL-WIN
PY 2011
VL 50
IS 2
BP 166
EP 167
PG 2
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA V29YM
UT WOS:000208783700008
ER
PT J
AU Koljonen, KII
Hannikainen, DC
McCollough, ML
AF Koljonen, K. I. I.
Hannikainen, D. C.
McCollough, M. L.
TI The re-occurrence of mHz quasi-periodic oscillations in Cygnus X-3
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; binaries: close; stars: oscillations;
X-rays: binaries; X-rays: individual: Cygnus X-3; X-rays: stars
AB We have re-analysed archival RXTE data of the X-ray binary Cygnus X-3 with a view to investigate the timing properties of the source. As compared to previous studies, we use an extensive sample of observations that include all the radio/X-ray spectral states that have been categorized in the source recently. In this study we identify two additional instances of quasi-periodic oscillations that have centroid frequencies in the mHz regime. These events are all associated to a certain extent with major radio flaring, which in turn is associated with relativistic jet ejection events. We review briefly scenarios whereby the quasi-periodic oscillations may arise.
C1 [Koljonen, K. I. I.; Hannikainen, D. C.] Aalto Univ, Metsahovi Radio Observ, FI-02540 Kylmala, Finland.
[Hannikainen, D. C.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland.
[Hannikainen, D. C.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
[McCollough, M. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Koljonen, KII (reprint author), Aalto Univ, Metsahovi Radio Observ, Metsahovintie 114, FI-02540 Kylmala, Finland.
EM karri@kurp.hut.fi; diana@kurp.hut.fi; mccolml@head.cfa.harvard.edu
OI Koljonen, Karri/0000-0002-9677-1533
FU NASA [NNG06GE72G, NNX06AB94G, NAS8-03060]; NASA High Energy Astrophysics
program
FX The authors thank the referee for the careful reading of the manuscript
and excellent suggestions that significantly improved the Letter. KIIK
acknowledges the Finnish Graduate School in Astronomy and Space Physics.
The authors gratefully thank the Vilho, Yrjo and Kalle Vaisala
Foundation for a travel grant that stimulated this discussion. This
research has made use of data and/or software provided by the High
Energy Astrophysics Science Archive Research center (HEASARC), which is
a service of the Astrophysics Science Division at NASA/GSFC and the High
Energy Astrophysics Division of the Smithsonian Astrophysical
Observatory. MLM wished to acknowledge support from NASA under
grant/contract NNG06GE72G, NNX06AB94G and NAS8-03060. The Green Bank
Interferometer is a facility of the National Science Foundation operated
by NRAO with support from the NASA High Energy Astrophysics program.
NR 31
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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 SEP
PY 2011
VL 416
IS 1
BP L84
EP L88
DI 10.1111/j.1745-3933.2011.01104.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA V29AV
UT WOS:000208722200018
ER
PT J
AU Foerster, S
Cords, M
Monfort, SL
AF Foerster, Steffen
Cords, Marina
Monfort, Steven L.
TI Social Behavior, Foraging Strategies, and Fecal Glucocorticoids in
Female Blue Monkeys (Cercopithecus mitis): Potential Fitness Benefits of
High Rank in a Forest Guenon
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Article
DE feeding competition; glucocorticoids; energetic stress; social status;
foraging behavior
ID POST-CONFLICT BEHAVIOR; LONG-TAILED MACAQUES; LEMURS LEMUR-CATTA; WILD
OLIVE BABOONS; CORTISOL-LEVELS; MACACA-FASCICULARIS; DOMINANCE RANK;
PATAS MONKEYS; FEEDING COMPETITION; CYNOMOLGUS MONKEYS
AB Socioecological theory predicts that aggressive feeding competition is associated with linear dominance hierarchies and reproductive advantages for high-ranking females. Female blue monkeys contest fruits and have a linear dominance hierarchy, yet previous research has shown no evidence that high-ranking females benefit from greater feeding success or fertility. Here, we assess whether individuals differ in fecal glucocorticoid (fGC) excretion and examine proximate determinants of such differences to infer potential fitness correlates of rank, using data collected from two study groups in the Kakamega Forest, Kenya. We found that higher ranking females had preferential access to fruits in both groups, although the behavioral mechanisms leading to this effect varied between groups. Despite a consistent rank difference in feeding on fruits, an overall rank effect on fGCs emerged in only one group; females of this group spent comparatively more time feeding on fruits, fruits accounted for a greater proportion of the diet, and females engaged in more frequent food-related agonism. In addition, more females in this group were lactating during a period of low fruit availability, when rank effects on fGCs were particularly strong. Regardless of fruit availability, among lactating females of both groups higher rank was associated with lower fGC levels, indicating lower energetic stress in higher ranking females when energy demands were particularly high. Individual rates of agonism, a potential psychological stressor, were unrelated to fGCs at all times. After we accounted for rates of agonism and feeding on fruits, females of one group who groomed others more had lower fGCs, suggesting that variable social coping behavior can contribute to fGC variation in some groups. This study provides the first empirical evidence that high-ranking female blue monkeys may obtain fitness benefits from their social status, by gaining priority of access to fruits during critical times in the reproductive cycle. Am. J. Primatol. 73:870-882, 2011. (C) 2011 Wiley-Liss, Inc.
C1 [Foerster, Steffen; Cords, Marina] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Foerster, Steffen] Natl Museums Kenya, Inst Primate Res, Nairobi, Kenya.
[Monfort, Steven L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
RP Foerster, S (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 1200 Amsterdam Ave,10th Floor Schermerhorn Extens, New York, NY 10027 USA.
EM sf2041@columbia.edu
FU National Science Foundation [BCS 0550509, BCS 0554747]; Columbia
University; Earthwatch Institute; Animal Behavior Society; American
Society of Primatologists; Institute of Primate Research, Nairobi
FX Contract grant sponsor: National Science Foundation; Contract grant
numbers: BCS 0550509; BCS 0554747; Contract grant sponsors: Columbia
University; The Earthwatch Institute; The Animal Behavior Society;
American Society of Primatologists.; We are grateful to the Ministry of
Science, Education and Technology, Government of Kenya, for permission
to work in the Kakamega Forest, to the staff at the Kakamega Forest
Station for their cooperation, and to Dr. D. Yole and the Institute of
Primate Research, Nairobi, for local sponsorship. Thanks go to W.
Adhuka, E. Mbone, C. Oduor, M. Ogutu, D. Shilabiga, and C. Zacharias for
help during various stages of data collection. We are grateful to N.
Presley for guidance and support with sample processing in the lab, and
to N. Heywood and S. Hodgkiss for assistance with hormone extractions.
NR 88
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U2 56
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD SEP
PY 2011
VL 73
IS 9
BP 870
EP 882
DI 10.1002/ajp.20955
PG 13
WC Zoology
SC Zoology
GA 805XL
UT WOS:000293764300004
PM 21495049
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Boltuch, D
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Cui, W
Dickherber, R
Duke, C
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Hui, CM
Humensky, TB
Imran, A
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Konopelko, A
Krawczynski, H
Krennrich, F
Lang, MJ
Maier, G
McArthur, S
McCutcheon, M
Moriarty, P
Ong, RA
Otte, AN
Ouellette, M
Pandel, D
Perkins, JS
Pichel, A
Pohl, M
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Rovero, AC
Schroedter, M
Sembroski, GH
Senturk, GD
Steele, D
Swordy, SP
Theiling, M
Thibadeau, S
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
Garson, A
Lee, K
Sadun, AC
Carini, M
Barnaby, D
Cook, K
Maune, J
Pease, A
Smith, S
Walters, R
Berdyugin, A
Lindfors, E
Nilsson, K
Pasanen, M
Sainio, J
Sillanpaa, A
Takalo, LO
Villforth, C
Montaruli, T
Baker, M
Lahteenmaki, A
Tornikoski, M
Hovatta, T
Nieppola, E
Aller, HD
Aller, MF
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Boltuch, D.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Cui, W.
Dickherber, R.
Duke, C.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Hui, C. M.
Humensky, T. B.
Imran, A.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Konopelko, A.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
Maier, G.
McArthur, S.
McCutcheon, M.
Moriarty, P.
Ong, R. A.
Otte, A. N.
Ouellette, M.
Pandel, D.
Perkins, J. S.
Pichel, A.
Pohl, M.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Rovero, A. C.
Schroedter, M.
Sembroski, G. H.
Senturk, G. Demet
Steele, D.
Swordy, S. P.
Theiling, M.
Thibadeau, S.
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.
Garson, A., III
Lee, K.
Sadun, A. C.
Carini, M.
Barnaby, D.
Cook, K.
Maune, J.
Pease, A.
Smith, S.
Walters, R.
Berdyugin, A.
Lindfors, E.
Nilsson, K.
Pasanen, M.
Sainio, J.
Sillanpaa, A.
Takalo, L. O.
Villforth, C.
Montaruli, T.
Baker, M.
Lahteenmaki, A.
Tornikoski, M.
Hovatta, T.
Nieppola, E.
Aller, H. D.
Aller, M. F.
TI TeV AND MULTI-WAVELENGTH OBSERVATIONS OF Mrk 421 IN 2006-2008
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE BL Lacertae objects: individual (Mrk 421); galaxies: jets; galaxies:
nuclei; gamma rays: galaxies; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; BL-LACERTAE OBJECTS; RAY TIMING EXPLORER; ENERGY
GAMMA-RAYS; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; X-RAY;
PARTICLE-ACCELERATION; BLAZAR MARKARIAN-421; CORRELATED VARIABILITY
AB We report on TeV gamma-ray observations of the blazar Mrk 421 (redshift of 0.031) with the VERITAS observatory and the Whipple 10m Cherenkov telescope. The excellent sensitivity of VERITAS allowed us to sample the TeV gamma-ray fluxes and energy spectra with unprecedented accuracy where Mrk 421 was detected in each of the pointings. A total of 47.3 hr of VERITAS and 96 hr of Whipple 10m data were acquired between 2006 January and 2008 June. We present the results of a study of the TeV gamma-ray energy spectra as a function of time and for different flux levels. On 2008 May 2 and 3, bright TeV gamma-ray flares were detected with fluxes reaching the level of 10 Crab. The TeV gamma-ray data were complemented with radio, optical, and X-ray observations, with flux variability found in all bands except for the radio wave band. The combination of the Rossi X-ray Timing Explorer and Swift X-ray data reveal spectral hardening with increasing flux levels, often correlated with an increase of the source activity in TeV gamma-rays. Contemporaneous spectral energy distributions were generated for 18 nights, each of which are reasonably described by a one-zone synchrotron self-Compton model.
C1 [Acciari, V. A.; Beilicke, M.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA.
[Arlen, T.; 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.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.; Garson, A., III; Lee, K.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Byrum, K.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Univ Coll Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Fortson, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[Cui, W.; Finley, J. P.; 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.
[Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Guenette, R.; Hanna, D.; Maier, G.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Humensky, T. B.; Swordy, S. P.; 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.
[Gall, D.; 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.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Ouellette, M.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA.
[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.
[Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Sadun, A. C.] Univ Colorado, Dept Phys, Denver, CO 80217 USA.
[Carini, M.; Barnaby, D.; Cook, K.; Maune, J.; Pease, A.; Smith, S.; Walters, R.] Western Kentucky Univ, Dept Phys & Astron, Bowling Green, KY 42103 USA.
[Berdyugin, A.; Lindfors, E.; Nilsson, K.; Pasanen, M.; Sainio, J.; Sillanpaa, A.; Takalo, L. O.; Villforth, C.] Univ Turku, Tuorla Observ, Dept Phys & Astron, SF-20500 Turku, Finland.
[Montaruli, T.; Baker, M.] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA.
[Lahteenmaki, A.; Tornikoski, M.; Hovatta, T.; Nieppola, E.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina.
RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
EM beilicke@physics.wustl.edu
RI Lahteenmaki, Anne/L-5987-2013;
OI Cui, Wei/0000-0002-6324-5772; 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 in the
U.K; Academy of Finland; NSF; University of Michigan; NASA [NNX08AV77G,
NNX08AT31G, NNX08AZ76G]
FX VERITAS 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 the 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. The authors are grateful to the RXTE
Science Operations Facility and GOF. The Metsahovi team acknowledges the
support from the Academy of Finland. The UMRAO is funded by the NSF and
the University of Michigan. Swift/BAT transient monitor results provided
by the Swift/BAT team. We also acknowledge Swift/XRT monitoring program
and target of opportunity support provided by the Swift Team and
supported by NASA grants NNX08AV77G and NNX08AT31G. We gratefully
acknowledge useful discussions with Erik Hoversten regarding Swift/UVOT
analysis. H. K and A. G. acknowledge support from the NASA grant
NNX08AZ76G for the analysis of the Suzaku data.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 25
DI 10.1088/0004-637X/738/1/25
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500025
ER
PT J
AU Acciari, VA
Aliu, E
Arlen, T
Aune, T
Beilicke, M
Benbow, W
Bradbury, SM
Buckley, JH
Bugaev, V
Byrum, K
Cannon, A
Cesarini, A
Ciupik, L
Collins-Hughes, E
Connolly, MP
Cui, W
Dickherber, R
Duke, C
Errando, M
Falcone, A
Finley, JP
Finnegan, G
Fortson, L
Furniss, A
Galante, N
Gall, D
Gillanders, GH
Godambe, S
Griffin, S
Grube, J
Guenette, R
Gyuk, G
Hanna, D
Holder, J
Hughes, G
Hui, CM
Humensky, TB
Kaaret, P
Karlsson, N
Kertzman, M
Kieda, D
Krawczynski, H
Krennrich, F
Lang, MJ
LeBohec, S
Maier, G
Majumdar, P
McArthur, S
McCann, A
Moriarty, P
Mukherjee, R
Ong, RA
Orr, M
Otte, AN
Park, N
Perkins, JS
Pohl, M
Prokoph, H
Quinn, J
Ragan, K
Reyes, LC
Reynolds, PT
Roache, E
Rose, HJ
Ruppel, J
Saxon, DB
Schroedter, M
Sembroski, GH
Senturk, GD
Smith, AW
Staszak, D
Tesic, G
Theiling, M
Thibadeau, S
Tsurusaki, K
Varlotta, A
Vassiliev, VV
Vincent, S
Vivier, M
Wakely, SP
Ward, JE
Weekes, TC
Weinstein, A
Weisgarber, T
Williams, DA
Zitzer, B
AF Acciari, V. A.
Aliu, E.
Arlen, T.
Aune, T.
Beilicke, M.
Benbow, W.
Bradbury, S. M.
Buckley, J. H.
Bugaev, V.
Byrum, K.
Cannon, A.
Cesarini, A.
Ciupik, L.
Collins-Hughes, E.
Connolly, M. P.
Cui, W.
Dickherber, R.
Duke, C.
Errando, M.
Falcone, A.
Finley, J. P.
Finnegan, G.
Fortson, L.
Furniss, A.
Galante, N.
Gall, D.
Gillanders, G. H.
Godambe, S.
Griffin, S.
Grube, J.
Guenette, R.
Gyuk, G.
Hanna, D.
Holder, J.
Hughes, G.
Hui, C. M.
Humensky, T. B.
Kaaret, P.
Karlsson, N.
Kertzman, M.
Kieda, D.
Krawczynski, H.
Krennrich, F.
Lang, M. J.
LeBohec, S.
Maier, G.
Majumdar, P.
McArthur, S.
McCann, A.
Moriarty, P.
Mukherjee, R.
Ong, R. A.
Orr, M.
Otte, A. N.
Park, N.
Perkins, J. S.
Pohl, M.
Prokoph, H.
Quinn, J.
Ragan, K.
Reyes, L. C.
Reynolds, P. T.
Roache, E.
Rose, H. J.
Ruppel, J.
Saxon, D. B.
Schroedter, M.
Sembroski, G. H.
Senturk, G. D.
Smith, A. W.
Staszak, D.
Tesic, G.
Theiling, M.
Thibadeau, S.
Tsurusaki, K.
Varlotta, A.
Vassiliev, V. V.
Vincent, S.
Vivier, M.
Wakely, S. P.
Ward, J. E.
Weekes, T. C.
Weinstein, A.
Weisgarber, T.
Williams, D. A.
Zitzer, B.
TI VERITAS OBSERVATIONS OF THE TeV BINARY LS I+61 degrees 303 DURING
2008-2010
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: general; gamma rays: general; X-rays: binaries
ID HIGH-ENERGY EMISSION; GAMMA-RAY EMISSION; X-RAY; ORBITAL MODULATION;
MICROQUASAR; SPECTRUM; LS-I-+61-303; RADIO; JET
AB We present the results of observations of the TeV binary LS I + 61 degrees 303 with the VERITAS telescope array between 2008 and 2010, at energies above 300 GeV. In the past, both ground-based gamma-ray telescopes VERITAS and MAGIC have reported detections of TeV emission near the apastron phases of the binary orbit. The observations presented here show no strong evidence for TeV emission during these orbital phases; however, during observations taken in late 2010, significant emission was detected from the source close to the phase of superior conjunction (much closer to periastron passage) at a 5.6 standard deviation (5.6 sigma) post-trials significance. In total, between 2008 October and 2010 December a total exposure of 64.5 hr was accumulated with VERITAS on LS I + 61 degrees 303, resulting in an excess at the 3.3 sigma significance level for constant emission over the entire integrated data set. The flux upper limits derived for emission during the previously reliably active TeV phases (i.e., close to apastron) are less than 5% of the Crab Nebula flux in the same energy range. This result stands in apparent contrast to previous observations by both MAGIC and VERITAS which detected the source during these phases at 10% of the Crab Nebula flux. During the two year span of observations, a large amount of X-ray data were also accrued on LS I + 61 degrees 303 by the Swift X-ray Telescope and the Rossi X-ray Timing Explorer Proportional Counter Array. We find no evidence for a correlation between emission in the X-ray and TeV regimes during 20 directly overlapping observations. We also comment on data obtained contemporaneously by the Fermi Large Area Telescope.
C1 [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
[Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA.
[Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
[Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA.
[Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.] 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.
[Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] 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.] Argonne Natl Lab, Argonne, IL 60439 USA.
[Cannon, A.; Collins-Hughes, E.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland.
[Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland.
[Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA.
[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.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA.
[Griffin, S.; Guenette, R.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.] DESY, D-15738 Zeuthen, Germany.
[Humensky, T. B.; Park, N.; Reyes, L. C.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA.
[Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA.
[Krennrich, F.; Orr, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland.
[Pohl, M.; Ruppel, J.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany.
[Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland.
[Senturk, G. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Smith, A. W.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA.
RP Holder, J (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA.
EM jholder@physics.udel.edu; awsmith@hep.anl.gov
OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610;
Ward, John E/0000-0003-1973-0794
FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian
Institution; NSERC in Canada; Science Foundation Ireland (SFI)
[10/RFP/AST2748]; STFC in the U.K; Argonne, a U.S. Department of Energy
Office of Science laboratory [DE-AC02-06CH11357]; NASA [NNX09AR91G]
FX This research is supported by grants from the U.S. Department of Energy,
the U.S. National Science Foundation, the Smithsonian Institution, by
NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and
by STFC in the U. K. We acknowledge the excellent work of the technical
support staff at the Fred Lawrence Whipple Observatory and the
collaborating institutions in the construction and operation of the
instrument.; The submitted manuscript has been created by employees of
UChicago Argonne, LLC, Operator of Argonne National Laboratory
("Argonne") in conjunction with the VERITAS collaboration. Argonne, a
U.S. Department of Energy Office of Science laboratory, is operated
under Contract No. DE-AC02-06CH11357. The U.S. Government retains for
itself, and others acting on its behalf, a paid-up nonexclusive,
irrevocable worldwide license in said article to reproduce, prepare
derivative works, distribute copies to the public, and perform publicly
and display publicly, by or on behalf of the Government.; J. Holder
acknowledges the support of the NASA Fermi Cycle 2 Guest Investigator
Program (grant number NNX09AR91G).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 3
DI 10.1088/0004-637X/738/1/3
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500003
ER
PT J
AU Alexander, DM
Bauer, FE
Brandt, WN
Daddi, E
Hickox, RC
Lehmer, BD
Luo, B
Xue, YQ
Young, M
Comastri, A
Del Moro, A
Fabian, AC
Gilli, R
Goulding, AD
Mainieri, V
Mullaney, JR
Paolillo, M
Rafferty, DA
Schneider, DP
Shemmer, O
Vignali, C
AF Alexander, D. M.
Bauer, F. E.
Brandt, W. N.
Daddi, E.
Hickox, R. C.
Lehmer, B. D.
Luo, B.
Xue, Y. Q.
Young, M.
Comastri, A.
Del Moro, A.
Fabian, A. C.
Gilli, R.
Goulding, A. D.
Mainieri, V.
Mullaney, J. R.
Paolillo, M.
Rafferty, D. A.
Schneider, D. P.
Shemmer, O.
Vignali, C.
TI X-RAY SPECTRAL CONSTRAINTS FOR z approximate to 2 MASSIVE GALAXIES: THE
IDENTIFICATION OF REFLECTION-DOMINATED ACTIVE GALACTIC NUCLEI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: high-redshift; infrared: galaxies;
ultraviolet: galaxies; X-rays: galaxies
ID DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; COMPTON-THICK QUASARS;
HEAVILY OBSCURED AGN; DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED
GALAXIES; STAR-FORMATION; HIGH-REDSHIFT; LUMINOSITY FUNCTION;
SEYFERT-GALAXIES
AB We use the 4 Ms Chandra Deep Field-South (CDF-S) survey to place direct constraints on the ubiquity of z approximate to 2 heavily obscured active galactic nuclei (AGNs) in K < 22 BzK-selected galaxies. Forty-seven (approximate to 21%) of the 222 BzK-selected galaxies in the central region of the CDF-S are detected at X-ray energies, 11 (approximate to 5%) of which have hard X-ray spectral slopes (Gamma less than or similar to 1), indicating the presence of heavily obscured AGN activity (N-H greater than or similar to 3 x 10(23) cm(-2)). The other 36 X-ray detected BzK galaxies appear to be relatively unobscured AGNs and starburst galaxies; we use X-ray variability analyses over a rest-frame baseline of approximate to 3 years to further confirm the presence of AGN activity in many of these systems. The majority (7 out of 11) of the heavily obscured AGNs have excess infrared emission over that expected from star formation (termed "infrared-excess galaxies"). However, we find that X-ray detected heavily obscured AGNs only comprise approximate to 25% of the infrared-excess galaxy population, which is otherwise composed of relatively unobscured AGNs and starburst galaxies. We find that the typical X-ray spectrum of the heavily obscured AGNs is better characterized by a pure reflection model than an absorbed power-law model, suggesting extreme Compton-thick absorption (N-H greater than or similar to 10(24) cm(-2)) in some systems. We verify this result by producing a composite rest-frame 2-20 keV spectrum, which has a similar shape as a reflection-dominated X-ray spectrum and reveals an emission feature at rest-frame energy approximate to 6.4 keV, likely to be due to Fe K. These heavily obscured AGNs are likely to be the distant analogs of the reflection-dominated AGNs recently identified at z approximate to 0 with >10 keV observatories. On the basis of these analyses, we estimate the space density for typical (intrinsic X-ray luminosities of L2-10 (keV) greater than or similar to 10(43) erg s (1)) heavily obscured and Compton-thick AGNs at z approximate to 2. Our space-density constraints are conservative lower limits but they are already consistent with the range of predictions from X-ray background models.
C1 [Alexander, D. M.; Hickox, R. C.; Del Moro, A.; Goulding, A. D.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England.
[Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Brandt, W. N.; Luo, B.; Xue, Y. Q.; Young, M.; Rafferty, D. A.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[Brandt, W. N.; Luo, B.; Xue, Y. Q.; Young, M.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA.
[Daddi, E.; Mullaney, J. R.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,Irfu SAp, F-91191 Gif Sur Yvette, France.
[Hickox, R. C.; Goulding, A. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lehmer, B. D.] Johns Hopkins Univ, Baltimore, MD 21218 USA.
[Lehmer, B. D.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Comastri, A.; Gilli, R.] INAF, Osservatorio Astron Bologna, I-04127 Bologna, Italy.
[Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Mainieri, V.] European So Observ, D-85748 Garching, Germany.
[Paolillo, M.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy.
[Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Vignali, C.] Univ Bologna, Dept Astron, I-40127 Bologna, Italy.
RP Alexander, DM (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England.
RI Daddi, Emanuele/D-1649-2012; Paolillo, Maurizio/J-1733-2012; Vignali,
Cristian/J-4974-2012; Brandt, William/N-2844-2015; Comastri,
Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015;
OI Daddi, Emanuele/0000-0002-3331-9590; Paolillo,
Maurizio/0000-0003-4210-7693; Vignali, Cristian/0000-0002-8853-9611;
Brandt, William/0000-0002-0167-2453; Comastri,
Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177;
Alexander, David/0000-0002-5896-6313
FU Royal Society; Philip Leverhulme Prize; Science and Technology
Facilities Council; Chilean CONICYT [FONDECYT 1101024]; FONDAP [CATA
15010003]; Chandra X-ray Center [SP8-9001X, G09-0134B, SP1-12007A,
SP1-12007B]; NASA [NNX10AC99G]; ERC-StG [UPGAL 240039]; French ANR
[ANR-08-JCJC-008]; Italian Space Agency (ASI) [I/009/10/0, I/088/06/0]
FX We acknowledge financial support from the Royal Society (D.M.A.,
A.C.F.), a Philip Leverhulme Prize (D. M. A., J.R.M.), the Science and
Technology Facilities Council (D.M.A., R.C.H., A.D.G., A.D.M.), the
Chilean CONICYT grants of FONDECYT 1101024 (F. E. B.) and FONDAP CATA
15010003 (F. E. B.), the Chandra X-ray Center grants SP8-9001X (R. C.
H.), G09-0134B (F. E. B.), SP1-12007A (W.N.B., B. D. L., Y.Q.X.), and
SP1-12007B (F. E. B.), the NASA ADP grant NNX10AC99G (W.N.B., B. D. L.,
Y.Q.X., M.Y.), the ERC-StG grant UPGAL 240039 (E. D.), the French ANR
under contract ANR-08-JCJC-008 (E. D.), and the Italian Space Agency
(ASI) under the ASI-INAF contracts I/009/10/0 and I/088/06/0 (A.C.,
R.G., C.V.). We thank the referee for a prompt and considered report and
thank Y. Ueda for providing the Suzaku data and best-fitting model for
Swift J0601.9-8636 used in Figure 5.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 44
DI 10.1088/0004-637X/738/1/44
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500044
ER
PT J
AU Andersson, K
Benson, BA
Ade, PAR
Aird, KA
Armstrong, B
Bautz, M
Bleem, LE
Brodwin, M
Carlstrom, JE
Chang, CL
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Foley, RJ
Forman, WR
Garmire, G
George, EM
Gladders, MD
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hrubes, JD
Jones, C
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Murray, SS
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Stubbs, CW
Vanderlinde, K
Vieira, JD
Vikhlinin, A
Williamson, R
Yang, Y
Zahn, O
Zenteno, A
AF Andersson, K.
Benson, B. A.
Ade, P. A. R.
Aird, K. A.
Armstrong, B.
Bautz, M.
Bleem, L. E.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Foley, R. J.
Forman, W. R.
Garmire, G.
George, E. M.
Gladders, M. D.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Jones, C.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Murray, S. S.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Stubbs, C. W.
Vanderlinde, K.
Vieira, J. D.
Vikhlinin, A.
Williamson, R.
Yang, Y.
Zahn, O.
Zenteno, A.
TI X-RAY PROPERTIES OF THE FIRST SUNYAEV-ZEL'DOVICH EFFECT SELECTED GALAXY
CLUSTER SAMPLE FROM THE SOUTH POLE TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: clusters: intracluster medium; X-rays: galaxies: clusters
ID SCALING RELATIONS; COSMOLOGICAL SIMULATIONS; RELATIVISTIC CORRECTIONS;
LENSING MEASUREMENTS; INTRACLUSTER MEDIUM; POWER SPECTRUM; VIRIAL
RADIUS; MASS; GAS; CONSTRAINTS
AB We present results of X-ray observations of a sample of 15 clusters selected via their imprint on the cosmic microwave background from the thermal Sunyaev-Zel'dovich (SZ) effect. These clusters are a subset of the first SZ-selected cluster catalog, obtained from observations of 178 deg(2) of sky surveyed by the South Pole Telescope (SPT). Using X-ray observations with Chandra and XMM-Newton, we estimate the temperature, T-X, and mass, M-g, of the intracluster medium within r(500) for each cluster. From these, we calculate Y-X = MgTX and estimate the total cluster mass using an M-500-Y-X scaling relation measured from previous X-ray studies. The integrated Comptonization, Y-SZ, is derived from the SZ measurements, using additional information from the X-ray-measured gas density profiles and a universal temperature profile. We calculate scaling relations between the X-ray and SZ observables and find results generally consistent with other measurements and the expectations from simple self-similar behavior. Specifically, we fit a Y-SZ-Y-X relation and find a normalization of 0.82 +/- 0.07, marginally consistent with the predicted ratio of Y-SZ/Y-X = 0.91 +/- 0.01 that would be expected from the density and temperature models used in this work. Using the Y-X-derived mass estimates, we fit a Y-SZ-M-500 relation and find a slope consistent with the self-similar expectation of Y-SZ proportional to M-5/3 with a normalization consistent with predictions from other X-ray studies. We find that the SZ mass estimates, derived from cosmological simulations of the SPT survey, are lower by a factor of 0.78 +/- 0.06 relative to the X-ray mass estimates. This offset is at a level of 1.3 sigma when considering the similar to 15% systematic uncertainty for the simulation-based SZ masses. Overall, the X-ray measurements confirm that the scaling relations of the SZ-selected clusters are consistent with the properties of other X-ray-selected samples of massive clusters, even allowing for the broad redshift range (0.29 < z < 1.08) of the sample.
C1 [Andersson, K.; Bautz, M.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Andersson, K.; Mohr, J. J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hrubes, J. D.; Leitch, E. M.; Marrone, D. P.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Armstrong, B.; Desai, S.; Song, J.; Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Brodwin, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Garmire, G.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[High, F. W.; Rest, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, VP62, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Vikhlinin, A.] Space Res Inst IKI, Moscow, Russia.
RP Andersson, K (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM kanderss@space.mit.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Stark, Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center
[PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA
through Chandra X-ray Observatory Center [GO0-11143]; NASA [NAS8-03060,
NNX09AQ04G, 2834-MIT-SAO-4018]; Chandra Award [AR0-11015A]; DFG "The
Dark Universe" [TRR33]; Excellence Cluster Universe; National Sciences
and Engineering Research Council of Canada; Quebec Fonds de recherche
sur la nature et les technologies; Canadian Institute for Advanced
Research; Brinson Foundation; KICP; Clay Fellowship; Hubble Fellowship
[HF-51259.01-A]; Alfred P. Sloan Research Fellowship; Keck Foundation
FX The South Pole Telescope is supported by the National Science Foundation
through grant ANT-0638937. Partial support is also provided by the NSF
Physics Frontier Center grant PHY-0114422 to the Kavli Institute of
Cosmological Physics at the University of Chicago, the Kavli Foundation,
and the Gordon and Betty Moore Foundation.; Support for X-ray analysis
was provided by NASA through Chandra Award Number GO0-11143 issued by
the Chandra X-ray Observatory Center, which is operated by the
Smithsonian Astrophysical Observatory for and on behalf of NASA under
contract NAS8-03060. Additional support is provided by,NASA through
XMM-Newton Award NNX09AQ04G and Chandra Award AR0-11015A. K. Andersson
is supported in part by NASA through SAO Award Number 2834-MIT-SAO-4018
issued by the Chandra X-ray Observatory Center.; The Munich group is
supported by the DFG through TRR33 "The Dark Universe" and the
Excellence Cluster Universe. The McGill group acknowledges funding from
the National Sciences and Engineering Research Council of Canada, the
Quebec Fonds de recherche sur la nature et les technologies and the
Canadian Institute for Advanced Research. The following individuals
acknowledge additional support: B. Stalder from the Brinson Foundation,
B. Benson from a KICP Fellowship, R. Foley from a Clay Fellowship, D.
Marrone from Hubble Fellowship grant HF-51259.01-A, N. W. Halverson
acknowledges support from an Alfred P. Sloan Research Fellowship. M.
Brodwin from the Keck Foundation, and A. T. Lee from the Miller
Institute for Basic Research in Science, University of California
Berkeley.
NR 91
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 48
DI 10.1088/0004-637X/738/1/48
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500048
ER
PT J
AU Hernandez, JIG
Casares, J
Rebolo, R
Israelian, G
Filippenko, AV
Chornock, R
AF Gonzalez Hernandez, Jonay I.
Casares, Jorge
Rebolo, Rafael
Israelian, Garik
Filippenko, Alexei V.
Chornock, Ryan
TI CHEMICAL ABUNDANCES OF THE SECONDARY STAR IN THE BLACK HOLE X-RAY BINARY
V404 CYGNI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; stars: abundances; stars: evolution; stars:
individual (V404 Cygni = GS 2023+338); supernovae: general; X-rays:
binaries
ID METAL-POOR STARS; NON-LTE ANALYSIS; GRO J1655-40; NOVA SCORPII; SOLAR
NEIGHBORHOOD; DOPPLER TOMOGRAPHY; NEUTRAL MAGNESIUM; SAX J1819.3-2525;
ACCRETION DISC; GALACTIC-HALO
AB We present a chemical abundance analysis of the secondary star in the black hole binary V404 Cygni, using Keck I/High Resolution Spectrometer. We adopt a chi(2)-minimization procedure to derive the stellar parameters, taking into account any possible veiling from the accretion disk. With these parameters we determine the atmospheric abundances of O, Na, Mg, Al, Si, Ca, Ti, Fe, and Ni. The abundances of Al, Si, and Ti appear to be slightly enhanced when comparing with average values in thin-disk solar-type stars. The O abundance, derived from optical lines, is particularly enhanced in the atmosphere of the secondary star in V404 Cygni. This, together with the peculiar velocity of this system as compared with the Galactic velocity dispersion of thin-disk stars, suggests that the black hole formed in a supernova (SN) or hypernova (HN) explosion. We explore different SN/HN models having various geometries to study possible contamination of nucleosynthetic products in the chemical abundance pattern of the secondary star. We find reasonable agreement between the observed abundances and the model predictions. However, the O abundance seems to be too high regardless of the choice of explosion energy or mass cut, when trying to fit other element abundances. Moreover, Mg appears to be underabundant for all explosion models, which produces Mg abundances roughly two times higher than the observed value.
C1 [Gonzalez Hernandez, Jonay I.; Casares, Jorge; Rebolo, Rafael; Israelian, Garik] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Gonzalez Hernandez, Jonay I.; Casares, Jorge; Rebolo, Rafael; Israelian, Garik] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Filippenko, Alexei V.; Chornock, Ryan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hernandez, JIG (reprint author), Inst Astrofis Canarias, E-38205 Tenerife, Spain.
EM jonay@iac.es; jcv@iac.es; rrl@iac.es; gil@iac.es;
alex@astro.berkeley.edu; rchornock@cfa.harvard.edu
RI Gonzalez Hernandez, Jonay I./L-3556-2014
OI Gonzalez Hernandez, Jonay I./0000-0002-0264-7356
FU Spanish Ministry of Science and Innovation (MICINN) [AYA20080-4874,
AYA2010-18080, AYA2005-05149]; US National Science Foundation
[AST-0908886]; W. M. Keck Foundation
FX We thank K. Maeda, H. Umeda, K. Nomoto, and N. Tominaga for providing us
with their spherical and aspherical explosion models. We are grateful to
T. Marsh for the use of the MOLLY analysis package. J.I.G.H.
acknowledges financial support from the Spanish Ministry of Science and
Innovation (MICINN) under the 2009 Juan de la Cierva Programme. J.I.G.H.
and G. I. are grateful for financial support from MICINN grant
AYA20080-4874, while J.C. acknowledges MICINN grant AYA2010-18080.
Additional funding was provided by MICINN grant AYA2005-05149, and (to
A. V. F.) by US National Science Foundation grant AST-0908886. The W. M.
Keck Observatory is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
NASA; it was made possible by the generous financial support of the W.
M. Keck Foundation. This work has made use of the VALD database and IRAF
facilities.
NR 68
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 95
DI 10.1088/0004-637X/738/1/95
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500095
ER
PT J
AU Hargis, JR
Rhode, KL
Strader, J
Brodie, JP
AF Hargis, Jonathan R.
Rhode, Katherine L.
Strader, Jay
Brodie, Jean P.
TI THE GLOBULAR CLUSTER POPULATION OF NGC 7457: CLUES TO THE EVOLUTION OF
FIELD S0 GALAXIES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies:
individual (NGC 7457); galaxies: photometry; galaxies: spiral
ID HUBBLE-SPACE-TELESCOPE; LOCAL GROUP; ELLIPTIC GALAXIES; SECULAR
EVOLUTION; CLASSICAL BULGES; SPIRAL GALAXIES; GALACTIC HALO; DISK
GALAXIES; MILKY-WAY; SYSTEMS
AB In this paper, we present the results of a wide-field imaging study of the globular cluster (GC) system of the field S0 galaxy NGC 7457. To derive the global properties of the GC system, we obtained deep BVR images with the WIYN 3.5 m telescope and Minimosaic Imager and studied the GC population of NGC 7457 to a projected radius of similar to 30 kpc. Our ground-based data were combined with archival and published Hubble Space Telescope data to probe the properties of the GC system close to the galaxy center and reduce contamination in the GC candidate sample from foreground stars and background galaxies. We performed surface photometry of NGC 7457 and compared the galaxy's surface brightness profile with the surface density profile of the GC system. The profiles have similar shapes in the inner 1' (3.9 kpc), but the GC system profile appears to flatten relative to the galaxy light at larger radii. The GC system of NGC 7457 is noticeably elliptical in our images; we measure epsilon = 0.66 +/- 0.14 for the GC distribution, which is consistent with our measured ellipticity of the galaxy light. We integrated the radial surface density profile of the GC system to derive a total number of GCs, N-GC = 210 +/- 30. The GC specific frequencies normalized by the galaxy luminosity and mass are S-N = 3.1 +/- 0.7 and T = 4.8 +/- 1.1, respectively. Comparing the derived GC system properties and other empirical data for NGC 7457 to S0 formation scenarios suggests that this field S0 galaxy may have formed in an unequal-mass merger.
C1 [Hargis, Jonathan R.; Rhode, Katherine L.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Strader, Jay] Harvard Univ, Coll Observ, Cambridge, MA USA.
RP Hargis, JR (reprint author), Indiana Univ, Dept Astron, 727 E 3rd St,Swain W 319, Bloomington, IN 47405 USA.
EM jhargis@astro.indiana.edu
FU NSF Faculty [AST-0847109]; National Aeronautics and Space Administration
FX This research was supported by an NSF Faculty Early Career Development
(CAREER) award (AST-0847109) to K.L.R. We are grateful to Mike Young for
acquiring the data for this study and to the staff of the WIYN
Observatory and Kitt Peak National Observatory for their assistance
during the observing run. J.R.H. thanks Steven Janowiecki and Liese van
Zee for useful conversations during the course of this work. We thank
the anonymous referee for his/her useful comments which have improved
the quality of the paper. This research has made use of the NASA/IPAC
Extragalactic Database (NED) which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.
NR 61
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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 SEP 1
PY 2011
VL 738
IS 1
AR 113
DI 10.1088/0004-637X/738/1/113
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500113
ER
PT J
AU Hernandez, AK
Tan, JC
Caselli, P
Butler, MJ
Jimenez-Serra, I
Fontani, F
Barnes, P
AF Hernandez, Audra K.
Tan, Jonathan C.
Caselli, Paola
Butler, Michael J.
Jimenez-Serra, Izaskun
Fontani, Francesco
Barnes, Peter
TI MAPPING LARGE-SCALE CO DEPLETION IN A FILAMENTARY INFRARED DARK CLOUD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; ISM: clouds; stars: formation
ID STAR-FORMATION; CORES; EXTINCTION; CLUSTERS; EMISSION; RADIO; MASS
AB Infrared Dark Clouds (IRDCs) are cold, high mass surface density and high density structures, likely to be representative of the initial conditions for massive star and star cluster formation. CO emission from IRDCs has the potential to be useful for tracing their dynamics, but may be affected by depleted gas phase abundances due to freeze out onto dust grains. Here we analyze (CO)-O-18 J = 1 -> 0 and J = 2 -> 1 emission line data, taken with the Instituto de Radioastronomia Milimetrica 30 m telescope, of the highly filamentary IRDC G035.39.-0033. We derive the excitation temperature as a function of position and velocity, with typical values of similar to 7 K, and thus derive total mass surface densities, Sigma(C18O), assuming standard gas phase abundances and accounting for optical depth in the line, which can reach values of similar to 1. The mass surface densities reach values of similar to 0.07 g cm(-2). We compare these results to the mass surface densities derived from mid-infrared extinction mapping, Sigma(SMF), by Butler & Tan, which are expected to be insensitive to the dust temperatures in the cloud. With a significance of greater than or similar to 10 sigma, we find Sigma(C18O)/Sigma(SMF) decreases by about a factor of five as Sigma increases from similar to 0.02 to similar to 0.2 g cm(-2), which we interpret as evidence for CO depletion. Several hundred solar masses are being affected, making this one of the most massive clouds in which CO depletion has been observed directly. We present a map of the depletion factor in the filament and discuss implications for the formation of the IRDC.
C1 [Hernandez, Audra K.; Butler, Michael J.; Barnes, Peter] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Tan, Jonathan C.] Univ Florida, Dept Phys & Astron, Gainesville, FL 32611 USA.
[Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England.
[Jimenez-Serra, Izaskun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fontani, Francesco] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France.
RP Hernandez, AK (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
EM audrah@astro.ufl.edu; jt@astro.ufl.edu; P.Caselli@leeds.ac.uk;
butler85@astro.ufl.edu; ijimenez-serra@cfa.harvard.edu; fontani@iram.fr;
peterb@astro.ufl.edu
OI Fontani, Francesco/0000-0003-0348-3418
FU SEAGEP Dissertation Fellowship; NSF [AST-0645412]; NASA [ATP09-0094,
ADAP10-0110]; University of Florida
FX We thank E. van Dishoeck and R. Visser for helpful discussions and the
comments of an anonymous referee, which helped improve the paper. A. K.
H. acknowledges support from a SEAGEP Dissertation Fellowship. J.C.T.
acknowledges support from NSF CAREER grant AST-0645412, NASA
Astrophysics Theory and Fundamental Physics grant ATP09-0094, NASA
Astrophysics Data Analysis Program ADAP10-0110, and a Faculty
Enhancement Opportunity grant from the University of Florida.
NR 31
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD SEP 1
PY 2011
VL 738
IS 1
AR 11
DI 10.1088/0004-637X/738/1/11
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500011
ER
PT J
AU Saez, C
Brandt, WN
Shemmer, O
Chomiuk, L
Lopez, LA
Marshall, HL
Miller, BP
Vignali, C
AF Saez, C.
Brandt, W. N.
Shemmer, O.
Chomiuk, L.
Lopez, L. A.
Marshall, H. L.
Miller, B. P.
Vignali, C.
TI THE X-RAY PROPERTIES OF TYPICAL HIGH-REDSHIFT RADIO-LOUD QUASARS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; galaxies: active; X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; LOW-ENERGY CUTOFFS; 5TH DATA
RELEASE; CHANDRA OBSERVATIONS; SPECTRAL PROPERTIES; ASTRONOMICAL DATA;
1ST SURVEY; H I; JETS
AB We report spectral, imaging, and variability results from four new XMM-Newton observations and two new Chandra observations of high-redshift (z greater than or similar to 4) radio-loud quasars (RLQs). Our targets span lower, and more representative, values of radio loudness than those of past samples of high-redshift RLQs studied in the X-ray regime. Our spectral analyses show power-law X-ray continua with a mean photon index, = 1.74 +/- 0.11, that is consistent with measurements of lower redshift RLQs. These continua are likely dominated by jet-linked X-ray emission, and they follow the expected anticorrelation between photon index and radio loudness. We find no evidence of iron K alpha emission lines or Compton-reflection continua. Our data also constrain intrinsic X-ray absorption in these RLQs. We find evidence for significant absorption (N-H approximate to 1.7 x 10(22)cm(-2)) in one RLQ of our sample (SDSS J0011+1446); the incidence of X-ray absorption in our sample appears plausibly consistent with that for high-redshift RLQs that have higher values of radio loudness. In the Chandra observation of PMNJ2219-2719 we detect apparent extended (similar to 14 kpc) X-ray emission that is most likely due to a jet; the X-ray luminosity of this putative jet is approximate to 2% that of the core. The analysis of a 4.9 GHz Very Large Array image of PMN J2219-2719 reveals a structure that matches the X-ray extension found in this source. We also find evidence for long-term (450-460 days) X-ray variability by 80%-100% in two of our targets.
C1 [Saez, C.; Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA.
[Chomiuk, L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Chomiuk, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lopez, L. A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Miller, B. P.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy.
[Vignali, C.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy.
RP Saez, C (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM saez@astro.psu.edu
RI Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015;
OI Vignali, Cristian/0000-0002-8853-9611; Brandt,
William/0000-0002-0167-2453; Shemmer, Ohad/0000-0003-4327-1460
FU NASA ADP [NNX10AC99G]; Chandra X-ray Center [G09-0112X]; AAUW American
Dissertation Fellowship; Italian Space Agency (ASI) under the ASI-INAF
[I/009/10/0, I/088/06/0]; Chandra Award [GO0-11112A]
FX We thank M. Young, B. Kelly, C. C. Cheung, and the anonymous referee for
helpful discussions and comments. We acknowledge support from NASA ADP
grant NNX10AC99G (CS, WNB), Chandra X-ray Center grant G09-0112X (CS,
WNB), and an AAUW American Dissertation Fellowship (LAL). C. Vignali
acknowledges support from the Italian Space Agency (ASI) under the
ASI-INAF contracts I/009/10/0 and I/088/06/0. B. P. Miller acknowledges
support by Chandra Award Number GO0-11112A. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc.
NR 63
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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 SEP 1
PY 2011
VL 738
IS 1
AR 53
DI 10.1088/0004-637X/738/1/53
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500053
ER
PT J
AU Tang, S
Grindlay, J
Los, E
Servillat, M
AF Tang, Sumin
Grindlay, Jonathan
Los, Edward
Servillat, Mathieu
TI DASCH ON KU Cyg: A similar to 5 YEAR DUST ACCRETION EVENT IN similar to
1900
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; stars: individual (KU Cyg)
ID H-ALPHA EMISSION; PROTOPLANETARY DISKS; RADIATION-PRESSURE; PHOTOMETRY;
VARIABILITY; BINARIES; SURFACE; STARS; THICK
AB KU Cyg is an eclipsing binary consisting of an F-type star accreting through a large accretion disk from a K5III red giant. Here we present the discovery of a 5 year dip around 1900 found from its 100 year DASCH light curve. It showed a similar to 0.5 mag slow fading from 1899 to 1903 and brightened back around 1904 on a relatively shorter timescale. The light curve shape of the 1899-1904 fading-brightening event differs from the dust production and dispersion process observed in R Coronae Borealis stars, which usually has a faster fading and slower recovery, and for KU Cyg is probably related to the accretion disk surrounding the F star. The slow fading in KU Cyg is probably caused by increases in dust extinction in the disk, and the subsequent quick brightening may be due to the evaporation of dust transported inward through the disk. The extinction excess which caused the fading may arise from increased mass transfer rate in the system or from dust clump ejections from the K giant.
C1 [Tang, Sumin; Grindlay, Jonathan; Los, Edward; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tang, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM stang@cfa.harvard.edu
FU NSF [AST-0407380, AST-0909073]; Cornel and Cynthia K. Sarosdy Fund for
DASCH
FX We are grateful to the anonymous referee for helpful comments and
suggestions. We thank Alison Doane, Jaime Pepper, and Bob Simcoe at CfA
for their work on DASCH, and many volunteers who have helped digitize
logbooks and clean and scan plates
(http://hea-www.harvard.edu/DASCH/team.php). We are grateful to the
logbook transcription team at the American Museum of Natural History in
New York City led by Michael Shara and Holly Barton. S. T. thanks Ruth
Murray-Clay, Matthew Holman, Philip Chang, and Li Zeng for helpful
discussions. This work was supported in part by NSF grants AST-0407380
and AST-0909073 and now also the Cornel and Cynthia K. Sarosdy Fund for
DASCH.
NR 23
TC 3
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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 SEP 1
PY 2011
VL 738
IS 1
AR 7
DI 10.1088/0004-637X/738/1/7
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500007
ER
PT J
AU Waldman, R
Sauer, D
Livne, E
Perets, H
Glasner, A
Mazzali, P
Truran, JW
Gal-Yam, A
AF Waldman, Roni
Sauer, Daniel
Livne, Eli
Perets, Hagai
Glasner, Ami
Mazzali, Paolo
Truran, James W.
Gal-Yam, Avishay
TI HELIUM SHELL DETONATIONS ON LOW-MASS WHITE DWARFS AS A POSSIBLE
EXPLANATION FOR SN 2005E
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE supernovae: individual (SN 2005E); white dwarfs
ID MONTE-CARLO TECHNIQUES; OFF-CENTER DETONATION; IA SUPERNOVAE; ABUNDANCE
STRATIFICATION; NONTHERMAL EXCITATION; RADIATIVE-TRANSFER; ENERGY
DEPOSITION; SYNTHETIC SPECTRA; LIGHT CURVES; MODELS
AB Recently, several Type Ib supernovae (SNe; with the prototypical SN 2005E) have been shown to have atypical properties. These SNe are faint (absolute peak magnitude of similar to-15) and fast SNe that show unique composition. They are inferred to have low ejecta mass (a few tenths of a solar mass) and to be highly enriched in calcium, but poor in silicon elements and nickel. These SNe were therefore suggested to belong to a new class of calcium-rich faint SNe explosions. Their properties were proposed to be the result of helium detonations that may occur on helium accreting white dwarfs. In this paper, we theoretically study the scenario of helium detonations and focus on the results of detonations in accreted helium layers on low-mass carbon-oxygen (CO) cores. We present new results from one-dimensional simulations of such explosions, including their light curves and spectra. We find that when the density of the helium layer is low enough the helium detonation produces large amounts of intermediate elements, such as calcium and titanium, together with a large amount of unburnt helium. Alternatively, enough carbon enrichment of the accreted helium as a result of convective undershoot at the early stages of the runaway can avoid the production of iron group elements as the alpha particles are consumed avoiding iron production. Our results suggest that the properties of calcium-rich faint SNe could indeed be consistent with the helium-detonation scenario on small CO cores. Above a certain density (larger CO cores) the detonation leaves mainly Ni-56 and unburnt helium, and the predicted spectrum will unlikely fit the unique features of this class of SNe. Finally, none of our studied models reproduces the bright, fast-evolving light curves of another type of peculiar SNe suggested to originate in helium detonations (SNe 1885A, 1939B, and 2002bj).
C1 [Waldman, Roni; Livne, Eli; Glasner, Ami] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
[Sauer, Daniel] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden.
[Perets, Hagai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany.
[Mazzali, Paolo] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Mazzali, Paolo] Ist Naz Astrofis Oss Astron, I-35122 Padua, Italy.
[Truran, James W.] Argonne Natl Lab, Div Phys, Argonne, IL 60439 USA.
[Truran, James W.] Univ Chicago, Dept Astron & Astrophys, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Truran, James W.] Univ Chicago, Joint Inst Nucl Astrophys, Chicago, IL 60637 USA.
[Gal-Yam, Avishay] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel.
RP Waldman, R (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
RI Sauer, Daniel/A-3033-2012; Perets, Hagai/K-9605-2015
OI Sauer, Daniel/0000-0002-0317-5063; Perets, Hagai/0000-0002-5004-199X
FU Weizmann-Minerva grant; Israeli Science Foundation; EU; Peter and
Patricia Gruber Awards; DOE at the Argonne National Laboratory
[DE-AC02-06CH11357]; NSF at the University of Chicago [PHY 08-22648]
FX We thank Stefano Valenti for computing the quasi-bolometric light curve
of SN 2005E from the observed data. We are grateful for Stuart Sim and
Markus Kromer at the Max-Planck Institute for Astrophysics for computing
a radiative transfer model to cross-check our model results. Nuclear
half-lives and decay energies used in the light curve model calculations
have been compiled using NuDat 2.5 (http://www.nndc.bnl.gov/nudat2) and
the Web-based Table of Nuclides of the Korea Atomic Energy Research
Institute (http://atom.kaeri.re.kr). Joint research by A. G. and P. A.
M. is supported by a Weizmann-Minerva grant. The work of A. G. is also
supported by the Israeli Science Foundation, an EU FP7 Marie Curie IRG
fellowship, and a research grant from the Peter and Patricia Gruber
Awards. This work is supported in part at the Argonne National
Laboratory by the DOE under contract No. DE-AC02-06CH11357, and at the
University of Chicago by the NSF under grant PHY 08-22648 for the
Physics Frontier Center "Joint Institute for Nuclear Astrophysics"
(JINA).
NR 45
TC 43
Z9 43
U1 1
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 SEP 1
PY 2011
VL 738
IS 1
AR 21
DI 10.1088/0004-637X/738/1/21
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808XO
UT WOS:000294015500021
ER
PT J
AU Wolf, S
Eugster, W
Potvin, C
Turner, BL
Buchmann, N
AF Wolf, Sebastian
Eugster, Werner
Potvin, Catherine
Turner, Benjamin L.
Buchmann, Nina
TI Carbon sequestration potential of tropical pasture compared with
afforestation in Panama
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE carbon dioxide fluxes; eddy covariance; FLUXNET; grazing; land-use
change; managed ecosystems; soil carbon
ID ECOSYSTEM CO2 EXCHANGE; AMAZONIAN RAIN-FOREST; LAND-USE CHANGES;
EDDY-COVARIANCE; SEASONAL-VARIATIONS; FLUX MEASUREMENTS; DIOXIDE UPTAKE;
WATER-VAPOR; BALANCE; CLIMATE
AB Tropical forest ecosystems play an important role in regulating the global climate, yet deforestation and land-use change mean that the tropical carbon sink is increasingly influenced by agroecosystems and pastures. Despite this, it is not yet fully understood how carbon cycling in the tropics responds to land-use change, particularly for pasture and afforestation. Thus, the objectives of our study were: (1) to elucidate the environmental controls and the impact of management on gross primary production (GPP), total ecosystem respiration (TER) and net ecosystem CO(2) exchange (NEE); (2) to estimate the carbon sequestration potential of tropical pasture compared with afforestation; and (3) to compare eddy covariance-derived carbon budgets with biomass and soil inventory data. We performed comparative measurements of NEE in a tropical C(4) pasture and an adjacent afforestation with native tree species in Sardinilla (Panama) from 2007 to 2009. Pronounced seasonal variation in GPP, TER and NEE were closely related to radiation, soil moisture, and C(3) vs. C(4) plant physiology. The shallow rooting depth of grasses compared with trees resulted in a higher sensitivity of the pasture ecosystem to water limitation and seasonal drought. During 2008, substantial amounts of carbon were sequestered by the afforestation (-442 gCm(-2), negative values denote ecosystem carbon uptake), which was in agreement with biometric observations (-450 gCm(-2)). In contrast, the pasture ecosystem was a strong carbon source in 2008 and 2009 (261 gCm(-2)), associated with seasonal drought and overgrazing. In addition, soil carbon isotope data indicated rapid carbon turnover after conversion from C(4) pasture to C(3) afforestation. Our results clearly show the potential for considerable carbon sequestration of tropical afforestation and highlight the risk of carbon losses from pasture ecosystems in a seasonal tropical climate.
C1 [Wolf, Sebastian; Eugster, Werner; Buchmann, Nina] ETH, Inst Agr Sci, CH-8092 Zurich, Switzerland.
[Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Potvin, Catherine; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Wolf, S (reprint author), ETH, Inst Agr Sci, Univ Str 2, CH-8092 Zurich, Switzerland.
EM sewolf@ethz.ch
RI Turner, Benjamin/E-5940-2011; daorui, han/G-3767-2011; Wolf,
Sebastian/B-4580-2010; Buchmann, Nina/E-6095-2011; Eugster,
Werner/E-5116-2010
OI Turner, Benjamin/0000-0002-6585-0722; Wolf,
Sebastian/0000-0001-7717-6993; Eugster, Werner/0000-0001-6067-0741
FU North-South Centre (former Swiss Centre for International Agriculture)
of ETH Zurich; Natural Sciences and Engineering Council of Canada;
Smithsonian Tropical Research Institute (STRI); Meteorology and
Hydrology Branch of the Panama Canal Authority (ACP), Republic of
Panama; SENACYT
FX Funding for this project was provided by the North-South Centre (former
Swiss Centre for International Agriculture) of ETH Zurich. Catherine
Potvin acknowledges the support from a Discovery grant of the Natural
Sciences and Engineering Council of Canada. We are grateful to the
Smithsonian Tropical Research Institute (STRI) for support with the
Sardinilla site and the Meteorology and Hydrology Branch of the Panama
Canal Authority (ACP), Republic of Panama, for providing meteorological
data. We thank Timothy Seipel for identifying grass species of the
pasture, Jefferson Hall and his project funded by SENACYT for providing
information on rooting depth at the afforestation site, Dayana Agudo and
Tania Romero (STRI) for laboratory support, Nicolas Gruber for inspiring
discussions, Rodrigo Vargas for valuable comments on the manuscript, and
Jose Monteza for tower maintenance and assistance in the field.
NR 64
TC 20
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U1 0
U2 79
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD SEP
PY 2011
VL 17
IS 9
BP 2763
EP 2780
DI 10.1111/j.1365-2486.2011.02460.x
PG 18
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 800WS
UT WOS:000293399000001
ER
PT J
AU Wright, EL
Black, CR
Cheesman, AW
Drage, T
Large, D
Turner, BL
Sjogersten, S
AF Wright, Emma L.
Black, Colin R.
Cheesman, Alexander W.
Drage, Trevor
Large, David
Turner, Benjamin L.
Sjoegersten, Sofie
TI Contribution of subsurface peat to CO2 and CH4 fluxes in a neotropical
peatland
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE carbon; methane; nutrient gradient; Panama; peatland; solid state C-13
CPMAS NMR; tropical
ID GREENHOUSE-GAS EMISSIONS; METHANE EMISSIONS; SWAMP FOREST; TROPICAL
PEATLAND; CARBON DYNAMICS; LATE PLEISTOCENE; ORGANIC-MATTER; WETLAND
SOILS; 3 ECOSYSTEMS; KALIMANTAN
AB Tropical peatlands play an important role in the global carbon cycling but little is known about factors regulating carbon dioxide (CO2) and methane (CH4) fluxes from these ecosystems. Here, we test the hypotheses that (i) CO2 and CH4 are produced mainly from surface peat and (ii) that the contribution of subsurface peat to net C emissions is governed by substrate availability. To achieve this, in situ and ex situ CO2 and CH4 fluxes were determined throughout the peat profiles under three vegetation types along a nutrient gradient in a tropical ombrotrophic peatland in Panama. The peat was also characterized with respect to its organic composition using C-13 solid state cross-polarization magic-angle spinning nuclear magnetic resonance spectroscopy. Deep peat contributed substantially to CO2 effluxes both with respect to actual in situ and potential ex situ fluxes. CH4 was produced throughout the peat profile with distinct subsurface peaks, but net emission was limited by oxidation in the surface layers. CO2 and CH4 production were strongly substrate-limited and a large proportion of the variance in their production (30% and 63%, respectively) was related to the quantity of carbohydrates in the peat. Furthermore, CO2 and CH4 production differed between vegetation types, suggesting that the quality of plant-derived carbon inputs is an important driver of trace gas production throughout the peat profile. We conclude that the production of both CO2 and CH4 from subsurface peat is a substantial component of the net efflux of these gases, but that gas production through the peat profile is regulated in part by the degree of decomposition of the peat.
C1 [Wright, Emma L.; Black, Colin R.; Sjoegersten, Sofie] Univ Nottingham, Sch Biosci, Nottingham NG7 2RD, England.
[Cheesman, Alexander W.] Univ Florida, Soil & Water Sci Dept, Gainesville, FL 32611 USA.
[Cheesman, Alexander W.; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Drage, Trevor; Large, David] Univ Nottingham, Sch Chem & Environm Engn, Nottingham NG7 2RD, England.
RP Sjogersten, S (reprint author), Univ Nottingham, Sch Biosci, Nottingham NG7 2RD, England.
EM Sofie.Sjogersten@nottingham.ac.uk
RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013;
OI Turner, Benjamin/0000-0002-6585-0722; Cheesman,
Alexander/0000-0003-3931-5766; Drage, Trevor/0000-0002-4939-1933
FU UK Biotechnology and Biological Sciences Research Council; University of
Nottingham; USDA-CREES National Research Initiative [2004-35107-14918]
FX Emma Wright thanks the UK Biotechnology and Biological Sciences Research
Council for her PhD scholarship. This project was supported by a
University of Nottingham New Investigator grant. Alexander Cheesman was
funded by a grant from the USDA-CREES National Research Initiative (No.
2004-35107-14918). We thank Tania Romero for laboratory assistance, Eric
Brown for field support and staff at the Smithsonian Tropical Research
Institute station in Bocas del Toro for logistical support.
NR 66
TC 22
Z9 22
U1 8
U2 69
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD SEP
PY 2011
VL 17
IS 9
BP 2867
EP 2881
DI 10.1111/j.1365-2486.2011.02448.x
PG 15
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 800WS
UT WOS:000293399000008
ER
PT J
AU Kattge, J
Diaz, S
Lavorel, S
Prentice, C
Leadley, P
Bonisch, G
Garnier, E
Westoby, M
Reich, PB
Wright, IJ
Cornelissen, JHC
Violle, C
Harrison, SP
van Bodegom, PM
Reichstein, M
Enquist, BJ
Soudzilovskaia, NA
Ackerly, DD
Anand, M
Atkin, O
Bahn, M
Baker, TR
Baldocchi, D
Bekker, R
Blanco, CC
Blonder, B
Bond, WJ
Bradstock, R
Bunker, DE
Casanoves, F
Cavender-Bares, J
Chambers, JQ
Chapin, FS
Chave, J
Coomes, D
Cornwell, WK
Craine, JM
Dobrin, BH
Duarte, L
Durka, W
Elser, J
Esser, G
Estiarte, M
Fagan, WF
Fang, J
Fernandez-Mendez, F
Fidelis, A
Finegan, B
Flores, O
Ford, H
Frank, D
Freschet, GT
Fyllas, NM
Gallagher, RV
Green, WA
Gutierrez, AG
Hickler, T
Higgins, SI
Hodgson, JG
Jalili, A
Jansen, S
Joly, CA
Kerkhoff, AJ
Kirkup, D
Kitajima, K
Kleyer, M
Klotz, S
Knops, JMH
Kramer, K
Kuhn, I
Kurokawa, H
Laughlin, D
Lee, TD
Leishman, M
Lens, F
Lenz, T
Lewis, SL
Lloyd, J
Llusia, J
Louault, F
Ma, S
Mahecha, MD
Manning, P
Massad, T
Medlyn, BE
Messier, J
Moles, AT
Muller, SC
Nadrowski, K
Naeem, S
Niinemets, U
Nollert, S
Nuske, A
Ogaya, R
Oleksyn, J
Onipchenko, VG
Onoda, Y
Ordonez, J
Overbeck, G
Ozinga, WA
Patino, S
Paula, S
Pausas, JG
Penuelas, J
Phillips, OL
Pillar, V
Poorter, H
Poorter, L
Poschlod, P
Prinzing, A
Proulx, R
Rammig, A
Reinsch, S
Reu, B
Sack, L
Salgado-Negre, B
Sardans, J
Shiodera, S
Shipley, B
Siefert, A
Sosinski, E
Soussana, JF
Swaine, E
Swenson, N
Thompson, K
Thornton, P
Waldram, M
Weiher, E
White, M
White, S
Wright, SJ
Yguel, B
Zaehle, S
Zanne, AE
Wirth, C
AF Kattge, J.
Diaz, S.
Lavorel, S.
Prentice, C.
Leadley, P.
Boenisch, G.
Garnier, E.
Westoby, M.
Reich, P. B.
Wright, I. J.
Cornelissen, J. H. C.
Violle, C.
Harrison, S. P.
van Bodegom, P. M.
Reichstein, M.
Enquist, B. J.
Soudzilovskaia, N. A.
Ackerly, D. D.
Anand, M.
Atkin, O.
Bahn, M.
Baker, T. R.
Baldocchi, D.
Bekker, R.
Blanco, C. C.
Blonder, B.
Bond, W. J.
Bradstock, R.
Bunker, D. E.
Casanoves, F.
Cavender-Bares, J.
Chambers, J. Q.
Chapin, F. S., III
Chave, J.
Coomes, D.
Cornwell, W. K.
Craine, J. M.
Dobrin, B. H.
Duarte, L.
Durka, W.
Elser, J.
Esser, G.
Estiarte, M.
Fagan, W. F.
Fang, J.
Fernandez-Mendez, F.
Fidelis, A.
Finegan, B.
Flores, O.
Ford, H.
Frank, D.
Freschet, G. T.
Fyllas, N. M.
Gallagher, R. V.
Green, W. A.
Gutierrez, A. G.
Hickler, T.
Higgins, S. I.
Hodgson, J. G.
Jalili, A.
Jansen, S.
Joly, C. A.
Kerkhoff, A. J.
Kirkup, D.
Kitajima, K.
Kleyer, M.
Klotz, S.
Knops, J. M. H.
Kramer, K.
Kuehn, I.
Kurokawa, H.
Laughlin, D.
Lee, T. D.
Leishman, M.
Lens, F.
Lenz, T.
Lewis, S. L.
Lloyd, J.
Llusia, J.
Louault, F.
Ma, S.
Mahecha, M. D.
Manning, P.
Massad, T.
Medlyn, B. E.
Messier, J.
Moles, A. T.
Mueller, S. C.
Nadrowski, K.
Naeem, S.
Niinemets, Ue.
Noellert, S.
Nueske, A.
Ogaya, R.
Oleksyn, J.
Onipchenko, V. G.
Onoda, Y.
Ordonez, J.
Overbeck, G.
Ozinga, W. A.
Patino, S.
Paula, S.
Pausas, J. G.
Penuelas, J.
Phillips, O. L.
Pillar, V.
Poorter, H.
Poorter, L.
Poschlod, P.
Prinzing, A.
Proulx, R.
Rammig, A.
Reinsch, S.
Reu, B.
Sack, L.
Salgado-Negre, B.
Sardans, J.
Shiodera, S.
Shipley, B.
Siefert, A.
Sosinski, E.
Soussana, J. -F.
Swaine, E.
Swenson, N.
Thompson, K.
Thornton, P.
Waldram, M.
Weiher, E.
White, M.
White, S.
Wright, S. J.
Yguel, B.
Zaehle, S.
Zanne, A. E.
Wirth, C.
TI TRY - a global database of plant traits
SO GLOBAL CHANGE BIOLOGY
LA English
DT Article
DE comparative ecology; database; environmental gradient; functional
diversity; global analysis; global change; interspecific variation;
intraspecific variation; plant attribute; plant functional type; plant
trait; vegetation model
ID RELATIVE GROWTH-RATE; TROPICAL RAIN-FOREST; HAWAIIAN
METROSIDEROS-POLYMORPHA; LITTER DECOMPOSITION RATES; LEAF ECONOMICS
SPECTRUM; OLD-FIELD SUCCESSION; SUB-ARCTIC FLORA; FUNCTIONAL TRAITS;
WIDE-RANGE; TERRESTRIAL BIOSPHERE
AB Plant traits - the morphological, anatomical, physiological, biochemical and phenological characteristics of plants and their organs - determine how primary producers respond to environmental factors, affect other trophic levels, influence ecosystem processes and services and provide a link from species richness to ecosystem functional diversity. Trait data thus represent the raw material for a wide range of research from evolutionary biology, community and functional ecology to biogeography. Here we present the global database initiative named TRY, which has united a wide range of the plant trait research community worldwide and gained an unprecedented buy-in of trait data: so far 93 trait databases have been contributed. The data repository currently contains almost three million trait entries for 69 000 out of the world's 300 000 plant species, with a focus on 52 groups of traits characterizing the vegetative and regeneration stages of the plant life cycle, including growth, dispersal, establishment and persistence. A first data analysis shows that most plant traits are approximately log-normally distributed, with widely differing ranges of variation across traits. Most trait variation is between species (interspecific), but significant intraspecific variation is also documented, up to 40% of the overall variation. Plant functional types (PFTs), as commonly used in vegetation models, capture a substantial fraction of the observed variation - but for several traits most variation occurs within PFTs, up to 75% of the overall variation. In the context of vegetation models these traits would better be represented by state variables rather than fixed parameter values. The improved availability of plant trait data in the unified global database is expected to support a paradigm shift from species to trait-based ecology, offer new opportunities for synthetic plant trait research and enable a more realistic and empirically grounded representation of terrestrial vegetation in Earth system models.
C1 [Kattge, J.; Boenisch, G.; Reichstein, M.; Frank, D.; Mahecha, M. D.; Massad, T.; Noellert, S.; Nueske, A.; Reu, B.; Zaehle, S.] Max Planck Inst Biogeochem, D-07745 Jena, Germany.
[Diaz, S.] Univ Nacl Cordoba, Inst Multidisciplinario Biol Vegetal, RA-5000 Cordoba, Argentina.
[Lavorel, S.] CNRS, Lab Ecol Alpine LECA, Grenoble, France.
[Prentice, C.; Westoby, M.; Wright, I. J.; Harrison, S. P.; Gallagher, R. V.; Leishman, M.; Lenz, T.; Medlyn, B. E.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia.
[Leadley, P.] Univ Paris 11, Lab Ecol Systemat & Evolut ESE, Paris, France.
[Garnier, E.; Violle, C.] CNRS, Ctr Ecol Fonct & Evolut, F-34293 Montpellier, France.
[Reich, P. B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
[Reich, P. B.] Univ Minnesota, Inst Environm, St Paul, MN 55108 USA.
[Reich, P. B.; Freschet, G. T.] Univ Western Sydney, Hawkesbury Inst Environm, Richmond, NSW 2753, Australia.
[Cornelissen, J. H. C.; van Bodegom, P. M.; Soudzilovskaia, N. A.; Cornwell, W. K.] Vrije Univ Amsterdam, Fac Earth & Life Sci, NL-1081 HV Amsterdam, Netherlands.
[Enquist, B. J.; Blonder, B.; Dobrin, B. H.; Messier, J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
[Ackerly, D. D.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.
[Anand, M.; White, S.] Univ Guelph, Sch Environm Sci, Guelph, ON N1G 2W1, Canada.
[Atkin, O.] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia.
[Bahn, M.] Univ Innsbruck, Inst Ecol, A-6020 Innsbruck, Austria.
[Baker, T. R.; Fyllas, N. M.; Lewis, S. L.; Lloyd, J.; Patino, S.; Phillips, O. L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
[Baldocchi, D.; Ma, S.] Univ Calif Berkeley, Dept Environm Sci, Berkeley, CA 94720 USA.
[Baldocchi, D.] Univ Calif Berkeley, Ctr Atmospher Sci, Berkeley, CA 94720 USA.
[Bekker, R.] Univ Groningen, Ctr Life Sci, NL-9700 CC Groningen, Netherlands.
[Blanco, C. C.; Mueller, S. C.; Pillar, V.] Univ Fed Rio Grande do Sul, Dept Ecol, BR-91501970 Porto Alegre, RS, Brazil.
[Bond, W. J.] Univ Cape Town, Dept Bot, ZA-7701 Rondebosch, South Africa.
[Bradstock, R.] Univ Wollongong, Sch Biol Sci, Wollongong, NSW 2522, Australia.
[Bunker, D. E.] New Jersey Inst Technol, Dept Biol Sci, Newark, NJ 07102 USA.
[Casanoves, F.; Finegan, B.; Salgado-Negre, B.] Trop Agr Ctr Res & Higher Educ CATIE, Turrialba 937170, Costa Rica.
[Cavender-Bares, J.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA.
[Chambers, J. Q.] Univ Calif Berkeley, Lawrence Berkeley Lab, Climate Sci Dept, Berkeley, CA 94720 USA.
[Chapin, F. S., III] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA.
[Chave, J.] CNRS, Lab Evolut & Diversite Biol, Toulouse, France.
[Coomes, D.] Univ Cambridge, Dept Plant Sci, Cambridge CB3 2EA, England.
[Craine, J. M.] Kansas State Univ, Div Biol, Manhattan, KS 66506 USA.
[Duarte, L.; Fang, J.; Kuehn, I.] Univ Fed Rio Grande do Sul, Dept Ecol, BR-91540000 Porto Alegre, RS, Brazil.
[Durka, W.; Klotz, S.] UFZ Helmholtz Ctr Environm Res, Dept Community Ecol, D-06120 Halle, Germany.
[Elser, J.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA.
[Esser, G.] Univ Giessen, Inst Plant Ecol, D-35392 Giessen, Germany.
[Estiarte, M.; Llusia, J.; Ogaya, R.; Penuelas, J.; Sardans, J.] Univ Autonoma Barcelona, Global Ecol Unit CREAF CEAB CSIC, E-08193 Barcelona, Spain.
[Fagan, W. F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
Peking Univ, Dept Ecol, Beijing 100871, Peoples R China.
[Fernandez-Mendez, F.] Univ Tolima, Dept Ciencias Forestales, Tolima, Colombia.
[Fidelis, A.] Univ Sao Paulo, Dept Ecol, BR-05508900 Sao Paulo, Brazil.
[Flores, O.] Univ Reunion, PVBMT, F-97410 St Pierre, France.
[Ford, H.] Univ York, Dept Biol, Bath, Avon, England.
[Green, W. A.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA.
[Gutierrez, A. G.] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany.
[Hickler, T.] LOEWE Biodivers & Climate Res Ctr, D-60325 Frankfurt, Germany.
[Higgins, S. I.] Goethe Univ Frankfurt, Inst Phys Geog, D-60438 Frankfurt, Germany.
[Hodgson, J. G.] Univ Sheffield, Dept Bot, Sheffield, S Yorkshire, England.
[Jalili, A.] Res Inst Forests & Rangelands, Dept Bot, Tehran, Iran.
[Jansen, S.] Univ Ulm, Inst Systemat Bot & Ecol, D-89081 Ulm, Germany.
[Joly, C. A.] Univ Estadual Campinas, Dept Plant Biol, Campinas, SP, Brazil.
Kenyon Coll, Dept Biol, Gambier, OH 43022 USA.
[Kerkhoff, A. J.] Kenyon Coll, Dept Math, Gambier, OH 43022 USA.
[Kirkup, D.] Royal Bot Gardens, Herbarium Lib Art & Archives, London TW9 3AE, England.
[Kitajima, K.] Univ Florida, Dept Biol, Gainesville, FL USA.
[Kleyer, M.] Carl von Ossietzky Univ Oldenburg, Inst Biol & Environm Sci, D-26129 Oldenburg, Germany.
[Knops, J. M. H.] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA.
[Kramer, K.] Alterra, Vegetat & Landscape Ecol, NL-6700 Wageningen, Netherlands.
[Kurokawa, H.] Tohoku Univ, Grad Sch Life Sci, Sendai, Miyagi 9808578, Japan.
[Laughlin, D.] No Arizona Univ, Sch Forestry, Flagstaff, AZ 86011 USA.
[Lee, T. D.; Weiher, E.] Univ Wisconsin, Dept Biol, Eau Claire, WI 54701 USA.
[Lens, F.] Netherlands Ctr Biodivers Nat, NL-2300 RA Leiden, Netherlands.
[Lloyd, J.] James Cook Univ, Cairns, Qld 4870, Australia.
[Louault, F.; Soussana, J. -F.] INRA, F-63100 Clermont Ferrand, France.
[Manning, P.] Newcastle Univ, Sch Agr, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England.
[Moles, A. T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Sydney, NSW 2031, Australia.
[Nadrowski, K.] Univ Leipzig, Inst Special Bot & Funct Biodiver, D-04103 Leipzig, Germany.
[Naeem, S.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA.
[Niinemets, Ue.] Estonian Univ Life Sci, Dept Plant Physiol, EE-51014 Tartu, Estonia.
[Oleksyn, J.] Polish Acad Sci, Inst Dendrol, PL-62035 Kornik, Poland.
[Onipchenko, V. G.] Moscow MV Lomonosov State Univ, Dept Geobot, Moscow 119991, Russia.
[Onoda, Y.; Wirth, C.] Kyushu Univ, Fac Sci, Dept Biol, Fukuoka 8128581, Japan.
[Ordonez, J.] Wageningen Univ, Law & Governance Grp, NL-6706 KN Wageningen, Netherlands.
[Overbeck, G.] Univ Fed Rio Grande do Sul, Dept Bot, BR-91501970 Porto Alegre, RS, Brazil.
[Ozinga, W. A.] Alterra, Ctr Ecosyst Studies, NL-6700 Wageningen, Netherlands.
[Paula, S.; Pausas, J. G.] Spanish Natl Res Council, Ctr Invest Desertificacio, Valencia 46113, Spain.
[Poorter, H.] Forschungszentrum Julich, D-52428 Julich, Germany.
[Poorter, L.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands.
[Poschlod, P.] Univ Regensburg, Inst Bot, D-93040 Regensburg, Germany.
[Prinzing, A.] Univ Rennes, Lab Ecobio, F-35042 Rennes, France.
[Proulx, R.] Univ Quebec Trois Rivieres, Trois Rivieres, PQ GA9 5H7, Canada.
[Rammig, A.] Potsdam Inst Climate Impact Res, D-14412 Potsdam, Germany.
[Reinsch, S.] Riso Natl Lab Sustainable Energy, Biosyst Div, DK-4000 Roskilde, Denmark.
[Sack, L.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Shiodera, S.] Hokkaido Univ, Ctr Sustainabil Sci, Sapporo, Hokkaido 060080, Japan.
[Siefert, A.] Syracuse Univ, Dept Biol, New York, NY 13244 USA.
[Shipley, B.] Univ Sherbrooke, Dept Biol, Sherbrooke, PQ J1K 2R1, Canada.
[Sosinski, E.] Embrapa Temperate Agr, Lab Environm Planning, BR-96010971 Pelotas, Brazil.
[Swaine, E.] Univ Aberdeen, Aberdeen AB25 2ZD, Scotland.
[Swenson, N.] Michigan State Univ, Dept Plant Biol & Ecol, E Lansing, MI 48824 USA.
[Thompson, K.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England.
[Thornton, P.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA.
[Waldram, M.] Univ Leicester, Dept Geog, Leicester LE1 7RH, Leics, England.
[White, M.] Utah State Univ, Dept Watershed Sci, Logan, UT 84322 USA.
[Wright, S. J.] Smithsonian Trop Res Inst, Balboa 084303092, Panama.
[Yguel, B.] Lab Ecobio Univ Rennes, CNRS, F-35042 Rennes, France.
[Zanne, A. E.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
RP Kattge, J (reprint author), Max Planck Inst Biogeochem, Hans Knoll Str 10, D-07745 Jena, Germany.
EM jkattge@bgc-jena.mpg.de
RI Oleksyn, Jacek/I-4539-2012; Manning, Peter/I-6523-2012; Messier,
Julie/K-3133-2012; Niinemets, Ulo/A-3816-2008; Reichstein,
Markus/A-7494-2011; JOLY, Carlos/C-4523-2012; Duarte,
Leandro/B-6552-2012; Overbeck, Gerhard/D-8695-2013; Leishman,
Michelle/G-9726-2012; Bahn, Michael/I-3536-2013; Cavender-Bares,
Jeannine/K-5716-2013; Phillips, Oliver/A-1523-2011; Wright,
Ian/G-4979-2012; Fidelis, Alessandra/B-9769-2012; Biodiversity & Climate
Res Ctr, BiK-F/C-4266-2012; Garnier, Eric/D-1650-2012; Lloyd,
Jonathan/F-8893-2010; Leadley, Paul/E-4773-2012; Kitajima,
Kaoru/E-8877-2012; Laughlin, Daniel/G-8855-2012; Muller,
Sandra/G-3739-2012; Durka, Walter/E-4667-2010; JOLY, Carlos/H-7925-2012;
Pillar, Valerio/B-9872-2008; Thornton, Peter/B-9145-2012; Craine,
Joseph/D-4569-2009; Gutierrez, Alvaro/C-1979-2009; Mahecha,
Miguel/F-2443-2010; Lens, Frederic/B-8482-2011; Ozinga, Wim/F-1640-2011;
Elser, James/A-7082-2008; Poorter, Hendrik/B-8062-2010; Coomes,
David/H-5630-2011; Swenson, Nathan/A-3514-2012; Higgins,
Steven/A-5138-2012; Jansen, Steven/A-9868-2012; James Cook University,
TESS/B-8171-2012; Soussana, Jean-Francois/P-2094-2016; Atkin,
Owen/C-8415-2009; Hickler, Thomas/S-6287-2016; Kuhn, Ingolf
/B-9756-2009; Sack, Lawren/A-5492-2008; Zaehle, Sonke/C-9528-2017;
Soussana, Jean-Francois/E-2543-2012; Ackerly, David/A-1247-2009; Wright,
Stuart/M-3311-2013; Pausas, Juli/C-5794-2008; Chambers,
Jeffrey/J-9021-2014; Baldocchi, Dennis/A-1625-2009; Onoda,
Yusuke/L-7179-2015; Soudzilovskaia, Nadejda/N-4140-2015; van Bodegom,
Peter/N-8150-2015; U-ID, Kyushu/C-5291-2016; Penuelas,
Josep/D-9704-2011; Estiarte, Marc/G-2001-2016; Kattge, Jens/J-8283-2016;
Moles, Angela/C-3083-2008
OI Flores, Olivier/0000-0002-1416-0449; Lewis, Simon/0000-0002-8066-6851;
Enquist, Brian/0000-0002-6124-7096; Fyllas,
Nikolaos/0000-0002-5651-5578; Sardans, Jordi/0000-0003-2478-0219;
Manning, Peter/0000-0002-7940-2023; Niinemets, Ulo/0000-0002-3078-2192;
Reichstein, Markus/0000-0001-5736-1112; JOLY,
Carlos/0000-0002-7945-2805; Duarte, Leandro/0000-0003-1771-0407;
Overbeck, Gerhard/0000-0002-8716-5136; Leishman,
Michelle/0000-0003-4830-5797; Bahn, Michael/0000-0001-7482-9776;
Phillips, Oliver/0000-0002-8993-6168; Wright, Ian/0000-0001-8338-9143;
Garnier, Eric/0000-0002-9392-5154; Lloyd, Jonathan/0000-0002-5458-9960;
Muller, Sandra/0000-0002-6316-2897; Durka, Walter/0000-0002-6611-2246;
Pillar, Valerio/0000-0001-6408-2891; Thornton,
Peter/0000-0002-4759-5158; Craine, Joseph/0000-0001-6561-3244; Mahecha,
Miguel/0000-0003-3031-613X; Lens, Frederic/0000-0002-5001-0149; Ozinga,
Wim/0000-0002-6369-7859; Elser, James/0000-0002-1460-2155; Poorter,
Hendrik/0000-0001-9900-2433; Swenson, Nathan/0000-0003-3819-9767;
Higgins, Steven/0000-0001-5695-9665; Jansen, Steven/0000-0002-4476-5334;
Cornwell, Will/0000-0003-4080-4073; Harrison, Sandy/0000-0001-5687-1903;
Medlyn, Belinda/0000-0001-5728-9827; Chapin III, F
Stuart/0000-0002-2558-9910; Soussana, Jean-Francois/0000-0002-1932-6583;
Atkin, Owen/0000-0003-1041-5202; Hickler, Thomas/0000-0002-4668-7552;
Kuhn, Ingolf /0000-0003-1691-8249; Sack, Lawren/0000-0002-7009-7202;
Zaehle, Sonke/0000-0001-5602-7956; White, Michael/0000-0002-0238-8913;
Fernandez Mendez, Fernando/0000-0001-8693-790X; Ackerly,
David/0000-0002-1847-7398; Wright, Stuart/0000-0003-4260-5676; Pausas,
Juli/0000-0003-3533-5786; Chambers, Jeffrey/0000-0003-3983-7847;
Baldocchi, Dennis/0000-0003-3496-4919; Onoda,
Yusuke/0000-0001-6245-2342; van Bodegom, Peter/0000-0003-0771-4500;
Penuelas, Josep/0000-0002-7215-0150; Estiarte, Marc/0000-0003-1176-8480;
Kattge, Jens/0000-0002-1022-8469; Moles, Angela/0000-0003-2041-7762
FU DIVERSITAS; IGBP; Global Land Project; UK Natural Environment Research
Council (NERC); French Foundation for Biodiversity Research (FRB); GIS
'Climat, Environnement et Societe' France
FX We would like to thank the subject editor, the publisher for caution and
patience, two anonymous reviewers for supportive comments. The TRY
initiative and database is hosted, developed and maintained at the
Max-Planck-Institute for Biogeochemistry (MPI-BGC) in Jena, Germany. TRY
is or has been supported by DIVERSITAS, IGBP, the Global Land Project,
the UK Natural Environment Research Council (NERC) through its programme
QUEST (Quantifying and Understanding the Earth System), the French
Foundation for Biodiversity Research (FRB), and GIS 'Climat,
Environnement et Societe' France. We wish to thank John Dickie and
Kenwin Liu for making the data from the KEW Seed Information Database
available in the context of the TRY initiative, Alastair Fitter, Henry
Ford and Helen Peat for making the Ecological Flora of the British Isles
available, and Andy Gillison for the VegClass database. We wish to thank
Brad Boyle and the SALVIAS project for building and making available a
global checklist of plant species names, and GBIF (Andrea Hahn) for
making the species occurrence data available. The authors thank the NSF
LTER program DEB 0620652 and the NSF LTREB program DEB 0716587 for
making data on plant traits available.
NR 253
TC 540
Z9 564
U1 77
U2 808
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1354-1013
EI 1365-2486
J9 GLOBAL CHANGE BIOL
JI Glob. Change Biol.
PD SEP
PY 2011
VL 17
IS 9
BP 2905
EP 2935
DI 10.1111/j.1365-2486.2011.02451.x
PG 31
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 800WS
UT WOS:000293399000011
ER
PT J
AU Lessios, HA
AF Lessios, Harilaos A.
TI Speciation Genes in Free-Spawning Marine Invertebrates
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID SEA-URCHIN SPERM; EGG VITELLINE ENVELOPE; GAMETE RECOGNITION PROTEINS;
POSITIVE SELECTION; CHARACTER DISPLACEMENT; RAPID EVOLUTION; SEXUAL
CONFLICT; STRONGYLOCENTROTUS-FRANCISCANUS; REPRODUCTIVE ISOLATION;
ADAPTIVE EVOLUTION
AB Research on speciation of marine organisms has lagged behind that of terrestrial ones, but the study of the evolution of molecules involved in the adhesion of gametes in free-spawning invertebrates is an exception. Here I review the function, species-specificity, and molecular variation of loci coding for bindin in sea urchins, lysin in abalone and their egg receptors, in an effort to assess the degree to which they contribute to the emergence of reproductive isolation during the speciation process. Bindin is a protein that mediates binding of the sperm to the vitelline envelope (VE) of the egg and the fusion of the gametes' membranes, whereas lysin is a protein involved only in binding to the VE. Both of these molecules are important in species recognition by the gametes, but they rarely constitute absolute blocks to interspecific hybridization. Intraspecific polymorphism is high in bindin, but low in lysin. Polymorphism in bindin is maintained by frequency-dependent selection due to sexual conflict arising from the danger of polyspermy under high densities of sperm. Monomorphism in lysin is the result of purifying selection arising from the need for species recognition. Interspecific divergence in lysin is due to strong positive selection, and the same is true for bindin of four out of seven genera of sea urchins studied to date. The differences between the sea urchin genera in the strength of selection can only partially be explained by the hypothesis of reinforcement. The egg receptor for lysin (VERL) is a glycoprotein with 22 repeats, 20 of which have evolved neutrally and homogenized by concerted evolution, whereas the first two repeats are under positive selection. Selection on lysin has been generated by the need to track changes in VERL, permitted by the redundant structure of this molecule. Both lysin and bindin are important in reproductive isolation, probably had a role in speciation, but it is hard to determine whether they meet the strictest criteria of "speciation loci," defined as genes whose differentiation has caused speciation.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
RP Lessios, HA (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama.
EM lessiosh@post.harvard.edu
NR 102
TC 34
Z9 34
U1 0
U2 49
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD SEP
PY 2011
VL 51
IS 3
BP 456
EP 465
DI 10.1093/icb/icr039
PG 10
WC Zoology
SC Zoology
GA 807OF
UT WOS:000293908300013
PM 21700571
ER
PT J
AU Puebla, O
Bermingham, E
Guichard, F
AF Puebla, O.
Bermingham, E.
Guichard, F.
TI Perspective: Matching, Mate Choice, and Speciation
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID SERRANID FISH HYPOPLECTRUS; MARINE SPECIES FLOCK; CORAL-REEF FISHES;
SEXUAL SELECTION; SYMPATRIC SPECIATION; COLOR MORPHS; EVOLUTION;
FEMALES; MODELS
AB Matching was developed in the 1960s to match such entities as residents and hospitals, colleges and students, or employers and employees. This approach is based on "preference lists," whereby each participant ranks potential partners according to his/her preferences and tries to match with the highest-ranking partner available. Here, we discuss the implications of matching for the study of mate choice and speciation. Matching differs from classic approaches in several respects, most notably because under this theoretical framework, the formation of mating pairs is context-dependant (i.e., it depends on the configuration of pairings in the entire population), because the stability of mating pairs is considered explicitly, and because mate choice is mutual. The use of matching to study mate choice and speciation is not merely a theoretical curiosity; its application can generate counter-intuitive predictions and lead to conclusions that differ fundamentally from classic theories about sexual selection and speciation. For example, it predicts that when mate choice is mutual and the stability of mating pairs is critical for successful reproduction, sympatric speciation is a robust evolutionary outcome. Yet the application of matching to the study of mate choice and speciation has been largely dominated by theoretical studies. We present the hamlets, a group of brightly colored Caribbean coral reef fishes in the genus Hypoplectrus (Serranidae), as a particularly apt system to test empirically specific predictions generated by the application of matching to mate choice and speciation.
C1 [Puebla, O.; Bermingham, E.] Smithsonian Trop Res Inst, Panama City, Panama.
[Bermingham, E.; Guichard, F.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
RP Puebla, O (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama.
EM oscar.puebla@mail.mcgill.ca
RI Guichard, Frederic/B-6188-2015
OI Guichard, Frederic/0000-0002-7369-482X
FU Marine Science Network
FX Marine Science Network.
NR 26
TC 8
Z9 8
U1 1
U2 17
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD SEP
PY 2011
VL 51
IS 3
BP 485
EP 491
DI 10.1093/icb/icr025
PG 7
WC Zoology
SC Zoology
GA 807OF
UT WOS:000293908300016
PM 21624930
ER
PT J
AU Hrcek, J
Miller, SE
Quicke, DLJ
Smith, MA
AF Hrcek, Jan
Miller, Scott E.
Quicke, Donald L. J.
Smith, M. Alex
TI Molecular detection of trophic links in a complex insect host-parasitoid
food web
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE cytochrome oxidase I; Diptera; Hymenoptera; immature stages;
Lepidoptera; Papua New Guinea
ID POLYMERASE-CHAIN-REACTION; DNA BARCODES; TROPICAL FOREST; NEW-GUINEA;
HERBIVOROUS INSECTS; MULTIPLEX PCR; CEREAL APHIDS; FLIES DIPTERA;
IDENTIFICATION; HYMENOPTERA
AB Previously, host-parasitoid links have been unveiled almost exclusively by time-intensive rearing, while molecular methods were used only in simple agricultural host-parasitoid systems in the form of species-specific primers. Here, we present a general method for the molecular detection of these links applied to a complex caterpillar-parasitoid food web from tropical rainforest of Papua New Guinea. We DNA barcoded hosts, parasitoids and their tissue remnants and matched the sequences to our extensive library of local species. We were thus able to match 87% of host sequences and 36% of parasitoid sequences to species and infer subfamily or family in almost all cases. Our analysis affirmed 93 hitherto unknown trophic links between 37 host species from a wide range of Lepidoptera families and 46 parasitoid species from Hymenoptera and Diptera by identifying DNA sequences for both the host and the parasitoid involved in the interaction. Molecular detection proved especially useful in cases where distinguishing host species in caterpillar stage was difficult morphologically, or when the caterpillar died during rearing. We have even detected a case of extreme parasitoid specialization in a pair of Choreutis species that do not differ in caterpillar morphology and ecology. Using the molecular approach outlined here leads to better understanding of parasitoid host specificity, opens new possibilities for rapid surveys of food web structure and allows inference of species associations not already anticipated.
C1 [Hrcek, Jan] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic.
[Hrcek, Jan] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic.
[Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Quicke, Donald L. J.] Univ London Imperial Coll Sci Technol & Med, Div Biol, Ascot SL5 7PY, Berks, England.
[Quicke, Donald L. J.] Nat Hist Museum, Dept Entomol, London SW7 5DB, England.
[Smith, M. Alex] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
[Smith, M. Alex] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada.
RP Hrcek, J (reprint author), Univ S Bohemia, Fac Sci, Branisovska 31, Ceske Budejovice 37005, Czech Republic.
EM janhrcek@gmail.com
RI Smith, M Alex/B-4468-2013; Hrcek, Jan/D-7335-2015;
OI Smith, M Alex/0000-0002-8650-2575; Hrcek, Jan/0000-0003-0711-6447;
Quicke, Donald/0000-0003-4471-6775; Miller, Scott/0000-0002-4138-1378
FU US National Science Foundation [DEB 0841885, 0816749, 0515678]; Czech
Science Foundation [206/08/H044, 206/09/0115, P505/10/0673]; Czech
Ministry of Education [LC06073, ME9082, MSM6007665801]; Grant Agency of
the University of South Bohemia [GAJU 136/2010/P]; NSF; Government of
Canada through Genome Canada; Ontario Genomics Institute
[2008-0GI-ICI-03]
FX We thank New Guinea Binatang Research Center parataxonomists, village
assistants, Vojtech Novotny, Lauren Helgen, Karolyn Darrow, Kristyna
Hrckova, Toko Pagi, David Pollock and Legi Sam for technical assistance
and general support. Lepidoptera taxonomy was assisted by Jeremy
Holloway, Jadranka Rota, Michael Shaffer, Tosio Kumata, Issei Ohshima
and others acknowledged in (Craft et al. 2010). Parasitoids were
identified by: Kees van Achterberg (Macrocentrinae), Celso Oliveira
Azevedo (Bethylidae), Yves Braet (Orgilinae), Michael W. Gates
(Chalcidoidea), Ian D. Gauld (Ichneumonidae), Donald L.J. Quicke
(Rogadinae), Michael J. Sharkey (Agathidinae), Hiroshi Shima
(Tachinidae), David Wahl (Ichneumonidae), James B. Whitfield
(Microgastrinae, Cardiochilinae) and Dicky Sick Ki Yu (Cheloninae). This
study is based on work supported by the US National Science Foundation
(DEB 0841885, 0816749, 0515678), Czech Science Foundation (206/08/H044,
206/09/0115 and P505/10/0673), Czech Ministry of Education (LC06073,
ME9082 and MSM6007665801) and Grant Agency of the University of South
Bohemia (GAJU 136/2010/P). The barcode library of local fauna was built
from NSF-funded research since 1995 in collaboration with Vojtech
Novotny, George Weiblen and Yves Basset. We thank Paul Hebert and all of
our colleagues at the Biodiversity Institute of Ontario for their
assistance and support. This Project was funded by the Government of
Canada through Genome Canada and the Ontario Genomics Institute
(2008-0GI-ICI-03).
NR 53
TC 61
Z9 64
U1 2
U2 65
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 SEP
PY 2011
VL 11
IS 5
BP 786
EP 794
DI 10.1111/j.1755-0998.2011.03016.x
PG 9
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 807QW
UT WOS:000293915800005
PM 21535428
ER
PT J
AU Ahlering, MA
Hailer, F
Roberts, MT
Foley, C
AF Ahlering, Marissa A.
Hailer, Frank
Roberts, Melissa T.
Foley, Charles
TI A simple and accurate method to sex savannah, forest and asian elephants
using noninvasive sampling techniques
SO MOLECULAR ECOLOGY RESOURCES
LA English
DT Article
DE Elephas maximus; Loxodonta a. africana; Loxodonta a. cyclotis; molecular
sexing; noninvasive
ID DNA; POPULATION; AFRICANA; NUCLEAR; TISSUE; TIME
AB We report the development of a reliable and efficient method for molecular sexing of all extant elephant taxa. We developed primers that amplify two short Y-specific fragments (SRY1 and AMELY2) and one longer X-specific fragment (PLP1), developed from elephant sequences in one multiplex PCR. All fragments were designed to be short (<200 basepairs) for use with degraded DNA and to be 50 basepairs apart to optimize visualization on agarose gels or as electropherograms. The multiplex PCR method matched sexes for at least 97.9% of the noninvasive savannah elephant samples and produced the expected female/male banding patterns for 14 African forest and 11 Asian elephant samples. We found this method to be more robust, efficient and less prone to contamination than previously developed sexing methods for elephants.
C1 [Ahlering, Marissa A.; Hailer, Frank; Roberts, Melissa T.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
[Foley, Charles] Wildlife Conservat Soc, Tanzania Program, Arusha, Tanzania.
RP Ahlering, MA (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,POB 37012, Washington, DC 20013 USA.
EM mahlering@tnc.org
RI Hailer, Frank/C-9114-2012
OI Hailer, Frank/0000-0002-2340-1726
FU Smithsonian Center for Conservation and Evolutionary Genetics;
Smithsonian Restricted Endowment Funds; Smithsonian Postdoctoral
Fellowship Program
FX For provision of samples we thank S. Dumnui, M. Limpoka, C. M. Wemmer,
A. Alfonso, F. Dallmeier and Linus Munishi. We thank the staff at the
African Conservation Centre and the Wildlife Conservation Society for
help with sample collection in the field. C. Foley thanks the Tanzania
Wildlife Research Institute and the Tanzania Commission for Science and
Technology for permission to work in Tarangire. Rob Fleischer and Jesus
Maldonado provided generous support and helpful discussions. Financial
support came from the Smithsonian Center for Conservation and
Evolutionary Genetics, the Smithsonian Restricted Endowment Funds, and
the Smithsonian Postdoctoral Fellowship Program.
NR 16
TC 7
Z9 7
U1 0
U2 8
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 SEP
PY 2011
VL 11
IS 5
BP 831
EP 834
DI 10.1111/j.1755-0998.2011.03030.x
PG 4
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 807QW
UT WOS:000293915800011
PM 21635697
ER
PT J
AU Mello, MAR
Marquitti, FMD
Guimaraes, PR
Kalko, EKV
Jordano, P
de Aguiar, MAM
AF Ribeiro Mello, Marco Aurelio
Darcie Marquitti, Flavia Maria
Guimaraes, Paulo R., Jr.
Viktoria Kalko, Elisabeth Klara
Jordano, Pedro
Martinez de Aguiar, Marcus Aloizio
TI The modularity of seed dispersal: differences in structure and
robustness between bat- and bird-fruit networks
SO OECOLOGIA
LA English
DT Article
DE Complex networks; Ecosystem services; Food webs; Guilds; Mutualisms
ID ANIMAL MUTUALISTIC NETWORKS; POLLINATION NETWORKS; BIODIVERSITY;
NESTEDNESS; COMMUNITY; PATTERNS; ECOLOGY; PLANTS; PHYLLOSTOMIDAE;
SPECIALIZATION
AB In networks of plant-animal mutualisms, different animal groups interact preferentially with different plants, thus forming distinct modules responsible for different parts of the service. However, what we currently know about seed dispersal networks is based only on birds. Therefore, we wished to fill this gap by studying bat-fruit networks and testing how they differ from bird-fruit networks. As dietary overlap of Neotropical bats and birds is low, they should form distinct mutualistic modules within local networks. Furthermore, since frugivory evolved only once among Neotropical bats, but several times independently among Neotropical birds, greater dietary overlap is expected among bats, and thus connectance and nestedness should be higher in bat-fruit networks. If bat-fruit networks have higher nestedness and connectance, they should be more robust to extinctions. We analyzed 1 mixed network of both bats and birds and 20 networks that consisted exclusively of either bats (11) or birds (9). As expected, the structure of the mixed network was both modular (M = 0.45) and nested (NODF = 0.31); one module contained only birds and two only bats. In 20 datasets with only one disperser group, bat-fruit networks (NODF = 0.53 +/- A 0.09, C = 0.30 +/- A 0.11) were more nested and had a higher connectance than bird-fruit networks (NODF = 0.42 +/- A 0.07, C = 0.22 +/- A 0.09). Unexpectedly, robustness to extinction of animal species was higher in bird-fruit networks (R = 0.60 +/- A 0.13) than in bat-fruit networks (R = 0.54 +/- A 0.09), and differences were explained mainly by species richness. These findings suggest that a modular structure also occurs in seed dispersal networks, similar to pollination networks. The higher nestedness and connectance observed in bat-fruit networks compared with bird-fruit networks may be explained by the monophyletic evolution of frugivory in Neotropical bats, among which the diets of specialists seem to have evolved from the pool of fruits consumed by generalists.
C1 [Ribeiro Mello, Marco Aurelio; Viktoria Kalko, Elisabeth Klara] Univ Ulm, Inst Expt Okol, D-89069 Ulm, Germany.
[Darcie Marquitti, Flavia Maria] Univ Estadual Campinas, Programa Posgrad Ecol, BR-13083970 Campinas, SP, Brazil.
[Guimaraes, Paulo R., Jr.] Univ Sao Paulo, Dept Ecol, BR-05508900 Sao Paulo, Brazil.
[Guimaraes, Paulo R., Jr.; Jordano, Pedro] CSIC, Integrat Ecol Grp, Estac Bio Donana, E-41080 Seville, Spain.
[Viktoria Kalko, Elisabeth Klara] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Martinez de Aguiar, Marcus Aloizio] Univ Estadual Campinas, Inst Fis Gleb Wataghin, BR-13083970 Campinas, SP, Brazil.
RP Mello, MAR (reprint author), Univ Ulm, Inst Expt Okol, Biol 3,Albert Einstein Allee 11, D-89069 Ulm, Germany.
EM marmello@gmail.com
RI Mello, Marco/B-1095-2008; Darcie Marquitti, Flavia Maria/B-2697-2013;
Guimaraes, Paulo/E-1915-2016; de Aguiar, Marcus/C-9137-2012; CSIC, EBD
Donana/C-4157-2011; Guimaraes-Junior, Paulo/M-1298-2016; Inst. of
Physics, Gleb Wataghin/A-9780-2017; Guimaraes, Paulo/B-1099-2008;
Jordano, Pedro/A-5162-2008; Jordano, Pedro/B-6678-2014
OI Mello, Marco/0000-0002-9098-9427; Darcie Marquitti, Flavia
Maria/0000-0003-0510-3992; de Aguiar, Marcus/0000-0003-1379-7568; CSIC,
EBD Donana/0000-0003-4318-6602; Jordano, Pedro/0000-0003-2142-9116;
Jordano, Pedro/0000-0003-2142-9116
FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (Brazil)
[2006/00265-0]; Alexander von Humboldt Foundation (Germany) [1134644];
Deutsche Forschungsgemeinschaft (Germany); Consejo Superior de
Investigaciones Cientificas (Spain)
FX We are especially grateful to all people who made their data available
in papers, monographs or databases. Carsten Dormann, Mario Almeida-Neto,
Nico Bluthgen, Roger Guimera and Vladimir Batagelj helped us use their
network software. Theodore Fleming made invaluable suggestions on an
early version of this manuscript. Diego Vazquez created the Interaction
Web Database (http://www.nceas.ucsb.edu/interactionweb/), from which we
took some datasets. Many colleagues, especially Wibke Thies, helped to
complement the 'Kalko BCI dataset' after its first publication in 2004.
Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (Brazil) funded
this project by giving Grants to M. A. R. M. (2006/00265-0), F. M. D.
M., M. A. M. A. and P. R. G. M. A. R. M. was also supported by the
Alexander von Humboldt Foundation (Germany, 1134644). E. K. V. K. was
supported by the Deutsche Forschungsgemeinschaft (Germany), and P.J. by
the Consejo Superior de Investigaciones Cientificas (Spain). Experiments
comply with the current laws of Germany, Brazil and Spain.
NR 53
TC 38
Z9 40
U1 7
U2 66
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD SEP
PY 2011
VL 167
IS 1
BP 131
EP 140
DI 10.1007/s00442-011-1984-2
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 807QE
UT WOS:000293914000013
PM 21479592
ER
PT J
AU Shefferson, RP
McCormick, MK
Whigham, DF
O'Neill, JP
AF Shefferson, Richard P.
McCormick, Melissa K.
Whigham, Dennis F.
O'Neill, John P.
TI Life history strategy in herbaceous perennials: inferring demographic
patterns from the aboveground dynamics of a primarily subterranean,
myco-heterotrophic orchid
SO OIKOS
LA English
DT Article
ID CAPTURE-RECAPTURE MODELS; POPULATION-GROWTH RATE; LADYS SLIPPER ORCHIDS;
ENVIRONMENTAL HETEROGENEITY; EVOLUTIONARY ECOLOGY; GENUS CYPRIPEDIUM;
MYCORRHIZAL FUNGI; MARKED ANIMALS; CLONAL PLANT; SURVIVAL
AB Myco-heterotrophs are non-photosynthetic plants that parasitize mycorrhizal fungi for their nutritional requirements, especially carbon. Because green plants sprout both to photosynthesize and to reproduce, the lack of photosynthesis in myco-heterotrophs suggests that these plants need only to sprout to reproduce. Further, they may be long-lived, with fitness favoring high, stable survival over frequent reproduction and leading to size-biased reproduction. We hypothesized that sprouting would be rare and would always lead to flowering in a ten-year monitoring study of a myco-heterotrophic plant, the autumn coral root Corallorhiza odontorhiza. We also postulated that these plants would exhibit strong size-based flowering patterns. We tested these hypotheses by parameterizing a variety of mark-recapture models of survival, fecundity, and demographic transitions among two life history stages: flowering and non-sprouting (vegetatively dormant). We further developed and tested novel models estimating the influence of reproduction on demographic transitions one, two, and three years after flowering. Our results suggested that this population is typically subterranean, with only a small proportion of living plants actually sprouting in any given year. Plants typically flowered and fruited when they sprouted (flowering frequency > 0.99), supporting our first hypothesis that sprouting occurs only in concert with reproduction. We also found that reproduction was associated with long-term reproductive demographic impacts-plants that flowered more in the past three years were more likely to continue doing so than those that flowered only once. Our use of 'memory' mark-recapture models, in which transitions across years are allowed to vary with demographic events occurring across several previous years, proved a powerful means of testing for their long-term impacts of reproductive events.
C1 [Shefferson, Richard P.] Univ Georgia, Odum Sch Ecol, Athens, GA 30601 USA.
[McCormick, Melissa K.; Whigham, Dennis F.; O'Neill, John P.] Smithsonian Environm Res Ctr, Plant Ecol Lab, Edgewater, MD 21037 USA.
RP Shefferson, RP (reprint author), Univ Georgia, Odum Sch Ecol, 140 E Green St, Athens, GA 30601 USA.
EM dormancy@uga.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU Smithsonian Environmental Research Center; Smithsonian Post-doctoral
Fellowship program
FX We thank the Odum School of Ecology at the Univ. of Georgia, Athens, GA,
USA, the Microbial Ecology and Wildlife Ecology labs at the Forestry and
Forest Products Research Inst., Tsukuba, Japan, and the National Science
Foundation (DEB-0316523) for providing logistical support during the
writing of this manuscript. Support for the long-term monitoring of the
population has been provided by the Smithsonian Environmental Research
Center and the Smithsonian Post-doctoral Fellowship program. Thanks are
also extended to Hanne Rasmussen who initiated the population study
during her tenure at SERC as a Senior Smithsonian Post-doctoral Fellow.
NR 61
TC 8
Z9 8
U1 1
U2 27
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 SEP
PY 2011
VL 120
IS 9
BP 1291
EP 1300
DI 10.1111/j.1600-0706.2011.19130.x
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 806GA
UT WOS:000293793100002
ER
PT J
AU Gorchov, DL
Thompson, E
O'Neill, J
Whigham, D
Noe, DA
AF Gorchov, David L.
Thompson, Emily
O'Neill, Jay
Whigham, Dennis
Noe, Douglas A.
TI Treefall gaps required for establishment, but not survival, of invasive
Rubus phoenicolasius in deciduous forest, Maryland, USA
SO PLANT SPECIES BIOLOGY
LA English
DT Article
DE classification and regression tree analysis; invasive non-native plants;
recruitment; Rubus phoenicolasius; seedling establishment; shade
tolerance
ID TROPICAL RAIN-FOREST; PHOTON FLUX-DENSITY; REGRESSION TREES; PLANT
INVASIONS; DISTURBANCE; INVASIBILITY; DIVERSITY; LIGHT; UNDERSTORY;
ABUNDANCE
AB Although plant invasions are often associated with disturbance, localized disturbances can promote invasion either by: (i) creating sites where individuals establish; or (ii) enabling an invader to colonize the entire stand. The former is expected when both establishment and survival to reproductive age require disturbed conditions, whereas the latter should occur in systems when either establishment or survival are limited to disturbed sites. We investigated the role of localized disturbance, specifically treefalls, in the invasion of the Asian Rubus phoenicolasius in a deciduous forest in Maryland, USA. We investigated the density and demography of R. phoenicolasius in treefall gaps of various sizes, but identical age to non-gap areas, using Classification and Regression Tree (CART) analyses to identify the most important predictors. To explore how the demography of established individuals responds to disturbed versus undisturbed conditions, we carried out a garden experiment with three different levels of shade (5, 12 and 22% full sun). We found vegetative and sexual reproduction, and seedling establishment, to be limited to large gaps in an old stand, but not in a stand in an earlier age of succession. However, in the garden experiment, established plants were able to survive and grow under all shade treatments. These findings indicate that R. phoenicolasius requires disturbances such as treefalls to establish in forests, but established plants will survive canopy closure, leading to stand-wide invasion. Managers should be able to prevent invasion, however, by inspecting large gaps for new recruits every 3 years.
C1 [Gorchov, David L.] Miami Univ, Dept Bot, Oxford, OH 45056 USA.
[Noe, Douglas A.] Miami Univ, Dept Stat, Oxford, OH 45056 USA.
[Gorchov, David L.; O'Neill, Jay; Whigham, Dennis] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Thompson, Emily] Coll William & Mary, Williamsburg, VA 23186 USA.
RP Gorchov, DL (reprint author), Miami Univ, Dept Bot, Oxford, OH 45056 USA.
EM gorchodl@muohio.edu
OI Whigham, Dennis/0000-0003-1488-820X
FU Smithsonian Institution; SERC REU
FX Miami University provided a Faculty Improvement Leave and the
Smithsonian Institution provided a Senior Fellowship that enabled D. L.
Gorchov to carry out this research at the Smithsonian Environmental
Research Center (SERC). Emily Thompson was supported by a SERC REU
fellowship. The following SERC laboratories and individuals provided
valuable guidance, assistance and equipment: Plant Ecology (Anne Innis,
Melissa McCormick, Ronald van den Heuvel), Forest Ecology (Jess Parker,
Michelle Berger, Jeni Keisman), Phytoplankton for providing the quantum
sensor and datalogger (Chuck Gallegos, Sam Benson, Sharyn Hedrick) and
Biocomplexity (Anne Chamberlain). Brianna Smith recorded tree damage
following the June 2002 storm, essential for the selection of the study
plots, and Brian York assisted with fieldwork.
NR 47
TC 9
Z9 9
U1 0
U2 34
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0913-557X
J9 PLANT SPEC BIOL
JI Plant Spec. Biol.
PD SEP
PY 2011
VL 26
IS 3
BP 221
EP 234
DI 10.1111/j.1442-1984.2011.00317.x
PG 14
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 808RU
UT WOS:000293996900004
ER
PT J
AU Kloc, B
Rapaport, LG
Warneke, M
Ballou, J
Mickelberg, J
AF Kloc, B.
Rapaport, L. G.
Warneke, M.
Ballou, J.
Mickelberg, J.
TI MOTHERS PREFER HELPERS: BIRTH SEX RATIO ADJUSTMENT IN CAPTIVE
CALLITRICHID
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 34th Annual Meeting of the American-Society-of-Primatologists
CY SEP 16-19, 2011
CL Austin, TX
SP Amer Soc Primatol
C1 [Kloc, B.; Rapaport, L. G.] Clemson Univ, Dept Biol Sci, Clemson, SC 29632 USA.
[Warneke, M.] Chicago Zool Soc, Chicago, IL USA.
[Ballou, J.; Mickelberg, J.] Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 7
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD SEP
PY 2011
VL 73
SU 1
MA 9
BP 35
EP 35
PG 1
WC Zoology
SC Zoology
GA 805XO
UT WOS:000293764600010
ER
PT J
AU Power, ML
Behler, JE
Evans, S
Williams, LE
AF Power, M. L.
Behler, J. E.
Evans, S.
Williams, L. E.
TI COMPOSITION OF THE MILK OF LABORATORY-HOUSED OWL MONKEYS
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Meeting Abstract
CT 34th Annual Meeting of the American-Society-of-Primatologists
CY SEP 16-19, 2011
CL Austin, TX
SP Amer Soc Primatol
C1 [Power, M. L.; Behler, J. E.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Nutr Lab, Washington, DC 20013 USA.
NR 0
TC 0
Z9 0
U1 0
U2 6
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD SEP
PY 2011
VL 73
SU 1
MA 66
BP 52
EP 52
PG 1
WC Zoology
SC Zoology
GA 805XO
UT WOS:000293764600061
ER
PT J
AU Cleveland, CC
Townsend, AR
Taylor, P
Alvarez-Clare, S
Bustamante, MMC
Chuyong, G
Dobrowski, SZ
Grierson, P
Harms, KE
Houlton, BZ
Marklein, A
Parton, W
Porder, S
Reed, SC
Sierra, CA
Silver, WL
Tanner, EVJ
Wieder, WR
AF Cleveland, Cory C.
Townsend, Alan R.
Taylor, Philip
Alvarez-Clare, Silvia
Bustamante, Mercedes M. C.
Chuyong, George
Dobrowski, Solomon Z.
Grierson, Pauline
Harms, Kyle E.
Houlton, Benjamin Z.
Marklein, Alison
Parton, William
Porder, Stephen
Reed, Sasha C.
Sierra, Carlos A.
Silver, Whendee L.
Tanner, Edmund V. J.
Wieder, William R.
TI Relationships among net primary productivity, nutrients and climate in
tropical rain forest: a pan-tropical analysis
SO ECOLOGY LETTERS
LA English
DT Review
DE Carbon cycle; climate; decomposition; meta-analysis; nitrogen; nutrient
limitation; phosphorus; primary production; tropical forest
ID LEAF-LITTER DECOMPOSITION; N-P STOICHIOMETRY; PHOSPHORUS LIMITATION;
TERRESTRIAL ECOSYSTEMS; AMAZONIAN FORESTS; NITROGEN-RETENTION;
REGRESSION TREES; GLOBAL PATTERNS; SOIL; AVAILABILITY
AB Tropical rain forests play a dominant role in global biosphere-atmosphere CO(2) exchange. Although climate and nutrient availability regulate net primary production (NPP) and decomposition in all terrestrial ecosystems, the nature and extent of such controls in tropical forests remain poorly resolved. We conducted a meta-analysis of carbon-nutrient-climate relationships in 113 sites across the tropical forest biome. Our analyses showed that mean annual temperature was the strongest predictor of aboveground NPP (ANPP) across all tropical forests, but this relationship was driven by distinct temperature differences between upland and lowland forests. Within lowland forests (< 1000 m), a regression tree analysis revealed that foliar and soil-based measurements of phosphorus (P) were the only variables that explained a significant proportion of the variation in ANPP, although the relationships were weak. However, foliar P, foliar nitrogen (N), litter decomposition rate (k), soil N and soil respiration were all directly related with total surface (0-10 cm) soil P concentrations. Our analysis provides some evidence that P availability regulates NPP and other ecosystem processes in lowland tropical forests, but more importantly, underscores the need for a series of large-scale nutrient manipulations - especially in lowland forests - to elucidate the most important nutrient interactions and controls.
C1 [Cleveland, Cory C.] Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA.
[Townsend, Alan R.] Univ Colorado, Dept Ecol & Evolutionary Biol, Environm Studies Program, Boulder, CO 80309 USA.
[Townsend, Alan R.; Taylor, Philip; Wieder, William R.] Univ Colorado, INSTAAR, Boulder, CO 80309 USA.
[Alvarez-Clare, Silvia] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Alvarez-Clare, Silvia] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL 32611 USA.
[Bustamante, Mercedes M. C.] Univ Brasilia, Dept Ecol, Brasilia, DF, Brazil.
[Chuyong, George] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon.
[Dobrowski, Solomon Z.] Univ Montana, Dept Forest Management, Missoula, MT 59812 USA.
[Grierson, Pauline] Univ Western Australia, Sch Plant Biol M090, Crawley, WA 6016, Australia.
[Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Panama.
[Houlton, Benjamin Z.; Marklein, Alison] Univ Calif Davis, Dept Land Air & Water Resources, Davis, CA 95616 USA.
[Parton, William] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA.
[Porder, Stephen] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA.
[Reed, Sasha C.] US Geol Survey, SW Biol Sci Ctr, Moab, UT 84532 USA.
[Sierra, Carlos A.] Max Planck Inst Biogeochem, Dept Biol Proc, D-07745 Jena, Germany.
[Silver, Whendee L.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England.
RP Cleveland, CC (reprint author), Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA.
EM cory.cleveland@umontana.edu
RI Sierra, Carlos/A-5694-2009; Grierson, Pauline/A-9240-2008; Silver,
Whendee/H-1118-2012; Marklein, Alison/I-3255-2016;
OI Sierra, Carlos/0000-0003-0009-4169; Grierson,
Pauline/0000-0003-2135-0272; Marklein, Alison/0000-0002-0865-5816;
Bustamante, Mercedes/0000-0003-1008-452X; WIEDER,
WILLIAM/0000-0001-7116-1985
FU National Science Foundation; University of California; State of
California; A.W. Mellon foundation
FX This paper is a contribution from the Tropical Nutrient Limitation
working group at the National Center for Ecological Analysis and
Synthesis (funded by the National Science Foundation), the University of
California and the State of California. We thank the staff of NCEAS for
logistical and technical support, R. Rawlinson for assistance with
figure production and the anonymous many others that helped locate data
and assemble the database. We are also grateful to three anonymous
referees and to D. Hooper for valuable comments on the submitted
manuscript. C.C. wishes to acknowledge financial support from the A.W.
Mellon foundation through a grant to investigate nutrient cycling in
tropical forests.
NR 97
TC 132
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U1 16
U2 228
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD SEP
PY 2011
VL 14
IS 9
BP 939
EP 947
DI 10.1111/j.1461-0248.2011.01658.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 804BI
UT WOS:000293628300014
PM 21749602
ER
PT J
AU Mueller, T
Olson, KA
Dressler, G
Leimgruber, P
Fuller, TK
Nicolson, C
Novaro, AJ
Bolgeri, MJ
Wattles, D
DeStefano, S
Calabrese, JM
Fagan, WF
AF Mueller, Thomas
Olson, Kirk A.
Dressler, Gunnar
Leimgruber, Peter
Fuller, Todd K.
Nicolson, Craig
Novaro, Andres J.
Bolgeri, Maria J.
Wattles, David
DeStefano, Stephen
Calabrese, Justin M.
Fagan, William F.
TI How landscape dynamics link individual- to population-level movement
patterns: a multispecies comparison of ungulate relocation data
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Animal movements; landscape dynamics; migration; NDVI; relocation data;
ungulates
ID GAZELLES PROCAPRA-GUTTUROSA; ANIMAL MOVEMENT; MIGRATION; SATELLITE;
DISTRIBUTIONS; ECOLOGY; ENVIRONMENTS; PRODUCTIVITY; SERENGETI; MAMMALS
AB Aim To demonstrate how the interrelations of individual movements form large-scale population-level movement patterns and how these patterns are associated with the underlying landscape dynamics by comparing ungulate movements across species.
Locations Arctic tundra in Alaska and Canada, temperate forests in Massachusetts, Patagonian Steppes in Argentina, Eastern Steppes in Mongolia.
Methods We used relocation data from four ungulate species (barren-ground caribou, Mongolian gazelle, guanaco and moose) to examine individual movements and the interrelation of movements among individuals. We applied and developed a suite of spatial metrics that measure variation in movement among individuals as population dispersion, movement coordination and realized mobility. Taken together, these metrics allowed us to quantify and distinguish among different large-scale population-level movement patterns such as migration, range residency and nomadism. We then related the population-level movement patterns to the underlying landscape vegetation dynamics via long-term remote sensing measurements of the temporal variability, spatial variability and unpredictability of vegetation productivity.
Results Moose, which remained in sedentary home ranges, and guanacos, which were partially migratory, exhibited relatively short annual movements associated with landscapes having very little broad-scale variability in vegetation. Caribou and gazelle performed extreme long-distance movements that were associated with broad-scale variability in vegetation productivity during the peak of the growing season. Caribou exhibited regular seasonal migration in which individuals were clustered for most of the year and exhibited coordinated movements. In contrast, gazelle were nomadic, as individuals were independently distributed and moved in an uncoordinated manner that relates to the comparatively unpredictable (yet broad-scale) vegetation dynamics of their landscape.
Main conclusions We show how broad-scale landscape unpredictability may lead to nomadism, an understudied type of long-distance movement. In contrast to classical migration where landscapes may vary at broad scales but in a predictable manner, long-distance movements of nomadic individuals are uncoordinated and independent from other such individuals. Landscapes with little broad-scale variability in vegetation productivity feature smaller-scale movements and allow for range residency. Nomadism requires distinct integrative conservation strategies that facilitate long-distance movements across the entire landscape and are not limited to certain migration corridors.
C1 [Mueller, Thomas; Dressler, Gunnar; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Mueller, Thomas; Leimgruber, Peter; Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Olson, Kirk A.; Fuller, Todd K.; Nicolson, Craig] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA.
[Novaro, Andres J.] Argentine Res Council, RA-8371 Junin De Los Andes, Neuqen, Argentina.
[Novaro, Andres J.] Wildlife Conservat Soc, Patagonian & Andean Steppe Program, RA-8371 Junin De Los Andes, Neuqen, Argentina.
[Bolgeri, Maria J.] Argentine Sci Agcy, RA-8371 Junin De Los Andes, Neuqen, Argentina.
[Bolgeri, Maria J.] Wildlife Conservat Soc, Patagonian & Andean Steppe Program, RA-8371 Junin De Los Andes, Neuqen, Argentina.
[Wattles, David; DeStefano, Stephen] Univ Massachusetts, US Geol Survey, Massachusetts Cooperat Fish & Wildlife Res Unit, Amherst, MA 01003 USA.
[Calabrese, Justin M.] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany.
RP Mueller, T (reprint author), Univ Maryland, Dept Biol, BioPsych Bldg,Room 3205, College Pk, MD 20742 USA.
EM muellert@gmail.com
RI Calabrese, Justin/B-9131-2012; Mueller, Thomas/A-1740-2014; Leimgruber,
Peter/O-1304-2015
OI Mueller, Thomas/0000-0001-9305-7716; Leimgruber,
Peter/0000-0002-3682-0153
FU National Science Foundation [DEB-0608224, DEB-0743557, DEB-0743385];
Massachusetts Division of Fisheries and Wildlife; Massachusetts
Department of Conservation and Recreation; Science Agency of Argentina
[34120]; Wildlife Conservation Society
FX Funding was provided in part by the National Science Foundation
(DEB-0608224, DEB-0743557, DEB-0743385), the Massachusetts Division of
Fisheries and Wildlife and the Massachusetts Department of Conservation
and Recreation, Science Agency of Argentina (PICT grant 34120) and the
Wildlife Conservation Society.
NR 50
TC 47
Z9 50
U1 12
U2 122
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1466-822X
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD SEP
PY 2011
VL 20
IS 5
BP 683
EP 694
DI 10.1111/j.1466-8238.2010.00638.x
PG 12
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 805BN
UT WOS:000293701300004
ER
PT J
AU Edgar, GJ
Banks, SA
Bessudo, S
Cortes, J
Guzman, HM
Henderson, S
Martinez, C
Rivera, F
Soler, G
Ruiz, D
Zapata, FA
AF Edgar, Graham J.
Banks, Stuart A.
Bessudo, Sandra
Cortes, Jorge
Guzman, Hector M.
Henderson, Scott
Martinez, Camilo
Rivera, Fernando
Soler, German
Ruiz, Diego
Zapata, Fernando A.
TI Variation in reef fish and invertebrate communities with level of
protection from fishing across the Eastern Tropical Pacific seascape
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE Colombia; coral reef; Costa Rica; Ecuador; effects of fishing;
Galapagos; marine reserve; Panama; UNESCO World Heritage
ID NINO-SOUTHERN OSCILLATION; MARINE RESERVE PROTECTION; CORAL-REEFS;
EL-NINO; POPULATION-DYNAMICS; GALAPAGOS-ISLANDS; MASS MORTALITIES;
SEA-URCHINS; FOOD WEBS; AREAS
AB Aim To quantify general differences in reef community structure between well-enforced and poorly enforced marine protected areas (MPAs) and fished sites across the Eastern Tropical Pacific (ETP) regional seascape
Location The Pacific continental margin and oceanic islands of Costa Rica, Panama, Colombia and Ecuador, including World Heritage sites at Galapagos, Coiba, Cocos and Malpelo
Methods Densities of reef fishes, mobile and sessile invertebrates, and macroalgae were quantified using underwater visual surveys at 136 'no-take' and 54 openly fished sites associated with seven large MPAs that encompassed a range of management strategies. Spatial variation inmultivariate and univariate community metrics was related to three levels of fishing pressure (high-protection MPAs, limited-protection MPAs, fishing zones) for both continental and oceanic reefs.
Results High-protection MPAs possessed a much greater biomass of higher carnivorous fishes, lower densities of asteroids and Eucidaris spp. urchins, and higher coral cover than limited-protection MPAs and fished zones. These results were generally consistent with the hypothesis that overfishing of predatory fishes within the ETP has led to increased densities of habitat-modifying macroinvertebrates, which has contributed to regional declines in coral cover. Major differences in ecological patterns were also evident between continental and oceanic biogeographic provinces.
Main conclusions Fishing down the food web, with associated trophic cascades, has occurred to a greater extent along the continental coast than off oceanic islands. Poorly enforced MPAs generate food
C1 [Edgar, Graham J.] Univ Tasmania, Tasmanian Aquaculture & Fisheries Inst, Hobart, Tas 7001, Australia.
[Edgar, Graham J.; Henderson, Scott] Conservat Int, Puerto Ayora, Galapagos, Ecuador.
[Edgar, Graham J.; Banks, Stuart A.; Ruiz, Diego] Charles Darwin Fdn, Puerto Ayora, Galapagos, Ecuador.
[Bessudo, Sandra; Soler, German] Fdn Malpelo, Bogota, Colombia.
[Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica.
[Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Panama.
[Martinez, Camilo] Univ San Francisco de Quito, ECOLAP, Quito, Ecuador.
[Rivera, Fernando] Inst NAZCA Invest Marinas, Rumipamba, Quito, Ecuador.
[Zapata, Fernando A.] Univ Valle, Dept Biol, Cali, Colombia.
RP Edgar, GJ (reprint author), Univ Tasmania, Tasmanian Aquaculture & Fisheries Inst, GPO Box 252-49, Hobart, Tas 7001, Australia.
EM g.edgar@utas.edu.au
RI Edgar, Graham/C-8341-2013
OI Edgar, Graham/0000-0003-0833-9001
FU Walton Family Foundation through the Eastern Tropical Pacific Seascape
Initiative; Gordon and Betty Moore Foundation; Darwin Initiative;
UNESCO; National Geographic Society; Galapagos National Park Service;
Charles Darwin Foundation; Conservation International; Universidad de
Costa Rica; Smithsonian Tropical Research Institute
FX We would particularly like to thank Angel Chiriboga, Adriana Alzate,
Alberto Rodriguez, Ana Maria Palacios, Ana Fonseca, Carlos Munoz,
Giancarlo Toti, Jerson Moreno, Juan Felipe Lazarus, Alba Marina Cobo,
Juan Jose Alvarado, Julio Delgado, Mariana Vera, Marlene Davey, Mauricio
Castrejon, Mishail Cohen, Natalia Tirado, Odalisca Breedy, Carlos
Guevara, Roby Pepolas and Soledad Luna for field assistance, and
Alejandro Velasco for digitizing images. Field studies were coordinated
with funding from the Walton Family Foundation through the Eastern
Tropical Pacific Seascape Initiative, and research cruises were
supported by the Gordon and Betty Moore Foundation (Marine Management
Area Science project), the Darwin Initiative, UNESCO, the National
Geographic Society, the Galapagos National Park Service, the Charles
Darwin Foundation, Conservation International, the Universidad de Costa
Rica and the Smithsonian Tropical Research Institute. Logistic support
and facilitation by the Galapagos National Park Service, MarViva and
Area de Conservacion Marina Isla del Coco (ACMIC) also greatly assisted
outcomes.
NR 59
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U1 8
U2 64
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1466-822X
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD SEP
PY 2011
VL 20
IS 5
BP 730
EP 743
DI 10.1111/j.1466-8238.2010.00642.x
PG 14
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 805BN
UT WOS:000293701300008
ER
PT J
AU Purcell, RH
Sun, B
Pass, LL
Power, ML
Moran, TH
Tamashiro, KLK
AF Purcell, Ryan H.
Sun, Bo
Pass, Lauren L.
Power, Michael L.
Moran, Timothy H.
Tamashiro, Kellie L. K.
TI Maternal stress and high-fat diet effect on maternal behavior, milk
composition, and pup ingestive behavior
SO PHYSIOLOGY & BEHAVIOR
LA English
DT Article
DE Prenatal stress; High-fat diet; Obesity; Maternal behavior; Independent
ingestion
ID PITUITARY-ADRENAL-AXIS; PRENATAL STRESS; INDEPENDENT INGESTION;
PREPREGNANCY OBESITY; INSULIN-RESISTANCE; UNITED-STATES; RATS;
LACTATION; EXPOSURE; OVERWEIGHT
AB Chronic variable prenatal stress or maternal high-fat diet results in offspring that are significantly heavier by the end of the first postnatal week with increased adiposity by weaning. It is unclear, however, what role maternal care and diet play in the ontogenesis of this phenotype and what contributions come from differences already established in the rat pups. In the present studies, we examined maternal behavior and milk composition as well as offspring ingestive behavior. Our aim was to better understand the development of the obese phenotype in offspring from dams subjected to prenatal stress and/or fed a high-fat (HF) diet during gestation and lactation. We found that dams maintained on a HF diet through gestation and lactation spent significantly more time nursing their pups during the first postnatal week. In addition, offspring of prenatal stress dams consumed more milk at postnatal day (PND) 3 and offspring of HF dams consume more milk on PND 7 in an independent ingestion test. Milk from HF dams showed a significant increase in fat content from PND 10-21. Together these results suggest that gestational dietary or stress manipulations can alter the rat offspring's developmental environment, evidence of which is apparent by PND 3. Alterations in maternal care, milk composition, and pup consumption during the early postnatal period may contribute to long-term changes in body weight and adiposity induced by maternal prenatal stress or high-fat diet. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Purcell, Ryan H.; Sun, Bo; Moran, Timothy H.; Tamashiro, Kellie L. K.] Johns Hopkins Univ, Sch Med, Dept Psychiat & Behav Sci, Baltimore, MD 21205 USA.
[Sun, Bo] Xi An Jiao Tong Univ, Sch Med, Dept Physiol & Pathophysiol, Xian 710049, Shaanxi, Peoples R China.
[Pass, Lauren L.] Howard Univ, Dept Biol, Washington, DC 20059 USA.
[Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Washington, DC 20013 USA.
RP Tamashiro, KLK (reprint author), Johns Hopkins Univ, Sch Med, Dept Psychiat & Behav Sci, 720 Rutland Ave,Ross 618, Baltimore, MD 21205 USA.
EM ktamashiro@jhmi.edu
OI Power, Michael/0000-0002-6120-3528; Purcell, Ryan/0000-0002-6652-2747
FU NIH [HD055030, DK077623]; Chinese Scholarship Council
FX We thank Dr. Nu-Chu Liang, Dr. Megan Dailey, and Guangjing Zhu for their
excellent technical assistance. This study was supported by NIH Grants
HD055030, DK077623, and the Chinese Scholarship Council.
NR 53
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U2 17
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0031-9384
J9 PHYSIOL BEHAV
JI Physiol. Behav.
PD SEP 1
PY 2011
VL 104
IS 3
BP 474
EP 479
DI 10.1016/j.physbeh.2011.05.012
PG 6
WC Psychology, Biological; Behavioral Sciences
SC Psychology; Behavioral Sciences
GA 799YS
UT WOS:000293323700016
PM 21605577
ER
PT J
AU Chisholm, RA
AF Chisholm, Ryan A.
TI Time-dependent solutions of the spatially implicit neutral model of
biodiversity
SO THEORETICAL POPULATION BIOLOGY
LA English
DT Article
DE Neutral theory; Spatially implicit neutral model; Time-dependent
solutions; Transient solutions; Population genetics; Moran model
ID RELATIVE SPECIES ABUNDANCE; MULTIPLE SAMPLES; NULL MODEL; DYNAMICS;
COMMUNITIES; DIVERSITY; INVASIBILITY; INVASION; PATTERNS; FORMULA
AB Previous research into the neutral theory of biodiversity has focused mainly on equilibrium solutions rather than time-dependent solutions. Understanding the time-dependent solutions is essential for applying neutral theory to ecosystems in which time-dependent processes, such as succession and invasion, are driving the dynamics. Time-dependent solutions also facilitate tests against data that are stronger than those based on static equilibrium patterns. Here I investigate the time-dependent solutions of the classic spatially implicit neutral model, in which a small local community is coupled to a much larger metacommunity through immigration. I present explicit general formulas for the eigenvalues, left eigenvectors and right eigenvectors of the models's transition matrix. The time-dependent solutions can then be expressed in terms of these eigenvalues and eigenvectors. Some of these results are translated directly from existing results for the classic Moran model of population genetics (the Moran model is equivalent to the spatially implicit neutral model after a reparameterization); others of the results are new. I demonstrate that the asymptotic time-dependent solution corresponding to just these first two eigenvectors can be a good approximation to the full time-dependent solution. I also demonstrate the feasibility of a partial eigendecomposition of the transition matrix, which facilitates direct application of the results to a biologically relevant example in which a newly invading species is initially present in the metacommunity but absent from the local community. (c) 2011 Elsevier Inc. All rights reserved.
C1 [Chisholm, Ryan A.] Princeton Univ, Princeton, NJ 08544 USA.
[Chisholm, Ryan A.] Smithsonian Trop Res Inst, DPO, AA 34002 USA.
RP Chisholm, RA (reprint author), Princeton Univ, Princeton, NJ 08544 USA.
EM ryan.chis@gmail.com
RI Chisholm, Ryan/H-8033-2012
NR 41
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U1 1
U2 6
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0040-5809
EI 1096-0325
J9 THEOR POPUL BIOL
JI Theor. Popul. Biol.
PD SEP
PY 2011
VL 80
IS 2
BP 71
EP 79
DI 10.1016/j.tpb.2011.06.002
PG 9
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 805XX
UT WOS:000293765500001
PM 21708180
ER
PT J
AU Briggs, WM
Soon, W
Legates, D
Carter, RM
AF Briggs, William M.
Soon, Willie
Legates, David
Carter, Robert M.
TI A Vaccine Against Arrogance
SO WATER AIR AND SOIL POLLUTION
LA English
DT Editorial Material
C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Legates, David] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA.
[Carter, Robert M.] James Cook Univ, Marine Geophys Lab, Townsville, Qld 4811, Australia.
RP Briggs, WM (reprint author), 300 E 71st Apt 3R, New York, NY 10021 USA.
EM matt@wmbriggs.com; wsoon@cfa.harvard.edu; legates@udel.edu;
bob.carter@jcu.edu.au
NR 5
TC 0
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U1 0
U2 6
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0049-6979
J9 WATER AIR SOIL POLL
JI Water Air Soil Pollut.
PD SEP
PY 2011
VL 220
IS 1-4
BP 5
EP 6
DI 10.1007/s11270-011-0873-y
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences; Water
Resources
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences;
Water Resources
GA 806CY
UT WOS:000293783700002
ER
PT J
AU Rice, RA
AF Rice, Robert A.
TI Fruits from shade trees in coffee: how important are they?
SO AGROFORESTRY SYSTEMS
LA English
DT Article
DE Shade coffee; Fruits; Agroforestry; Farm income; Guatemala; Peru
ID AGROFORESTRY; SYSTEMS; NICARAGUA; MEXICO
AB Agroforestry systems often receive attention and support in the literature for what is perceived as the benefits from multiple products associated with the trees that create the "forest" component of the setting. A comparison of small coffee growers' use of fruits derived from the coffee agroforestry holding in Guatemala and Peru reveals that significant differences exist between these groups-not merely in the importance of the fruits themselves, but in the ways they are used. The overall importance of fruits from the coffee system accounts for a relatively small portion of the total value coming from the coffee area (about 10%), but the consumption and sales of the various products do generate needed income or sustenance for most farmers. The fate of fruits shows significant differences between the two countries. Whether at the farm level or on a per hectare basis, Guatemalan coffee farmers are more linked into a market economy and sell significantly more fruits than Peruvian farmers. The opposite is the case when on-farm consumption (use value) of the fruits is compared. While the potential value of these products may be quite large (from $95 to $270/ha), we find that little gets consumed or sold, resulting in tremendous loss of potential benefits that could flow from these sources. Both groups lose more fruits than are sold or used, with Guatemalans foregoing more than three times the dollar value per hectare than Peruvians ($151/ha vs. $44/ha). Data about the economic context within which these growers and the fruits from coffee are found reveal possible reasons as to why we see the differences in use and exchange values realized in the two countries.
C1 Smithsonian Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
RP Rice, RA (reprint author), Smithsonian Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA.
EM ricer@si.edu
FU Summit Foundation, Guatemala; Winrock International, Peru
FX I am grateful to Summit Foundation and Winrock International for grant
funds supporting this project in Guatemala and Peru, respectively.
Gerardo Medina and Victor Guzman helped collect data and provide
insights in Peru, and Rony Mejia and Erika Curley did likewise in
Guatemala-proving indispensible in their efforts. I thank reviewers for
their comments, along with the editor of AS. Any errors found here are
mine alone.
NR 26
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U1 1
U2 19
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-4366
J9 AGROFOREST SYST
JI Agrofor. Syst.
PD SEP
PY 2011
VL 83
IS 1
BP 41
EP 49
DI 10.1007/s10457-011-9385-4
PG 9
WC Agronomy; Forestry
SC Agriculture; Forestry
GA 799KQ
UT WOS:000293286000004
ER
PT J
AU Benson, JF
Hostetler, JA
Onorato, DP
Johnson, WE
Roelke, ME
O'Brien, SJ
Jansen, D
Oli, MK
AF Benson, John F.
Hostetler, Jeffrey A.
Onorato, David P.
Johnson, Warren E.
Roelke, Melody E.
O'Brien, Stephen J.
Jansen, Deborah
Oli, Madan K.
TI Intentional genetic introgression influences survival of adults and
subadults in a small, inbred felid population
SO JOURNAL OF ANIMAL ECOLOGY
LA English
DT Article
DE admixture; AIC; Cox proportional hazard; demographic parameter;
heterosis; hybridization; model averaging
ID FLORIDA PANTHER; HYBRID VIGOR; CONSERVATION; HYBRIDIZATION; MANAGEMENT;
EXTINCTION; DISPERSAL; MODELS; METAPOPULATION; RESTORATION
AB 1. Inbreeding and low genetic diversity can cause reductions in individual fitness and increase extinction risk in animal populations. Intentional introgression, achieved by releasing genetically diverse individuals into inbred populations, has been used as a conservation tool to improve demographic performance in endangered populations.
2. By the 1980s, Florida panthers (Puma concolor coryi) had been reduced to a small, inbred population that appeared to be on the brink of extinction. In 1995, female pumas from Texas (P. c. stanleyana) were released in occupied panther range as part of an intentional introgression programme to restore genetic variability and improve demographic performance of panthers.
3. We used 25 years (1981-2006) of continuous radiotelemetry and genetic data to estimate and model subadult and adult panther survival and cause-specific mortality to provide rigorous sex and age class-specific survival estimates and evaluate the effect of the introgression programme on these parameters.
4. Genetic ancestry influenced annual survival of subadults and adults after introgression, as F-1 generation admixed panthers ((s) over cap = 0 98) survived better than pre-introgression type panthers ((s) over cap = 0 77) and other admixed individuals ((s) over cap = 0 82). Furthermore, heterozygosity was higher for admixed panthers relative to pre-introgression type panthers and positively influenced survival.
5. Our results are consistent with hybrid vigour; however, extrinsic factors such as low density of males in some areas of panther range may also have contributed to higher survival of F-1 panthers. Regardless, improved survival of F-1 subadults and adults likely contributed to the numerical increase in panthers following introgression, and our results indicate that intentional admixture, achieved here by releasing individuals from another population, appears to have been successful in improving demographic performance in this highly endangered population.
C1 [Benson, John F.; Onorato, David P.] Florida Fish & Wildlife Conservat Commiss, US Fish & Wildlife Res Inst, Naples, FL 34114 USA.
[Hostetler, Jeffrey A.; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA.
[Johnson, Warren E.; Roelke, Melody E.; O'Brien, Stephen J.] NCI, Lab Genom Div, Frederick, MD 21702 USA.
[Roelke, Melody E.] NCI, SAIC Frederick, Frederick, MD 21702 USA.
[Jansen, Deborah] Big Cypress Natl Preserve, Ochopee, FL 34141 USA.
RP Hostetler, JA (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,MRC SS03, Washington, DC 20013 USA.
EM hostetlerj@si.edu
RI Hostetler, Jeffrey/A-3345-2011; Johnson, Warren/D-4149-2016
OI Hostetler, Jeffrey/0000-0003-3669-1758; Johnson,
Warren/0000-0002-5954-186X
FU Florida Panther Research and Management Trust; National Park Service;
University of Florida; United States Fish and Wildlife Service
FX We thank D. Land, M. Cunningham, Roy McBride, M. Lotz, D. Shindle, S.
Schulze, D. Giardina, A. Johnson, S. Bass, L. Oberhofer, M. Alvarado, H.
Fitting and Rocky McBride, Rowdy McBride, C. McBride and others for
assistance with fieldwork. We also thank B. Bolker, D. Valle, J. White,
J. Nichols and G. White for statistical assistance or advice and D.
Land, Roy McBride, B. Bolker, J. Nichols, A. Singh, M. Lotz, M.
Cunningham, T. O'Meara, J. Gore, P. Mahoney and two anonymous reviewers
for reviewing earlier versions of this manuscript. This work was funded
through the Florida Panther Research and Management Trust Fund, National
Park Service, University of Florida, and a grant from the United States
Fish and Wildlife Service.
NR 70
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U2 57
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0021-8790
J9 J ANIM ECOL
JI J. Anim. Ecol.
PD SEP
PY 2011
VL 80
IS 5
BP 958
EP 967
DI 10.1111/j.1365-2656.2011.01809.x
PG 10
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA 798BN
UT WOS:000293176400007
PM 21338353
ER
PT J
AU Garcia-Robledo, C
Horvitz, CC
AF Garcia-Robledo, Carlos
Horvitz, Carol C.
TI Experimental demography and the vital rates of generalist and specialist
insect herbivores on native and novel host plants
SO JOURNAL OF ANIMAL ECOLOGY
LA English
DT Article
DE Cephaloleia; demography; exotic host plants; La Selva Biological
Station; native herbivores; preadaptation; Zingiberales
ID PHENOTYPIC PLASTICITY; LIFE-HISTORY; EVOLUTIONARY CONSEQUENCES;
BIOLOGICAL INVASIONS; NATURAL ENEMIES; LEAF BEETLES; CHRYSOMELIDAE;
COLEOPTERA; ENVIRONMENT; ADAPTATION
AB 1. Colonization success of species when confronted with novel environments is of interest in ecological, evolutionary and conservation contexts. Such events may represent the first step for ecological diversification. They also play an important role in adaptive divergence and speciation.
2. A species that is able to do well across a range of environments has a higher plasticity than one whose success is restricted to a single or few environments. The breadth of environments in which a species can succeed is ultimately determined by the full pattern of its vital rates in each environment.
3. Examples of organisms colonizing novel environments are insect herbivores expanding their diets to novel host plants. One expectation for insect herbivores is that species with specialized diets may display less plasticity when faced with novel hosts than generalist species.
4. We examine this hypothesis for two generalist and two specialist neotropical beetles (genus Cephaloleia: Chrysomelidae) currently expanding their diets from native to novel plants of the order Zingiberales. Using an experimental approach, we estimated changes in vital rates, life-history traits and lifetime fitness for each beetle species when feeding on native or novel host plants.
5. We did not find evidence supporting more plasticity for generalists than for specialists. Instead, we found similar patterns of survival and fecundity for all herbivores. Larvae survived worse on novel hosts; adults survived at least as well or better, but reproduced less on the novel host than on natives.
6. Some of the novel host plants represent challenging environments where population growth was negative. However, in four novel plant-herbivore interactions, instantaneous population growth rates were positive.
7. Positive instantaneous population growth rates during initial colonization of novel host plants suggest that both generalist and specialist Cephaloleia beetles may be pre-adapted to feed on some novel hosts. This plasticity in host use is a key factor for successful colonization of novel hosts. Future success or failure in the colonization of these novel hosts will depend on the demographic rates described in this research, natural selection and the evolutionary responses of life-history traits in novel environments.
C1 [Garcia-Robledo, Carlos; Horvitz, Carol C.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA.
EM garciac@si.edu
FU J. McLamore Fellowship - University of Miami; OTS (Organization for
Tropical Studies) - Donald and Beverly Stone and Christiane and
Christopher Tyson Fellowships; College of Arts and Sciences; University
of Miami; US National Institutes of Health; National Institute of Aging
[P01 AG022500-01]; NSF [DEB-0614457]
FX The authors thank the staff of La Selva Biological Station -
Organization for Tropical Studies. We want to thank G. Frias, J.G.
Huertas, G. Huertas and R. Sanchez, for assistance in the field and
laboratory. We thank the National Museum of Natural History, Smithsonian
Institution for granting us access to the entomological Collection. C.
L. Staines (Smithsonian Institution) provided invaluable advice during
the development of this project. This research was funded by the J.
McLamore Fellowship - University of Miami and the OTS (Organization for
Tropical Studies) - Donald and Beverly Stone and Christiane and
Christopher Tyson Fellowships to C. Garcia-Robledo and the Cooper
Fellowship, College of Arts and Sciences, University of Miami, the US
National Institutes of Health, National Institute of Aging P01
AG022500-01 and NSF DEB-0614457 grants to C. C. Horvitz. Comments by T.
H. Fleming, D. J. Futuyma, E. K. Kuprewicz, K. D. Waddington, B. A.
Whitlock and three anonymous reviewers improved this manuscript
substantially. This is Contribution No. 665 of the Program in Tropical
Biology, Evolution and Behavior, Department of Biology, University of
Miami.
NR 61
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U2 49
PU WILEY-BLACKWELL
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 SEP
PY 2011
VL 80
IS 5
BP 976
EP 989
DI 10.1111/j.1365-2656.2011.01843.x
PG 14
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA 798BN
UT WOS:000293176400009
PM 21534952
ER
PT J
AU Brady, SG
Litman, JR
Danforth, BN
AF Brady, Sean G.
Litman, Jessica R.
Danforth, Bryan N.
TI Rooting phylogenies using gene duplications: An empirical example from
the bees (Apoidea)
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Apoidea; Hymenoptera; Elongation factor-1 alpha; Molecular phylogeny;
Paralogy; Rooting
ID ELONGATION FACTOR-1-ALPHA; NUCLEAR GENES; NUCLEOTIDE SUBSTITUTION;
DROSOPHILA-MELANOGASTER; MOLECULAR PHYLOGENETICS; 1-ALPHA EF-1-ALPHA;
RAPID RADIATIONS; ALLODAPINE BEES; EARLY EVOLUTION; UNIVERSAL TREE
AB The placement of the root node in a phylogeny is fundamental to characterizing evolutionary relationships. The root node of bee phylogeny remains unclear despite considerable previous attention. In order to test alternative hypotheses for the location of the root node in bees, we used the F1 and F2 paralogs of elongation factor 1-alpha (EF-1 alpha) to compare the tree topologies that result when using outgroup versus paralogous rooting. Fifty-two taxa representing each of the seven bee families were sequenced for both copies of EF-1 alpha. Two datasets were analyzed. In the first (the "concatenated" dataset), the F1 and F2 copies for each species were concatenated and the tree was rooted using appropriate outgroups (sphecid and crabronid wasps). In the second dataset (the "duplicated" dataset), the F1 and F2 copies were aligned to each another and each copy for all taxa were treated as separate terminals. In this dataset, the root was placed between the F1 and F2 copies (e.g., paralog rooting). Bayesian analyses demonstrate that the outgroup rooting approach outperforms paralog rooting, recovering deeper clades and showing stronger support for groups well established by both morphological and other molecular data. Sequence characteristics of the two copies were compared at the amino acid level, but little evidence was found to suggest that one copy is more functionally conserved. Although neither approach yields an unambiguous root to the tree, both approaches strongly indicate that the root of bee phylogeny does not fall near Colletidae, as has been previously proposed. We discuss paralog rooting as a general strategy and why this approach performs relatively poorly with our particular dataset. Published by Elsevier Inc.
C1 [Brady, Sean G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
[Litman, Jessica R.; Danforth, Bryan N.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA.
RP Brady, SG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC-188, Washington, DC 20560 USA.
EM bradys@si.edu; jrl72@cornell.edu; bnd1@cornell.edu
FU National Science Foundation [DEB-0211701, DEB-0742998, EF-0431330]
FX We thank colleagues listed in Table 1 who generously provided valuable
specimens for this study. Comments from the editor and two anonymous
reviewers substantially improved the manuscript. This project was
supported by National Science Foundation Grants DEB-0211701 and
DEB-0742998 to B.N.D and EF-0431330 to S.G.B.
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TC 10
Z9 10
U1 0
U2 10
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 SEP
PY 2011
VL 60
IS 3
BP 295
EP 304
DI 10.1016/j.ympev.2011.05.002
PG 10
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 790HX
UT WOS:000292580200003
PM 21600997
ER
PT J
AU Driskell, AC
Norman, JA
Pruett-Jones, S
Mangall, E
Sonsthagen, S
Christidis, L
AF Driskell, Amy C.
Norman, Janette A.
Pruett-Jones, Stephen
Mangall, Elizabeth
Sonsthagen, Sarah
Christidis, Les
TI A multigene phylogeny examining evolutionary and ecological
relationships in the Australo-papuan wrens of the subfamily Malurinae
(Aves)
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Fairy-wrens; Maluridae; Phylogeny; Australia; New Guinea; Passeriformes
ID MELIPHAGIDAE; HONEYEATERS; PARADISE; MALURUS; PLUMAGE
AB Nucleotide sequences from four mitochondrial genes and three nuclear introns were used to examine phylogenetic relationships within the Australo-papuan fairy-wrens (Passeriformes: Maluridae: Malurinae). A well-resolved and well-supported phylogenetic hypothesis of all species in the subfamily was generated. The tree contained three clades corresponding to groups with similar plumages previously identified in earlier studies: the "bi-color," "blue," and "chestnut-shouldered" groups. The genus Malurus was not monophyletic - Malurus grayi formed a clade with two New Guinean genera Sipodotus and Clytomyias. We recommend M. grayi be reclassified into the genus Chenorhamphus Oustalet 1898. One other taxonomic change is recommended based on the large genetic distance between the two subspecies of Chenorhamphus grayi - the elevation of C. g. campbelli to specific status (= C. campbelli). Although the family Maluridae appears to have had its origins in Australia, the DNA data supports a New Guinean origin for the Malurini (Sipodotus, Clytomyias, Chenorhamphus, Malurus). Published by Elsevier Inc.
C1 [Driskell, Amy C.; Sonsthagen, Sarah] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA.
[Norman, Janette A.] Museum Victoria, Dept Sci, Melbourne, Vic 3001, Australia.
[Norman, Janette A.; Christidis, Les] Univ Melbourne, Dept Genet, Parkville, Vic 3052, Australia.
[Pruett-Jones, Stephen] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA.
[Mangall, Elizabeth] Monash Univ, Sch Biol Sci, Clayton, Vic 3168, Australia.
[Christidis, Les] So Cross Univ, Natl Marine Sci Ctr, Coffs Harbour, NSW 2054, Australia.
RP Driskell, AC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM driskella@si.edu
FU Australian Research Council [DP0344222]; National Science Foundation
(USA); Wettenhall Foundation; Chicago Zoological Society; University of
Chicago; Chevron Pty. Ltd.
FX This work was supported by an Australian Research Council grant
(DP0344222) to LC. SP-J received financial support from the National
Science Foundation (USA), the Wettenhall Foundation, Chicago Zoological
Society, University of Chicago, and Chevron Pty. Ltd. We thank the
following institutions and individuals for provision of tissue samples:
Museum Victoria, Australian Museum, Australian National Wildlife
Collection (CSIRO), Western Australian Museum, University of Washington
Burke Museum, Academy of Natural Sciences Philadelphia, University of
Kansas Natural History Museum and Biodiversity Research Center, Yale
Peabody Museum, Jordan Karubian, and Michael Webster.
NR 25
TC 22
Z9 24
U1 3
U2 16
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 SEP
PY 2011
VL 60
IS 3
BP 480
EP 485
DI 10.1016/j.ympev.2011.03.030
PG 6
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 790HX
UT WOS:000292580200019
PM 21466855
ER
PT J
AU Mireles, F
Pinedo, JL
Davila, JI
Oliva, JE
Speakman, RJ
Glascock, MD
AF Mireles, F.
Pinedo, J. L.
Davila, J. I.
Oliva, J. E.
Speakman, R. J.
Glascock, M. D.
TI Assessing sediment pollution from the Julian Adame-Alatorre dam by
instrumental neutron activation analysis
SO MICROCHEMICAL JOURNAL
LA English
DT Article
DE Environmental pollution; Sediment; Enrichment factor; INAA
ID ENRICHMENT FACTORS; TRACE-ELEMENTS; INAA; SOIL
AB The rapid industrial development in regions of Mexico during recent years has had the side effect of introducing toxic metals, fertilizers, and pesticides into the ecosystem. Sediment cores were collected from eight locations around the Julian Adame-Alatorre dam located in the Municipality of Villanueva in the State of Zacatecas, Mexico. The cores were analyzed for 32 major, trace, and rare earth elements (As, La, Lu, Nd, Sm, U, Yb, Ce, Co, Cr, Cs, Eu, Fe, Hf, Rb, Sb, Sc, Sr, Ta, Tb, Th, Zn, Zr, Al, Ba, Ca, Dy, K, Mn, Na, Ti, and V) in order to estimate the health risk. The samples were analyzed by instrument neutron activation analysis (INAA) using thermal neutron fluxes of 8 x 10(13) and 5 x 10(13) n cm(-2) s(-1) for short and long irradiations, respectively. The results of the contamination levels for elements such as As, Ba, Cr, Fe, Mn, Ta, V. and Zn were compared with the Mexican regulations and the guidelines of USEPA. Enrichment factors for quantified elements identified high As, Sb, Hf, and Cs contents using Fe as a crustal reference. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Mireles, F.; Pinedo, J. L.; Davila, J. I.; Oliva, J. E.] Univ Autonoma Zacatecas, Unidad Acad Estudios Nucl, Zacatecas 98068, Mexico.
[Speakman, R. J.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
[Glascock, M. D.] Univ Missouri, Res Reactor Ctr, Columbia, MO 65211 USA.
RP Mireles, F (reprint author), Univ Autonoma Zacatecas, Unidad Acad Estudios Nucl, Cipres 10, Zacatecas 98068, Mexico.
EM fmireles@uaz.edu.mx
OI Glascock, Michael D./0000-0003-0686-7556; Speakman,
Robert/0000-0003-2063-154X
FU US Department of Energy [DE-FG07-021D14380]
FX The authors are grateful to Dr William H. Miller and operators of the
University of Missouri Research Reactor for their valuable assistance in
the INAA. "This work was supported in part by the US Department of
Energy grant DE-FG07-021D14380".
NR 15
TC 5
Z9 5
U1 0
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0026-265X
J9 MICROCHEM J
JI Microchem J.
PD SEP
PY 2011
VL 99
IS 1
BP 20
EP 25
DI 10.1016/j.microc.2011.03.014
PG 6
WC Chemistry, Analytical
SC Chemistry
GA 788FR
UT WOS:000292431300004
ER
PT J
AU Vinogradova, NT
Ponte, RM
Tamisiea, ME
Quinn, KJ
Hill, EM
Davis, JL
AF Vinogradova, N. T.
Ponte, R. M.
Tamisiea, M. E.
Quinn, K. J.
Hill, E. M.
Davis, J. L.
TI Self-attraction and loading effects on ocean mass redistribution at
monthly and longer time scales
SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS
LA English
DT Article
ID SEA-LEVEL; BOTTOM PRESSURE; GLOBAL OCEAN; SATELLITE ALTIMETRY; ICE
SHEETS; GRACE; VARIABILITY; CIRCULATION; PATTERNS; TRENDS
AB Self-attraction and loading (SAL) effects caused by changes in mass loads associated with land hydrology, atmospheric pressure, and ocean dynamics produce time-varying, nonuniform spatial patterns in ocean bottom pressure (OBP). Such mass redistribution produced by SAL effects is shown to be an important component of OBP variability on scales from months to years and to provide for a better description of the OBP annual cycle observed by GRACE (Gravity Recovery and Climate Experiment). The SAL-induced ocean mass variations have magnitudes comparable to the dynamic OBP signals at subannual, annual, and interannual time scales in many ocean regions and should not be ignored in studies of ocean mass. Annual variations account for the most variability in SAL-related mass signals and can be induced by all the loads considered, with hydrology having the largest contribution. At subannual and interannual time scales, impact of hydrology is minimal and variations are mostly related to load changes from ocean dynamics and from changes in atmospheric circulation, depending on ocean region. The results demonstrate that the large-scale SAL effects are not negligible in the analysis of GRACE-derived global observations of OBP. The estimated SAL effects can explain on average 0.2 cm(2) (16%) of the variance in the GRACE annual cycle (expressed in terms of equivalent water height), exceeding 1 cm(2) in both open ocean and coastal regions with strong annual SAL signals.
C1 [Vinogradova, N. T.; Ponte, R. M.; Quinn, K. J.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA.
[Tamisiea, M. E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England.
[Hill, E. M.; Davis, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Vinogradova, NT (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA.
EM nadya@aer.com
RI Davis, James/D-8766-2013; Hill, Emma/B-7037-2011;
OI Davis, James/0000-0003-3057-477X; Hill, Emma/0000-0003-0231-5818; Ponte,
Rui/0000-0001-7206-6461
FU NASA [NNX07AM77G]; GRACE project [NN08CD19C]
FX The work was supported by NASA grant NNX07AM77G and by the GRACE project
through contract NN08CD19C to AER.
NR 36
TC 7
Z9 7
U1 2
U2 9
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-OCEANS
JI J. Geophys. Res.-Oceans
PD AUG 31
PY 2011
VL 116
AR C08041
DI 10.1029/2011JC007037
PG 10
WC Oceanography
SC Oceanography
GA 816ZM
UT WOS:000294640600002
ER
PT J
AU Croll, SG
Mecklenburg, MF
Zee, M
AF Croll, Stuart G.
Mecklenburg, Marion F.
Zee, Malia
TI Pigments and the long term structure of artists\' oil paint
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 242nd National Meeting of the American-Chemical-Society (ACS)
CY AUG 28-SEP 01, 2011
CL Denver, CO
SP Amer Chem Soc (ACS)
C1 [Croll, Stuart G.; Zee, Malia] N Dakota State Univ, Dept Coatings & Polymer Mat, Fargo, ND 58108 USA.
[Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA.
EM Stuart.Croll@ndsu.edu
NR 0
TC 0
Z9 0
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0065-7727
J9 ABSTR PAP AM CHEM S
JI Abstr. Pap. Am. Chem. Soc.
PD AUG 28
PY 2011
VL 242
MA 45-PMSE
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 880BE
UT WOS:000299378306617
ER
PT J
AU Smith, FA
Lyons, SK
AF Smith, Felisa A.
Lyons, S. Kathleen
TI How big should a mammal be? A macroecological look at mammalian body
size over space and time
SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE macroecology; temporal scales; spatial scales; mammalian body mass;
biogeography; the comparative method
ID CLIMATE-CHANGE; ENERGETIC CONSTRAINTS; SPECIES OCCUPANCY; GEOGRAPHIC
RANGE; METABOLIC THEORY; GENERAL-MODEL; CARBON-CYCLE; COPES RULE;
EVOLUTION; DYNAMICS
AB Macroecology was developed as a big picture statistical approach to the study of ecology and evolution. By focusing on broadly occurring patterns and processes operating at large spatial and temporal scales rather than on localized and/or fine-scaled details, macroecology aims to uncover general mechanisms operating at organism, population, and ecosystem levels of organization. Macroecological studies typically involve the statistical analysis of fundamental species-level traits, such as body size, area of geographical range, and average density and/or abundance. Here, we briefly review the history of macroecology and use the body size of mammals as a case study to highlight current developments in the field, including the increasing linkage with biogeography and other disciplines. Characterizing the factors underlying the spatial and temporal patterns of body size variation in mammals is a daunting task and moreover, one not readily amenable to traditional statistical analyses. Our results clearly illustrate remarkable regularities in the distribution and variation of mammalian body size across both geographical space and evolutionary time that are related to ecology and trophic dynamics and that would not be apparent without a broader perspective.
C1 [Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
[Lyons, S. Kathleen] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Smith, FA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
EM fasmith@unm.edu
FU International Biogeography Society; National Science Foundation
FX We thank Dave Jenkins and Bob Ricklefs for the invitation to participate
in the January 2011 International Biogeography Society Symposium
'Biogeography and Ecology: two lenses in one telescope' and both the
International Biogeography Society and the National Science Foundation
for financial support. The manuscript was greatly improved by comments
provided by D. Jenkins, R. Ricklefs and R. Poulin. We are especially
grateful to our many colleagues and students for assistance with
research and body size over the years, particularly Jim Brown and Morgan
Ernest. This is contribution number 17 from the IMPSS research
coordination network.
NR 111
TC 36
Z9 37
U1 3
U2 34
PU ROYAL SOC
PI LONDON
PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND
SN 0962-8436
EI 1471-2970
J9 PHILOS T R SOC B
JI Philos. Trans. R. Soc. B-Biol. Sci.
PD AUG 27
PY 2011
VL 366
IS 1576
BP 2364
EP 2378
DI 10.1098/rstb.2011.0067
PG 15
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 793KB
UT WOS:000292819200004
PM 21768152
ER
PT J
AU Feist, J
Nagele, S
Ticknor, C
Schneider, BI
Collins, LA
Burgdorfer, J
AF Feist, J.
Nagele, S.
Ticknor, C.
Schneider, B. I.
Collins, L. A.
Burgdoerfer, J.
TI Attosecond Two-Photon Interferometry for Doubly Excited States of Helium
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID EMISSION; DYNAMICS; PULSES; ATOMS
AB We show that the correlation dynamics in coherently excited doubly excited resonances of helium can be followed in real time by two-photon interferometry. This approach promises to map the evolution of the two-electron wave packet onto experimentally easily accessible noncoincident single-electron spectra. We analyze the interferometric signal in terms of a semianalytical model which is validated by a numerical solution of the time-dependent two-electron Schrodinger equation in its full dimensionality.
C1 [Feist, J.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Nagele, S.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria.
[Ticknor, C.; Collins, L. A.] Los Alamos Natl Lab, Div Theoret, Los Alamos, NM 87545 USA.
[Schneider, B. I.] Natl Sci Fdn, Off Cyberinfrastruct, Arlington, VA 22230 USA.
RP Feist, J (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
EM jfeist@cfa.harvard.edu; stefan.nagele@tuwien.ac.at
RI Nagele, Stefan/E-6938-2011; Feist, Johannes/J-7394-2012; Ticknor,
Christopher/B-8651-2014;
OI Nagele, Stefan/0000-0003-1213-0294; Feist, Johannes/0000-0002-7972-0646;
Ticknor, Christopher/0000-0001-9972-4524
FU FWF-Austria [SFB016, P21141-N16]; NSF; NNSA of the U.S. DOE
[DE-AC52-06NA25396]; TACC [TG-PHY090031]
FX The authors thank Renate Pazourek for valuable discussions. We
acknowledge support by the FWF-Austria, Grants No. SFB016 and No.
P21141-N16 (S. N. and J. B.) and by the NSF through a grant to ITAMP (J.
F.). C. T. and L. A. C. acknowledge support from LANL, which is operated
by LANS, LLC for the NNSA of the U.S. DOE under Contract No.
DE-AC52-06NA25396. The computational results have been achieved by using
the Vienna Scientific Cluster, Institutional Computing resources at Los
Alamos National Laboratory, and NSF TeraGrid resources provided by NICS
and TACC under Grant No. TG-PHY090031.
NR 24
TC 17
Z9 17
U1 0
U2 9
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 AUG 26
PY 2011
VL 107
IS 9
AR 093005
DI 10.1103/PhysRevLett.107.093005
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 812XX
UT WOS:000294328300005
PM 21929238
ER
PT J
AU Reed, RD
Papa, R
Martin, A
Hines, HM
Counterman, BA
Pardo-Diaz, C
Jiggins, CD
Chamberlain, NL
Kronforst, MR
Chen, R
Halder, G
Nijhout, HF
McMillan, WO
AF Reed, Robert D.
Papa, Riccardo
Martin, Arnaud
Hines, Heather M.
Counterman, Brian A.
Pardo-Diaz, Carolina
Jiggins, Chris D.
Chamberlain, Nicola L.
Kronforst, Marcus R.
Chen, Rui
Halder, Georg
Nijhout, H. Frederik
McMillan, W. Owen
TI optix Drives the Repeated Convergent Evolution of Butterfly Wing Pattern
Mimicry
SO SCIENCE
LA English
DT Article
ID HELICONIUS BUTTERFLIES; GENETICS
AB Mimicry-whereby warning signals in different species evolve to look similar-has long served as a paradigm of convergent evolution. Little is known, however, about the genes that underlie the evolution of mimetic phenotypes or to what extent the same or different genes drive such convergence. Here, we characterize one of the major genes responsible for mimetic wing pattern evolution in Heliconius butterflies. Mapping, gene expression, and population genetic work all identify a single gene, optix, that controls extreme red wing pattern variation across multiple species of Heliconius. Our results show that the cis-regulatory evolution of a single transcription factor can repeatedly drive the convergent evolution of complex color patterns in distantly related species, thus blurring the distinction between convergence and homology.
C1 [Reed, Robert D.; Papa, Riccardo; Martin, Arnaud] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
[Papa, Riccardo] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA.
[Papa, Riccardo] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, Rio Piedras, PR 00931 USA.
[Hines, Heather M.; McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA.
[Counterman, Brian A.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA.
[Pardo-Diaz, Carolina; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
[Chamberlain, Nicola L.; Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Cambridge, MA 02138 USA.
[Chen, Rui] Baylor Human Genome Sequencing Ctr, Houston, TX 77030 USA.
[Halder, Georg] Univ Texas Houston, MD Anderson Canc Ctr, Dept Biochem & Mol Biol, Houston, TX 77030 USA.
[Nijhout, H. Frederik] Duke Univ, Dept Biol, Durham, NC 27708 USA.
[McMillan, W. Owen] Smithsonian Trop Res Inst, Panama City, Panama.
RP Reed, RD (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
EM rreed@uci.edu; rpapa.lab@gmail.com
RI Jiggins, Chris/B-9960-2008; Reed, Robert/A-2419-2008; Halder,
Georg/F-2966-2015; Pardo-Diaz, Carolina/C-7936-2016
OI Jiggins, Chris/0000-0002-7809-062X; Martin, Arnaud/0000-0002-5980-2249;
Halder, Georg/0000-0001-7580-3236; Pardo-Diaz,
Carolina/0000-0002-7259-1183
FU NSF; NIH; Centre National de la Recherche Scientifique-Guyane; Peruvian
Ministerio de Agricultura and Instituto Nacional De Recursos Naturales
[004-2008-INRENA-IFFS-DCB, 011756-AG-INRENA]; French Guiana Ministere de
L'Ecologie, de L'Energie, du Developpemet Durable et de la Mar
[BIODAD-2010-0433]; Ecuadorian Ministerio del Ambiente Ecuadorian
[013-09 IC-FAU-DNB/MA]; Panamanian Autoridad Nacional del Ambiente
[SC/A-7-11]
FX We thank M. A. Flores and A. Portugal for help rearing butterflies,
M.-J. Sung for help with electron microscopy, J. Miller for help with
microarray analysis, and J. Mallet for sharing samples. Supported by
funding from NSF (R.D.R., W.O.M., M.R.K.), NIH (H.M.H., M.R.K.), and
Centre National de la Recherche Scientifique-Guyane (B.A.C.) Sequences
are available on GenBank (JN102349-JN102354). Microarray data are
available on Gene Expression Omnibus (GSE30221). Permission to collect
and export butterfly tissue was provided by the Peruvian Ministerio de
Agricultura and Instituto Nacional De Recursos Naturales
(004-2008-INRENA-IFFS-DCB and 011756-AG-INRENA); the French Guiana
Ministere de L'Ecologie, de L'Energie, du Developpemet Durable et de la
Mar (BIODAD-2010-0433); the Ecuadorian Ministerio del Ambiente
Ecuadorian (013-09 IC-FAU-DNB/MA); and the Panamanian Autoridad Nacional
del Ambiente (SC/A-7-11). W.O.M., F.N, and R.D.R. designed experiments
and conducted initial work. R.P. produced butterfly crosses and
generated and analyzed the microarray data with H.M.H. A.M. generated in
situ hybridization data. B.A.C., C.P.-D., C.D.J., N.L.C, and M.R.K.
contributed nucleotide association data. R.C. and G.H. assisted with
positional cloning. R.P., A.M., B.A.C., and R.D.R. prepared figures and
R.D.R. wrote the manuscript with support from R.P., A.M., and W.O.M. The
authors declare that they have no competing financial interests.
NR 15
TC 142
Z9 143
U1 10
U2 120
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 AUG 26
PY 2011
VL 333
IS 6046
BP 1137
EP 1141
DI 10.1126/science.1208227
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811VM
UT WOS:000294244300046
PM 21778360
ER
PT J
AU Cherot, F
Costa, L
Touchet, M
AF Cherot, F.
Costa, L.
Touchet, M.
TI Miscellanea Miridologica II. New combinations and new synonymies in the
tribe Mirini (Hemiptera: Heteroptera: Miridae)
SO ZOOTAXA
LA English
DT Article
DE Heteroptera; Miridae; Mirini; new synonymies; new combinations; French
Guyana; Brazil; Panama; Paramaribo
AB Six new synonymies and four new combinations are proposed: Guianella Carvalho 1946 = Boliviomiris Carvalho, 1987 and Pilosicerus Carvalho, 1992 (new subjective junior synonyms). Guianella pilosa Maldonado & Carvalho, 1981 = G. antennalis (Carvalho, 1987) and G. rondoniensis (Carvalho, 1992) (new subjective junior synonyms). Urucuiana Carvalho & Rosas, 1965 = Bahiamiris Carvalho, 1975 (new subjective junior synonym). Urucuiana tuberculata Carvalho & Rosas, 1965 = U. cajabiana (Carvalho, 1977) (new subjective junior synonym). Guianella antennalis, G. rondoniensis, U. cajabiana, and U. rubrornata (Carvalho, 1975) (new combinations). Urucuiana tuberculata is reported from French Guyana for the first time.
C1 [Cherot, F.] Serv Publ Wallonie, Dept Etud Milieu Nat & Agr, Agr Ressources Nat & Environm DGO3, B-5030 Gembloux, Belgium.
[Cherot, F.] Univ Libre Bruxelles, Dept Biol Organismes, B-1050 Brussels, Belgium.
[Costa, L.] Museu Nacl, BR-20940040 Rio De Janeiro, Brazil.
[Touchet, M.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Cherot, F (reprint author), Serv Publ Wallonie, Dept Etud Milieu Nat & Agr, Agr Ressources Nat & Environm DGO3, 23 Ave Marechal Juin, B-5030 Gembloux, Belgium.
EM frederic.cherot@spw.wallonie.be
NR 11
TC 1
Z9 1
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 AUG 26
PY 2011
IS 3004
BP 57
EP 62
PG 6
WC Zoology
SC Zoology
GA 811ZA
UT WOS:000294256300005
ER
PT J
AU Honer, J
Low, R
Weimer, H
Pfau, T
Buchler, HP
AF Honer, Jens
Loew, R.
Weimer, Hendrik
Pfau, Tilman
Buechler, Hans Peter
TI Artificial Atoms Can Do More Than Atoms: Deterministic Single Photon
Subtraction from Arbitrary Light Fields
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ELECTROMAGNETICALLY INDUCED TRANSPARENCY; QUANTUM INFORMATION;
EXCITATION; MEMORIES; STATES
AB We study the interplay of photons interacting with an artificial atom in the presence of a controlled dephasing. Such artificial atoms consisting of several independent scatterers can exhibit remarkable properties superior to single atoms with a prominent example being a superatom based on Rydberg blockade. We demonstrate that the induced dephasing allows for the controlled absorption of a single photon from an arbitrary incoming probe field. This unique tool in photon-matter interaction opens a way for building novel quantum devices, and several potential applications such as a single photon transistor, high fidelity n-photon counters, or the creation of nonclassical states of light by photon subtraction are presented.
C1 [Honer, Jens; Weimer, Hendrik; Buechler, Hans Peter] Univ Stuttgart, Inst Theoret Phys 3, Stuttgart, Germany.
[Loew, R.; Pfau, Tilman] Univ Stuttgart, Phys Inst 5, Stuttgart, Germany.
[Weimer, Hendrik] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Honer, J (reprint author), Univ Stuttgart, Inst Theoret Phys 3, Stuttgart, Germany.
RI Pfau, Tilman/G-1774-2011; Loew, Robert/I-8206-2014
FU Deutsche Forschungsgemeinschaft (DFG) [SFB/TRR 21]; National Science
Foundation [NSF PHY05-51164]; German Academic Exchange Service (DAAD)
FX We thank W. Schleich and G. Agarwal for fruitful discussions. Support by
the Deutsche Forschungsgemeinschaft (DFG) within SFB/TRR 21 and National
Science Foundation under Grant No. NSF PHY05-51164 is acknowledged. H.
W. is supported by the German Academic Exchange Service (DAAD) and by
the National Science Foundation through a grant for the Institute for
Theoretical Atomic, Molecular and Optical Physics at Harvard University
and Smithsonian Astrophysical Observatory.
NR 34
TC 63
Z9 63
U1 3
U2 14
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 AUG 25
PY 2011
VL 107
IS 9
AR 093601
DI 10.1103/PhysRevLett.107.093601
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 812DT
UT WOS:000294268700005
PM 21929241
ER
PT J
AU Zauderer, BA
Berger, E
Soderberg, AM
Loeb, A
Narayan, R
Frail, DA
Petitpas, GR
Brunthaler, A
Chornock, R
Carpenter, JM
Pooley, GG
Mooley, K
Kulkarni, SR
Margutti, R
Fox, DB
Nakar, E
Patel, NA
Volgenau, NH
Culverhouse, TL
Bietenholz, MF
Rupen, MP
Max-Moerbeck, W
Readhead, ACS
Richards, J
Shepherd, M
Storm, S
Hull, CLH
AF Zauderer, B. A.
Berger, E.
Soderberg, A. M.
Loeb, A.
Narayan, R.
Frail, D. A.
Petitpas, G. R.
Brunthaler, A.
Chornock, R.
Carpenter, J. M.
Pooley, G. G.
Mooley, K.
Kulkarni, S. R.
Margutti, R.
Fox, D. B.
Nakar, E.
Patel, N. A.
Volgenau, N. H.
Culverhouse, T. L.
Bietenholz, M. F.
Rupen, M. P.
Max-Moerbeck, W.
Readhead, A. C. S.
Richards, J.
Shepherd, M.
Storm, S.
Hull, C. L. H.
TI Birth of a relativistic outflow in the unusual gamma-ray transient Swift
J164449.3+573451
SO NATURE
LA English
DT Article
ID TIDAL DISRUPTION; BLACK-HOLES; RADIO-SOURCES; GALAXIES; OUTBURST; STARS
AB Active galactic nuclei, which are powered by long-term accretion onto central supermassive black holes, produce(1) relativistic jets with lifetimes of at least one million years, and the observation of the birth of such a jet is therefore unlikely. Transient accretion onto a supermassive black hole, for example through the tidal disruption(2,3) of a stray star, thus offers a rare opportunity to study the birth of a relativistic jet. On 25 March 2011, an unusual transient source (Swift J164449.3+573451) was found(4), potentially representing(5,6) such an accretion event. Here we report observations spanning centimetre to millimetre wavelengths and covering the first month of evolution of a luminous radio transient associated with Swift J164449.3+573451. The radio transient coincides(7) with the nucleus of an inactive galaxy. We conclude that we are seeing a newly formed relativistic outflow, launched by transient accretion onto a million-solar-mass black hole. A relativistic outflow is not predicted in this situation, but we show that the tidal disruption of a star naturally explains the observed high-energy properties and radio luminosity and the inferred rate of such events. The weaker beaming in the radio-frequency spectrum relative to c-rays or X-rays suggests that radio searches may uncover similar events out to redshifts of z approximate to 6.
C1 [Zauderer, B. A.; Berger, E.; Soderberg, A. M.; Loeb, A.; Narayan, R.; Petitpas, G. R.; Chornock, R.; Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Frail, D. A.; Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Carpenter, J. M.; Mooley, K.; Kulkarni, S. R.; Max-Moerbeck, W.; Readhead, A. C. S.; Richards, J.; Shepherd, M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Pooley, G. G.] Univ Cambridge, Cavendish Lab, Mullard Radio Observ, Cambridge CB3 0HE, England.
[Margutti, R.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Fox, D. B.] Penn State Univ, Dept Astron, University Pk, PA 16802 USA.
[Nakar, E.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
[Volgenau, N. H.; Culverhouse, T. L.] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
[Bietenholz, M. F.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa.
[Bietenholz, M. F.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
[Storm, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Hull, C. L. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Zauderer, BA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bzauderer@cfa.harvard.edu; eberger@cfa.harvard.edu
OI Narayan, Ramesh/0000-0002-1919-2730
FU NASA; NSF; Ministry of Universities and Research of Italy; IRG; ISF;
Smithsonian Institution; Academia Sinica; California Institute of
Technology; University of Chicago; states of California, Illinois and
Maryland; University of Cambridge; STFC
FX E.B. is supported in part by funds from NASA. A.L. is supported in part
by NSF and NASA grants. R. M. acknowledges support from a Swift ASI
grant and from the Ministry of Universities and Research of Italy. E.N.
is partly supported by IRG and ISF grants. The EVLA and the Very Long
Baseline Array are operated by the NRAO, a facility of the NSF operated
under cooperative agreement by the AUI. The SMA is a joint project
between the SAO and the ASIAA, and is funded by the Smithsonian
Institution and the Academia Sinica. CARMA development and operations
are supported by the NSF under a cooperative agreement, and by the
Associates of the California Institute of Technology, the University of
Chicago and the states of California, Illinois and Maryland. The AMI
arrays are supported by the University of Cambridge and the STFC. This
work is partly based on observations with the 100-m telescope of the
MPIfR at Effelsberg. This work made use of data supplied by the UK Swift
Science Data Centre at the University of Leicester.
NR 21
TC 157
Z9 157
U1 0
U2 2
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD AUG 25
PY 2011
VL 476
IS 7361
BP 425
EP 428
DI 10.1038/nature10366
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 811KT
UT WOS:000294209400030
PM 21866155
ER
PT J
AU Graves, GR
Lane, DF
O'Neill, JP
Valqui, T
AF Graves, Gary R.
Lane, Daniel F.
O'Neill, John P.
Valqui, Thomas
TI A distinctive new subspecies of the Royal Sunangel (Aves:
Trochiliformes; Heliangelus regalis) from the Cordillera Azul, northern
Peru
SO ZOOTAXA
LA English
DT Article
DE Cordillera Azul; Heliangelus regalis johnsoni new subspecies;
hummingbirds; Loreto; Peru; Royal Sunangel
ID ECUADORIAN ANDES; NATURAL-HISTORY; SAN-MARTIN; HUMMINGBIRD; PATTERNS;
PLUMAGE; VALLEY; BIRDS
AB A recently discovered and morphologically distinct population of the poorly known Royal Sunangel from the Cordillera Azul, Department of Loreto, Peru, is described as a new subspecies, Heliangelus regalis johnsoni. Males of johnsoni differ from those of nominate regalis in exhibiting intense indigo iridescence, particularly on the crown, throat and upper breast.
C1 [Graves, Gary R.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA.
[Lane, Daniel F.; O'Neill, John P.; Valqui, Thomas] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
[Valqui, Thomas] Ctr Ornithol & Biodivers, CORBIDI, Surco Lima, Peru.
RP Graves, GR (reprint author), Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, MRC-116,POB 37012, Washington, DC 20013 USA.
EM gravesg@si.edu
FU Smithsonian Institution
FX We thank INRENA (Luis Alfaro Lozano) for issuing the collecting permit
(number 150702454), Irma Franke, Manuel Sanchez, Marta Sanchez, Demetrio
Huachaca, Abraham Urbay, Orlando Riva, Aruldo and Carlos Ruiz, Herminio
del Aguila, Cristain Albujar, Louise Augustine, James Armacost, and
Leticia Alamia for assistance in the field and in Lima, John McCormack
for assistance with spectrophotometry, and Brian Schmidt for procuring
the digital elevation map. Graves' travel was supported by the Alexander
Wetmore Fund (Smithsonian Institution).
NR 25
TC 1
Z9 1
U1 0
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 AUG 24
PY 2011
IS 3002
BP 52
EP 58
PG 7
WC Zoology
SC Zoology
GA 811YV
UT WOS:000294255800005
ER
PT J
AU Hershler, R
Liu, HP
Landye, JJ
AF Hershler, Robert
Liu, Hsiu-Ping
Landye, J. Jerry
TI New species and records of springsnails (Caenogastropoda: Cochliopidae:
Tryonia) from the Chihuahuan Desert (Mexico and United States), an
imperiled biodiversity hotspot
SO ZOOTAXA
LA English
DT Article
DE springs; Mexico; Texas; gastropods; mitochondrial DNA; endemism;
taxonomy; conservation
ID NORTH-AMERICAN SOUTHWEST; PHYLOGENETIC-RELATIONSHIPS; GASTROPODS
RISSOOIDEA; RIVER-BASIN; HYDROBIIDAE; BIOGEOGRAPHY; CALIFORNIA;
CHECKLIST; GENUS; FISH
AB We describe 13 new, narrowly localized species of the aquatic gastropod genus Tryonia from springs in the Chihuahuan Desert (Chihuahua and Texas): T. allendae n. sp., T. angosturae n. sp., T. chuviscarae n. sp., T. contrerasi n. sp., T. julimesensis n. sp., T. metcalfi n. sp., T. minckleyi n. sp., T. molinae n. sp., T. oasiensis n. sp., T. ovata n. sp., T. peregrina n. sp., T. taylori n. sp. and T. zaragozae n. sp.. These novelties are distinguished by shell and other morphologic characters and are well differentiated genetically from each other and from other congeners (mtCOI sequence divergence >= 1.9%). We also provide two new records for T. seemani (Frauenfeld, 1863), which is distributed near the southern limit of the Chihuahuan Desert (Durango State) and previously had been thought to be possibly extinct. Bayesian analysis of a mtCOI dataset resolved two clades composed of novelties described herein: one (containing four species) is distributed in several drainages in Chihuahua, the other (containing three species) is a local species flock in the Rio Conchos basin (also in Chihuahua) that lives in the warmest waters yet recorded for Tryonia (41-44 degrees C). (The phylogenetic relationships of the other new species were not well supported.) Both of these clades contain sympatric species pairs; co-occurrence of Tryonia congeners previously had been reported only in Ash Meadows (southern Nevada). Some of the species described herein are from previously unsurveyed localities and may help delineate new areas of endemism within the Chihuahuan Desert. One of the new species (T. julimesensis) became extinct between 1991 and 2001 and another (T. oasiensis) disappeared from its single known locality shortly after it was first discovered in 2009 and also may be extinct. The other species treated herein are at risk of extirpation owing to the declining extent and condition of their unprotected habitats.
C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Liu, Hsiu-Ping] Metropolitan State Coll, Dept Biol, Denver, CO 80217 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; liu.hsiuping@gmail.com
FU National Science Foundation [GB-6477x]; Smithsonian Biodiversity Program
FX J.J.L.'s early collections were made under the auspices of a National
Science Foundation grant to W. L. Minckley (GB-6477x) and a collecting
permit from the Secretaria de Industria y Comercio (# 5803). More recent
fieldwork was supported by awards (to R. H.) from the Smithsonian
Biodiversity Program; collecting permits were provided by La Secretaria
de Relaciones Exteriores (DAN 01874, 03358) and facilitated by Angelica
Narvaez (U. S. Embassy Mexico City, Office of Environment, Science and
Technology Affairs). We thank Andrew Simons and Jonathan Slaght
(BellMNH), Fred Naggs (NHMUK) and Art Metcalf (UTEP) for loans of
material under their care. Various individuals assisted with fieldwork,
including Phil Hines, William G. Kepner, Sandra Tyler Landye, Charles O.
Minckley, Saundra King Minckley, Wendell L. Minckley, Donna Portz,
Dwight W. Taylor, Sandra Willoughby and Darrell Wong. Yolanda Villacampa
measured shells and prepared scanning electron micrographs, and Karolyn
Darrow inked the anatomical drawings.
NR 50
TC 3
Z9 4
U1 0
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 AUG 23
PY 2011
IS 3001
BP 1
EP 32
PG 32
WC Zoology
SC Zoology
GA 810IQ
UT WOS:000294119400001
ER
PT J
AU Baird, E
Kreiss, E
Wcislo, W
Warrant, E
Dacke, M
AF Baird, Emily
Kreiss, Eva
Wcislo, William
Warrant, Eric
Dacke, Marie
TI Nocturnal insects use optic flow for flight control
SO BIOLOGY LETTERS
LA English
DT Article
DE flight; optic flow; insect vision; Megalopta; bumble-bee
ID FLYING SWEAT BEES; VISUAL CONTROL; SPEED; DROSOPHILA; HONEYBEES;
EVOLUTION
AB To avoid collisions when navigating through cluttered environments, flying insects must control their flight so that their sensory systems have time to detect obstacles and avoid them. To do this, day-active insects rely primarily on the pattern of apparent motion generated on the retina during flight (optic flow). However, many flying insects are active at night, when obtaining reliable visual information for flight control presents much more of a challenge. To assess whether nocturnal flying insects also rely on optic flow cues to control flight in dim light, we recorded flights of the nocturnal neotropical sweat bee, Megalopta genalis, flying along an experimental tunnel when: (i) the visual texture on each wall generated strong horizontal (front-to-back) optic flow cues, (ii) the texture on only one wall generated these cues, and (iii) horizontal optic flow cues were removed from both walls. We find that Megalopta increase their groundspeed when horizontal motion cues in the tunnel are reduced (conditions (ii) and (iii)). However, differences in the amount of horizontal optic flow on each wall of the tunnel (condition (ii)) do not affect the centred position of the bee within the flight tunnel. To better understand the behavioural response of Megalopta, we repeated the experiments on day-active bumble-bees (Bombus terrestris). Overall, our findings demonstrate that despite the limitations imposed by dim light, Megalopta-like their day-active relatives-rely heavily on vision to control flight, but that they use visual cues in a different manner from diurnal insects.
C1 [Baird, Emily; Kreiss, Eva; Warrant, Eric; Dacke, Marie] Lund Univ, Dept Biol, Lund, Sweden.
[Kreiss, Eva] Univ Bonn, Dept Zool, D-5300 Bonn, Germany.
[Wcislo, William] Smithsonian Trop Res Inst, Balboa, Panama.
RP Baird, E (reprint author), Lund Univ, Dept Biol, Lund, Sweden.
EM emily.baird@cob.lu.se
RI Baird, Emily/G-8763-2014
OI Baird, Emily/0000-0003-3625-3897
FU AFOSR/EOARD [FA8655-08-C-4004, FA8655-07-C-4011]; Wenner Gren
Foundation; Swedish Research Council
FX This work was funded by the AFOSR/EOARD (grants FA8655-08-C-4004 and
FA8655-07-C-4011), the Wenner Gren Foundation and the Swedish Research
Council.
NR 14
TC 23
Z9 23
U1 6
U2 32
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 AUG 23
PY 2011
VL 7
IS 4
BP 499
EP 501
DI 10.1098/rsbl.2010.1205
PG 3
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 791CM
UT WOS:000292639100007
PM 21307047
ER
PT J
AU Ryder, TB
Horton, BM
Moore, IT
AF Ryder, Thomas B.
Horton, Brent M.
Moore, Ignacio T.
TI Understanding testosterone variation in a tropical lek-breeding bird
SO BIOLOGY LETTERS
LA English
DT Article
DE cooperation; competition; lekking; reproductive coalitions;
testosterone; wire-tailed manakin
ID COURTSHIP DISPLAY; TAILED MANAKIN; BEHAVIOR; EVOLUTION
AB Male reproductive coalitions, in which males cooperate to attract females, are a rare strategy among vertebrates. While some studies have investigated ultimate aspects of these relationships, little is known about the mechanistic role that hormones play in modulating cooperative behaviours. Here, we examined male testosterone variation in a tropical lekking bird, the wire-tailed manakin (Pipra filicauda), which exhibits cooperative male-male display coalitions. We found that testosterone levels in territorial males were comparable to those of temperate breeding birds, a surprising result given their environmental, social and reproductive dynamics. In addition, social status rather than plumage was a strong predictor of testosterone variation. Territorial males had significantly higher testosterone levels than did two other plumage classes of floater males, who do not hold territories. We hypothesize that testosterone variation plays an important role in the establishment of male dominance hierarchies (competition), while concurrently facilitating stable display partnerships (cooperation).
C1 [Ryder, Thomas B.; Horton, Brent M.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA.
[Horton, Brent M.] Emory Univ, Dept Psychol, Rollins Res Ctr, Atlanta, GA 30322 USA.
[Moore, Ignacio T.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA.
RP Ryder, TB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk,POB 37012-MRC5503, Washington, DC 20008 USA.
EM rydert@si.edu
OI Moore, Ignacio/0000-0001-8875-8913
FU National Science Foundation [IOS 0545735]
FX Thanks to Tiputini Biological station for logistical support. National
Science Foundation provided funding to I.T.M. (IOS 0545735).
NR 17
TC 4
Z9 4
U1 2
U2 17
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 AUG 23
PY 2011
VL 7
IS 4
BP 506
EP 509
DI 10.1098/rsbl.2010.1219
PG 4
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 791CM
UT WOS:000292639100009
PM 21325306
ER
PT J
AU Safavi-Naini, A
Rabl, P
Weck, PF
Sadeghpour, HR
AF Safavi-Naini, A.
Rabl, P.
Weck, P. F.
Sadeghpour, H. R.
TI Microscopic model of electric-field-noise heating in ion traps
SO PHYSICAL REVIEW A
LA English
DT Article
ID METAL-SURFACES; GAS ATOMS; RANGE; ADSORPTION; MOLECULES; SOLIDS
AB Motional heating of ions in microfabricated traps is one of the open challenges hindering experimental realizations of large-scale quantum processing devices. Recently, a series of measurements of the heating rates in surface-electrode ion traps characterized their frequency, distance, and temperature dependencies, but our understanding of the microscopic origin of this noise remains incomplete. In this work we develop a theoretical model for the electric field noise which is associated with a random distribution of adsorbed atoms on the trap electrode surface. By using first-principles calculations of the fluctuating dipole moments of the adsorbed atoms we evaluate the distance, frequency, and temperature dependence of the resulting electric field fluctuation spectrum. Our theory reproduces correctly the d(-4) dependence with distance of the ion from the electrode surface and calculates the noise spectrum beyond the standard scenario of two-level fluctuators by incorporating all the relevant vibrational states. Our model predicts a regime of 1/f noise which commences at roughly the frequency of the fundamental phonon transition rate and a thermally activated noise spectrum which for higher temperatures exhibits a crossover as a function of frequency.
C1 [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Safavi-Naini, A.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Rabl, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria.
[Weck, P. F.] Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
[Weck, P. F.] Univ Nevada, Harry Reid Ctr, Las Vegas, NV 89154 USA.
RP Safavi-Naini, A (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
RI Rabl, Peter/F-2810-2012;
OI Rabl, Peter/0000-0002-2560-8835; , Philippe/0000-0002-7610-2893
FU NSF
FX The authors thank D. Wineland for valuable discussions. This work was
supported by the NSF through a grant to ITAMP at the Harvard-Smithsonian
Center for Astrophysics.
NR 46
TC 39
Z9 39
U1 1
U2 7
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 AUG 22
PY 2011
VL 84
IS 2
AR 023412
DI 10.1103/PhysRevA.84.023412
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 810NC
UT WOS:000294131000008
ER
PT J
AU Bezanson, R
van Dokkum, PG
Franx, M
Brammer, GB
Brinchmann, J
Kriek, M
Labbe, I
Quadri, RF
Rix, HW
van de Sande, J
Whitaker, KE
Williams, RJ
AF Bezanson, Rachel
van Dokkum, Pieter G.
Franx, Marijn
Brammer, Gabriel B.
Brinchmann, Jarle
Kriek, Mariska
Labbe, Ivo
Quadri, Ryan F.
Rix, Hans-Walter
van de Sande, Jesse
Whitaker, Katherine E.
Williams, Rik J.
TI REDSHIFT EVOLUTION OF THE GALAXY VELOCITY DISPERSION FUNCTION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: elliptical and lenticular, cD;
galaxies: evolution; galaxies: formation
ID DIGITAL SKY SURVEY; COMPACT MASSIVE GALAXY; ELLIPTIC GALAXIES; QUIESCENT
GALAXIES; FUNDAMENTAL PLANE; PASSIVE GALAXIES; SURFACE-DENSITY; SIZE
EVOLUTION; STAR-FORMATION; DATA RELEASE
AB We present a study of the evolution of the galaxy velocity dispersion function (VDF) from z = 0 to z = 1.5 using photometric data from the Ultra-Deep and the NEWFIRM Medium-Band Survey in the COSMOS field. The VDF has been measured locally using direct kinematic measurements from the Sloan Digital Sky Survey (SDSS), but direct studies of the VDF at high redshift are difficult as they require velocity dispersion measurements of many thousands of galaxies. Taylor et al. demonstrated that dynamical and stellar masses are linearly related when the structure of the galaxy is accounted for. We show that the stellar mass, size, and Sersic index can reliably predict the velocity dispersions of SDSS galaxies. We apply this relation to galaxies at high redshift and determine the evolution of the inferred VDF. We find that the VDF at z similar to 0.5 is very similar to the VDF at z = 0. At higher redshifts, we find that the number density of galaxies with dispersions less than or similar to 200 km s(-1) is lower, but the number of high-dispersion galaxies is constant or even higher. At fixed cumulative number density, the velocity dispersions of galaxies with log N[Mpc(-3)] < -3.5 increase with time by a factor of similar to 1.4 from z similar to 1.5-0, whereas the dispersions of galaxies with lower number density are approximately constant or decrease with time. The VDF appears to show less evolution than the stellar mass function, particularly at the lowest number densities. We note that these results are still somewhat uncertain and we suggest several avenues for further calibrating the inferred velocity dispersions.
C1 [Bezanson, Rachel; van Dokkum, Pieter G.; Whitaker, Katherine E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Franx, Marijn; Brinchmann, Jarle; Labbe, Ivo; van de Sande, Jesse] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Brammer, Gabriel B.] European So Observ, Santiago 19, Chile.
[Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Quadri, Ryan F.; Williams, Rik J.] Carnegie Observ, Pasadena, CA 91101 USA.
[Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Bezanson, R (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
RI Brinchmann, Jarle/M-2616-2015;
OI Brinchmann, Jarle/0000-0003-4359-8797; van de Sande,
Jesse/0000-0003-2552-0021; Bezanson, Rachel/0000-0001-5063-8254
FU NSF [AST-0807974]; HST [GO-12177.01A]
FX We thank the referee for his/her feedback and acknowledge support from
NSF grant AST-0807974 and HST grant GO-12177.01A.
NR 49
TC 40
Z9 40
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 20
PY 2011
VL 737
IS 2
AR L31
DI 10.1088/2041-8205/737/2/L31
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 819OZ
UT WOS:000294837500006
ER
PT J
AU Binder, B
Williams, BF
Eracleous, M
Seth, AC
Dalcanton, JJ
Skillman, ED
Weisz, DR
Anderson, SF
Gaetz, TJ
Plucinsky, PP
AF Binder, B.
Williams, B. F.
Eracleous, M.
Seth, A. C.
Dalcanton, J. J.
Skillman, E. D.
Weisz, D. R.
Anderson, S. F.
Gaetz, T. J.
Plucinsky, P. P.
TI A DEEP CHANDRA VIEW OF THE NGC 404 CENTRAL ENGINE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 404); galaxies: nuclei;
X-rays: general
ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES;
BLACK-HOLE BINARIES; X-RAY; BRIGHTNESS PROFILES; ELLIPTIC GALAXIES;
SPIRAL GALAXIES; NEARBY GALAXIES; LINER GALAXIES
AB We present the results of a 100 ks Chandra observation of the NGC 404 nuclear region. The long exposure and excellent spatial resolution of Chandra have enabled us to critically examine the nuclear environment of NGC 404, which is known to host a nuclear star cluster and potentially an intermediate-mass black hole (IMBH; on the order of a few times 10(5) M-circle dot). We find two distinct X-ray sources: a hard, central point source coincident with the optical and radio centers of the galaxy, and a soft extended region that is coincident with areas of high H alpha emission and likely recent star formation. When we fit the 0.3-8 keV spectra of each region separately, we find the hard nuclear point source to be dominated by a power law (Gamma = 1.88), while the soft off-nuclear region is best fit by a thermal plasma model (kT = 0.67 keV). We therefore find evidence for both a power-law component and hot gas in the nuclear region of NGC 404. We estimate the 2-10 keV luminosity to be 1.3(-0.5)(+0.8) x 10(37) erg s(-1). A low level of diffuse X-ray emission was detected out to similar to 15 '' (similar to 0.2 kpc) from the nucleus. We compare our results to the observed relationships between power-law photon index and Eddington ratio for both X-ray binaries and low-luminosity active galaxies and find NGC 404 to be consistent with other low-luminosity active galaxies. We therefore favor the conclusion that NGC 404 harbors an IMBH accreting at a very low level.
C1 [Binder, B.; Williams, B. F.; Dalcanton, J. J.; Weisz, D. R.; Anderson, S. F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Eracleous, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Eracleous, M.] Penn State Univ, Ctr Gravitat Wave Phys, University Pk, PA 16802 USA.
[Seth, A. C.; Gaetz, T. J.; Plucinsky, P. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Skillman, E. D.; Weisz, D. R.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
RP Binder, B (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
FU Chandra [GO1-12118X]; NASA [NAS8-03060]
FX The authors thank the anonymous referee for helpful comments. B. Binder
and B. F. Williams acknowledge support from Chandra grant GO1-12118X. T.
Gaetz and P. P. Plucinsky acknowledge support of NASA Contract
NAS8-03060.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 77
DI 10.1088/0004-637X/737/2/77
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600031
ER
PT J
AU Blanton, EL
Randall, SW
Clarke, TE
Sarazin, CL
McNamara, BR
Douglass, EM
McDonald, M
AF Blanton, E. L.
Randall, S. W.
Clarke, T. E.
Sarazin, C. L.
McNamara, B. R.
Douglass, E. M.
McDonald, M.
TI A VERY DEEP CHANDRA OBSERVATION OF A2052: BUBBLES, SHOCKS, AND SLOSHING
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: general; galaxies: clusters:
individual (A2052); galaxies: clusters: intracluster medium; radio
continuum: galaxies; X-rays: galaxies: clusters
ID FLOW CLUSTER ABELL-2052; GALACTIC NUCLEUS FEEDBACK; RAY-EMITTING GAS;
X-RAY; GALAXY CLUSTERS; COOLING FLOWS; COLD FRONTS; PERSEUS CLUSTER;
GASEOUS ATMOSPHERE; RADIO-SOURCE
AB We present the first results from a very deep (similar to 650 ks) Chandra X-ray observation of A2052, as well as archival Very Large Array radio observations. The data reveal detailed structure in the inner parts of the cluster, including bubbles evacuated by radio lobes of the active galactic nucleus (AGN), compressed bubble rims, filaments, and loops. Two concentric shocks are seen, and a temperature rise is measured for the innermost one. On larger scales, we report the first detection of an excess surface brightness spiral feature. The spiral has cooler temperatures, lower entropies, and higher abundances than its surroundings, and is likely the result of sloshing gas initiated by a previous cluster-cluster or sub-cluster merger. Initial evidence for previously unseen bubbles at larger radii related to earlier outbursts from the AGN is presented.
C1 [Blanton, E. L.; Douglass, E. M.] Boston Univ, Dept Astron, Boston, MA 02215 USA.
[Blanton, E. L.; Randall, S. W.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA.
[Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA.
[McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada.
[Douglass, E. M.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada.
[McDonald, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Blanton, E. L.; Douglass, E. M.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
RP Blanton, EL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM eblanton@bu.edu; srandall@head.cfa.harvard.edu;
tracy.clarke@nrl.navy.mil; sarazin@virginia.edu;
mcnamara@sciborg.uwaterloo.ca; emdoug@bu.edu; mcdonald@astro.umd.edu
RI Blanton, Elizabeth/H-4501-2014;
OI Randall, Scott/0000-0002-3984-4337
FU National Aeronautics and Space Administration [GO9-0147X]; Chandra X-ray
Center through NASA [NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration, through Chandra Award Number GO9-0147X. Basic research
in radio astronomy at the Naval Research Laboratory is supported by 6.1
Base funding. S. W. R. was supported in part by the Chandra X-ray Center
through NASA contract NAS8-03060. We thank Frazer Owen for useful
discussions.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 99
DI 10.1088/0004-637X/737/2/99
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600053
ER
PT J
AU Goldsmith, PF
Liseau, R
Bell, TA
Black, JH
Chen, JH
Hollenbach, D
Kaufman, MJ
Li, D
Lis, DC
Melnick, G
Neufeld, D
Pagani, L
Snell, R
Benz, AO
Bergin, E
Bruderer, S
Caselli, P
Caux, E
Encrenaz, P
Falgarone, E
Gerin, M
Goicoechea, JR
Hjalmarson, A
Larsson, B
Le Bourlot, J
Le Petit, F
De Luca, M
Nagy, Z
Roueff, E
Sandqvist, A
van der Tak, F
van Dishoeck, EF
Vastel, C
Viti, S
Yildiz, U
AF Goldsmith, Paul F.
Liseau, Rene
Bell, Tom A.
Black, John H.
Chen, Jo-Hsin
Hollenbach, David
Kaufman, Michael J.
Li, Di
Lis, Dariusz C.
Melnick, Gary
Neufeld, David
Pagani, Laurent
Snell, Ronald
Benz, Arnold O.
Bergin, Edwin
Bruderer, Simon
Caselli, Paola
Caux, Emmanuel
Encrenaz, Pierre
Falgarone, Edith
Gerin, Maryvonne
Goicoechea, Javier R.
Hjalmarson, Ake
Larsson, Bengt
Le Bourlot, Jacques
Le Petit, Franck
De Luca, Massimo
Nagy, Zsofia
Roueff, Evelyne
Sandqvist, Aage
van der Tak, Floris
van Dishoeck, Ewine F.
Vastel, Charlotte
Viti, Serena
Yildiz, Umut
TI HERSCHEL* MEASUREMENTS OF MOLECULAR OXYGEN IN ORION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: abundances; ISM: individual objects (Orion); ISM:
molecules; submillimeter: ISM
ID DENSE INTERSTELLAR CLOUDS; WAVE-ASTRONOMY-SATELLITE; INTER-STELLAR
CLOUDS; GAS-PHASE CHEMISTRY; DISSOCIATIVE RECOMBINATION; APERTURE
SYNTHESIS; O-2 ABUNDANCE; UPPER LIMITS; ROTATIONAL-EXCITATION;
INELASTIC-COLLISIONS
AB We report observations of three rotational transitions of molecular oxygen (O-2) in emission from the H-2 Peak 1 position of vibrationally excited molecular hydrogen in Orion. We observed the 487 GHz, 774 GHz, and 1121 GHz lines using the Heterodyne Instrument for the Far Infrared on the Herschel Space Observatory, having velocities of 11 km s(-1) to 12 km s(-1) and widths of 3 km s(-1). The beam-averaged column density is N(O-2) = 6.5 x 10(16) cm(-2), and assuming that the source has an equal beam-filling factor for all transitions (beam widths 44, 28, and 19 ''), the relative line intensities imply a kinetic temperature between 65 K and 120 K. The fractional abundance of O-2 relative to H-2 is (0.3-7.3) x 10(-6). The unusual velocity suggests an association with a similar to 5 '' diameter source, denoted Peak A, the Western Clump, or MF4. The mass of this source is similar to 10 M-circle dot and the dust temperature is >= 150 K. Our preferred explanation of the enhanced O-2 abundance is that dust grains in this region are sufficiently warm (T >= 100 K) to desorb water ice and thus keep a significant fraction of elemental oxygen in the gas phase, with a significant fraction as O-2. For this small source, the line ratios require a temperature >= 180 K. The inferred O-2 column density similar or equal to 5 x 10(18) cm(-2) can be produced in Peak A, having N(H-2) similar or equal to 4 x 10(24) cm(-2). An alternative mechanism is a low-velocity (10-15 km s(-1)) C-shock, which can produce N(O-2) up to 10(17) cm(-2).
C1 [Goldsmith, Paul F.; Chen, Jo-Hsin; Li, Di] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Liseau, Rene; Black, John H.; Hjalmarson, Ake] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden.
[Bell, Tom A.; Goicoechea, Javier R.] CSIC INTA, Ctr Astrobiol, Madrid 28850, Spain.
[Hollenbach, David] SETI Inst, Mountain View, CA 94043 USA.
[Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Lis, Dariusz C.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA.
[Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Pagani, Laurent; Encrenaz, Pierre] Observ Paris, CNRS, UMR8112, F-75014 Paris, France.
[Pagani, Laurent; Encrenaz, Pierre] LERMA, F-75014 Paris, France.
[Snell, Ronald] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Benz, Arnold O.; Bruderer, Simon] ETH, Inst Astron, CH-8092 Zurich, Switzerland.
[Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England.
[Caux, Emmanuel; Vastel, Charlotte] Univ Toulouse, UPS OMP, IRAP, Toulouse, France.
[Caux, Emmanuel; Vastel, Charlotte] IRAP, CNRS, F-31028 Toulouse 4, France.
[Falgarone, Edith; Gerin, Maryvonne] Ecole Normale Super, F-75231 Paris 05, France.
[Falgarone, Edith; Gerin, Maryvonne] Observ Paris, UMR8112, CNRS, LRA LERMA, F-75231 Paris 05, France.
[Larsson, Bengt; Sandqvist, Aage] Stockholm Univ, AlbaNova Univ Ctr, Stockholm Observ, SE-10691 Stockholm, Sweden.
[Le Bourlot, Jacques; Le Petit, Franck; De Luca, Massimo; Roueff, Evelyne] LUTH, Observ Paris, Paris, France.
[Nagy, Zsofia; van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands.
[Nagy, Zsofia; van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands.
[van Dishoeck, Ewine F.; Yildiz, Umut] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Viti, Serena] UCL, Dept Phys & Astron, London, England.
RP Goldsmith, PF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Paul.F.Goldsmith@jpl.nasa.gov
RI Yildiz, Umut/C-5257-2011; Goldsmith, Paul/H-3159-2016
OI Yildiz, Umut/0000-0001-6197-2864;
FU NSF [AST-0540882]; National Aeronautics and Space Administration
FX We are indebted to the many people who worked so hard and for so long to
make the Herschel mission and the HIFI instrument a success. HIFI has
been designed and built by a consortium of institutes and university
departments from across Europe, Canada, and the US under the leadership
of SRON Netherlands Institute for Space Research, Groningen, The
Netherlands with major contributions from Germany, France, and the US
Consortium members are Canada: CSA, U. Waterloo; France: CESR, LAB,
LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy:
ASI, IFSI-INAF, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK;
Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia
(CSIC-INTA); Sweden: Chalmers University of Technology-MC2, RSS, & GARD,
Onsala Space Observatory, Swedish National Space Board, Stockholm
University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA:
Caltech, JPL, NHSC. The O2 excitation calculations were
carried out using the RADEX code (Van der Tak et al. 2007). We
appreciate the effort that went into making critical spectroscopic data
available through the Jet Propulsion Laboratory Molecular Spectroscopy
Data Base (http://spec.jpl.nasa.gov/), the Cologne Database for
Molecular Spectroscopy, (http://www.astro.uni-koeln.de/cdms/and Muller
et al. 2001) and the Leiden Atomic and Molecular Database
(http://www.strw.leidenuniv.nl/similar to moldata/ and Schoier et al.
2005). We thank Holger Muller for helpful discussions about molecular
spectroscopy. Colin Borys of the NASA Herschel Science Center gave us
valuable assistance in unraveling the pointing offsets of the two HIFI
polarization beams. We thank Nathaniel Cuningham and John Bally for
sending us the FITS image used to make Figure 2. We appreciate the input
from John Pearson and Harshal Gupta in terms of useful discussions about
molecular structure and astrophysics. Volker Tolls provided valuable
information about the WBS noise bandwidth and noise after combining WBS
spectral channels. We have benefited from discussions with D. Quan about
grain warmup and its impact on molecular cloud chemistry. The Caltech
Submillimeter Observatory is supported by the NSF under award
AST-0540882. This work was carried out in part at the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. We thank K. Oberg for
helpful information on desorption of molecules from grains, and the
referee for a number of valuable suggestions.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 96
DI 10.1088/0004-637X/737/2/96
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600050
ER
PT J
AU Jee, MJ
Dawson, KS
Hoekstra, H
Perlmutter, S
Rosati, P
Brodwin, M
Suzuki, N
Koester, B
Postman, M
Lubin, L
Meyers, J
Stanford, SA
Barbary, K
Barrientos, F
Eisenhardt, P
Ford, HC
Gilbank, DG
Gladders, MD
Gonzalez, A
Harris, DW
Huang, X
Lidman, C
Rykoff, ES
Rubin, D
Spadafora, AL
AF Jee, M. J.
Dawson, K. S.
Hoekstra, H.
Perlmutter, S.
Rosati, P.
Brodwin, M.
Suzuki, N.
Koester, B.
Postman, M.
Lubin, L.
Meyers, J.
Stanford, S. A.
Barbary, K.
Barrientos, F.
Eisenhardt, P.
Ford, H. C.
Gilbank, D. G.
Gladders, M. D.
Gonzalez, A.
Harris, D. W.
Huang, X.
Lidman, C.
Rykoff, E. S.
Rubin, D.
Spadafora, A. L.
TI SCALING RELATIONS AND OVERABUNDANCE OF MASSIVE CLUSTERS AT z greater
than or similar to 1 FROM WEAK-LENSING STUDIES WITH THE HUBBLE SPACE
TELESCOPE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology: observations; dark matter; galaxies: clusters: general;
galaxies: high-redshift; gravitational lensing: weak; X-rays: galaxies:
clusters
ID IRAC SHALLOW SURVEY; CHANDRA X-RAY; CHARGE-TRANSFER INEFFICIENCY;
RELAXED GALAXY CLUSTERS; COLOR-MAGNITUDE DIAGRAM; HIGH-REDSHIFT
CLUSTERS; PIXEL-BASED CORRECTION; DARK-MATTER; ADVANCED CAMERA;
RED-SEQUENCE
AB We present weak gravitational lensing analysis of 22 high-redshift (z greater than or similar to 1) clusters based on Hubble Space Telescope images. Most clusters in our sample provide significant lensing signals and are well detected in their reconstructed two-dimensional mass maps. Combining the current results and our previous weak-lensing studies of five other high-z clusters, we compare gravitational lensing masses of these clusters with other observables. We revisit the question whether the presence of the most massive clusters in our sample is in tension with the current. CDM structure formation paradigm. We find that the lensing masses are tightly correlated with the gas temperatures and establish, for the first time, the lensing mass-temperature relation at z greater than or similar to 1. For the power-law slope of the M-T-X relation (M proportional to T-alpha), we obtain alpha = 1.54 +/- 0.23. This is consistent with the theoretical self-similar prediction alpha = 3/2 and with the results previously reported in the literature for much lower redshift samples. However, our normalization is lower than the previous results by 20%-30%, indicating that the normalization in the M-T-X relation might evolve. After correcting for Eddington bias and updating the discovery area with a more conservative choice, we find that the existence of the most massive clusters in our sample still provides a tension with the current. CDM model. The combined probability of finding the four most massive clusters in this sample after the marginalization over cosmological parameters is less than 1%.
C1 [Jee, M. J.; Lubin, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Dawson, K. S.; Harris, D. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands.
[Perlmutter, S.; Suzuki, N.; Meyers, J.; Barbary, K.; Huang, X.; Rykoff, E. S.; Rubin, D.; Spadafora, A. L.] EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA.
[Rosati, P.] European So Observ, D-85748 Garching, Germany.
[Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Koester, B.; Gladders, M. D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Postman, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA.
[Barbary, K.; Rubin, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Barrientos, F.] Univ Catolica Chile, Dept Astron & Astrophys, Santiago, Chile.
[Eisenhardt, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Ford, H. C.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Gilbank, D. G.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada.
[Gonzalez, A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Lidman, C.] Australian Astron Observ, Epping, NSW 1710, Australia.
RP Jee, MJ (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA.
RI Perlmutter, Saul/I-3505-2015;
OI Perlmutter, Saul/0000-0002-4436-4661; Hoekstra, Henk/0000-0002-0641-3231
FU NASA [NAS 5-26555, 9290, 9919, 10496, GO-10496]; TABASGO foundation;
Office of Science, Office of High Energy and Nuclear Physics, of the
U.S. Department of Energy [AC02-05CH11231]; JSPS [20040003]; Netherlands
Organisation for Scientific Research (NWO); Marie Curie International
Reintegration Grant; DFG; W. M. Keck Foundation; U.S. Department of
Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48];
[DE-AC52-07NA27344]
FX Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained at the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS 5-26555, under program 9290, 9919, and 10496.; M.J.J.
acknowledges support for the current research from the TABASGO
foundation presented in the form of the Large Synoptic Survey Telescope
Cosmology Fellowship. Financial support for this work was in part
provided by NASA through program GO-10496 from the Space Telescope
Science Institute, which is operated by AURA, Inc., under NASA contract
NAS 5-26555. This work was also supported in part by the Director,
Office of Science, Office of High Energy and Nuclear Physics, of the U.
S. Department of Energy under Contract No. AC02-05CH11231, as well as a
JSPS core-to-core program "International Research Network for Dark
Energy" and by JSPS research grant 20040003. H.H. acknowledges support
from the Netherlands Organisation for Scientific Research (NWO) through
a VIDI grant. H. H. is also supported by a Marie Curie International
Reintegration Grant. P. R. acknowledges partial support by the DFG
cluster of excellence Origin and Structure of the Universe. Support for
M. B. was provided by the W. M. Keck Foundation. The work of S.A.S. was
performed under the auspices of the U.S. Department of Energy by
Lawrence Livermore National Laboratory in part under Contract
W-7405-Eng-48 and in part under Contract DE-AC52-07NA27344. The work of
P. E. was carried out at the Jet Propulsion Laboratory, California
Institute of Technology, under a contract with NASA.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 59
DI 10.1088/0004-637X/737/2/59
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600013
ER
PT J
AU Liu, X
Shen, Y
Strauss, MA
Hao, L
AF Liu, Xin
Shen, Yue
Strauss, Michael A.
Hao, Lei
TI ACTIVE GALACTIC NUCLEUS PAIRS FROM THE SLOAN DIGITAL SKY SURVEY. I. THE
FREQUENCY ON similar to 5-100 kpc SCALES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: interactions; galaxies:
nuclei; quasars: general
ID SUPERMASSIVE BLACK-HOLES; SPECTROSCOPIC TARGET SELECTION; STAR-FORMING
GALAXIES; NARROW-LINE REGION; 7TH DATA RELEASE; SIMILAR-TO 3-4; HOST
GALAXIES; BINARY QUASARS; METALLICITY RELATION; FORMATION HISTORIES
AB Galaxy-galaxy mergers and close interactions have long been regarded as a viable mechanism for channeling gas toward the central supermassive black holes (SMBHs) of galaxies which are triggered as active galactic nuclei (AGNs). AGN pairs, in which the central SMBHs of a galaxy merger are both active, are expected to be common from such events. We conduct a systematic study of 1286 AGN pairs at (z) over bar similar to 0.1 with line-of-sight velocity offsets Delta v < 600 km s(-1) and projected separations r(p) < 100 h(70)(-1) kpc, selected from the Seventh Data Release of the Sloan Digital Sky Survey (SDSS). This AGN pair sample was drawn from 138,070 AGNs optically identified based on diagnostic emission line ratios and/or line widths. The fraction of AGN pairs with 5 h(70)(-1) kpc less than or similar to r(p) < 100 h(70)(-1) kpc among all spectroscopically selected AGNs at 0.02 < z < 0.16 is 3.6% after correcting for SDSS spectroscopic incompleteness; similar to 30% of these pairs show morphological tidal features in their SDSS images, and the fraction becomes greater than or similar to 80% for pairs with the brightest nuclei. Our sample increases the number of known AGN pairs on these scales by more than an order of magnitude. We study their AGN and host-galaxy star formation properties in a companion paper.
C1 [Liu, Xin; Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Liu, Xin; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Hao, Lei] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China.
RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NSF [AST-0707266]; NASA through Chandra X-ray Center [PF0-110076];
Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; Smithsonian
Astrophysical Observatory; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England; American Museum of Natural
History; Astrophysical Institute Potsdam; University of Basel;
University of Cambridge; Case Western Reserve University; University of
Chicago; Drexel University; Fermilab; Institute for Advanced Study;
Japan Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington
FX We thank J. Greene and P. Kampczyk for helpful comments, and an
anonymous referee for a prompt and careful report. We are grateful to
the MPA-JHU team, especially J. Brinchmann, who have made their catalog
of derived galaxy properties publicly available. X. L. and M. A. S.
acknowledge the support of NSF grant AST-0707266. Support for the work
of X. L. was provided by NASA through an Einstein Postdoctoral
Fellowship grant number PF0-110076 awarded by the Chandra X-ray Center,
which is operated by the Smithsonian Astrophysical Observatory for NASA
under contract NAS8-03060. Y.S. acknowledges support from a Clay
Postdoctoral Fellowship through the Smithsonian Astrophysical
Observatory.; 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 website is www.sdss.org/.; The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the American Museum of Natural
History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory, and the University of
Washington.
NR 99
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
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AR 101
DI 10.1088/0004-637X/737/2/101
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600055
ER
PT J
AU Marriage, TA
Acquaviva, V
Ade, PAR
Aguirre, P
Amiri, M
Appel, JW
Barrientos, LF
Battistelli, ES
Bond, JR
Brown, B
Burger, B
Chervenak, J
Das, S
Devlin, MJ
Dicker, SR
Doriese, WB
Dunkley, J
Dunner, R
Essinger-Hileman, T
Fisher, RP
Fowler, JW
Hajian, A
Halpern, M
Hasselfield, M
Hernandez-Monteagudo, C
Hilton, GC
Hilton, M
Hincks, AD
Hlozek, R
Huffenberger, KM
Hughes, DH
Hughes, JP
Infante, L
Irwin, KD
Juin, JB
Kaul, M
Klein, J
Kosowsky, A
Lau, JM
Limon, M
Lin, YT
Lupton, RH
Marsden, D
Martocci, K
Mauskopf, P
Menanteau, F
Moodley, K
Moseley, H
Netterfield, CB
Niemack, MD
Nolta, MR
Page, LA
Parker, L
Partridge, B
Quintana, H
Reese, ED
Reid, B
Sehgal, N
Sherwin, BD
Sievers, J
Spergel, DN
Staggs, ST
Swetz, DS
Switzer, ER
Thornton, R
Trac, H
Tucker, C
Warne, R
Wilson, G
Wollack, E
Zhao, Y
AF Marriage, Tobias A.
Acquaviva, Viviana
Ade, Peter A. R.
Aguirre, Paula
Amiri, Mandana
Appel, John William
Felipe Barrientos, L.
Battistelli, Elia S.
Bond, J. Richard
Brown, Ben
Burger, Bryce
Chervenak, Jay
Das, Sudeep
Devlin, Mark J.
Dicker, Simon R.
Doriese, W. Bertrand
Dunkley, Joanna
Duenner, Rolando
Essinger-Hileman, Thomas
Fisher, Ryan P.
Fowler, Joseph W.
Hajian, Amir
Halpern, Mark
Hasselfield, Matthew
Hernandez-Monteagudo, Carlos
Hilton, Gene C.
Hilton, Matt
Hincks, Adam D.
Hlozek, Renee
Huffenberger, Kevin M.
Handel Hughes, David
Hughes, John P.
Infante, Leopoldo
Irwin, Kent D.
Baptiste Juin, Jean
Kaul, Madhuri
Klein, Jeff
Kosowsky, Arthur
Lau, Judy M.
Limon, Michele
Lin, Yen-Ting
Lupton, Robert H.
Marsden, Danica
Martocci, Krista
Mauskopf, Phil
Menanteau, Felipe
Moodley, Kavilan
Moseley, Harvey
Netterfield, Calvin B.
Niemack, Michael D.
Nolta, Michael R.
Page, Lyman A.
Parker, Lucas
Partridge, Bruce
Quintana, Hernan
Reese, Erik D.
Reid, Beth
Sehgal, Neelima
Sherwin, Blake D.
Sievers, Jon
Spergel, David N.
Staggs, Suzanne T.
Swetz, Daniel S.
Switzer, Eric R.
Thornton, Robert
Trac, Hy
Tucker, Carole
Warne, Ryan
Wilson, Grant
Wollack, Ed
Zhao, Yue
TI THE ATACAMA COSMOLOGY TELESCOPE: SUNYAEV-ZEL'DOVICH-SELECTED GALAXY
CLUSTERS AT 148 GHz IN THE 2008 SURVEY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; galaxies:
clusters: general; radio continuum: general; surveys
ID SOUTH-POLE TELESCOPE; BACKGROUND POWER SPECTRUM; COSMIC DISTANCE SCALE;
X-RAY MEASUREMENTS; HUBBLE CONSTANT; LENSING MEASUREMENTS; PRESSURE
PROFILE; SOURCE CATALOG; DARK ENERGY; CONSTRAINTS
AB We report on 23 clusters detected blindly as Sunyaev-Zel'dovich (SZ) decrements in a 148 GHz, 455 deg(2) map of the southern sky made with data from the Atacama Cosmology Telescope 2008 observing season. All SZ detections announced in this work have confirmed optical counterparts. Ten of the clusters are new discoveries. One newly discovered cluster, ACT-CL J0102-4915, with a redshift of 0.75 ( photometric), has an SZ decrement comparable to the most massive systems at lower redshifts. Simulations of the cluster recovery method reproduce the sample purity measured by optical follow-up. In particular, for clusters detected with a signal-to-noise ratio greater than six, simulations are consistent with optical follow-up that demonstrated this subsample is 100% pure. The simulations further imply that the total sample is 80% complete for clusters with mass in excess of 6 x 10(14) solar masses referenced to the cluster volume characterized by 500 times the critical density. The Compton y-X-ray luminosity mass comparison for the 11 best-detected clusters visually agrees with both self-similar and non-adiabatic, simulation-derived scaling laws.
C1 [Marriage, Tobias A.; Acquaviva, Viviana; Das, Sudeep; Dunkley, Joanna; Hajian, Amir; Lin, Yen-Ting; Lupton, Robert H.; Spergel, David N.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Acquaviva, Viviana; Hughes, John P.; Menanteau, Felipe] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
[Ade, Peter A. R.; Mauskopf, Phil; Tucker, Carole] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Aguirre, Paula; Felipe Barrientos, L.; Duenner, Rolando; Infante, Leopoldo; Baptiste Juin, Jean; Lin, Yen-Ting; Quintana, Hernan] Pontificia Univ Catolica Chile, Fac Fis, Dept Astron & Astrofis, Santiago 22, Chile.
[Amiri, Mandana; Battistelli, Elia S.; Burger, Bryce; Halpern, Mark; Hasselfield, Matthew] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z4, Canada.
[Appel, John William; Das, Sudeep; Dunkley, Joanna; Essinger-Hileman, Thomas; Fisher, Ryan P.; Fowler, Joseph W.; Hajian, Amir; Hincks, Adam D.; Lau, Judy M.; Limon, Michele; Martocci, Krista; Niemack, Michael D.; Page, Lyman A.; Parker, Lucas; Reid, Beth; Sherwin, Blake D.; Staggs, Suzanne T.; Switzer, Eric R.; Zhao, Yue] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA.
[Battistelli, Elia S.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy.
[Bond, J. Richard; Hajian, Amir; Nolta, Michael R.; Sievers, Jon] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Brown, Ben; Kosowsky, Arthur] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Chervenak, Jay; Moseley, Harvey; Wollack, Ed] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Das, Sudeep] Univ Calif Berkeley, LBL, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Das, Sudeep] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Devlin, Mark J.; Dicker, Simon R.; Kaul, Madhuri; Klein, Jeff; Limon, Michele; Marsden, Danica; Reese, Erik D.; Swetz, Daniel S.; Thornton, Robert] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Doriese, W. Bertrand; Fowler, Joseph W.; Hilton, Gene C.; Irwin, Kent D.; Niemack, Michael D.; Swetz, Daniel S.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[Dunkley, Joanna; Hlozek, Renee] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England.
[Hernandez-Monteagudo, Carlos] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Hilton, Matt; Moodley, Kavilan; Warne, Ryan] Univ KwaZulu Natal, Sch Math Sci, Astrophys & Cosmol Res Unit, ZA-4041 Durban, South Africa.
[Hilton, Matt; Moodley, Kavilan] Ctr High Performance Comp, Rosebank, Cape Town, South Africa.
[Huffenberger, Kevin M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA.
[Handel Hughes, David] INAOE, Puebla, Mexico.
[Lau, Judy M.; Sehgal, Neelima] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Lau, Judy M.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
[Limon, Michele] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
[Lin, Yen-Ting] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan.
[Martocci, Krista] Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Netterfield, Calvin B.; Switzer, Eric R.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
[Partridge, Bruce] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA.
[Reid, Beth] Univ Barcelona, ICC, E-08028 Barcelona, Spain.
[Thornton, Robert] W Chester Univ Penn, Dept Phys, W Chester, PA 19383 USA.
[Trac, Hy] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
[Trac, Hy] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Wilson, Grant] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Marriage, TA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RI Klein, Jeffrey/E-3295-2013; Spergel, David/A-4410-2011; Hilton, Matthew
James/N-5860-2013; Trac, Hy/N-8838-2014; Wollack, Edward/D-4467-2012;
OI Trac, Hy/0000-0001-6778-3861; Wollack, Edward/0000-0002-7567-4451;
Huffenberger, Kevin/0000-0001-7109-0099; Menanteau,
Felipe/0000-0002-1372-2534; Sievers, Jonathan/0000-0001-6903-5074;
Limon, Michele/0000-0002-5900-2698
FU U.S. National Science Foundation [AST-0408698, PHY-0355328, AST-0707731,
PIRE-0507768]; Comision Nacional de Investigacion Cientifica y
Technologica de Chile (CONICYT); Princeton University; University of
Pennsylvania; Canada Foundation for Innovation under the Compute Canada;
Government of Ontario; Ontario Research Fund-Research Excellence;
University of Toronto; NASA [NNX08AH30G]; FONDECYT [3085031]; Natural
Science and Engineering Research Council of Canada (NSERC); NSF
[AST-0546035, AST-0606975]; FONDAP Centro de Astrofisica; U.S.
Department of Energy [DE-AC3-76SF00515]; CONICYT; MECESUP; Fundacion
Andes; Rhodes Trust; NSF Physics Frontier Center [PHY-0114422]; World
Premier International Research Center Initiative, MEXT, Japan
FX The ACT project was proposed in 2000 and funded by the U.S. National
Science Foundation on 2004 January 1. Many have contributed to the
project since its inception. We especially wish to thank Asad Aboobaker,
Christine Allen, Dominic Benford, Paul Bode, Kristen Burgess, Angelica
de Oliveira-Costa, Sean Frazier, Nick Hand, Peter Hargrave, Norm
Jarosik, Amber Miller, Carl Reintsema, Felipe Rojas, Uros Seljak, Martin
Spergel, Johannes Staghun, Carl Stahle, Max Tegmark, Masao Uehara,
Katerina Visnjic, and Ed Wishnow. It is a pleasure to acknowledge Bob
Margolis, ACT's project manager. Reed Plimpton and David Jacobson worked
at the telescope during the 2008 season. Naoki Itoh and Satoshi Nozawa
provided code for calculating relativistic corrections to the SZ. ACT
operates in the Parque Astronomico Atacama in northern Chile under the
auspices of Programa de Astronomia, a program of the Comision Nacional
de Investigacion Cientifica y Technologica de Chile (CONICYT).; This
work was supported by the U.S. National Science Foundation through
awards AST-0408698 for the ACT project, and PHY-0355328, AST-0707731,
and PIRE-0507768. Funding was also provided by Princeton University and
the University of Pennsylvania. The PIRE program made possible exchanges
between Chile, South Africa, Spain, and the United States that enabled
this research program. Computations were performed on the GPC
supercomputer at the SciNet HPC Consortium. SciNet is funded by the
Canada Foundation for Innovation under the auspices of Compute Canada;
the Government of Ontario; Ontario Research Fund-Research Excellence;
and the University of Toronto.; T.M. was supported through NASA grant
NNX08AH30G. J.B.J. was supported by the FONDECYT grant 3085031. A.D.H.
received additional support from a Natural Science and Engineering
Research Council of Canada (NSERC) PGS-D scholarship. A.K. and B.P. were
partially supported through NSF AST-0546035 and AST-0606975,
respectively, for work on ACT. H.Q. and L.I. acknowledge partial support
from FONDAP Centro de Astrofisica. N.S. is supported by the U.S.
Department of Energy contract to SLAC no. DE-AC3-76SF00515. R.D. was
supported by CONICYT, MECESUP, and Fundacion Andes. R.H. was supported
by the Rhodes Trust. E.S. acknowledges support by NSF Physics Frontier
Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics.
Y.T.L. acknowledges support from the World Premier International
Research Center Initiative, MEXT, Japan. The ACT data will be made
public through LAMBDA (http://lambda.gsfc.nasa.gov/) and the ACT Web
site (http://www.physics.princeton.edu/act/).
NR 72
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
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AR 61
DI 10.1088/0004-637X/737/2/61
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600015
ER
PT J
AU Neilsen, J
Remillard, RA
Lee, JC
AF Neilsen, Joseph
Remillard, Ronald A.
Lee, Julia C.
TI THE PHYSICS OF THE "HEARTBEAT" STATE OF GRS 1915+105
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries: close; black hole physics;
instabilities; stars: winds, outflows; X-rays: individual (GRS 1915+105)
ID QUASI-PERIODIC OSCILLATION; RELATIVISTIC IRON LINE; COMPTON-HEATED
WINDS; GALACTIC BLACK-HOLE; ACCRETION DISK WIND; X-RAY; RADIO-EMISSION;
MICROQUASAR GRS-1915+105; WARM ABSORBER; JET FORMATION
AB We present the first detailed phase-resolved spectral analysis of a joint Chandra High-Energy Transmission Grating Spectrometer and Rossi X-ray Timing Explorer observation of the. variability class in the microquasar GRS 1915+105. The rho cycle displays a high-amplitude, double-peaked flare that recurs roughly every 50 s and is sometimes referred to as the "heartbeat" oscillation. The spectral and timing properties of the oscillation are consistent with the radiation pressure instability and the evolution of a local Eddington limit in the inner disk. We exploit strong variations in the X-ray continuum, iron emission lines, and the accretion disk wind to probe the accretion geometry over nearly six orders of magnitude in distance from the black hole. At small scales (1-10 R-g), we detect a burst of bremsstrahlung emission that appears to occur when a portion of the inner accretion disk evaporates due to radiation pressure. Jet activity, as inferred from the appearance of a short X-ray hard state, seems to be limited to times near minimum luminosity, with a duty cycle of similar to 10%. On larger scales (10(5)-10(6) R-g), we use detailed photoionization arguments to track the relationship between the fast X-ray variability and the accretion disk wind. For the first time, we are able to show that changes in the broadband X-ray spectrum produce changes in the structure and density of the accretion disk wind on timescales as short as 5 s. These results clearly establish a causal link between the X-ray oscillations and the disk wind and therefore support the existence of a disk-jet-wind connection. Furthermore, our analysis shows that themass-loss rate in the wind may be sufficient to cause long-term oscillations in the accretion rate, leading to state transitions in GRS 1915+105.
C1 [Neilsen, Joseph; Lee, Julia C.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Neilsen, Joseph; Lee, Julia C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
RP Neilsen, J (reprint author), Harvard Univ, Dept Phys, 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 grant [AR0-11004X]; Harvard University Graduate School of Arts
and Sciences; Harvard University Faculty of Arts and Sciences; NASA
FX We thank the anonymous referee for comments that improved the quality
and clarity of our paper. We thank Claude Canizares, Norbert Schulz, Tim
Kallman, and Mike Nowak for helpful discussions of spectral variability,
and we thank Guy Pooley for making the radio observations publicly
available. J.N. and J.C.L. gratefully acknowledge funding support from
Chandra grant AR0-11004X, the Harvard University Graduate School of Arts
and Sciences, and the Harvard University Faculty of Arts and Sciences;
R.A.R. acknowledges partial support from the NASA contract to MIT for
support of RXTE instruments.
NR 85
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
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PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600023
ER
PT J
AU Schlafly, EF
Finkbeiner, DP
AF Schlafly, Edward F.
Finkbeiner, Douglas P.
TI MEASURING REDDENING WITH SLOAN DIGITAL SKY SURVEY STELLAR SPECTRA AND
RECALIBRATING SFD
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; Galaxy: stellar content; ISM: clouds
ID DATA RELEASE; ULTRAVIOLET EXTINCTION; OPEN CLUSTERS; STARS; SEGUE;
TELESCOPE; CALIBRATION; VALIDATION; SDSS
AB We present measurements of dust reddening using the colors of stars with spectra in the Sloan Digital Sky Survey. We measure reddening as the difference between the measured and predicted colors of a star, as derived from stellar parameters from the Sloan Extension for Galactic Understanding and Exploration Stellar Parameter Pipeline. We achieve uncertainties of 56, 34, 25, and 29 mmag in the colors u - g, g - r, r - i, and i - z, per star, though the uncertainty varies depending on the stellar type and the magnitude of the star. The spectrum-based reddening measurements confirm our earlier "blue tip" reddening measurements, finding reddening coefficients different by -3%, 1%, 1%, and 2% in u - g, g - r, r - i, and i - z from those found by the blue tip method, after removing a 4% normalization difference. These results prefer an R-V = 3.1 Fitzpatrick reddening law to O'Donnell or Cardelli et al. reddening laws. We provide a table of conversion coefficients from the Schlegel et al. (SFD) maps of E(B - V) to extinction in 88 bandpasses for four values of R-V, using this reddening law and the 14% recalibration of SFD first reported by Schlafly et al. and confirmed in this work.
C1 [Schlafly, Edward F.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schlafly, EF (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
OI Schlafly, Edward Ford/0000-0002-3569-7421
FU NASA [NNX10AD69G]; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy
FX David Schlegel suggested using SDSS stellar spectra to measure reddening
several years ago, and his encouragement and advice were invaluable at
the inception of this project. D. F. and E. S. acknowledge support of
NASA grant NNX10AD69G for this research.; Funding for SDSS-III has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Science Foundation, and the U.S. Department
of Energy. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is
managed by the Astrophysical Research Consortium for the Participating
Institutions of the SDSS-III Collaboration including the University of
Arizona, the Brazilian Participation Group, Brookhaven National
Laboratory, University of Cambridge, University of Florida, the French
Participation Group, the German Participation Group, the Instituto de
Astrofisica de Canarias, the Michigan State/Notre Dame/JINA
Participation Group, Johns Hopkins University, Lawrence Berkeley
National Laboratory, Max Planck Institute for Astrophysics, New Mexico
State University, New York University, Ohio State University,
Pennsylvania State University, University of Portsmouth, Princeton
University, the Spanish Participation Group, University of Tokyo,
University of Utah, Vanderbilt University, University of Virginia,
University of Washington, and Yale University.
NR 33
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 103
DI 10.1088/0004-637X/737/2/103
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600057
ER
PT J
AU Volk, K
Hrivnak, BJ
Matsuura, M
Bernard-Salas, J
Szczerba, R
Sloan, GC
Kraemer, KE
van Loon, JT
Kemper, F
Woods, PM
Zijlstra, AA
Sahai, R
Meixner, M
Gordon, KD
Gruendl, RA
Tielens, AGGM
Indebetouw, R
Marengo, M
AF Volk, Kevin
Hrivnak, Bruce J.
Matsuura, Mikako
Bernard-Salas, Jeronimo
Szczerba, Ryszard
Sloan, G. C.
Kraemer, Kathleen E.
van Loon, Jacco Th.
Kemper, F.
Woods, Paul M.
Zijlstra, Albert A.
Sahai, Raghvendra
Meixner, Margaret
Gordon, Karl D.
Gruendl, Robert A.
Tielens, Alexander G. G. M.
Indebetouw, Remy
Marengo, Massimo
TI DISCOVERY AND ANALYSIS OF 21 mu m FEATURE SOURCES IN THE MAGELLANIC
CLOUDS (vol 735, pg 127, 2011)
SO ASTROPHYSICAL JOURNAL
LA English
DT Correction
C1 [Volk, Kevin; Meixner, Margaret; Gordon, Karl D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hrivnak, Bruce J.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA.
[Matsuura, Mikako] UCL, UCL Inst Origins, Dept Phys & Astron, London WC1E 6BT, England.
[Bernard-Salas, Jeronimo] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Szczerba, Ryszard] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Kraemer, Kathleen E.] USAF, Res Lab, AFRL RVBYB, Hanscom AFB, MA 01731 USA.
[van Loon, Jacco Th.] Univ Keele, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Kemper, F.; Woods, Paul M.; Zijlstra, Albert A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gruendl, Robert A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Tielens, Alexander G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Matsuura, Mikako] Univ Coll London, Mullard Space Sci Lab, UCL Inst Origins, Dorking RH5 6NT, Surrey, England.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10647, Taiwan.
[Woods, Paul M.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Marengo, Massimo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Volk, K (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM volk@stsci.edu
NR 1
TC 0
Z9 0
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 20
PY 2011
VL 737
IS 2
AR 107
DI 10.1088/0004-637X/737/2/107
PG 1
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600061
ER
PT J
AU Volonteri, M
Natarajan, P
Gultekin, K
AF Volonteri, Marta
Natarajan, Priyamvada
Gueltekin, Kayhan
TI HOW IMPORTANT IS THE DARK MATTER HALO FOR BLACK HOLE GROWTH?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: evolution; galaxies: formation
ID HIGH-REDSHIFT GALAXIES; GRAVITATIONAL RECOIL; HOST GALAXIES; BULGE MASS;
EVOLUTION; QUASARS; CORRELATE; DISCS; SEEDS; SIGMA
AB In this paper, we examine whether the properties of central black holes in galactic nuclei correlate with their host dark matter halos. We analyze the entire sample of galaxies where black hole mass, velocity dispersion sigma, and asymptotic circular velocity V-c have all been measured. We fit MBH-sigma and M-BH-V-c to a power law, and find that in both relationships the scatter and slope are similar. This model-independent analysis suggests that although the black hole masses are not uniquely determined by dark matter halo mass, when considered for the current sample as a whole, the M-BH-V-c correlation may be as strong (or as weak) as MBH-sigma. Although the data are sparse, there appears to be more scatter in the correlation for both sigma and V-c at the low-mass end. This is not unexpected given our current understanding of galaxy and black hole assembly. In fact, there are several compelling reasons that account for this: (1) supermassive black hole (SMBH) formation is likely less efficient in low-mass galaxies with large angular momentum content, (2) SMBH growth is less efficient in low-mass disk galaxies that have not experienced major mergers, and (3) dynamical effects, such as gravitational recoil, increase scatter preferentially at the low-mass end. Therefore, the recent observational claim of the absence of central SMBHs in bulgeless, low-mass galaxies, or deviations from the correlations defined by high-mass black holes in large galaxies today is, in fact, predicated by current models of black hole growth. We show how this arises as a direct consequence of the coupling between dark matter halos and central black holes at the earliest epochs.
C1 [Volonteri, Marta; Gueltekin, Kayhan] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Natarajan, Priyamvada] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Natarajan, Priyamvada] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
RP Volonteri, M (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
OI Gultekin, Kayhan/0000-0002-1146-0198
FU John Simon Guggenheim Foundation; SAO [TM1-12007X]; NASA [ATP
NNX10AC84G, NNX07AH22G]
FX P.N. thanks the John Simon Guggenheim Foundation for the award of a
Guggenheim fellowship and the Institute for Theory and Computation at
the Harvard Smithsonian Center for Astrophysics for hosting her. M.V.
acknowledges support from SAO Award TM1-12007X and NASA awards ATP
NNX10AC84G and NNX07AH22G.
NR 37
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Z9 54
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 AUG 20
PY 2011
VL 737
IS 2
AR 50
DI 10.1088/0004-637X/737/2/50
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 808WV
UT WOS:000294013600004
ER
PT J
AU Foerder, P
Galloway, M
Barthel, T
Moore, DE
Reiss, D
AF Foerder, Preston
Galloway, Marie
Barthel, Tony
Moore, Donald E., III
Reiss, Diana
TI Insightful Problem Solving in an Asian Elephant
SO PLOS ONE
LA English
DT Article
ID SELF-RECOGNITION; MAXIMUS; INTELLIGENCE; EVOLUTION; BEHAVIOR; BRAIN;
TRUNK
AB The "aha" moment or the sudden arrival of the solution to a problem is a common human experience. Spontaneous problem solving without evident trial and error behavior in humans and other animals has been referred to as insight. Surprisingly, elephants, thought to be highly intelligent, have failed to exhibit insightful problem solving in previous cognitive studies. We tested whether three Asian elephants (Elephas maximus) would use sticks or other objects to obtain food items placed out-of-reach and overhead. Without prior trial and error behavior, a 7-year-old male Asian elephant showed spontaneous problem solving by moving a large plastic cube, on which he then stood, to acquire the food. In further testing he showed behavioral flexibility, using this technique to reach other items and retrieving the cube from various locations to use as a tool to acquire food. In the cube's absence, he generalized this tool utilization technique to other objects and, when given smaller objects, stacked them in an attempt to reach the food. The elephant's overall behavior was consistent with the definition of insightful problem solving. Previous failures to demonstrate this ability in elephants may have resulted not from a lack of cognitive ability but from the presentation of tasks requiring trunk-held sticks as potential tools, thereby interfering with the trunk's use as a sensory organ to locate the targeted food.
C1 [Foerder, Preston; Reiss, Diana] CUNY, Grad Ctr, Biopsychol & Behav Neurosci Program, New York, NY 10021 USA.
[Galloway, Marie; Barthel, Tony; Moore, Donald E., III] Smithsonian Natl Zool Pk, Washington, DC USA.
[Reiss, Diana] CUNY, Hunter Coll, Dept Psychol, New York, NY 10021 USA.
RP Foerder, P (reprint author), CUNY, Grad Ctr, Biopsychol & Behav Neurosci Program, New York, NY 10021 USA.
EM dlr28@columbia.edu
FU Graduate Center of the City University of New York
FX Funding was provided by a Graduate Center of the City University of New
York Doctoral Student Research Grant. The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 32
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Z9 18
U1 13
U2 77
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 AUG 18
PY 2011
VL 6
IS 8
AR e23251
DI 10.1371/journal.pone.0023251
PG 7
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 810LN
UT WOS:000294126900013
PM 21876741
ER
PT J
AU Davis, DR
Mc Kay, F
Oleiro, M
Vitorino, MD
Wheeler, GS
AF Davis, Donald R.
Mc Kay, Fernando
Oleiro, Marina
Vitorino, Marcelo Diniz
Wheeler, Gregory S.
TI BIOLOGY AND SYSTEMATICS OF THE LEAFMINING GRACILLARIIDAE OF BRAZILIAN
PEPPER TREE, SCHINUS TEREBINTHIFOLIUS RADDI, WITH DESCRIPTIONS OF A NEW
GENUS AND FOUR NEW SPECIES)
SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY
LA English
DT Article
DE Adult and larval morphology; larval biology; Anacardiaceae; biological
control; Astronium balansae; Caloptilia coruscans; leaf mining;
hypermetamorphosis; Lithrea molleoides; Morella faya; parasitoid;
Schinus fasciculatus; Schinus lentiscifolius; Schinus weinmannifolius;
Smilacaceae; Smilax; stem mining
ID HOST-SPECIFICITY; LEPIDOPTERA; ANACARDIACEAE; FLORIDA; AGENT
AB Recent surveys in southern Florida, USA, Brazil and Argentina, for biological control agents to assist in the control of the invasive Brazilian peppertree, have discovered several previously unknown species of plant mining Lepidoptera of the family Gracillariidae,. Morphological descriptions with summaries of their biology for the following four new species and one new genus are presented: Caloptilia schinusifolia Davis and Wheeler, from Brazil and possibly Argentina; Eucosmophora schinusivora Davis and Wheeler, from Argentina and Brazil; Leurocephala schinusae Davis and Mc Kay, new genus and species, from Argentina and Brazil; and Marmara habecki Davis, new species, from Florida, USA. The larvae of all four species exhibit a hypermetamorphic development consisting of early instar sapfeeding and later instar tissue feeding stages typical for members of Gracillariidae. Larvae of M. habecki were also observed to possess an additional nonfeeding, transitional instar prior to the final instar as is typical for the genus (Wagner et al. 2000). Larvae of the new genus Leurocephala were discovered to undergo an intermediate, nearly, apodal tissue feeding stage between the sapfeeding and final tissue feeding instars. Unique specimens representing an additional three species of Gracillariidae also have been reared from this tree in Argentina or Brazil, but these could not be identified because of inadequate material. COI barcodes were obtained for Marmara habecki, M. smilacisella, and an undescribed Marmara from Brazil. Each species was separated by a minimum barcode divergence of > 4.5% (Fig. 111).
C1 [Davis, Donald R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
[Mc Kay, Fernando; Oleiro, Marina] ARS, USDA, S Amer Biol Control Lab, RA-1686 Buenos Aires, DF, Argentina.
[Vitorino, Marcelo Diniz] Univ Reg Blumenau FURB, Programa Posgrad Engn Florestal PPGEF, BR-89012900 Blumenau, SC, Brazil.
[Wheeler, Gregory S.] ARS, USDA, Invas Plant Res Lab, Ft Lauderdale, FL 33314 USA.
RP Davis, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA.
EM davisd@si.edu; diniz@furb.br; greg.wheeler@ars.usda.gov
RI Vitorino, Marcelo/C-1952-2013
FU Cenome Canada through the Ontario Genomics Institute; NSERC; Ontario
Ministry of Research and Innovation; Florida Fish and Wildlife
Federation; South Florida Water Management District
FX We wish to thank Young Sohn of the Department of Entomology, Smithsonian
Institution and Diana Marques, Lisbon, Portugal, for the line
illustrations, and Patricia Gentili-Poole of the Department of
Entomology, Smithsonian Institution, who assisted with graphics and
final preparation of plates. SEM images were clone by R Gentili-Poole,
assisted by Scott Whittaker of the SEM Laboratory, National Museum of
Natural History. Mignon Davis of the Department of Entomology,
Smithsonian Institution recorded specimen data and assisted with
specimen CUT-adorn We wish to thank Akito Kawahara for providing DNA
sequence data for specimens provided of Leurocephala schinusae, Deborah
Mathews Lott and the late Dale Habeck of the McGuire Center for
Lepidoptera and Biodiversity, Florida Museum of Natural History,
Gainesville, Florida, for the loan of essential specimens and for
rearing data from Schinus terebiuthifolius. We are indebted to Jason
Weintraub, Academy of Natural Sciences, Philadelphia, and David Wagner,
University of Connecticut, Storrs, CT., for loans of Marmara
smilacisella, and to Frank Howarth, B. P. Bishop Museum, Bernarr
Kumashiro of the Hawaii Department of Agriculture, Honolulu, and Tracy
Johnson of the Institute of Pacific Islands Forestry, USDA Forest
Service, Volcano, Hawaii for the loan of Caloptilia coruscans.
Parasitoid identifications were generously provided by David Wahl of the
American Entomological institute for Ichneumonidae, James Whitfield of
the University of Illinois and Robert Kula of the USDA/ARS Systematic
Entomology Lab for Braconidae, and Michael Gates of the USDA/ARS
Systematic Entomology Lab for Chalcidoidea. The DNA barcode sequences
were generated at the Biodiversity Institute of Ontario with funding to
Paul D.N. Hebert from Cenome Canada through the Ontario Genomics
Institute, NSERC, and the Ontario Ministry of Research and Innovation.
Stephanie Kirk and Jeremy deWaard of the Biodiversity Institute of
Ontario also were helpful in preparing specimens for barcoding.; Lauren
Helgen of the Department of Entomology, Smithsonian Institution assisted
DRD in preparing the Marmara tree, figure HE Wendy Meyers, Citrus
Research and Education Center, University or Florida, Lake Alfred,
Florida provided specimens for identification of Marmara habecki
collected from survey traps. Brazilian insect collections were conducted
under the Instituto Brasileiro do Meio Ambiente IBAMA permits. This
project was partially funded by Florida Fish and Wildlife Federation and
South Florida Water Management District.
NR 54
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U1 1
U2 10
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 AUG 17
PY 2011
VL 65
IS 2
BP 61
EP 93
PG 33
WC Entomology
SC Entomology
GA 812VM
UT WOS:000294321000001
ER
PT J
AU Barkley, MP
Palmer, PI
Ganzeveld, L
Arneth, A
Hagberg, D
Karl, T
Guenther, A
Paulot, F
Wennberg, PO
Mao, JQ
Kurosu, TP
Chance, K
Muller, JF
De Smedt, I
Van Roozendael, M
Chen, D
Wang, YX
Yantosca, RM
AF Barkley, Michael P.
Palmer, Paul I.
Ganzeveld, Laurens
Arneth, Almut
Hagberg, Daniel
Karl, Thomas
Guenther, Alex
Paulot, Fabien
Wennberg, Paul O.
Mao, Jingqiu
Kurosu, Thomas P.
Chance, Kelly
Mueller, J. -F.
De Smedt, Isabelle
Van Roozendael, Michel
Chen, Dan
Wang, Yuxuan
Yantosca, Robert M.
TI Can a "state of the art" chemistry transport model simulate Amazonian
tropospheric chemistry?
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID TROPICAL RAIN-FOREST; VOLATILE ORGANIC-COMPOUNDS; MASTER CHEMICAL
MECHANISM; FIRE EMISSIONS EXPERIMENT; PLANETARY BOUNDARY-LAYER; MCM V3
PART; ISOPRENE EMISSIONS; ATMOSPHERIC CHEMISTRY; NONMETHANE
HYDROCARBONS; UNITED-STATES
AB We present an evaluation of a nested high-resolution Goddard Earth Observing System (GEOS)-Chem chemistry transport model simulation of tropospheric chemistry over tropical South America. The model has been constrained with two isoprene emission inventories: (1) the canopy-scale Model of Emissions of Gases and Aerosols from Nature (MEGAN) and (2) a leaf-scale algorithm coupled to the Lund-Potsdam-Jena General Ecosystem Simulator (LPJ-GUESS) dynamic vegetation model, and the model has been run using two different chemical mechanisms that contain alternative treatments of isoprene photo-oxidation. Large differences of up to 100 Tg C yr (1) exist between the isoprene emissions predicted by each inventory, with MEGAN emissions generally higher. Based on our simulations we estimate that tropical South America (30-85 degrees W, 14 degrees N-25 degrees S) contributes about 15-35% of total global isoprene emissions. We have quantified the model sensitivity to changes in isoprene emissions, chemistry, boundary layer mixing, and soil NOx emissions using ground-based and airborne observations. We find GEOS-Chem has difficulty reproducing several observed chemical species; typically hydroxyl concentrations are underestimated, whilst mixing ratios of isoprene and its oxidation products are overestimated. The magnitude of model formaldehyde (HCHO) columns are most sensitive to the choice of chemical mechanism and isoprene emission inventory. We find GEOS-Chem exhibits a significant positive bias (10-100%) when compared with HCHO columns from the Scanning Imaging Absorption Spectrometer for Atmospheric Chartography (SCIAMACHY) and Ozone Monitoring Instrument (OMI) for the study year 2006. Simulations that use the more detailed chemical mechanism and/or lowest isoprene emissions provide the best agreement to the satellite data, since they result in lower-HCHO columns.
C1 [Barkley, Michael P.] Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England.
[Palmer, Paul I.] Univ Edinburgh, Sch Geosci, Edinburgh EH9 3JW, Midlothian, Scotland.
[Ganzeveld, Laurens] Univ Wageningen & Res Ctr, Dept Environm Sci, NL-6708 PB Wageningen, Netherlands.
[Arneth, Almut; Hagberg, Daniel] Lund Univ, Geobiosphere Sci Ctr, Dept Phys Geog & Ecosyst Anal, SE-22362 Lund, Sweden.
[Kurosu, Thomas P.; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Mueller, J. -F.; De Smedt, Isabelle; Van Roozendael, Michel] Belgian Inst Space Aeron, B-1180 Brussels, Belgium.
[Karl, Thomas; Guenther, Alex] Natl Ctr Atmospher Res, Boulder, CO 80307 USA.
[Mao, Jingqiu] Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08628 USA.
[Paulot, Fabien; Wennberg, Paul O.] CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA.
[Wang, Yuxuan] Tsinghua Univ, Minist Educ Key Lab Earth Syst Modeling, Ctr Earth Syst Sci, Inst Global Change Studies, Beijing 100084, Peoples R China.
[Yantosca, Robert M.] Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
[Arneth, Almut] Karlsruhe Inst Technol, Inst Meteorol & Climate Res, Karlsruhe, Germany.
[Chen, Dan] Tsinghua Univ, Dept Environm Sci & Engn, Beijing 100084, Peoples R China.
[Wennberg, Paul O.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Barkley, MP (reprint author), Univ Leicester, Dept Phys & Astron, EOS Grp, Univ Rd, Leicester LE1 7RH, Leics, England.
EM mpb14@le.ac.uk
RI Wang, Yuxuan/C-6902-2014; Yantosca, Robert/F-7920-2014; Palmer,
Paul/F-7008-2010; Chen, Dan/R-4486-2016; Mao, Jingqiu/F-2511-2010;
Wennberg, Paul/A-5460-2012; Paulot, Fabien/C-1002-2011; Karl,
Thomas/D-1891-2009; Arneth, Almut/B-2702-2013; Chem, GEOS/C-5595-2014
OI Wang, Yuxuan/0000-0002-1649-6974; Yantosca, Robert/0000-0003-3781-1870;
Chance, Kelly/0000-0002-7339-7577; Mao, Jingqiu/0000-0002-4774-9751;
Karl, Thomas/0000-0003-2869-9426;
FU NASA; Natural Environment Research Council (NERC) [NE/G013810/1,
NE/D001471]; Swedish Research Council Formas
FX The authors would like to thank all members of the GABRIEL Science team
for their provision of the aircraft data. We would also like to thank
Lee Murray (Harvard University) for his help with the local lightning
distribution and Daniel Stone and Mat Evans (University of Leeds) for
their help setting up the box model. The GEOS-Chem model is managed at
Harvard University with support from the NASA Atmospheric Chemistry
Modeling and Analysis Program. This work was supported by the Natural
Environment Research Council (NERC research grants NE/G013810/1 and
NE/D001471). A. A. and D. H. acknowledge support from the Swedish
Research Council Formas.
NR 112
TC 24
Z9 24
U1 2
U2 34
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD AUG 17
PY 2011
VL 116
AR D16302
DI 10.1029/2011JD015893
PG 28
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 810MH
UT WOS:000294128900003
ER
PT J
AU Pavicic, M
AF Pavicic, Mladen
TI Near-Deterministic Discrimination of All Bell States with Linear Optics
(Retracted article. See vol. 109, pg. 079902, 2012)
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID ENTANGLED PHOTON PAIRS; QUANTUM TELEPORTATION; BEAM SPLITTER;
INTERFEROMETRY; INTERFERENCE; GENERATION; EFFICIENCY
AB For a reliable implementation of quantum teleportation, a near-deterministic (close to 100%) discrimination of all four Bell states of entangled qubits is required. One can carry it out with linear optical elements only if conditional dynamics are allowed. Here we present a setup in which we repeatedly disentangle and reentangle photons in three of four states, so as to separate photons in one of them, conditioned on keeping the other two at bay. The efficiency of a realistic implementation of our setup with current technology is over 90% for an ideal source of photons on demand.
C1 [Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 10001, Croatia.
[Pavicic, Mladen] Harvard Univ, Dept Phys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Pavicic, M (reprint author), Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 10001, Croatia.
EM mpavicic@grad.hr
FU Ministry of Science Education & Sport of Croatia [082-0982562-3160];
U.S. National Science Foundation; Smithsonian Astrophysical Observatory
FX Supported by the Ministry of Science Education & Sport of Croatia
(Project No. 082-0982562-3160) and by a U.S. National Science Foundation
grant to the Institute for Theoretical Atomic, Molecular, and Optical
Physics at Harvard University and Smithsonian Astrophysical Observatory.
I thank my host Hossein Sadeghpour for his hospitality.
NR 30
TC 11
Z9 12
U1 3
U2 16
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 AUG 17
PY 2011
VL 107
IS 8
AR 080403
DI 10.1103/PhysRevLett.107.080403
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 808KQ
UT WOS:000293977000001
PM 21929149
ER
PT J
AU Janzen, DH
Hallwachs, W
Burns, JM
Hajibabaei, M
Bertrand, C
Hebert, PDN
AF Janzen, Daniel H.
Hallwachs, Winnie
Burns, John M.
Hajibabaei, Mehrdad
Bertrand, Claudia
Hebert, Paul D. N.
TI Reading the Complex Skipper Butterfly Fauna of One Tropical Place
SO PLOS ONE
LA English
DT Article
ID PARASITOID FLIES DIPTERA; RICAN DRY FOREST; DNA BARCODES; SWEEP SAMPLES;
COSTA-RICA; HESPERIIDAE HESPERIINAE; FOLIAGE INSECTS; LEPIDOPTERA;
GENUS; BIODIVERSITY
AB Background: An intense, 30-year, ongoing biodiversity inventory of Lepidoptera, together with their food plants and parasitoids, is centered on the rearing of wild-caught caterpillars in the 120,000 terrestrial hectares of dry, rain, and cloud forest of Area de Conservacion Guanacaste (ACG) in northwestern Costa Rica. Since 2003, DNA barcoding of all species has aided their identification and discovery. We summarize the process and results for a large set of the species of two speciose subfamilies of ACG skipper butterflies (Hesperiidae) and emphasize the effectiveness of barcoding these species (which are often difficult and time-consuming to identify).
Methodology/Principal Findings: Adults are DNA barcoded by the Biodiversity Institute of Ontario, Guelph, Canada; and they are identified by correlating the resulting COI barcode information with more traditional information such as food plant, facies, genitalia, microlocation within ACG, caterpillar traits, etc. This process has found about 303 morphologically defined species of eudamine and pyrgine Hesperiidae breeding in ACG (about 25% of the ACG butterfly fauna) and another 44 units indicated by distinct barcodes (n = 9,094), which may be additional species and therefore may represent as much as a 13% increase. All but the members of one complex can be identified by their DNA barcodes.
Conclusions/Significance: Addition of DNA barcoding to the methodology greatly improved the inventory, both through faster (hence cheaper) accurate identification of the species that are distinguishable without barcoding, as well as those that require it, and through the revelation of species "hidden" within what have long been viewed as single species. Barcoding increased the recognition of species-level specialization. It would be no more appropriate to ignore barcode data in a species inventory than it would be to ignore adult genitalia variation or caterpillar ecology.
C1 [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA.
[Burns, John M.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Hajibabaei, Mehrdad; Bertrand, Claudia; Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada.
RP Janzen, DH (reprint author), Univ Penn, Dept Biol, Philadelphia, PA 19104 USA.
EM djanzen@sas.upenn.edu
RI Hebert, Paul/C-4161-2013
OI Hebert, Paul/0000-0002-3081-6700
FU National Museum of Natural History Small Grants Program; U.S. National
Science Foundation [BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730,
0515699]; Wege Foundation; International Conservation Fund of Canada;
Jessie B. Cox Charitable Trust; Blue Moon Fund; Guanacaste Dry Forest
Conservation Fund; Area de Conservacion Guanacaste; University of
Pennsylvania; Gordon and Betty Moore Foundation; Natural Sciences and
Engineering Research Council of Canada; Canada Research Chairs program
FX This research was supported by the National Museum of Natural History
Small Grants Program (J.M.B.); U.S. National Science Foundation grants
BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, and 0515699, and
grants from the Wege Foundation, International Conservation Fund of
Canada, Jessie B. Cox Charitable Trust, Blue Moon Fund, Guanacaste Dry
Forest Conservation Fund, Area de Conservacion Guanacaste, and
University of Pennsylvania (D.H.J.); and the Gordon and Betty Moore
Foundation, the Natural Sciences and Engineering Research Council of
Canada, and the Canada Research Chairs program (P.D.N.H.). The funders
had no role in study design, data collection and analysis, decision to
publish, or preparation of the manuscript.
NR 51
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U1 1
U2 13
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 AUG 16
PY 2011
VL 6
IS 8
AR e19874
DI 10.1371/journal.pone.0019874
PG 15
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 810KZ
UT WOS:000294125500002
PM 21857895
ER
PT J
AU Swei, A
Rowley, JJL
Rodder, D
Diesmos, MLL
Diesmos, AC
Briggs, CJ
Brown, R
Cao, TT
Cheng, TL
Chong, RA
Han, B
Hero, JM
Hoang, HD
Kusrini, MD
Duong, TTL
McGuire, JA
Meegaskumbura, M
Min, MS
Mulcahy, DG
Neang, T
Phimmachak, S
Rao, DQ
Reeder, NM
Schoville, SD
Sivongxay, N
Srei, N
Stock, M
Stuart, BL
Torres, LS
Dao, TAT
Tunstall, TS
Vieites, D
Vredenburg, VT
AF Swei, Andrea
Rowley, Jodi J. L.
Roedder, Dennis
Diesmos, Mae L. L.
Diesmos, Arvin C.
Briggs, Cheryl J.
Brown, Rafe
Trung Tien Cao
Cheng, Tina L.
Chong, Rebecca A.
Han, Ben
Hero, Jean-Marc
Huy Duc Hoang
Kusrini, Mirza D.
Duong Thi Thuy Le
McGuire, Jimmy A.
Meegaskumbura, Madhava
Min, Mi-Sook
Mulcahy, Daniel G.
Thy Neang
Phimmachak, Somphouthone
Rao, Ding-Qi
Reeder, Natalie M.
Schoville, Sean D.
Sivongxay, Niane
Srei, Narin
Stoeck, Matthias
Stuart, Bryan L.
Torres, Lilia S.
Dao Thi Anh Tran
Tunstall, Tate S.
Vieites, David
Vredenburg, Vance T.
TI Is Chytridiomycosis an Emerging Infectious Disease in Asia?
SO PLOS ONE
LA English
DT Article
ID AMPHIBIAN CHYTRID FUNGUS; PATHOGEN BATRACHOCHYTRIUM-DENDROBATIDIS;
POPULATION DECLINES; RANA-CATESBEIANA; CLIMATE-CHANGE; FROGS;
PREVALENCE; EXTINCTIONS; HAPLOTYPES; INTENSITY
AB The disease chytridiomycosis, caused by the fungus Batrachochytrium dendrobatidis (Bd), has caused dramatic amphibian population declines and extinctions in Australia, Central and North America, and Europe. Bd is associated with >200 species extinctions of amphibians, but not all species that become infected are susceptible to the disease. Specifically, Bd has rapidly emerged in some areas of the world, such as in Australia, USA, and throughout Central and South America, causing population and species collapse. The mechanism behind the rapid global emergence of the disease is poorly understood, in part due to an incomplete picture of the global distribution of Bd. At present, there is a considerable amount of geographic bias in survey effort for Bd, with Asia being the most neglected continent. To date, Bd surveys have been published for few Asian countries, and infected amphibians have been reported only from Indonesia, South Korea, China and Japan. Thus far, there have been no substantiated reports of enigmatic or suspected disease-caused population declines of the kind that has been attributed to Bd in other areas. In order to gain a more detailed picture of the distribution of Bd in Asia, we undertook a widespread, opportunistic survey of over 3,000 amphibians for Bd throughout Asia and adjoining Papua New Guinea. Survey sites spanned 15 countries, approximately 36 degrees latitude, 111 degrees longitude, and over 2000 m in elevation. Bd prevalence was very low throughout our survey area (2.35% overall) and infected animals were not clumped as would be expected in epizootic events. This suggests that Bd is either newly emerging in Asia, endemic at low prevalence, or that some other ecological factor is preventing Bd from fully invading Asian amphibians. The current observed pattern in Asia differs from that in many other parts of the world.
C1 [Swei, Andrea] Cary Inst Ecosyst Studies, Millbrook, NY USA.
[Rowley, Jodi J. L.] Australian Museum, Dept Herpetol, Sydney, NSW 2000, Australia.
[Roedder, Dennis] Zool Forsch Museum Alexander Koenig, Bonn, N Rhine Westpha, Germany.
[Diesmos, Mae L. L.] Univ Santo Tomas, Dept Biol Sci, Manila, Philippines.
[Diesmos, Arvin C.] Natl Museum Philippines, Manila, Philippines.
[Briggs, Cheryl J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA.
[Brown, Rafe] Univ Kansas, KU Biodivers Inst, Lawrence, KS 66045 USA.
[Trung Tien Cao] Vinh Univ, Fac Biol, Vinh City, Nghe An, Vietnam.
[Cheng, Tina L.; Reeder, Natalie M.; Torres, Lilia S.; Vredenburg, Vance T.] San Francisco State Univ, Dept Biol, San Francisco, CA 94132 USA.
[Chong, Rebecca A.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA.
[Han, Ben] SW Forestry Univ, Fac Life Sci, Kunming, Yunnan, Peoples R China.
[Hero, Jean-Marc] Griffith Univ Gold Coast Campus, Sch Environm, Gold Coast, Qld, Australia.
[Huy Duc Hoang; Duong Thi Thuy Le; Dao Thi Anh Tran] Univ Sci Ho Chi Minh City, Fac Biol, Ho Chi Minh City, Vietnam.
[Kusrini, Mirza D.] Bogor Agr Univ Darmaga Campus, Fac Forestry, Dept Forest Resources Conservat & Ecotourism, Bogor, W Java, Indonesia.
[McGuire, Jimmy A.; Tunstall, Tate S.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
[Meegaskumbura, Madhava] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA.
[Min, Mi-Sook] Seoul Natl Univ, Res Inst Vet Sci Vet Med, Seoul, South Korea.
[Mulcahy, Daniel G.] Smithsonian Inst, Suitland, MD USA.
[Thy Neang] Minist Environm, Dept Natl Pk, Phnom Penh, Cambodia.
[Phimmachak, Somphouthone; Sivongxay, Niane] Natl Univ Laos, Fac Sci, Dept Biol, Viangchan, Laos.
[Rao, Ding-Qi] Chinese Acad Sci, Kunming Inst Zool, Kunming, Peoples R China.
[Schoville, Sean D.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA.
[Srei, Narin] Royal Univ Phnom Penh, Dept Biol, Phnom Penh, Cambodia.
[Srei, Narin] Royal Univ Phnom Penh, Ctr Biodivers Conservat, Phnom Penh, Cambodia.
[Stoeck, Matthias] Univ Lausanne, Dept Ecol & Evolut, Lausanne, Vaud, Switzerland.
[Stuart, Bryan L.] N Carolina Museum Nat Sci, Raleigh, NC USA.
[Vieites, David] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain.
RP Swei, A (reprint author), Cary Inst Ecosyst Studies, Millbrook, NY USA.
EM swei@berkeley.edu
RI Schoville, Sean/J-8061-2012; Vieites, David/B-4481-2009; Briggs,
Cheryl/F-7456-2013;
OI Rowley, Jodi/0000-0002-2011-9143; Vieites, David/0000-0001-5551-7419;
Vredenburg, Vance/0000-0002-9682-1190
FU National Science Foundation-National Institutes of Health Ecology of
Infectious Diseases [EF-0723563]; California Academy of Sciences
FX Funding was provided by the joint National Science Foundation-National
Institutes of Health Ecology of Infectious Diseases (EF-0723563,
http://www.nsf.gov). Additional funding was secured by David A. Neeley
through the California Academy of Sciences. The funders had no role in
study design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 51
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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 AUG 16
PY 2011
VL 6
IS 8
AR e23179
DI 10.1371/journal.pone.0023179
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 810KZ
UT WOS:000294125500018
PM 21887238
ER
PT J
AU Levin, II
Valkiunas, G
Santiago-Alarcon, D
Cruz, LL
Iezhova, TA
O'Brien, SL
Hailer, F
Dearborn, D
Schreiber, EA
Fleischer, RC
Ricklefs, RE
Parker, PG
AF Levin, Iris I.
Valkiunas, Gediminas
Santiago-Alarcon, Diego
Cruz, Larisa Lee
Iezhova, Tatjana A.
O'Brien, Sarah L.
Hailer, Frank
Dearborn, Don
Schreiber, E. A.
Fleischer, Robert C.
Ricklefs, Robert E.
Parker, Patricia G.
TI Hippoboscid-transmitted Haemoproteus parasites (Haemosporida) infect
Galapagos Pelecaniform birds: Evidence from molecular and morphological
studies, with a description of Haemoproteus iwa
SO INTERNATIONAL JOURNAL FOR PARASITOLOGY
LA English
DT Article
DE Haemoproteus; Haemoproteus iwa; Plasmodium; Haemosporidians; Malaria;
Blood parasite; Hippoboscidae; Galapagos
ID DOVE ZENAIDA-GALAPAGOENSIS; AVIAN MALARIA PARASITES; BLOOD PARASITES;
HEMOSPORIDIAN PARASITES; FOREST BIRDS; AGE-CLASS; SP-NOV; N-SP;
CONSERVATION; PREVALENCE
AB Haemosporidian parasites are widely distributed and common parasites of birds, and the application of molecular techniques has revealed remarkable diversity among their lineages. Four haemosporidian genera infect avian hosts (Plasmodium, Haemoproteus, Leucocytozoon and Fallisia), and Haemoproteus is split into two sub-genera based on morphological evidence and phylogenetic support for two divergent sister clades. One clade (Haemoproteus (Parahaemoproteus)) contains parasites developing in birds belonging to several different orders, except pigeons and doves (Columbiformes), while the other (Haemoproteus (Haemoproteus)) has previously been shown to only infect dove hosts. Here we provide molecular and morphological identification of Haemoproteus parasites from several seabird species that are closely related to those found in dove hosts. We also document a deeply divergent clade with two haemosporidian lineages recovered primarily from frigatebirds (Fregatidae, Pelecaniformes) that is sister to the hippoboscid-(Hippoboscidae) transmitted dove parasites. One of the lineages in this new clade of parasites belongs to Haemoproteus iwa and is distributed in two species of frigatebird (Fregata) hosts from Hawaii, the Galapagos Islands, the eastern Pacific and throughout the Caribbean Basin. Haemosporidian parasites are often considered rare in seabirds due in part to the lack or low activity of some dipteran vectors (e.g., mosquitos, biting midges) in marine and coastal environments; however, we show that H. iwa is prevalent and is very likely vectored among frigatebirds by hippoboscid flies which are abundant on frigatebirds and other seabirds. This study supports the existence of two sister clades of avian Haemoproteus in accord with the subgeneric classification of avian hemoproteids. Description of H. iwa from Galapagos Fregata minor is given based on morphology of blood stages and segments of the mitochondrial cytochrome b gene, which can be used for identification. This study shows that hippoboscid flies warrant more attention as vectors of avian Haemoproteus spp., particularly in marine and coastal environments. (C) 2011 Australian Society for Parasitology Inc. Published by Elsevier Ltd. All rights reserved.
C1 [Levin, Iris I.; Santiago-Alarcon, Diego; Ricklefs, Robert E.; Parker, Patricia G.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
[Levin, Iris I.; Santiago-Alarcon, Diego; Ricklefs, Robert E.; Parker, Patricia G.] Whitney R Harris World Ecol Ctr, St Louis, MO 63121 USA.
[Valkiunas, Gediminas; Iezhova, Tatjana A.] Nat Res Ctr, Inst Ecol, LT-08412 Vilnius 21, Lithuania.
[Cruz, Larisa Lee] Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England.
[O'Brien, Sarah L.; Parker, Patricia G.] WildCare Inst, St Louis, MO 63110 USA.
[Hailer, Frank; Fleischer, Robert C.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Genet Lab, Washington, DC 20013 USA.
[Dearborn, Don] Bates Coll, Dept Biol, Lewiston, ME 04240 USA.
[Schreiber, E. A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20008 USA.
RP Levin, II (reprint author), Univ Missouri, Dept Biol, 1 Univ Blvd, St Louis, MO 63121 USA.
EM Iris.Levin@umsl.edu
RI Hailer, Frank/C-9114-2012
OI Hailer, Frank/0000-0002-2340-1726
FU Des Lee Collaborative Vision; Saint Louis Zoo, USA; Whitney R. Harris
World Ecology Center, Sigma Xi; American Museum of Natural History;
Whitney R. Harris World Ecology Center, Idea Wild; Frank M. Chapman
Memorial Fund; St. Louis Zoo; Organization for Tropical Studies; T.L.
Cross, Seabird Research, Inc.; Smithsonian's James Bond Fund; CONACYT,
Mexico; Galapagos Genetics Epidemilogy and Pathology Laboratory in
Galapagos; Darwin Initiative
FX We would like to thank S. Harden, C. McKinley, M. Favazza, A. Carrion,
M. Evans, P. Baiao, J. Higashiguchi, N. Gottdenker, J. Rabenold, J.
Bollmer, L. Padilla, M. Cruz, S. Deem, J. Merkel, E. Sari, H. Vargas, A.
Monopoli, M. Pallo, G. Buitron and E. Buettner for their contributions
or participation during field studies and R. Adlard at the Queensland
Museum, Brisbane, Australia, for providing the type material of H. iwa.
We thank the Galapagos National Park for sampling permission and the
Charles Darwin Research Station for logistical support. This manuscript
was improved by suggestions from the Parker laboratory. For permission
to collect non-Galapagos frigatebird samples we thank (i) the Belize
Ministry of Natural Resources and the Environment and the Belize Audubon
Society, (ii) the Cayman Islands Department of the Environment and the
National Trust, and (iii) in Panama the Autoridad Nacional del Ambiente,
Smithsonian Tropical Research Institute, George Angehr and Jim Kushlan.
This work was supported by the Des Lee Collaborative Vision and by two
grants from the Field Research for Conservation programme of the Saint
Louis Zoo, USA, as well as by grants to I. Levin and P.G. Parker from
the Whitney R. Harris World Ecology Center, Sigma Xi and the Frank M.
Chapman Memorial Fund of the American Museum of Natural History; also by
grants to D. Santiago-Alarcon and P.G. Parker from the Whitney R. Harris
World Ecology Center, Idea Wild, the Frank M. Chapman Memorial Fund, the
Field Research for Conservation programme of the St. Louis Zoo and the
Organization for Tropical Studies. Funding to B.A. Schreiber came from
T.L. Cross, Seabird Research, Inc., and the Smithsonian's James Bond
Fund. L.L. Cruz was funded by CONACYT, Mexico, with support from the
Galapagos Genetics Epidemilogy and Pathology Laboratory in Galapagos and
the Darwin Initiative. This research was done in accordance with UMSL's
Institutional Animal Care and Use Committee.
NR 57
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PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0020-7519
EI 1879-0135
J9 INT J PARASITOL
JI Int. J. Parasit.
PD AUG 15
PY 2011
VL 41
IS 10
BP 1019
EP 1027
DI 10.1016/j.ijpara.2011.03.014
PG 9
WC Parasitology
SC Parasitology
GA 815IL
UT WOS:000294519200002
PM 21683082
ER
PT J
AU Breedy, O
Guzman, HM
AF Breedy, Odalisca
Guzman, Hector M.
TI A revision of the genus Heterogorgia Verrill, 1868 (Anthozoa:
Octocorallia: Plexauridae)
SO ZOOTAXA
LA English
DT Article
DE Alcyonacea; Cnidaria; Coelenterata; eastern Pacific; gorgonians; soft
corals; western Atlantic
ID COELENTERATA; GORGONIIDAE; PACIFIC
AB The genus Heterogorgia Verrill, 1868 is poorly known. Lack of good illustrations and clear definitions have historically led authors to assign or transfer species erroneously to it. The genus was established by Verrill for three eastern Pacific species, another was described by Breedy and Guzman in 2005, and the geographic distribution was extended with the discovery of a western Atlantic species described by Castro in 1990. Heterogorgia is characterised by colonies composed of a number of stout stems that branch laterally and irregularly and arise from a conspicuous spreading holdfast. Coenen-chymal sclerites are mostly colourless spindles; anthocodiae have strong spindles arranged in collaret and points; and the calyces are prominently armed with whorls of strongly projecting thorns. To define Heterogorgia we examined original type material of all eastern Pacific and western Atlantic species described until now and reference specimens from recent expeditions along the eastern Pacific. Morphological characters are analysed and illustrated using scanning electron micrographs. Lectotypes are designated for H. tortuosa and H. verrucosa to establish their taxonomic status. We conclude that Heterogorgia is comprised of five valid species at present: Heterogorgia hickmani and H. verrucosa for the Galapagos Islands and Ecuador mainland; H. papillosa for Mexico; H. tortuosa and H. verrucosa for Costa Rica and Panama; and H. uatumani for Brazil and Bahamas. The genera Astromuricea, Bebryce, Echinogorgia and Psammogorgia are proposed for the western Pacific species that were historically misplaced in Heterogorgia. We recommend that regional biodiversity estimates and biogeography analyses consider the erroneous status of the species that are still listed as Heterogorgia within the data sets.
C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica.
[Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, San Jose, Costa Rica.
[Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica.
EM odalisca.breedy@ucr.ac.cr; guzmanh@si.edu
FU Vicerrectoria de Investigacion (University of Costa Rica); Conservation
International, Nature Conservancy; Smithsonian Tropical Research
Institute, Panama; Foundation Herbette
FX We are grateful to Phil Alderslade (CSIRO Marine and Atmospheric
Research, Tasmania), Stephen Cairns (USNM), Leen van Ofwegen
(Netherlands Centre for Biodiversity Naturalis, Leiden), and Sergio
Vargas (Molecular Geo- and Palaeobiology, Geobiology and Palaeontology,
LMU Munchen) for critical reviews of the manuscript. We are grateful to
Eric Lazo-Wasem (YPM), Ardis Johnston (MCZ), Stephen Cairns (USNM),
Sheila Halsey and Andrew Cabrinovic (BM), Cleaveland P. Hickman, Jr.
(Washington & Lee University, Lexington) and Clovis Castro (MNRJ) for
the loan of type material. We acknowledge the following people and
institutions for their invaluable collaboration in field and laboratory
work: Jorge Cortes (CIMAR), Carlos Guevara (STRI), Fernando Rivera,
Pricilla Martinez, Roberta Nebot (IIN); Rita Vargas (UCR), Percy Denyer
(Escuela Centroamericana de Geologia, UCR), and Peter Baungartner and
Pierre Vonlanthen (Institut de Geologie et Paleontologie, Universite de
Lausanne). We thank the Ministerio de Ambiente de Costa Rica for
allowing visits to Parque Nacional Manuel Antonio, Parque Nacional
Marino Ballena, Parque Nacional Isla del Cano, Costa Rica; Autoridad
Nacional del Ambiente de Panama (ANAM) for providing permits to work in
the Coiba National Park; the Charles Darwin Research Station for
specimen collection and support in the March 2007 field trip to the
Galapagos Islands, Ecuador, and finally to IIN and Conservation
International through the Eastern Tropical Pacific Seascape project,
Walton Family Foundation for support in the July 2010 field trip to
Ecuador.; This project was funded by the Vicerrectoria de Investigacion
(University of Costa Rica), Conservation International, The Nature
Conservancy, and the Smithsonian Tropical Research Institute, Panama;
Foundation Herbette provided additional support for SEM facilities at
the University of Lausanne.
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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 AUG 15
PY 2011
IS 2995
BP 27
EP 44
PG 18
WC Zoology
SC Zoology
GA 806YH
UT WOS:000293853400002
ER
PT J
AU Wolf, S
Eugster, W
Potvin, C
Buchmann, N
AF Wolf, Sebastian
Eugster, Werner
Potvin, Catherine
Buchmann, Nina
TI Strong seasonal variations in net ecosystem CO2 exchange of a tropical
pasture and afforestation in Panama
SO AGRICULTURAL AND FOREST METEOROLOGY
LA English
DT Article
DE Eddy covariance; Carbon dioxide fluxes; Soil respiration; Land use;
ENSO; FLUXNET
ID CARBON EXCHANGE; TERRESTRIAL ECOSYSTEMS; FLUX MEASUREMENTS; SOIL
RESPIRATION; RAIN-FOREST; ENERGY; WATER; RATES; PRODUCTIVITY;
BIODIVERSITY
AB Pasture and afforestation are land-use types of major importance in the tropics, yet, most flux tower studies have been conducted in mature tropical forests. As deforestation in the tropics is expected to continue, it is critical to improve our understanding of alternative land-use types, and the impact of interactions between land use and climate on ecosystem carbon dynamics. Thus, we measured net ecosystem CO2 fluxes of a pasture and an adjacent tropical afforestation (native tree species plantation) in Sardinilla, Panama from 2007 to 2009. The objectives of our paired site study were: (1) to assess seasonal and inter-annual variations in net ecosystem CO2 exchange (NEE) of pasture and afforestation, (2) to identify the environmental controls of net ecosystem CO2 fluxes, and (3) to constrain eddy covariance derived total ecosystem respiration (TER) with chamber-based soil respiration (R-Soil) measurements. We observed distinct seasonal variations in NEE that were more pronounced in the pasture compared to the afforestation, reflecting changes in plant and microbial activities. The land conversion from pasture to afforestation increased the potential for carbon uptake by trees vs. grasses throughout most of the year. R-Soil contributed about 50% to TER, with only small differences between ecosystems or seasons. Radiation and soil moisture were the main environmental controls of CO2 fluxes while temperature had no effect on NEE. The pasture ecosystem was more strongly affected by soil water limitations during the dry season, probably due to the shallower root system of grasses compared to trees. Thus, it seems likely that predicted increases in precipitation variability will impact seasonal variations of CO2 fluxes in Central Panama, in particular of pasture ecosystems. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Wolf, Sebastian; Eugster, Werner; Buchmann, Nina] ETH, Inst Agr Sci, Univ Str 2, CH-8092 Zurich, Switzerland.
[Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
[Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Wolf, S (reprint author), ETH, Inst Agr Sci, Univ Str 2, CH-8092 Zurich, Switzerland.
EM sewolf@ethz.ch
RI Buchmann, Nina/E-6095-2011; Wolf, Sebastian/B-4580-2010; Eugster,
Werner/E-5116-2010
OI Wolf, Sebastian/0000-0001-7717-6993; Eugster, Werner/0000-0001-6067-0741
FU North-South Centre (former Swiss Centre for International Agriculture)
of ETH Zurich
FX Funding for this project was provided by the North-South Centre (former
Swiss Centre for International Agriculture) of ETH Zurich. We thank the
Meteorology and Hydrology Branch of the Panama Canal Authority (ACP),
Republic of Panama, for providing meteorological data. We are grateful
to Timothy Seipel for identifying grass species of the pasture and for
valuable comments on the manuscript. Many thanks also to Nicolas Gruber
for inspiring discussions. We particularly thank Jose Monteza for
assistance in the field.
NR 63
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PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-1923
EI 1873-2240
J9 AGR FOREST METEOROL
JI Agric. For. Meteorol.
PD AUG 15
PY 2011
VL 151
IS 8
BP 1139
EP 1151
DI 10.1016/j.agrformet.2011.04.002
PG 13
WC Agronomy; Forestry; Meteorology & Atmospheric Sciences
SC Agriculture; Forestry; Meteorology & Atmospheric Sciences
GA 785JR
UT WOS:000292225800012
ER
PT J
AU Wing, SL
AF Wing, Scott L.
TI Deep Future The Next 100,000 Years of Life on Earth
SO SCIENCE
LA English
DT Book Review
C1 [Wing, Scott L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Wing, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
EM wings@si.edu
NR 1
TC 1
Z9 1
U1 1
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 AUG 12
PY 2011
VL 333
IS 6044
BP 825
EP 825
DI 10.1126/science.1209934
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 806DJ
UT WOS:000293785400022
ER
PT J
AU Sternberg, A
Gal-Yam, A
Simon, JD
Leonard, DC
Quimby, RM
Phillips, MM
Morrell, N
Thompson, IB
Ivans, I
Marshall, JL
Filippenko, AV
Marcy, GW
Bloom, JS
Patat, F
Foley, RJ
Yong, D
Penprase, BE
Beeler, DJ
Prieto, CA
Stringfellow, GS
AF Sternberg, A.
Gal-Yam, A.
Simon, J. D.
Leonard, D. C.
Quimby, R. M.
Phillips, M. M.
Morrell, N.
Thompson, I. B.
Ivans, I.
Marshall, J. L.
Filippenko, A. V.
Marcy, G. W.
Bloom, J. S.
Patat, F.
Foley, R. J.
Yong, D.
Penprase, B. E.
Beeler, D. J.
Allende Prieto, C.
Stringfellow, G. S.
TI Circumstellar Material in Type Ia Supernovae via Sodium Absorption
Features
SO SCIENCE
LA English
DT Article
ID HIGH-RESOLUTION OBSERVATIONS; INTERSTELLAR-MEDIUM; D-LINES; PROGENITORS;
GALAXIES; GAS; CONSTRAINTS; BINARIES; OUTFLOWS; SPECTRUM
AB Type Ia supernovae are key tools for measuring distances on a cosmic scale. They are generally thought to be the thermonuclear explosion of an accreting white dwarf in a close binary system. The nature of the mass donor is still uncertain. In the single-degenerate model it is a main-sequence star or an evolved star, whereas in the double-degenerate model it is another white dwarf. We show that the velocity structure of absorbing material along the line of sight to 35 type Ia supernovae tends to be blueshifted. These structures are likely signatures of gas outflows from the supernova progenitor systems. Thus, many type Ia supernovae in nearby spiral galaxies may originate in single-degenerate systems.
C1 [Sternberg, A.; Gal-Yam, A.] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
[Simon, J. D.; Thompson, I. B.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Quimby, R. M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA.
[Phillips, M. M.; Morrell, N.] Las Campanas Observ, Carnegie Observ, La Serena, Chile.
[Ivans, I.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Marshall, J. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA.
[Filippenko, A. V.; Marcy, G. W.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Patat, F.] ESO, D-85748 Garching, Germany.
[Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Yong, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia.
[Penprase, B. E.; Beeler, D. J.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Allende Prieto, C.] Inst Astrofis Canarias, Tenerife 38205, Spain.
[Allende Prieto, C.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
[Stringfellow, G. S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
RP Sternberg, A (reprint author), Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel.
EM assaf.sternberg@weizmann.ac.il; avishay.gal-yam@weizmann.ac.il
OI Patat, Ferdinando/0000-0002-0537-3573; Gal-Yam,
Avishay/0000-0002-3653-5598
FU W. M. Keck Foundation; French-Israeli Astrophysics Network; Israeli
Science Foundation; European Union; Weizmann-UK program; Peter Gruber
Award; Patricia Gruber Award; NSF [AST-0908886]; TABASGO Foundation;
Clay Fellowship
FX We thank the anonymous reviewers for their comments. Some of the data
presented here were obtained at the W. M. Keck Observatory, which is
operated as a scientific partnership among the California Institute of
Technology, the University of California, and NASA; the observatory was
made possible by the generous financial support of the W. M. Keck
Foundation. We thank the staffs of the various observatories at which we
obtained data, as well as J. G. Cohen, G. D. Becker, A. L. Kraus, W. L.
W. Sargent, E. Norris, G. J. Herczeg, G. Preston, and I. Toro-Martinez
for their data contributions. We thank T. Barlow for work on developing
the MAKEE reduction pipeline, and J. X. Prochaska and B. Weiner for
advice. A. G. acknowledges support by The French-Israeli Astrophysics
Network program, The Israeli Science Foundation, a European Union FP7
Marie Curie IRG Fellowship, The Weizmann-UK program, and a research
grant from the Peter and Patricia Gruber Awards. A.V.F.'s group at the
University of California Berkeley has been supported by NSF grant
AST-0908886 and the TABASGO Foundation. R. J. F. is supported by a Clay
Fellowship. G. S. S. thanks S. Hawley for allocating Director's
Discretionary Time at Apache Point Observatory (APO), and the APO
observing staff. The data described in the paper are presented in the
Supporting Online Material.
NR 38
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U2 15
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 AUG 12
PY 2011
VL 333
IS 6044
BP 856
EP 859
DI 10.1126/science.1203836
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 806DJ
UT WOS:000293785400034
PM 21836010
ER
PT J
AU Brown, WR
Kilic, M
Hermes, JJ
Prieto, CA
Kenyon, SJ
Winget, DE
AF Brown, Warren R.
Kilic, Mukremin
Hermes, J. J.
Allende Prieto, Carlos
Kenyon, Scott J.
Winget, D. E.
TI A 12 MINUTE ORBITAL PERIOD DETACHED WHITE DWARF ECLIPSING BINARY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: close; binaries: eclipsing; gravitational waves; stars:
individual (SDSS J065133.338+284423.37); white dwarfs
ID AM CVN STARS; LIGHT CURVES; MASS-TRANSFER; DISCOVERY; SYSTEM; PULSAR
AB We have discovered a detached pair of white dwarfs (WDs) with a 12.75 minute orbital period and a 1315 km s(-1) radial velocity amplitude. We measure the full orbital parameters of the system using its light curve, which shows ellipsoidal variations, Doppler boosting, and primary and secondary eclipses. The primary is a 0.25 M-circle dot tidally distorted helium WD, only the second tidally distorted WD known. The unseen secondary is a 0.55 M-circle dot carbon-oxygen WD. The two WDs will come into contact in 0.9 Myr due to loss of energy and angular momentum via gravitational wave radiation. Upon contact the systems may merge (yielding a rapidly spinning massive WD), form a stable interacting binary, or possibly explode as an underluminous Type Ia supernova. The system currently has a gravitational wave strain of 10(-22), about 10,000 times larger than the Hulse-Taylor pulsar; this system would be detected by the proposed Laser Interferometer Space Antenna gravitational wave mission in the first week of operation. This system's rapid change in orbital period will provide a fundamental test of general relativity.
C1 [Brown, Warren R.; Kilic, Mukremin; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Hermes, J. J.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain.
[Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
RP Brown, WR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
EM wbrown@cfa.harvard.edu; mkilic@cfa.harvard.edu;
jjhermes@astro.as.utexas.edu; callende@iac.es; skenyon@cfa.harvard.edu;
dew@astro.as.utexas.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU Smithsonian Institution; NASA; National Science Foundation
[AST-0909107]; Norman Hackerman Advanced Research Program
[003658-0252-2009]
FX We thank John Kuehne for his assistance with the observations. This work
was supported in part by the Smithsonian Institution and by NASA through
the Spitzer Space Telescope Fellowship Program and in part by the
National Science Foundation under grant AST-0909107 and the Norman
Hackerman Advanced Research Program under grant 003658-0252-2009.
NR 35
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U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2011
VL 737
IS 1
AR L23
DI 10.1088/2041-8205/737/1/L23
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797PC
UT WOS:000293138800023
ER
PT J
AU Stello, D
Huber, D
Kallinger, T
Basu, S
Mosser, B
Hekker, S
Mathur, S
Garcia, RA
Bedding, TR
Kjeldsen, H
Gilliland, RL
Verner, GA
Chaplin, WJ
Benomar, O
Meibom, S
Grundahl, F
Elsworth, YP
Molenda-Zakowicz, J
Szabo, R
Christensen-Dalsgaard, J
Tenenbaum, P
Twicken, JD
Uddin, K
AF Stello, Dennis
Huber, Daniel
Kallinger, Thomas
Basu, Sarbani
Mosser, Benoit
Hekker, Saskia
Mathur, Savita
Garcia, Rafael A.
Bedding, Timothy R.
Kjeldsen, Hans
Gilliland, Ronald L.
Verner, Graham A.
Chaplin, William J.
Benomar, Othman
Meibom, Soren
Grundahl, Frank
Elsworth, Yvonne P.
Molenda-Zakowicz, Joanna
Szabo, Robert
Christensen-Dalsgaard, Jorgen
Tenenbaum, Peter
Twicken, Joseph D.
Uddin, Kamal
TI AMPLITUDES OF SOLAR-LIKE OSCILLATIONS: CONSTRAINTS FROM RED GIANTS IN
OPEN CLUSTERS OBSERVED BY KEPLER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE binaries: general; open clusters and associations: individual (NGC 6791,
NGC 6819, NGC 6811); stars: interiors; stars: oscillations
ID MAIN-SEQUENCE STARS; MULTISITE CAMPAIGN; ASTEROSEISMOLOGY; EVOLUTION;
PROCYON; MODELS; ISOCHRONES; PARAMETERS; PHYSICS
AB Scaling relations that link asteroseismic quantities to global stellar properties are important for gaining understanding of the intricate physics that underpins stellar pulsations. The common notion that all stars in an open cluster have essentially the same distance, age, and initial composition implies that the stellar parameters can be measured to much higher precision than what is usually achievable for single stars. This makes clusters ideal for exploring the relation between the mode amplitude of solar-like oscillations and the global stellar properties. We have analyzed data obtained with NASA's Kepler space telescope to study solar-like oscillations in 100 red giant stars located in either of the three open clusters, NGC 6791, NGC 6819, and NGC 6811. By fitting the measured amplitudes to predictions from simple scaling relations that depend on luminosity, mass, and effective temperature, we find that the data cannot be described by any power of the luminosity-to-mass ratio as previously assumed. As a result we provide a new improved empirical relation which treats luminosity and mass separately. This relation turns out to also work remarkably well for main-sequence and subgiant stars. In addition, the measured amplitudes reveal the potential presence of a number of previously unknown unresolved binaries in the red clump in NGC 6791 and NGC 6819, pointing to an interesting new application for asteroseismology as a probe into the formation history of open clusters.
C1 [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.; Benomar, Othman] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
[Kallinger, Thomas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kallinger, Thomas] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Mosser, Benoit] Univ Paris 07, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France.
[Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands.
[Mathur, Savita] NCAR, High Altitude Observ, Boulder, CO 80307 USA.
[Garcia, Rafael A.] Univ Paris 7 Diderot, IRFU SAp, Lab AIM, Ctr Saclay,CEA DSM CNRS, F-91191 Gif Sur Yvette, France.
[Kjeldsen, Hans; Grundahl, Frank; Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Verner, Graham A.; Chaplin, William J.; Elsworth, Yvonne P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[Verner, Graham A.] Queen Mary Univ London, Astron Unit, London, England.
[Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Molenda-Zakowicz, Joanna] Uniwersytetu Wroclawskiego, Inst Astronomiczny, PL-51622 Wroclaw, Poland.
[Szabo, Robert] Hungarian Acad Sci, Konkoly Observ, H-1121 Budapest, Hungary.
[Tenenbaum, Peter; Twicken, Joseph D.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA.
NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA.
RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.
OI Kallinger, Thomas/0000-0003-3627-2561; Bedding,
Timothy/0000-0001-5943-1460; Szabo, Robert/0000-0002-3258-1909; Bedding,
Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776
FU NASA's Science Mission Directorate; ARC; NWO; NSF; Polish-Ministry [N
N203 405139]; Lendulet-program OTKA [K83790, MB08C 81013]
FX Funding for this Discovery mission is provided by NASA's Science Mission
Directorate. We thank the entire Kepler team without whom this
investigation would not have been possible. We acknowledge support from
the ARC, NWO, NSF, Polish-Ministry grant N N203 405139, and
Lendulet-program OTKA grants K83790 and MB08C 81013.
NR 50
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2011
VL 737
IS 1
AR L10
DI 10.1088/2041-8205/737/1/L10
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797PC
UT WOS:000293138800010
ER
PT J
AU Winn, JN
Matthews, JM
Dawson, RI
Fabrycky, D
Holman, MJ
Kallinger, T
Kuschnig, R
Sasselov, D
Dragomir, D
Guenther, DB
Moffat, AFJ
Rowe, JF
Rucinski, S
Weiss, WW
AF Winn, Joshua N.
Matthews, Jaymie M.
Dawson, Rebekah I.
Fabrycky, Daniel
Holman, Matthew J.
Kallinger, Thomas
Kuschnig, Rainer
Sasselov, Dimitar
Dragomir, Diana
Guenther, David B.
Moffat, Anthony F. J.
Rowe, Jason F.
Rucinski, Slavek
Weiss, Werner W.
TI A SUPER-EARTH TRANSITING A NAKED-EYE STAR
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; planets and satellites: formation; planets and
satellites: interiors; stars: individual (55 Cnc)
ID FINE GUIDANCE SENSOR; LIGHT-CURVE PROJECT; 55 CANCRI; HD 17156;
LOW-MASS; PLANETS; SYSTEM; TELESCOPE; PHOTOMETRY; SEARCH
AB We have detected transits of the innermost planet "e" orbiting 55 Cnc (V = 6.0), based on two weeks of nearly continuous photometric monitoring with the MOST space telescope. The transits occur with the period (0.74 days) and phase that had been predicted by Dawson & Fabrycky, and with the expected duration and depth for the crossing of a Sun-like star by a hot super-Earth. Assuming the star's mass and radius to be 0.963(-0.029)(+0.051) M-circle dot and 0.943+/-0.010 R-circle dot, the planet's mass, radius, and mean density are 8.63+/-0.35 M-circle plus, 2.00+/-0.14 R-circle plus, and 5.9(-1.1)(+1.5) g cm(-3), respectively. The mean density is comparable to that of Earth, despite the greater mass and consequently greater compression of the interior of 55 Cnc e. This suggests a rock-iron composition supplemented by a significant mass of water, gas, or other light elements. Outside of transits, we detected a sinusoidal signal resembling the expected signal due to the changing illuminated phase of the planet, but with a full range (168 +/- 70 ppm) too large to be reflected light or thermal emission. This signal has no straightforward interpretation and should be checked with further observations. The host star of 55 Cnc e is brighter than that of any other known transiting planet, which will facilitate future investigations.
C1 [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Matthews, Jaymie M.; Kallinger, Thomas; Dragomir, Diana] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Dawson, Rebekah I.; Holman, Matthew J.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabrycky, Daniel] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Kallinger, Thomas; Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Rucinski, Slavek] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Winn, JN (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.
OI Kallinger, Thomas/0000-0003-3627-2561; Dragomir,
Diana/0000-0003-2313-467X; Fabrycky, Daniel/0000-0003-3750-0183
FU NSERC (Canada); Austrian Science Fund; FQRNT scholarship; National
Science Foundation; NASA [HF-51272.01-A, NNX09AB33G]
FX J.M., D.G., A.M., and S.R. thank NSERC (Canada) for financial support.
T. K. is supported by a contract to the Canadian Space Agency. R. K. and
W. W. were supported by the Austrian Science Fund. D. D. is supported by
a FQRNT scholarship. R. D. is supported by a National Science Foundation
Graduate Research Fellowship, and D. C. F. by NASA Hubble Fellowship
HF-51272.01-A. M. H. and J.W. were supported by NASA Origins award
NNX09AB33G.
NR 33
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 10
PY 2011
VL 737
IS 1
AR L18
DI 10.1088/2041-8205/737/1/L18
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797PC
UT WOS:000293138800018
ER
PT J
AU Gay, CD
Stancil, PC
Lepp, S
Dalgarno, A
AF Gay, C. D.
Stancil, P. C.
Lepp, S.
Dalgarno, A.
TI THE HIGHLY DEUTERATED CHEMISTRY OF THE EARLY UNIVERSE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; molecular data; molecular processes; nuclear reactions,
nucleosynthesis, abundances
ID DISSOCIATIVE RECOMBINATION; INTERSTELLAR-MEDIUM; DEUTERIUM; HYDROGEN;
H-2; UNCERTAINTIES; COLLISIONS; ABUNDANCE; ENERGY
AB A comprehensive chemistry of the highly deuterated species D(2), D(2)(+), D(2)H(+), and D(3)(+) in the early universe is presented. Fractional abundances for each are calculated as a function of redshift z in the recombination era. The abundances of the isotopologues are found to display similar behavior. Fractionation enhances the abundances of most of the more highly deuterated species as the redshift decreases due to the closing of some reaction channels as the gas temperature cools. Rate coefficients for the majority of the reactions involving the deuterated species are uncertain resulting in a corresponding uncertainty in their predicted abundances.
C1 [Gay, C. D.; Stancil, P. C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
[Gay, C. D.; Stancil, P. C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA.
[Lepp, S.] Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA.
[Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gay, CD (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
EM cgay1383@gmail.com; stancil@physast.uga.edu; lepp@unlv.nevada.edu;
adalgarno@cfa.harvard.edu
FU NSF [AST-0607733, AST-0607524, AST-0607532]
FX We acknowledge support from NSF Grants AST-0607733 (C. D. G., P. C. S.),
AST-0607524 (S. L.), and AST-0607532 (A.D.).
NR 33
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U1 1
U2 15
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2011
VL 737
IS 1
AR 44
DI 10.1088/0004-637X/737/1/44
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 800BM
UT WOS:000293332200044
ER
PT J
AU Li, JT
Wang, QD
Li, ZY
Chen, Y
AF Li, Jiang-Tao
Wang, Q. Daniel
Li, Zhiyuan
Chen, Yang
TI DYNAMIC S0 GALAXIES. II. THE ROLE OF DIFFUSE HOT GAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 1291,
NGC 2681, NGC 2787, NGC 3115, NGC 5866)
ID X-RAY-EMISSION; GALACTIC NUCLEUS FEEDBACK; NORMAL ELLIPTIC GALAXIES;
COOL INTERSTELLAR-MEDIUM; STAR-FORMATION; MOLECULAR GAS; MULTIPARAMETRIC
ANALYSIS; LENTICULAR GALAXIES; STELLAR POPULATION; EINSTEIN SAMPLE
AB Cold gas loss is thought to be important in star formation quenching and morphological transition during the evolution of S0 galaxies. In high-density environments, this gas loss can be achieved via many external mechanisms. However, in relatively isolated environments, where these external mechanisms cannot be efficient, the gas loss must then be dominated by some internal processes. We have performed Chandra analysis of hot gas in five nearby isolated S0 galaxies, based on the quantitative subtraction of various stellar contributions. We find that all the galaxies studied in the present work are X-ray faint, with the luminosity of the hot gas (L-X) typically accounting for less than or similar to 5% of the expected Type Ia supernova (SN) energy injection rate. We have further compared our results with those from relevant recent papers, in order to investigate the energy budget, cold-hot gas relation, and gas removal from S0 galaxies in isolated environments. We find that elliptical and S0 galaxies are not significantly different in L-X at the low-mass end (typically with K-band luminosity L-K less than or similar to 10(11) L-circle dot,L-K). However, at the high-mass end, S0 galaxies tend to have significantly lower L-X than elliptical galaxies of the same stellar masses, as already shown in previous observational and theoretical works. We further discuss the potential relationship of the diffuse X-ray emission with the cold (atomic and molecular) gas content in the S0 and elliptical galaxies included in our study. We find that L-X/L-K(2) tends to correlate positively with the total cold gas mass (MH2+H I) for cold-gas-poor galaxies with MH2+HI less than or similar to 10(8)M(circle dot), while they anti-correlate with each other for cold-gas-rich galaxies. This cold-hot gas relationship can be explained in a scenario of early-type galaxy evolution, with the leftover cold gas from the precursor star-forming galaxy mainly removed by the long-lasting Type Ia supernova (SN) feedback. The two different trends for cold-gas-rich and cold-gas-poor galaxies may be the results of the initial fast decreasing SN rate and the later fast decreasing mass loading to hot gas, respectively.
C1 [Li, Jiang-Tao; Chen, Yang] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China.
[Li, Jiang-Tao; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Li, Jiang-Tao; Chen, Yang] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Peoples R China.
[Li, Zhiyuan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Li, JT (reprint author), Nanjing Univ, Dept Astron, 22 Hankou Rd, Nanjing 210093, Peoples R China.
OI Li, Jiang-Tao/0000-0001-6239-3821
FU NASA [AR7-8016A, G08-9088B]; NSFC [10725312, 10673003]; China 973
Program [2009CB824800]
FX This work is supported by NASA through the CXC/SAO grants AR7-8016A and
G08-9088B, by NSFC through the grants 10725312 and 10673003, and the
China 973 Program grant 2009CB824800.
NR 68
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2011
VL 737
IS 1
AR 41
DI 10.1088/0004-637X/737/1/41
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 800BM
UT WOS:000293332200041
ER
PT J
AU Nelson, T
Mukai, K
Orio, M
Luna, GJM
Sokoloski, JL
AF Nelson, T.
Mukai, K.
Orio, M.
Luna, G. J. M.
Sokoloski, J. L.
TI X-RAY AND ULTRAVIOLET EMISSION FROM THE RECURRENT NOVA RS OPHIUCHI IN
QUIESCENCE: SIGNATURES OF ACCRETION AND SHOCKED GAS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE novae, cataclysmic variables; ultraviolet: stars; white dwarfs; X-rays:
stars
ID SYMBIOTIC STARS; CATACLYSMIC VARIABLES; 1985 OUTBURST; WHITE-DWARFS;
SPECTROSCOPY; BINARIES; ROSAT; SIMULATIONS; VARIABILITY; EXTINCTION
AB RS Ophiuchi is a recurrent nova system that experiences outbursts every similar to 20 years, implying accretion at a high rate onto a massive white dwarf. However, previous X-ray observations of the system in quiescence have detected only faint emission that is difficult to reconcile with the high accretion rate (>2 x 10(-8) M-circle dot yr(-1)) predicted by nova theory for such frequent outbursts. Here, we use new Chandra and XMM-Newton observations obtained 537 and 744 days after the 2006 outburst to constrain both the accretion rate onto the white dwarf and the properties of the nova ejecta at these times. We detect low level UV variability with the XMM-Newton Optical Monitor on day 744 that is consistent with accretion disk flickering, and use this to place a lower limit on the accretion rate at this epoch. The X-ray spectra in both observations are well described by a two component thermal plasma model. We identify the first component as the nova shell, which can emit X-rays for up to a decade after the outburst. The other component likely arises in the accretion disk boundary layer, and can be equally well fit by a single temperature plasma or a cooling flow model. Although the flux of the single temperature model implies an accretion rate that is 40 times too low to power the observed nova outburst rate (assuming that half of the accretion luminosity is emitted as X-rays in the boundary layer), the best-fit cooling flow model implies (M)over dot < 1.2 x 10(-8) M-circle dot yr(-1) 537 days after the outburst, which is within a factor of two of the theoretical accretion rate required to power an outburst every 20 years. Furthermore, we place an upper limit on the accretion rate through an optically thick region of the boundary layer of 2.0 x 10(-8) M-circle dot yr(-1). Thus, these new quiescence data are consistent with the accretion rate expectations of nova theory. Finally, we discuss the possible origins of the low temperature associated with the accretion component, which is a factor of 10 lower than in T CrB, an otherwise similar recurrent nova.
C1 [Nelson, T.; Mukai, K.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA.
[Nelson, T.; Mukai, K.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA.
[Nelson, T.; Mukai, K.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA.
[Orio, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[Orio, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Luna, G. J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Sokoloski, J. L.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA.
RP Nelson, T (reprint author), Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA.
EM thomas.nelson@nasa.gov
FU NASA [GO9-0027X, NAS8-03060, NNX09AF82G]; NASA-GSFC
FX We thank the anonymous referee for detailed comments and suggestions.
Support for this work was provided by NASA through Chandra award
GO9-0027X issued by the Chandra X-ray Observatory Center, which is
operated by the SAO for and on behalf of NASA under contract NAS8-03060,
and through award NNX09AF82G (to J.L.S.). This research made use of data
obtained from the High Energy Astrophysics Science Archive Research
Center (HEASARC), provided by NASA's Goddard Space Flight Center. T.N.
and M.O. acknowledge the support of the NASA-GSFC XMM-Newton program.
NR 54
TC 9
Z9 9
U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2011
VL 737
IS 1
AR 7
DI 10.1088/0004-637X/737/1/7
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 800BM
UT WOS:000293332200007
ER
PT J
AU Shen, CC
Lin, J
Murphy, NA
AF Shen, Chengcai
Lin, Jun
Murphy, Nicholas A.
TI NUMERICAL EXPERIMENTS ON FINE STRUCTURE WITHIN RECONNECTING CURRENT
SHEETS IN SOLAR FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE instabilities; magnetic reconnection; magnetohydrodynamics (MHD);
methods: numerical; plasmas; Sun: flares
ID CORONAL MASS EJECTION; FLUX-CORRECTED TRANSPORT; MAGNETIC RECONNECTION;
2-RIBBON FLARES; ERUPTIONS; LOOPS; INFLOWS; MOTIONS; ARCADE; MODEL
AB We perform resistive magnetohydrodynamic simulations to study the internal structure of current sheets that form during solar eruptions. The simulations start with a vertical current sheet in mechanical and thermal equilibrium that separates two regions of the magnetic field with opposite polarity which are line-tied at the lower boundary representing the photosphere. Reconnection commences gradually due to an initially imposed perturbation, but becomes faster when plasmoids form and produce small-scale structures inside the current sheet. These structures include magnetic islands or plasma blobs flowing in both directions along the sheet, and X-points between pairs of adjacent islands. Among these X-points, a principal one exists at which the reconnection rate reaches maximum. A fluid stagnation point (S-point) in the sheet appeared where the reconnection outflow bifurcates. The S-point and the principal X-point (PX-point) are not co-located in space though they are very close to one another. Their relative positions alternate as reconnection progresses and determine the direction of motion of individual magnetic islands. Newly formed islands move upward if the S-point is located above the PX-point, and downward if the S-point is below the PX-point. Merging of magnetic islands was observed occasionally between islands moving in the same direction. Reconnected plasma flow was observed to move faster than blobs nearby.
C1 [Shen, Chengcai; Lin, Jun] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China.
[Shen, Chengcai] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China.
[Lin, Jun; Murphy, Nicholas A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Shen, CC (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Yunnan, Peoples R China.
RI LIN, JUN/B-9890-2017;
OI Murphy, Nicholas/0000-0001-6628-8033
FU Program 973 [2011CB811403]; NSFC [10873030]; CAS [2009J2-34]; NASA
[NNX11AB61G]; Smithsonian Institution
FX The authors acknowledge useful discussions with J. C. Raymond and T. G.
Forbes. This work was supported by Program 973 grant 2011CB811403, NSFC
grant 10873030, and CAS grant 2009J2-34. J. L. and N.M. acknowledge
support from NASA grant NNX11AB61G to SAO, and from a grant from the
Smithsonian Institution Sprague Endowment Fund during FY10. Some
important calculations in this work were completed with the help of the
HPC Center, Kunming Institute of Botany, CAS.
NR 63
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U1 1
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 10
PY 2011
VL 737
IS 1
AR 14
DI 10.1088/0004-637X/737/1/14
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 800BM
UT WOS:000293332200014
ER
PT J
AU Gao, B
AF Gao, Bo
TI Analytic description of atomic interaction at ultracold temperatures.
II. Scattering around a magnetic Feshbach resonance
SO PHYSICAL REVIEW A
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATE; RELAXATION RATES; COLLISIONS; GASES
AB Starting from a multichannel quantum-defect theory, we derive analytic descriptions of a magnetic Feshbach resonance in an arbitrary partial wave l and the atomic interactions around it. An analytic formula, applicable to both broad and narrow resonances of arbitrary l, is presented for ultracold atomic scattering around a Feshbach resonance. Other related issues addressed include (a) the parametrization of a magnetic Feshbach resonance of arbitrary l, (b) rigorous definitions of "broad" and "narrow" resonances of arbitrary l and their different scattering characteristics, and (c) the tuning of the effective range and the generalized effective range by a magnetic field.
C1 [Gao, Bo] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA.
[Gao, Bo] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
RP Gao, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, 60 Garden St, Cambridge, MA 02138 USA.
EM bo.gao@utoledo.edu
RI Gao, Bo/B-8774-2008
OI Gao, Bo/0000-0002-6680-3725
FU NSF [PHY-0758042]
FX This work was partially supported by the NSF through a grant for ITAMP
at Harvard University and Smithsonian Astrophysical Observatory. The
work at Toledo was supported in part by the NSF under the Grant No.
PHY-0758042.
NR 58
TC 17
Z9 17
U1 1
U2 8
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 AUG 8
PY 2011
VL 84
IS 2
AR 022706
DI 10.1103/PhysRevA.84.022706
PG 12
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 803YC
UT WOS:000293618000009
ER
PT J
AU Longrich, NR
Olson, SL
AF Longrich, Nicholas R.
Olson, Storrs L.
TI The bizarre wing of the Jamaican flightless ibis Xenicibis xympithecus:
a unique vertebrate adaptation
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE Threskiornithidae; flightlessness; Jamaica; Quaternary
AB Birds have frequently evolved to exploit insular environments by becoming adapted to a terrestrial lifestyle and losing the ability to fly, usually via reducing the wings and pectoral girdle. The enigmatic flightless ibis Xenicibis xympithecus (Threskiornithidae) from the Quaternary of Jamaica provides a rare example of flight loss in ibises. We report on previously undescribed fossils of Xenicibis, and show that the wing differed radically from that of all other birds, flightless or volant. The metacarpus is elongate, grotesquely inflated and has extremely thick walls; phalanges are short and block-like; the radius is distally expanded; and the humerus is elongate. The furcula, coracoid and sternum are all well developed. We propose that the elongate forelimb and massive hand functioned in combat as a jointed club or flail. This hypothesis is supported by the morphology of the carpometacarpus, by features permitting rapid extension of the wing and by the presence of fractures in wing bones. Although other birds use the wings as weapons, none resemble Xenicibis, which represents a unique and extraordinary morphological solution to this functional problem. Xenicibis strikingly illustrates how similar selective pressures, acting on a similar starting point, can result in novel outcomes.
C1 [Longrich, Nicholas R.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06520 USA.
[Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20013 USA.
RP Longrich, NR (reprint author), Yale Univ, Dept Geol & Geophys, POB 208109, New Haven, CT 06520 USA.
EM nicholas.longrich@yale.edu
FU NSF; Alberta Ingenuity Graduate Studentship; Yale Institute for
Biospheric Studies
FX We thank Ross MacPhee for the opportunity to study the Red Hills
fossils. Discussions with Helen F. James and Richard L. Zusi and
guidance from B. Rosemary Grant were helpful in developing this project.
N.R.L. received support from an NSF Graduate Research Fellowship, an
Alberta Ingenuity Graduate Studentship and the Yale Institute for
Biospheric Studies. Finally, we thank the reviewers for their helpful
reviews of this paper. Fossil specimens are deposited in the Department
of Paleobiology, National Museum of Natural History (USNM), Smithsonian
Institution, Washington, DC.
NR 25
TC 3
Z9 4
U1 1
U2 13
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 AUG 7
PY 2011
VL 278
IS 1716
BP 2333
EP 2337
DI 10.1098/rspb.2010.2117
PG 5
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 783KT
UT WOS:000292081900012
PM 21208965
ER
PT J
AU Akre, KL
Farris, HE
Lea, AM
Page, RA
Ryan, MJ
AF Akre, Karin L.
Farris, Hamilton E.
Lea, Amanda M.
Page, Rachel A.
Ryan, Michael J.
TI Signal Perception in Frogs and Bats and the Evolution of Mating Signals
SO SCIENCE
LA English
DT Article
ID PHYSALAEMUS-PUSTULOSUS; TUNGARA FROGS; MATE CHOICE; SEXUAL SELECTION;
FEMALE PREFERENCES; CALL DURATION; PSYCHOPHYSICS; ADVERTISEMENT;
COMPLEXITY; TRAITS
AB Psychophysics measures the relationship between a stimulus's physical magnitude and its perceived magnitude. Because decisions are based on perception of stimuli, this relationship is critical to understanding decision-making. We tested whether psychophysical laws explain how female tungara frogs (Physalaemus pustulosus) and frog-eating bats (Trachops cirrhosus) compare male frog calls, and how this imposes selection on call evolution. Although both frogs and bats prefer more elaborate calls, they are less selective as call elaboration increases, because preference is based on stimulus ratios. Thus, as call elaboration increases, both relative attractiveness and relative predation risk decrease because of how receivers perceive and compare stimuli. Our data show that female cognition can limit the evolution of sexual signal elaboration.
C1 [Akre, Karin L.; Lea, Amanda M.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, New Orleans, LA 70112 USA.
[Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Kresge Hearing Labs, New Orleans, LA 70112 USA.
[Page, Rachel A.; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Akre, KL (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
EM kakre@mail.utexas.edu
FU NSF [IBN0078150]; NIH [P20RR016816]; STRI, NSF [0608131]; American
Association of University Women; P.E.O. Scholar award
FX We thank J. Saunders, S. Ozeroff, A. Shah, K. Miller, K. Loukes, S.
Troxell, S. Griffin, M. Moscoso, V. Fugere, and W. Wohlwend for help
conducting experiments. A. Mason and WABC 2011 participants gave helpful
suggestions. STRI provided excellent logistical support. Supported by an
NSF graduate research fellowship (K.L.A.), NIH grant P20RR016816
(H.E.F.), NSF grant IBN0078150 (M.J.R.), STRI, NSF grant 0608131, the
American Association of University Women, and a P.E.O. Scholar award
(R.A.P.).
NR 29
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U1 8
U2 93
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 AUG 5
PY 2011
VL 333
IS 6043
BP 751
EP 752
DI 10.1126/science.1205623
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 802LH
UT WOS:000293512100041
PM 21817052
ER
PT J
AU Bruna, EM
Izzo, TJ
Inouye, BD
Uriarte, M
Vasconcelos, HL
AF Bruna, Emilio M.
Izzo, Thiago J.
Inouye, Brian D.
Uriarte, Maria
Vasconcelos, Heraldo L.
TI Asymmetric Dispersal and Colonization Success of Amazonian Plant-Ants
Queens
SO PLOS ONE
LA English
DT Article
ID LONG-DISTANCE DISPERSAL; SPECIES COEXISTENCE; SEED DISPERSAL; HOST
PLANTS; MUTUALISM; PATTERNS; RECRUITMENT; COMPETITION; LIMITATION;
COMMUNITY
AB Background: The dispersal ability of queens is central to understanding ant life-history evolution, and plays a fundamental role in ant population and community dynamics, the maintenance of genetic diversity, and the spread of invasive ants. In tropical ecosystems, species from over 40 genera of ants establish colonies in the stems, hollow thorns, or leaf pouches of specialized plants. However, little is known about the relative dispersal ability of queens competing for access to the same host plants.
Methodology/Principal Findings: We used empirical data and inverse modeling-a technique developed by plant ecologists to model seed dispersal-to quantify and compare the dispersal kernels of queens from three Amazonian ant species that compete for access to host-plants. We found that the modal colonization distance of queens varied 8-fold, with the generalist ant species (Crematogaster laevis) having a greater modal distance than two specialists (Pheidole minutula, Azteca sp.) that use the same host-plants. However, our results also suggest that queens of Azteca sp. have maximal distances that are four-sixteen times greater than those of its competitors.
Conclusions/Significance: We found large differences between ant species in both the modal and maximal distance ant queens disperse to find vacant seedlings used to found new colonies. These differences could result from interspecific differences in queen body size, and hence wing musculature, or because queens differ in their ability to identify potential host plants while in flight. Our results provide support for one of the necessary conditions underlying several of the hypothesized mechanisms promoting coexistence in tropical plant-ants. They also suggest that for some ant species limited dispersal capability could pose a significant barrier to the rescue of populations in isolated forest fragments. Finally, we demonstrate that inverse models parameterized with field data are an excellent means of quantifying the dispersal of ant queens.
C1 [Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA.
[Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL USA.
[Izzo, Thiago J.] Univ Fed Mato Grosso, Dept Bot & Ecol, Cuiaba, Mato Grosso, Brazil.
[Inouye, Brian D.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA.
[Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA.
[Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38400 Uberlandia, MG, Brazil.
[Bruna, Emilio M.; Izzo, Thiago J.; Inouye, Brian D.; Uriarte, Maria; Vasconcelos, Heraldo L.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil.
[Bruna, Emilio M.; Izzo, Thiago J.; Inouye, Brian D.; Uriarte, Maria; Vasconcelos, Heraldo L.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil.
RP Bruna, EM (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA.
EM embruna@ufl.edu
RI Bruna, Emilio/H-2769-2012; Vasconcelos, Heraldo/C-3353-2013; Izzo,
Thiago/K-7405-2012; Uriarte, Maria/L-8944-2013; Bruna, Elena/C-4939-2014
OI Bruna, Emilio/0000-0003-3381-8477; Vasconcelos,
Heraldo/0000-0001-6969-7131; Izzo, Thiago/0000-0002-4613-3787; Bruna,
Elena/0000-0001-5427-1461
FU US National Science Foundation [DEB-0453631, DEB-0452720]; University of
Florida
FX This research was supported by Grants DEB-0453631 and DEB-0452720 from
the US National Science Foundation (http://nsf.gov). Publication of this
article was funded in part by the University of Florida Open-Access
Publishing Fund. The funders had no role in study design, data
collection and analysis, decision to publish, or preparation of the
manuscript.
NR 51
TC 9
Z9 9
U1 1
U2 21
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 AUG 3
PY 2011
VL 6
IS 8
AR e22937
DI 10.1371/journal.pone.0022937
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 803CQ
UT WOS:000293558900045
PM 21826219
ER
PT J
AU Zug, GR
Gotte, SW
Jacobs, JF
AF Zug, George R.
Gotte, Steve W.
Jacobs, Jeremy F.
TI Pythons in Burma: Short-tailed python (Reptilia: Squamata)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE biogeography; herpetofauna; morphometrics; scalation
ID SOUTHEAST-ASIA; CONSERVATION; AMPHIBIANS
AB Short-tailed pythons, Python curtus species group, occur predominantly in the Malayan Peninsula, Sumatra, and Borneo. The discovery of an adult female in Mon State, Myanmar, led to a review of the distribution of all group members (spot-mapping of all localities of confirmed occurrence) and an examination of morphological variation in P. brongersmai. The resulting maps demonstrate a limited occurrence of these pythons within peninsular Malaya, Sumatra, and Borneo with broad absences in these regions. Our small samples limit the recognition of regional differentiation in the morphology of P. brongersmai populations; however, the presence of unique traits in the Myanmar python and its strong allopatry indicate that it is a unique genetic lineage, and it is described as Python kyaiktiyo new species.
C1 [Zug, George R.; Jacobs, Jeremy F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Gotte, Steve W.] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Museum Support Ctr, Suitland, MD 20746 USA.
RP Zug, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
EM zugg@si.edu
NR 53
TC 3
Z9 4
U1 0
U2 1
PU BIOL SOC WASHINGTON
PI WASHINGTON
PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA
SN 0006-324X
J9 P BIOL SOC WASH
JI Proc. Biol. Soc. Wash.
PD AUG 2
PY 2011
VL 124
IS 2
BP 112
EP 136
PG 25
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 805XY
UT WOS:000293765600007
ER
PT J
AU Pyle, P
Welch, AJ
Fleischer, RC
AF Pyle, Peter
Welch, Andreanna J.
Fleischer, Robert C.
TI A NEW SPECIES OF SHEARWATER (PUFFINUS) RECORDED FROM MIDWAY ATOLL,
NORTHWESTERN HAWAIIAN ISLANDS
SO CONDOR
LA English
DT Article
DE Bryan's Shearwater; Puffinus bryani; morphometrics; cytochrome b;
phylogenetics; Procellariiformes
ID BAYESIAN PHYLOGENETIC INFERENCE; MITOCHONDRIAL-DNA; JOUANINS PETREL;
AVES; PHYLOGEOGRAPHY; PROCELLARIIDAE; SYSTEMATICS; PTERODROMA; SEQUENCE;
BIOLOGY
AB Small black-and-white shearwaters of the genus Puffinus are distributed globally, and their phylogenetic relationships are complex and uncertain. In 1963 a small shearwater collected at Midway Atoll in the North Pacific Ocean was identified as a Little Shearwater (P. assimilis), but several physical features suggest closer alliance with Audubon's Shearwater (P. lherminieri) and its relatives. Biometrics indicate that the taxon this specimen represents is smaller than any other known shearwater, and phylogenetic analyses indicate it is distinct, with a pair-wise sequence divergence of at least 3.8% from related taxa. We thus propose a new species based on the specimen: Bryan's Shearwater (Puffinus bryani nom. nov.). The breeding and nonbreeding ranges of Bryan's Shearwater are unknown, but a physical resemblance to the North Atlantic boydi (of controversial taxonomic status within Puffinus) suggests an affiliation with subtropical or tropical waters. Bryan's Shearwater is apparently rare and could be threatened by extinction; therefore, additional information is needed to increase our understanding of this taxon and its conservation requirements.
C1 [Pyle, Peter] Inst Bird Populat, Point Reyes Stn, CA 94956 USA.
[Welch, Andreanna J.; Fleischer, Robert C.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
[Welch, Andreanna J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
RP Pyle, P (reprint author), Inst Bird Populat, POB 1346, Point Reyes Stn, CA 94956 USA.
EM ppyle@birdpop.org
FU National Science Foundation [DEB-0745604]; Smithsonian Institution
FX We are indebted to Storrs Olson and Steve N. G. Howell for assistance
studying the specimen at USNM and for discussion of small shearwaters.
We are grateful to Gary Graves and James Dean for permission to sample
the novel specimen and measure specimens at USNM and to Nick Holmes for
providing the tissue of P. newelli. We thank Maureen Flannery at the
California Academy of Sciences, Carla Cicero at the Museum of Vertebrate
Zoology, and Carla Kishinami of the Bishop Museum for assistance
measuring specimens, and members of the Center for Conservation and
Evolutionary Genetics at the National Zoological Park, Smithsonian
Institution, especially Nancy Rotzel and Carl McIntosh, for logistic
support. National Science Foundation grant DEB-0745604 to Margaret
Ostrom, Robert Fleischer, and Helen James, and the Smithsonian
Institution, provided funds for the DNA analyses. We thank Richard Pyle
of the Bishop Museum for help in the naming of P. bryani, and we thank
Richard and Leilani Pyle and Anita Manning for background information on
Edward Bryan, grandfather of the first author of this paper. Comments
from Steve N. G. Howell, Hadoram Shirihai, and four anonymous reviewers
helped to improve the manuscript. This is contribution number 402 of The
Institute for Bird Populations.
NR 45
TC 8
Z9 10
U1 1
U2 6
PU COOPER ORNITHOLOGICAL SOC
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0010-5422
J9 CONDOR
JI Condor
PD AUG
PY 2011
VL 113
IS 3
BP 518
EP 527
DI 10.1525/cond.2011.100117
PG 10
WC Ornithology
SC Zoology
GA 818ZZ
UT WOS:000294796500006
ER
PT J
AU Diggs, NE
Marra, PP
Cooper, RJ
AF Diggs, Nora E.
Marra, Peter P.
Cooper, Robert J.
TI RESOURCE LIMITATION DRIVES PATTERNS OF HABITAT OCCUPANCY DURING THE
NONBREEDING SEASON FOR AN OMNIVOROUS SONGBIRD
SO CONDOR
LA English
DT Article
DE behavioral dominance; Catharus guttatus; diet; habitat quality; Hermit
Thrush; stable isotopes; winter
ID WINTERING HERMIT THRUSHES; STABLE-ISOTOPES; TEMPORAL VARIATION;
CATHARUS-GUTTATUS; MIGRATORY BIRD; FRUIT REMOVAL; MIGRANT BIRD; FAT
STORAGE; DIET; DOMINANCE
AB The role of food in limiting migratory birds during the nonbreeding period is poorly understood, in part because of the complexities of quantifying food availability and diet. We tracked overwinter changes in the availability of arthropods and fruits, the primary winter foods of the Hermit Thrush (Catharus guttatus), a short-distance migrant. Fruit availability declined over the winter, and arthropod availability fluctuated with changing temperature. Concurrently, using fecal samples and stable isotopes, we tracked relative food consumption. In fecal samples fruit declined from early to mid season and delta(13)C and delta(15)N isotope signatures in blood became more enriched, consistent with a decline in fruit consumption and an increase in arthropod consumption. Larger-bodied birds, predominantly males, maintained territories in which the abundance of arthropods was higher, had a greater proportion of arthropods in their diet and less variation in delta(13)C (indicator of a stable diet) and fat loads over the winter. In contrast, smaller-bodied birds, primarily females, gained fat midwinter in response to unpredictable and lower-quality resources. These results are consistent with both a size-mediated form of dominance and sexual habitat segregation, such that smaller bodied birds, mainly females, may be behaviorally excluded from optimal territories. Future research should focus on the long-term consequences of food limitation in the nonbreeding season and size and sex-mediated dominance behavior on both the condition of birds within a season and on subsequent breeding success and survival.
C1 [Diggs, Nora E.; Marra, Peter P.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Diggs, Nora E.; Cooper, Robert J.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA.
RP Diggs, NE (reprint author), Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA.
EM diggsn@si.edu
FU LowCountry Institute; Spring Island community; University of Georgia's
Warnell School of Forestry and Natural Resources; Smithsonian
Institution
FX Funding was provided by the LowCountry Institute and supported by the
Spring Island community. Chris Marsh was especially instrumental in
facilitating and supporting this research. Additional funding and
resources were provided by the University of Georgia's Warnell School of
Forestry and Natural Resources and a Smithsonian Institution Fellowship.
We thank all those who helped in the field, especially S. Conrad, S.
Buck, and A. Byrd. Thanks to C. Studds, B. Ballentine, M. Reudink, B.
Ryder, and R. Curry for reviews and advice.
NR 48
TC 12
Z9 12
U1 2
U2 30
PU COOPER ORNITHOLOGICAL SOC
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0010-5422
J9 CONDOR
JI Condor
PD AUG
PY 2011
VL 113
IS 3
BP 646
EP 654
DI 10.1525/cond.2011.090201
PG 9
WC Ornithology
SC Zoology
GA 818ZZ
UT WOS:000294796500020
ER
PT J
AU Farris, HE
Ryan, MJ
AF Farris, Hamilton E.
Ryan, Michael J.
TI Relative comparisons of call parameters enable auditory grouping in
frogs
SO NATURE COMMUNICATIONS
LA English
DT Article
ID FEMALE TUNGARA FROGS; STREAM SEGREGATION; PHYSALAEMUS-PUSTULOSUS; SEXUAL
SELECTION; GREY TREEFROGS; BACKGROUND-NOISE; SPATIAL RELEASE; MATING
SIGNALS; COCKTAIL PARTY; COMPLEX SOUNDS
AB Whereas many studies on mate choice have measured the relative attractiveness of acoustic sexual signals, there is little understanding of another critical process: grouping and assigning the signals to their sources. For female tungara frogs, assigning the distinct components of male calls to the correct source is a challenge because males sing in aggregations, producing overlapping calls that lead to perceptual errors analogous to those of the 'cocktail party problem'. Here we show that for presentation of >2 call components, however, subjects are more likely to group the two components with the smallest relative differences in call parameters, including relative spatial separation (a primitive acoustic cue) and relative similarity to the species-specific call sequence (a schema-based cue). Thus, like humans, the cognitive rules for the perception of auditory groups amidst multiple sound sources include the use of relative comparisons, a flexible strategy for dynamic acoustic environments.
C1 [Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, New Orleans, LA 70112 USA.
[Farris, Hamilton E.] Louisiana State Univ, Hlth Sci Ctr, Kresge Hearing Labs, New Orleans, LA 70112 USA.
[Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Farris, HE (reprint author), Louisiana State Univ, Hlth Sci Ctr, Ctr Neurosci, New Orleans, LA 70112 USA.
EM hfarri@lsuhsc.edu
FU NSF [IBN 98 16564]; NIH [P20RR016816]
FX Helpful input was provided by: T. Forrest, W. Wilczynski, X. Bernal, A.
Baugh, E. Golob, A. Lea and S. Rand. N. Lessios, A. Dapper, L. Zeigler,
S. Ozeroff and J. Saunders assisted in collecting frogs and running
experiments. This research was supported by NSF IBN 98 16564 to MJR. HEF
was supported by NIH P20RR016816 (to N. Bazan). We thank the Smithsonian
Tropical Research Institute for their hospitality and logistical
support.
NR 60
TC 15
Z9 15
U1 1
U2 14
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2041-1723
J9 NAT COMMUN
JI Nat. Commun.
PD AUG
PY 2011
VL 2
AR 410
DI 10.1038/ncomms1417
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 819DV
UT WOS:000294806500003
PM 21811239
ER
PT J
AU Larsen, SS
de Mink, SE
Eldridge, JJ
Langer, N
Bastian, N
Seth, A
Smith, LJ
Brodie, J
Efremov, YN
AF Larsen, S. S.
de Mink, S. E.
Eldridge, J. J.
Langer, N.
Bastian, N.
Seth, A.
Smith, L. J.
Brodie, J.
Efremov, Yu N.
TI Resolved photometry of extragalactic young massive star clusters
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE open clusters and associations: general; galaxies: star clusters:
general; galaxies: spiral; Hertzsprung-Russell and C-M diagrams
ID MULTIPLE STELLAR POPULATIONS; COLOR-MAGNITUDE DIAGRAMS;
LARGE-MAGELLANIC-CLOUD; RED SUPERGIANT RATIO; STARBURST GALAXY NGC-1569;
PERIOD-AGE RELATION; BLUE-TO-RED; GLOBULAR-CLUSTERS; SPIRAL GALAXIES;
MAIN-SEQUENCE
AB Aims. We present colour-magnitude diagrams (CMDs) of young massive star clusters in several galaxies located well beyond the Local Group. The richness of these clusters allows us to obtain large samples of post-main sequence stars and test how well the observed CMDs are reproduced by canonical stellar isochrones.
Methods. We use imaging of seven clusters in the galaxies NGC 1313, NGC 1569, NGC 1705, NGC 5236 and NGC 7793 obtained with the Advanced Camera for Surveys on board the Hubble Space Telescope and carry out PSF-fitting photometry of individual stars in the clusters. The clusters have ages in the range similar to(5-50) x 10(6) years and masses of similar to 10(5) M-circle dot-10(6) M-circle dot. Although crowding prevents us from obtaining photometry in the inner regions of the clusters, we are still able to measure up to 30-100 supergiant stars in each of the richest clusters. The resulting CMDs and luminosity functions are compared with photometry of artificially generated clusters, designed to reproduce the photometric errors and completeness as realistically as possible.
Results. In agreement with previous studies, our CMDs show no clear gap between the H-burning main sequence and the He-burning supergiant stars, contrary to predictions by common stellar isochrones. In general, the isochrones also fail to match the observed number ratios of red-to-blue supergiant stars, although the difficulty of separating blue supergiants from the main sequence complicates this comparison. In several cases we observe a large spread (1-2 mag) in the luminosities of the supergiant stars that cannot be accounted for by observational errors. We find that this spread can be reproduced by including an age spread of similar to(10-30) x 10(6) years in the models. However, age spreads cannot fully account for the observed morphology of the CMDs and other processes, such as the evolution of interacting binary stars, may also play a role.
Conclusions. Colour-magnitude diagrams can be successfully obtained for massive star clusters out to distances of at least 4-5 Mpc. Comparing such CMDs with models based on canonical isochrones we find several areas of disagreement. One interesting possibility is that an age spread of up to similar to 30 Myr may be present in some clusters. The data presented here may provide useful constraints on models for single and/or binary stellar evolution.
C1 [Larsen, S. S.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands.
[de Mink, S. E.; Smith, L. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Eldridge, J. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Langer, N.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany.
[Seth, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Brodie, J.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Efremov, Yu N.] Moscow M V Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Smith, L. J.] European Space Agcy, Res & Sci Support Dept, Baltimore, MD 21218 USA.
RP Larsen, SS (reprint author), Univ Utrecht, Astron Inst, Princetonpl 5, NL-3584 CC Utrecht, Netherlands.
EM s.s.larsen@astro-uu.nl
OI de Mink, Selma/0000-0001-9336-2825
FU NASA, Space Telescope Science Institute [HST-HF-51270.01-A]; NASA [NAS
5-26555]; Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)
FX We thank Livia Origlia for discussion and comments, and the anonymous
referee for a careful reading of the manuscript and several suggestions
that helped us clarify the presentation. S.d.M. is supported by NASA
through Hubble Fellowship grant HST-HF-51270.01-A awarded by the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Inc., for NASA, under contract
NAS 5-26555. S.S.L. acknowledges support from the Nederlandse
Organisatie voor Wetenschappelijk Onderzoek (NWO) via a VIDI grant.
NR 96
TC 32
Z9 32
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 AUG
PY 2011
VL 532
AR A147
DI 10.1051/0004-6361/201117185
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 807ZS
UT WOS:000293942700046
ER
PT J
AU Schinzel, FK
Sokolovsky, KV
D'Ammando, F
Burnett, TH
Max-Moerbeck, W
Cheung, CC
Fegan, SJ
Casandjian, JM
Reyes, LC
Villata, M
Raiteri, CM
Agudo, I
Calle, OJAB
Carosati, D
Casas, R
Gomez, JL
Gurwell, MA
Hsiao, HY
Jorstad, SG
Kimeridze, G
Konstantinova, TS
Kopatskaya, EN
Koptelova, E
Kurtanidze, OM
Kurtanidze, SO
Larionov, VM
Larionova, EG
Larionova, LV
Marscher, AP
Morozova, DA
Nikolashvili, MG
Roca-Sogorb, M
Ros, JA
Sigua, LA
Spiridonova, O
Troitsky, IS
Vlasyuk, VV
Lobanov, AP
Zensus, JA
AF Schinzel, F. K.
Sokolovsky, K. V.
D'Ammando, F.
Burnett, T. H.
Max-Moerbeck, W.
Cheung, C. C.
Fegan, S. J.
Casandjian, J. M.
Reyes, L. C.
Villata, M.
Raiteri, C. M.
Agudo, I.
Calle, O. J. A. Bravo
Carosati, D.
Casas, R.
Gomez, J. L.
Gurwell, M. A.
Hsiao, H. Y.
Jorstad, S. G.
Kimeridze, G.
Konstantinova, T. S.
Kopatskaya, E. N.
Koptelova, E.
Kurtanidze, O. M.
Kurtanidze, S. O.
Larionov, V. M.
Larionova, E. G.
Larionova, L. V.
Marscher, A. P.
Morozova, D. A.
Nikolashvili, M. G.
Roca-Sogorb, M.
Ros, J. A.
Sigua, L. A.
Spiridonova, O.
Troitsky, I. S.
Vlasyuk, V. V.
Lobanov, A. P.
Zensus, J. A.
TI Identification of gamma-ray emission from 3C 345 and NRAO 512
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; quasars: individual: 3C 345; gamma rays: galaxies;
quasars: individual: NRAO512; quasars: individual: B3 1640+396
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; SWIFT ULTRAVIOLET/OPTICAL
TELESCOPE; BL-LACERTAE OBJECTS; ALL-SKY SURVEY; LIKELIHOOD RATIO; SOURCE
CATALOG; DATA RELEASE; SOURCE LIST; VARIABILITY
AB For more than 15 years, since the days of the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO; 1991-2000), it has remained an open question why the prominent blazar 3C 345 was not reliably detected at gamma-ray energies >= 20 MeV. Recently a bright gamma-ray source (0FGL J1641.4+3939/1FGL J1642.5+3947), potentially associated with 3C 345, was detected by the Large Area Telescope (LAT) on Fermi. Multiwavelength observations from radio bands to X-rays (mainly GASP-WEBT and Swift) of possible counterparts (3C 345, NRAO512, B3 1640+396) were combined with 20 months of Fermi-LAT monitoring data (August 2008-April 2010) to associate and identify the dominating gamma-ray emitting counterpart of 1FGL J1642.5+3947. The source 3C 345 is identified as the main contributor for this gamma-ray emitting region. However, after November 2009 (15 months), a significant excess of photons from the nearby quasar NRAO512 started to contribute and thereafter was detected with increasing gamma-ray activity, possibly adding flux to 1FGL J1642.5+3947. For the same time period and during the summer of 2010, an increase of radio, optical and X-ray activity of NRAO512 was observed. No gamma-ray emission from B3 1640+396 was detected.
C1 [Schinzel, F. K.; Sokolovsky, K. V.; Lobanov, A. P.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Sokolovsky, K. V.] Astro Space Ctr Lebedev, Inst Phys, Moscow 117997, Russia.
[D'Ammando, F.] INAF IASF Palermo, I-90146 Palermo, Italy.
[D'Ammando, F.; Larionova, E. G.] INAF IASF Roma, I-00133 Rome, Italy.
[Burnett, T. H.] Univ Washington, Dept Phys, Seattle, WA 98195 USA.
[Max-Moerbeck, W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA.
[Cheung, C. C.] USN, Res Lab, Washington, DC 20375 USA.
[Fegan, S. J.] Ecole Polytech, Lab Leprince Ringuet, F-91128 Palaiseau, France.
[Casandjian, J. M.] CEA IRFU CNRS Univ Paris Diderot, Lab AIM, Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France.
[Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Agudo, I.; Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Calle, O. J. A. Bravo; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain.
[Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain.
[Casas, R.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Hsiao, H. Y.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan.
[Kimeridze, G.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Larionov, V. M.] Pulkovo Astron Observ, St Petersburg 196140, Russia.
[Ros, J. A.] Agrupacio Astron Sabadell, Sabadell 08206, Spain.
[Spiridonova, O.; Vlasyuk, V. V.] Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia.
RP Schinzel, FK (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM schinzel@mpifr-bonn.mpg.de
RI Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013;
Larionova, Elena/H-7287-2013; Lobanov, Andrei/G-5891-2014; Kurtanidze,
Omar/J-6237-2014; Sokolovsky, Kirill/D-2246-2015; Agudo,
Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy,
Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina,
Tatiana/H-6873-2013
OI Villata, Massimo/0000-0003-1743-6946; Larionova,
Liudmila/0000-0002-0274-1481; Larionov, Valeri/0000-0002-4640-4356;
Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova,
Elena/0000-0002-2471-6500; Sokolovsky, Kirill/0000-0001-5991-6863;
Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804;
Troitskiy, Ivan/0000-0002-4218-0148; Jorstad,
Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676
FU International Max Planck Research School (IMPRS) for Astronomy and
Astrophysics at the Universities of Bonn and Cologne; Russian RFBR
foundation [09-02-00092]; Spanish Ministry of Science and Innovation;
Regional Government of Andalucia [AYA2007-67626-C03-03, P09-FQM-4784];
Georgian National Science Foundation [GNSF/ST08/4-404]; NASA
[NNX08AV65G, NNX08AV61G, NNX09AT99G]; National Science Foundation
[AST-0907893]; Smithsonian Institution; Academia Sinica
FX The authors would like to thank Ann Wehrle, Benoit Lott, Seth Digel,
Gino Tosti, Dave Thompson, and Greg Taylor for their helpful comments
and useful discussions, which improved the quality of this manuscript.
We thank the A&A referee for extensive comments. The Fermi-LAT
Collaboration acknowledges generous ongoing support from a number of
agencies and institutes that have supported both the development and the
operation of the LAT as well as scientific data analysis. These include
the National Aeronautics and Space Administration and the Department of
Energy in the United States, the Commissariat a l'Energie Atomique and
the Centre National de la Recherche Scientifique/Institut National de
Physique Nucleaire et de Physique des Particules in France, the Agenzia
Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in
Italy, the Ministry of Education, Culture, Sports, Science and
Technology (MEXT), High Energy Accelerator Research Organization (KEK)
and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A.
Wallenberg Foundation, the Swedish Research Council and the Swedish
National Space Board in Sweden. Additional support for science analysis
during the operations phase is gratefully acknowledged from the Istituto
Nazionale di Astrofisica in Italy and the Centre National d'Etudes
Spatiales in France. Frank Schinzel and Kirill Sokolovsky were supported
for this research through a stipend from the International Max Planck
Research School (IMPRS) for Astronomy and Astrophysics at the
Universities of Bonn and Cologne. M. Villata organized the
optical-to-radio observations by GASP-WEBT as the president of the
collaboration. Additional support for science analysis during the
operations phase is gratefully acknowledged from the Istituto Nazionale
di Astrofisica in Italy and the Centre National d'Etudes Spatiales in
France. The St. Petersburg University team acknowledges support from
Russian RFBR foundation via grant 09-02-00092. Acquisition of the MAPCAT
data is supported in part by the Spanish Ministry of Science and
Innovation and the Regional Government of Andalucia through grants
AYA2007-67626-C03-03 and P09-FQM-4784, respectively. The Abastumani team
acknowledges financial support by the Georgian National Science
Foundation through grant GNSF/ST08/4-404. A. Marscher and S. Jorstad
received support for this work from NASA grants NNX08AV65G, NNX08AV61G,
and NNX09AT99G, and National Science Foundation grant AST-0907893 to
Boston University. 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 paper is partly based on
observations carried out at the German-Spanish Calar Alto Observatory,
which is jointly operated by the MPIA and the IAA-CSIC. This research
has made use of NASA's Astrophysics Data System, the SIMBAD database,
operated at CDS, Strasbourg, France and the NASA/IPAC Extragalactic
Database (NED) which is operated by the JPL, Caltech, under contract
with NASA. This research has made use of data from the MOJAVE database
that is maintained by the MOJAVE team (Lister et al. 2009).
NR 59
TC 2
Z9 2
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 AUG
PY 2011
VL 532
AR A150
DI 10.1051/0004-6361/201016145
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 807ZS
UT WOS:000293942700049
ER
PT J
AU Enoch, ML
Corder, S
Duchene, G
Bock, DC
Bolatto, AD
Culverhouse, TL
Kwon, W
Lamb, JW
Leitch, EM
Marrone, DP
Muchovej, SJ
Perez, LM
Scott, SL
Teuben, PJ
Wright, MCH
Zauderer, BA
AF Enoch, Melissa L.
Corder, Stuartt
Duchene, Gaspard
Bock, Douglas C.
Bolatto, Alberto D.
Culverhouse, Thomas L.
Kwon, Woojin
Lamb, James W.
Leitch, Erik M.
Marrone, Daniel P.
Muchovej, Stephen J.
Perez, Laura M.
Scott, Stephen L.
Teuben, Peter J.
Wright, Melvyn C. H.
Zauderer, B. Ashley
TI DISK AND ENVELOPE STRUCTURE IN CLASS 0 PROTOSTARS. II. HIGH-RESOLUTION
MILLIMETER MAPPING OF THE SERPENS SAMPLE
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE ISM: individual objects (Serpens); stars: formation; submillimeter: ISM;
techniques: interferometric
ID CURRENT STAR-FORMATION; YOUNG STELLAR OBJECTS; SPITZER C2D SURVEY;
MOLECULAR CLOUD; UNBIASED SUBMILLIMETER; EMBEDDED PROTOSTARS;
SUBARCSECOND SURVEY; MIDINFRARED SURVEYS; CORE; PERSEUS
AB We present high-resolution CARMA 230 GHz continuum imaging of nine deeply embedded protostars in the Serpens Molecular Cloud, including six of the nine known Class 0 protostars in Serpens. This work is part of a program to characterize disk and envelope properties for a complete sample of Class 0 protostars in nearby low-mass star-forming regions. Here, we present CARMA maps and visibility amplitudes as a function of uv-distance for the Serpens sample. Observations are made in the B, C, D, and E antenna configurations, with B configuration observations utilizing the CARMA Paired Antenna Calibration System. Combining data from multiple configurations provides excellent uv-coverage (4-500 k lambda), allowing us to trace spatial scales from 10(2) to 10(4) AU. We find evidence for compact disk components in all of the observed Class 0 protostars, suggesting that disks form at very early times (t < 0.2 Myr) in Serpens. We make a first estimate of disk masses using the flux at 50 k lambda, where the contribution from the envelope should be negligible, assuming an unresolved disk. The resulting disk masses range from 0.04 M-circle dot to 1.7 M-circle dot, with a mean of approximately 0.2 M-circle dot. Our high-resolution maps are also sensitive to binary or multiple sources with separations greater than or similar to 250 AU, but significant evidence of multiplicity on scales < 2000 AU is seen in only one source.
C1 [Enoch, Melissa L.; Duchene, Gaspard; Wright, Melvyn C. H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Corder, Stuartt] NRAO ALMA JAO, Santiago, Chile.
[Duchene, Gaspard] UJF Grenoble 1 CNRS INSU, Inst Planetol & Astrophys Grenoble IPAG UMR 5274, F-38041 Grenoble, France.
[Bock, Douglas C.] Combined Array Res Millimeter Wave Astron, Big Pine, CA 93513 USA.
[Bolatto, Alberto D.; Teuben, Peter J.; Zauderer, B. Ashley] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bolatto, Alberto D.; Teuben, Peter J.; Zauderer, B. Ashley] Univ Maryland, Lab Millimeter Wave Astron, College Pk, MD 20742 USA.
[Culverhouse, Thomas L.; Lamb, James W.; Leitch, Erik M.; Muchovej, Stephen J.; Scott, Stephen L.] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA.
[Kwon, Woojin] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Leitch, Erik M.; Marrone, Daniel P.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Perez, Laura M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Zauderer, B. Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Enoch, ML (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
OI Marrone, Daniel/0000-0002-2367-1080
FU NASA [HST-HF-51259.01]; Jet Propulsion Laboratory (JPL); California
Institute of Technology; National Science Foundation; CARMA partner
universities
FX The authors thank the referee for comments and suggestions that improved
this manuscript. Support for this work was provided by NASA through the
Spitzer Space Telescope Fellowship Program, through a contract issued by
the Jet Propulsion Laboratory (JPL), California Institute of Technology,
under a contract with NASA. D. P. M. was supported by NASA through
Hubble Fellowship grant HST-HF-51259.01 Support for CARMA construction
was derived from the states of California, Illinois, and Maryland, the
Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris
Foundation, the Associates of the California Institute of Technology,
and the National Science Foundation. Ongoing CARMA development and
operations are supported by the National Science Foundation under a
cooperative agreement, and by the CARMA partner universities.
NR 54
TC 34
Z9 34
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2011
VL 195
IS 2
AR 21
DI 10.1088/0067-0049/195/2/21
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RP
UT WOS:000294773000010
ER
PT J
AU Ogle, PM
Wehrle, AE
Balonek, T
Gurwell, MA
AF Ogle, Patrick M.
Wehrle, Ann E.
Balonek, Thomas
Gurwell, Mark A.
TI BLAZAR 3C 454.3 IN OUTBURST AND QUIESCENCE DURING 2005-2007: TWO
VARIABLE SYNCHROTRON EMISSION PEAKS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: jets; quasars: individual (3C 454.3)
ID SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; RAY BRIGHT
BLAZARS; SPACE-TELESCOPE OBSERVATIONS; BL LACERTAE OBJECTS; BASE-LINE
ARRAY; MULTIWAVELENGTH OBSERVATIONS; PHOTOMETRIC CALIBRATION; INFRARED
OBSERVATIONS; NONTHERMAL SOURCES
AB We monitored the flaring blazar 3C 454.3 during 2005 June-July with the Spitzer Infrared Spectrograph (IRS: 15 epochs), Infrared Array Camera (IRAC: 12 epochs), and Multiband Imaging Photometer (MIPS: 2 epochs). We also made Spitzer IRS, IRAC, and MIPS observations from 2006 December to 2007 January when the source was in a low state, the latter simultaneous with a single Chandra X-ray observation. In addition, we present optical and submillimeter (sub-mm) monitoring data. The 2005-2007 period saw three major outbursts. We present evidence that the radio-optical spectral energy distribution (SED) actually consists of two variable synchrotron peaks, the primary at IR and the secondary at sub-mm wavelengths. The lag between the optical and sub-mm outbursts may indicate that these two peaks arise from two distinct regions along the jet separated by a distance of 0.9-3 pc. The flux at 5-35 mu m varied by a factor of 40 and the IR peak varied in frequency from 4 x 10(12) Hz to 4 x 10(13) Hz between the highest and lowest states in 2005 and 2006, respectively. Variability was well correlated across the mid-IR band, with no measurable lag. Flares that doubled in flux occurred on a timescale of similar to 5 days, yielding a variability size of <0.05 pc. The IR SED peak moved to higher frequency as a flare brightened, then returned to lower frequency as it decayed. The fractional variability amplitude increased with frequency, which we attribute to decreasing synchrotron self-absorption optical depth. Mid-IR flares may signal the re-energization of a shock that runs into inhomogeneities along the pre-existing jet or in the external medium. The synchrotron peak frequencies during each major outburst may depend upon both the distance from the jet apex and the physical conditions in the shocks. Variation of the Doppler parameter along a curved or helical jet is another possibility. Frequency variability of the IR synchrotron peak may have important consequences for the interpretation of the blazar sequence, and the presence of a secondary peak may give insight into jet structure.
C1 [Ogle, Patrick M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
[Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA.
[Balonek, Thomas] Colgate Univ, Dept Phys & Astron, Colgate, NY 13346 USA.
[Gurwell, Mark A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Ogle, PM (reprint author), CALTECH, Spitzer Sci Ctr, Mail Code 220-6, Pasadena, CA 91125 USA.
EM ogle@ipac.caltech.edu
FU Jet Propulsion Laboratory, California Institute of Technology under NASA
[1407]; 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 NASA contract 1407. Optical
observations at Palomar Observatory were made possible through the NASA
Space Interferometry Mission Preparatory Science Program for the Key
Project on Active Galactic Nuclei. Support for this work was provided by
NASA through awards issued by JPL/Caltech. 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 work is partly
based on data taken and assembled by the WEBT collaboration and stored
in the WEBT archive at the Osservatorio Astronomico di Torino-INAF
(http://www.oato.inaf.it/blazars/webt/). We are grateful to Karl Gordon
(Arizona) and Jason Surace (Spitzer Science Center) for assistance in
processing MIPS and IRAC data, and to Booth Hartley for customizing IPAC
Skyview for use on Intel Macs. We are grateful to Massimo Villata and
Claudia Raiteri for providing WEBT data and for helpful discussions, and
to Bill Keel (U. of Alabama) and Marco Chiaberge (STScI) for working
with us on the Hubble images. We have made use of data from the
NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA.
NR 90
TC 9
Z9 9
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2011
VL 195
IS 2
AR 19
DI 10.1088/0067-0049/195/2/19
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RP
UT WOS:000294773000008
ER
PT J
AU Radburn-Smith, DJ
de Jong, RS
Seth, AC
Bailin, J
Bell, EF
Brown, TM
Bullock, JS
Courteau, S
Dalcanton, JJ
Ferguson, HC
Goudfrooij, P
Holfeltz, S
Holwerda, BW
Purcell, C
Sick, J
Streich, D
Vlajic, M
Zucker, DB
AF Radburn-Smith, D. J.
de Jong, R. S.
Seth, A. C.
Bailin, J.
Bell, E. F.
Brown, T. M.
Bullock, J. S.
Courteau, S.
Dalcanton, J. J.
Ferguson, H. C.
Goudfrooij, P.
Holfeltz, S.
Holwerda, B. W.
Purcell, C.
Sick, J.
Streich, D.
Vlajic, M.
Zucker, D. B.
TI THE GHOSTS SURVEY. I. HUBBLE SPACE TELESCOPE ADVANCED CAMERA FOR SURVEYS
DATA
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE galaxies: distances and redshifts; galaxies: formation; galaxies: halos;
galaxies: spiral; galaxies: stellar content; galaxies: structure;
techniques: photometric
ID RED GIANT BRANCH; DIGITAL SKY SURVEY; DARK-MATTER SUBSTRUCTURE; TRACING
GALAXY FORMATION; MILKY-WAY SATELLITES; ON SPIRAL GALAXIES; STELLAR
HALO; GLOBULAR-CLUSTER; LUMINOSITY FUNCTION; DISTANCE INDICATOR
AB We present an overview of the GHOSTS survey, the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS). In the first paper of this series, we describe the sample, explore the benefits of using resolved stellar populations, and discuss our ACS F606W and F814W photometry. We use artificial star tests to assess completeness and use overlapping regions to estimate photometric uncertainties. The median depth of the survey at 50% completeness is 2.7 mag below the tip of the red giant branch (TRGB). We comprehensively explore and parameterize contamination from unresolved background galaxies and foreground stars using archival fields of high-redshift ACS observations. Left uncorrected, these would account for 10(0.65xF814W-19.0) detections per mag per arcsec(2). We therefore identify several selection criteria that typically remove 95% of the contaminants. Even with these culls, background galaxies are a significant limitation to the surface brightness detection limit which, for this survey, is typically V similar to 30 mag arcsec(-2). The resulting photometric catalogs are publicly available and contain some 3.1 million stars across 76 ACS fields, predominantly of low extinction. The uniform magnitudes of TRGB stars in these fields enable galaxy distance estimates with 2%-7% accuracy.
C1 [Radburn-Smith, D. J.; Dalcanton, J. J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[de Jong, R. S.; Streich, D.; Vlajic, M.] Leibniz Inst Astrophys Potsdam, D-14482 Potsdam, Germany.
[Seth, A. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bailin, J.; Bell, E. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Brown, T. M.; Ferguson, H. C.; Goudfrooij, P.; Holfeltz, S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Bullock, J. S.] Univ Calif Irvine, Ctr Cosmol, Dept Phys & Astron, Irvine, CA 92697 USA.
[Courteau, S.; Sick, J.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada.
[Holwerda, B. W.] European Space Agcy, Estec, NL-2200 AG Noordwijk, Netherlands.
[Purcell, C.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA.
[Zucker, D. B.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Zucker, D. B.] Australian Astron Observ, Coonabarabran, NSW 1710, Australia.
RP Radburn-Smith, DJ (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA.
RI Bullock, James/K-1928-2015;
OI Bullock, James/0000-0003-4298-5082; Brown, Thomas/0000-0002-1793-9968;
Holwerda, Benne/0000-0002-4884-6756; Bell, Eric/0000-0002-5564-9873
FU NASA [9765, 10523, 10889, NAS5-26555]; Space Telescope Science
Institute; NASA Office of Space Science [NNX09AF08G]; Natural Sciences
and Engineering Research Council of Canada
FX Support for Proposal numbers 9765, 10523, and 10889 was 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. Additionally, some of the
data presented in this paper were obtained from the Multimission Archive
at the Space Telescope Science Institute (MAST). Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX09AF08G and by other grants and contracts. 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. We
acknowledge the usage of the HyperLeda database
(http://leda.univ-lyon1.fr). This research has also made use of NASA's
Astrophysics Data System Bibliographic Services. S.C. acknowledges the
support of a Discovery Grant from the Natural Sciences and Engineering
Research Council of Canada.
NR 103
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD AUG
PY 2011
VL 195
IS 2
AR 18
DI 10.1088/0067-0049/195/2/18
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 818RP
UT WOS:000294773000007
ER
PT J
AU Agnihotri, R
Dutta, K
Soon, W
AF Agnihotri, Rajesh
Dutta, Koushik
Soon, Willie
TI Temporal derivative of Total Solar Irradiance and anomalous Indian
summer monsoon: An empirical evidence for a Sun-climate connection
SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS
LA English
DT Article
DE Total Solar Irradiance (TSI); Tropical precipitation; Indian monsoon;
Temporal derivative of TSI
ID NORTH-ATLANTIC CLIMATE; LAST MILLENNIUM; SURFACE-TEMPERATURE;
MAGNETIC-FIELD; ASIAN MONSOON; TIME-SERIES; COSMIC-RAYS; VARIABILITY;
RAINFALL; HOLOCENE
AB Identifying the pattern of natural climate variability is of immense importance to delineate the effects of anthropogenic climate changes. Global and regional climates are suspected to vary, in unison or with delays, with the Total Solar Irradiance (TSI) at decadal to centennial timescales. Here we show that the Indian summer monsoon rainfall correlates well with the temporal derivative of TSI on multi-decadal timescales. This linkage between the temporal derivative of TSI and the Indian summer monsoon is tested and corroborated both for the instrumental period (1871-2006) and for the last similar to 300 years using a speleothem delta O-18 record representing rainfall in southwestern India. Our analyses indicate that anomalous dry periods of the Indian monsoon are mostly coincident with negative TSI derivative. This study thus demonstrates the potential of 'TSI derivative' as an important indicator of natural monsoon variability on an interdecadal timescale. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Dutta, Koushik] Univ Minnesota, Large Lakes Observ, Duluth, MN 55812 USA.
[Agnihotri, Rajesh] CSIR, Radio & Atmospher Sci Div, Natl Phys Lab, New Delhi 110012, India.
[Agnihotri, Rajesh] Natl Inst Oceanog, Council Sci & Ind Res, Panaji 403004, Goa, India.
[Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dutta, K (reprint author), Univ Minnesota, Large Lakes Observ, 2205 E 5th St, Duluth, MN 55812 USA.
EM rajagni9@gmail.com; kdutta@d.umn.edu; wsoon@cfa.harvard.edu
FU National Physical Laboratory, New Delhi; National Institute of
Oceanography, Goa (components of Council of Scientific and Industrial
Research, Govt. of India)
FX RA thanks Directors of the National Physical Laboratory, New Delhi and
the National Institute of Oceanography, Goa (components of Council of
Scientific and Industrial Research, Govt. of India) for the facilities
provided and the financial support. We thank Professor Robert M. Carter
for help in editing the manuscript. We also thank M.G. Yadava (Physical
Research Laboratory, Ahmedabad, India) for sharing his published 6180
data of Akalagavi speleothem, and N.A. Krivova (Max Planck Institute for
Solar System Research, Katlenburg-Lindau, Germany) for sharing the
reconstructed TSI data. We are also grateful to two anonymous referees
for sharing their insights and knowledge on the subject of solar
variability and its potential connections to climate change.
NR 86
TC 10
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U1 0
U2 9
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1364-6826
J9 J ATMOS SOL-TERR PHY
JI J. Atmos. Sol.-Terr. Phys.
PD AUG
PY 2011
VL 73
IS 13
BP 1980
EP 1987
DI 10.1016/j.jastp.2011.06.006
PG 8
WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences
GA 816IL
UT WOS:000294591800042
ER
PT J
AU Ikarashi, S
Kohno, K
Aguirre, JE
Aretxaga, I
Arumugam, V
Austermann, JE
Bock, JJ
Bradford, CM
Cirasuolo, M
Earle, L
Ezawa, H
Furusawa, H
Furusawa, J
Glenn, J
Hatsukade, B
Hughes, DH
Iono, D
Ivison, RJ
Johnson, S
Kamenetzky, J
Kawabe, R
Lupu, R
Maloney, P
Matsuhara, H
Mauskopf, PD
Motohara, K
Murphy, EJ
Nakajima, K
Nakanishi, K
Naylor, BJ
Nguyen, HT
Perera, TA
Scott, KS
Shimasaku, K
Takagi, T
Takata, T
Tamura, Y
Tanaka, K
Tsukagoshi, T
Wilner, DJ
Wilson, GW
Yun, MS
Zmuidzinas, J
AF Ikarashi, S.
Kohno, K.
Aguirre, J. E.
Aretxaga, I.
Arumugam, V.
Austermann, J. E.
Bock, J. J.
Bradford, C. M.
Cirasuolo, M.
Earle, L.
Ezawa, H.
Furusawa, H.
Furusawa, J.
Glenn, J.
Hatsukade, B.
Hughes, D. H.
Iono, D.
Ivison, R. J.
Johnson, S.
Kamenetzky, J.
Kawabe, R.
Lupu, R.
Maloney, P.
Matsuhara, H.
Mauskopf, P. D.
Motohara, K.
Murphy, E. J.
Nakajima, K.
Nakanishi, K.
Naylor, B. J.
Nguyen, H. T.
Perera, T. A.
Scott, K. S.
Shimasaku, K.
Takagi, T.
Takata, T.
Tamura, Y.
Tanaka, K.
Tsukagoshi, T.
Wilner, D. J.
Wilson, G. W.
Yun, M. S.
Zmuidzinas, J.
TI Detection of an ultrabright submillimetre galaxy in the
Subaru/XMM-Newton Deep Field using AzTEC/ASTE
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: high-redshift; galaxies: ISM; galaxies: starburst;
submillimetre: galaxies
ID DEGREE EXTRAGALACTIC SURVEY; CLERK-MAXWELL-TELESCOPE; 1200-MU-M MAMBO
SURVEY; STAR-FORMATION HISTORY; HIGH-REDSHIFT GALAXIES; GOODS-N FIELD;
NUMBER COUNTS; MOLECULAR GAS; PHOTOMETRIC REDSHIFTS; SOURCE CATALOG
AB We report on the detection of an extremely bright (similar to 37 mJy at 1100 mu m and similar to 91 mJy at 880 mu m) submillimetre galaxy (SMG), AzTEC-ASTE-SXDF1100.001 (hereafter referred to as SXDF1100.001 or Orochi), discovered in the 1100 mu m observations of the Subaru/XMM-Newton Deep Field using AzTEC on ASTE. Subsequent CARMA 1300-mu m and SMA 880-mu m observations successfully pinpoint the location of Orochi and suggest that it has two components, one extended [full width at half-maximum (FWHM) of similar to 4 arcsec] and one compact (unresolved). Z-Spec on CSO has also been used to obtain a wide-band spectrum from 190 to 308 GHz, although no significant emission/absorption lines were found. The derived upper limit to the line-to-continuum flux ratio is 0.1-0.3 (2 sigma) across the Z-Spec band.
Based on the analysis of the derived spectral energy distribution from optical to radio wavelengths of possible counterparts near the SMA/CARMA peak position, we suggest that Orochi is a lensed, optically dark SMG lying at z similar to 3.4 behind a foreground, optically visible (but red) galaxy at z similar to 1.4. The deduced apparent (i.e., no correction for magnification) infrared luminosity (L-IR) and star formation rate (SFR) are 6 x 10(13) L-circle dot and 11 000 M-circle dot yr(-1), respectively, assuming that the L-IR is dominated by star formation. These values suggest that Orochi will consume its gas reservoir within a short time-scale (3 x 10(7) yr), which is indeed comparable to those in extreme starbursts like the centres of local ultraluminous infrared galaxies (ULIRGs).
C1 [Kohno, K.; Shimasaku, K.] Univ Tokyo, Sch Sci, Research Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan.
[Aguirre, J. E.; Lupu, R.; Scott, K. S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Aretxaga, I.; Hughes, D. H.] INAOE, Puebla 72000, Pue, Mexico.
[Arumugam, V.; Cirasuolo, M.; Ivison, R. J.; Matsuhara, H.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Austermann, J. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Ikarashi, S.; Kohno, K.; Motohara, K.; Tsukagoshi, T.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan.
[Bock, J. J.; Bradford, C. M.; Naylor, B. J.; Nguyen, H. T.; Zmuidzinas, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Bock, J. J.; Bradford, C. M.; Murphy, E. J.; Zmuidzinas, J.] CALTECH, Pasadena, CA 91125 USA.
[Cirasuolo, M.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Earle, L.; Glenn, J.; Kamenetzky, J.; Maloney, P.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Ezawa, H.; Nakanishi, K.] Natl Astron Observ, ALMA Project Off, Mitaka, Tokyo 1818588, Japan.
[Furusawa, H.; Furusawa, J.; Takata, T.] Natl Astron Observ, Astron Data Ctr, Mitaka, Tokyo 1818588, Japan.
[Hatsukade, B.; Iono, D.; Kawabe, R.; Tamura, Y.] Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan.
[Johnson, S.; Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Takagi, T.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan.
[Mauskopf, P. D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Nakajima, K.; Shimasaku, K.] Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
[Perera, T. A.] Illinois Wesleyan Univ, Bloomington, IL 61701 USA.
[Tanaka, K.] Keio Univ, Fac Sci & Technol, Dept Phys, Kohoku Ku, Yokohama, Kanagawa 2238522, Japan.
[Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ikarashi, S (reprint author), Univ Tokyo, Inst Astron, 2-21-1 Osawa, Tokyo 1810015, Japan.
EM ikarashi@ioa.s.u-tokyo.ac.jp
RI MOTOHARA, KENTARO/G-4905-2014; Lupu, Roxana/P-9060-2014; Ivison,
R./G-4450-2011
OI MOTOHARA, KENTARO/0000-0002-0724-9146; Lupu, Roxana/0000-0003-3444-5908;
Ivison, R./0000-0001-5118-1313
FU MEXT; Smithsonian Institution; Academia Sinica; National Science
Foundation; CARMA partner universities
FX We would like to thank everyone who helped staff and support the
AzTEC/ASTE 2008 operations and data calibration, including N. Ukita, M.
Tashiro, M. Uehara, S. Doyle, P. Horner, J. Cortes, J. Karakla, and G.
Wallace. The ASTE project is driven by the Nobeyama Radio Observatory
(NRO), a branch of the National Astronomical Observatory of Japan
(NAOJ), in collaboration with the University of Chile and Japanese
institutions including the University of Tokyo, Nagoya University, Osaka
Prefecture University, Ibaraki University and Hokkaido University.
Partial observations with ASTE were carried out remotely from Japan
using NTT's GEMnet2 and its partner R&E networks, which are based on the
AccessNova collaboration of the University of Chile, NTT Laboratories
and the NAOJ. This study was supported in part by the MEXT Grant-in-Aid
for Specially Promoted Research (No. 20001003). 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. Support
for CARMA construction was derived from the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S.
McDonnell Foundation, the Associates of the California Institute of
Technology, the University of Chicago, the states of California,
Illinois, and Maryland, and the National Science Foundation. The ongoing
CARMA development and operations are supported by the National Science
Foundation under a cooperative agreement, and by the CARMA partner
universities.
NR 107
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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 AUG
PY 2011
VL 415
IS 4
BP 3081
EP 3096
DI 10.1111/j.1365-2966.2011.18918.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811JK
UT WOS:000294204900010
ER
PT J
AU Foster, C
Spitler, LR
Romanowsky, AJ
Forbes, DA
Pota, V
Bekki, K
Strader, J
Proctor, RN
Arnold, JA
Brodie, JP
AF Foster, Caroline
Spitler, Lee R.
Romanowsky, Aaron J.
Forbes, Duncan A.
Pota, Vincenzo
Bekki, Kenji
Strader, Jay
Proctor, Robert N.
Arnold, Jacob A.
Brodie, Jean P.
TI Global properties of 'ordinary' early-type galaxies: photometry and
spectroscopy of stars and globular clusters in NGC 4494
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: abundances; galaxies: haloes; galaxies: individual: NGC 4494;
galaxies: kinematics and dynamics; galaxies: star clusters: general
ID COMPACT DWARF GALAXIES; HUBBLE-SPACE-TELESCOPE; SIGHT VELOCITY
DISTRIBUTIONS; STELLAR POPULATION SYNTHESIS; INFRARED CALCIUM TRIPLET;
SUPERMASSIVE BLACK-HOLES; DARK-MATTER; ELLIPTIC GALAXIES; SAURON
PROJECT; FORNAX CLUSTER
AB We present a comprehensive analysis of the spatial, kinematic and chemical properties of stars and globular clusters (GCs) in the 'ordinary' elliptical galaxy NGC 4494 using data from the Keck and Subaru telescopes. We derive galaxy surface brightness and colour profiles out to large galactocentric radii. We compare the latter to metallicities derived using the near-infrared Calcium Triplet. We obtain stellar kinematics out to similar to 3.5 effective radii. The latter appear flattened or elongated beyond similar to 1.8 effective radii in contrast to the relatively round photometric isophotes. In fact, NGC 4494 may be a flattened galaxy, possibly even an S0, seen at an inclination of similar to 45 degrees. We publish a catalogue of 431 GC candidates brighter than i(0) = 24 based on the photometry, of which 109 are confirmed spectroscopically and 54 have measured spectroscopic metallicities. We also report the discovery of three spectroscopically confirmed ultra-compact dwarfs around NGC 4494 with measured metallicities of -0.4 less than or similar to [Fe/H] less than or similar to -0.3. Based on their properties, we conclude that they are simply bright GCs. The metal-poor GCs are found to be rotating with similar amplitude as the galaxy stars, while the metal-rich GCs show marginal rotation. We supplement our analysis with available literature data and results. Using model predictions of galaxy formation, and a suite of merger simulations, we find that many of the observational properties of NGC 4494 may be explained by formation in a relatively recent gas-rich major merger. Complete studies of individual galaxies incorporating a range of observational avenues and methods such as the one presented here will be an invaluable tool for constraining the fine details of galaxy formation models, especially at large galactocentric radii.
C1 [Foster, Caroline; Spitler, Lee R.; Forbes, Duncan A.; Pota, Vincenzo] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Romanowsky, Aaron J.; Arnold, Jacob A.; Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Bekki, Kenji] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
[Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Proctor, Robert N.] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo, Brazil.
RP Foster, C (reprint author), Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
EM cfoster@astro.swin.edu.au
RI Spitler, Lee/A-9867-2013; Bekki, Kenji/H-8821-2014;
OI Spitler, Lee/0000-0001-5185-9876; Foster, Caroline/0000-0003-0247-1204
FU Anglo-Australian Observatory; ARC; NSF [AST-0808099, AST-0909237,
AST-0071048]; W.M. Keck Foundation; National Aeronautics and Space
Administration
FX We would like to thank the anonymous referee for his/her careful reading
of our manuscript and helpful comments. Soeren Larsen is acknowledged
for providing us with the HST/WFPC2 GC catalogue. We thank Michele
Cappellari and Loren Hoffman for helpful discussions. CF thanks the
Anglo-Australian Observatory for financial support in the form of a
graduate top-up scholarship. DAF thanks the ARC for financial support.
JPB and AJR acknowledge support from NSF grant AST-0808099 and
AST-0909237. Based in part on data collected at Subaru Telescope and
obtained from the SMOKA, which is operated by the Astronomy Data Center,
National Astronomical Observatory of Japan. Part of the Subaru data
analysed was obtained through a Gemini time exchange, program
GN-2008A-C-12. 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. We acknowledge the
usage of the HyperLeda data base (http://leda.univ-lyon1.fr) and of NED,
which is operated by the Jet Propulsion Laboratory, California Institute
of Technology, under contract with the National Aeronautics and Space
Administration. 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 124
TC 52
Z9 52
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG
PY 2011
VL 415
IS 4
BP 3393
EP 3416
DI 10.1111/j.1365-2966.2011.18965.x
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811JK
UT WOS:000294204900038
ER
PT J
AU Valtchanov, I
Virdee, J
Ivison, RJ
Swinyard, B
van der Werf, P
Rigopoulou, D
da Cunha, E
Lupu, R
Benford, DJ
Riechers, D
Smail, I
Jarvis, M
Pearson, C
Gomez, H
Hopwood, R
Altieri, B
Birkinshaw, M
Coia, D
Conversi, L
Cooray, A
De Zotti, G
Dunne, L
Frayer, D
Leeuw, L
Marston, A
Negrello, M
Portal, MS
Scott, D
Thompson, MA
Vaccari, M
Baes, M
Clements, D
Michalowski, MJ
Dannerbauer, H
Serjeant, S
Auld, R
Buttiglione, S
Cava, A
Dariush, A
Dye, S
Eales, S
Fritz, J
Ibar, E
Maddox, S
Pascale, E
Pohlen, M
Rigby, E
Rodighiero, G
Smith, DJB
Temi, P
Carpenter, J
Bolatto, A
Gurwell, M
Vieira, JD
AF Valtchanov, I.
Virdee, J.
Ivison, R. J.
Swinyard, B.
van der Werf, P.
Rigopoulou, D.
da Cunha, E.
Lupu, R.
Benford, D. J.
Riechers, D.
Smail, Ian
Jarvis, M.
Pearson, C.
Gomez, H.
Hopwood, R.
Altieri, B.
Birkinshaw, M.
Coia, D.
Conversi, L.
Cooray, A.
De Zotti, G.
Dunne, L.
Frayer, D.
Leeuw, L.
Marston, A.
Negrello, M.
Portal, M. Sanchez
Scott, D.
Thompson, M. A.
Vaccari, M.
Baes, M.
Clements, D.
Michalowski, M. J.
Dannerbauer, H.
Serjeant, S.
Auld, R.
Buttiglione, S.
Cava, A.
Dariush, A.
Dye, S.
Eales, S.
Fritz, J.
Ibar, E.
Maddox, S.
Pascale, E.
Pohlen, M.
Rigby, E.
Rodighiero, G.
Smith, D. J. B.
Temi, P.
Carpenter, J.
Bolatto, A.
Gurwell, M.
Vieira, J. D.
TI Physical conditions of the interstellar medium of high-redshift,
strongly lensed submillimetre galaxies from the Herschel-ATLAS
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: evolution; galaxies: individual: SDP.81: H-ATLAS
J090311.6+003906; galaxies: individual: SDP.130: H-ATLAS
J091305.0-005343; infrared: galaxies; radio continuum: galaxies;
submillimetre: ISM
ID FAR-INFRARED/RADIO CORRELATION; C-II LINE; STAR-FORMATION; MU-M;
PHOTODISSOCIATION REGIONS; EXTRAGALACTIC SOURCES; PHOTOMETRIC REDSHIFTS;
SPIRE INSTRUMENT; EARLY UNIVERSE; MOLECULAR GAS
AB We present Herschel-Spectral and Photometric Imaging Receiver (SPIRE) Fourier transform spectrometer (FTS) and radio follow-up observations of two Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS)-detected strongly lensed distant galaxies. In one of the targeted galaxies H-ATLAS J090311.6+003906 (SDP. 81), we detect [O III] 88 mu m and [C II] 158 mu m lines at a signal-to-noise ratio of similar to 5. We do not have any positive line identification in the other fainter target H-ATLAS J091305.0-005343 (SDP. 130). Currently, SDP. 81 is the faintest submillimetre galaxy with positive line detections with the FTS, with continuum flux just below 200 mJy in the 200-600 mu m wavelength range. The derived redshift of SDP. 81 from the two detections is z = 3.043 +/- 0.012, in agreement with ground-based CO measurements. This is the first detection by Herschel of the [O III] 88 mu m line in a galaxy at redshift higher than 0.05. Comparing the observed lines and line ratios with a grid of photodissociation region (PDR) models with different physical conditions, we derive the PDR cloud density n approximate to 2000 cm(-3) and the far-ultraviolet ionizing radiation field G(0) approximate to 200 (in units of the Habing field - the local Galactic interstellar radiation field of 1.6 x 10(-6) W m(-2)). Using the CO-derived molecular mass and the PDR properties, we estimate the effective radius of the emitting region to be 500-700 pc. These characteristics are typical for star-forming, high-redshift galaxies. The radio observations indicate that SDP. 81 deviates significantly from the local far-infrared/radio (FIR/radio) correlation, which hints that some fraction of the radio emission is coming from an active galactic nucleus (AGN). The constraints on the source size from millimetre-wave observations put a very conservative upper limit of the possible AGN contribution to less than 33 per cent. These indications, together with the high [OIII]/FIR ratio and the upper limit of [O I] 63 mu m/[C II] 158 mu m, suggest that some fraction of the ionizing radiation is likely to originate from the AGN.
C1 [Valtchanov, I.; Altieri, B.; Coia, D.; Conversi, L.; Marston, A.; Portal, M. Sanchez] ESA, European Space Astron Ctr, Herschel Sci Ctr, Villanueva De La Canada 28691, Spain.
[Virdee, J.; Swinyard, B.; Rigopoulou, D.; Pearson, C.] STFC Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England.
[Virdee, J.; Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England.
[Ivison, R. J.; Ibar, E.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Ivison, R. J.; van der Werf, P.; Michalowski, M. J.] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Swinyard, B.] UCL, Dept Phys & Astron, London WC1E 6BT, England.
[van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[da Cunha, E.] Univ Crete, Dept Phys, Iraklion 71003, Greece.
[da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Lupu, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Benford, D. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab Code 665, Greenbelt, MD 20771 USA.
[Riechers, D.; Carpenter, J.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Smail, Ian] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England.
[Jarvis, M.] Univ Hertfordshire, Sci & Technol Res Ctr, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Gomez, H.; Auld, R.; Dariush, A.; Dye, S.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales.
[Hopwood, R.; Clements, D.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England.
[Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England.
[Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA.
[De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy.
[De Zotti, G.] Scuola Int Super Studi Avanzati, I-34136 Trieste, Italy.
[Dunne, L.; Thompson, M. A.; Maddox, S.; Rigby, E.; Smith, D. J. B.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England.
[Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA.
[Leeuw, L.] Univ Johannesburg, Dept Phys, ZA-2006 Auckland Pk, South Africa.
[Leeuw, L.] SETI Inst, Mountain View, CA 94043 USA.
[Negrello, M.; Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England.
[Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Vaccari, M.; Buttiglione, S.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy.
[Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium.
[Dannerbauer, H.] CEA Saclay, DAPNIA Serv Astrophys, F-91191 Gif Sur Yvette, France.
[Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain.
[Dariush, A.] Inst Res Fundamental Sci IPM, Sch Astron, Tehran, Iran.
[Temi, P.] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA.
[Bolatto, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Valtchanov, I (reprint author), ESA, European Space Astron Ctr, Herschel Sci Ctr, Villanueva De La Canada 28691, Spain.
EM ivaltchanov@sciops.esa.int
RI Benford, Dominic/D-4760-2012; Gomez, Haley/C-2800-2009; Baes,
Maarten/I-6985-2013; Smail, Ian/M-5161-2013; Lupu, Roxana/P-9060-2014;
Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava,
Antonio/C-5274-2017;
OI Dye, Simon/0000-0002-1318-8343; Smith, Daniel/0000-0001-9708-253X;
Rodighiero, Giulia/0000-0002-9415-2296; da Cunha,
Elisabete/0000-0001-9759-4797; Altieri, Bruno/0000-0003-3936-0284;
Benford, Dominic/0000-0002-9884-4206; Baes, Maarten/0000-0002-3930-2757;
Smail, Ian/0000-0003-3037-257X; Lupu, Roxana/0000-0003-3444-5908;
Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577;
Cava, Antonio/0000-0002-4821-1275; Maddox, Stephen/0000-0001-5549-195X;
Scott, Douglas/0000-0002-6878-9840
FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany);
ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA,
CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC
(UK); NASA (USA)
FX The Herschel-ATLAS is a project with Herschel, which is an ESA space
observatory with science instruments provided by Europeanled Principal
Investigator consortia and with important participation from NASA. The
H-ATLAS website is http://www.h-atlas.org/. PACS has been developed by a
consortium of institutes led by MPE (Germany) and including UVIE
(Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA
(Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This
development has been supported by the funding agencies BMVIT (Austria),
ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF
(Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a
consortium of institutes led by Cardiff University (UK) and including
Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI,
University of Padua (Italy); IAC (Spain); Stockholm Observatory
(Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex
(UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has
been supported by national funding agencies: CSA (Canada); NAOC (China);
CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden);
STFC (UK); and NASA (USA).
NR 77
TC 41
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U1 0
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG
PY 2011
VL 415
IS 4
BP 3473
EP 3484
DI 10.1111/j.1365-2966.2011.18959.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811JK
UT WOS:000294204900045
ER
PT J
AU Ryde, F
Pe'er, A
Nymark, T
Axelsson, M
Moretti, E
Lundman, C
Battelino, M
Bissaldi, E
Chiang, J
Jackson, MS
Larsson, S
Longo, F
McGlynn, S
Omodei, N
AF Ryde, Felix
Pe'er, Asaf
Nymark, Tanja
Axelsson, Magnus
Moretti, Elena
Lundman, Christoffer
Battelino, Milan
Bissaldi, Elisabetta
Chiang, James
Jackson, Miranda S.
Larsson, Stefan
Longo, Francesco
McGlynn, Sinead
Omodei, Nicola
TI Observational evidence of dissipative photospheres in gamma-ray bursts
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms: thermal; gamma-ray burst: general
ID PROMPT EMISSION; THERMAL EMISSION; SYNCHROTRON SOURCES; SPECTRAL
COMPONENT; FERMI OBSERVATIONS; LORENTZ FACTOR; GRB SPECTRA; MODEL;
EVOLUTION; RADIATION
AB The emission from a gamma-ray burst (GRB) photosphere can give rise to a variety of spectral shapes. The spectrum can retain the shape of a Planck function or it can be broadened and have the shape of a Band function. This fact is best illustrated by studying GRB090902B. The main gamma-ray spectral component is initially close to a Planck function, which can only be explained by emission from the jet photosphere. Later, the same component evolves into a broader Band function. This burst thus provides observational evidence that the photosphere can give rise to a non-thermal spectrum. We show that such a broadening is most naturally explained by subphotospheric dissipation in the jet. The broadening mainly depends on the strength and location of the dissipation, the magnetic field strength and the relation between the energy densities of thermal photons and electrons. We suggest that the evolution in spectral shape observed in GRB090902B is due to a decrease in the bulk Lorentz factor of the flow, leading to the main dissipation becoming subphotospheric. Such a change in the flow parameters can also explain the correlation observed between the peak energy of the spectrum and low-energy power-law slope, a, a correlation commonly observed in GRBs. We conclude that photospheric emission could indeed be a ubiquitous feature during the prompt phase in GRBs and play a decisive role in creating the diverse spectral shapes and spectral evolutions that are observed.
C1 [Ryde, Felix; Nymark, Tanja; Axelsson, Magnus; Moretti, Elena; Lundman, Christoffer; Battelino, Milan; Jackson, Miranda S.; McGlynn, Sinead] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ryde, Felix; Nymark, Tanja; Axelsson, Magnus; Moretti, Elena; Lundman, Christoffer; Battelino, Milan; Jackson, Miranda S.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden.
[Pe'er, Asaf] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bissaldi, Elisabetta] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria.
[Bissaldi, Elisabetta] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria.
[Chiang, James; Omodei, Nicola] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Chiang, James; Omodei, Nicola] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA.
[Larsson, Stefan] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden.
[Longo, Francesco] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy.
[Longo, Francesco] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[McGlynn, Sinead] Tech Univ Munich, D-85748 Garching, Germany.
RP Ryde, F (reprint author), Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
EM fryde@kth.se
RI Bissaldi, Elisabetta/K-7911-2016;
OI Bissaldi, Elisabetta/0000-0001-9935-8106; Omodei,
Nicola/0000-0002-5448-7577; Axelsson, Magnus/0000-0003-4378-8785;
Moretti, Elena/0000-0001-5477-9097
FU Swedish National Space Board; Carl Tryggers Stiftelse for Vetenskaplig
Forskning; Swedish Research Council [2009-691]; Istituto Nazionale di
Astrofisica in Italy; Centre National d'Etudes Spatiales in France
FX We thank Peter Meszaros for useful comments on the manuscript. FR wishes
to express his gratitude to the Swedish National Space Board for
financial support. EM acknowledges with thanks financial support from
Carl Tryggers Stiftelse for Vetenskaplig Forskning and MA is supported
by the Swedish Research Council (grant 2009-691).; Additional support
for science analysis during the operations phase is gratefully
acknowledged from the Istituto Nazionale di Astrofisica in Italy and the
Centre National d'Etudes Spatiales in France.
NR 79
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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 AUG
PY 2011
VL 415
IS 4
BP 3693
EP 3705
DI 10.1111/j.1365-2966.2011.18985.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811JK
UT WOS:000294204900064
ER
PT J
AU Narayan, R
Fabian, AC
AF Narayan, Ramesh
Fabian, Andrew C.
TI Bondi flow from a slowly rotating hot atmosphere
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: clusters:
intracluster medium; galaxies: jets; galaxies: nuclei; X-rays: galaxies
ID ADVECTION-DOMINATED ACCRETION; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC
NUCLEI; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; SGR-A-ASTERISK;
SPHERICAL ACCRETION; ANGULAR-MOMENTUM; THERMAL CONDUCTION; ELLIPTIC
GALAXY; COOLING FLOW
AB A supermassive black hole in the nucleus of an elliptical galaxy at the centre of a cool-core group or cluster of galaxies is immersed in hot gas. Bondi accretion should occur at a rate determined by the properties of the gas at the Bondi radius and the mass of the black hole. X-ray observations of massive nearby elliptical galaxies, including M87 in the Virgo cluster, indicate a Bondi accretion rate. M-B which roughly matches the total kinetic power of the jets, suggesting that there is a tight coupling between the jet power and the mass accretion rate. While the Bondi model considers non-rotating gas, it is likely that the external gas has some angular momentum, which previous studies have shown could decrease the accretion rate drastically. We investigate here the possibility that viscosity acts at all radii to transport angular momentum outwards so that the accretion inflow proceeds rapidly and steadily. The situation corresponds to a giant advection-dominated accretion flow ( ADAF) which extends from beyond the Bondi radius down to the black hole. We find solutions of the ADAF equations in which the gas accretes at just a factor of a few less than. M-B. These solutions assume that the atmosphere beyond the Bondi radius rotates with a sub-Keplerian velocity and that the viscosity parameter is large, alpha >= 0.1, both of which are reasonable for the problem at hand. The infall time of the ADAF solutions is no more than a few times the free-fall time. Thus, the accretion rate at the black hole is closely coupled to the surrounding gas, enabling tight feedback to occur. We show that jet powers of a few per cent of. M(B)c(2) are expected if either a fraction of the accretion power is channelled into the jet or the black hole spin energy is tapped by a strong magnetic field pressed against the black hole by the pressure of the accretion flow. We discuss the Bernoulli parameter of the flow, the role of convection and the possibility that these as well as magnetohydrodynamic effects may invalidate the model. If the latter comes to pass, it would imply that the rough agreement between observed jet powers and the Bondi accretion rate is a coincidence and jet power is determined by factors other than the mass accretion rate.
C1 [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM rnarayan@cfa.harvard.edu; acf@ast.cam.ac.uk
OI Narayan, Ramesh/0000-0002-1919-2730
FU NSF [AST-1041590]; NASA [NNX11AE16G]; Royal Society
FX We thank the referee for a thoughtful review. RN thanks the Institute of
Astronomy, Cambridge, for hospitality while much of this work was
carried out. RN's research was supported in part by NSF grant
AST-1041590 and NASA grant NNX11AE16G. ACF thanks the Royal Society for
support.
NR 67
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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 AUG
PY 2011
VL 415
IS 4
BP 3721
EP 3730
DI 10.1111/j.1365-2966.2011.18987.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811JK
UT WOS:000294204900066
ER
PT J
AU Mathis, WN
Marinoni, L
AF Mathis, Wayne N.
Marinoni, Luciane
TI A review of Parydra (Diptera: Ephydridae) from Brazil
SO ZOOLOGIA
LA English
DT Review
DE Neotropical Region; shore flies; taxonomy
AB Species of the shore-fly Parydra Stenhammar, 1844 from Brazil are reviewed with an emphasis on the fauna from southern Brazil, where one new species, Parydra arcuata sp. nov. - state of Parana, municipality of Castro (8 km N, 24 degrees 45.3'S, 49 degrees 58.9'W)-, has been discovered and is herein described. To facilitate identification of species, we have included a diagnosis of the genus. We have also provided illustrations of structures of the male terminalia for all included species.
C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA.
[Marinoni, Luciane] Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil.
RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA.
EM mathisw@si.edu; lmarinoni@ufpr.br
RI Marinoni, Luciane /C-5720-2013
FU CNPq [401609/2009-0]
FX We gratefully acknowledge the assistance and cooperation of many
organizations and individuals who contributed to the field work and
production of this paper. The illustrations were expertly produced by
Mirian N. Morales, who is gratefully acknowledged and thanked. The
latter also expertly photographed and assembled the plate of heads and
the hindleg of P. arcuata sp. nov. (Figs 7-10) in addition to general
enhan-all plates. We also thank Philip J. Clausen for permission to use
his previously published illustrations of the other species known from
Brazil. For reviewing a draft of this paper we thank two anonymous
reviewers. Recent field work in Brazil (December 2009-June 2010) that
resulted in the vast majority of specimens studied in this paper was
supported by a grant from CNPq (Visiting Researcher/Process
401609/2009-0), which we gratefully acknowledge and thank. We thank
Dianne Mathis for helping with all aspects of the production of this
paper, especially the field work in Brazil. We also thank A. Bernardo
Carvalho and his lab (Elisa, Monica, Susana) for hosting us while
conducting field work along the coast of Sao Paulo. While making visits
to museums we were graciously hosted by David A. Grimaldi (AMNH), Jon
Gelhaus (ANSP), Marcia S. Couri (MNRJ), and Carlos J.E. Lamas (MZUSP).
We express cordial and grateful thanks for their time and many
gentilities.
NR 28
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PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA
PI CURITIBA
PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL
SN 1984-4670
J9 ZOOLOGIA-CURITIBA
JI Zoologia
PD AUG
PY 2011
VL 28
IS 4
BP 505
EP 512
DI 10.1590/S1984-46702011000400012
PG 8
WC Zoology
SC Zoology
GA 816BX
UT WOS:000294574800012
ER
PT J
AU Aguilar, R
Johnson, EG
Hines, AH
Roberts, PM
Goodison, MR
Kramer, MA
AF Aguilar, Robert
Johnson, Eric G.
Hines, Anson H.
Roberts, Paige M.
Goodison, Michael R.
Kramer, Margaret A.
TI SPATIAL DYNAMICS OF THE BLUE CRAB CALLINECTES SAPIDUS FISHERY IN
CHESAPEAKE BAY: UNDERSTANDING POST-MATURATION PROCESSES TO IMPROVE
EFFICACY OF MARINE STOCK ENHANCEMENT.
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Aguilar, Robert; Johnson, Eric G.; Hines, Anson H.; Roberts, Paige M.; Goodison, Michael R.; Kramer, Margaret A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 1
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 481
EP 481
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200032
ER
PT J
AU Breitburg, D
Hondorp, D
Audemard, C
Carnegie, R
Burrell, R
Clark, V
AF Breitburg, Denise
Hondorp, Darryl
Audemard, Corinne
Carnegie, Ryan
Burrell, Rebecca
Clark, Virginia
TI BREATHLESS NIGHTS: DIEL-CYCLING HYPOXIA AND THE PREVALENCE OF PERKINSUS
MARINUS (DERMO) INFECTIONS IN CHESAPEAKE BAY OYSTERS.
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Breitburg, Denise; Burrell, Rebecca; Clark, Virginia] Smithsonian Environm Res Ctr, Edgewater, MD 20678 USA.
[Hondorp, Darryl] USGS, Ann Arbor, MI 48105 USA.
[Audemard, Corinne; Carnegie, Ryan] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
NR 0
TC 0
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U1 0
U2 5
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 488
EP 488
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200055
ER
PT J
AU Clark, VM
Breitburg, DL
Burrell, RB
AF Clark, Virginia M.
Breitburg, Denise L.
Burrell, Rebecca B.
TI THE EFFECT OF DIEL-CYCLING HYPOXIA ON EASTERN OYSTER (CRASSOSTREA
VIRGINICA) CLEARANCE
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Clark, Virginia M.; Breitburg, Denise L.; Burrell, Rebecca B.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
NR 0
TC 0
Z9 0
U1 1
U2 6
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 496
EP 496
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200083
ER
PT J
AU Hines, AH
Johnson, EG
Aguilar, R
Kramer, M
Roberts, P
Soulen, H
Zohar, Y
Zmora, O
AF Hines, Anson H.
Johnson, Eric G.
Aguilar, Robert
Kramer, Margaret
Roberts, Paige
Soulen, Heather
Zohar, Yonathan
Zmora, Oded
TI FIELD ASSESSMENT OF THE FEASIBILITY OF ENHANCING THE CHESAPEAKE BLUE
CRAB STOCK
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Hines, Anson H.; Johnson, Eric G.; Aguilar, Robert; Kramer, Margaret; Roberts, Paige; Soulen, Heather] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Zohar, Yonathan; Zmora, Oded] Univ Maryland Baltimore Cty, Baltimore, MD 21202 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 4
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 516
EP 516
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200150
ER
PT J
AU Johnson, E
Hines, A
Soulen, H
Roberts, P
Kramer, M
Goodison, M
Aguilar, R
AF Johnson, Eric
Hines, Anson
Soulen, Heather
Roberts, Paige
Kramer, Margaret
Goodison, Michael
Aguilar, Robert
TI EVIDENCE FOR LARGE-SCALE RECRUITMENT LIMITATION OF BLUE CRABS IN UPPER
CHESAPEAKE BAY
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Johnson, Eric; Hines, Anson; Soulen, Heather; Roberts, Paige; Kramer, Margaret; Goodison, Michael; Aguilar, Robert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 2
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 518
EP 519
PG 2
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200160
ER
PT J
AU Kramer, M
Hines, AH
Johnson, EG
AF Kramer, Margaret
Hines, Anson H.
Johnson, Eric G.
TI ANNUAL, SEASONAL AND SIZE-DEPENDENT PATTERNS OF JUVENILE BLUE CRAB,
CALLINECTES SAPIDUS, MORTALITY IN UPPER CHESAPEAKE BAY
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Kramer, Margaret; Hines, Anson H.; Johnson, Eric G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 522
EP 523
PG 2
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200174
ER
PT J
AU Malek, JC
Breitburg, DL
AF Malek, Jennafer C.
Breitburg, Denise L.
TI THE EFFECTS OF DISEASE ON THE SPATIAL DISTRIBUTION OF THE EASTERN
OYSTER, CRASSOSTREA VIRGINICA, ALONG AN INTERTIDAL STRESS GRADIENT
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Malek, Jennafer C.; Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
NR 0
TC 0
Z9 0
U1 0
U2 2
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 529
EP 529
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200198
ER
PT J
AU Roberts, PM
Aguilar, R
Johnson, EG
Hines, AH
Goodison, MR
Kramer, MA
AF Roberts, Paige M.
Aguilar, Robert
Johnson, Eric G.
Hines, Anson H.
Goodison, Michael R.
Kramer, Margaret A.
TI POPULATION AND FISHERY DYNAMICS OF BLUE CRABS (CALLINECTES SAPIDUS) IN A
SUBESTUARY OF CHESAPEAKE BAY
SO JOURNAL OF SHELLFISH RESEARCH
LA English
DT Meeting Abstract
C1 [Roberts, Paige M.; Aguilar, Robert; Johnson, Eric G.; Hines, Anson H.; Goodison, Michael R.; Kramer, Margaret A.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
NR 0
TC 0
Z9 0
U1 0
U2 4
PU NATL SHELLFISHERIES ASSOC
PI GROTON
PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD,
GROTON, CT 06340 USA
SN 0730-8000
J9 J SHELLFISH RES
JI J. Shellfish Res.
PD AUG
PY 2011
VL 30
IS 2
BP 549
EP 549
PG 1
WC Fisheries; Marine & Freshwater Biology
SC Fisheries; Marine & Freshwater Biology
GA 812SC
UT WOS:000294312200263
ER
PT J
AU Montoya-Lerma, J
Solarte, YA
Giraldo-Calderon, GI
Quinones, ML
Ruiz-Lopez, F
Wilkerson, RC
Gonzalez, R
AF Montoya-Lerma, James
Solarte, Yezid A.
Isabel Giraldo-Calderon, Gloria
Quinones, Martha L.
Ruiz-Lopez, Freddy
Wilkerson, Richard C.
Gonzalez, Ranulfo
TI Malaria vector species in Colombia - A review
SO MEMORIAS DO INSTITUTO OSWALDO CRUZ
LA English
DT Article
DE Anopheles; Colombia; review
ID ANOPHELES-DARLINGI ROOT; AMPLIFIED POLYMORPHIC DNA; D-AND-K; INTERNAL
TRANSCRIBED SPACER; POLYMERASE-CHAIN-REACTION; DIPTERA-CULICIDAE;
NUNEZTOVARI DIPTERA; PLASMODIUM-VIVAX; SOUTH-AMERICA; PACIFIC COAST
AB Here we present a comprehensive review of the literature on the vectorial importance of the major Anopheles malaria vectors in Colombia. We provide basic information on the geographical distribution, altitudinal range, immature habitats, adult behaviour, feeding preferences and anthropophily, endophily and infectivity rates. We additionally review information on the life cycle, longevity and population fluctuation of Colombian Anopheles species. Emphasis was placed on the primary vectors that have been epidemiologically incriminated in malaria transmission: Anopheles darlingi, Anopheles albimanus and Anopheles nuneztovari. The role of a selection of local, regional or secondary vectors (e. g., Anopheles pseudopunctipennis and Anopheles neivai) is also discussed. We highlight the importance of combining biological, morphological and molecular data for the correct taxonomical determination of a given species, particularly for members of the species complexes. We likewise emphasise the importance of studying the bionomics of primary and secondary vectors along with an examination of the local conditions affecting the transmission of malaria. The presence and spread of the major vectors and the emergence of secondary species capable of transmitting human Plasmodia are of great interest. When selecting control measures, the anopheline diversity in the region must be considered. Variation in macroclimate conditions over a species' geographical range must be well understood and targeted to plan effective control measures based on the population dynamics of the local Anopheles species.
C1 [Montoya-Lerma, James; Isabel Giraldo-Calderon, Gloria; Gonzalez, Ranulfo] Univ Valle, Dept Biol, Cali, Colombia.
[Solarte, Yezid A.] Univ Valle, Inst Inmunol Valle, Cali, Colombia.
[Solarte, Yezid A.] Consorcio Invest Cient Caucaseco, Cali, Colombia.
[Quinones, Martha L.] Univ Nacl Colombia, Dept Publ Hlth, Fac Med, Bogota, Colombia.
[Ruiz-Lopez, Freddy; Wilkerson, Richard C.] Walter Reed Army Inst Res, Smithsonian Inst, Div Entomol, Museum Support Ctr, Suitland, MD USA.
RP Montoya-Lerma, J (reprint author), Univ Valle, Dept Biol, Cali, Colombia.
EM james.montoya@correounivalle.edu.co
RI Solarte, Yezid/C-1196-2013;
OI Solarte, Yezid/0000-0003-4173-0256; Montoya-Lerma,
James/0000-0003-2122-1323
FU NIAID/NIH [U19AI089702]
FX NIAID/NIH for the establishment of an ICEMR/CLAIM (U19AI089702)
NR 169
TC 35
Z9 37
U1 1
U2 11
PU FUNDACO OSWALDO CRUZ
PI RIO DE JANEIRO, RJ
PA AV BRASIL 4365, 21045-900 RIO DE JANEIRO, RJ, BRAZIL
SN 0074-0276
EI 1678-8060
J9 MEM I OSWALDO CRUZ
JI Mem. Inst. Oswaldo Cruz
PD AUG
PY 2011
VL 106
SU 1
BP 223
EP 238
PG 16
WC Parasitology; Tropical Medicine
SC Parasitology; Tropical Medicine
GA 814IA
UT WOS:000294440600028
PM 21881778
ER
PT J
AU O'Dea, A
Hakansson, E
Taylor, PD
Okamura, B
AF O'Dea, Aaron
Hakansson, Eckart
Taylor, Paul D.
Okamura, Beth
TI Environmental change prior to the K-T boundary inferred from temporal
variation in the morphology of cheilostome bryozoans
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE K-T boundary; Extinction; zs-MART; Bryozoa; Fluctuating asymmetry;
Environmental change
ID CRETACEOUS-TERTIARY BOUNDARY; ZOOID SIZE; STEVNS-KLINT; MAASTRICHTIAN
CHALK; MARINE BRYOZOAN; CUPULADRIID BRYOZOANS; PALEOGENE BOUNDARY; MASS
EXTINCTION; NORTH-SEA; FLUCTUATING ASYMMETRY
AB Fluctuations in the marine environment just prior to the K-T extinction event have been inferred from several geological sections around the world. Most previous studies have employed isotope or trace element proxies. This study uses morphological changes in erect and free-living cheilostome bryozoans as a proxy to investigate environmental change through the final stages of the Maastrichtian at the Nye Kiev section in Denmark. The metrics used are: (1) mean zooid size as a proxy for temperature; (2) intracolony variation in zooid size as a proxy for degree of seasonality; (3) density of defensive avicularia as a proxy for palaeoproductivity; and (4) colony size and asymmetry as proxies for unfavourable environmental conditions. Three semi-distinct phases in the benthic environment are evident: The lowest 3.5 m of the roughly 4.5 m section experienced apparently normal marine conditions. Next, low estimates of benthic seasonality, and highly symmetrical and large colonies with many avicularia indicate a time of increased environmental stability. Subsequent to this quiescence, the uppermost similar to 20 cm of the section witnessed environmental volatility and deterioration with mean zooid sizes in all species falling dramatically suggesting a rapid warming or dysoxic event, sharply increasing seasonality estimates implying unusual oceanographical states, and the growth of small, asymmetrical colonies with few avicularia all suggesting unfavourable conditions. These data therefore indicate that strong environmental perturbations occurred just prior to the K-T boundary in the Danish Basin. Such events may have contributed to biotic turnover at the K-T boundary because cause and effect in macroevolution can be delayed. However, potential mechanisms of turnover need to be robustly tested within a detailed palaeoenvironmental framework construct from a suite of independent proxies. (C) 2011 Elsevier B.V. All rights reserved.
C1 Smithsonian Trop Res Inst, Panama City, Panama.
[O'Dea, Aaron; Okamura, Beth] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England.
[Hakansson, Eckart] Univ Western Australia, Sch Earth & Environm, Crawley, WA 6009, Australia.
[Taylor, Paul D.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England.
RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM odeaa@si.edu
RI O'Dea, Aaron/D-4114-2011; Hakansson, Eckart/H-9331-2014
FU BBSRC; Sigma Xi; John Ray Trust; Bristol University Alumni Foundation
FX We thank Gail Lambourne, Mark Wilkinson, Mike Benton, Steve Hageman,
Nicholas Larsen, Peter Miller, Phil Basson, and Roger Hughes for
logistical help and discussion. Finn Surlyk, Erik Thomsen, Steve Hageman
and Kresten Anderskouv improved the manuscript with helpful comments.
Funding was provided through a BBSRC PhD studentship, a Sigma Xi grant,
a John Ray Trust Research Bursary, a Bristol University Alumni
Foundation Grant.
NR 115
TC 10
Z9 10
U1 2
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD AUG 1
PY 2011
VL 308
IS 3-4
BP 502
EP 512
DI 10.1016/j.palaeo.2011.06.001
PG 11
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 813UY
UT WOS:000294396900020
ER
PT J
AU Funk, VA
Roque, N
AF Funk, Vicki A.
Roque, Nadia
TI The monotypic Andean genus Fulcaldea (Compositae, Barnadesioideae) gains
a new species from northeastern Brazil
SO TAXON
LA English
DT Article
DE Arnaldoa; Asteraceae; Bahia; Barnadesieae; Chapada Diamantina;
Dasyphyllum; Mutisieae
ID ASTERACEAE; PHYLOGENY; SUBFAMILY; POLLEN
AB The family Compositae has ca. 25,000 species and is estimated to have diverged approximately 45 Ma. Within the Family, the small subfamily Barnadesioideae (91 spp.) is the sister group of the rest of Compositae. Four of its nine genera have only one species; one of these, Fulcaldea, is restricted to northern Peru and Ecuador as is its sister group, Arnaldoa (3 spp.). A new species, Fulcaldea stuessyi, is described from the Chapada Diamantina of Bahia, Brazil, a remarkable 4000 km disjunction. The new species is clearly a member of Fulcaldea sharing a number of important characters with the type, F laurifolia, including a single-flowered capitulum, "plumose" pappus, shrubby habit, and style with a unique swelling. It is distinguished from that species by its red corolla and pappus, greater number of series of phyllaries, and much greater length of the corolla, style, and pappus. The location of the new taxon may be the result of vicariance or long-distance dispersal; it is named in honor of Professor Tod Stuessy.
C1 [Funk, Vicki A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, US Natl Herbarium, Washington, DC 20560 USA.
[Roque, Nadia] Univ Fed Bahia, Inst Biol, Herbario Alexandre Leal Costa, BR-40170110 Salvador, BA, Brazil.
RP Funk, VA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, US Natl Herbarium, Washington, DC 20560 USA.
EM funkv@si.edu
RI Roque, Nadia/I-3157-2012
FU CNPq [PQ 307156/2010-9]; National Museum of Natural History, Smithsonian
Institution
FX We give special thanks to Ivan Abreu (Universidade Federal da Bahia) who
collected the type specimen and provided the photographs of Fulcaldea
stuessyi. Also, thanks to Michael Dillon (F) and Gwilym Lewis (K) who
supplied the photos of F. laurifolia. The authors are grateful to Alice
Tangerini (US) for the color illustrations; some of the parts were
helpfully sketched by Natanael Nascimento dos Santos from the holotype.
Thanks to Carol Kelloff for the rapid sequencing of the Fulcaldea
stuessyi DNA and the pollen photos, to Raymund Chan for help with
sequence data analysis, and to Mauricio Bonifacino for his help with the
maps. This work was supported by grants from CNPq (PQ 307156/2010-9),
and the National Museum of Natural History, Smithsonian Institution.
Finally, we thank Associate Editor Jun Wen and reviewers Michael Dillon
(F), Estrella Urtubey (SI), and D.J. Nicholas Hind (K) for their helpful
comments.
NR 22
TC 3
Z9 6
U1 0
U2 1
PU INT ASSOC PLANT TAXONOMY
PI VIENNA
PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA
SN 0040-0262
J9 TAXON
JI Taxon
PD AUG
PY 2011
VL 60
IS 4
BP 1095
EP 1103
PG 9
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 815DT
UT WOS:000294507000012
ER
PT J
AU Peterson, PM
Romaschenko, K
Barker, NP
Linder, HP
AF Peterson, Paul M.
Romaschenko, Konstantin
Barker, Nigel P.
Linder, H. Peter
TI Centropodieae and Ellisochloa, a new tribe and genus in Chloridoideae
(Poaceae)
SO TAXON
LA English
DT Article
DE C(3) and C(4) photosynthesis; Centropodia; Centropodieae; Chloridoideae;
classification; Danthonioideae; Ellisochloa; Merxmuellera; plastid DNA
sequences; phylogeny
ID MULTIGENE PHYLOGENETIC TREES; HAUSTORIAL SYNERGIDS; DANTHONIOID GRASSES;
C-4 PHOTOSYNTHESIS; SEQUENCE DATA; ERAGROSTIS-WALTERI; MATK SEQUENCES;
1ST RECORD; NEW-WORLD; CLASSIFICATION
AB There has been confusion among taxonomists regarding the subfamilial placement of Merxmuellera papposa, M. rangei, and four species of Centropodia even though many researchers have included them in molecular studies. We conducted a phylogenetic analysis of 127 species using seven plastid regions (rps3, rps16-trnK, rps16, rpl32-trnL, ndhF, ndhA, matK) to infer the evolutionary relationships of Centropodia, M. papposa, and M. rangei with other grasses. Merxmuellera papposa and M. rangei form a clade that is sister to three species of Centropodia, and together they are sister to the remaining tribes in Chloridoideae. We provide the carbon isotope ratios for four species indicating that Merxmuellera papposa and M. rangei are photosynthetically C(3), and Centropodia glauca and C. mossamdensis are C(4). We present evidence in favor of the expansion of subfamily Chloridoideae to include a new tribe, Centropodieae, which includes two genera, Centropodia and a new genus, Ellisochloa with two species, Ellisochloa papposa and E. rangei. The name Danthonia papposa Nees is lectotypified.
C1 [Peterson, Paul M.; Romaschenko, Konstantin] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
[Romaschenko, Konstantin] CSIC ICUB, Bot Inst Barcelona, Lab Mol Systemat, Barcelona 08038, Spain.
[Barker, Nigel P.] Rhodes Univ, Dept Bot, Mol Ecol & Systemat Grp, ZA-6140 Grahamstown, South Africa.
[Linder, H. Peter] Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland.
RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
EM peterson@si.edu
RI Linder, Hans Peter/F-5316-2010; Romaschenko, Konstantin/K-3096-2014
OI Romaschenko, Konstantin/0000-0002-7248-4193
FU National Geographic Society Committee for Research and Exploration
[8087-06]; Smithsonian Institution's, Restricted Endowments Fund;
Scholarly Studies Program; Research Opportunities; Atherton Seidell
Foundation; Biodiversity Surveys and Inventories Program; Small Grants
Program; Laboratory of Analytical Biology
FX We thank the National Geographic Society Committee for Research and
Exploration (Grant No. 8087-06) for field and laboratory support; the
Smithsonian Institution's, Restricted Endowments Fund, the Scholarly
Studies Program, Research Opportunities, Atherton Seidell Foundation,
Biodiversity Surveys and Inventories Program, Small Grants Program, and
the Laboratory of Analytical Biology, all for financial support. We
would also like to acknowledge Lee Weigt, Gabriel Johnson, Jeffery Hunt,
and David Erickson for help in the laboratory; Robert J. Soreng, Jeffery
M. Saarela, Carol R. Annable, and Nancy F. Refulio Rodriguez for
accompanying the first author on numerous field expeditions; Robert J.
Soreng for many extended discussions pertinent to the manuscript; Alain
Touwaide for help preparing the Latin diagnoses; HPL and NPB would like
to acknowledge the late Mr. Paseka Mafa, from whose M.Sc. thesis
(University of Cape Town) on the anatomical information on Merxmuellera
papposa was taken; and Lynn G. Clark and three anonymous reviewers for
providing helpful comments on the manuscript.
NR 56
TC 24
Z9 25
U1 1
U2 8
PU INT ASSOC PLANT TAXONOMY
PI VIENNA
PA C/O UNIV VIENNA, INST BOTANY, RENNWEG 14, A-1030 VIENNA, AUSTRIA
SN 0040-0262
J9 TAXON
JI Taxon
PD AUG
PY 2011
VL 60
IS 4
BP 1113
EP 1122
PG 10
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 815DT
UT WOS:000294507000014
ER
PT J
AU Shui, YM
Wen, J
Chen, WH
AF Shui, Yu-Min
Wen, Jun
Chen, Wen-Hong
TI Parashorea chinensis Wang Hsie and P. chinensis var. kwangsiensis Lin
Chi: Two exceptional cases of names with a corporate authorship
SO TAXON
LA English
DT Article
DE authorship; citation; nomenclature; Parashorea chinensis; Parashorea
chinensis var. kwangsiensis
AB Parashorea chinensis Wang Hsie and Parashorea chinensis var. kwangsiensis Lin Chi (Dipterocarpaceae) are economically and ecologically important tree taxa in China and Vietnam. Their authorship should be "Wang Hsie" and "Lin Chi", respectively, which represent two logograms of working groups that existed in the particular circumstances from the 1960s to the 1970s in China. The author of Parashorea chinensis has sometimes been designated inappropriately as H. Wang. We herein discuss in detail these two unique cases in the context of the International Code of Botanical Nomenclature.
C1 [Shui, Yu-Min; Wen, Jun; Chen, Wen-Hong] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650204, Yunnan Province, Peoples R China.
[Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, US Natl Herbarium, Washington, DC 20013 USA.
RP Wen, J (reprint author), Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, 132 Lanhei Rd, Kunming 650204, Yunnan Province, Peoples R China.
EM wenj@si.edu
FU National Geographic Society [NGS 8288-07]
FX We thank Prof. C.Y. Wu and Prof. H.W. Li in Kunming Institute of Botany,
Chinese Academy of Sciences (CAS), Prof. Y.K. Yang in Nanjing
Pharmaceutical University, Prof. D.M. Wang and Prof. Y.K. Sima in Yunnan
Forestry Academy for their helpful discussions, Ms. Z.D. Wei of Kunming
Institute of Botany, CAS, for collecting some references, two anonymous
reviewers for their constructive comments, and Dr. John McNeill for his
help and contributions to our manuscript. The paper was derived from
discussions during our expedition to Southeast Yunnan bordering Vietnam
sponsored by the National Geographic Society (grant number NGS 8288-07).
NR 18
TC 0
Z9 0
U1 1
U2 2
PU INT ASSOC PLANT TAXONOMY-IAPT
PI BRATISLAVA
PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23
BRATISLAVA, SLOVAKIA
SN 0040-0262
EI 1996-8175
J9 TAXON
JI Taxon
PD AUG
PY 2011
VL 60
IS 4
BP 1165
EP 1167
PG 3
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 815DT
UT WOS:000294507000018
ER
PT J
AU Cernusak, LA
Winter, K
Turner, BL
AF Cernusak, Lucas A.
Winter, Klaus
Turner, Benjamin L.
TI Transpiration modulates phosphorus acquisition in tropical tree
seedlings
SO TREE PHYSIOLOGY
LA English
DT Article
DE elevated CO(2); mass flow; phosphorus concentration; water-use
efficiency
ID WATER-USE EFFICIENCY; SOIL ORGANIC PHOSPHORUS; CARBON-ISOTOPE
DISCRIMINATION; MOENCH VOSS SEEDLINGS; WHOLE-PLANT WATER; N-P RATIOS;
NUTRIENT LIMITATION; FICUS-INSIPIDA; PIONEER TREE; ELEVATED CO2
AB Several experiments were conducted with tropical tree and liana seedlings in which transpiration ratio and leaf phosphorus to carbon ratio (P:C) were measured. Transpiration ratio was expressed as kg H(2)O transpired g(-1) C incorporated into plant biomass, and leaf P:C as mg P g(-1) C. Leaf P:C was positively correlated with transpiration ratio across 19 species for plants grown under similar conditions (R(2) = 0.35, P < 0.01, n = 19). For five species in the dataset, multiple treatments were imposed to cause intra-specific variation in transpiration ratio. Within four of these five species, leaf P:C correlated positively with transpiration ratio. The slope and strength of the correlation varied among species. In one experiment, whole-plant P:C was measured in addition to leaf P:C. Patterns of correlation between whole-plant P:C and transpiration ratio were similar to those between leaf P:C and transpiration ratio. Together, these observations suggest that transpiration can influence the rate of P uptake from soil in tropical tree and liana seedlings. We suggest that this occurs through transport of inorganic phosphate and organic P compounds to root surfaces by transpiration-induced mass flow of the soil solution. The positive correlation between leaf P:C and transpiration ratio suggests that leaf P:C could decline in tropical forests as atmospheric CO(2) concentration rises, due to decreasing transpiration ratios.
C1 [Cernusak, Lucas A.] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia.
[Winter, Klaus; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa 03092, Ancon, Panama.
RP Cernusak, LA (reprint author), Australian Natl Univ, Res Sch Biol, GPO Box 4, Canberra, ACT 0200, Australia.
EM lucas.cernusak@anu.edu.au
RI Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011
OI Turner, Benjamin/0000-0002-6585-0722; Cernusak,
Lucas/0000-0002-7575-5526
FU Smithsonian Tropical Research Institute; Australian Research Council
[DP0771427, FT100100329]
FX L.A.C. was supported by a Tupper Fellowship from the Smithsonian
Tropical Research Institute, by a Discovery Grant from the Australian
Research Council (DP0771427), and by a Future Fellowship from the
Australian Research Council (FT100100329).
NR 69
TC 22
Z9 22
U1 4
U2 34
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0829-318X
J9 TREE PHYSIOL
JI Tree Physiol.
PD AUG
PY 2011
VL 31
IS 8
BP 878
EP 885
DI 10.1093/treephys/tpr077
PG 8
WC Forestry
SC Forestry
GA 815VL
UT WOS:000294558000009
PM 21856654
ER
PT J
AU Beltran, MT
Cesaroni, R
Zhang, Q
Galvan-Madrid, R
Beuther, H
Fallscheer, C
Neri, R
Codella, C
AF Beltran, M. T.
Cesaroni, R.
Zhang, Q.
Galvan-Madrid, R.
Beuther, H.
Fallscheer, C.
Neri, R.
Codella, C.
TI Molecular outflows and hot molecular cores in G24.78+0.08 at
sub-arcsecond angular resolution
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM: individual objects: G24.78+0.08; ISM: molecules; ISM: jets and
outflows; stars: formation
ID MASSIVE STAR-FORMATION; YOUNG STELLAR OBJECTS; FORMATION REGIONS;
ROTATING TOROIDS; HII REGION; ACCRETION; VELOCITY; G10.6-0.4; CLUSTER;
MODEL
AB Context. This study is part of a large project to study the physics of accretion and molecular outflows towards a selected sample of high-mass star-forming regions that show evidence of infall and rotation from previous studies. Aims. We wish to make a thorough study at high-angular resolution of the structure and kinematics of the HMCs and corresponding molecular outflows in the high-mass star-forming region G24.78+0.08. Methods. We carried out SMA and IRAM PdBI observations at 1.3 and 1.4 mm, respectively, of dust and of typical high-density and molecular outflow tracers with resolutions of <1 ''. Complementary IRAM 30-m (CO)-C-12 and (CO)-C-13 observations were carried out to recover the short spacing information of the molecular outflows. Results. The millimeter continuum emission towards cores G24 A1 and A2 has been resolved into three and two cores, respectively, and named A1, A1b, A1c, A2, and A2b. All these cores are aligned in a southeast-northwest direction coincident with that of the molecular outflows detected in the region, which suggests a preferential direction for star formation in this region. The masses of the cores range from 7 to 22 M-circle dot, and the rotational temperatures from 128 to 180 K. The high-density tracers have revealed the existence of two velocity components towards A1. One of them peaks close to the position of the millimeter continuum peak and of the HC HII region and is associated with the velocity gradient seen in CH3CN towards this core, while the other one peaks southwest of core A1 and is not associated with any millimeter continuum emission peak. The position-velocity plots along outflow A and the (CO)-C-13 (2-1) averaged blueshifted and redshifted emission indicate that this outflow is driven by core A2. Core A1 apparently does not drive any outflow. The knotty appearance of the highly collimated outflow C and the (CO)-C-12 position-velocity plot suggest an episodic outflow, where the knots are made of swept-up ambient gas.
C1 [Beltran, M. T.; Cesaroni, R.; Codella, C.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Zhang, Q.; Galvan-Madrid, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Galvan-Madrid, R.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico.
[Galvan-Madrid, R.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Beuther, H.; Fallscheer, C.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Fallscheer, C.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada.
[Neri, R.] IRAM, F-38406 St Martin Dheres, France.
RP Beltran, MT (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM mbeltran@arcetri.astro.it
OI Beltran Sorolla, Maria Teresa/0000-0003-3315-5626; Cesaroni,
Riccardo/0000-0002-2430-5103; Codella, Claudio/0000-0003-1514-3074;
Zhang, Qizhou/0000-0003-2384-6589
NR 36
TC 14
Z9 14
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2011
VL 532
AR A91
DI 10.1051/0004-6361/201117200
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 799JS
UT WOS:000293283600102
ER
PT J
AU Singh, V
Shastri, P
Risaliti, G
AF Singh, V.
Shastri, P.
Risaliti, G.
TI X-ray spectral properties of Seyfert galaxies and the unification scheme
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: Seyfert; X-rays: galaxies; galaxies: active
ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; BRIGHT QUASAR SURVEY;
K-ALPHA-LINES; ASCA OBSERVATIONS; STARBURST CONNECTION; LOCAL UNIVERSE;
IMAGING SURVEY; UNIFIED MODEL; EMISSION-LINE
AB Context. The unification scheme of Seyfert galaxies predicts that the observed differences between types 1 and 2 Seyfert galaxies are solely due to the differing orientations of the toroidal-shaped obscuring material around AGN. The observed X-ray spectra of Seyfert type 2s compared to type 1s are expected to be affected by higher absorbing column density owing to the edge-on view of the obscuring torus.
Aims. We study the 0.5-10 keV X-ray spectral properties of Seyfert type 1s and type 2s with the aim of testing the predictions of Seyfert unification scheme in the X-ray regime.
Methods. We use an optically selected Seyfert sample in which type 1s and type 2s have matched distributions in parameters that are independent of the orientation of AGN and the host galaxy.
Results. The 0.5-10 keV XMM-Newton pn X-ray spectra of Seyfert galaxies are in general best fitted with a model that consists of (i) an absorbed powerlaw; (ii) a narrow Gaussian fitted to the Fe K alpha emission line; and (iii) an often seen soft-excess component characterized by either a thermal plasma model with temperature kT similar to 0.1-1.0 keV or a steep powerlaw or both. The 2.0-10 keV hard X-ray continuum emission in several Seyfert type 2s is dominated by reflection and suggests the Compton-thick obscuration. Results of the statistical comparison between the distributions of (i) the observed X-ray luminosities in the soft (0.5-2.0 keV) and hard (2.0-10.0 keV) bands; (ii) the X-ray absorbing column densities; (iii) the equivalent widths of Fe K alpha line; and (iv) the flux ratios of hard X-ray to [OIII] lambda 5007 angstrom, for the two Seyfert subtypes are consistent with the obscuration and orientation-based unification scheme.
C1 [Singh, V.; Shastri, P.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
[Singh, V.] Univ Calicut, Dept Phys, Calicut 673635, Kerala, India.
[Risaliti, G.] INAF Osservatorio Arcetri, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Singh, V (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
EM veeresh@iiap.res.in
OI Risaliti, Guido/0000-0002-3556-977X
FU ESA; USA (NASA)
FX This work is based on observations with XMM-Newton, an ESA science
mission with instruments and contributions directly funded by ESA Member
States and the USA (NASA). Also, this research 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. Authors thank the
anonymous referee for useful comments and suggestions for improving the
manuscript.
NR 100
TC 10
Z9 10
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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2011
VL 532
AR A84
DI 10.1051/0004-6361/201016387
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 799JS
UT WOS:000293283600095
ER
PT J
AU Wright, SJ
Yavitt, JB
Wurzburger, N
Turner, BL
Tanner, EVJ
Sayer, EJ
Santiago, LS
Kaspari, M
Hedin, LO
Harms, KE
Garcia, MN
Corre, MD
AF Wright, S. Joseph
Yavitt, Joseph B.
Wurzburger, Nina
Turner, Benjamin L.
Tanner, Edmund V. J.
Sayer, Emma J.
Santiago, Louis S.
Kaspari, Michael
Hedin, Lars O.
Harms, Kyle E.
Garcia, Milton N.
Corre, Marife D.
TI Potassium, phosphorus, or nitrogen limit root allocation, tree growth,
or litter production in a lowland tropical forest
SO ECOLOGY
LA English
DT Article
DE Barro Colorado Nature Monument, Panama; fertilization; fine litter; fine
roots; nitrogen; nutrient limitation; phosphorus; potassium; tree
growth; tropics
ID TERRESTRIAL ECOSYSTEMS; NUTRIENT LIMITATION; RAIN-FOREST; PANAMA;
DYNAMICS; BIOMASS; SOILS; MOIST; FERTILIZATION; DECOMPOSITION
AB We maintained a factorial nitrogen (N), phosphorus (P), and potassium (K) addition experiment for 11 years in a humid lowland forest growing on a relatively fertile soil in Panama to evaluate potential nutrient limitation of tree growth rates, fine-litter production, and fine-root biomass. We replicated the eight factorial treatments four times using 32 plots of 40x40 m each. The addition of K was associated with significant decreases in stand-level fine-root biomass and, in a companion study of seedlings, decreases in allocation to roots and increases in height growth rates. The addition of K and N together was associated with significant increases in growth rates of saplings and poles (1-10 cm in diameter at breast height) and a further marginally significant decrease in stand-level fine-root biomass. The addition of P was associated with a marginally significant (P = 0.058) increase in fine-litter production that was consistent across all litter fractions. Our experiment provides evidence that N, P, and K all limit forest plants growing on a relatively fertile soil in the lowland tropics, with the strongest evidence for limitation by K among seedlings, saplings, and poles.
C1 [Wright, S. Joseph; Wurzburger, Nina; Turner, Benjamin L.; Kaspari, Michael; Harms, Kyle E.; Garcia, Milton N.] Smithsonian Trop Res Inst, Balboa, Panama.
[Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA.
[Wurzburger, Nina; Hedin, Lars O.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08540 USA.
[Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England.
[Sayer, Emma J.] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England.
[Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA.
[Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA.
[Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Corre, Marife D.] Univ Gottingen, Busgen Inst, D-37077 Gottingen, Germany.
RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.
EM wrightj@si.edu
RI Turner, Benjamin/E-5940-2011; Sayer, Emma/B-2514-2010; Wright,
Stuart/M-3311-2013; Santiago, Louis/E-3185-2016
OI Turner, Benjamin/0000-0002-6585-0722; Sayer, Emma/0000-0002-3322-4487;
Wright, Stuart/0000-0003-4260-5676; Santiago, Louis/0000-0001-5994-6122
FU Smithsonian Institution; Andrew W. Mellon Foundation; NOAA [GC07-172]
FX Rufino Gonzalez and Omar Hernandez have added nutrients since 1998 and
collected most of the data presented here. Funding was provided by
grants from the Scholarly Studies program of the Smithsonian Institution
and the Andrew W. Mellon Foundation to S. J. Wright and from NOAA
(proposal number GC07-172) to L. O. Hedin.
NR 47
TC 162
Z9 176
U1 11
U2 147
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 AUG
PY 2011
VL 92
IS 8
BP 1616
EP 1625
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 801RW
UT WOS:000293459100008
PM 21905428
ER
PT J
AU Maciejewski, M
Vogelsberger, M
White, SDM
Springel, V
AF Maciejewski, Michal
Vogelsberger, Mark
White, Simon D. M.
Springel, Volker
TI Bound and unbound substructures in Galaxy-scale dark matter haloes
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods: numerical; dark matter
ID PHASE-SPACE STRUCTURES; FINDING ALGORITHM; UNIVERSE; MODELS; FINDER
AB We analyse the coarse-grained phase-space structure of the six Galaxy-scale darkmatter haloes of the Aquarius Project using a state-of-the-art 6D substructure finder. Within r(50), we find that about 35 per cent of the mass is in identifiable substructures, predominantly tidal streams, but including about 14 per cent in self-bound subhaloes. The slope of the differential substructure mass function is close to -2, which should be compared to similar to -1.9 for the population of self-bound subhaloes. Near r(50), about 60 per cent of the mass is in substructures, with about 30 per cent in self-bound subhaloes. The inner 35 kpc of the highest resolution simulation has only 0.5 per cent of its mass in self-bound subhaloes, but 3.3 per cent in detected substructure, again primarily tidal streams. The densest tidal streams near the solar position have a 3D mass density about 1 per cent of the local mean, and populate the high-velocity tail of the velocity distribution.
C1 [Maciejewski, Michal; Vogelsberger, Mark; White, Simon D. M.; Springel, Volker] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
RP Maciejewski, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany.
EM michalm@mpa-garching.mpg.de
NR 28
TC 18
Z9 18
U1 0
U2 1
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 AUG
PY 2011
VL 415
IS 3
BP 2475
EP 2484
DI 10.1111/j.1365-2966.2011.18871.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811AO
UT WOS:000294173900038
ER
PT J
AU Birnboim, Y
Dekel, A
AF Birnboim, Yuval
Dekel, Avishai
TI Gravitational quenching by clumpy accretion in cool-core clusters:
convective dynamical response to overheating
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE hydrodynamics; galaxies: clusters: general; galaxies: formation;
galaxies: haloes; X-rays: galaxies: clusters
ID HIGH-VELOCITY CLOUDS; ANISOTROPIC THERMAL CONDUCTION; FAST-ALPHA SURVEY;
X-RAY-EMISSION; GALAXY CLUSTERS; INTRACLUSTER MEDIUM; MASSIVE GALAXIES;
ENTROPY PROFILES; MAGNETIC-FIELDS; HEAT-CONDUCTION
AB Many galaxy clusters pose a 'cooling-flow problem', where the observed X-ray emission from their cores is not accompanied by enough cold gas or star formation. A continuous energy source is required to balance the cooling rate over the whole core volume. We address the feasibility of a gravitational heating mechanism, utilizing the gravitational energy released by the gas that streams into the potential well of the cluster dark matter halo. We focus here on a specific form of gravitational heating in which the energy is transferred to the medium thorough the drag exerted on inflowing gas clumps. Using spherisymmetric hydro simulations with a subgrid representation of these clumps, we confirm our earlier estimates that in haloes >= 10(13) M-circle dot the gravitational heating is more efficient than the cooling everywhere. The worry was that this could overheat the core and generate an instability that might push it away from equilibrium. However, we find that the overheating does not change the global halo properties, and that convection can stabilize the cluster by carrying energy away from the overheated core. In a typical rich cluster of 10(14-15) M-circle dot, with similar to 5 per cent of the accreted baryons in gas clumps of similar to 10(8) M-circle dot, we derive upper and lower limits for the temperature and entropy profiles and show that they are consistent with those observed in cool-core clusters. We predict the density and mass of cold gas and the level of turbulence driven by the clump accretion. We conclude that gravitational heating is a feasible mechanism for preventing cooling flows in clusters.
C1 [Birnboim, Yuval] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Birnboim, Yuval; Dekel, Avishai] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel.
RP Birnboim, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ybirnboim@cfa.harvard.edu; dekel@phys.huji.ac.il
OI Birnboim, Yuval/0000-0002-6547-8545
FU ISF [6/08]; GIF [G-1052-104.7/2009]; DIP; NSF [AST-1010033]
FX We thank Ami Glasner for his advice on mixing length theory. We
acknowledge fruitful discussions with Peng Oh, Orly Gnat, Jerry Ostriker
and Ian Parrish, and thank the referee for helpful comments. This
research has been partly supported by ISF grant 6/08, by GIF grant
G-1052-104.7/2009, by a DIP grant and by NSF grant AST-1010033. YB was
an ITC fellow at CfA, Harvard.
NR 83
TC 20
Z9 21
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 AUG
PY 2011
VL 415
IS 3
BP 2566
EP 2579
DI 10.1111/j.1365-2966.2011.18880.x
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811AO
UT WOS:000294173900046
ER
PT J
AU Johnston, KG
Keto, E
Robitaille, TP
Wood, K
AF Johnston, Katharine G.
Keto, Eric
Robitaille, Thomas P.
Wood, Kenneth
TI The standard model of low-mass star formation applied to massive stars:
multiwavelength modelling of IRAS 20126+4104
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; radiative transfer; stars: formation; ISM:
jets and outflows; infrared: stars
ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; T-TAURI STARS;
2-DIMENSIONAL RADIATIVE-TRANSFER; INTERSTELLAR DUST GRAINS; PROTOSTELLAR
ENVELOPES; MOLECULAR OUTFLOW; SIZE DISTRIBUTION; FORMING REGIONS; DISK
AB In order to investigate whether massive stars form similarly to their low-mass counterparts, we have used the standard envelope plus disc geometry successfully applied to low-mass protostars to model the near-IR to submillimetre spectral energy distribution (SED) and several mid-IR images of the embedded massive star IRAS 20126+4104. We have used a Monte Carlo radiative transfer dust code to model the continuum absorption, emission and scattering through two azimuthally symmetric dust geometries, the first consisting of a rotationally flattened envelope with outflow cavities, and the second which also includes a flared accretion disc. Our results show that the envelope plus disc model reproduces the observed SED and images more accurately than the model without a disc, although the latter model more closely reproduces the morphology of the mid-IR emission within a radius of 1.1 arcsec or similar to 1800 au. We have put forward several possible causes of this discontinuity, including inner truncation of the disc due to stellar irradiation or precession of the outflow cavity. Our best-fitting envelope plus disc model has a disc radius of 9200 au. We find that it is unlikely that the outer regions of such a disc would be in hydrostatic or centrifugal equilibrium, however we calculate that the temperatures within the disc would keep it stable to fragmentation.
C1 [Johnston, Katharine G.; Keto, Eric; Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Johnston, Katharine G.; Wood, Kenneth] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
[Johnston, Katharine G.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Johnston, KG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM johnston@mpia.de; keto@cfa.harvard.edu
OI Robitaille, Thomas/0000-0002-8642-1329
NR 54
TC 11
Z9 11
U1 0
U2 1
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 AUG
PY 2011
VL 415
IS 3
BP 2953
EP 2968
DI 10.1111/j.1365-2966.2011.18913.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 811AO
UT WOS:000294173900078
ER
PT J
AU Boyce, WM
Vickers, W
Morrison, SA
Sillett, TS
Caldwell, L
Wheeler, SS
Barker, CM
Cummings, R
Reisen, WK
AF Boyce, Walter M.
Vickers, Winston
Morrison, Scott A.
Sillett, T. Scott
Caldwell, Luke
Wheeler, Sarah S.
Barker, Christopher M.
Cummings, Robert
Reisen, William K.
TI Surveillance for West Nile Virus and Vaccination of Free-Ranging Island
Scrub-Jays (Aphelocoma insularis) on Santa Cruz Island, California
SO VECTOR-BORNE AND ZOONOTIC DISEASES
LA English
DT Article
DE Birds; Mosquito(es); Surveillance; West Nile; Conservation
ID CULEX-TARSALIS DIPTERA; VECTOR COMPETENCE; BIRDS; CULICIDAE;
TRANSMISSION; ANTIBODIES; DISPERSAL; INFECTION; MOSQUITOS; DISEASES
AB Transmission of West Nile virus (WNV) on mainland California poses an ongoing threat to the island scrub-jay (ISSJ, Aphelocoma insularis), a species that occurs only on Santa Cruz Island, California, and whose total population numbers < 5000. Our report describes the surveillance and management efforts conducted since 2006 that are designed to understand and mitigate for the consequences of WNV introduction into the ISSJ population. We suspect that WNV would most likely be introduced to the island via the movement of infected birds from the mainland. However, antibody testing of > 750 migrating and resident birds on the island from 2006 to 2009 indicated that WNV had not become established by the end of 2009. Several species of competent mosquito vectors were collected at very low abundance on the island, including the important mainland vectors Culex tarsalis and Culex quinquefasciatus. However, the island was generally cooler than areas of mainland California that experienced intense WNV transmission, and these lower temperatures may have reduced the likelihood of WNV becoming established because they do not support efficient virus replication in mosquitoes. A vaccination program was initiated in 2008 to create a rescue population of ISSJ that would be more likely to survive a catastrophic outbreak. To further that goal, we recommend managers vaccinate > 100 ISSJ each year as part of ongoing research and monitoring efforts.
C1 [Boyce, Walter M.; Vickers, Winston] Univ Calif Davis, Wildlife Hlth Ctr, Sch Vet Med, Davis, CA 95616 USA.
[Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA.
[Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA.
[Caldwell, Luke] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA.
[Wheeler, Sarah S.; Barker, Christopher M.; Reisen, William K.] Univ Calif Davis, Ctr Vectorborne Dis, Sch Vet Med, Davis, CA 95616 USA.
[Cummings, Robert] Orange Cty Vector Control Dist, Garden Grove, CA USA.
RP Boyce, WM (reprint author), Univ Calif Davis, Wildlife Hlth Ctr, Sch Vet Med, Old Davis Rd, Davis, CA 95616 USA.
EM wmboyce@ucdavis.edu
FU Nature Conservancy; US Fish and Wildlife Service, Channel Islands
National Park; NIAID NIH [RO1-AI55607]; American Recovery and
Reinvestment Act support
FX We thank The Nature Conservancy, the UC Natural Reserve System's Santa
Cruz Island field station, Channel Islands National Park, our many
talented assistants in the field, and our many collaborators in the ISSJ
Conservation Initiative, especially L. Laughrin, K. Faulkner, and C.
Collins. Bird sera and mosquitoes were tested under BSL3 conditions at
the UC Davis CVECs laboratory under the direction of Ying Fang. This
research was funded, in part, by The Nature Conservancy, The US Fish and
Wildlife Service, Channel Islands National Park, and NIAID NIH Grant
RO1-AI55607, using American Recovery and Reinvestment Act support.
NR 31
TC 12
Z9 14
U1 2
U2 14
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1530-3667
J9 VECTOR-BORNE ZOONOT
JI Vector-Borne Zoonotic Dis.
PD AUG
PY 2011
VL 11
IS 8
BP 1063
EP 1068
DI 10.1089/vbz.2010.0171
PG 6
WC Public, Environmental & Occupational Health; Infectious Diseases
SC Public, Environmental & Occupational Health; Infectious Diseases
GA 804BT
UT WOS:000293629600011
PM 21438695
ER
PT J
AU Carvalho, MR
Herrera, FA
Jaramillo, CA
Wing, SL
Callejas, R
AF Carvalho, Monica R.
Herrera, Fabiany A.
Jaramillo, Carlos A.
Wing, Scott L.
Callejas, Ricardo
TI PALEOCENE MALVACEAE FROM NORTHERN SOUTH AMERICA AND THEIR
BIOGEOGRAPHICAL IMPLICATIONS
SO AMERICAN JOURNAL OF BOTANY
LA English
DT Article
DE Colombia; Eumalvoideae; fossil leaves; leaf architecture; Malvaceae;
neotropics; paleobiogeography; pollen
ID TRIBE HIBISCEAE MALVACEAE; NEOTROPICAL RAIN-FOREST; LONG-DISTANCE
DISPERSAL; PLASTID DNA-SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; CERREJON
FORMATION; AMAZONIAN FORESTS; LEAF ARCHITECTURE; CHLOROPLAST GENE; XYLEM
EVOLUTION
AB Premise of the study: The clade Bombacoideae + Malvoideae ('Malvatheca group' sensu Baum et al.) in Malvaceae comprises a mostly tropical lineage with derived taxa that now thrive in higher latitudes. The sparse fossil record, especially for Malvoideae, obscures interpretations of past distributions. We describe fossil leaves of Malvoideae from the middle-late Paleocene Cerrejon Formation in Colombia, which contains evidence for the earliest known neotropical rainforest.
Methods: Fifty-six leaf compressions belonging to Malvaceae were collected from the Cerrejon Formation in northern Colombia. Leaf architectural characters were scored and optimized for 81 genera of Malvaceae. Synapomorphic characters and unique character combinations support natural affinities for the fossil leaves. Fossil pollen from the same formation was also assessed.
Key results: Despite convergence of overall leaf architecture among many Malvaceae, Malvaciphyllum macondicus sp. nov. can be assigned to the clade Eumalvoideae because of distal and proximal bifurcations of the costal secondary and agrophic veins, a synapomorphy for this clade.
Conclusions: The leaf compressions, the oldest fossils for Eumalvoideae, indicate a minimum divergence time of 58-60 Ma, older than existing estimates from molecular analyses of living species. The abundance of eumalvoid leaves and of bombacoid pollen in the midlate Paleocene of Colombia suggests that the Malvatheca group (Malvoideae + Bombacoideae) was already a common element in neotropical forests and does not support an Australasian origin for Eumalvoideae.
C1 [Carvalho, Monica R.; Callejas, Ricardo] Univ Antioquia, Inst Biol, Medellin, Colombia.
[Carvalho, Monica R.; Herrera, Fabiany A.; Jaramillo, Carlos A.] CTPA, Smithsonian Trop Res Inst, Panama City, Panama.
[Carvalho, Monica R.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Herrera, Fabiany A.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA.
[Herrera, Fabiany A.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Wing, Scott L.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Carvalho, MR (reprint author), Univ Antioquia, Inst Biol, Medellin, Colombia.
EM moccada@gmail.edu
OI Wing, Scott/0000-0002-2954-8905
FU Smithsonian Tropical Research Institute; Department of Botany of the
Smithsonian Museum of Natural History; Smithsonian Paleobiology
Endowment Fund; Smithsonian Unrestricted Endowment; NSF [DEB-0733725,
DEB-0919071]; Fundacion para la Promocion de la Investigacion y la
Tecnologia, Banco de la Republica; Colombian Petroleum Institute;
Fundacion Ares; Evolving Earth Foundation; Geological Society of America
Foundation; Gary S. Morgan Student Research Award; Lewis & Clark
Foundation-American Philosophical Society
FX This work was supported by a short-term fellowship at the Smithsonian
Tropical Research Institute and a partial Jose Cuatrecasas fellowship in
the Department of Botany of the Smithsonian Museum of Natural History
(MRC), Carbones del Cerrejon and the Smithsonian Paleobiology Endowment
Fund (FAH), a Smithsonian Unrestricted Endowment Grant (CJ, SW), and NSF
grants DEB-0733725 (CJ), and DEB-0919071 (MRC), the Fundacion para la
Promocion de la Investigacion y la Tecnologia, Banco de la Republica,
the Colombian Petroleum Institute, and Fundacion Ares (CJ, FAH), the
Evolving Earth Foundation (FAH), the Geological Society of America
Foundation (FAH), the Gary S. Morgan Student Research Award (FAH), and
the Lewis & Clark Foundation-American Philosophical Society (FH). The
authors thank L. Teicher, F. Chavez, G. Hernandez, C. Montes, A. Rincon,
and the geology team at the Cerrejon mine for fieldwork support. M.R.C.
especially thanks Laurence Dorr for taxonomic discussions and Lisa
Barnett, Peter Wilf, Vicky Funk, Emily Wood, Alvaro Idarraga, and
curators at US, A, HUA and SCZ herbaria.
NR 106
TC 18
Z9 20
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 AUG
PY 2011
VL 98
IS 8
BP 1337
EP 1355
DI 10.3732/ajb.1000539
PG 19
WC Plant Sciences
SC Plant Sciences
GA 802LR
UT WOS:000293513400024
PM 21821594
ER
PT J
AU Hystad, P
Setton, E
Cervantes, A
Poplawski, K
Deschenes, S
Brauer, M
van Donkelaar, A
Lamsal, L
Martin, R
Jerrett, M
Demers, P
AF Hystad, Perry
Setton, Eleanor
Cervantes, Alejandro
Poplawski, Karla
Deschenes, Steeve
Brauer, Michael
van Donkelaar, Aaron
Lamsal, Lok
Martin, Randall
Jerrett, Michael
Demers, Paul
TI Creating National Air Pollution Models for Population Exposure
Assessment in Canada
SO ENVIRONMENTAL HEALTH PERSPECTIVES
LA English
DT Article
DE air pollution; Canada; fixed-site monitors; gradients; land use
regression; population exposure assessment; satellite data
ID LAND-USE REGRESSION; VOLATILE ORGANIC-COMPOUNDS; AMBIENT
NITROGEN-DIOXIDE; FINE PARTICULATE MATTER; INTRAURBAN VARIABILITY;
SPATIAL VARIABILITY; MAJOR ROAD; URBAN; GIS; EMISSIONS
AB BACKGROUND: Population exposure assessment methods that capture local-scale pollutant variability are needed for large-scale epidemiological studies and surveillance, policy, and regulatory purposes. Currently, such exposure methods are limited.
METHODS: We created 2006 national pollutant models for fine particulate matter [PM with aerodynamic diameter <= 2.5 mu m (PM2.5)], nitrogen dioxide (NO2), benzene, ethylbenzene, and 1,3-butadiene from routinely collected fixed-site monitoring data in Canada. In multiple regression models, we incorporated satellite estimates and geographic predictor variables to capture background and regional pollutant variation and used deterministic gradients to capture local-scale variation. The national NO2 and benzene models are evaluated with independent measurements from previous land use regression models that were conducted in seven Canadian cities. National models are applied to census block-face points, each of which represents the location of approximately 89 individuals, to produce estimates of population exposure.
RESULTS: The national NO2 model explained 73% of the variability in fixed-site monitor concentrations, PM2.5 46%, benzene 62%, ethylbenzene 67%, and 1,3-butadiene 68%. The NO2 model predicted, on average, 43% of the within-city variability in the independent NO2 data compared with 18% when using inverse distance weighting of fixed-site monitoring data. Benzene models performed poorly in predicting within-city benzene variability. Based on our national models, we estimated Canadian ambient annual average population-weighted exposures (in micrograms per cubic meter) of 8.39 for PM2.5, 23.37 for NO2, 1.04 for benzene, 0.63 for ethylbenzene, and 0.09 for 1,3-butadiene.
CONCLUSIONS: The national pollutant models created here improve exposure assessment compared with traditional monitor-based approaches by capturing both regional and local-scale pollution variation. Applying national models to routinely collected population location data can extend land use modeling techniques to population exposure assessment and to informing surveillance, policy, and regulation.
C1 [Hystad, Perry] Univ British Columbia, Sch Populat & Publ Hlth, Vancouver, BC V6T 1Z3, Canada.
[Setton, Eleanor; Deschenes, Steeve] Univ Victoria, Dept Geog, Victoria, BC, Canada.
[Cervantes, Alejandro] Univ British Columbia, Dept Geog, Vancouver, BC V6T 1Z3, Canada.
[Poplawski, Karla; Brauer, Michael; Demers, Paul] Univ British Columbia, Sch Environm Hlth, Vancouver, BC V6T 1Z3, Canada.
[van Donkelaar, Aaron; Lamsal, Lok; Martin, Randall] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada.
[Martin, Randall] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jerrett, Michael] Univ Calif Berkeley, Sch Publ Hlth, Div Environm Hlth Sci, Berkeley, CA 94720 USA.
[Demers, Paul] Occupat Canc Res Ctr, Toronto, ON, Canada.
RP Hystad, P (reprint author), Univ British Columbia, Sch Populat & Publ Hlth, 2206 E Mall, Vancouver, BC V6T 1Z3, Canada.
EM phystad@gmail.com
RI Lamsal, Lok/G-4781-2012;
OI Brauer, Michael/0000-0002-9103-9343
FU Canadian Partnership against Cancer
FX The research was supported by a grant from the Canadian Partnership
against Cancer. Health Canada also provided support for the development
of the satellite-derived pollution estimates.
NR 49
TC 39
Z9 41
U1 2
U2 34
PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE
PI RES TRIANGLE PK
PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233,
RES TRIANGLE PK, NC 27709-2233 USA
SN 0091-6765
J9 ENVIRON HEALTH PERSP
JI Environ. Health Perspect.
PD AUG
PY 2011
VL 119
IS 8
BP 1123
EP 1129
DI 10.1289/ehp.1002976
PG 7
WC Environmental Sciences; Public, Environmental & Occupational Health;
Toxicology
SC Environmental Sciences & Ecology; Public, Environmental & Occupational
Health; Toxicology
GA 801MU
UT WOS:000293444300030
PM 21454147
ER
PT J
AU Hershler, R
Thompson, FG
Liu, HP
AF Hershler, Robert
Thompson, Fred G.
Liu, Hsiu-Ping
TI A LARGE RANGE EXTENSION AND MOLECULAR PHYLOGENETIC ANALYSIS OF THE
MONOTYPIC NORTH AMERICAN AQUATIC GASTROPOD GENUS CINCINNATIA
(HYDROBIIDAE)
SO JOURNAL OF MOLLUSCAN STUDIES
LA English
DT Article
ID MITOCHONDRIAL-DNA SEQUENCES; NYMPHOPHILINE GASTROPODS; SYSTEMATICS;
RISSOOIDEA; INFERENCE; MRBAYES
AB The freshwater gastropod genus Cincinnatia (Hydrobiidae: Nymphophilinae) contains a single species, C. integra (Say, 1821), which is distributed across much of eastern North America from the Great Lakes region to the Texas Gulf Coastal Plain. Here we use morphological and molecular evidence to evaluate the taxonomic status of a Cincinnatia population that was recently discovered in an upper reach of the Rio Panuco basin (northeastern Mexico) c. 700 km distant from its most closely proximal congeners. The Panuco basin population cannot be consistently differentiated from C. integra by its shells, although it differs from previously reported material of this species in several details of reproductive anatomy. The Panuco basin population differs from specimens from the type locality area and five other populations of C. integra by 1.5-2.6% mtCOI sequence divergence, but was no more differentiated than most of the other populations and was not consistently resolved as a monophyletic subunit of Cincinnatia using these molecular data. Based on this evidence we treat this population as belonging to C. integra pending a more comprehensive study of morphological and genetic variation across the broad geographic range of this species. This new record represents a large range extension not only for Cincinnatia, but also for the entire North American nymphophiline radiation, whose previously recorded southern limit was the Cuatro Cienegas basin in Coahuila.
C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
[Thompson, Fred G.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA.
[Liu, Hsiu-Ping] Metropolitan State Coll Denver, Dept Biol, Denver, CO 80217 USA.
RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA.
EM hershlerr@si.edu
FU Department of Invertebrate Zoology, National Museum of Natural History,
Smithsonian Institution
FX Mexican fieldwork was conducted under the auspices of a collecting
permit (# DOO.02.-0207) issued by the Secretaria del Medio Ambiente y
Recursos Naturales Instituto Nacional de Ecologia Direccion General de
Vida Silvestre to FGT collaborator Alfonso Correa-Sandoval (Instituto
Tecnologico de Ciudad Victoria, Tamaulipas). Liath Appleton assisted
with this fieldwork. Scanning electron micrographs were taken by Yolanda
Villacampa. Karolyn Darrow photographed type material and inked the line
drawings. Dan Cole assisted with map preparation. The first author's
contribution to this project was supported by the Department of
Invertebrate Zoology, National Museum of Natural History, Smithsonian
Institution.
NR 19
TC 1
Z9 1
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0260-1230
J9 J MOLLUS STUD
JI J. Molluscan Stud.
PD AUG
PY 2011
VL 77
BP 232
EP 240
DI 10.1093/mollus/eyr008
PN 3
PG 9
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 799SB
UT WOS:000293305300004
ER
PT J
AU Miura, O
Frankel, V
Torchin, ME
AF Miura, Osamu
Frankel, Victor
Torchin, Mark E.
TI DIFFERENT DEVELOPMENTAL STRATEGIES IN GEMINATE MUD SNAILS,
CERITHIDEOPSIS CALIFORNICA AND C. PLICULOSA, ACROSS THE ISTHMUS OF
PANAMA
SO JOURNAL OF MOLLUSCAN STUDIES
LA English
DT Article
ID EGG SIZE; MARINE-INVERTEBRATES; REPRODUCTIVE STRATEGIES; EVOLUTION;
HISTORY; TRAITS; STAGE; TIME
AB Larval developmental strategy is a key life-history trait governing many aspects of the ecology and evolution of marine invertebrates. We compared developmental strategies of two geminate, or sister, species of mud snails (Potamididae) on either side of the Isthmus of Panama, Cerithideopsis californica on the Pacific and C. pliculosa on the Atlantic coast. We found that these snails, separated by the rise of the Isthmus about 3 Ma, had different reproductive strategies. Larvae of C. californica hatched as small swimming veligers, whereas larvae of C. pliculosa hatched as large swimming-crawling veligers. Additionally, the larval duration of C. pliculosa was about 1 week shorter than that of C. californica under controlled laboratory conditions. This pattern of larval development is consistent with models of life-history evolution in which larger propagules are selected in low-productivity environments (in this case, the Atlantic) and smaller ones are favoured in highly productive environments (the Pacific).
C1 [Miura, Osamu] Kyoto Univ, Grad Sch Global Environm Studies, Sakyo Ku, Kyoto 6068501, Japan.
[Miura, Osamu; Frankel, Victor; Torchin, Mark E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Miura, O (reprint author), Kochi Univ, Div Marine Biotechnol, Oceanog Sect, Ctr Sci Res, Kochi 7838502, Japan.
EM miurao@kochi-u.ac.jp
FU STRI; Smithsonian Marine Science Network; Japan Society for the
Promotion of Science
FX We thank C. Schloder, Y. Kam, J. Javier and staff of the Punta Galeta
Marine Station (Smithsonian Institution) for their field and laboratory
assistance. We thank K. McDonald and two anonymous reviewers for
providing useful comments on the manuscript. Support was provided by
STRI and a Smithsonian Marine Science Network Postdoctoral Fellowship
(to O.M.) and Japan Society for the Promotion of Science (Grant-in-Aid
for JSPS Fellows to O.M.).
NR 18
TC 8
Z9 8
U1 0
U2 11
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0260-1230
J9 J MOLLUS STUD
JI J. Molluscan Stud.
PD AUG
PY 2011
VL 77
BP 255
EP 258
DI 10.1093/mollus/eyr012
PN 3
PG 4
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 799SB
UT WOS:000293305300007
ER
PT J
AU Puillandre, N
Kantor, YI
Sysoev, A
Couloux, A
Meyer, C
Rawlings, T
Todd, JA
Bouchet, P
AF Puillandre, N.
Kantor, Yu. I.
Sysoev, A.
Couloux, A.
Meyer, C.
Rawlings, T.
Todd, J. A.
Bouchet, P.
TI THE DRAGON TAMED? A MOLECULAR PHYLOGENY OF THE CONOIDEA (GASTROPODA)
SO JOURNAL OF MOLLUSCAN STUDIES
LA English
DT Article
ID MOLLUSCA; CONUS; CLASSIFICATION; NEOGASTROPODA; DISCOVERY; PEPTIDES;
ANATOMY; VENOMS; TOXINS; SNAILS
AB The superfamily Conoidea constitutes one of the most diverse and taxonomically challenging groups among marine molluscs. Classifications based on shell or radular characters are highly contradictory and disputed. Whereas the monophyly of the Conidae and Terebridae has not been challenged, the other constituents of the superfamily are placed in a 'trash' group, the turrids, the non-monophyly of which has been demonstrated by anatomical and molecular evidence. We present here a new molecular phylogeny based on a total of 102 conoidean genera (87 'turrids', 5 cones and 10 terebrids) and three mitochondrial genes [cytochrome oxidase I (COI), 12S rRNA and 16S rRNA]. The resulting tree recognizes 14 clades. When the Conidae (Conus s.l.) and Terebridae are ranked as families for consistency of usage, the 'turrids' must be split into 12 families of comparable rank. A new genus-level classification of the Conoidea is published in an accompanying paper.
C1 [Puillandre, N.; Bouchet, P.] Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7138, F-75231 Paris, France.
[Kantor, Yu. I.] Russian Acad Sci, AN Severtsov Inst Ecol & Evolut, Moscow 119071, Russia.
[Sysoev, A.] Moscow MV Lomonosov State Univ, Zool Museum, Moscow 125009, Russia.
[Couloux, A.] Ctr Natl Sequencage, GENOSCOPE, F-91057 Evry, France.
[Meyer, C.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Rawlings, T.] Cape Breton Univ, Dept Biol, Sydney, NS B1P 6L2, Canada.
[Todd, J. A.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England.
RP Puillandre, N (reprint author), Museum Natl Hist Nat, Dept Systemat & Evolut, UMR 7138, 55 Rue Buffon, F-75231 Paris, France.
EM puillandre@mnhn.fr
RI Kantor, Yuri/D-5259-2014;
OI Kantor, Yuri/0000-0002-3209-4940; Todd, Jonathan/0000-0002-0433-1611
FU Total Foundation; French Ministry of Foreign Affairs; MNHN-IRD-PNI
Santo; Stavros Niarchos Foundation; AURORA; Lounsbery Foundation;
Florida Institution of Oceanography; NERC [GR3/13110]; Systematics
Association [22/03/2000]; NSF [0316338]; RFBR [09-04-00911-a];
Consortium National de Recherche en Genomique; Service de Systematique
Moleculaire [UMS 2700 CNRS-MNHN]
FX The PANGLAO 2004 Marine Biodiversity Project was funded by the Total
Foundation and the French Ministry of Foreign Affairs, the MNHN-IRD-PNI
Santo 2006 expedition was made possible by grants, among others, from
the Total Foundation and the Stavros Niarchos Foundation, and the AURORA
2007 cruise was made possible through a grant from the Lounsbery
Foundation. The Coral Sea and Solomon Islands cruises took place on
board R/V Alis deployed from Noumea by the Institut de Recherche pour le
Developpement (IRD), and Bertrand Richer de Forges was cruise leader for
the Solomons, Coral Sea and Vanuatu expeditions. Ellen Strong,
Marie-Catherine Boisselier and Sarah Samadi are thanked for their role
in molecular sampling during these expeditions. Cruises in the Gulf of
Panama (2000) and the Lower Florida Keys (2001) were on R/V Urraca and
R/V Bellows, respectively, and we thank the captain and crew of each and
the respective expedition leaders H. Lessios (STRI, Panama) and T.
Collins (FIU, Miami). The Lower Florida Keys cruise was supported by a
grant from the Florida Institution of Oceanography. We also thank R.
Bieler (FMNH, Chicago) and Paula Mikkelsen (PRI, New York) for inviting
one of us (TR) on their research cruise on the R/V Eugenie Clarke in
2001 and for specimens collected during their research activities in the
Florida Keys. Work was conducted in Paris by YuIK and AS during several
visits under the MNHN visiting curatorships programme. They express
their thanks to Virginie Heros, Barbara Buge, Philippe Maestrati and
Pierre Lozouet for assistance during their stay in Paris. This work was
supported by NERC Standard Research Grant GR3/13110 and Systematics
Association Research Grant (22/03/2000) (PI JAT), NSF: DEB #0316338 (PI
Alan Kohn), grant of RFBR 09-04-00911-a 'Venomous predatory gastropod
molluscs: evolutionary and morphological aspects' (PI Yu. I. Kantor),
the Consortium National de Recherche en Genomique and the Service de
Systematique Moleculaire (UMS 2700 CNRS-MNHN). It is part of the
agreement 2005/67 between the Genoscope and the Museum National
d'Histoire Naturelle on the project Macrophylogeny of Life directed by
Guillaume Lecointre. The phylogenetic analyses were performed on the
vital-it clusters (www.vital-it.ch). Serge Gofas, Jon-Arne Sneli,
Baldomero Olivera and Maren Watkins provided additional specimens and
sequences. Barbara Buge curated and photographed the voucher specimens
in MNHN and Joanna Griffin helped curate the voucher specimens in the
NHM. Claire Griffin and Julia Llewellyn-Hughes undertook the sequencing
of all samples processed at the NHM. The authors also thank several
colleagues for their help in the identification of specimens: Dick
Kilburn ('turrids'), Bruce Marshall ('turrids'), Jim McLean ('turrids'),
Baldomero Olivera (Conidae), Yves Terryn (Terebridae), Alain Robin,
Gilbert Jaux, Jean-Claude Martin and Kurt Kreipl (outgroups).
NR 39
TC 41
Z9 42
U1 3
U2 26
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0260-1230
EI 1464-3766
J9 J MOLLUS STUD
JI J. Molluscan Stud.
PD AUG
PY 2011
VL 77
BP 259
EP 272
DI 10.1093/mollus/eyr015
PN 3
PG 14
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 799SB
UT WOS:000293305300008
ER
PT J
AU Hong, T
AF Hong, Terry
TI Nanjing Requiem
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian Book Dragon, Washington, DC USA.
RP Hong, T (reprint author), Smithsonian Book Dragon, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU REED BUSINESS INFORMATION
PI NEW YORK
PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD AUG
PY 2011
VL 136
IS 13
BP 84
EP 84
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 807BT
UT WOS:000293869000128
ER
PT J
AU Hirsch, BT
AF Hirsch, Ben T.
TI Long-term adult male sociality in ring-tailed coatis (Nasua nasua)
SO MAMMALIA
LA English
DT Article
DE food competition; Iguazu; mating system; Nasua; predation
ID WHITE-NOSED COATIS; OCELOT LEOPARDUS-PARDALIS; GROUP SPATIAL POSITION;
ATLANTIC FOREST; ACTIVITY PATTERNS; HABITAT USE; NARICA; ARGENTINA;
BEHAVIOR; BRAZIL
C1 [Hirsch, Ben T.] Smithsonian Trop Res Inst, DPO, AA 34002 USA.
[Hirsch, Ben T.] New York State Museum & Sci Serv, Biol Survey, Albany, NY 12230 USA.
RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, DPO, AA 34002 USA.
EM hirschb@si.edu
FU National Science Foundation [BCS-0314525]
FX I thank Y. Di Blanco, S. Escobar, C. Ferrari, V. Munoz, F. Silva, and M.
Tammone for help and assistance with the fieldwork. I am particularly
grateful to C. Janson for the immeasurable amount of advice he gave me
during all aspects of this project, and Matt Gompper for comments on an
earlier draft of the manuscript. I thank the Administration de Parques
Nacionales for permission to carry out work in Iguazu. This study was
funded in part by a National Science Foundation grant (BCS-0314525).
NR 38
TC 3
Z9 3
U1 13
U2 81
PU WALTER DE GRUYTER & CO
PI BERLIN
PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY
SN 0025-1461
J9 MAMMALIA
JI Mammalia
PD AUG
PY 2011
VL 75
IS 3
BP 301
EP 304
DI 10.1515/MAMM.2011.030
PG 4
WC Zoology
SC Zoology
GA 803FT
UT WOS:000293567900013
ER
PT J
AU Meyer, KA
Mackay, DH
van Ballegooijen, AA
Parnell, CE
AF Meyer, K. A.
Mackay, D. H.
van Ballegooijen, A. A.
Parnell, C. E.
TI Solar Magnetic Carpet I: Simulation of Synthetic Magnetograms
SO SOLAR PHYSICS
LA English
DT Article
DE Sun: magnetic fields; Sun: magnetic carpet
ID MICHELSON DOPPLER IMAGER; CHROMOSPHERIC NETWORK; VELOCITY-FIELDS; FLUX
EMERGENCE; SUN; INTRANETWORK; EVOLUTION; TRACKING; ELEMENTS; REGIONS
AB This paper describes a new 2D model for the photospheric evolution of the magnetic carpet. It is the first in a series of papers working towards constructing a realistic 3D non-potential model for the interaction of small-scale solar magnetic fields. In the model, the basic evolution of the magnetic elements is governed by a supergranular flow profile. In addition, magnetic elements may evolve through the processes of emergence, cancellation, coalescence and fragmentation. Model parameters for the emergence of bipoles are based upon the results of observational studies. Using this model, several simulations are considered, where the range of flux with which bipoles may emerge is varied. In all cases the model quickly reaches a steady state where the rates of emergence and cancellation balance. Analysis of the resulting magnetic field shows that we reproduce observed quantities such as the flux distribution, mean field, cancellation rates, photospheric recycle time and a magnetic network. As expected, the simulation matches observations more closely when a larger, and consequently more realistic, range of emerging flux values is allowed (4x10(16) -aEuro parts per thousand 10(19) Mx). The model best reproduces the current observed properties of the magnetic carpet when we take the minimum absolute flux for emerging bipoles to be 4x10(16) Mx. In future, this 2D model will be used as an evolving photospheric boundary condition for 3D non-potential modeling.
C1 [Meyer, K. A.; Mackay, D. H.; Parnell, C. E.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
[van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Meyer, KA (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland.
EM karen@mcs.st-and.ac.uk
OI van Ballegooijen, Adriaan/0000-0002-5622-3540
FU ISSI (Bern); STFC; Royal Society; EU
FX KAM would like to thank ISSI (Bern) for their support of the team "Solar
small-scale transient phenomena and their role in coronal heating", and
teammates for their encouragement and support of her as a young
researcher. She would also like to thank the Harvard-Smithsonian Center
for Astrophysics (Boston, MA) for its warm hospitality and helpful
discussions during her six-week stay in summer 2010. KAM and DHM
gratefully acknowledge the support of the STFC. DHM would like to thank
the Royal Society for their support through the Research Grant Scheme.
DHM and CEP acknowledge the support of the EU-FP7 project SWIFF.
Finally, we thank the anonymous referee, who's helpful comments and
suggestions have improved the paper.
NR 41
TC 10
Z9 10
U1 0
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0038-0938
J9 SOL PHYS
JI Sol. Phys.
PD AUG
PY 2011
VL 272
IS 1
BP 29
EP 58
DI 10.1007/s11207-011-9809-3
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 801UB
UT WOS:000293465000003
ER
PT J
AU Abdo, AA
Ackermann, M
Ajello, M
Baldini, L
Ballet, J
Barbiellini, G
Bastieri, D
Bechtol, K
Bellazzini, R
Berenji, B
Blandford, RD
Bloom, ED
Bonamente, E
Borgland, AW
Bouvier, A
Bregeon, J
Brez, A
Brigida, M
Bruel, P
Buehler, R
Buson, S
Caliandro, GA
Cameron, RA
Cannon, A
Caraveo, PA
Carrigan, S
Casandjian, JM
Cavazzuti, E
Cecchi, C
Celik, O
Charles, E
Chekhtman, A
Chiang, J
Ciprini, S
Claus, R
Cohen-Tanugi, J
Conrad, J
Cutini, S
de Angelis, A
de Palma, F
Dermer, CD
Silva, EDE
Drell, PS
Dubois, R
Dumora, D
Escande, L
Favuzzi, C
Fegan, SJ
Finke, J
Focke, WB
Fortin, P
Frailis, M
Fuhrmann, L
Fukazawa, Y
Fukuyama, T
Funk, S
Fusco, P
Gargano, F
Gasparrini, D
Gehrels, N
Georganopoulos, M
Germani, S
Giebels, B
Giglietto, N
Giommi, P
Giordano, F
Giroletti, M
Glanzman, T
Godfrey, G
Grenier, IA
Guiriec, S
Hadasch, D
Hayashida, M
Hays, E
Horan, D
Hughes, RE
Johannesson, G
Johnson, AS
Johnson, WN
Kadler, M
Kamae, T
Katagiri, H
Kataoka, J
Knodlseder, J
Kuss, M
Lande, J
Latronico, L
Lee, SH
Longo, F
Loparco, F
Lott, B
Lovellette, MN
Lubrano, P
Madejski, GM
Makeev, A
Max-Moerbeck, W
Mazziotta, MN
McEnery, JE
Mehault, J
Michelson, PF
Mitthumsiri, W
Mizuno, T
Monte, C
Monzani, ME
Morselli, A
Moskalenko, IV
Murgia, S
Nakamori, T
Naumann-Godo, M
Nishino, S
Nolan, PL
Norris, JP
Nuss, E
Ohsugi, T
Okumura, A
Omodei, N
Orlando, E
Ormes, JF
Ozaki, M
Paneque, D
Panetta, JH
Parent, D
Pavlidou, V
Pearson, TJ
Pelassa, V
Pepe, M
Pesce-Rollins, M
Pierbattista, M
Piron, F
Porter, TA
Raino, S
Rando, R
Razzano, M
Readhead, A
Reimer, A
Reimer, O
Reyes, LC
Richards, JL
Ritz, S
Roth, M
Sadrozinski, HFW
Sanchez, D
Sander, A
Sgro, C
Siskind, EJ
Smith, PD
Spandre, G
Spinelli, P
Stawarz, L
Stevenson, M
Strickman, MS
Suson, DJ
Takahashi, H
Takahashi, T
Tanaka, T
Thayer, JG
Thayer, JB
Thompson, DJ
Tibaldo, L
Torres, DF
Tosti, G
Tramacere, A
Troja, E
Usher, TL
Vandenbroucke, J
Vasileiou, V
Vianello, G
Vilchez, N
Vitale, V
Waite, AP
Wang, P
Wehrle, AE
Winer, BL
Wood, KS
Yang, Z
Yatsu, Y
Ylinen, T
Zensus, JA
Ziegler, M
Aleksic, J
Antonelli, LA
Antoranz, P
Backes, M
Barrio, JA
Gonzalez, JB
Bednarek, W
Berdyugin, A
Berger, K
Bernardini, E
Biland, A
Blanch, O
Bock, RK
Boller, A
Bonnoli, G
Bordas, P
Tridon, DB
Bosch-Ramon, V
Bose, D
Braun, I
Bretz, T
Camara, M
Carmona, E
Carosi, A
Colin, P
Colombo, E
Contreras, JL
Cortina, J
Covino, S
Dazzi, F
de Angelis, A
del Pozo, ED
Mendez, CD
De Lotto, B
De Maria, M
De Sabata, F
Ortega, AD
Doert, M
Dominguez, A
Prester, DD
Dorner, D
Doro, M
Elsaesser, D
Ferenc, D
Fonseca, MV
Font, L
Lopez, RJG
Garczarczyk, M
Gaug, M
Giavitto, G
Godinovi, N
Hadasch, D
Herrero, A
Hildebrand, D
Hohne-Monch, D
Hose, J
Hrupec, D
Jogler, T
Klepser, S
Krahenbuhl, T
Kranich, D
Krause, J
La Barbera, A
Leonardo, E
Lindfors, E
Lombardi, S
Lopez, M
Lorenz, E
Majumdar, P
Makariev, E
Maneva, G
Mankuzhiyil, N
Mannheim, K
Maraschi, L
Mariotti, M
Martinez, M
Mazin, D
Meucci, M
Miranda, JM
Mirzoyan, R
Miyamoto, H
Moldon, J
Moralejo, A
Nieto, D
Nilsson, K
Orito, R
Oya, I
Paoletti, R
Paredes, JM
Partini, S
Pasanen, M
Pauss, F
Pegna, RG
Perez-Torres, MA
Persic, M
Peruzzo, J
Pochon, J
Prada, F
Moroni, PGP
Prandini, E
Puchades, N
Puljak, I
Reichardt, T
Rhode, W
Ribo, M
Rico, J
Rissi, M
Rugamer, S
Saggion, A
Saito, K
Saito, TY
Salvati, M
Sanchez-Conde, M
Satalecka, K
Scalzotto, V
Scapin, V
Schultz, C
Schweizer, T
Shayduk, M
Shore, SN
Sierpowska-Bartosik, A
Sillanpaa, A
Sitarek, J
Sobczynska, D
Spanier, F
Spiro, S
Stamerra, A
Steinke, B
Storz, J
Strah, N
Struebig, JC
Suric, T
Takalo, LO
Tavecchio, F
Temnikov, P
Terzic, T
Tescaro, D
Teshima, M
Vankov, H
Wagner, RM
Weitzel, Q
Zabalza, V
Zandanel, F
Zanin, R
Villata, M
Raiteri, C
Aller, HD
Aller, MF
Chen, WP
Jordan, B
Koptelova, E
Kurtanidze, OM
Lahteenmaki, A
McBreen, B
Larionov, VM
Lin, CS
Nikolashvili, MG
Reinthal, R
Angelakis, E
Capalbi, M
Carraminana, A
Carrasco, L
Cassaro, P
Cesarini, A
Falcone, A
Gurwell, MA
Hovatta, T
Kovalev, YA
Kovalev, YY
Krichbaum, TP
Krimm, HA
Lister, ML
Moody, JW
Maccaferri, G
Mori, Y
Nestoras, I
Orlati, A
Pace, C
Pagani, C
Pearson, R
Perri, M
Piner, BG
Ros, E
Sadun, AC
Sakamoto, T
Tammi, J
Zook, A
AF Abdo, A. A.
Ackermann, M.
Ajello, M.
Baldini, L.
Ballet, J.
Barbiellini, G.
Bastieri, D.
Bechtol, K.
Bellazzini, R.
Berenji, B.
Blandford, R. D.
Bloom, E. D.
Bonamente, E.
Borgland, A. W.
Bouvier, A.
Bregeon, J.
Brez, A.
Brigida, M.
Bruel, P.
Buehler, R.
Buson, S.
Caliandro, G. A.
Cameron, R. A.
Cannon, A.
Caraveo, P. A.
Carrigan, S.
Casandjian, J. M.
Cavazzuti, E.
Cecchi, C.
Celik, Oe.
Charles, E.
Chekhtman, A.
Chiang, J.
Ciprini, S.
Claus, R.
Cohen-Tanugi, J.
Conrad, J.
Cutini, S.
de Angelis, A.
de Palma, F.
Dermer, C. D.
do Couto e Silva, E.
Drell, P. S.
Dubois, R.
Dumora, D.
Escande, L.
Favuzzi, C.
Fegan, S. J.
Finke, J.
Focke, W. B.
Fortin, P.
Frailis, M.
Fuhrmann, L.
Fukazawa, Y.
Fukuyama, T.
Funk, S.
Fusco, P.
Gargano, F.
Gasparrini, D.
Gehrels, N.
Georganopoulos, M.
Germani, S.
Giebels, B.
Giglietto, N.
Giommi, P.
Giordano, F.
Giroletti, M.
Glanzman, T.
Godfrey, G.
Grenier, I. A.
Guiriec, S.
Hadasch, D.
Hayashida, M.
Hays, E.
Horan, D.
Hughes, R. E.
Johannesson, G.
Johnson, A. S.
Johnson, W. N.
Kadler, M.
Kamae, T.
Katagiri, H.
Kataoka, J.
Knoedlseder, J.
Kuss, M.
Lande, J.
Latronico, L.
Lee, S. -H.
Longo, F.
Loparco, F.
Lott, B.
Lovellette, M. N.
Lubrano, P.
Madejski, G. M.
Makeev, A.
Max-Moerbeck, W.
Mazziotta, M. N.
McEnery, J. E.
Mehault, J.
Michelson, P. F.
Mitthumsiri, W.
Mizuno, T.
Monte, C.
Monzani, M. E.
Morselli, A.
Moskalenko, I. V.
Murgia, S.
Nakamori, T.
Naumann-Godo, M.
Nishino, S.
Nolan, P. L.
Norris, J. P.
Nuss, E.
Ohsugi, T.
Okumura, A.
Omodei, N.
Orlando, E.
Ormes, J. F.
Ozaki, M.
Paneque, D.
Panetta, J. H.
Parent, D.
Pavlidou, V.
Pearson, T. J.
Pelassa, V.
Pepe, M.
Pesce-Rollins, M.
Pierbattista, M.
Piron, F.
Porter, T. A.
Raino, S.
Rando, R.
Razzano, M.
Readhead, A.
Reimer, A.
Reimer, O.
Reyes, L. C.
Richards, J. L.
Ritz, S.
Roth, M.
Sadrozinski, H. F. -W.
Sanchez, D.
Sander, A.
Sgro, C.
Siskind, E. J.
Smith, P. D.
Spandre, G.
Spinelli, P.
Stawarz, L.
Stevenson, M.
Strickman, M. S.
Suson, D. J.
Takahashi, H.
Takahashi, T.
Tanaka, T.
Thayer, J. G.
Thayer, J. B.
Thompson, D. J.
Tibaldo, L.
Torres, D. F.
Tosti, G.
Tramacere, A.
Troja, E.
Usher, T. L.
Vandenbroucke, J.
Vasileiou, V.
Vianello, G.
Vilchez, N.
Vitale, V.
Waite, A. P.
Wang, P.
Wehrle, A. E.
Winer, B. L.
Wood, K. S.
Yang, Z.
Yatsu, Y.
Ylinen, T.
Zensus, J. A.
Ziegler, M.
Aleksic, J.
Antonelli, L. A.
Antoranz, P.
Backes, M.
Barrio, J. A.
Becerra Gonzalez, J.
Bednarek, W.
Berdyugin, A.
Berger, K.
Bernardini, E.
Biland, A.
Blanch, O.
Bock, R. K.
Boller, A.
Bonnoli, G.
Bordas, P.
Tridon, D. Borla
Bosch-Ramon, V.
Bose, D.
Braun, I.
Bretz, T.
Camara, M.
Carmona, E.
Carosi, A.
Colin, P.
Colombo, E.
Contreras, J. L.
Cortina, J.
Covino, S.
Dazzi, F.
de Angelis, A.
De Cea del Pozo, E.
Delgado Mendez, C.
De Lotto, B.
De Maria, M.
De Sabata, F.
Diago Ortega, A.
Doert, M.
Dominguez, A.
Prester, D. Dominis
Dorner, D.
Doro, M.
Elsaesser, D.
Ferenc, D.
Fonseca, M. V.
Font, L.
Garcia Lopez, R. J.
Garczarczyk, M.
Gaug, M.
Giavitto, G.
Godinovi, N.
Hadasch, D.
Herrero, A.
Hildebrand, D.
Hoehne-Moench, D.
Hose, J.
Hrupec, D.
Jogler, T.
Klepser, S.
Kraehenbuehl, T.
Kranich, D.
Krause, J.
La Barbera, A.
Leonardo, E.
Lindfors, E.
Lombardi, S.
Lopez, M.
Lorenz, E.
Majumdar, P.
Makariev, E.
Maneva, G.
Mankuzhiyil, N.
Mannheim, K.
Maraschi, L.
Mariotti, M.
Martinez, M.
Mazin, D.
Meucci, M.
Miranda, J. M.
Mirzoyan, R.
Miyamoto, H.
Moldon, J.
Moralejo, A.
Nieto, D.
Nilsson, K.
Orito, R.
Oya, I.
Paoletti, R.
Paredes, J. M.
Partini, S.
Pasanen, M.
Pauss, F.
Pegna, R. G.
Perez-Torres, M. A.
Persic, M.
Peruzzo, J.
Pochon, J.
Prada, F.
Moroni, P. G. Prada
Prandini, E.
Puchades, N.
Puljak, I.
Reichardt, T.
Rhode, W.
Ribo, M.
Rico, J.
Rissi, M.
Ruegamer, S.
Saggion, A.
Saito, K.
Saito, T. Y.
Salvati, M.
Sanchez-Conde, M.
Satalecka, K.
Scalzotto, V.
Scapin, V.
Schultz, C.
Schweizer, T.
Shayduk, M.
Shore, S. N.
Sierpowska-Bartosik, A.
Sillanpaa, A.
Sitarek, J.
Sobczynska, D.
Spanier, F.
Spiro, S.
Stamerra, A.
Steinke, B.
Storz, J.
Strah, N.
Struebig, J. C.
Suric, T.
Takalo, L. O.
Tavecchio, F.
Temnikov, P.
Terzic, T.
Tescaro, D.
Teshima, M.
Vankov, H.
Wagner, R. M.
Weitzel, Q.
Zabalza, V.
Zandanel, F.
Zanin, R.
Villata, M.
Raiteri, C.
Aller, H. D.
Aller, M. F.
Chen, W. P.
Jordan, B.
Koptelova, E.
Kurtanidze, O. M.
Lahteenmaki, A.
McBreen, B.
Larionov, V. M.
Lin, C. S.
Nikolashvili, M. G.
Reinthal, R.
Angelakis, E.
Capalbi, M.
Carraminana, A.
Carrasco, L.
Cassaro, P.
Cesarini, A.
Falcone, A.
Gurwell, M. A.
Hovatta, T.
Kovalev, Yu A.
Kovalev, Y. Y.
Krichbaum, T. P.
Krimm, H. A.
Lister, M. L.
Moody, J. W.
Maccaferri, G.
Mori, Y.
Nestoras, I.
Orlati, A.
Pace, C.
Pagani, C.
Pearson, R.
Perri, M.
Piner, B. G.
Ros, E.
Sadun, A. C.
Sakamoto, T.
Tammi, J.
Zook, A.
CA Fermi-LAT Collaboration
MAGIC Collaboration
TI FERMI LARGE AREA TELESCOPE OBSERVATIONS OF MARKARIAN 421: THE MISSING
PIECE OF ITS SPECTRAL ENERGY DISTRIBUTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; BL Lacertae objects: general; BL Lacertae
objects: individual (Mrk 421); galaxies: active; gamma rays: general;
radiation mechanisms: non-thermal
ID BL-LACERTAE OBJECTS; X-RAY-SPECTRA; ACTIVE GALAXY MARKARIAN-421; TEV
BLAZAR MARKARIAN-421; LOG-PARABOLIC SPECTRA; BLACK-HOLE MASSES;
MULTIWAVELENGTH OBSERVATIONS; RADIO-SOURCES; CRAB-NEBULA; 3C 454.3
AB We report on the gamma-ray activity of the high-synchrotron-peaked BL Lacertae object Markarian 421 (Mrk 421) during the first 1.5 years of Fermi operation, from 2008 August 5 to 2010 March 12. We find that the Large Area Telescope (LAT) gamma-ray spectrum above 0.3 GeV can be well described by a power-law function with photon index Gamma = 1.78 +/- 0.02 and average photon flux F(>0.3 GeV) = (7.23 +/- 0.16) x 10(-8) ph cm(-2) s(-1). Over this time period, the Fermi-LAT spectrum above 0.3 GeV was evaluated on seven-day-long time intervals, showing significant variations in the photon flux (up to a factor similar to 3 from the minimum to the maximum flux) but mild spectral variations. The variability amplitude at X-ray frequencies measured by RXTE/ASM and Swift/BAT is substantially larger than that in gamma-rays measured by Fermi-LAT, and these two energy ranges are not significantly correlated. We also present the first results from the 4.5 month long multifrequency campaign on Mrk 421, which included the VLBA, Swift, RXTE, MAGIC, the F-GAMMA, GASP-WEBT, and other collaborations and instruments that provided excellent temporal and energy coverage of the source throughout the entire campaign (2009 January 19 to 2009 June 1). During this campaign, Mrk 421 showed a low activity at all wavebands. The extensive multi-instrument (radio to TeV) data set provides an unprecedented, complete look at the quiescent spectral energy distribution (SED) for this source. The broadband SED was reproduced with a leptonic (one-zone synchrotron self-Compton) and a hadronic model (synchrotron proton blazar). Both frameworks are able to describe the average SED reasonably well, implying comparable jet powers but very different characteristics for the blazar emission site.
C1 [Abdo, A. A.] Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA.
[Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tramacere, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA.
[Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Shore, S. N.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy.
[Ballet, J.; Casandjian, J. M.; Grenier, I. A.; Naumann-Godo, M.; Pierbattista, M.; Tibaldo, L.] Univ Paris Diderot, CNRS, Lab AIM, CEA IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France.
[Barbiellini, G.; Longo, F.; De Lotto, B.; De Maria, M.; De Sabata, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy.
[Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
[Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, J.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.; Doro, M.; Lombardi, S.; Lopez, M.; Mariotti, M.; Peruzzo, J.; Prandini, E.; Saggion, A.; Scalzotto, V.; Schultz, C.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy.
[Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy.
[Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy.
[Bouvier, A.; Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA.
[Bouvier, A.; Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy.
[Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy.
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[Cannon, A.; McBreen, B.] Univ Coll Dublin, Dublin 4, Ireland.
[Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy.
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[Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland.
[Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA.
[Yatsu, Y.; Mori, Y.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan.
[Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden.
[Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden.
[Aleksic, J.; Blanch, O.; Cortina, J.; Giavitto, G.; Klepser, S.; Martinez, M.; Mazin, D.; Moralejo, A.; Puchades, N.; Reichardt, T.; Rico, J.; Tescaro, D.; Zanin, R.] Univ Autonoma Barcelona, IFAE, E-08193 Bellaterra, Barcelona, Spain.
[Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Salvati, M.; Spiro, S.] INAF Natl Inst Astrophys, I-00136 Rome, Italy.
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[Antoranz, P.; Leonardo, E.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Pegna, R. G.; Moroni, P. G. Prada; Stamerra, A.] INFN Pisa, I-53100 Siena, Italy.
[Backes, M.; Doert, M.; Rhode, W.; Strah, N.] Tech Univ Dortmund, D-44221 Dortmund, Germany.
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[Becerra Gonzalez, J.; Berger, K.; Diago Ortega, A.; Garcia Lopez, R. J.; Herrero, A.; Sanchez-Conde, M.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain.
[Bednarek, W.; Sierpowska-Bartosik, A.; Sitarek, J.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland.
[Berdyugin, A.; Lindfors, E.; Pasanen, M.; Sillanpaa, A.; Takalo, L. O.; Reinthal, R.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland.
[Bernardini, E.; Majumdar, P.; Satalecka, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany.
[Biland, A.; Boller, A.; Braun, I.; Dorner, D.; Hildebrand, D.; Kraehenbuehl, T.; Kranich, D.; Lorenz, E.; Pauss, F.; Rissi, M.; Weitzel, Q.] ETH, CH-8093 Zurich, Switzerland.
[Bordas, P.; Bosch-Ramon, V.; Moldon, J.; Paredes, J. M.; Ribo, M.; Zabalza, V.] Univ Barcelona ICC IEEC, E-08028 Barcelona, Spain.
[Bretz, T.; Elsaesser, D.; Hoehne-Moench, D.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Storz, J.; Struebig, J. C.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany.
[Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain.
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[Prester, D. Dominis; Ferenc, D.; Godinovi, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Rijeka, Inst R Boskovic, Croatian MAGIC Consortium, HR-10000 Zagreb, Croatia.
[Prester, D. Dominis; Ferenc, D.; Godinovi, N.; Hrupec, D.; Puljak, I.; Suric, T.; Terzic, T.] Univ Split, HR-10000 Zagreb, Croatia.
[Font, L.] Univ Autonoma Barcelona, E-08193 Bellaterra, Spain.
[Makariev, E.; Maneva, G.; Temnikov, P.; Vankov, H.] Inst Nucl Energy Res, BG-1784 Sofia, Bulgaria.
[Maraschi, L.; Tavecchio, F.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikiio, Finland.
[Persic, M.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy.
[Shore, S. N.] Univ Pisa, Dipartimento Fis Enrico Fermi, I-56127 Pisa, Italy.
[Villata, M.; Raiteri, C.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Chen, W. P.; Koptelova, E.; Lin, C. S.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan.
[Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland.
[Lahteenmaki, A.; Hovatta, T.; Tammi, J.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia.
[Larionov, V. M.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Carraminana, A.; Carrasco, L.] Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico.
[Cassaro, P.] INAF Ist Radioastron, Sez Noto, I-96017 Noto, SR, Italy.
[Cesarini, A.] Natl Univ Ireland Galway, Dept Phys, Galway, Ireland.
[Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovalev, Yu A.; Kovalev, Y. Y.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia.
[Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
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[Maccaferri, G.; Orlati, A.] INAF Ist Radioastron, Stn Radioastron Med, I-40059 Bologna, Italy.
[Pagani, C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Piner, B. G.] Whittier Coll, Dept Phys & Astron, Whittier, CA USA.
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RP Abdo, AA (reprint author), Natl Acad Sci, Natl Res Council Res Associate, Washington, DC 20001 USA.
EM justin.finke@nrl.navy.mil; dpaneque@mppmu.mpg.de;
anita.reimer@uibk.ac.at
RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Font, Lluis/L-4197-2014;
Moskalenko, Igor/A-1301-2007; Contreras Gonzalez, Jose Luis/K-7255-2014;
Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Maneva,
Galina/L-7120-2016; Backes, Michael/N-5126-2016; Torres,
Diego/O-9422-2016; Temnikov, Petar/L-6999-2016; Orlando, E/R-5594-2016;
Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; Tosti,
Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Ozaki,
Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Lahteenmaki,
Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson,
Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Rico,
Javier/K-8004-2014; Fernandez, Ester/K-9734-2014; Lopez Moya,
Marcos/L-2304-2014; GAug, Markus/L-2340-2014; Moralejo Olaizola,
Abelardo/M-2916-2014; Ribo, Marc/B-3579-2015; Morselli,
Aldo/G-6769-2011; Prada Moroni, Pier Giorgio/G-5565-2011; Braun,
Isabel/C-9373-2012; Reimer, Olaf/A-3117-2013; Thompson,
David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery,
Julie/D-6612-2012; Baldini, Luca/E-5396-2012; Mannheim,
Karl/F-6705-2012; lubrano, pasquale/F-7269-2012; Kuss,
Michael/H-8959-2012; Doro, Michele/F-9458-2012; giglietto,
nicola/I-8951-2012; Kovalev, Yuri/J-5671-2013; Funk, Stefan/B-7629-2015;
Pavlidou, Vasiliki/C-2944-2011; Antoranz, Pedro/H-5095-2015; Delgado,
Carlos/K-7587-2014; Nieto, Daniel/J-7250-2015; Kovalev,
Yuri/N-1053-2015; Pearson, Timothy/N-2376-2015; Loparco,
Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Johannesson,
Gudlaugur/O-8741-2015; Miranda, Jose Miguel/F-2913-2013
OI Becerra Gonzalez, Josefa/0000-0002-6729-9022; Dominguez,
Alberto/0000-0002-3433-4610; Bastieri, Denis/0000-0002-6954-8862;
Omodei, Nicola/0000-0002-5448-7577; Ribo, Marc/0000-0002-9931-4557;
Pesce-Rollins, Melissa/0000-0003-1790-8018; Giroletti,
Marcello/0000-0002-8657-8852; Perri, Matteo/0000-0003-3613-4409;
Angelakis, Emmanouil/0000-0001-7327-5441; Cesarini,
Andrea/0000-0002-8611-8610; leonardo, elvira/0000-0003-0271-7673;
Villata, Massimo/0000-0003-1743-6946; Fonseca Gonzalez, Maria
Victoria/0000-0003-2235-0725; Caraveo, Patrizia/0000-0003-2478-8018; De
Lotto, Barbara/0000-0003-3624-4480; Sgro', Carmelo/0000-0001-5676-6214;
SPINELLI, Paolo/0000-0001-6688-8864; Rando,
Riccardo/0000-0001-6992-818X; Persic, Massimo/0000-0003-1853-4900;
Spanier, Felix/0000-0001-6802-4744; Raiteri, Claudia
Maria/0000-0003-1784-2784; Ros, Eduardo/0000-0001-9503-4892; Cassaro,
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Moroni, Pier Giorgio/0000-0001-9712-9916; giommi,
paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517;
Frailis, Marco/0000-0002-7400-2135; Font, Lluis/0000-0003-2109-5961;
Moskalenko, Igor/0000-0001-6141-458X; Contreras Gonzalez, Jose
Luis/0000-0001-7282-2394; Mazziotta, Mario /0000-0001-9325-4672; Backes,
Michael/0000-0002-9326-6400; Torres, Diego/0000-0002-1522-9065;
Temnikov, Petar/0000-0002-9559-3384; Barrio, Juan/0000-0002-0965-0259;
Cortina, Juan/0000-0003-4576-0452; Larionov, Valeri/0000-0002-4640-4356;
Rico, Javier/0000-0003-4137-1134; Lopez Moya,
Marcos/0000-0002-8791-7908; GAug, Markus/0000-0001-8442-7877; Moralejo
Olaizola, Abelardo/0000-0002-1344-9080; Morselli,
Aldo/0000-0002-7704-9553; Braun, Isabel/0000-0002-9389-0502; Reimer,
Olaf/0000-0001-6953-1385; Thompson, David/0000-0001-5217-9135; lubrano,
pasquale/0000-0003-0221-4806; Doro, Michele/0000-0001-9104-3214;
giglietto, nicola/0000-0002-9021-2888; Bonnoli,
Giacomo/0000-0003-2464-9077; Stamerra, Antonio/0000-0002-9430-5264;
Prandini, Elisa/0000-0003-4502-9053; Kadler,
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Bordas, Pol/0000-0002-0266-8536; Cutini, Sara/0000-0002-1271-2924;
Paredes, Josep M./0000-0002-1566-9044; Oya, Igor/0000-0002-3881-9324;
Berenji, Bijan/0000-0002-4551-772X; Gasparrini,
Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793;
Baldini, Luca/0000-0002-9785-7726; Kovalev, Yuri/0000-0001-9303-3263;
Funk, Stefan/0000-0002-2012-0080; Pavlidou,
Vasiliki/0000-0002-0870-1368; Antoranz, Pedro/0000-0002-3015-3601;
Delgado, Carlos/0000-0002-7014-4101; Nieto, Daniel/0000-0003-3343-0755;
Pearson, Timothy/0000-0001-5213-6231; Loparco,
Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395;
Johannesson, Gudlaugur/0000-0003-1458-7036; Miranda, Jose
Miguel/0000-0002-1472-9690
FU Academy of Finland [212656, 210338]; Russian RFBR foundation
[09-02-00092]; RFBR [08-02-00545]; NASA [NNX08AW31G]; NSF [AST-0808050];
Smithsonian Institution; Academia Sinica; Georgian National Science
Foundation [GNSF/ST07/4-180]
FX We acknowledge the use of public data from the Swift and RXTE data
archives. The Metsahovi team acknowledges the support from the Academy
of Finland for the observing projects (numbers 212656, 210338, among
others). This research has made use of data obtained from the National
Radio Astronomy Observatory's Very Long Baseline Array (VLBA), projects
BK150, BP143, and BL149 (MOJAVE). The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc. The St.
Petersburg University team acknowledges support from the Russian RFBR
foundation via grant 09-02-00092. AZT-24 observations are made within an
agreement between Pulkovo, Rome and Teramo observatories. This research
is partly based on observations with the 100 m telescope of the MPIfR
(Max-Planck-Institut fur Radioastronomie) at Effelsberg, as well as with
the Medicina and Noto telescopes operated by INAF-Istituto di
Radioastronomia. RATAN-600 observations were supported in part by the
RFBR grant 08-02-00545 and the OVRO 40 m program was funded in part by
NASA (NNX08AW31G) and the NSF (AST-0808050). 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. M.
Villata organized the optical-to-radio observations by GASP-WEBT as the
president of the collaboration. The Abastumani Observatory team
acknowledges financial support by the Georgian National Science
Foundation through grant GNSF/ST07/4-180.
NR 102
TC 105
Z9 106
U1 1
U2 28
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 AUG 1
PY 2011
VL 736
IS 2
AR 131
DI 10.1088/0004-637X/736/2/131
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795MD
UT WOS:000292977400056
ER
PT J
AU An, D
Ramirez, SV
Sellgren, K
Arendt, RG
Boogert, ACA
Robitaille, TP
Schultheis, M
Cotera, AS
Smith, HA
Stolovy, SR
AF An, Deokkeun
Ramirez, Solange V.
Sellgren, Kris
Arendt, Richard G.
Boogert, A. C. Adwin
Robitaille, Thomas P.
Schultheis, Mathias
Cotera, Angela S.
Smith, Howard A.
Stolovy, Susan R.
TI MASSIVE YOUNG STELLAR OBJECTS IN THE GALACTIC CENTER. I. SPECTROSCOPIC
IDENTIFICATION FROM SPITZER INFRARED SPECTROGRAPH OBSERVATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: nucleus; infrared: ISM; ISM: molecules; stars: formation
ID 2-DIMENSIONAL RADIATIVE-TRANSFER; RECOMBINATION LINE OBSERVATIONS;
SPECTRAL ENERGY-DISTRIBUTIONS; DIFFUSE INTERSTELLAR-MEDIUM; CENTER
MOLECULAR CLOUDS; COMPACT RADIO-SOURCES; MU-M; CARBON-DIOXIDE;
STAR-FORMATION; MILKY-WAY
AB We present results from our spectroscopic study, using the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope, designed to identify massive young stellar objects (YSOs) in the Galactic center (GC). Our sample of 107 YSO candidates was selected based on Infrared Array Camera (IRAC) colors from the high spatial resolution, high sensitivity Spitzer/IRAC images in the Central Molecular Zone, which spans the central similar to 300 pc region of the Milky Way. We obtained IRS spectra over 5-35 mu m using both high- and low-resolution IRS modules. We spectroscopically identify massive YSOs by the presence of a 15.4 mu m shoulder on the absorption profile of 15 mu m CO2 ice, suggestive of CO2 ice mixed with CH3OH ice on grains. This 15.4 mu m shoulder is clearly observed in 16 sources and possibly observed in an additional 19 sources. We show that nine massive YSOs also reveal molecular gas-phase absorption from CO2, C2H2, and/or HCN, which traces warm and dense gas in YSOs. Our results provide the first spectroscopic census of the massive YSO population in the GC. We fit YSO models to the observed spectral energy distributions and find YSO masses of 8-23 M-circle dot, which generally agree with the masses derived from observed radio continuum emission. We find that about 50% of photometrically identified YSOs are confirmed with our spectroscopic study. This implies a preliminary star formation rate of similar to 0.07 M-circle dot yr(-1) at the GC.
C1 [An, Deokkeun] Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
[Ramirez, Solange V.; Boogert, A. C. Adwin] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
[Arendt, Richard G.] NASA, Goddard Space Flight Ctr, CRESST, UMBC,GSFC, Greenbelt, MD 20771 USA.
[Robitaille, Thomas P.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Schultheis, Mathias] Observ Besancon, F-25000 Besancon, France.
[Cotera, Angela S.] SETI Inst, Mountain View, CA 94043 USA.
[Stolovy, Susan R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA.
RP An, D (reprint author), Ewha Womans Univ, Dept Sci Educ, Seoul 120750, South Korea.
EM deokkeun@ewha.ac.kr
OI Arendt, Richard/0000-0001-8403-8548; Robitaille,
Thomas/0000-0002-8642-1329
FU NASA; Ministry of Education, Science, and Technology [2010-0025122]
FX We thank the referee for careful and detailed comments. 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. This research
has made use of the SIMBAD database, operated at CDS, Strasbourg,
France. This research was supported by the Basic Science Research
Program through the National Research Foundation of Korea (NRF) funded
by the Ministry of Education, Science, and Technology (No.
2010-0025122).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2011
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DI 10.1088/0004-637X/736/2/133
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
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UT WOS:000292977400058
ER
PT J
AU Hsieh, PY
Matsushita, S
Liu, GL
Ho, PTP
Oi, N
Wu, YL
AF Hsieh, Pei-Ying
Matsushita, Satoki
Liu, Guilin
Ho, Paul T. P.
Oi, Nagisa
Wu, Ya-Lin
TI PHYSICAL PROPERTIES OF THE CIRCUMNUCLEAR STARBURST RING IN THE BARRED
GALAXY NGC 1097
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 1097); galaxies: ISM; galaxies: Seyfert;
galaxies: starburst; radio lines: ISM; submillimeter: ISM
ID DENSE MOLECULAR GAS; STAR-FORMATION LAW; SPIRAL STRUCTURE; NUCLEAR
RINGS; SCHMIDT LAW; BLACK-HOLE; CLOUDS; NGC-1097; EMISSION; DISK
AB We report high-resolution (CO)-C-12(J = 2-1), (CO)-C-13(J = 2-1), and (CO)-C-12(J = 3-2) imaging of the Seyfert 1/starburst ring galaxy NGC 1097 with the Submillimeter Array for the purpose of studying the physical and kinematic properties of the 1 kpc circumnuclear starburst ring. Individual star clusters as detected in the Hubble Space Telescope map of Pa alpha line emission have been used to determine the star formation rate (SFR), and are compared with the properties of the molecular gas. The molecular ring has been resolved into individual clumps at the giant molecular cloud association (GMA) scale of 200-300 pc in all three CO lines. The intersection between the dust lanes and the starburst ring, which is associated with the orbit-crowding region, is resolved into two physically/kinematically distinct features in the 1.'' 5 x 1.'' 0 (105 x 70 pc) (CO)-C-12(J = 2-1) map. The clumps associated with the dust lanes have broader line widths, higher surface gas densities, and lower SFRs, while the narrow line clumps associated with the starburst ring have opposite characteristics. A Toomre-Q value lower than unity at the radius of the ring suggests that the molecular ring is gravitationally unstable to fragmentation at GMA scale. The line widths and surface density of the gas mass of the clumps show an azimuthal variation related to the large-scale dynamics. The SFR, on the other hand, is not significantly affected by the dynamics, but has a correlation with the intensity ratio of (CO)-C-12 (J = 3-2) and (CO)-C-12(J = 2-1), which traces the denser gas associated with star formation. Our resolved CO map, especially in the orbit-crowding region, observationally demonstrates for the first time that the physical/kinematic properties of GMAs are affected by the large-scale bar-potential dynamics in NGC 1097.
C1 [Hsieh, Pei-Ying] Natl Cent Univ, Inst Astrophys, Jhongli City 32001, Taoyuan County, Peoples R China.
[Hsieh, Pei-Ying; Matsushita, Satoki; Ho, Paul T. P.; Wu, Ya-Lin] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Matsushita, Satoki] Joint ALMA Off, Santiago 7630355, Chile.
[Liu, Guilin] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Oi, Nagisa] Grad Univ Adv Studies, Sch Sci, Dept Astron, Tokyo 1818588, Japan.
[Wu, Ya-Lin] Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan.
RP Hsieh, PY (reprint author), Natl Cent Univ, Inst Astrophys, 300 Jhongda Rd, Jhongli City 32001, Taoyuan County, Peoples R China.
EM pyhsieh@asiaa.sinica.edu.tw
FU NSC [97-2112-M-001-007-MY3, 97-2112-M-001-021-MY3]
FX We thank the SMA staff for maintaining the operation of the array. We
thank the anonymous referee for a careful reading and detailed comments
that improved the manuscript. We thank G. Petitpas for providing the
JCMT data. P.-Y. Hsieh especially acknowledges the fruitful discussions
with L.-H. Lin, K. Sakamoto, N. Scoville, W. Maciejewski, and L. Ho on
the manuscript. This project is funded by NSC 97-2112-M-001-007-MY3 and
NSC 97-2112-M-001-021-MY3.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
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DI 10.1088/0004-637X/736/2/129
PG 17
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SC Astronomy & Astrophysics
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UT WOS:000292977400054
ER
PT J
AU Koposov, SE
Gilmore, G
Walker, MG
Belokurov, V
Evans, NW
Fellhauer, M
Gieren, W
Geisler, D
Monaco, L
Norris, JE
Okamoto, S
Penarrubia, J
Wilkinson, M
Wyse, RFG
Zucker, DB
AF Koposov, Sergey E.
Gilmore, G.
Walker, M. G.
Belokurov, V.
Evans, N. Wyn
Fellhauer, M.
Gieren, W.
Geisler, D.
Monaco, L.
Norris, J. E.
Okamoto, S.
Penarrubia, J.
Wilkinson, M.
Wyse, R. F. G.
Zucker, D. B.
TI ACCURATE STELLAR KINEMATICS AT FAINT MAGNITUDES: APPLICATION TO THE
BOOTES I DWARF SPHEROIDAL GALAXY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: individual (Bootes I); galaxies: kinematics
and dynamics; methods: data analysis; techniques: radial velocities
ID MILKY-WAY SATELLITES; SIGHT VELOCITY DISTRIBUTIONS; ABSORPTION-LINE
SPECTRA; FINE-STRUCTURE CONSTANT; DIGITAL SKY SURVEY; DARK-MATTER;
LUMINOSITY FUNCTION; LOCAL GROUP; GALACTIC SATELLITES; GIANT STARS
AB We develop, implement, and characterize an enhanced data reduction approach which delivers precise, accurate, radial velocities from moderate resolution spectroscopy with the fiber-fed VLT/FLAMES+GIRAFFE facility. This facility, with appropriate care, delivers radial velocities adequate to resolve the intrinsic velocity dispersions of the very faint dwarf spheroidal (dSph) galaxies. Importantly, repeated measurements let us reliably calibrate our individual velocity errors (0.2 km s(-1) <= delta(V) <= 5 km s(-1)) and directly detect stars with variable radial velocities. We show, by application to the Bootes I dSph, that the intrinsic velocity dispersion of this system is significantly below 6.5 km s(-1) reported by previous studies. Our data favor a two-population model of Bootes I, consisting of a majority "cold" stellar component, with velocity dispersion 2.4(-0.5)(+0.9) km s(-1), and a minority "hot" stellar component, with velocity dispersion similar to 9 km s(-1), although we cannot completely rule out a single component distribution with velocity dispersion 4.6(-0.6)(0.8) km s(-1). We speculate that this complex velocity distribution actually reflects the distribution of velocity anisotropy in Bootes I, which is a measure of its formation processes.
C1 [Koposov, Sergey E.; Gilmore, G.; Walker, M. G.; Belokurov, V.; Evans, N. Wyn; Okamoto, S.; Penarrubia, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Koposov, Sergey E.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia.
[Walker, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fellhauer, M.; Gieren, W.; Geisler, D.; Monaco, L.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Monaco, L.] European So Observ, Santiago 19, Chile.
[Norris, J. E.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Wilkinson, M.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Wyse, R. F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Zucker, D. B.] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia.
[Zucker, D. B.] Australian Astron Observ, Epping, NSW 1710, Australia.
RP Koposov, SE (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RI Koposov, Sergey/F-2754-2012; Walker, Matthew/P-1777-2014
OI Koposov, Sergey/0000-0003-2644-135X; Walker, Matthew/0000-0003-2496-1925
FU Chilean Center for Astrophysics FONDAP [15010003]; BASAL Center for
Astrophysics and Associated Technologies CATA [PFB-06/2007]; NASA
[HST-HF-51283]; Space Telescope Science Institute; [NAS 5-26555]
FX We thank Michael Siegel and Ricardo Munoz for providing us with their
photometric variability and kinematic data for Bootes I. Most of the
data processing has been done using the python programming language and
the following open source modules: numpy,11
scipy,12 matplotlib,13 pypar,14
ipython15 (Perez & Granger 2007), astrolibpy,16
and pyfits17 (pyfits is a product of the Space Telescope
Science Institute, which is operated by AURA for NASA). This research
has also made use of NASA's Astrophysics Data System Bibliographic
Services and TOPCAT software18 (Taylor 2005). W. G., D. G.,
and M. F. gratefully acknowledge financial support for this work from
the Chilean Center for Astrophysics FONDAP 15010003, and from the BASAL
Center for Astrophysics and Associated Technologies CATA under grant
PFB-06/2007. M. G. W. is supported by NASA through Hubble Fellowship
grant HST-HF-51283, 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. The data in this
study were obtained in ESO Program 182.B-0372A (PI; G. Gilmore).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2011
VL 736
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AR 146
DI 10.1088/0004-637X/736/2/146
PG 17
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SC Astronomy & Astrophysics
GA 795MD
UT WOS:000292977400071
ER
PT J
AU Paolillo, M
Puzia, TH
Goudfrooij, P
Zepf, SE
Maccarone, TJ
Kundu, A
Fabbiano, G
Angelini, L
AF Paolillo, Maurizio
Puzia, Thomas H.
Goudfrooij, Paul
Zepf, Stephen E.
Maccarone, Thomas J.
Kundu, Arunav
Fabbiano, Giuseppina
Angelini, Lorella
TI PROBING THE GC-LMXB CONNECTION IN NGC 1399: A WIDE-FIELD STUDY WITH THE
HUBBLE SPACE TELESCOPE AND CHANDRA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC
1399); galaxies: star clusters: general; X-rays: binaries; X-rays:
galaxies; X-rays: individual (NGC 1399)
ID X-RAY BINARIES; GLOBULAR-CLUSTER SYSTEM; EARLY-TYPE GALAXIES; ELLIPTIC
GALAXIES; LUMINOSITY FUNCTION; STAR-CLUSTERS; FORNAX; NGC-1399; CAMERA;
SPECTROSCOPY
AB We present a wide-field study of the globular cluster (GC)/low-mass X-ray binary (LMXB) connection in the giant elliptical NGC 1399. The large field of view of the Advanced Camera for Surveys/WFC, combined with Hubble Space Telescope and Chandra high resolution, allow us to constrain the LMXB formation scenarios in elliptical galaxies. We confirm that NGC 1399 has the highest LMXB fraction in GCs of all nearby elliptical galaxies studied so far, even though the exact value depends on galactocentric distance due to the interplay of a differential GC versus galaxy light distribution and the GC color dependence. In fact, LMXBs are preferentially hosted by bright, red GCs out to > 5R(eff) of the galaxy light. The finding that GCs hosting LMXBs follow the radial distribution of their parent GC population argues against the hypothesis that the external dynamical influence of the galaxy affects the LMXB formation in GCs. On the other hand, field-LMXBs closely match the host galaxy light, thus indicating that they are originally formed in situ and not inside GCs. We measure GC structural parameters, finding that the LMXB formation likelihood is influenced independently by mass, metallicity, and GC structural parameters. In particular, the GC central density plays a major role in predicting which GCs host accreting binaries. Finally, our analysis shows that LMXBs in GCs are marginally brighter than those in the field, and in particular the only color-confirmed GC with L-X > 10(39) erg s(-1) shows no variability, which may indicate a superposition of multiple LMXBs in these systems.
C1 [Paolillo, Maurizio] Univ Naples Federico II, Dept Phys Sci, I-80126 Naples, Italy.
[Paolillo, Maurizio] Ist Nazl Fis Nucl, Napoli Unit, Dept Phys Sci, I-80126 Naples, Italy.
[Puzia, Thomas H.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada.
[Puzia, Thomas H.] Pontificia Univ Catolica Chile, Dept Astron & Astrophys, Santiago, Chile.
[Goudfrooij, Paul] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[Maccarone, Thomas J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Kundu, Arunav] Eureka Sci, Oakland, CA 94602 USA.
[Fabbiano, Giuseppina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Angelini, Lorella] NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Paolillo, M (reprint author), Univ Naples Federico II, Dept Phys Sci, I-80126 Naples, Italy.
EM paolillo@na.infn.it
RI Paolillo, Maurizio/J-1733-2012
OI Paolillo, Maurizio/0000-0003-4210-7693
FU Herzberg Institute of Astrophysics of the National Research Council of
Canada; ASI-INAF [I/009/10/0]; HST [HST-AR-11264]; NASA [NNX08AJ60G,
NAS5-26555]; Space Telescope Science Institute [GO-10129]
FX We thank E. Flaccomio, A. Zezas for useful suggestions and comments, and
T. Richtler for providing access to his ground-based photometric
catalogs. T. H. P. acknowledges financial support in form of the
Plaskett Research Fellowship at the Herzberg Institute of Astrophysics
of the National Research Council of Canada. He is also grateful for the
support and warm hospitality at the Federico II University of Naples
where parts of this work were conducted. We thank the anonymous referee
for many useful suggestions. M. P. acknowledges support from the
ASI-INAF contract I/009/10/0.; A. K. acknowledges support from HST
archival program HST-AR-11264. S.E.Z. acknowledges support for this work
from the NASA ADP grant NNX08AJ60G.; Support for HST Program GO-10129
was provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS5-26555.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2011
VL 736
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AR 90
DI 10.1088/0004-637X/736/2/90
PG 16
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SC Astronomy & Astrophysics
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UT WOS:000292977400015
ER
PT J
AU Ragan, SE
Bergin, EA
Wilner, D
AF Ragan, Sarah E.
Bergin, Edwin A.
Wilner, David
TI VERY LARGE ARRAY OBSERVATIONS OF AMMONIA IN INFRARED-DARK CLOUDS. I.
COLUMN DENSITY AND TEMPERATURE STRUCTURE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy: structure; ISM: abundances; ISM: clouds; radio lines: ISM;
stars: formation; techniques: interferometric; techniques: spectroscopic
ID MASS STAR-FORMATION; GALACTIC DISTRIBUTION; INITIAL CONDITIONS;
MOLECULAR CLOUDS; NH3 OBSERVATIONS; CORES; PRECURSORS; REGIONS; ORION;
INTERMEDIATE
AB We present Very Large Array observations of NH3 (1,1) and (2,2) in a sample of six infrared-dark clouds (IRDCs) with distances from 2 to 5 kpc. We find that ammonia serves as an excellent tracer of dense gas in IRDCs, showing no evidence of depletion, and the average abundance in these clouds is 8.1 x 10(-7). Our sample consists of four IRDCs with 24 mu m embedded protostars and two that appear starless. We calculate the kinetic temperature of the gas in IRDCs and find no significant difference between starless and star-forming IRDCs. We find that the bulk of the gas is between 8 and 13 K, indicating that any embedded or nearby stars or clusters do not affect the gas temperature dramatically. Though IRDCs have temperatures and volume densities on par with local star formation regions of lower mass, they consist of much more mass which induces very high internal pressures. In order for IRDCs to survive as coherent structures, the internal pressure must be balanced by a confining pressure provided by the high concentration of molecular clouds in the spiral arm in which they reside. The high molecular concentration and pressure are roughly consistent with gas dynamics of a bar galaxy.
C1 [Ragan, Sarah E.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Ragan, Sarah E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ragan, SE (reprint author), Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA.
OI Ragan, Sarah/0000-0003-4164-5588
FU National Science Foundation [0707777]
FX We thank the anonymous referee for a detailed review of the manuscript
and whose comments significantly improved this paper. S. R. is grateful
to Claire Chandler, Rachel Friesen, and John Monnier for help with data
reduction, and to Henrik Beuther and Paul Clark for useful discussions.
This work was supported by the National Science Foundation under Grant
0707777.
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SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2011
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DI 10.1088/0004-637X/736/2/163
PG 10
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SC Astronomy & Astrophysics
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UT WOS:000292977400088
ER
PT J
AU Arnold, JA
Romanowsky, AJ
Brodie, JP
Chomiuk, L
Spitler, LR
Strader, J
Benson, AJ
Forbes, DA
AF Arnold, Jacob A.
Romanowsky, Aaron J.
Brodie, Jean P.
Chomiuk, Laura
Spitler, Lee R.
Strader, Jay
Benson, Andrew J.
Forbes, Duncan A.
TI THE FOSSIL RECORD OF TWO-PHASE GALAXY ASSEMBLY: KINEMATICS AND
METALLICITIES IN THE NEAREST S0 GALAXY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: bulges; galaxies: formation; galaxies: halos; galaxies:
individual (NGC 3115); galaxies: kinematics and dynamics; globular
clusters: general
ID GLOBULAR-CLUSTER SYSTEMS; SIGHT VELOCITY DISTRIBUTIONS; ELLIPTIC
GALAXIES; PLANETARY-NEBULAE; MERGER REMNANTS; MINOR MERGERS; STELLAR
POPULATIONS; VLT SPECTROSCOPY; SIZE EVOLUTION; DISK GALAXIES
AB We present a global analysis of kinematics and metallicity in the nearest S0 galaxy, NGC 3115, along with implications for its assembly history. The data include high-quality wide-field imaging from Suprime-Cam on the Subaru telescope, and multi-slit spectra of the field stars and globular clusters (GCs) obtained using Keck-DEIMOS/LRIS and Magellan-IMACS. Within two effective radii, the bulge (as traced by the stars and metal-rich GCs) is flattened and rotates rapidly (v/sigma greater than or similar to 1.5). At larger radii, the rotation declines dramatically to v/sigma similar to 0.7, but remains well aligned with the inner regions. The radial decrease in characteristic metallicity of both the metal-rich and metal-poor GC subpopulations produces strong gradients with power-law slopes of -0.17 +/- 0.04 and -0.38 +/- 0.06 dex dex(-1), respectively. We argue that this pattern is not naturally explained by a binary major merger, but instead by a two-phase assembly process where the inner regions have formed in an early violent, dissipative phase, followed by the protracted growth of the outer parts via minor mergers with typical mass ratios of similar to 15-20:1.
C1 [Arnold, Jacob A.; Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
[Chomiuk, Laura; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA.
[Spitler, Lee R.; Forbes, Duncan A.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
[Benson, Andrew J.] CALTECH, Pasadena, CA 91125 USA.
RP Arnold, JA (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA.
RI Spitler, Lee/A-9867-2013
OI Spitler, Lee/0000-0001-5185-9876
FU W. M. Keck Foundation; National Science Foundation [AST-0808099,
AST-0909237]; UCSC University Affiliated Research Center; FONDAP Center
for Astrophysics CONICYT [15010003]; Gordon and Betty Moore Foundation;
Australian Government
FX We thank Andi Burkert, Avishai Dekel, Loren Hoffman, Chris Moody, and
Joel Primack for useful discussions, the referee Igor Chilingarian for
helpful comments, and Ewan O'Sullivan for contributing observing time.
Based in part on data collected at Subaru Telescope (operated by the
National Astronomical Observatory of Japan) via a Gemini Observatory
time exchange (GN-2008A-C-12), and also the 6.5 m Magellan Telescopes
located at Las Campanas Observatory, Chile. Some of the data presented
herein were obtained at the W. M. Keck Observatory, operated as a
scientific partnership among the California Institute of Technology, the
University of California and the National Aeronautics and Space
Administration, and made possible by the generous financial support of
the W. M. Keck Foundation. This material is based upon work supported by
the National Science Foundation under Grants AST-0808099 and AST-0909237
and a Graduate Research Fellowship, and also by the UCSC University
Affiliated Research Center's Aligned Research Program. A.J.R. was
further supported by the FONDAP Center for Astrophysics CONICYT
15010003. A.J.B. acknowledges the support of the Gordon and Betty Moore
Foundation. L. C. is a Jansky Fellow at 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. We acknowledge financial support from the
Access to Major Research Facilities Programme, a component of the
International Science Linkages Programme established under the
Australian Government's innovation statement, Backing Australia's
Ability.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2011
VL 736
IS 2
AR L26
DI 10.1088/2041-8205/736/2/L26
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OZ
UT WOS:000293138500003
ER
PT J
AU Kaltenegger, L
Sasselov, D
AF Kaltenegger, L.
Sasselov, D.
TI EXPLORING THE HABITABLE ZONE FOR KEPLER PLANETARY CANDIDATES
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE astrobiology; atmospheric effects; Earth; methods: data analysis;
planets and satellites: general; stars: individual (Kepler)
ID MAIN-SEQUENCE STARS; CLIMATE; CONSTRAINTS; ATMOSPHERE; GLIESE-581;
EXOPLANETS; EARTHS; LIFE
AB This Letter outlines a simple approach to evaluate habitability of terrestrial planets by assuming different types of planetary atmospheres and using corresponding model calculations. Our approach can be applied for current and future candidates provided by the Kepler mission and other searches. The resulting uncertainties and changes in the number of planetary candidates in the HZ for the Kepler 2011 February data release are discussed. To first order, the HZ depends on the effective stellar flux distribution in wavelength and time, the planet albedo, and greenhouse gas effects. We provide a simple set of parameters which can be used for evaluating future planet candidates from transit searches.
C1 [Kaltenegger, L.] MPIA, D-69117 Heidelberg, Germany.
[Kaltenegger, L.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kaltenegger, L (reprint author), MPIA, Koenigstuhl 17, D-69117 Heidelberg, Germany.
EM lkaltene@cfa.harvard.edu
FU NAI; DFG [ENP Ka 3142/1-1]
FX We are grateful to Jim Kasting and Franck Selsis for comments and
discussion. L.K. acknowledges support from NAI and DFG funding ENP Ka
3142/1-1.
NR 24
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2011
VL 736
IS 2
AR L25
DI 10.1088/2041-8205/736/2/L25
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OZ
UT WOS:000293138500002
ER
PT J
AU Vercellone, S
Striani, E
Vittorini, V
Donnarumma, I
Pacciani, L
Pucella, G
Tavani, M
Raiteri, CM
Villata, M
Romano, P
Fiocchi, M
Bazzano, A
Bianchin, V
Ferrigno, C
Maraschi, L
Pian, E
Turler, M
Ubertini, P
Bulgarelli, A
Chen, AW
Giuliani, A
Longo, F
Barbiellini, G
Cardillo, M
Cattaneo, PW
Del Monte, E
Evangelista, Y
Feroci, M
Ferrari, A
Fuschino, F
Gianotti, F
Giusti, M
Lazzarotto, F
Pellizzoni, A
Piano, G
Pilia, M
Rapisarda, M
Rappoldi, A
Sabatini, S
Soffitta, P
Trifoglio, M
Trois, A
Giommi, P
Lucarelli, F
Pittori, C
Santolamazza, P
Verrecchia, F
Agudo, I
Aller, HD
Aller, MF
Arkharov, AA
Bach, U
Berdyugin, A
Borman, GA
Chigladze, R
Efimov, YS
Efimova, NV
Gomez, JL
Gurwell, MA
McHardy, IM
Joshi, M
Kimeridze, GN
Krajci, T
Kurtanidze, OM
Kurtanidze, SO
Larionov, VM
Lindfors, E
Molina, SN
Morozova, DA
Nazarov, SV
Nikolashvili, MG
Nilsson, K
Pasanen, M
Reinthal, R
Ros, JA
Sadun, AC
Sakamoto, T
Sallum, S
Sergeev, SG
Schwartz, RD
Sigua, LA
Sillanpaa, A
Sokolovsky, KV
Strelnitski, V
Takalo, L
Taylor, B
Walker, G
AF Vercellone, S.
Striani, E.
Vittorini, V.
Donnarumma, I.
Pacciani, L.
Pucella, G.
Tavani, M.
Raiteri, C. M.
Villata, M.
Romano, P.
Fiocchi, M.
Bazzano, A.
Bianchin, V.
Ferrigno, C.
Maraschi, L.
Pian, E.
Tuerler, M.
Ubertini, P.
Bulgarelli, A.
Chen, A. W.
Giuliani, A.
Longo, F.
Barbiellini, G.
Cardillo, M.
Cattaneo, P. W.
Del Monte, E.
Evangelista, Y.
Feroci, M.
Ferrari, A.
Fuschino, F.
Gianotti, F.
Giusti, M.
Lazzarotto, F.
Pellizzoni, A.
Piano, G.
Pilia, M.
Rapisarda, M.
Rappoldi, A.
Sabatini, S.
Soffitta, P.
Trifoglio, M.
Trois, A.
Giommi, P.
Lucarelli, F.
Pittori, C.
Santolamazza, P.
Verrecchia, F.
Agudo, I.
Aller, H. D.
Aller, M. F.
Arkharov, A. A.
Bach, U.
Berdyugin, A.
Borman, G. A.
Chigladze, R.
Efimov, Yu S.
Efimova, N. V.
Gomez, J. L.
Gurwell, M. A.
McHardy, I. M.
Joshi, M.
Kimeridze, G. N.
Krajci, T.
Kurtanidze, O. M.
Kurtanidze, S. O.
Larionov, V. M.
Lindfors, E.
Molina, S. N.
Morozova, D. A.
Nazarov, S. V.
Nikolashvili, M. G.
Nilsson, K.
Pasanen, M.
Reinthal, R.
Ros, J. A.
Sadun, A. C.
Sakamoto, T.
Sallum, S.
Sergeev, S. G.
Schwartz, R. D.
Sigua, L. A.
Sillanpaa, A.
Sokolovsky, K. V.
Strelnitski, V.
Takalo, L.
Taylor, B.
Walker, G.
TI THE BRIGHTEST GAMMA-RAY FLARING BLAZAR IN THE SKY: AGILE AND
MULTI-WAVELENGTH OBSERVATIONS OF 3C 454.3 DURING 2010 NOVEMBER
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: jets; radiation mechanisms: non-thermal;
quasars: general; quasars: individual (3C 454.3)
ID CRAZY-DIAMOND; WEBT; OUTBURST; CAMPAIGN; 3C-454.3; TELESCOPE; SPECTRUM;
RADIO; PHASE; POWER
AB Since 2005, the blazar 3C 454.3 has shown remarkable flaring activity at all frequencies, and during the last four years it has exhibited more than one gamma-ray flare per year, becoming the most active gamma-ray blazar in the sky. We present for the first time the multi-wavelength AGILE, Swift, INTEGRAL, and GASP-WEBT data collected in order to explain the extraordinary gamma-ray flare of 3C 454.3 which occurred in 2010 November. On 2010 November 20 (MJD 55520), 3C 454.3 reached a peak flux (E > 100 MeV) of F(gamma)(p) = (6.8 +/- 1.0) x 10(-5) photons cm(-2) s(-1) on a timescale of about 12 hr, more than a factor of six higher than the flux of the brightest steady gamma-ray source, the Vela pulsar, and more than a factor of three brighter than its previous super-flare on 2009 December 2-3. The multi-wavelength data make possible a thorough study of the present event: the comparison with the previous outbursts indicates a close similarity to the one that occurred in 2009. By comparing the broadband emission before, during, and after the gamma-ray flare, we find that the radio, optical, and X-ray emission varies within a factor of 2-3, whereas the gamma-ray flux by a factor of 10. This remarkable behavior is modeled by an external Compton component driven by a substantial local enhancement of soft seed photons.
C1 [Striani, E.; Tavani, M.; Cardillo, M.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy.
[Striani, E.; Tavani, M.] INFN Roma Tor Vergata, I-00133 Rome, Italy.
[Vittorini, V.; Donnarumma, I.; Pacciani, L.; Tavani, M.; Fiocchi, M.; Bazzano, A.; Ubertini, P.; Cardillo, M.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Giusti, M.; Lazzarotto, F.; Piano, G.; Sabatini, S.; Soffitta, P.] INAF IASF Roma, I-00133 Rome, Italy.
[Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy.
[Tavani, M.; Ferrari, A.] CIFS Torino, I-10133 Turin, Italy.
[Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Bianchin, V.; Bulgarelli, A.; Fuschino, F.; Gianotti, F.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Ferrigno, C.; Tuerler, M.] Univ Geneva, ISDC, CH-1290 Versoix, Switzerland.
[Maraschi, L.] Osserv Astron Brera, INAF, I-23807 Merate, Italy.
[Pian, E.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy.
[Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy.
[Pian, E.] ESO, D-85748 Garching, Germany.
[Chen, A. W.; Giuliani, A.] INAF IASF Milano, I-20133 Milan, Italy.
[Longo, F.; Barbiellini, G.] Ist Nazl Fis Nucl, I-34127 Trieste, Italy.
[Longo, F.; Barbiellini, G.] Dipartimento Fis, I-34127 Trieste, Italy.
[Cattaneo, P. W.; Rappoldi, A.] Ist Nazl Fis Nucl, I-27100 Pavia, Italy.
[Ferrari, A.] Univ Turin, Dipartimento Fis Gen, I-10125 Turin, Italy.
[Pellizzoni, A.; Pilia, M.; Trois, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, Italy.
[Pilia, M.] Univ Insubria, Dipartimento Fis, I-22100 Como, Italy.
[Giommi, P.; Lucarelli, F.; Pittori, C.; Santolamazza, P.; Verrecchia, F.] ASI ASDC, I-00044 Rome, Italy.
[Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Agudo, I.; Joshi, M.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Arkharov, A. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg, Russia.
[Bach, U.; Sokolovsky, K. V.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Berdyugin, A.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland.
[Borman, G. A.; Efimov, Yu S.; Nazarov, S. V.; Sergeev, S. G.] Crimean Astrophys Observ, UA-98049 Nauchnyi, Crimea, Ukraine.
[Chigladze, R.; Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia.
[Efimova, N. V.; Larionov, V. M.; Morozova, D. A.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McHardy, I. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Krajci, T.] Astrokolkhoz Observ, Cloudcroft, NM 88317 USA.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FIN-21500 Piikkio, Finland.
[Ros, J. A.] Agrupacio Astron Sabadell, Sabadell, Spain.
[Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO 80217 USA.
[Sakamoto, T.] NASA, GSFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA.
[Sallum, S.; Strelnitski, V.; Walker, G.] Maria Mitchell Observ, Nantucket, MA 02554 USA.
[Sallum, S.] MIT, Cambridge, MA 02139 USA.
[Schwartz, R. D.] Galaxy View Observ, Sequim, WA 98382 USA.
[Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Vercellone, S.; Romano, P.] INAF IASF Palermo, I-90146 Palermo, Italy.
RP Vercellone, S (reprint author), INAF IASF Palermo, Via Ugo La Malfa 153, I-90146 Palermo, Italy.
EM stefano.vercellone@iasf-palermo.inaf.it
RI Morozova, Daria/H-1298-2013; Ferrigno, Carlo/H-4139-2012; Pittori,
Carlotta/C-7710-2016; Lazzarotto, Francesco/J-4670-2012; Larionov,
Valeri/H-1349-2013; Efimova, Natalia/I-2196-2013; Kurtanidze,
Omar/J-6237-2014; Sokolovsky, Kirill/D-2246-2015; Trifoglio,
Massimo/F-5302-2015; Molina, Sol Natalia/F-9968-2015; Agudo,
Ivan/G-1701-2015;
OI Morozova, Daria/0000-0002-9407-7804; Pittori,
Carlotta/0000-0001-6661-9779; Villata, Massimo/0000-0003-1743-6946;
Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Larionov,
Valeri/0000-0002-4640-4356; Efimova, Natalia/0000-0002-8071-4753;
Sokolovsky, Kirill/0000-0001-5991-6863; Trifoglio,
Massimo/0000-0002-2505-3630; Molina, Sol Natalia/0000-0002-4112-2157;
Agudo, Ivan/0000-0002-3777-6182; Bulgarelli, Andrea/0000-0001-6347-0649;
Pacciani, Luigi/0000-0001-6897-5996; Cardillo,
Martina/0000-0001-8877-3996; giommi, paolo/0000-0002-2265-5003; trois,
alessio/0000-0002-3180-6002; Feroci, Marco/0000-0002-7617-3421;
Soffitta, Paolo/0000-0002-7781-4104; Fuschino,
Fabio/0000-0003-2139-3299; Lucarelli, Fabrizio/0000-0002-6311-764X;
Pian, Elena/0000-0001-8646-4858; Verrecchia,
Francesco/0000-0003-3455-5082; Gianotti, Fulvio/0000-0003-4666-119X;
Lazzarotto, Francesco/0000-0003-4871-4072; Donnarumma,
Immacolata/0000-0002-4700-4549; Sabatini, Sabina/0000-0003-2076-5767;
Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia
Maria/0000-0003-1784-2784; Fiocchi, Mariateresa/0000-0001-5697-6019;
Tavani, Marco/0000-0003-2893-1459
FU ASI-INAF [I/009/10/0]; RFBR [09-02-00092]; MICIIN [AYA2010-14844]; CEIC
[P09-FQM-4784]; NSF [AST-0907893]; NASA [NNX08AV65G, NNX10AU15G];
NSF/REU [AST-0851892]; Nantucket Maria Mitchell Association; ASI
[I/089/06/2]; [GNSF/ST08/4-404]
FX We thank the referee for useful comments. We thank A. P. Marscher and S.
G. Jorstad for Perkins and Liverpool Telescopes optical data. We
acknowledge financial contribution from agreement ASI-INAF I/009/10/0,
ASI contract I/089/06/2, RFBR Foundation grant 09-02-00092, MICIIN grant
AYA2010-14844, CEIC grant P09-FQM-4784, NSF grant AST-0907893, NASA
Fermi GI grants NNX08AV65G and NNX10AU15G, NSF/REU grant AST-0851892,
the Nantucket Maria Mitchell Association, and grant GNSF/ST08/4-404.
NR 36
TC 35
Z9 35
U1 0
U2 12
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD AUG 1
PY 2011
VL 736
IS 2
AR L38
DI 10.1088/2041-8205/736/2/L38
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OZ
UT WOS:000293138500015
ER
PT J
AU McDade, LA
Maddison, DR
Guralnick, R
Piwowar, HA
Jameson, ML
Helgen, KM
Herendeen, PS
Hill, A
Vis, ML
AF McDade, Lucinda A.
Maddison, David R.
Guralnick, Robert
Piwowar, Heather A.
Jameson, Mary Liz
Helgen, Kristofer M.
Herendeen, Patrick S.
Hill, Andrew
Vis, Morgan L.
TI Biology Needs a Modern Assessment System for Professional Productivity
SO BIOSCIENCE
LA English
DT Article
DE academic assessment; systematic biology; scientific productivity;
digital objects; curation of natural history collections
ID DATA-PUBLISHING FRAMEWORK; BIODIVERSITY; IMPACT; INDEX; PUBLICATION;
TAXONOMY
AB Stimulated in large part by the advent of the Internet, research productivity in many academic disciplines has changed dramatically over the last two decades. However, the assessment system that governs professional success has not kept pace, creating a mismatch between modes of scholarly productivity and academic assessment criteria. In this article, we describe the problem and present ideas for solutions. We argue that adjusting assessment criteria to correspond to modern scholarly productivity is essential for the success of individual scientists and of our discipline as a whole. The authors and endorsers of this article commit to a number of actions that constitute steps toward ensuring that all forms of scholarly productivity are credited. The emphasis here is on systematic biology, but we are not alone in experiencing this mismatch between productivity and assessment. An additional goal in this article is to begin a conversation about the problem with colleagues in other subdisciplines of biology.
C1 [McDade, Lucinda A.] Rancho Santa Ana Bot Garden, Claremont, CA USA.
[McDade, Lucinda A.] Claremont Grad Univ, Claremont, CA USA.
[Maddison, David R.] Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA.
[Guralnick, Robert] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA.
[Piwowar, Heather A.] Natl Evolutionary Synth Ctr, Durham, NC USA.
[Jameson, Mary Liz] Wichita State Univ, Dept Biol Sci, Wichita, KS 67208 USA.
[Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Herendeen, Patrick S.] Chicago Bot Garden, Glencoe, IL USA.
[Hill, Andrew] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA.
[Vis, Morgan L.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA.
RP McDade, LA (reprint author), Rancho Santa Ana Bot Garden, Claremont, CA USA.
EM lucinda.mcdade@cgu.edu
OI Piwowar, Heather/0000-0003-1613-5981
FU National Science Foundation [DEB-0935231]
FX We are grateful to the participants who attended the four workshops on
the future of systematics and biodiversity research at which these ideas
were developed and discussed. Vicki Funk, John Lundberg, John Oswald, A.
Townsend Peterson, L. Alan Prather, Nathan Sheffield, and Erin Tripp
provided especially valuable input on earlier drafts of the manuscript.
The Chicago Botanic Garden; the National Center for Evolutionary
Synthesis (Durham, North Carolina); California State University at Long
Beach; and the National Museum of Natural History, Smithsonian
Institution, hosted these workshops, which were supported by a grant
from the National Science Foundation (DEB-0935231).
NR 35
TC 18
Z9 18
U1 0
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 AUG
PY 2011
VL 61
IS 8
BP 619
EP 625
DI 10.1525/bio.2011.61.8.8
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 806JQ
UT WOS:000293804100010
ER
PT J
AU Gingerich, O
AF Gingerich, Owen
TI The Zodiac of Paris: How an Improbable Controversy over an Ancient
Egyptian Artifact Provoked a Modern Debate between Religion and Science
SO JOURNAL FOR THE HISTORY OF ASTRONOMY
LA English
DT Book Review
C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM ginger@cfa.harvard.edu
NR 1
TC 0
Z9 0
U1 0
U2 1
PU SCIENCE HISTORY PUBLICATIONS LTD
PI CAMBRIDGE
PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND
SN 0021-8286
J9 J HIST ASTRON
JI J. Hist. Astron.
PD AUG
PY 2011
VL 42
BP 418
EP 419
PN 3
PG 2
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 805KL
UT WOS:000293725200014
ER
PT J
AU Capogrosso-Sansone, B
Guglielmino, M
Penna, V
AF Capogrosso-Sansone, B.
Guglielmino, M.
Penna, V.
TI Mott-insulator-SF transition lobe in the presence of a second superfluid
component
SO LASER PHYSICS
LA English
DT Article
ID BOSE-FERMI MIXTURES; OPTICAL LATTICES; PHYSICS; GASES; ATOMS
AB A two-component bosonic mixture loaded in a two-dimensional optical lattice is analyzed. By means of Mean-Field techniques and Worm algorithm Monte Carlo simulations, we study the effect of the presence of a second minority superfluid component on the first Mott lobe. We observe a reduction of the latter and different renormalization of the two boundaries. Our results are of interest for current experimental setups.
C1 [Capogrosso-Sansone, B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
[Guglielmino, M.; Penna, V.] Politecn Torino, Dipartimento Fis, I-10129 Turin, Italy.
[Penna, V.] Politecn Torino, CNISM Unita Ric, I-10129 Turin, Italy.
RP Capogrosso-Sansone, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA.
EM marco.guglielmino@polito.it
FU Insitute for Atomic, Molecular, and Optical Physics (ITAMP)
FX B. Capogrosso-Sansone (BCS) would like to thank D. Schneble, D. Pertot,
B. Gadway, N. Prokof'ev, and L. Pollet for interesting discussion. V.
Penna would like to thank E. Zaremba and M. Rigol for stimulating
comments on the application of mean-field techniques. The work of BCS
was supported by the Insitute for Atomic, Molecular, and Optical Physics
(ITAMP).
NR 32
TC 5
Z9 5
U1 4
U2 4
PU MAIK NAUKA/INTERPERIODICA/SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013-1578 USA
SN 1054-660X
J9 LASER PHYS
JI Laser Phys.
PD AUG
PY 2011
VL 21
IS 8
BP 1443
EP 1447
DI 10.1134/S1054660X11150023
PG 5
WC Optics; Physics, Applied
SC Optics; Physics
GA 804JS
UT WOS:000293650700022
ER
PT J
AU Frick, MG
Kopitsky, K
Bolten, AB
Bjorndal, KA
Martins, HR
AF Frick, Michael G.
Kopitsky, Kerry
Bolten, Alan B.
Bjorndal, Karen A.
Martins, Helen R.
TI Sympatry in grapsoid crabs (genera Planes and Plagusia) from olive
ridley sea turtles (Lepidochelys olivacea), with descriptions of crab
diets and masticatory structures
SO MARINE BIOLOGY
LA English
DT Article
ID FUNCTIONAL-MORPHOLOGY; CARETTA-CARETTA; INANIMATE FLOTSAM; FOREGUT
OSSICLES; COLUMBUS CRABS; GASTRIC MILL; DECAPODA; BRACHYURA; CRUSTACEA;
MINUTUS
AB Grapsoid crabs of the genera Planes and Plagusia are commonly referred to as "rafting crabs" due to their propensity to live on flotsam and pelagic marine animals. Planes minutus and Planes major (=Planes cyaneus) are epibionts of sea turtles. Occurrences of grapsoid crabs in the genera Planes and Plagusia were evaluated on a total of 27 olive ridley sea turtles, Lepidochelys olivacea, from the eastern tropic Pacific (1998-2001) and the Hawaiian Islands (2002) captured in July-December each year. This is the first report of Planes marinus and Plagusia squamosa on sea turtles, and of P. major, P. marinus, and P. squamosa in sympatry on a confined substrate. Stomach content analyses showed P. major and P. marinus consumed a variety of neuston and marine vegetation, with the former consuming considerably more animal material. Epibiotic P. squamosa consumed mostly plant material. The three Planes species had distinctive differences in gastric mill tooth morphology. The versatile mouthparts of P. marinus are described and resemble those of their congeners. Most female P. major and P. marinus collected were ovigerous and present in all survey months.
C1 [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA.
[Kopitsky, Kerry] Univ Delaware, Coll Marine Studies, Newark, DE 19716 USA.
[Bolten, Alan B.; Bjorndal, Karen A.] Univ Florida, Dept Biol, Archie Carr Ctr Sea Turtle Res, Gainesville, FL 32611 USA.
[Martins, Helen R.] Univ Azores, Dept Oceanog & Fisheries, P-9901862 Horta, Azores, Portugal.
RP Frick, MG (reprint author), Smithsonian Natl Zool Pk, Friends Natl Zoo, MRC 5516, Washington, DC 20013 USA.
EM frickm@si.edu
OI Bjorndal, Karen/0000-0002-6286-1901
FU PADI foundation
FX We thank Kristina L. Williams (Caretta Research Project) for her help in
measuring and cataloguing crabs. Pacific collections were supported by
the National Marine Fisheries Service Southwest Fisheries Science Center
and the National Oceanic and Atmospheric Administration and thanks are
extended to all personnel working on the cruises mentioned in this
report. The microscopy equipment used for this study was provided
through a grant to M. Frick by the PADI foundation. All necessary
collection permits were granted through NMFS/NOAA to K. Kopitsky, who
collected all of the Pacific grapsoids examined herein. Two anonymous
reviewers provided helpful comments that improved the original draft of
the present study.
NR 44
TC 7
Z9 7
U1 2
U2 23
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD AUG
PY 2011
VL 158
IS 8
BP 1699
EP 1708
DI 10.1007/s00227-011-1684-9
PG 10
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 795UM
UT WOS:000293001400003
ER
PT J
AU Rodgers, PJ
Reaka, ML
Hines, AH
AF Rodgers, Paula J.
Reaka, Marjorie L.
Hines, Anson H.
TI A comparative analysis of sperm storage and mating strategies in five
species of brachyuran crabs
SO MARINE BIOLOGY
LA English
DT Article
ID CALLINECTES-SAPIDUS; BLUE-CRAB; CHIONOECETES-OPILIO; SEXUAL COMPETITION;
INTERTIDAL CRABS; STORED SPERM; MALE SIZE; DECAPODA; ALLOCATION; MAJIDAE
AB Variation in female sperm storage is explained, in part, by the amount of sperm transferred at mating. Laboratory mating experiments were conducted on Eurypanopeus depressus and Rhithropanopeus harrisii from the Chesapeake Bay and Pachygrapsus transversus from Florida, while mated pairs of Uca beebei and U. terpsichores were collected from mudflats in Panama. All experiments and collections were conducted during the summer of 2006 and 2007. More sperm was transferred to larger than smaller females, and by species with long copulation durations (R. harrisii and E. depressus). These two species live in cryptic habitats, have high sperm/egg ratios, and likely store sperm across multiple broods. In contrast, P. transversus and U. beebei mate conspicuously, have short copulations, transfer fewer sperm, and have low sperm/egg ratios. Comparisons of sperm transfer across different mating strategies and habitats provide a better understanding of female sperm storage in the Brachyura.
C1 [Rodgers, Paula J.; Reaka, Marjorie L.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Rodgers, Paula J.; Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Rodgers, PJ (reprint author), Montgomery Coll, Div Biol, Rockville, MD 20850 USA.
EM prodgers@umd.edu
FU Smithsonian Pre-doctoral fellowship; COSMOS club; Explorer's Club
FX We thank the Virginia Institute of Marine Science, Smithsonian Marine
Station and Smithsonian Tropical Research Institute for access to their
collection sites and for providing supplies for this study. Dr. J.
Christy provided valuable information and training for collecting field
mating fiddler crabs in Panama. This research was supported with funds
from the Smithsonian Pre-doctoral fellowship, and travel funding was
provided by the COSMOS club (Young Scholars grant) and the Explorer's
Club (Explorer's grant). We also thank our field assistant in Panama,
Carolina Sanz-Hawkins and the undergraduate research assistants at the
University of Maryland, Travis Anthony, Sharhyr Kahliq, Jay Lee and
Kristen Riffert who helped measure eggs and two anonymous reviewers who
provided valuable feedback for this paper.
NR 48
TC 6
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U1 1
U2 19
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD AUG
PY 2011
VL 158
IS 8
BP 1733
EP 1742
DI 10.1007/s00227-011-1687-6
PG 10
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 795UM
UT WOS:000293001400006
ER
PT J
AU Siwak, M
Rucinski, SM
Matthews, JM
Kuschnig, R
Guenther, DB
Moffat, AFJ
Sasselov, D
Weiss, WW
AF Siwak, Michal
Rucinski, Slavek M.
Matthews, Jaymie M.
Kuschnig, Rainer
Guenther, David B.
Moffat, Anthony F. J.
Sasselov, Dimitar
Weiss, Werner W.
TI Analysis of MOST light curves of five young stars in Taurus-Auriga and
Lupus 3 star-forming regions
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: individual: RY Tau; stars: individual: V410 Tau; stars:
individual: V987 Tau; stars: individual: Lupus 3-14; stars: individual:
Lupus 3-48; stars: rotation
ID HIGH-RESOLUTION SPECTROSCOPY; STELLAR SURFACE-STRUCTURE; LINED T TAURI;
DIFFERENTIAL ROTATION; RY-TAURI; KAPPA(1) CETI; V410 TAURI; PHOTOMETRY;
VARIABILITY; HDE-283572
AB Continuous photometric observations of five young stars obtained by the MOST satellite in 2009 and 2010 in the Taurus and Lupus star formation regions are presented. Using light-curve modelling under the assumption of internal invariability of spots, we obtained small values of the solar-type differential-rotation parameter (k = 0.0005-0.009) for three spotted weak-line T Tauri stars, V410 Tau, V987 Tau and Lupus 3-14; for another spotted weak-line T Tauri star (WTTS), Lupus 3-48, the data are consistent with a rigidly rotating surface (k = 0). Three flares of similar rise (4 min and 30 s) and decay (1 h and 45 min) times were detected in the light curve of Lupus 3-14. The brightness of the classical T Tauri star RY Tau continuously decreased over 3 weeks of its observations with a variable modulation not showing any obvious periodic signal.
C1 [Siwak, Michal; Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Siwak, Michal] Cracov Pedag Univ, Mt Suhora Astron Observ, PL-30084 Krakow, Poland.
[Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Guenther, David B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada.
[Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Siwak, M (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada.
EM siwak@nac.oa.uj.edu.pl
FU Canadian Space Agency; Natural Sciences and Engineering Research Council
of Canada; Austrian Space Agency; Austrian Science Fund
FX MS acknowledges the Canadian Space Agency Post-Doctoral position grant
to SMR within the framework of the Space Science Enhancement Program.
The Natural Sciences and Engineering Research Council of Canada supports
the research of DBG, JMM, AFJM and SMR. Additional support for AFJM
comes from FQRNT (Quebec). RK is supported by the Canadian Space Agency
and WWW is supported by the Austrian Space Agency and the Austrian
Science Fund.
NR 29
TC 9
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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 AUG
PY 2011
VL 415
IS 2
BP 1119
EP 1124
DI 10.1111/j.1365-2966.2011.18683.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805VE
UT WOS:000293756300011
ER
PT J
AU Guggenberger, E
Kolenberg, K
Chapellier, E
Poretti, E
Szabo, R
Benko, JM
Paparo, M
AF Guggenberger, E.
Kolenberg, K.
Chapellier, E.
Poretti, E.
Szabo, R.
Benko, J. M.
Paparo, M.
TI The CoRoT star 105288363: strong cycle-to-cycle changes of the Blazhko
modulation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques: photometric; stars: individual: CoRoT ID 105288363; stars:
variables: RR Lyrae
ID RR-LYRAE STARS; MAGNETIC-FIELD MEASUREMENTS; LIGHT CURVES; MW LYR;
VARIABILITY; EXCITATION; BEHAVIOR; KEPLER
AB We present an analysis of the COnvection, ROtation and planetary Transits (CoRoT) star 105288363, a new Blazhko RR Lyrae star of type RRab (f(0) = 1.7623 d(-1)), observed with the CoRoT spacecraft during the second long run in the direction of the Galactic Centre (LRc02, time-base 145 d). The CoRoT data are characterized by an excellent time-sampling and a low noise amplitude of 0.07 mmag in the 2-12 d(-1) range and allow us to study not only the fine details of the variability of the star, but also long-term changes in the pulsation behaviour and the stability of the Blazhko cycle. We use, among other methods, standard Fourier analysis techniques and O-C diagrams to investigate the pulsational behaviour of the Blazhko star 105288363. In addition to the frequency pattern expected for a Blazhko RR Lyrae star, we find an independent mode (f(1) = 2.984 d(-1)) showing a f(0)/f(1) ratio of 0.59 which is similar to that observed in other Blazhko RR Lyrae stars. The bump and hump phenomena are also analysed, with their variations over the Blazhko cycle. We carefully investigated the strong cycle-to-cycle changes in the Blazhko modulation (P-B = 35.6 d), which seem to happen independently and partly diametrically in the amplitude and phase modulations. Furthermore, the phasing between the two types of modulations is found to change during the course of the observations.
C1 [Guggenberger, E.; Kolenberg, K.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chapellier, E.] Univ Nice Sophia Antipolis, Observ Cote Azur, UMR 6525, F-06108 Nice 02, France.
[Poretti, E.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy.
[Szabo, R.; Benko, J. M.; Paparo, M.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary.
RP Guggenberger, E (reprint author), Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM elisabeth.guggenberger@univie.ac.at
OI Poretti, Ennio/0000-0003-1200-0473; Benko, Jozsef/0000-0003-3851-6603;
Szabo, Robert/0000-0002-3258-1909
FU Austrian Fonds zur Forderung der wissenschaftlichen Forschung (FWF)
[T359-N16, P19962-N16]; PRIN-INAF; ESA PECS [98022, 98114]; Hungarian
OTKA [K83790]
FX This research has made use of the ExoDat data base, operated at
LAM-OAMP, Marseille, France, on behalf of the CoRoT/Exoplanet programme.
KK and EG acknowledge support from the Austrian Fonds zur Forderung der
wissenschaftlichen Forschung (FWF), project numbers T359-N16 and
P19962-N16. EP acknowledges support from the PRIN-INAF 2010
'Asteroseismology: looking inside the stars'. MP, JMB and RS acknowledge
the support of the ESA PECS projects Nos. 98022 and 98114. RS and JMB
are supported by the Hungarian OTKA grant K83790.
NR 54
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U2 5
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 AUG
PY 2011
VL 415
IS 2
BP 1577
EP 1589
DI 10.1111/j.1365-2966.2011.18812.x
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805VE
UT WOS:000293756300049
ER
PT J
AU Rosolowsky, E
Pineda, JE
Gao, Y
AF Rosolowsky, Erik
Pineda, Jaime E.
Gao, Yu
TI Minimal HCN emission from molecular clouds in M33
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars: formation; ISM: clouds; galaxies: individual: M33; radio lines:
ISM
ID STAR-FORMING GALAXIES; DENSE GAS; FORMATION LAW; SCHMIDT LAW; CO;
GRADIENT; TRACERS; REGIONS; COMPLEX; CORES
AB Since HCN emission has been shown to be a linear tracer of ongoing star formation activity, we have searched for HCN (J = 1 -> 0) emission from known GMCs in the nearby galaxy M33. No significant HCN emission has been found along any of the lines of sight. We find two lines of sight with CO-to-HCN integrated intensity ratios up to 280, nearly a factor of 6 above what is found in comparable regions of the Milky Way. Star formation tracers suggest that the HCN-to-star formation rate ratio (L-HCN/(M) over dot(star)) is a factor of 6 lower than what is observed in the Milky Way (on average) and local extragalactic systems. Simple chemical models accounting for the subsolar N/O ratio suggest that depletion cannot account for the high CO-to-HCN ratios. Given HCN formation requires high extinction (A(V) > 4), low metallicity may yield reduced dust shielding and thus a high CO/HCN ratio. The turbulence and structure of GMCs in M33 are comparable to those found in other systems, so the differences are unlikely to result from different GMC properties. Since lower CO-to-HCN ratios are associated with the highest rates of star formation, we attribute the deficits in part to evolutionary effects within GMCs.
C1 [Rosolowsky, Erik] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada.
[Pineda, Jaime E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Pineda, Jaime E.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Gao, Yu] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
RP Rosolowsky, E (reprint author), Univ British Columbia Okanagan, 3333 Univ Way, Kelowna, BC V1V 1V7, Canada.
EM erik.rosolowsky@ubc.ca
RI Pineda, Jaime/J-7405-2013
OI Pineda, Jaime/0000-0002-3972-1978
FU NSF AAP [AST-0502605]; NSERC of Canada; China NSF Innovation Team
[10621303, 10425313]; Ministry of Science & Technology and Chinese
Academy of Sciences; CNRS/INSU (France); MPG (Germany); IGN (Spain)
FX ER and JEP are supported by an NSF AAP Fellowship (AST-0502605). ER is
further supported by a Discovery Grant from NSERC of Canada. YG's
research is partially supported by China NSF Innovation Team
(#10621303), Distinguished Young Scholars (#10425313), 973 of the
Ministry of Science & Technology and Chinese Academy of Sciences'
Hundred Talent Program. We are grateful for the comments of an anonymous
referee, in particular regarding the importance of ultraviolet
dissociation at regulating the CO/HCN abundance. This work is based on
observations with the IRAM 30-m telescope. IRAM is supported by
CNRS/INSU (France), the MPG (Germany) and the IGN (Spain).
NR 43
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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 AUG
PY 2011
VL 415
IS 2
BP 1977
EP 1984
DI 10.1111/j.1365-2966.2011.18851.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805VE
UT WOS:000293756300080
ER
PT J
AU Crouch, T
AF Crouch, Tom
TI NASA ART: 50 years of exploration
SO PHYSICS TODAY
LA English
DT Article
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Crouch, T (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 0
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U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD AUG
PY 2011
VL 64
IS 8
BP 42
EP 47
PG 6
WC Physics, Multidisciplinary
SC Physics
GA 805ZB
UT WOS:000293768500021
ER
PT J
AU Olson, KA
Mueller, T
Kerby, JT
Bolortsetseg, S
Leimgruber, P
Nicolson, CR
Fuller, TK
AF Olson, Kirk A.
Mueller, Thomas
Kerby, Jeff T.
Bolortsetseg, Sanjaa
Leimgruber, Peter
Nicolson, Craig R.
Fuller, Todd K.
TI Death by a thousand huts? Effects of household presence on density and
distribution of Mongolian gazelles
SO CONSERVATION LETTERS
LA English
DT Article
DE Distance sampling; grassland; human wildlife conflict; NDVI; Mongolian
gazelles; Procapra gutturosa; population estimation
ID PROCAPRA-GUTTUROSA; CONSERVATION; POPULATION; LIVESTOCK; WILDLIFE;
PASTORALISM; MANAGEMENT; MIGRATION; CONFLICTS; RAILROAD
AB In late spring 2005, we surveyed Mongolian gazelle (Procapra gutturosa) populations in a 275,000-km(2) portion the eastern steppe of Mongolia to estimate their population size and assess their distribution with respect to forage and human households. We estimated a total population of 1.126 million (95% CI, 843,000-1,500,000), and found that gazelle distribution could be accurately predicted by a Normalized Difference Vegetation Index (NDVI) as an approximated measurement of vegetation productivity, and thus habitat quality. However, the presence of households had a considerable impact on gazelle density; in most regions, density was 76-98% lower than in survey blocks where no households were found. We show that in addition to large regional differences in gazelle density throughout their range, the presence of herding households had a negative impact on gazelle density in selected habitat. The conservation of ungulates that depend on the ability to make long-distance nomadic movements requires not only that access to habitat is unimpeded but also that the subtle impacts of activities associated with the presence of people need to be considered.
C1 [Olson, Kirk A.; Nicolson, Craig R.; Fuller, Todd K.] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA.
[Olson, Kirk A.] Natl Univ Mongolia, Fac Biol, Ulaanbaatar, Mongol Peo Rep.
[Mueller, Thomas] Univ Maryland, Grad Program Behav Evolut & Systemat, College Pk, MD 20742 USA.
[Mueller, Thomas; Leimgruber, Peter] Smithsonian Natl Zool Pk, Conservat Biol Inst, Front Royal, VA USA.
[Kerby, Jeff T.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA.
[Bolortsetseg, Sanjaa] Wildlife Conservat Soc, Mongolia Country Program, Ulaanbaatar, Mongol Peo Rep.
RP Fuller, TK (reprint author), Univ Massachusetts, Dept Environm Conservat, 160 Holdsworth Way, Amherst, MA 01003 USA.
EM tkfuller@eco.umass.edu
RI Mueller, Thomas/A-1740-2014; Leimgruber, Peter/O-1304-2015;
OI Mueller, Thomas/0000-0001-9305-7716; Leimgruber,
Peter/0000-0002-3682-0153; Kerby, Jeffrey/0000-0002-2739-9096
FU Wildlife Conversation Society; University of Massachusetts Amherst;
Smithsonian Institute; National Science Foundation [DEB-0743557,
DEB-0743385]
FX We thank both Dorj and Otgon for their hard work in driving and ensuring
the safe operation of the vehicles during this survey. The Mongolian
Border Authority granted permission to work within their jurisdiction.
This work represents a collaborative effort between the National
University of Mongolia, University of Massachusetts, University of
Maryland, the Smithsonian Institute, and the Wildlife Conversation
Society. Funds were provided by the Wildlife Conversation Society, the
University of Massachusetts Amherst, The Smithsonian Institute, and the
National Science Foundation (DEB-0743557, DEB-0743385).
NR 46
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U1 1
U2 18
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1755-263X
J9 CONSERV LETT
JI Conserv. Lett.
PD AUG-SEP
PY 2011
VL 4
IS 4
BP 304
EP 312
DI 10.1111/j.1755-263X.2011.00180.x
PG 9
WC Biodiversity Conservation
SC Biodiversity & Conservation
GA 798SV
UT WOS:000293233200008
ER
PT J
AU Oliveira, LC
Neves, LG
Raboy, BE
Dietz, JM
AF Oliveira, Leonardo C.
Neves, Leonardo G.
Raboy, Becky E.
Dietz, James M.
TI Abundance of Jackfruit (Artocarpus heterophyllus) Affects Group
Characteristics and Use of Space by Golden-Headed Lion Tamarins
(Leontopithecus chrysomelas) in Cabruca Agroforest
SO ENVIRONMENTAL MANAGEMENT
LA English
DT Article
DE Cabruca; Agroforest; Leontopithecus chrysomelas; Endangered species;
Jackfruit; Conservation
ID HOME-RANGE SIZE; RAIN-FOREST FRAGMENTATION; SHADE CACAO PLANTATIONS;
ATLANTIC-FOREST; SOUTHERN BAHIA; ECOLOGICAL CONSTRAINTS; METAPOPULATION
DYNAMICS; POPULATION-DENSITY; FOOD AVAILABILITY; SPECIES RICHNESS
AB Cabruca is an agroforest of cacao trees shaded by native forest trees. It is the predominant vegetation type throughout eastern part of the range of the golden-headed lion tamarins, Leontopithecus chrysomelas, an endangered primate endemic to Atlantic Forest. Understanding how lion tamarins use this agroforest is a conservation priority. To address this question, we documented the diet, home range size, group sizes and composition, density, number of litters and body condition of lion tamarins living in cabruca, and other habitats. Jackfruit, Artocarpus heterophyllus, was the most used species used by lion tamarins in cabruca and was widely available and used throughout the year. In cabruca, home range size was the smallest (22-28 ha) and density of lion tamarins was the highest (1.7 ind/ha) reported for the species. Group size averaged 7.4 individuals and was not significantly different among the vegetation types. In cabruca, groups produced one or two litters a year, and all litters were twins. Adult males in cabruca were significantly heavier than males in primary forest. Our study is the first to demonstrate that breeding groups of golden-headed lion tamarins can survive and reproduce entirely within cabruca agroforest. Jackfruit proved to be a keystone resource for lion tamarins in cabruca, and bromeliads were important as an animal prey foraging microhabitat. In cases where cabruca contains concentrated resources, such as jackfruit and bromeliads, lion tamarins may not only survive and reproduce but may fare better than in other forest types, at least for body condition and reproduction.
C1 [Oliveira, Leonardo C.; Dietz, James M.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Oliveira, Leonardo C.; Neves, Leonardo G.] IESB, Nucleo Biodiversidade, Ilheus, BA, Brazil.
[Raboy, Becky E.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Washington, DC USA.
RP Oliveira, LC (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
EM leonardoco@gmail.com
RI Oliveira, Leonardo/G-1290-2012
OI Oliveira, Leonardo/0000-0002-1774-0713
FU Lion Tamarins of Brazil Fund; World Wildlife Fund-US; Durrell Wildlife
Conservation Trust; Margot Marsh Biodiversity Foundation; Tulsa Zoo;
Sigma Xi; University of Maryland (UM) Biology Department; Seeds of
Change; Wildlife Conservation Society; International Foundation of
Science; Rufford Small Grants Foundation; Idea Wild; University of
Maryland (Board of Visitors); CAPES/Fulbright (Fundacao Coordenacao de
Aperfeicoamento de Pessoal de Nivel Superior-CAPES/Fulbright)
FX We thank the Brazilian Institute of Environment and Renewable Natural
Resources (Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais
Renovaveis-IBAMA) for the permits to capture the groups. We are grateful
to the owners and their employees of the Fazenda Almada, Santa Rita,
Riachuelo and Sao Jose and the private reserves (RPPNs) Ararauna and
Serra do Teimoso for allowing us to conduct our study in their
properties and for the support provided for the field team. We also
thank our field assistants Daniel Batista, Gilvan Gomes Mota, Gilvanio
Gomes Mota, Jose Renato, Jiomario dos Santos Souza, Edimalvan da
Purificacao and Paula Roberta Pedreira dos Reis. To Gotz Schroth for
suggestions on an early version of the manuscript and to Sara Ziegler
for helping with the figures. Financial support was provided to BER and
JMD by the Lion Tamarins of Brazil Fund, World Wildlife Fund-US, the
Durrell Wildlife Conservation Trust, the Margot Marsh Biodiversity
Foundation, and the Tulsa Zoo, to BER by Sigma Xi, and to LCO by
University of Maryland (UM) Biology Department, Seeds of Change, Lion
Tamarins of Brazil Fund, the Wildlife Conservation Society,
International Foundation of Science, The Rufford Small Grants Foundation
and Idea Wild. LCO received doctoral fellowships from the University of
Maryland (Board of Visitors, Ann G. Wylie Dissertation Fund, Drs. Wayne
T. and Mary T. Hockmeyer Doctoral Fellowship), and CAPES/Fulbright
(Fundacao Coordenacao de Aperfeicoamento de Pessoal de Nivel
Superior-CAPES/Fulbright).
NR 89
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U1 4
U2 53
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0364-152X
J9 ENVIRON MANAGE
JI Environ. Manage.
PD AUG
PY 2011
VL 48
IS 2
BP 248
EP 262
DI 10.1007/s00267-010-9582-3
PG 15
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 796AT
UT WOS:000293023300003
PM 21079956
ER
PT J
AU De Leon, LF
Raeymaekers, JAM
Bermingham, E
Podos, J
Herrel, A
Hendry, AP
AF Fernando De Leon, Luis
Raeymaekers, Joost A. M.
Bermingham, Eldredge
Podos, Jeffrey
Herrel, Anthony
Hendry, Andrew P.
TI EXPLORING POSSIBLE HUMAN INFLUENCES ON THE EVOLUTION OF DARWIN'S FINCHES
SO EVOLUTION
LA English
DT Article
DE contemporary evolution; diversification; ecological speciation;
Galapagos; adaptive radiation; human impact
ID GALAPAGOS GROUND FINCHES; ISLA DAPHNE MAJOR; CONTEMPORARY EVOLUTION;
BEAK SHAPE; CONSERVATION BIOLOGY; EXTERNAL MORPHOLOGY;
NATURAL-SELECTION; SYMPATRIC MORPHS; CICHLID FISH; BITE FORCE
AB Humans are an increasingly common influence on the evolution of natural populations. Potential arenas of influence include altered evolutionary trajectories within populations and modifications of the process of divergence among populations. We consider this second arena in the medium ground finch (Geospiza fortis) on Santa Cruz Island, Galapagos, Ecuador. Our study compared the G. fortis population at a relatively undisturbed site, El Garrapatero, to the population at a severely disturbed site, Academy Bay, which is immediately adjacent to the town of Puerto Ayora. The El Garrapatero population currently shows beak size bimodality that is tied to assortative mating and disruptive selection, whereas the Academy Bay population was historically bimodal but has lost this property in conjunction with a dramatic increase in local human population density. We here evaluate potential ecological-adaptive drivers of the differences in modality by quantifying relationships between morphology (beak and head dimensions), functional performance (bite force), and environmental characteristics (diet). Our main finding is that associations among these variables are generally weaker at Academy Bay than at El Garrapatero, possibly because novel foods are used at the former site irrespective of individual morphology and performance. These results are consistent with the hypothesis that the rugged adaptive landscapes promoting and maintaining diversification in nature can be smoothed by human activities, thus hindering ongoing adaptive radiation.
C1 [Fernando De Leon, Luis; Hendry, Andrew P.] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada.
[Fernando De Leon, Luis; Hendry, Andrew P.] McGill Univ, Dept Biol, Montreal, PQ H3A 2K6, Canada.
[Fernando De Leon, Luis; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama.
[Raeymaekers, Joost A. M.] Katholieke Univ Leuven, Lab Anim Divers & Systemat, B-3000 Louvain, Belgium.
[Podos, Jeffrey] Univ Massachusetts, Dept Biol, Amherst, MA 01003 USA.
[Herrel, Anthony] MNHN, CNRS, UMR 7179, Dept Ecol & Gest Biodivers, F-75231 Paris 5, France.
RP De Leon, LF (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada.
EM luis.deleonreyna@mail.mcgill.ca
RI De Leon, Luis Fernando/H-1112-2011; Hendry, Andrew/C-5765-2008; Herrel,
Anthony/C-3712-2013; Raeymaekers, Joost/J-9538-2014
OI Hendry, Andrew/0000-0002-4807-6667; Herrel, Anthony/0000-0003-0991-4434;
Raeymaekers, Joost/0000-0003-2732-7495
FU Secretaria Nacional de Ciencia; Tecnologia e Innovacion; Instituto para
la Formacion y Aprovechamiento de los Recursos Humanos, Panama; US
National Science Foundation; Natural Sciences and Engineering Research
Council of Canada; Smithsonian Tropical Research Institute; Research
Foundation Flanders
FX Logistical support and permits were provided by the Galapagos National
Park Service and the Charles Darwin Research Station. Field assistance
was provided by E. Hilton, M. Rossi-Santos, D. Ruiz, A. Gabela, P.
Kelley, M. Hendry, S. Huber, K. Huyghe, B. Vanhooydonck, and D. Delaney.
We especially thank A. McKellar who contributed the species-level data
from Puerto Ayora itself. K. Cottenie provided suggestions for data
analysis. D. Sharpe provided comments on the manuscript. Funding was
provided by the Secretaria Nacional de Ciencia, Tecnologia e Innovacion
and the Instituto para la Formacion y Aprovechamiento de los Recursos
Humanos, Panama (L.F. De Leon); the US National Science Foundation (J.
Podos); the Natural Sciences and Engineering Research Council of Canada
(A. P. Hendry); the Smithsonian Tropical Research Institute (E.
Bermingham); and Research Foundation Flanders (J. Raeymaekers). We thank
the associated editor and two anonymous reviewers for providing valuable
comments on an earlier version of this manuscript.
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PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD AUG
PY 2011
VL 65
IS 8
BP 2258
EP 2272
DI 10.1111/j.1558-5646.2011.01297.x
PG 15
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 798DL
UT WOS:000293182700010
PM 21790573
ER
PT J
AU Tonra, CM
Marra, PP
Holberton, RL
AF Tonra, Christopher M.
Marra, Peter P.
Holberton, Rebecca L.
TI Early elevation of testosterone advances migratory preparation in a
songbird
SO JOURNAL OF EXPERIMENTAL BIOLOGY
LA English
DT Article
DE androgen; condition; dark-eyed junco; Junco hyemalis; migration
phenology
ID DARK-EYED JUNCOS; WHITE-CROWNED SPARROWS; AVIAN LIFE HISTORIES;
NON-BREEDING SEASON; HABITAT QUALITY; NONBREEDING SEASON; AMERICAN
REDSTARTS; SPRING MIGRATION; FAT DEPOSITION; BIRD
AB The timing of events associated with spring migration can be an important determinant of fitness for migratory birds. The need to prepare and maintain physical condition for migration is one demand that must be met for early arrival on breeding areas, and this demand is compounded by the energetic demands of the physiological transition to breeding. Here, we examined whether migratory birds, specifically males, can adequately meet both of these demands by elevating the sex steroid testosterone early during migratory preparation. To test this, we used a captive experiment in which we photostimulated male dark-eyed juncos (Junco hyemalis) and manipulated circulating testosterone. We predicted males with elevated testosterone would prepare to migrate and breed faster than control males or males where the ability of testosterone to bind with receptors, or be converted to estradiol, was inhibited (testosterone inhibited). We measured migratory preparation using mass, food intake, fat deposits and nocturnal activity (Zugunruhe). To estimate breeding preparation, we measured the diameter of the cloacal protuberance (CP). We found that males in the testosterone treatment group began migratory preparation approximately 10. days before controls. There was no difference in the magnitude of peak migratory condition between testosterone-implanted birds and controls. Males implanted with testosterone also reached the onset of breeding preparation faster and had larger peak CP diameter compared with controls. Testosterone-inhibited birds showed no signs of migratory preparation and only a weak increase in CP diameter. These results demonstrate that early elevation of testosterone during migratory preparation could incur benefits for males in terms of the ability to depart earlier from non-breeding areas and arrive in a more advanced breeding condition. This experiment demonstrates that there may be important physiological underpinnings to known winter to breeding season carry-over effects in migratory birds.
C1 [Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Sch Biol & Ecol, Lab Avian Biol, Orono, ME 04469 USA.
[Tonra, Christopher M.; Marra, Peter P.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA.
RP Tonra, CM (reprint author), Univ Maine, Sch Biol & Ecol, Lab Avian Biol, Orono, ME 04469 USA.
EM TonraC@si.edu
RI Tonra, Christopher/B-1620-2013
FU National Science Foundation [0649679, 0615701]; American Museum of
Natural History
FX This research was funded by grants awarded to P. P. M. (0649679) and R.
L. H. (0615701) from the National Science Foundation and to C. M. T.
from the Frank M. Chapman Memorial Fund of the American Museum of
Natural History. We are grateful to Evan Adams, Leah Culp, Kristi
Kennedy, Mel Kierman, Adrienne Leppold, Doug Perez, Kayla Porcelli and
Wes Wright for assistance with bird care and data collection, and K.
Porcelli for assistance with androgen assays. Bill Halteman and Colin
Studds provided valuable input on data analysis. We thank Bill Glanz,
Brian Olsen, members of the UMaine Lab of Avian Biology reading group
and three anonymous reviewers for comments on an earlier draft of this
manuscript.
NR 62
TC 21
Z9 21
U1 1
U2 18
PU COMPANY OF BIOLOGISTS LTD
PI CAMBRIDGE
PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL,
CAMBS, ENGLAND
SN 0022-0949
J9 J EXP BIOL
JI J. Exp. Biol.
PD AUG
PY 2011
VL 214
IS 16
BP 2761
EP 2767
DI 10.1242/jeb.054734
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 797YW
UT WOS:000293167300020
PM 21795574
ER
PT J
AU Forboseh, PF
Sunderland, TCH
Comiskey, JA
Balinga, M
AF Forboseh, Philip F.
Sunderland, Terry C. H.
Comiskey, James A.
Balinga, Michael
TI Tree population dynamics of three altitudinal vegetation communities on
Mount Cameroon (1989-2004)
SO JOURNAL OF MOUNTAIN SCIENCE
LA English
DT Article
DE Growth rates; Recruitment; Mortality; Altitude; Half-life; Mount
Cameroon
ID TROPICAL RAIN-FORESTS; MORTALITY; RECRUITMENT; BUDONGO; CANOPY; GROWTH
AB Changes in permanent sample plots in the lowland, submontane and montane forests on Mount Cameroon (4,095 m above sea level), an active volcano, are described for 15 years from 1989 to 2004. Throughout the study period, the stocking level of trees with a diameter at breast height (DBH) a parts per thousand yen 10 cm in the three forests were lower than in pan-tropical stands suggesting a significant impact of volcanic and human-related activities on the vegetation communities on the mountain. Annual mortality rates in the submontane and montane forests were consistent with those reported for comparable altitudinal ranges in the Blue Mountains of Jamaica. The annual mortality rate was higher in the lowland forest than other lowland sites included. Divergence between recruitment and mortality rates was large suggesting that the three vegetation communities have not reached their climax. The seven-year difference in half-life of large trees (with a DBH a parts per thousand yen 50 cm) in the submontane and montane forests suggests an altitudinal effect on turnover of larger trees that in turn contributes to the frequent small stature of high altitude forests. There was little evidence of an altitudinal effect on species turnover and growth rate. This finding supports generalizations about the zero effect of growth on the stature of high altitude trees. Understanding forest dynamics is crucially important in the management of tropical montane environments and in this instance particularly so given the recent creation of the Mount Cameroon National Park.
C1 [Sunderland, Terry C. H.] Ctr Int Forestry Res CIFOR, Bogor, Indonesia.
[Forboseh, Philip F.] Plan Cameroon, Yaounde, Cameroon.
[Comiskey, James A.] Natl Pk Serv, Inventory & Monitoring Program, Frederiscksburg, VA 22405 USA.
[Comiskey, James A.] Smithsonian Inst, S Dillon Ripley Ctr, Washington, DC 20560 USA.
[Balinga, Michael] Ctr Int Forestry Res CIFOR, Ouagadougou, Burkina Faso.
RP Sunderland, TCH (reprint author), Ctr Int Forestry Res CIFOR, POB 0113 BOBCD, Bogor, Indonesia.
EM t.sunderland@cgiar.org
NR 49
TC 2
Z9 2
U1 1
U2 10
PU SCIENCE PRESS
PI BEIJING
PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA
SN 1672-6316
J9 J MT SCI-ENGL
JI J Mt. Sci.
PD AUG
PY 2011
VL 8
IS 4
BP 495
EP 504
DI 10.1007/s11629-011-2031-9
PG 10
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 796CL
UT WOS:000293027700001
ER
PT J
AU Pena, V
Adey, WH
Riosmena-Rodriguez, R
Jung, MY
Afonso-Carrillo, J
Choi, HG
Barbara, I
AF Pena, Viviana
Adey, Walter H.
Riosmena-Rodriguez, Rafael
Jung, Moon-Yung
Afonso-Carrillo, Julio
Choi, Han-Gu
Barbara, Ignacio
TI MESOPHYLLUM SPHAERICUM SP. NOV. (CORALLINALES, RHODOPHYTA): A NEW
MAERL-FORMING SPECIES FROM THE NORTHEAST ATLANTIC
SO JOURNAL OF PHYCOLOGY
LA English
DT Article
DE Corallinales; Galicia; Iberian Peninsula; maerl; Mesophyllum canariense;
Mesophyllum erubescens; Mesophyllum sphaericum; NE Atlantic; nuclear SSU
rDNA; rhodolith
ID RNA GENE-SEQUENCES; SOUTH-AFRICA; IBERIAN PENINSULA; RHODYMENIALES
RHODOPHYTA; PHYLOGENETIC TREES; ALGAE CORALLINALES; ORD NOV; AUSTRALIA;
FOSLIE; REPRESENTATIVES
AB Mesophyllum sphaericum sp. nov. is described based on spherical maerl individuals (up to 10 cm) collected in a shallow subtidal maerl bed in Galicia (NW Spain). The thalli of these specimens are radially organized, composed of arching tiers of compact medullary filaments. Epithallial cells have flattened to rounded outermost walls, and they occur in a single layer. Subepithallial initials are as long as, or longer than the daughter cells that subtend them. Cell fusions are abundant. Multiporate asexual conceptacles are protruding, mound-like with a flattened pore plate, lacking a peripheral raised rim. Filaments lining the pore canal and the conceptacle roof are composed of five to six cells with straight elongate and narrow cells at their base. Carposporangial conceptacles are uniporate, protruding, and conical. Spermatangial conceptacles were not observed. Molecular results placed M. sphaericum near to M. erubescens, but M. sphaericum is anatomically close to M. canariense. The examination of the holotype and herbarium specimens of M. canariense indicated that both species have pore canal filaments with elongate basal cells, but they differ in number of cells (five to six in M. sphaericum vs. four in M. canariense). Based on the character of pore canal filaments, M. canariense shows similarities with M. erubescens (three to five celled). The outermost walls of epithallial cells of M. canariense are flared compared to the round to flattened ones of M. erubescens, the latter being widely accepted for the genus Mesophyllum. The addition of M. sphaericum as new maerl-forming species suggests that European maerl beds are more biodiverse than previously understood.
C1 [Pena, Viviana; Barbara, Ignacio] Univ A Coruna, Lab Algas Marinas, Dept Biol Anim Biol Vegetal & Ecol, E-15071 La Coruna, Spain.
[Adey, Walter H.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Riosmena-Rodriguez, Rafael] Univ Baja California Sur UABCS, Dept Biol Marina, La Paz 23080, Bcs, Mexico.
[Jung, Moon-Yung; Choi, Han-Gu] Korea Polar Res Inst, KORDI, Div Life Sci, Inchon 406840, South Korea.
[Afonso-Carrillo, Julio] Univ La Laguna, Dept Biol Vegetal Bot, E-38271 San Cristobal la Laguna, Canary Islands, Spain.
RP Pena, V (reprint author), Univ A Coruna, Lab Algas Marinas, Dept Biol Anim Biol Vegetal & Ecol, Campus A Zapateira S-N, E-15071 La Coruna, Spain.
EM vpena@udc.es
RI Pena, Viviana/A-6095-2014
OI Pena, Viviana/0000-0001-7003-3850
FU Xunta de Galicia [PGI-DIT03PXIB10301PR]; Ministerio de Educacion y
Ciencia, FEDER [CGL2006-03576/BOS]; Basic Research Program of the Korea
Polar Research Institute [PE10060/PE11030]; CONACYT
FX This study was supported by the research projects PGI-DIT03PXIB10301PR
(Xunta de Galicia) and CGL2006-03576/BOS (Ministerio de Educacion y
Ciencia, FEDER). This work was also supported by a grant from the Basic
Research Program of the Korea Polar Research Institute project
PE10060/PE11030, and a grant from CONACYT SEMARNAT to R. R. R. We thank
Drs. Michael Guiry, Paul C. Silva, and Richard Moe for their wise
remarks on algal nomenclature, and Jose Santos for comments on the Latin
diagnosis. We also thank Drs. Tommy Presto (Trondheim Herbarium, TRH)
and Bruno de Reviers (Museum National d'Histoire Naturelle, PC) for the
loan of the holotype and other herbarium specimens of Mesophyllum
canariense. We are also grateful to both anonymous reviewers for their
comments on the manuscript.
NR 80
TC 20
Z9 22
U1 0
U2 13
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD AUG
PY 2011
VL 47
IS 4
BP 911
EP 927
DI 10.1111/j.1529-8817.2011.01015.x
PG 17
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 797BA
UT WOS:000293096000020
PM 27020026
ER
PT J
AU Bonachea, LA
Ryan, MJ
AF Bonachea, Luis A.
Ryan, Michael J.
TI Predation risk increases permissiveness for heterospecific advertisement
calls in tungara frogs, Physalaemus pustulosus
SO ANIMAL BEHAVIOUR
LA English
DT Article
DE Leptodactylus pentadactylus; mate choice; permissiveness; Physalaemus
pustulosus; predation risk; sexual selection; tungara frog
ID SEXUAL SELECTION; MATE CHOICE; SPECIES RECOGNITION; MATING CALL; FEMALE;
SPECIATION; COSTS; CUES; HYBRIDIZATION; PREFERENCE
AB Factors that influence the strength of sexual selection within a population may have important consequences for the evolution and maintenance of reproductive isolation between populations. Here we examine the role of one such factor, predation risk, in influencing female permissiveness for heterospecific advertisement calls. Specifically, we tested the effect of simulated predation risk on mate choice in female tungara frogs, Physalaemus pustulosus, using variation in ambient light levels, travel time and the presence of auditory cues of local predators. Simulated predation risk increased female permissiveness for advertisement calls along an artificial gradient of calls intermediate between conspecifics and a congener, Physalaemus enesefae. Across the entire gradient, the presence of auditory cues of the predatory frog Leptodactylus pentadactylus in association with the conspecific call dramatically increased the likelihood of females choosing the intermediate call. In addition, higher ambient light levels and simulation of increased travel distances both increased the likelihood that females would choose intermediate calls over conspecific calls. These results suggest that, although mate choice may be important in causing reproductive isolation between allopatric populations, spatial or temporal variation in predation risk may strongly influence the expression of mate choice and thus the outcome of secondary contact. (C) 2011 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved.
C1 [Bonachea, Luis A.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Bonachea, LA (reprint author), San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA.
EM luis.bonachea@sjsu.edu
NR 40
TC 9
Z9 9
U1 0
U2 22
PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
J9 ANIM BEHAV
JI Anim. Behav.
PD AUG
PY 2011
VL 82
IS 2
BP 347
EP 352
DI 10.1016/j.anbehav.2011.05.009
PG 6
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA 795FX
UT WOS:000292960400023
ER
PT J
AU Crosier, AE
Comizzoli, P
Baker, T
Davidson, A
Munson, L
Howard, J
Marker, LL
Wildt, DE
AF Crosier, Adrienne E.
Comizzoli, Pierre
Baker, Tom
Davidson, Autumn
Munson, Linda
Howard, JoGayle
Marker, Laurie L.
Wildt, David E.
TI Increasing Age Influences Uterine Integrity, But Not Ovarian Function or
Oocyte Quality, in the Cheetah (Acinonyx jubatus)
SO BIOLOGY OF REPRODUCTION
LA English
DT Article
DE aging; carnivore reproduction; felid; gamete; ovary; ovum; uterus
ID IN-VITRO FERTILIZATION; GROWTH-FACTOR RECEPTOR; FREE-RANGING CHEETAHS;
DOMESTIC CAT; ENDOMETRIAL HYPERPLASIA; MELENGESTROL ACETATE;
ARTIFICIAL-INSEMINATION; EMBRYO DEVELOPMENT; ESTROGEN-RECEPTOR;
EJACULATE TRAITS
AB Although the cheetah (Acinonyx jubatus) routinely lives for more than 12 yr in ex situ collections, females older than 8 yr reproduce infrequently. We tested the hypothesis that reproduction is compromised in older female cheetahs due to a combination of disrupted gonadal, oocyte, and uterine function/integrity. Specifically, we assessed 1) ovarian response to gonadotropins; 2) oocyte meiotic, fertilization, and developmental competence; and 3) uterine morphology in three age classes of cheetahs (young, 2-5 yr, n = 17; prime, 6-8 yr, n = 8; older, 9-15 yr, n = 9). Ovarian activity was stimulated with a combination of equine chorionic gonadotropin and human chorionic gonadotropin (hCG), and fecal samples were collected for 45 days before gonadotropin treatment and for 30 days after oocyte recovery by laparoscopy. Twenty-six to thirty hours post-hCG, uterine morphology was examined by ultrasound, ovarian follicular size determined by laparoscopy, and aspirated oocytes assessed for nuclear status or inseminated in vitro. Although no influence of age on fecal hormone concentrations or gross uterine morphology was found (P > 0.05), older females produced fewer (P < 0.05) total antral follicles and oocytes compared to younger counterparts. Regardless of donor age, oocytes had equivalent (P > 0.05) nuclear status and ability to reach metaphase II and fertilize in vitro. A histological assessment of voucher specimens revealed an age-related influence on uterine tissue integrity, with more than 87% and more than 56% of older females experiencing endometrial hyperplasia and severe pathologies, respectively. Our collective findings reveal that lower reproductive success in older cheetahs appears to be minimally influenced by ovarian and gamete aging and subsequent dysfunction. Rather, ovaries from older females are responsive to gonadotropins, produce normative estradiol/progestogen concentrations, and develop follicles containing oocytes with the capacity to mature and be fertilized. A more likely cause of reduced fertility may be the high prevalence of uterine endometrial hyperplasia and related pathologies. The discovery that a significant proportion of oocytes from older females have developmental capacity in vitro suggests that in vitro fertilization and embryo transfer may be useful for "rescuing" the genome of older, nonreproductive cheetahs.
C1 [Crosier, Adrienne E.; Comizzoli, Pierre; Howard, JoGayle; Wildt, David E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Crosier, Adrienne E.; Comizzoli, Pierre; Howard, JoGayle; Wildt, David E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC USA.
[Baker, Tom; Davidson, Autumn; Munson, Linda] Univ Calif Davis, Sch Vet Med, Davis, CA 95616 USA.
[Marker, Laurie L.] Cheetah Conservat Fund, Otjiwarongo, Namibia.
RP Crosier, AE (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM crosiera@si.edu
FU Ohrstrom Foundation; William H. Donner Foundation, Inc.; Smithsonian's
Undersecretary for Science Endowment; Friends of the National Zoo
FX Supported by the Ohrstrom Foundation, the William H. Donner Foundation,
Inc., the Smithsonian's Undersecretary for Science Endowment, and
Friends of the National Zoo.
NR 65
TC 19
Z9 19
U1 2
U2 30
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
EI 1529-7268
J9 BIOL REPROD
JI Biol. Reprod.
PD AUG
PY 2011
VL 85
IS 2
BP 243
EP 253
DI 10.1095/biolreprod.110.089417
PG 11
WC Reproductive Biology
SC Reproductive Biology
GA 795WH
UT WOS:000293008200004
PM 21565998
ER
PT J
AU Saltonstall, K
AF Saltonstall, Kristin
TI Remnant native Phragmites australis maintains genetic diversity despite
multiple threats
SO CONSERVATION GENETICS
LA English
DT Article
DE Common reed; Conservation; Hybridization; Marsh; Native; Invasive
species; Restoration
ID MULTILOCUS GENOTYPE DATA; COMMON REED; NONCODING REGIONS; CRYPTIC
INVASION; CHLOROPLAST DNA; NORTH-AMERICA; TIDAL MARSHES; SALT MARSHES;
HYBRIDIZATION; MARKERS
AB Over the past century, an increasing number of species have been negatively impacted by anthropogenic factors such as habitat disturbance and introduced species. One such plant, Phragmites australis subsp. americanus is a perennial emergent grass found in tidal and inland marshes of the Atlantic coast of the United States. While rarely dominant, it grows in mixed communities and across much of this area its distribution has been reduced dramatically, likely due to eutrophication and the invasion of conspecific P. australis introduced from Europe. In this study, two noncoding cpDNA markers and six microsatellite loci were used to characterize genetic diversity among 58 remnant native P. australis stands from North Carolina to Maine. Five chloroplast DNA haplotypes were identified along with 42 multilocus genotypes. Bayesian exploration detected no population structure (e.g., optimal K = 1), indicating that these individuals form a single population. The analysis also detected no presence of hybrids of native and introduced P. australis in the samples, despite the close proximity of individuals to each other in many cases. These results suggest that the genetic composition of native P. australis across the region remains homogeneous and pure, providing managers with justification for its conservation and a potentially large source of germplasm for use in restoration activities.
C1 Smithsonian Trop Res Inst, Panama City, Panama.
RP Saltonstall, K (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama.
EM kristin.saltonstall@aya.yale.edu
NR 48
TC 19
Z9 19
U1 4
U2 44
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1566-0621
J9 CONSERV GENET
JI Conserv. Genet.
PD AUG
PY 2011
VL 12
IS 4
BP 1027
EP 1033
DI 10.1007/s10592-011-0205-1
PG 7
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 794FL
UT WOS:000292880800014
ER
PT J
AU Hartig, F
Calabrese, JM
Reineking, B
Wiegand, T
Huth, A
AF Hartig, Florian
Calabrese, Justin M.
Reineking, Bjoern
Wiegand, Thorsten
Huth, Andreas
TI Statistical inference for stochastic simulation models - theory and
application
SO ECOLOGY LETTERS
LA English
DT Review
DE Bayesian statistics; indirect inference; intractable likelihood; inverse
modelling; likelihood approximation; likelihood-free inference; maximum
likelihood; model selection; parameter estimation; stochastic simulation
ID APPROXIMATE BAYESIAN COMPUTATION; CHAIN MONTE-CARLO; MAXIMUM-LIKELIHOOD;
PARAMETER-ESTIMATION; COMMUNITY DYNAMICS; POPULATION-GROWTH; SYSTEMS;
SELECTION; DISPERSAL; ECOLOGY
AB Statistical models are the traditional choice to test scientific theories when observations, processes or boundary conditions are subject to stochasticity. Many important systems in ecology and biology, however, are difficult to capture with statistical models. Stochastic simulation models offer an alternative, but they were hitherto associated with a major disadvantage: their likelihood functions can usually not be calculated explicitly, and thus it is difficult to couple them to well-established statistical theory such as maximum likelihood and Bayesian statistics. A number of new methods, among them Approximate Bayesian Computing and Pattern-Oriented Modelling, bypass this limitation. These methods share three main principles: aggregation of simulated and observed data via summary statistics, likelihood approximation based on the summary statistics, and efficient sampling. We discuss principles as well as advantages and caveats of these methods, and demonstrate their potential for integrating stochastic simulation models into a unified framework for statistical modelling.
C1 [Hartig, Florian; Calabrese, Justin M.; Wiegand, Thorsten; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, D-04318 Leipzig, Germany.
[Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.
[Reineking, Bjoern] Univ Bayreuth, D-95440 Bayreuth, Germany.
RP Hartig, F (reprint author), UFZ Helmholtz Ctr Environm Res, Permoserstr 15, D-04318 Leipzig, Germany.
EM florian.hartig@ufz.de
RI Hartig, Florian/G-4510-2010; Calabrese, Justin/B-9131-2012; Wiegand,
Thorsten/H-5877-2016;
OI Hartig, Florian/0000-0002-6255-9059; Wiegand,
Thorsten/0000-0002-3721-2248; Reineking, Bjorn/0000-0001-5277-9181
FU ERC [233066]
FX We would like to thank Marti J. Anderson, Thomas Banitz, Joseph
Chipperfield and Carsten Dormann for comments and suggestions. We are
indebted to the insightful comments of three anonymous referees, which
greatly helped to improve this manuscript. F. H. was supported by ERC
advanced grant 233066 to T. W.
NR 100
TC 88
Z9 88
U1 11
U2 110
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD AUG
PY 2011
VL 14
IS 8
BP 816
EP 827
DI 10.1111/j.1461-0248.2011.01640.x
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 793ZY
UT WOS:000292864400012
PM 21679289
ER
PT J
AU Schad, J
Dechmann, DKN
Voigt, CC
Sommer, S
AF Schad, J.
Dechmann, D. K. N.
Voigt, C. C.
Sommer, S.
TI MHC class II DRB diversity, selection pattern and population structure
in a neotropical bat species, Noctilio albiventris
SO HEREDITY
LA English
DT Article
DE major histocompatibility complex polymorphism; selection; population
structure; neotropical bat; Noctilio albiventris; Panama
ID MAJOR HISTOCOMPATIBILITY COMPLEX; SACCOPTERYX-BILINEATA CHIROPTERA;
FREQUENCY-DEPENDENT SELECTION; NUCLEOTIDE SUBSTITUTION; OVERDOMINANT
SELECTION; REGION CONFIGURATIONS; PHYLOGENETIC ANALYSIS;
STATISTICAL-METHODS; MAXIMUM-LIKELIHOOD; POSITIVE SELECTION
AB Genes of the major histocompatibility complex (MHC) have a crucial role in the immune response of vertebrates, alter the individual odour and are involved in shaping mating preferences. Pathogen-mediated selection, sexual selection and maternal-fetal interactions have been proposed as the main drivers of frequently observed high levels of polymorphism in functionally important parts of the MHC. Bats constitute the second largest mammalian order and have recently emerged as important vectors of infectious diseases. In addition, Chiroptera are interesting study subjects in evolutionary ecology in the context of olfactory communication, mate choice and associated fitness benefits. Thus, it is surprising that they belong to the least studied mammalian taxa in terms of their MHC diversity. In this study, we investigated the variability in the functionally important MHC class II gene DRB, evidence for selection and population structure in the group-living lesser bulldog bat, Noctilio albiventris, in Panama. We found a single expressed, polymorphic Noal-DRB gene. The substitution pattern of the nucleotide sequences of the 18 detected alleles provided evidence for positive selection acting above the evolutionary history of the species in shaping MHC diversity. Roosting colonies were not genetically differentiated but females showed lower levels of heterozygosity than males, which might be a sign that the sexes differ in the selection pressures acting on the MHC. This study provides the prerequisites for further investigations of the role of the individual MHC constitution in parasite resistance, olfactory communication and mate choice in N. albiventris and other bats. Heredity (2011) 107, 115-126; doi:10.1038/hdy.2010.173; published online 19 January 2011
C1 [Schad, J.; Dechmann, D. K. N.; Voigt, C. C.; Sommer, S.] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany.
[Dechmann, D. K. N.] Max Planck Inst Ornithol, Vogelwarte Radolfzell, Radolfzell am Bodensee, Germany.
[Dechmann, D. K. N.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Sommer, S (reprint author), Leibniz Inst Zoo & Wildlife Res, Alfred Kowalke St 17, D-10315 Berlin, Germany.
EM sommer@izw-berlin.de
FU German Science Foundation [VO 890/11-1]
FX We thank Silke L Voigt-Heucke, Antje Kretzschmar, Megan Lupek, Martin
Wikelski and Apanie Wood for help with catching bats and sample
collection. We thank Wieslaw Babik for initial advice on the vectorette
PCR approach. We are grateful to Charles Gunn for linguistic advice. We
thank three anonymous reviewers for helpful comments on former versions
of the manuscript. The German Science Foundation funded C. Voigt, S.
Speck and D. Dechmann (VO 890/11-1). All capture and handling of
animals, as well as collection and export of samples were done in
concordance with Panamanian laws under permits from the Panamanian
authorities (ANAM) and under an IUCAC protocol. We are indebted to the
Smithsonian Tropical Research Institute and their staff for help with
logistics and interaction with the Panamanian authorities.
NR 109
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U1 4
U2 39
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0018-067X
EI 1365-2540
J9 HEREDITY
JI Heredity
PD AUG
PY 2011
VL 107
IS 2
BP 115
EP 126
DI 10.1038/hdy.2010.173
PG 12
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 794PD
UT WOS:000292911500004
PM 21245894
ER
PT J
AU Chuyong, GB
Kenfack, D
Harms, KE
Thomas, DW
Condit, R
Comita, LS
AF Chuyong, George B.
Kenfack, David
Harms, Kyle E.
Thomas, Duncan W.
Condit, Richard
Comita, Liza S.
TI Habitat specificity and diversity of tree species in an African wet
tropical forest
SO PLANT ECOLOGY
LA English
DT Article
DE Habitat specificity; Tree diversity; Topographically defined habitats;
Torus translation test; Tropical forest; Korup forest dynamics plot;
Cameroon
ID RAIN-FOREST; SOIL-PHOSPHORUS; ECTOMYCORRHIZAL TREES; EDAPHIC FACTORS;
NATIONAL-PARK; ASSOCIATIONS; DISTRIBUTIONS; CAMEROON; NUTRIENTS;
DIFFERENTIATION
AB Niche differentiation with respect to habitat has been hypothesized to shape patterns of diversity and species distributions in plant communities. African forests have been reported to be relatively less diverse compared to highly diversed regions of the Amazonian or Southeast Asian forests, and might be expected to have less niche differentiation. We examined patterns of structural and floristic differences among five topographically defined habitats for 494 species with stems a parts per thousand yen1 cm dbh in a 50-ha plot in Korup National Park, Cameroon. In addition, we tested for species-habitat associations for 272 species (with more than 50 individuals in the plot) using Torus translation randomization tests. Tree density and basal area were lowest in areas with negative convexity, which contained streams or were inundated during rainy periods and highest in moist well-drained habitats. Species composition and diversity varied along the topographical gradient from low flat to ridge top habitats. The low depression and low flat habitats were characterized by high diversity and similar species composition, relative to slopes, high gullies and ridge tops. Sixty-three percent of the species evaluated showed significant positive associations with at least one of the five habitat types. The majority of associations were with low depressions (75 species) and the fewest with ridge tops (8 species). The large number of species-habitat associations and the pronounced contrast between low (valley) and elevated (ridgetop) habitats in the Korup plot shows that niche differentiation with respect to edaphic variables (e.g., soil moisture, nutrients) contributes to local scale tree species distributions and to the maintenance of diversity in African forests.
C1 [Chuyong, George B.] Univ Buea, Dept Plant & Anim Sci, Buea, Cameroon.
[Kenfack, David] Harvard Univ, Arnold Arboretum, Ctr Trop Forest Sci, Cambridge, MA 02138 USA.
[Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA.
[Thomas, Duncan W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA.
[Condit, Richard] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Panama.
[Comita, Liza S.] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
RP Chuyong, GB (reprint author), Univ Buea, Dept Plant & Anim Sci, POB 63, Buea, Cameroon.
EM chuyong99@yahoo.com
OI Comita, Liza/0000-0002-9169-1331
FU U.S. National Science Foundation [DEB-9806828]; NSF [DEB 0211004, OISE
0314581, EF-0553768]; National Center for Ecological Analysis and
Synthesis; University of California, Santa Barbara; State of California
FX We thank the Ministry of Environment and Forests, Cameroon for
permission to conduct the field program in the Korup National Park. The
Korup FDP is affiliated with the Center for Tropical Forest Science, a
global network of large-scale demographic tree plots. Analyses were
partially supported by U.S. National Science Foundation award
DEB-9806828 to the Center for Tropical Forest Science of the Smithsonian
Institution. KEH acknowledges support from NSF (DEB 0211004 and OISE
0314581) that contributed toward the completion of this manuscript. LSC
acknowledges support from the National Center for Ecological Analysis
and Synthesis, a Center funded by NSF (Grant #EF-0553768), the
University of California, Santa Barbara, and the State of California.
NR 54
TC 22
Z9 25
U1 2
U2 38
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1385-0237
J9 PLANT ECOL
JI Plant Ecol.
PD AUG
PY 2011
VL 212
IS 8
BP 1363
EP 1374
DI 10.1007/s11258-011-9912-4
PG 12
WC Plant Sciences; Ecology; Forestry
SC Plant Sciences; Environmental Sciences & Ecology; Forestry
GA 793KM
UT WOS:000292820600011
ER
PT J
AU Dettai, A
Adamowizc, SJ
Allcock, L
Arango, CP
Barnes, DKA
Barratt, I
Chenuil, A
Couloux, A
Cruaud, C
David, B
Denis, F
Denys, G
Diaz, A
Eleaume, M
Feral, JP
Froger, A
Gallut, C
Grant, R
Griffiths, HJ
Held, C
Hemery, LG
Hosie, G
Kuklinski, P
Lecointre, G
Linse, K
Lozouet, P
Mah, C
Monniot, F
Norman, MD
O'Hara, T
Ozouf-Costaz, C
Piedallu, C
Pierrat, B
Poulin, E
Puillandre, N
Riddle, M
Samadi, S
Saucede, T
Schubart, C
Smith, PJ
Stevens, DW
Steinke, D
Strugnell, JM
Tarnowska, K
Wadley, V
Ameziane, N
AF Dettai, Agnes
Adamowizc, Sarah J.
Allcock, Louise
Arango, Claudia P.
Barnes, David K. A.
Barratt, Iain
Chenuil, Anne
Couloux, Arnaud
Cruaud, Corinne
David, Bruno
Denis, Francoise
Denys, Gael
Diaz, Angie
Eleaume, Marc
Feral, Jean-Pierre
Froger, Aurelie
Gallut, Cyril
Grant, Rachel
Griffiths, Huw J.
Held, Christoph
Hemery, Lenaig G.
Hosie, Graham
Kuklinski, Piotr
Lecointre, Guillaume
Linse, Katrin
Lozouet, Pierre
Mah, Christopher
Monniot, Francoise
Norman, Mark D.
O'Hara, Timothy
Ozouf-Costaz, Catherine
Piedallu, Claire
Pierrat, Benjamin
Poulin, Elie
Puillandre, Nicolas
Riddle, Martin
Samadi, Sarah
Saucede, Thomas
Schubart, Christoph
Smith, Peter J.
Stevens, Darren W.
Steinke, Dirk
Strugnell, Jan M.
Tarnowska, K.
Wadley, Victoria
Ameziane, Nadia
TI DNA barcoding and molecular systematics of the benthic and demersal
organisms of the CEAMARC survey
SO POLAR SCIENCE
LA English
DT Article
DE Barcode; Cytochrome oxidase 1; CEAMARC; Taxonomy; Systematics
AB The Dumont d'Urville Sea (East Antarctic region) has been less investigated for DNA barcoding and molecular taxonomy than other parts of the Southern Ocean, such as the Ross Sea and the Antarctic Peninsula. The Collaborative East Antarctic MARine Census (CEAMARC) took place in this area during the austral summer of 2007-2008. The Australian vessel RSV Aurora Australis collected very diverse samples of demersal and benthic organisms. The specimens were sorted centrally, and then distributed to taxonomic experts for molecular and morphological taxonomy and identification, especially barcoding. The COI sequences generated from CEAMARC material provide a sizeable proportion of the Census of Antarctic Marine Life barcodes although the studies are still ongoing, and represent the only source of sequences for a number of species. Barcoding appears to be a valuable method for identification within most groups, despite low divergences and haplotype sharing in a few species, and it is also useful as a preliminary taxonomic exploration method. Several new species are being described. CEAMARC samples have already provided new material for phylogeographic and phylogenetic studies in cephalopods, pycnogonids, teleost fish, crinoids and sea urchins, helping these studies to provide a better insight in the patterns of evolution in the Southern Ocean.
C1 [Dettai, Agnes; Denys, Gael; Eleaume, Marc; Froger, Aurelie; Gallut, Cyril; Hemery, Lenaig G.; Lecointre, Guillaume; Lozouet, Pierre; Monniot, Francoise; Ozouf-Costaz, Catherine; Piedallu, Claire; Puillandre, Nicolas; Samadi, Sarah; Ameziane, Nadia] Museum Natl Hist Nat, F-75231 Paris 05, France.
[Adamowizc, Sarah J.; Steinke, Dirk] Univ Guelph, Biodivers Inst Ontario, Canadian Ctr DNA Barcoding, Guelph, ON N1G 2W1, Canada.
[Allcock, Louise] Natl Univ Ireland Galway, Martin Ryan Marine Sci Inst, Galway, Ireland.
[Allcock, Louise; Barratt, Iain] Queens Univ Belfast, Sch Biol Sci, Belfast BT9 7BL, Antrim, North Ireland.
[Arango, Claudia P.] Queensland Museum, Biodivers Program, South Brisbane, Qld 4101, Australia.
[Barnes, David K. A.; Griffiths, Huw J.; Linse, Katrin] British Antarctic Survey, Cambridge CB3 0ET, England.
[Chenuil, Anne; Feral, Jean-Pierre; Tarnowska, K.] Univ Mediterranee CNRS, UMR DIMAR 6540, COM Stn Marine Endoume, Marseille, France.
[Couloux, Arnaud; Cruaud, Corinne] Ctr Natl Sequencage, Genoscope, F-91057 Evry, France.
[David, Bruno; Pierrat, Benjamin; Saucede, Thomas] Univ Bourgogne, CNRS, UMR Biogeosci 5561, Dijon, France.
[Denis, Francoise] Univ Maine, F-72000 Le Mans, France.
[Diaz, Angie; Poulin, Elie] Univ Chile, Fac Ciencias, Dept Ciencias Ecol, Inst Ecol & Biodiversidad, Santiago, Chile.
[Grant, Rachel] Univ Cambridge, Scott Polar Res Inst, Cambridge CB2 1ER, England.
[Held, Christoph] Alfred Wegener Inst Polar & Marine Res, D-27568 Bremerhaven, Germany.
[Hosie, Graham; Riddle, Martin; Wadley, Victoria] Australian Antarctic Div, Dept Sustainabil Environm Water Populat & Communi, Kingston, Tas 7050, Australia.
[Kuklinski, Piotr] Nat Hist Museum, London SW6 5BD, England.
[Kuklinski, Piotr] Polish Acad Sci, Inst Oceanol, PL-81712 Sopot, Poland.
[Mah, Christopher] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20007 USA.
[Norman, Mark D.; O'Hara, Timothy] Museum Victoria, Melbourne, Vic 3001, Australia.
[Schubart, Christoph] Univ Regensburg, D-93040 Regensburg, Germany.
[Smith, Peter J.; Stevens, Darren W.] Natl Inst Water & Atmospher Res NIWA, Wellington 6241, New Zealand.
[Strugnell, Jan M.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England.
RP Dettai, A (reprint author), Museum Natl Hist Nat, CP 26,43 Rue Cuvier, F-75231 Paris 05, France.
EM adettai@mnhn.fr
RI FERAL, Jean-Pierre/A-8199-2008; Steinke, Dirk/D-4700-2009; samadi,
sarah/G-5011-2010; Arango, Claudia/A-5531-2008; Allcock,
Louise/A-7359-2012; Poulin, Elie/C-2654-2012; CHENUIL, Anne
/E-3902-2012; Diaz, Angie/I-8033-2016; Strugnell, Jan/P-9921-2016;
OI FERAL, Jean-Pierre/0000-0001-7627-0160; Arango,
Claudia/0000-0003-1098-830X; Allcock, Louise/0000-0002-4806-0040;
Poulin, Elie/0000-0001-7736-0969; CHENUIL, Anne /0000-0001-8141-7147;
Diaz, Angie/0000-0003-4944-588X; Hemery, Lenaig/0000-0001-5337-4514
FU TRV Umitaka Maru (IPY project) [53]; Australian Antarctic Division;
Japanese Science Foundation; French polar institute IPEV (ICOTA
program); French polar institute IPEV (REVOLTA program); CNRS; MNHN; ANR
(White Project) [ANTFLOCKs USAR no07-BLAN-0213-01]; Consortium National
de Recherche en Genomique; 'Service de Systematique Moleculaire' of the
Museum national d'Histoire naturelle [IFR 101]; Polish Ministry of
Science and Higher Education [539/NCAML/2009/0]; Genome Canada through
the Ontario Genomics Institute; Alfred P. Sloan Foundation; Australian
Antarctic Science Grants [AA3010]; CAML coordination grant [34]; New
Zealand Government under the NZ International Polar Year-Census of
Antarctic Marine Life Project; "Action Transversale du MNHN : Taxonomie
moleculaire : DNA Barcode et gestion durable des collections"
(MNHN-Barcode initiative; co-PI Jean-Noel Labat and Sarah Samadi); Sloan
Foundation; ATM of MNHN "Biodiversite actuelle et fossile. Crises,
stress, restaurations et panchronisme : le message systematiqu"
FX We thank the crew and participants of the cruises involved in the
capture of the samples, and especially the chief scientists of the
CAML-CEAMARC cruises. The CAML-CEAMARC cruises of RSV Aurora Australis
and TRV Umitaka Maru (IPY project no53) were supported by the Australian
Antarctic Division, the Japanese Science Foundation, the French polar
institute IPEV (ICOTA and REVOLTA programs), the CNRS, the MNHN and the
ANR (White Project ANTFLOCKs USAR no07-BLAN-0213-01 directed by
Guillaume Lecointre). This project is a contribution to the EBA-SCAR
program.; This work was supported by the 'Consortium National de
Recherche en Genomique', and the 'Service de Systematique Moleculaire'
of the Museum national d'Histoire naturelle (IFR 101). It is part of the
agreement number 2005/67 between the Genoscope and the Museum national
d'Histoire naturelle on the project 'Macrophylogeny of life' directed by
Guillaume Lecointre. P. Kuklinski is also supported by the Polish
Ministry of Science and Higher Education (539/NCAML/2009/0). Funding for
barcoding at the CCDB was provided by Genome Canada through the Ontario
Genomics Institute. DS was supported by the Alfred P. Sloan Foundation.
Work on Pycnogonida is supported by the Australian Antarctic Science
Grants (project AA3010), and CAML coordination grant #34 to C. P.
Arango. New Zealand authors were supported by research funded by the New
Zealand Government under the NZ International Polar Year-Census of
Antarctic Marine Life Project. Part of the work in the MNHN was
supported by the "Action Transversale du MNHN : Taxonomie moleculaire :
DNA Barcode et gestion durable des collections" (MNHN-Barcode
initiative; co-PI Jean-Noel Labat and Sarah Samadi); part of these data
fed the MarBol project supported by the Sloan Foundation. This work was
also supported by the ATM of MNHN "Biodiversite actuelle et fossile.
Crises, stress, restaurations et panchronisme : le message systematiqu".
NR 84
TC 9
Z9 9
U1 1
U2 14
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1873-9652
EI 1876-4428
J9 POLAR SCI
JI Polar Sci.
PD AUG
PY 2011
VL 5
IS 2
BP 298
EP 312
DI 10.1016/j.polar.2011.02.002
PG 15
WC Ecology; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA V33ZX
UT WOS:000209057800018
ER
PT J
AU Freeman, EW
Meyer, JM
Putman, S
Schulte, BA
Brown, JL
AF Freeman, Elizabeth W.
Meyer, Jordana M.
Putman, Sarah
Schulte, Bruce A.
Brown, Janine L.
TI Using a simplified field progestagen method to assess ovarian activity
in female African elephants
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE African elephants; Loxodonta africana; Non-invasive endocrinology;
Pregnancy
ID LOXODONTA-AFRICANA; SOUTH-AFRICA; NATIONAL-PARK; NORTH-AMERICA;
POPULATION; PREGNANCY; ENDOCRINOLOGY; URINARY; STRESS;
IMMUNOCONTRACEPTION
AB Non-invasive endocrine monitoring is an important conservation tool frequently used to support the management of wildlife species. Investigating ovarian activity and pregnancy rates of free-ranging African elephants can enhance our knowledge about the physiology of this highly social and long-lived species. The utility of a new, field-friendly progestagen enzymeimmunoassay (EIA) method was tested by monitoring ovarian activity of 40 females in Addo Elephant National Park (AENP), South Africa. Fecal samples were collected opportunistically from known individuals (June 2007-September 2009) and fecal progestagen metabolites (FPM) were extracted in the field and analyzed on-site using a visual, qualitative EIA. Those results were compared to the laboratory quantitative EIA assessment of hormone concentrations in the U.S. Qualitative FPM concentrations were strongly correlated with quantitative concentrations (r(s) = 0.72). Fecal samples collected from pregnant elephants (n = 22) had significantly higher FPM concentrations than non-pregnant individuals, and month of gestation was the strongest predictor of FPM concentrations. Endocrine profiles suggested that five older females were no longer cycling normally. Simplified field endocrine techniques could transform endangered species research under field conditions and provide reliable and economical new tools for making sensible conservation management decisions based on real-time hormone results. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Freeman, Elizabeth W.] George Mason Univ, New Century Coll, Fairfax, VA 22030 USA.
[Freeman, Elizabeth W.; Meyer, Jordana M.; Putman, Sarah; Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA.
[Schulte, Bruce A.] Western Kentucky Univ, Dept Biol, Bowling Green, KY 42101 USA.
RP Freeman, EW (reprint author), George Mason Univ, New Century Coll, 4400 Univ Dr,MS 5D3, Fairfax, VA 22030 USA.
EM efreeman@gmu.edu
FU Smithsonian Women's Committee; International Elephant Foundation;
Division of Integrative Biology and Neuroscience of the National Science
Foundation [02-17062, -17068, -16862]
FX We wish to thank Laura Broederdorf, Michelle Schroeder, and Remy
Schoenemann for their assistance with fecal sample collection and
processing. The authors would like to acknowledge the support of the
Smithsonian Women's Committee, Walcott Endowment and Scholarly Studies
Program, as well as the International Elephant Foundation. The fieldwork
was performed with the permission (Permit # 2002-12-11 BSCH) and support
of personnel in the South African National Parks, particularly Addo
Elephant National Park. Support for the field site was provided by the
Division of Integrative Biology and Neuroscience of the National Science
Foundation (Award Nos. 02-17062, -17068 and -16862 to BAS, Thomas
Goodwin and the late L.E.L. "Bets" Rasmussen, respectively).
NR 50
TC 5
Z9 5
U1 1
U2 13
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 AUG
PY 2011
VL 144
IS 8
BP 2105
EP 2111
DI 10.1016/j.biocon.2011.04.033
PG 7
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 791JJ
UT WOS:000292661200006
ER
PT J
AU Innis, AF
Forseth, IN
Whigham, DF
McCormick, MK
AF Innis, Anne F.
Forseth, Irwin N.
Whigham, Dennis F.
McCormick, Melissa K.
TI Genetic diversity in the invasive Rubus phoenicolasius as compared to
the native Rubus argutus using inter-simple sequence repeat (ISSR)
markers
SO BIOLOGICAL INVASIONS
LA English
DT Article
DE Rubus phoenicolasius; Rubus argutus; Invasive; ISSR; Genetic diversity
ID LIFE-HISTORY TRAITS; CYTISUS-SCOPARIUS; ALIEN PLANTS; CHINA;
POPULATIONS; WEED
AB Invasive species are one of most significant factors in human-influenced global change. Management actions that prevent the spread and impacts of invasive species require knowledge of their ecological and genetic characteristics. The genetic characteristics of the invasive wine raspberry, Rubus phoenicolasius Maxim. (Rosaceae) and the native sawtooth blackberry, Rubus argutus Link, were examined in two forest habitats on the Maryland Coastal Plain. Using inter-simple sequence repeat (ISSR) markers we quantified the genetic diversity of both species. We analyzed genetic diversity using analysis of molecular variance (AMOVA) and found less genetic diversity in the invasive species, R. phoenicolasius, with variation between sites was 0.418 between sites and 0.075 within sites as compared to the native, R. argutus, where the variation between sites was 1.538 and 0.370 within sites. The lower genetic diversity in the invasive may be due to a history of limited introductions or frequent self-fertilization and clonal reproduction.
C1 [Innis, Anne F.; Forseth, Irwin N.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Innis, Anne F.; Whigham, Dennis F.; McCormick, Melissa K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Innis, AF (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
EM anneinnis@yahoo.com
OI Whigham, Dennis/0000-0003-1488-820X
FU Smithsonian Graduate Fellowship; University of Maryland
FX This research was supported by the Smithsonian Graduate Fellowship and
the Chesapeake Bay Fund of the University of Maryland.
NR 24
TC 3
Z9 4
U1 0
U2 27
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1387-3547
J9 BIOL INVASIONS
JI Biol. Invasions
PD AUG
PY 2011
VL 13
IS 8
BP 1735
EP 1738
DI 10.1007/s10530-011-0012-0
PG 4
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 789YS
UT WOS:000292556200005
ER
PT J
AU Meskens, C
Mckenna, D
Hance, T
Windsor, D
AF Meskens, Christophe
Mckenna, Duane
Hance, Thierry
Windsor, Donald
TI Host plant taxonomy and phenotype influence the structure of a
neotropical host plant-hispine beetle food web
SO ECOLOGICAL ENTOMOLOGY
LA English
DT Article
DE Chrysomelidae; food web; hispine beetles; host specificity; modular
structure; modularity; nestedness; niche overlap
ID ANIMAL MUTUALISTIC NETWORKS; TROPICAL FORESTS; ECOLOGICAL NETWORKS; LEAF
BEETLES; INSECT HERBIVORES; TROPHIC NETWORKS; CHRYSOMELIDAE;
SPECIALIZATION; SPECIFICITY; NESTEDNESS
AB 1. Past studies of plant-phytophage communities have encountered both nested and modular/compartmented food web structures, revealing potentially important differences in the nature of interactions.
2. We analysed qualitatively and quantitatively a taxonomically resolved plant-hispine beetle food web from Panama (lower Central America) to characterise its structure. The study included all beetles in the subfamily Cassidinae (Chrysomelidae) found feeding on common monocotyledonous plants in the Tropical forest understorey and edge habitats.
3. Nestedness, a structural property common to many food webs, was not observed in this study, however strong evidence for a modular structure was uncovered.
4. Our findings suggest the feeding niches of hispine beetles are constrained within module boundaries, which largely correspond to plant ordinal and familial limits, and secondarily to plant attributes, including the morphology of immature leaves.
5. We conclude that modularity in this food web is largely a product of narrow, discrete hispine beetle host specificity for larger phylogenetically related plant taxa.
C1 [Meskens, Christophe; Hance, Thierry] Catholic Univ Louvain, Biodivers Res Ctr, Earth & Life Inst, B-1348 Louvain, Belgium.
[Mckenna, Duane] Univ Memphis, Dept Biol, Memphis, TN 38152 USA.
[Windsor, Donald] Smithsonian Trop Res Inst, Ancon, Panama.
RP Meskens, C (reprint author), Catholic Univ Louvain, Biodivers Res Ctr, Earth & Life Inst, 4-5 Pl Croix Sud, B-1348 Louvain, Belgium.
EM cmeskens@yahoo.fr
RI McKenna, Duane/H-2252-2011
FU FRFC (Belgium); UCL-FSR (Belgium); Fonds Leopold III pour l'Exploration
et la Conservation de la Nature - Belgium; Earth and Life Institute of
the Universite catholique de Louvain (Belgium); Smithsonian Tropical
Research Institute (STRI-Panama); Autoridad National del Ambiante (ANAM
- Panama) [DAPVS-01-2007, 2008]
FX The authors thank Ph. Lebrun, A. Descampe, M. Pigeon, P. Guimaraes, J.
Bascompte, and two anonymous reviewers for suggestions and comments that
improved analyses and content. We acknowledge R. Guimera and L. Amaral
for providing their software (NETCARTO). This work was funded by a FRFC
grant (Belgium), an UCL-FSR PhD fellowship (Belgium) and by a research
travel grant (Fonds Leopold III pour l'Exploration et la Conservation de
la Nature - Belgium). Additional funding, and logistical and
collaborative support was given by the Earth and Life Institute of the
Universite catholique de Louvain (Belgium), the Smithsonian Tropical
Research Institute (STRI-Panama), and Autoridad National del Ambiante
(ANAM - Panama; Scientific Permits: DAPVS-01-2007, 2008). The present
publication is number BRC 130 of the Biodiversity Research Centre
(BDIV-UCL, Belgium).
NR 67
TC 8
Z9 8
U1 0
U2 18
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0307-6946
J9 ECOL ENTOMOL
JI Ecol. Entomol.
PD AUG
PY 2011
VL 36
IS 4
BP 480
EP 489
DI 10.1111/j.1365-2311.2011.01294.x
PG 10
WC Entomology
SC Entomology
GA 791TU
UT WOS:000292689900010
ER
PT J
AU Brown, SD
Wall, JD
Kucken, AM
Gilmour, CC
Podar, M
Brandt, CC
Teshima, H
Detter, JC
Han, CS
Land, ML
Lucas, S
Han, J
Pennacchio, L
Nolan, M
Pitluck, S
Woyke, T
Goodwin, L
Palumbo, AV
Elias, DA
AF Brown, Steven D.
Wall, Judy D.
Kucken, Amy M.
Gilmour, Cynthia C.
Podar, Mircea
Brandt, Craig C.
Teshima, Hazuki
Detter, John C.
Han, Cliff S.
Land, Miriam L.
Lucas, Susan
Han, James
Pennacchio, Len
Nolan, Matt
Pitluck, Sam
Woyke, Tanja
Goodwin, Lynne
Palumbo, Anthony V.
Elias, Dwayne A.
TI Genome Sequence of the Mercury-Methylating and Pleomorphic Desulfovibrio
africanus Strain Walvis Bay
SO JOURNAL OF BACTERIOLOGY
LA English
DT Article
ID SULFATE-REDUCING BACTERIUM; DESULFURICANS LS
AB Desulfovibrio africanus strain Walvis Bay is an anaerobic sulfate-reducing bacterium capable of producing methylmercury (MeHg), a potent human neurotoxin. The mechanism of methylation by this and other organisms is unknown. We present the 4.2-Mb genome sequence to provide further insight into microbial mercury methylation and sulfate-reducing bacteria.
C1 [Brown, Steven D.; Podar, Mircea; Brandt, Craig C.; Land, Miriam L.; Palumbo, Anthony V.; Elias, Dwayne A.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA.
[Wall, Judy D.; Kucken, Amy M.] Univ Missouri, Div Biochem, Columbia, MO 65211 USA.
[Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Teshima, Hazuki; Detter, John C.; Han, Cliff S.; Goodwin, Lynne] Los Alamos Natl Lab, Biosci Div, Los Alamos, NM 87545 USA.
[Teshima, Hazuki; Detter, John C.; Han, Cliff S.; Land, Miriam L.; Lucas, Susan; Han, James; Pennacchio, Len; Nolan, Matt; Pitluck, Sam; Woyke, Tanja; Goodwin, Lynne] DOE Joint Genome Inst, Walnut Creek, CA 94598 USA.
RP Brown, SD (reprint author), Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA.
EM brownsd@ornl.gov
RI Gilmour, Cynthia/G-1784-2010; Palumbo, Anthony/A-4764-2011; Elias,
Dwayne/B-5190-2011; Land, Miriam/A-6200-2011; Brown, Steven/A-6792-2011;
OI Gilmour, Cynthia/0000-0002-1720-9498; Palumbo,
Anthony/0000-0002-1102-3975; Elias, Dwayne/0000-0002-4469-6391; Land,
Miriam/0000-0001-7102-0031; Brown, Steven/0000-0002-9281-3898; Podar,
Mircea/0000-0003-2776-0205
FU Office of Biological and Environmental Research (OBER); Office of
Science, U.S. Department of Energy (DOE) [DE-AC02-05CH11231]; U.S.
Department of Energy [DE-AC05-00OR22725]; [DE-FG02-073464396]
FX This research was supported by the Office of Biological and
Environmental Research (OBER), Office of Science, U.S. Department of
Energy (DOE), as part of the Mercury Science Focus Area Program at Oak
Ridge National Laboratory and by grant DE-FG02-073464396 (to J.D.W.).
Oak Ridge National Laboratory is managed by UT-Battelle, LLC, for the
U.S. Department of Energy under contract DE-AC05-00OR22725. The work
conducted by the U.S. Department of Energy Joint Genome Institute is
supported by the Office of Science of the U.S. Department of Energy
under contract no. DE-AC02-05CH11231.
NR 22
TC 5
Z9 6
U1 0
U2 8
PU AMER SOC MICROBIOLOGY
PI WASHINGTON
PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA
SN 0021-9193
J9 J BACTERIOL
JI J. Bacteriol.
PD AUG
PY 2011
VL 193
IS 15
BP 4037
EP 4038
DI 10.1128/JB.05223-11
PG 2
WC Microbiology
SC Microbiology
GA 791WF
UT WOS:000292698100049
PM 21642452
ER
PT J
AU Thompson, JR
Spies, TA
Olsen, KA
AF Thompson, Jonathan R.
Spies, Thomas A.
Olsen, Keith A.
TI Canopy damage to conifer plantations within a large mixed-severity
wildfire varies with stand age
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE Biscuit Fire; Burn severity; Land use legacy; Klamath Mountains; Random
Forest analysis; Geostatistical regression
ID SOUTHWESTERN OREGON; RANDOM FORESTS; FIRE SEVERITY; CROWN FIRE;
CLASSIFICATION; PRODUCTIVITY; CALIFORNIA; MOUNTAINS; CLIMATE; MODEL
AB The 2002 Biscuit Fire burned at mixed-severities encompassing over 200,000 ha of publicly owned forest-land, including more than 8300 ha of conifer plantations. We used pre- and post-fire digital aerial photography to examine how the level of canopy damage varied within these plantations in relation to topography, weather, vegetation-cover, and management history, with an emphasis on the age of the plantation. We examined 198 plantations that varied widely in age (5-47 years), size (1.25-47 ha), and landscape context. The average level of canopy damage within the plantations was 77%. Based on Random Forest variable importance values, plantation age was the best predictor of canopy damage. Average annual precipitation, elevation and topographic position were ranked second, third, and fourth, respectively. A model selection procedure, using geo-statistical regression models and Akaike's information criterion, corroborated the importance of plantation age relative to the other predictors tested and also suggested that the influence of age varied over time. The top ranked regression model indicated that the level of canopy damage reached its maximum around age 15 and stayed relatively high until age 25 before declining. Published by Elsevier B.V.
C1 [Thompson, Jonathan R.] Smithsonian Conservat Biol Inst, Smithsonian Inst, Front Royal, VA 22630 USA.
[Spies, Thomas A.] US Forest Serv, USDA, Pacific NW Res Stn, Corvallis, OR 97331 USA.
[Olsen, Keith A.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA.
RP Thompson, JR (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Inst, 1500 Remt Rd, Front Royal, VA 22630 USA.
EM thompsonjr@si.edu; tspies@fs.fed.us; keith.olsen@oregonstate.edu
FU Joint Fire Science Program
FX This research was funded by the Joint Fire Science Program. We thank
Duck Creek Inc., for technical help and W. Cohen, T. Atzet, and R.
Miller for helpful reviews.
NR 34
TC 7
Z9 7
U1 0
U2 10
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD AUG 1
PY 2011
VL 262
IS 3
BP 355
EP 360
DI 10.1016/j.foreco.2011.04.001
PG 6
WC Forestry
SC Forestry
GA 788EP
UT WOS:000292428500007
ER
PT J
AU Crofoot, MC
Rubenstein, DI
Maiya, AS
Berger-Wolf, TY
AF Crofoot, Margaret C.
Rubenstein, Daniel I.
Maiya, Arun S.
Berger-Wolf, Tanya Y.
TI Aggression, Grooming and Group-Level Cooperation in White-Faced
Capuchins (Cebus capucinus): Insights From Social Networks
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Article
DE intergroup competition; social network analysis; Barro Colorado Island;
collective action
ID FEMALE BABOONS; CLIQUE IDENTIFICATION; ASSOCIATION PATTERNS; MONKEYS;
DOMINANCE; PRIMATES; BEHAVIOR; RECIPROCITY; STRATEGIES; CENTRALITY
AB The form of animal social systems depends on the nature of agonistic and affiliative interactions. Social network theory provides tools for characterizing social structure that go beyond simple dyadic interactions and consider the group as a whole. We show three groups of capuchin monkeys from Barro Colorado Island, Panama, where there are strong connections between key aspects of aggression, grooming, and proximity networks, and, at least among females, those who incur risk to defend their group have particular "social personalities.'' Although there is no significant correlation for any of the network measures between giving and receiving aggression, suggesting that dominance relationships do not follow a simple hierarchy, strong correlations emerge for many measures between the aggression and grooming networks. At the local, but not global, scale, receiving aggression and giving grooming are strongly linked in all groups. Proximity shows no correlation with aggression at either the local or the global scale, suggesting that individuals neither seek out nor avoid aggressors. Yet, grooming has a global but not local connection to proximity. Extensive groomers who tend to direct their efforts at other extensive groomers also spend time in close proximity to many other individuals. These results indicate the important role that prosociality plays in shaping female social relationships. We also show that females who receive the least aggression, and thus pay low costs for group living, are most likely to participate in group defense. No consistent "social personality'' traits characterize the males who invest in group defense. Am. J. Primatol. 73:821-833, 2011. (C) 2011 Wiley-Liss, Inc.
C1 [Crofoot, Margaret C.; Rubenstein, Daniel I.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
[Crofoot, Margaret C.] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany.
[Crofoot, Margaret C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Maiya, Arun S.; Berger-Wolf, Tanya Y.] Univ Illinois, Dept Comp Sci, Chicago, IL USA.
RP Rubenstein, DI (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, 106A Guyot Hall, Princeton, NJ 08544 USA.
EM dir@princeton.edu
OI Berger-Wolf, Tanya/0000-0001-7610-1412
FU Smithsonian Tropical Research Institute; Max Planck Institute for
Ornithology; Department of Migration and Immuno-ecology; Princeton
University; Wenner-Gren Foundation for Anthropological Research; NSF
[IIS-0705822, IIS-0747369]
FX Contract grant sponsors: Smithsonian Tropical Research Institute, the
Max Planck Institute for Ornithology, Department of Migration and
Immuno-ecology, Princeton University, and the Wenner-Gren Foundation for
Anthropological Research; NSF; Contract grant numbers: IIS-0705822;
IIS-0747369.
NR 70
TC 18
Z9 19
U1 4
U2 71
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0275-2565
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD AUG
PY 2011
VL 73
IS 8
SI SI
BP 821
EP 833
DI 10.1002/ajp.20959
PG 13
WC Zoology
SC Zoology
GA 781RG
UT WOS:000291950600012
PM 21590698
ER
PT J
AU Bayona, G
Montes, C
Cardona, A
Jaramillo, C
Ojeda, G
Valencia, V
Ayala-Calvo, C
AF Bayona, German
Montes, Camilo
Cardona, Agustin
Jaramillo, Carlos
Ojeda, German
Valencia, Victor
Ayala-Calvo, Carolina
TI Intraplate subsidence and basin filling adjacent to an oceanic
arc-continent collision: a case from the southern Caribbean-South
America plate margin
SO BASIN RESEARCH
LA English
DT Article
ID NEOTROPICAL RAIN-FOREST; SIERRA-DE-PERIJA; TECTONIC EVOLUTION; MARACAIBO
BASIN; CERREJON FORMATION; COLOMBIAN ANDES; FORELAND BASIN; PALEOCENE;
VENEZUELA; GEOCHRONOLOGY
AB The upper Campanian-Lower Eocene synorogenic sedimentary wedge of the Rancheria Basin was deposited in an intraplate basin resting on a tilted continental crustal block that was deformed by collision and subsequent subduction of the Caribbean Plate. Upper Cretaceous-Lower Eocene strata rest unconformably upon Jurassic igneous rocks of the Santa Marta Massif, with no major thrust faults separating the Santa Marta Massif from the Rancheria Basin. The upper Campanian-Lower Eocene succession includes, from base to top: foraminifera-rich calcareous mudstone, mixed carbonate-siliciclastic strata and mudstone, coal and immature fluvial sandstone beds. Diachronous collision and eastward tilting of the plate margin (Santa Marta Massif and Central Cordillera) favoured the generation of accommodation space in a continuous intraplate basin (Rancheria, Cesar and western Maracaibo) during the Maastrichtian to Late Palaeocene. Terrigenous detritus from the distal colliding margin filled the western segments of the continuous intraplate basin (Rancheria and Cesar Basins); in the Late Paleocene, continental depositional systems migrated eastwards as far as the western Maracaibo Basin. In Early Eocene time, reactivation of former extensional structures fragmented the intraplate basin into the Rancheria-Cesar Basins to the west, and the western Maracaibo Basin and Palmar High to the East. This scenario of continent-oceanic arc collision, crustal-scale tilting, intraplate basin generation and fault reactivation may apply for Upper Cretaceous-Palaeogene syntectonic basins in western Colombia and Ecuador, and should be considered in other settings where arc-continent collision is followed by subduction.
C1 [Bayona, German; Montes, Camilo; Cardona, Agustin; Ayala-Calvo, Carolina] Corp Geol ARES, Bogota, Colombia.
[Bayona, German; Montes, Camilo; Cardona, Agustin; Jaramillo, Carlos] Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
[Ojeda, German] ECOPETROL SA, Bogota, Colombia.
[Valencia, Victor] Washington State Univ, Sch Earth & Environm Sci, Pullman, WA 99164 USA.
RP Bayona, G (reprint author), Corp Geol ARES, Bogota, Colombia.
EM gbayona@cgares.org
OI Montes, Camilo/0000-0002-3553-0787
FU Corporacion Geologica ARES; Smithsonian Tropical Research Institute
FX Carbones del Cerrejon supplied field and travel expenses for this
research, as well as the access to surface and subsurface data from 2004
to 2007. We thank Carbones del Guasare S. A. for access to surface and
subsurface data in the Paso Diablo coal mine. Additional financial
support for this project comes from Corporacion Geologica ARES and the
Smithsonian Tropical Research Institute. We thank Omar Montenegro and
Carolina Ojeda for analysing petrographic samples of the uppermost
Cerrejon Formation, Hernando Mahecha and John Rico for designing some
figures and Natasha Atkins for editorial corrections. We also thank the
Agencia Nacional de Hidrocarburos and Carbones del Cerrejon for
permission to publish seismic lines and for access to biostratigraphic
data for Well B. We acknowledge comments and suggestions of Etienne
Jaillard, James Pindell, Peter DeCelles, Andrea Fildani and an anonymous
reviewer on an earlier version of this manuscript, which greatly
improved the content of this manuscript. We appreciate the detailed
editorial suggestions and comments of the editor, Peter van der Beek,
which helped to improve the presentation of data and ideas.
NR 66
TC 17
Z9 19
U1 2
U2 14
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0950-091X
EI 1365-2117
J9 BASIN RES
JI Basin Res.
PD AUG
PY 2011
VL 23
IS 4
BP 403
EP 422
DI 10.1111/j.1365-2117.2010.00495.x
PG 20
WC Geosciences, Multidisciplinary
SC Geology
GA 786WO
UT WOS:000292338800002
ER
PT J
AU Powell, S
AF Powell, S.
TI How much do army ants eat? On the prey intake of a neotropical
top-predator
SO INSECTES SOCIAUX
LA English
DT Article
DE Army ants; Predation; Diet; Column raid; Swarm raid; Biomass
ID ECITON-BURCHELLI; COLONY; HYMENOPTERA; FORMICIDAE; ECOLOGY; RATES
AB New World army ants (Ecitoninae) are nomadic group-predators that are widely thought to have a substantial impact on their prey. Nevertheless, quantitative data on prey intake by army ants is scarce and mostly limited to chance encounters. Here, I quantify the prey intake of the army ant Eciton hamatum at the contrasting scales of raid, colony (sum of simultaneous raids), and population. Like most army ants, E. hamatum conducts narrow 'column raids' and has a specialized diet of ant prey. I show that individual raids often had periods of no prey intake, and raid intake rates, calculated in g/min, differed significantly among colonies. Moreover, neither mean nor peak raid intake rates were correlated with colony size. Similarly, colony intake rates differed significantly among colonies, and mean colony intake rates were not correlated with colony size. However, mean colony intake rates were significantly higher than mean raid intake rates, and peak colony intake rate was correlated with colony size. Having multiple raids thus improves colony-level intake rates, and larger colonies can harvest more prey per unit time. Mean colony intake rate across colonies was 0.067 g/min dry weight and mean daily colony intake was calculated at 38.2 g. This intake is comparable to that of Eciton burchellii, which has a more generalized diet and conducts spectacular 'swarm raids' that are seen as having a greater impact on prey than column raids. Population size on Barro Colorado Island, Panama, was estimated to be 57 colonies, which extrapolates to a daily population intake of nearly 2 kg of prey dry weight, or 120 g/km(2). Broadly, these findings demonstrate that column raiding army ants experience considerable variation in prey intake for individual raids, but can still achieve notable impact at the larger scales of colony and population. Furthermore, they challenge the idea that swarm-raiding species necessarily have greater intake and thus impact on prey. Instead, I suggest that conducting multiple column raids may be a strategy that allows for comparable intake from a more specialized diet.
C1 [Powell, S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Powell, S (reprint author), Univ Arizona, Dept Ecol & Evolut Biol, BioSci W Room 310,1041 E Lowell St, Tucson, AZ 85721 USA.
EM scottpowell@mac.com
FU Smithsonian Tropical Research Institute, Panama
FX This manuscript is dedicated to Carl W. Rettenmeyer. His positive
influence on my career and life are immeasurable. I also thank Ellie
Clark, Egbert G. Leigh Jr., and William T. Wcislo for valuable
discussion, as well as the staff of the Smithsonian Tropical Research
Institute for logistical support. This research was funded primarily by
a Short-Term Fellowship from the Smithsonian Tropical Research
Institute, Panama, with additional support from Carl Rettenmeyer.
NR 31
TC 5
Z9 6
U1 1
U2 26
PU BIRKHAUSER VERLAG AG
PI BASEL
PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND
SN 0020-1812
J9 INSECT SOC
JI Insect. Soc.
PD AUG
PY 2011
VL 58
IS 3
BP 317
EP 324
DI 10.1007/s00040-011-0152-3
PG 8
WC Entomology
SC Entomology
GA 782XJ
UT WOS:000292045800006
ER
PT J
AU Sarkar, IN
Trizna, M
AF Sarkar, Indra Neil
Trizna, Michael
TI The Barcode of Life Data Portal: Bridging the Biodiversity Informatics
Divide for DNA Barcoding
SO PLOS ONE
LA English
DT Article
ID TAXONOMY; BIOINFORMATICS; SOFTWARE; GENETICS; TOOL
AB With the volume of molecular sequence data that is systematically being generated globally, there is a need for centralized resources for data exploration and analytics. DNA Barcode initiatives are on track to generate a compendium of molecular sequence-based signatures for identifying animals and plants. To date, the range of available data exploration and analytic tools to explore these data have only been available in a boutique form-often representing a frustrating hurdle for many researchers that may not necessarily have resources to install or implement algorithms described by the analytic community. The Barcode of Life Data Portal (BDP) is a first step towards integrating the latest biodiversity informatics innovations with molecular sequence data from DNA barcoding. Through establishment of community driven standards, based on discussion with the Data Analysis Working Group (DAWG) of the Consortium for the Barcode of Life (CBOL), the BDP provides an infrastructure for incorporation of existing and next-generation DNA barcode analytic applications in an open forum.
C1 [Sarkar, Indra Neil] Univ Vermont, Ctr Clin & Translat Sci, Burlington, VT 05405 USA.
[Sarkar, Indra Neil] Univ Vermont, Dept Microbiol & Mol Genet, Burlington, VT 05405 USA.
[Sarkar, Indra Neil] Univ Vermont, Dept Comp Sci, Burlington, VT USA.
[Trizna, Michael] Smithsonian Inst, Consortium Barcode Life, Washington, DC 20560 USA.
RP Sarkar, IN (reprint author), Univ Vermont, Ctr Clin & Translat Sci, Burlington, VT 05405 USA.
EM neil.sarkar@uvm.edu
OI Trizna, Michael/0000-0002-0537-8382; Sarkar, Indra
Neil/0000-0003-2054-7356
FU National Institutes of Health [R01LM009725]; Alfred P. Sloan Foundation
FX INS is supported in part by a grant from the National Institutes of
Health (R01LM009725). Financial support for much of the Data Analysis
Working Group (DAWG) activities, including the development of the
Barcode of Life Data Portal (BDP), is primarily from the Alfred P. Sloan
Foundation. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript.
NR 18
TC 10
Z9 11
U1 2
U2 13
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUL 27
PY 2011
VL 6
IS 7
AR e14689
DI 10.1371/journal.pone.0014689
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 799JJ
UT WOS:000293282700001
PM 21818249
ER
PT J
AU Miller, W
Hayes, VM
Ratan, A
Petersen, DC
Wittekindt, NE
Miller, J
Walenz, B
Knight, J
Qi, J
Zhao, FQ
Wang, QY
Bedoya-Reina, OC
Katiyar, N
Tomsho, LP
Kasson, LM
Hardie, RA
Woodbridge, P
Tindall, EA
Bertelsen, MF
Dixon, D
Pyecroft, S
Helgen, KM
Lesk, AM
Pringle, TH
Patterson, N
Zhang, Y
Kreiss, A
Woods, GM
Jones, ME
Schuster, SC
AF Miller, Webb
Hayes, Vanessa M.
Ratan, Aakrosh
Petersen, Desiree C.
Wittekindt, Nicola E.
Miller, Jason
Walenz, Brian
Knight, James
Qi, Ji
Zhao, Fangqing
Wang, Qingyu
Bedoya-Reina, Oscar C.
Katiyar, Neerja
Tomsho, Lynn P.
Kasson, Lindsay McClellan
Hardie, Rae-Anne
Woodbridge, Paula
Tindall, Elizabeth A.
Bertelsen, Mads Frost
Dixon, Dale
Pyecroft, Stephen
Helgen, Kristofer M.
Lesk, Arthur M.
Pringle, Thomas H.
Patterson, Nick
Zhang, Yu
Kreiss, Alexandre
Woods, Gregory M.
Jones, Menna E.
Schuster, Stephan C.
TI Genetic diversity and population structure of the endangered marsupial
Sarcophilus harrisii (Tasmanian devil)
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE wildlife conservation; ancient DNA; population genetics; semiconductor
sequencing; selective breeding
ID FACIAL-TUMOR DISEASE; GENOME SEQUENCE; CANCER; TRANSMISSION
AB The Tasmanian devil (Sarcophilus harrisii) is threatened with extinction because of a contagious cancer known as Devil Facial Tumor Disease. The inability to mount an immune response and to reject these tumors might be caused by a lack of genetic diversity within a dwindling population. Here we report a whole-genome analysis of two animals originating from extreme northwest and southeast Tasmania, the maximal geographic spread, together with the genome from a tumor taken from one of them. A 3.3-Gb de novo assembly of the sequence data from two complementary next-generation sequencing platforms was used to identify 1 million polymorphic genomic positions, roughly one-quarter of the number observed between two genetically distant human genomes. Analysis of 14 complete mitochondrial genomes from current and museum specimens, as well as mitochondrial and nuclear SNP markers in 175 animals, suggests that the observed low genetic diversity in today's population preceded the Devil Facial Tumor Disease disease outbreak by at least 100 y. Using a genetically characterized breeding stock based on the genome sequence will enable preservation of the extant genetic diversity in future Tasmanian devil populations.
C1 [Hayes, Vanessa M.; Petersen, Desiree C.; Hardie, Rae-Anne; Woodbridge, Paula; Tindall, Elizabeth A.] Childrens Canc Inst Australia, Randwick, NSW 2031, Australia.
[Hayes, Vanessa M.; Petersen, Desiree C.; Hardie, Rae-Anne; Woodbridge, Paula; Tindall, Elizabeth A.] Univ New S Wales, Lowy Canc Res Ctr, Randwick, NSW 2031, Australia.
[Miller, Webb; Ratan, Aakrosh; Wittekindt, Nicola E.; Qi, Ji; Zhao, Fangqing; Wang, Qingyu; Bedoya-Reina, Oscar C.; Katiyar, Neerja; Tomsho, Lynn P.; Kasson, Lindsay McClellan; Lesk, Arthur M.; Zhang, Yu; Schuster, Stephan C.] Penn State Univ, Ctr Comparat Genom & Bioinformat, University Pk, PA 16802 USA.
[Hayes, Vanessa M.; Petersen, Desiree C.; Miller, Jason; Walenz, Brian] J Craig Venter Inst, Rockville, MD 20850 USA.
[Knight, James] 454 Life Sci, Branford, CT 06405 USA.
[Bertelsen, Mads Frost] Copenhagen Zoo, Ctr Zoo & Wild Anim Hlth, DK-2000 Frederiksberg, Denmark.
[Dixon, Dale] Museum & Art Gallery No Terr, Darwin, NT 0801, Australia.
[Pyecroft, Stephen] Mt Pleasant Anim Hlth Labs, Dept Primary Ind & Water, Kings Meadows, Tas 7249, Australia.
[Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Pringle, Thomas H.] Sperling Fdn, Eugene, OR 97405 USA.
[Patterson, Nick] Broad Inst Massachusetts Inst Technol & Harvard U, Cambridge Ctr, Cambridge, MA 02142 USA.
[Woods, Gregory M.] Menzies Res Inst, Hobart, Tas 7000, Australia.
[Kreiss, Alexandre; Woods, Gregory M.; Jones, Menna E.] Univ Tasmania, Hobart, Tas 7001, Australia.
RP Hayes, VM (reprint author), Childrens Canc Inst Australia, Randwick, NSW 2031, Australia.
EM vhayes@jcvi.org; scs@bx.psu.edu
RI Jones, Menna/J-7975-2012; Wittekindt, Nicola/G-3469-2013; Woods,
Greg/J-7533-2014; QI, JI/E-2797-2016;
OI Wittekindt, Nicola/0000-0002-3310-0919; Woods, Greg/0000-0001-8421-7917;
Bertelsen, Mads/0000-0001-9201-7499
FU Gordon and Betty Moore Foundation; GENEWORKS, Australia; Allco
Foundation, Sydney; National Institute of General Medical Sciences
(National Institutes of Health) [R01-GM077117]; Roche
FX We thank Erin Noonan, Willow Farmer, Shelly Lachish, and Paul Humphrey
for assistance with sample processing; Rodrigo Hamede, Shelly Lachish,
Clare Hawkins, Fiona Hume, Billie Lazenby, Dydee Mann, Chrissie Pukk,
Jim Richley, Shaun Thurstans, and Jason Wiersma for field collections;
Tim Faulkner and John Weigel for captive animal contributions; Gavin
Dally for facilitating access to museum collections; Wee Siang Teo for
technical assistance; Tim T. Harkins for advice on sequencing
technologies; Somasekar Seshagiri for advice on tumor alleles; Bill
Murphy for providing SI Appendix, Fig. S3; and George Perry for
insightful comments about the manuscript. This project was funded by
grants from the Gordon and Betty Moore Foundation (to S.C.S. and V.M.H.)
for genome sequencing costs, and GENEWORKS, Australia (to V.M.H.) for
tumor-transcript sequencing costs; genotyping costs were covered by a
donation from the Allco Foundation, Sydney (to V.M.H.); and National
Institute of General Medical Sciences (National Institutes of Health)
Grant R01-GM077117 (to J.M. and B.W.). V. M. H. is a Cancer Institute of
New South Wales Fellow, Australia and S.C.S. is supported by the Gordon
and Betty Moore Foundation. Additional support was provided by Roche (to
S.C.S.).
NR 31
TC 83
Z9 85
U1 5
U2 134
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 26
PY 2011
VL 108
IS 30
BP 12348
EP 12353
DI 10.1073/pnas.1102838108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 797LS
UT WOS:000293129900035
PM 21709235
ER
PT J
AU Rabeling, C
Gonzales, O
Schultz, TR
Bacci, M
Garcia, MVB
Verhaagh, M
Ishak, HD
Mueller, UG
AF Rabeling, Christian
Gonzales, Omar
Schultz, Ted R.
Bacci, Mauricio, Jr.
Garcia, Marcos V. B.
Verhaagh, Manfred
Ishak, Heather D.
Mueller, Ulrich G.
TI Cryptic sexual populations account for genetic diversity and ecological
success in a widely distributed, asexual fungus-growing ant
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE Attini; clonality; Formicidae; thelytoky; mutualism
ID APIS-MELLIFERA-CAPENSIS; MYCOCEPURUS-SMITHII HYMENOPTERA;
THELYTOCOUS-PARTHENOGENESIS; FIRE ANT; CLONAL REPRODUCTION; BAYES
FACTORS; RECOMBINATION; FORMICIDAE; EVOLUTION; SELECTION
AB Sex and recombination are central processes in life generating genetic diversity. Organisms that rely on asexual propagation risk extinction due to the loss of genetic diversity and the inability to adapt to changing environmental conditions. The fungus-growing ant species Mycocepurus smithii was thought to be obligately asexual because only parthenogenetic populations have been collected from widely separated geographic localities. Nonetheless, M. smithii is ecologically successful, with the most extensive distribution and the highest population densities of any fungus-growing ant. Here we report that M. smithii actually consists of a mosaic of asexual and sexual populations that are nonrandomly distributed geographically. The sexual populations cluster along the Rio Amazonas and the Rio Negro and appear to be the source of independently evolved and widely distributed asexual lineages, or clones. Either apomixis or automixis with central fusion and low recombination rates is inferred to be the cytogenetic mechanism underlying parthenogenesis in M. smithii. Males appear to be entirely absent from asexual populations, but their existence in sexual populations is indicated by the presence of sperm in the reproductive tracts of queens. A phylogenetic analysis of the genus suggests that M. smithii is monophyletic, rendering a hybrid origin of asexuality unlikely. Instead, a mitochondrial phylogeny of sexual and asexual populations suggests multiple independent origins of asexual reproduction, and a divergence-dating analysis indicates that M. smithii evolved 0.5-1.65 million years ago. Understanding the evolutionary origin and maintenance of asexual reproduction in this species contributes to a general understanding of the adaptive significance of sex.
C1 [Rabeling, Christian; Gonzales, Omar; Ishak, Heather D.; Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Rabeling, Christian; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Bacci, Mauricio, Jr.] Sao Paulo State Univ, Ctr Study Social Insects, BR-13506900 Rio Claro, SP, Brazil.
[Garcia, Marcos V. B.] Embrapa Amazonia Ocidental, BR-69010970 Manaus, Amazonas, Brazil.
[Verhaagh, Manfred] Staatliches Museum Nat Karlsruhe, D-76133 Karlsruhe, Germany.
RP Rabeling, C (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
EM crabeling@gmail.com
FU Museum of Comparative Zoology; Harvard University; National Science
Foundation (NSF) [DEB-0808164, DEB-0949689, DEB-0431330, DEB-0639879,
DEB-0110073, DEB-998379]; Explorer's Club Exploration Fund; Lewis and
Clark Field Scholarship; Section of Integrative Biology; University of
Texas at Austin; Smithsonian Scholarly Studies Program; Smithsonian
Restricted Endowments Fund; Fundacao de Apoio a Pesquisa do Estado de
Sao Paulo [2008/54386-9]; Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico [476250/2008-0, 304661/2009-0];
Bundesministerium fur Bildung und Forschung (BMBF); Conselho National de
Pesquisa e Tecnologia [BMBF01LT0014/CNPq 690018/00-2, ENV52-2]; Wheeler
Lost Pines Endowment
FX We thank the following scientists for generously contributing specimens
and institutions for providing permission and access to study sites: G.
Alpert, C. Brandao, S. Cappellari, J. Carpenter, S. Cover, R. Feitosa,
F. Fernandez, J. Fontenla, A. Harada, A. Henriques, A. Himler, J.
Lattke, J. Longino, W. Mackay, J. Maes, J. Martins, B. Merz, N. Pitman,
R. Poggi, V. Raineri, C. Samper, S. Sanchez-Pena, J. Santisteban, R.
Silva, the late R. Snelling, J. Sosa-Calvo, H. Vasconcelos, P. Ward, and
E. Wilson; the Autoridad Nacional del Ambiente and Smithsonian Tropical
Research Institute, Panama; Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico and the Instituto Brasileiro do Meio Ambiente e
dos Recursos Naturais Renovaveis; the Forestry Division and Wildlife
Section of Trinidad; the Minesterio del Ambiente y Energia, Costa Rica;
and the Office of the President of Guyana. P. Armstrong and E. Okonski
kindly provided assistance in the laboratory. L. Hayek and S.
Arnaud-Haond provided valuable advice on statistical analyses. D.
Bolnik, S. Brady, D. Gotzek, D. Hillis, M. Singer, P. Ward, and two
anonymous reviewers improved the manuscript with helpful comments. C.R.
gratefully acknowledges financial support from Ernst Mayr grants (Museum
of Comparative Zoology) and the Green Fund (Harvard University), a
National Science Foundation (NSF) Doctoral Dissertation Improvement
Grant (DEB-0808164), the Explorer's Club Exploration Fund, a Lewis and
Clark Field Scholarship, and research grants from the Section of
Integrative Biology and a Miller Endowed University Continuing
Fellowship from the University of Texas at Austin; T.R.S. was supported
by the NSF (DEB-0949689 and DEB-0431330), the Smithsonian Scholarly
Studies Program, and the Smithsonian Restricted Endowments Fund; M.B.
received support from the Fundacao de Apoio a Pesquisa do Estado de Sao
Paulo (2008/54386-9) and the Conselho Nacional de Desenvolvimento
Cientifico e Tecnologico (476250/2008-0 and 304661/2009-0); M.V.B.G. and
M.V. acknowledge the Bundesministerium fur Bildung und Forschung (BMBF)
and the Conselho National de Pesquisa e Tecnologia (BMBF01LT0014/CNPq
690018/00-2) for kindly providing funding for SHIFT Project ENV52-2;
U.G.M. was funded by grants from the NSF (DEB-0639879, DEB-0110073, and
DEB-998379) and the Wheeler Lost Pines Endowment. This study is a
chapter of C.R.'s doctoral dissertation.
NR 76
TC 24
Z9 24
U1 6
U2 36
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 26
PY 2011
VL 108
IS 30
BP 12366
EP 12371
DI 10.1073/pnas.1105467108
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 797LS
UT WOS:000293129900038
PM 21768368
ER
PT J
AU Nunes, FLD
Norris, RD
Knowlton, N
AF Nunes, Flavia L. D.
Norris, Richard D.
Knowlton, Nancy
TI Long Distance Dispersal and Connectivity in Amphi-Atlantic Corals at
Regional and Basin Scales
SO PLOS ONE
LA English
DT Article
ID POPULATION-STRUCTURE; GENE FLOW; SIDERASTREA-STELLATA; LARVAL
METAMORPHOSIS; GENOTYPIC DIVERSITY; SPECIES BOUNDARIES;
MITOCHONDRIAL-DNA; CARIBBEAN CORALS; SPAWNING CORALS; PLANULA LARVAE
AB Among Atlantic scleractinian corals, species diversity is highest in the Caribbean, but low diversity and high endemism are observed in various peripheral populations in central and eastern Atlantic islands and along the coasts of Brazil and West Africa. The degree of connectivity between these distantly separated populations is of interest because it provides insight into processes at both evolutionary and ecological time scales, such as speciation, recruitment dynamics and the persistence of coral populations. To assess connectivity in broadly distributed coral species of the Atlantic, DNA sequence data from two nuclear markers were obtained for six coral species spanning their distributional ranges. At basin-wide scales, significant differentiation was generally observed among populations in the Caribbean, Brazil and West Africa. Concordance of patterns in connectivity among co-distributed taxa indicates that extrinsic barriers, such as the Amazon freshwater plume or long stretches of open ocean, restrict dispersal of coral larvae from region to region. Within regions, dispersal ability appears to be influenced by aspects of reproduction and life history. Two broadcasting species, Siderastrea siderea and Montastraea cavernosa, were able to maintain gene flow among populations separated by as much as 1,200 km along the coast of Brazil. In contrast, brooding species, such as Favia gravida and Siderastrea radians, had more restricted gene flow along the Brazilian coast.
C1 [Nunes, Flavia L. D.] Univ Geneva, Lab Artificial & Nat Evolut, Geneva, Switzerland.
[Nunes, Flavia L. D.; Norris, Richard D.; Knowlton, Nancy] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA.
[Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Nunes, FLD (reprint author), Univ Geneva, Lab Artificial & Nat Evolut, Geneva, Switzerland.
EM nunesf@gmail.com
RI Nunes, Flavia/B-5041-2011
OI Nunes, Flavia/0000-0002-3947-6634
FU John Dove Isaacs Chair in Natural Philosophy; Center of Marine
Biodiversity and Conservation
FX This work was supported by the John Dove Isaacs Chair in Natural
Philosophy to NK, by an anonymous private donation to the SIO Graduate
Department to FN, and by a Graduate Fellowship from the Center of Marine
Biodiversity and Conservation to FN. The funders had no role in study
design, data collection and analysis, decision to publish, or
preparation of the manuscript.
NR 70
TC 25
Z9 25
U1 2
U2 31
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUL 22
PY 2011
VL 6
IS 7
AR e22298
DI 10.1371/journal.pone.0022298
PG 12
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 797BJ
UT WOS:000293097300028
PM 21799816
ER
PT J
AU Chen, GX
AF Chen, G. X.
TI Breit-Pauli R-matrix method for electron-impact excitation to magnetic
sublevels and x-ray-line polarization of ions
SO PHYSICAL REVIEW A
LA English
DT Article
ID FE-XVII; SOLAR-FLARES; HE-LIKE; BEAM; MICROCALORIMETER; DIAGNOSTICS;
RADIATION; PROGRAM; PLASMAS; RATIOS
AB The Breit-Pauli R-matrix (BPRM) method was employed to calculate x-ray line polarization resulting from electron-impact excitation to excited-state magnetic sublevels (MS) of complex ions. In the development of this work, the calculation of MS electron-impact excitation cross sections in the present BPRM method is computationally efficient when the angular integration of the scattering polar angle is performed in an analytical manner. The BPRM method is then applied to calculate the line polarization of 3C (lambda = 15.01 angstrom) and 3D(lambda = 15.26 angstrom), two well-known x-ray lines of 17 (an ion with a medium nuclear charge and ion charge). We demonstrate in this work the resonance effects in MS cross sections, which contribute to the energy dependence in the polarization. The BPRM calculations of Fe XVII are further compared with the results calculated by the Dirac R-matrix (DRM) method. Generally, most of the results calculated from the BPRM method and the DRM method are in good agreement. This comparison confirms the earlier DRM calculations of resonance effects in MS electron-impact excitation cross sections of 3C and 3D, and thus demonstrates the applicability of the BPRM method to the calculation of x-ray line polarization of 3C and 3D, important for the analysis of x-ray spectra observed on an electron beam ion trap.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Chen, GX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Smithsonian Astrophysical Observatory (SAO); NASA [TM0-11001X and
TM8-9001X]
FX This work was supported in part by a grant from Smithsonian
Astrophysical Observatory (SAO) and by NASA to SAO for the Chandra X-ray
Center through grants TM0-11001X and TM8-9001X.
NR 27
TC 2
Z9 2
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 JUL 22
PY 2011
VL 84
IS 1
AR 012705
DI 10.1103/PhysRevA.84.012705
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 795VE
UT WOS:000293003700007
ER
PT J
AU Cairns, SD
AF Cairns, Stephen D.
TI Global Diversity of the Stylasteridae (Cnidaria: Hydrozoa: Athecatae)
SO PLOS ONE
LA English
DT Article
ID GENERIC REVISION; SCLERACTINIAN CORALS; ALEUTIAN ISLANDS; COELENTERATA;
ASSOCIATIONS; ALASKA
AB The history and rate of discovery of the 247 valid Recent stylasterid species are discussed and graphed, with emphasis on five historical pulses of species descriptions. A table listing all genera, their species numbers, and their bathymetric ranges are presented. The number of species in 19 oceanographic regions is mapped, the southwestern temperate Pacific (region including New Zealand) having the most species; species are cosmopolitan from the Arctic Circle to the Antarctic at depths from 0 to 2789 m. The current phylogenetic classification of the genera is briefly discussed. An illustrated glossary of 53 morphological characters is presented. Biological and ecological information pertaining to reproduction, development, commensals, and distribution is discussed. Aspects of stylasterid mineralogy and taxa of commercial value are discussed, concluding with suggestions for future work.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.
EM cairnss@si.edu
NR 82
TC 21
Z9 22
U1 1
U2 5
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 JUL 22
PY 2011
VL 6
IS 7
AR e21670
DI 10.1371/journal.pone.0021670
PG 13
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 797BJ
UT WOS:000293097300004
PM 21799741
ER
PT J
AU Weitekamp, M
AF Weitekamp, Margaret
TI Spacesuit: Fashioning Apollo
SO NATURE
LA English
DT Book Review
C1 [Weitekamp, Margaret] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Weitekamp, M (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
EM weitekampm@si.edu
NR 1
TC 0
Z9 0
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 21
PY 2011
VL 475
IS 7356
BP 294
EP 294
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 794PA
UT WOS:000292911200017
ER
PT J
AU Liu, X
Shen, Y
Strauss, MA
AF Liu, Xin
Shen, Yue
Strauss, Michael A.
TI COSMIC TRAIN WRECK BY MASSIVE BLACK HOLES: DISCOVERY OF A
KILOPARSEC-SCALE TRIPLE ACTIVE GALACTIC NUCLEUS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: interactions; galaxies:
nuclei; galaxies: stellar content
ID DIGITAL SKY SURVEY; STELLAR VELOCITY DISPERSIONS; HOST GALAXIES;
EMISSION-LINE; NEARBY GALAXIES; X-RAY; CLASSIFICATION; EVOLUTION;
SYSTEMS; SEARCH
AB Hierarchical galaxy mergers will lead to the formation of binary and, in the case of a subsequent merger before a binary coalesces, triple supermassive black holes (SMBHs), given that most massive galaxies harbor SMBHs. A triple of SMBHs becomes visible as a triple active galactic nucleus (AGN) when the BHs accrete large amounts of gas at the same time. Here, we report the discovery of a kiloparsec-scale triple AGN, SDSS J1027+1749 at z = 0.066, from our systematic search for hierarchical mergers of AGNs. The galaxy contains three emission-line nuclei, two of which are offset by 450 and 110 km s(-1) in velocity and by 2.4 and 3.0 kpc in projected separation from the central nucleus. All three nuclei are classified as obscured AGNs based on optical diagnostic emission line ratios, with black hole mass estimates M. greater than or similar to 10(8) M-circle dot from stellar velocity dispersions measured in the associated stellar components. Based on dynamical friction timescale estimates, the three stellar components in SDSS J1027+1749 will merge in similar to 40 Myr, and their associated SMBHs may evolve into a gravitationally interacting triple system in less than or similar to 200 Myr. Our result sets a lower limit of similar to 5x10(-5) for the fraction of kiloparsec-scale triples in optically selected AGNs at z similar to 0.1.
C1 [Liu, Xin; Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Strauss, Michael A.] Princeton Univ Observ, Princeton, NJ 08544 USA.
RP Liu, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [PF0-110076, NAS8-03060]; Clay Postdoctoral Fellowship through the
Smithsonian Astrophysical Observatory; NSF [AST-0707266]; Alfred P.
Sloan Foundation; National Science Foundation; U.S. Department of
Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education
Funding Council for England; American Museum of Natural History;
Astrophysical Institute Potsdam; University of Basel; University of
Cambridge; Case Western Reserve University; University of Chicago;
Drexel University; Fermilab; Institute for Advanced Study; Japan
Participation Group; Johns Hopkins University; Joint Institute for
Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and
Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST);
Los Alamos National Laboratory; Max-Planck-Institute for Astronomy
(MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State
University; Ohio State University; University of Pittsburgh; University
of Portsmouth; Princeton University; United States Naval Observatory;
University of Washington
FX We thank an anonymous referee for a prompt and helpful report. Support
for the work of X.L. was provided by NASA through Einstein Postdoctoral
Fellowship grant number PF0-110076 awarded by the Chandra X-ray Center,
which is operated by the Smithsonian Astrophysical Observatory for NASA
under contract NAS8-03060. Y.S. acknowledges support from a Clay
Postdoctoral Fellowship through the Smithsonian Astrophysical
Observatory. M.A.S. acknowledges the support of NSF grant AST-0707266.;
Funding for the SDSS and SDSS-II has been provided by the Alfred P.
Sloan Foundation, the Participating Institutions, the National Science
Foundation, the U.S. Department of Energy, the National Aeronautics and
Space Administration, the Japanese Monbukagakusho, the Max Planck
Society, and the Higher Education Funding Council for England. The SDSS
Web site is http://www.sdss.org/.; The SDSS is managed by the
Astrophysical Research Consortium for the Participating Institutions.
The Participating Institutions are the American Museum of Natural
History, Astrophysical Institute Potsdam, University of Basel,
University of Cambridge, Case Western Reserve University, University of
Chicago, Drexel University, Fermilab, the Institute for Advanced Study,
the Japan Participation Group, Johns Hopkins University, the Joint
Institute for Nuclear Astrophysics, the Kavli Institute for Particle
Astrophysics and Cosmology, the Korean Scientist Group, the Chinese
Academy of Sciences (LAMOST), Los Alamos National Laboratory, the
Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for
Astrophysics (MPA), New Mexico State University, Ohio State University,
University of Pittsburgh, University of Portsmouth, Princeton
University, the United States Naval Observatory, and the University of
Washington.
NR 50
TC 15
Z9 15
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 20
PY 2011
VL 736
IS 1
AR L7
DI 10.1088/2041-8205/736/1/L7
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OX
UT WOS:000293138300007
ER
PT J
AU Reale, F
Guarrasi, M
Testa, P
DeLuca, EE
Peres, G
Golub, L
AF Reale, Fabio
Guarrasi, Massimiliano
Testa, Paola
DeLuca, Edward E.
Peres, Giovanni
Golub, Leon
TI SOLAR DYNAMICS OBSERVATORY DISCOVERS THIN HIGH TEMPERATURE STRANDS IN
CORONAL ACTIVE REGIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Sun: corona; Sun: UV radiation
ID X-RAY-TELESCOPE; HOT PLASMA; POWER SPECTRA; LOOPS; TRACE; EMISSION;
RHESSI; SUN
AB One scenario proposed to explain the million degree solar corona is a finely stranded corona where each strand is heated by a rapid pulse. However, such fine structure has neither been resolved through direct imaging observations nor conclusively shown through indirect observations of extended superhot plasma. Recently, it has been shown that the observed difference in the appearance of cool and warm coronal loops (similar to 1 MK and similar to 2-3 MK, respectively)-warm loops appearing "fuzzier" than cool loops-can be explained by models of loops composed of subarcsecond strands, which are impulsively heated up to similar to 10 MK. That work predicts that images of hot coronal loops (greater than or similar to 6MK) should again show fine structure. Here we show that the predicted effect is indeed widely observed in an active region with the Solar Dynamics Observatory, thus supporting a scenario where impulsive heating of fine loop strands plays an important role in powering the active corona.
C1 [Reale, Fabio; Guarrasi, Massimiliano; Peres, Giovanni] Univ Palermo, Dipartimento Fis, I-90134 Palermo, Italy.
[Reale, Fabio; Peres, Giovanni] INAF Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy.
[Testa, Paola; DeLuca, Edward E.; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Reale, F (reprint author), Univ Palermo, Dipartimento Fis, Piazza Parlamento 1, I-90134 Palermo, Italy.
RI DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; Reale, Fabio/0000-0002-1820-4824;
Golub, Leon/0000-0001-9638-3082
FU Italian Ministero dell'Universita e Ricerca; Agenzia Spaziale Italiana
(ASI) [I/023/09/0]; Lockheed-Martin [SP02H1701R]
FX F.R., G.P., and M.G. acknowledge support from Italian Ministero
dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI), contract
I/023/09/0. P.T. was supported by contract SP02H1701R from
Lockheed-Martin to the Smithsonian Astrophysical Observatory.
NR 28
TC 30
Z9 30
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 20
PY 2011
VL 736
IS 1
AR L16
DI 10.1088/2041-8205/736/1/L16
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OX
UT WOS:000293138300016
ER
PT J
AU van de Sande, J
Kriek, M
Franx, M
van Dokkum, PG
Bezanson, R
Whitaker, KE
Brammer, G
Labbe, I
Groot, PJ
Kaper, L
AF van de Sande, Jesse
Kriek, Mariska
Franx, Marijn
van Dokkum, Pieter G.
Bezanson, Rachel
Whitaker, Katherine E.
Brammer, Gabriel
Labbe, Ivo
Groot, Paul J.
Kaper, Lex
TI THE STELLAR VELOCITY DISPERSION OF A COMPACT MASSIVE GALAXY AT z=1.80
USING X-SHOOTER: CONFIRMATION OF THE EVOLUTION IN THE MASS-SIZE AND
MASS-DISPERSION RELATIONS
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: evolution; galaxies: formation; galaxies: structure
ID SIMILAR-TO 2; MEDIUM-BAND SURVEY; DIGITAL SKY SURVEY; ULTRA-DEEP-FIELD;
QUIESCENT GALAXIES; ELLIPTIC GALAXIES; POPULATION SYNTHESIS;
STAR-FORMATION; SPECTRA; GROWTH
AB Recent photometric studies have shown that early-type galaxies at fixed stellar mass were smaller and denser at earlier times. In this Letter, we assess that finding by deriving the dynamical mass of such a compact quiescent galaxy at z = 1.8. We have obtained a high-quality spectrum with full UV-NIR wavelength coverage of galaxy NMBS-C7447 using X-Shooter on the Very Large Telescope. We determined a velocity dispersion of 294 +/- 51 km s(-1). Given this velocity dispersion and the effective radius of 1.64 +/- 0.15 kpc (as determined from Hubble Space Telescope Wide Field Camera 3 F160W observations) we derive a dynamical mass of (1.7 +/- 0.5) x 10(11) M-circle dot. Comparison of the full spectrum with stellar population synthesis models indicates that NMBS-C774 has a relatively young stellar population (0.40 Gyr) with little or no star formation and a stellar mass of M-star similar to 1.5 x 10(11) M-circle dot. The dynamical and photometric stellar masses are in good agreement. Thus, our study supports the conclusion that the mass densities of quiescent galaxies were indeed higher at earlier times, and this earlier result is not caused by systematic measurement errors. By combining available spectroscopic measurements at different redshifts, we find that the velocity dispersion at fixed dynamical mass was a factor of similar to 1.8 higher at z = 1.8 compared with z = 0. Finally, we show that the apparent discrepancies between the few available velocity dispersion measurements at z > 1.5 are consistent with the intrinsic scatter of the mass-size relation.
C1 [van de Sande, Jesse; Franx, Marijn; Labbe, Ivo] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[van Dokkum, Pieter G.; Bezanson, Rachel; Whitaker, Katherine E.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Brammer, Gabriel] European So Observ, Santiago 19, Chile.
[Groot, Paul J.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands.
[Kaper, Lex] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands.
RP van de Sande, J (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands.
RI Groot, Paul/K-4391-2016;
OI Groot, Paul/0000-0002-4488-726X; van de Sande,
Jesse/0000-0003-2552-0021; Bezanson, Rachel/0000-0001-5063-8254
FU NASA [NAS 5-26555]; Netherlands Foundation for Research (NWO); NASA
through Space Telescope Science Institute [HST-GO-12167.1]
FX Based on observations with the NASA/ESA Hubble Space Telescope (HST),
obtained at the Space Telescope Science Institute, which is operated by
AURA, Inc., under NASA contract NAS 5-26555.; We thank the anonymous
referee for his comments, Johan Fynbo and Joanna Holt on the reduction
of the UVB and VIS X-Shooter data, and the NMBS team for their
contribution. This research was supported by grants from the Netherlands
Foundation for Research (NWO), the Leids Kerkhoven-Bosscha Fonds.
Support for program HST-GO-12167.1 was provided by NASA through a grant
from the Space Telescope Science Institute.
NR 50
TC 67
Z9 67
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 20
PY 2011
VL 736
IS 1
AR L9
DI 10.1088/2041-8205/736/1/L9
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OX
UT WOS:000293138300009
ER
PT J
AU Berta, ZK
Charbonneau, D
Bean, J
Irwin, J
Burke, CJ
Desert, JM
Nutzman, P
Falco, EE
AF Berta, Zachory K.
Charbonneau, David
Bean, Jacob
Irwin, Jonathan
Burke, Christopher J.
Desert, Jean-Michel
Nutzman, Philip
Falco, Emilio E.
TI THE GJ1214 SUPER-EARTH SYSTEM: STELLAR VARIABILITY, NEW TRANSITS, AND A
SEARCH FOR ADDITIONAL PLANETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; eclipses; planets and satellites: individual (GJ 1214b);
stars: individual (GJ 1214); stars: low-mass; stars: rotation; starspots
ID LOW-MASS STARS; HUBBLE-SPACE-TELESCOPE; RADIAL-VELOCITY VARIATIONS;
EXOPLANET HD 189733B; M-DWARF STARS; EXTRASOLAR PLANET; LIGHT-CURVE; GJ
1214B; HOT JUPITER; PHOTOMETRIC CALIBRATION
AB The super-Earth GJ1214b transits a nearby M dwarf that exhibits a 1% intrinsic variability in the near-infrared. Here, we analyze new observations to refine the physical properties of both the star and planet. We present three years of out-of-transit photometric monitoring of the stellar host GJ1214 from the MEarth Observatory and find the rotation period to be long, most likely an integer multiple of 53 days, suggesting low levels of magnetic activity and an old age for the system. We show that such variability will not pose significant problems to ongoing studies of the planet's atmosphere with transmission spectroscopy. We analyze two high-precision transit light curves from ESO's Very Large Telescope (VLT) along with seven others from the MEarth and Fred Lawrence Whipple Observatory 1.2 m telescopes, finding physical parameters for the planet that are consistent with previous work. The VLT light curves show tentative evidence for spot occultations during transit. Using two years of MEarth light curves, we place limits on additional transiting planets around GJ1214 with periods out to the habitable zone of the system. We also improve upon the previous photographic V-band estimate for the star, finding V = 14.71 +/- 0.03.
C1 [Berta, Zachory K.; Charbonneau, David; Bean, Jacob; Irwin, Jonathan; Burke, Christopher J.; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Nutzman, Philip] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Falco, Emilio E.] Smithsonian Astrophys Observ, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
RP Berta, ZK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM zberta@cfa.harvard.edu
OI Berta-Thompson, Zachory/0000-0002-3321-4924
FU NASA; David and Lucile Packard Fellowship for Science and Engineering;
National Science Foundation [AST-0807690]
FX We are extremely grateful to the KeplerCam observers Margaret Mclean,
Gil Esquerdo, Mark Everett, Pete Challis, and Joel Hartman who collected
V-band monitoring observations, as well as Gaspar Bakos, Dave Latham,
and Matt Holman for donated time and Lars Buchhave and Xavier Bonfils
for correcting the sign in the published gamma velocity. We thank the
referee for thoughtful and helpful comments that improved the paper
significantly. J.B. acknowledges funding from NASA through the Sagan
Fellowship Program. The MEarth team gratefully acknowledges funding from
the David and Lucile Packard Fellowship for Science and Engineering
(awarded to D. C.). This material is based upon work supported by the
National Science Foundation under grant number AST-0807690. The MEarth
team is greatly indebted to the staff at the Fred Lawrence Whipple
Observatory for their efforts in construction and maintenance of the
facility, and explicitly thank Wayne Peters, Ted Groner, Karen
Erdman-Myres, Grace Alegria, Rodger Harris, Bob Hutchins, Dave Martina,
Dennis Jankovsky, and Tom Welsh for their support.
NR 101
TC 61
Z9 61
U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 12
DI 10.1088/0004-637X/736/1/12
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600012
ER
PT J
AU Borucki, WJ
Koch, DG
Basri, G
Batalha, N
Brown, TM
Bryson, ST
Caldwell, D
Christensen-Dalsgaard, J
Cochran, WD
DeVore, E
Dunham, EW
Gautier, TN
Geary, JC
Gilliland, R
Gould, A
Howell, SB
Jenkins, JM
Latham, DW
Lissauer, JJ
Marcy, GW
Rowe, J
Sasselov, D
Boss, A
Charbonneau, D
Ciardi, D
Doyle, L
Dupree, AK
Ford, EB
Fortney, J
Holman, MJ
Seager, S
Steffen, JH
Tarter, J
Welsh, WF
Allen, C
Buchhave, LA
Christiansen, JL
Clarke, BD
Das, S
Desert, JM
Endl, M
Fabrycky, D
Fressin, F
Haas, M
Horch, E
Howard, A
Isaacson, H
Kjeldsen, H
Kolodziejczak, J
Kulesa, C
Li, J
Lucas, PW
Machalek, P
McCarthy, D
MacQueen, P
Meibom, S
Miquel, T
Prsa, A
Quinn, SN
Quintana, EV
Ragozzine, D
Sherry, W
Shporer, A
Tenenbaum, P
Torres, G
Twicken, JD
Van Cleve, J
Walkowicz, L
Witteborn, FC
Still, M
AF Borucki, William J.
Koch, David G.
Basri, Gibor
Batalha, Natalie
Brown, Timothy M.
Bryson, Stephen T.
Caldwell, Douglas
Christensen-Dalsgaard, Jorgen
Cochran, William D.
DeVore, Edna
Dunham, Edward W.
Gautier, Thomas N., III
Geary, John C.
Gilliland, Ronald
Gould, Alan
Howell, Steve B.
Jenkins, Jon M.
Latham, David W.
Lissauer, Jack J.
Marcy, Geoffrey W.
Rowe, Jason
Sasselov, Dimitar
Boss, Alan
Charbonneau, David
Ciardi, David
Doyle, Laurance
Dupree, Andrea K.
Ford, Eric B.
Fortney, Jonathan
Holman, Matthew J.
Seager, Sara
Steffen, Jason H.
Tarter, Jill
Welsh, William F.
Allen, Christopher
Buchhave, Lars A.
Christiansen, Jessie L.
Clarke, Bruce D.
Das, Santanu
Desert, Jean-Michel
Endl, Michael
Fabrycky, Daniel
Fressin, Francois
Haas, Michael
Horch, Elliott
Howard, Andrew
Isaacson, Howard
Kjeldsen, Hans
Kolodziejczak, Jeffery
Kulesa, Craig
Li, Jie
Lucas, Philip W.
Machalek, Pavel
McCarthy, Donald
MacQueen, Phillip
Meibom, Soren
Miquel, Thibaut
Prsa, Andrej
Quinn, Samuel N.
Quintana, Elisa V.
Ragozzine, Darin
Sherry, William
Shporer, Avi
Tenenbaum, Peter
Torres, Guillermo
Twicken, Joseph D.
Van Cleve, Jeffrey
Walkowicz, Lucianne
Witteborn, Fred C.
Still, Martin
TI CHARACTERISTICS OF PLANETARY CANDIDATES OBSERVED BY KEPLER. II. ANALYSIS
OF THE FIRST FOUR MONTHS OF DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: statistics; planets and satellites: detection;
surveys
ID TERRESTRIAL PLANETS; INITIAL CHARACTERISTICS; TRANSITING PLANET; TARGET
STARS; CADENCE DATA; DWARF STARS; LOW-DENSITY; HABITABILITY; SYSTEM;
FIELD
AB On 2011 February 1 the Kepler mission released data for 156,453 stars observed from the beginning of the science observations on 2009 May 2 through September 16. There are 1235 planetary candidates with transit-like signatures detected in this period. These are associated with 997 host stars. Distributions of the characteristics of the planetary candidates are separated into five class sizes: 68 candidates of approximately Earth-size (R-p < 1.25 R-circle plus), 288 super-Earth-size (1.25 R-circle plus <= R-p < 2 R-circle plus), 662 Neptune-size (2 R-circle plus <= R-p < 6 R-circle plus), 165 Jupiter-size (6 R-circle plus <= R-p < 15 R-circle plus), and 19 up to twice the size of Jupiter (15 R-circle plus <= R-p < 22 R-circle plus). In the temperature range appropriate for the habitable zone, 54 candidates are found with sizes ranging from Earth-size to larger than that of Jupiter. Six are less than twice the size of the Earth. Over 74% of the planetary candidates are smaller than Neptune. The observed number versus size distribution of planetary candidates increases to a peak at two to three times the Earth-size and then declines inversely proportional to the area of the candidate. Our current best estimates of the intrinsic frequencies of planetary candidates, after correcting for geometric and sensitivity biases, are 5% for Earth-size candidates, 8% for super-Earth-size candidates, 18% for Neptune-size candidates, 2% for Jupiter-size candidates, and 0.1% for very large candidates; a total of 0.34 candidates per star. Multi-candidate, transiting systems are frequent; 17% of the host stars have multi-candidate systems, and 34% of all the candidates are part of multi-candidate systems.
C1 [Borucki, William J.; Koch, David G.; Bryson, Stephen T.; Lissauer, Jack J.; Rowe, Jason; Haas, Michael] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Basri, Gibor; Marcy, Geoffrey W.; Howard, Andrew; Isaacson, Howard; Walkowicz, Lucianne] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA.
[Brown, Timothy M.; Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA.
[Caldwell, Douglas; DeVore, Edna; Jenkins, Jon M.; Doyle, Laurance; Tarter, Jill; Christiansen, Jessie L.; Clarke, Bruce D.; Li, Jie; Machalek, Pavel; Quintana, Elisa V.; Tenenbaum, Peter; Twicken, Joseph D.; Van Cleve, Jeffrey; Still, Martin] SETI Inst, Mountain View, CA 94043 USA.
[Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Danish Asteroseismol Ctr, Aarhus, Denmark.
[Cochran, William D.; Endl, Michael; MacQueen, Phillip] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA.
[Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA.
[Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Geary, John C.; Latham, David W.; Sasselov, Dimitar; Charbonneau, David; Dupree, Andrea K.; Holman, Matthew J.; Buchhave, Lars A.; Desert, Jean-Michel; Fressin, Francois; Meibom, Soren; Quinn, Samuel N.; Ragozzine, Darin; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Gilliland, Ronald] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA.
[Howell, Steve B.; Sherry, William] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
[Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA.
[Ciardi, David] CALTECH, Exoplanet Sci Inst, Pasadena, CA 91125 USA.
[Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Fortney, Jonathan; Fabrycky, Daniel] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Seager, Sara] MIT, Cambridge, MA 02139 USA.
[Steffen, Jason H.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Allen, Christopher; Witteborn, Fred C.] Orbital Sci Corp, Mountain View, CA 94043 USA.
[Das, Santanu] Univ Calif Santa Cruz, Univ Affiliated Res Ctr, Santa Cruz, CA 95064 USA.
[Horch, Elliott] So Connecticut State Univ, New Haven, CT 06515 USA.
[Kolodziejczak, Jeffery] MSFC, Huntsville, AL 35805 USA.
[Kulesa, Craig; McCarthy, Donald] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
[Kulesa, Craig; McCarthy, Donald] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Lucas, Philip W.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England.
[Miquel, Thibaut] French Space Agcy, CNES, Toulouse, France.
[Prsa, Andrej] Villanova Univ, Dept Astron, Villanova, PA 19085 USA.
RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
EM William.J.Borucki@nasa.gov; Fred.C.Witteborn@nasa.gov;
Martin.Still@nasa.gov
RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard,
Andrew/D-4148-2015;
OI Caldwell, Douglas/0000-0003-1963-9616; Howard,
Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354;
Buchhave, Lars A./0000-0003-1605-5666; Ciardi,
David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky,
Daniel/0000-0003-3750-0183
FU NASA's Science Mission Directorate; W. M. Keck Foundation
FX Kepler was competitively selected as the tenth Discovery mission.
Funding for this mission is provided by NASA's Science Mission
Directorate. 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 Keck
Observatory was made possible by the generous financial support of the
W. M. Keck Foundation. We sincerely thank Andrew Gould for his timely,
thorough, and very helpful review of this paper. The authors thank many
people who gave so generously of their time to make this mission a
success.
NR 46
TC 528
Z9 528
U1 25
U2 106
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 2011
VL 736
IS 1
AR 19
DI 10.1088/0004-637X/736/1/19
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600019
ER
PT J
AU Cucchiara, A
Levan, AJ
Fox, DB
Tanvir, NR
Ukwatta, TN
Berger, E
Kruhler, T
Yoldas, AK
Wu, XF
Toma, K
Greiner, J
Olivares, F
Rowlinson, A
Amati, L
Sakamoto, T
Roth, K
Stephens, A
Fritz, A
Fynbo, JPU
Hjorth, J
Malesani, D
Jakobsson, P
Wiersema, K
O'Brien, PT
Soderberg, AM
Foley, RJ
Fruchter, AS
Rhoads, J
Rutledge, RE
Schmidt, BP
Dopita, MA
Podsiadlowski, P
Willingale, R
Wolf, C
Kulkarni, SR
D'Avanzo, P
AF Cucchiara, A.
Levan, A. J.
Fox, D. B.
Tanvir, N. R.
Ukwatta, T. N.
Berger, E.
Kruehler, T.
Yoldas, A. Kuepcue
Wu, X. F.
Toma, K.
Greiner, J.
Olivares E, F.
Rowlinson, A.
Amati, L.
Sakamoto, T.
Roth, K.
Stephens, A.
Fritz, Alexander
Fynbo, J. P. U.
Hjorth, J.
Malesani, D.
Jakobsson, P.
Wiersema, K.
O'Brien, P. T.
Soderberg, A. M.
Foley, R. J.
Fruchter, A. S.
Rhoads, J.
Rutledge, R. E.
Schmidt, B. P.
Dopita, M. A.
Podsiadlowski, P.
Willingale, R.
Wolf, C.
Kulkarni, S. R.
D'Avanzo, P.
TI A PHOTOMETRIC REDSHIFT OF z similar to 9.4 FOR GRB 090429B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE early universe; galaxies: high-redshift; gamma-ray burst: individual
(GRB 090429R); techniques: photometric
ID GAMMA-RAY BURSTS; GALAXY LUMINOSITY FUNCTION; CORE-COLLAPSE SUPERNOVAE;
DIGITAL SKY SURVEY; SWIFT-ERA; HOST GALAXIES; LIGHT CURVES; DUST;
AFTERGLOW; TELESCOPE
AB Gamma-ray bursts (GRBs) serve as powerful probes of the early universe, with their luminous afterglows revealing the locations and physical properties of star-forming galaxies at the highest redshifts, and potentially locating first-generation (Population III) stars. Since GRB afterglows have intrinsically very simple spectra, they allow robust redshifts from low signal-to-noise spectroscopy, or photometry. Here we present a photometric redshift of z similar to 9.4 for the Swift detected GRB 090429B based on deep observations with Gemini-North, the Very Large Telescope, and the GRB Optical and Near-infrared Detector. Assuming a Small Magellanic Cloud dust law (which has been found in a majority of GRB sight lines), the 90% likelihood range for the redshift is 9.06 < z < 9.52, although there is a low-probability tail toward somewhat lower redshifts. Adopting Milky Way or Large Magellanic Cloud dust laws leads to very similar conclusions, while a Maiolino law does allow somewhat lower redshift solutions, though in all cases the most likely redshift is found to be z > 7. The non-detection of the host galaxy to deep limits (Y (AB) similar to 28, which would correspond roughly to 0.001L* at z = 1) in our late-time optical and infrared observations with the Hubble Space Telescope strongly supports the extreme-redshift origin of GRB 090429B, since we would expect to have detected any low-z galaxy, even if it were highly dusty. Finally, the energetics of GRB 090429B are comparable to those of other GRBs and suggest that its progenitor is not greatly different from those of lower redshift bursts.
C1 [Cucchiara, A.; Fox, D. B.; Wu, X. F.; Toma, K.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Cucchiara, A.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Cucchiara, A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England.
[Tanvir, N. R.; Rowlinson, A.; Wiersema, K.; O'Brien, P. T.; Willingale, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Ukwatta, T. N.] George Washington Univ, Dept Phys, Washington, DC 20052 USA.
[Ukwatta, T. N.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Berger, E.; Soderberg, A. M.; Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kruehler, T.; Greiner, J.; Olivares E, F.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
[Kruehler, T.] Tech Univ Munich, D-85748 Garching, Germany.
[Yoldas, A. Kuepcue] European So Observ, D-85748 Garching, Germany.
[Yoldas, A. Kuepcue] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Wu, X. F.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China.
[Amati, L.] INAF IASF Bologna, I-40129 Bologna, Italy.
[Roth, K.; Stephens, A.; Fritz, Alexander] Gemini Observ, Hilo, HI 96720 USA.
[Fynbo, J. P. U.; Hjorth, J.; Malesani, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark.
[Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland.
[Fruchter, A. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Rhoads, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA.
[Rutledge, R. E.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Schmidt, B. P.; Dopita, M. A.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
[Podsiadlowski, P.; Wolf, C.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
[Kulkarni, S. R.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[D'Avanzo, P.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy.
RP Cucchiara, A (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA.
EM acucchiara@lbl.gov
RI Fynbo, Johan/L-8496-2014; Hjorth, Jens/M-5787-2014; Dopita,
Michael/P-5413-2014; Jakobsson, Pall/L-9950-2015; Amati,
Lorenzo/N-5586-2015; Wu, Xuefeng/G-5316-2015;
OI Fynbo, Johan/0000-0002-8149-8298; Hjorth, Jens/0000-0002-4571-2306;
Dopita, Michael/0000-0003-0922-4986; Jakobsson,
Pall/0000-0002-9404-5650; Amati, Lorenzo/0000-0001-5355-7388; Wu,
Xuefeng/0000-0002-6299-1263; Kruehler, Thomas/0000-0002-8682-2384
FU NSF [GN-2009A-Q-26]; NASA [NAS 5-26555]; DFG [HA 1850/28-1]; Science and
Technology Funding Council; Danish National Research Foundation;
Deutscher Akademischer Austausch-Dienst (DAAD)
FX The Gemini data, acquired under the program ID GN-2009A-Q-26, are based
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), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio
de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Based on
observations made with the NASA/ESA Hubble Space Telescope, obtained
from the data archive at the Space Telescope Institute. STScI is
operated by the association of Universities for Research in Astronomy,
Inc. under the NASA contract NAS 5-26555. Data presented in this paper
is associated with programme GO-11189. Part of the funding for GROND
(both hardware as well as personnel) was generously granted by the
Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). T. K.
acknowledges support by the DFG cluster of excellence "Origin and
Structure of the Universe." A. R. acknowledges funding from the Science
and Technology Funding Council. The Dark Cosmology Centre is funded by
the Danish National Research Foundation. F.O.E. acknowledges funding of
his Ph.D. through the Deutscher Akademischer Austausch-Dienst (DAAD).
NR 70
TC 175
Z9 176
U1 1
U2 11
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 7
DI 10.1088/0004-637X/736/1/7
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600007
ER
PT J
AU Espada, D
Munoz-Mateos, JC
de Paz, AG
Sabater, J
Boissier, S
Verley, S
Athanassoula, E
Bosma, A
Leon, S
Verdes-Montenegro, L
Yun, M
Sulentic, J
AF Espada, D.
Munoz-Mateos, J. C.
Gil de Paz, A.
Sabater, J.
Boissier, S.
Verley, S.
Athanassoula, E.
Bosma, A.
Leon, S.
Verdes-Montenegro, L.
Yun, M.
Sulentic, J.
TI STAR FORMATION IN THE EXTENDED GASEOUS DISK OF THE ISOLATED GALAXY CIG
96
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 864); galaxies: ISM; galaxies: spiral;
galaxies: structure; stars: formation
ID CHEMO-SPECTROPHOTOMETRIC EVOLUTION; SPITZER-SPACE-TELESCOPE; EXTREME
OUTER DISK; SPIRAL GALAXIES; BARRED GALAXIES; NEARBY GALAXIES;
RADIAL-DISTRIBUTION; STARBURST GALAXIES; DUST ATTENUATION; FORMING
GALAXIES
AB We study the Kennicutt-Schmidt star formation law and efficiency in the gaseous disk of the isolated galaxy CIG 96 (NGC 864), with special emphasis on its unusually large atomic gas (H I) disk (rH (I)/r(25) = 3.5, r(25) = 1.'85). We present deep Galaxy Evolution Explorer near- and far-UV observations, used as a recent star formation tracer, and we compare them with new, high-resolution (16 '' or 1.6 kpc) Very Large Array H I observations. The UV and H I maps show good spatial correlation outside the inner 1', where the H I phase dominates over H-2. Star-forming regions in the extended gaseous disk are mainly located along the enhanced H I emission within two (relatively) symmetric, giant gaseous spiral arm-like features, which emulate an H I pseudo-ring at r similar or equal to 3'. Inside this structure, two smaller gaseous spiral arms extend from the northeast and southwest of the optical disk and connect to the previously mentioned H I pseudo-ring. Interestingly, we find that the (atomic) Kennicutt-Schmidt power-law index systematically decreases with radius, from N similar or equal to 3.0 +/- 0.3 in the inner disk (0.'8-1.'7) to N = 1.6 +/- 0.5 in the outskirts of the gaseous disk (3.'3-4.'2). Although the star formation efficiency (SFE), the star formation rate per unit of gas, decreases with radius where the H I component dominates as is common in galaxies, we find that there is a break of the correlation at r = 1.5r(25). At radii 1.5r(25) < r < 3.5r(25), mostly within the H I pseudo-ring structure, regions exist whose SFE remains nearly constant, SFE similar or equal to 10(-11) yr(-1). We discuss possible mechanisms that might be triggering the star formation in the outskirts of this galaxy, and we suggest that the constant SFE for such large radii (r > 2r(25)) and at such low surface densities might be a common characteristic in extended UV disk galaxies.
C1 [Espada, D.; Sabater, J.; Verdes-Montenegro, L.; Sulentic, J.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Espada, D.] Natl Astron Observ Japan, Tokyo 1818588, Japan.
[Espada, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Munoz-Mateos, J. C.; Gil de Paz, A.] Univ Complutense Madrid, Dept Astrofis, E-28040 Madrid, Spain.
[Munoz-Mateos, J. C.; Gil de Paz, A.] Univ Complutense Madrid, CC Atmosfera, E-28040 Madrid, Spain.
[Munoz-Mateos, J. C.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Sabater, J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Boissier, S.; Athanassoula, E.; Bosma, A.] Univ Aix Marseille, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France.
[Boissier, S.; Athanassoula, E.; Bosma, A.] CNRS, UMR 6110, F-13388 Marseille 13, France.
[Verley, S.] Univ Granada, Dept Fis Teor & Cosmos, Granada, Spain.
[Leon, S.] Joint ALMA Observ ESO, Santiago, Chile.
[Yun, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP Espada, D (reprint author), CSIC, Inst Astrofis Andalucia, Apdo 3004, E-18080 Granada, Spain.
EM daniel.espada@nao.ac.jp
RI Gil de Paz, Armando/J-2874-2016;
OI Gil de Paz, Armando/0000-0001-6150-2854; Sabater,
Jose/0000-0003-1149-6294
FU NASA [NNX09AQ356, 1374189, NAS5-98034]; European Community
[MOIF-CT-2006-40298]; DGI [AYA2008-06181-C02]; Junta de Andalucia
(Spain) [P08-FQM-4205]; Junta de Andalucia Grant [FQM108]; Spanish MEC
Grant [AYA-2007-67625-C02-02]; Juan de la Cierva fellowship; Spanish
Programa Nacional de Astronomia y Astrofisica [AyA2006-02358,
AyA2009-10368]; Consolider-GTC project; Spanish Ramon y Cajal program;
National Radio Astronomy Observatory; Alfred P. Sloan Foundation;
National Science Foundation; U.S. Department of Energy; Japanese
Monbukagakusho; Max Planck Society; Higher Education Funding Council for
England
FX We thank the anonymous referee for a careful reading and very detailed
report, which helped to improve this paper significantly. D. E.,
A.G.d.P., and L. V.-M. acknowledge support for this work from the GALEX
Guest Investigator program under NASA grant NNX09AQ356. D. E. was
supported by a Marie Curie International Fellowship within the Sixth
European Community Framework Programme (MOIF-CT-2006-40298). D. E.,
J.S., and L. V.-M. were partially supported by the DGI Grant
AYA2008-06181-C02 and the Junta de Andalucia (Spain) P08-FQM-4205. S. V.
was partially supported by Junta de Andalucia Grant FQM108, Spanish MEC
Grant AYA-2007-67625-C02-02, and a Juan de la Cierva fellowship.
A.G.d.P. and J.C.M.-M. are partially financed by the Spanish Programa
Nacional de Astronomia y Astrofisica under grants AyA2006-02358 and
AyA2009-10368 and the Consolider-GTC project. A.G.d.P. is also financed
by the Spanish Ramon y Cajal program. J.C.M.-M. acknowledges financial
support from NASA JPL/Spitzer grant RSA 1374189; he also acknowledges
support from the National Radio Astronomy Observatory, which is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. GALEX is operated for NASA by
the California Institute of Technology under NASA contract NAS5-98034.
The Spitzer Space Telescope is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration. Funding for the SDSS and
SDSS-II was 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 has made use of the
NASA/IPAC Extragalactic Database, which is operated by JPL/Caltech,
under contract with NASA. We acknowledge the usage of the HyperLeda
database (http://leda.univ-lyon1.fr).
NR 73
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 20
DI 10.1088/0004-637X/736/1/20
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600020
ER
PT J
AU Forbrich, J
Osten, RA
Wolk, SJ
AF Forbrich, Jan
Osten, Rachel A.
Wolk, Scott J.
TI SIMULTANEOUS X-RAY AND RADIO OBSERVATIONS OF YOUNG STELLAR OBJECTS IN
NGC 1333 AND IC 348
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE radio continuum: stars; stars: pre-main sequence; stars: protostars;
X-rays: stars
ID SPITZER OBSERVATIONS; CORONET CLUSTER; STARS; EMISSION; NGC-1333; CLOUD;
MULTIWAVELENGTH; PROTOSTARS; CHANDRA; FLARES
AB Young stellar objects (YSOs) and in particular protostars are known to show a variety of high-energy processes. Observations in the X-ray and centimetric radio wavelength ranges are thought to constrain some of these processes, e. g., coronal-type magnetic activity. There is a well-known empirical correlation of radio and X-ray luminosities in active stars, the so-called Gudel-Benz (GB) relation. Previous evidence of whether YSOs are compatible with this relation remains inconclusive for the earliest evolutionary stages. The main difficulty is that due to the extreme variability of these sources, simultaneous observations are essential. Until now, only a few YSOs and only a handful of protostars have been observed simultaneously in the X-ray and radio range. To expand the sample, we have obtained such observations of two young clusters rich in protostars, NGC 1333 and IC 348. While the absolute sensitivity is lower for these regions than for more nearby clusters like CrA, we find that even in deep continuum observations carried out with the NRAO Very Large Array (VLA), the radio detection fraction for protostars in these clusters is much lower than the X-ray detection fraction. Very few YSOs are detected in both bands, and we find the radio and X-ray populations among YSOs to be largely distinct. We combine these new results with previous simultaneous Chandra and VLA observations of star-forming regions and find that YSOs with detections in both bands appear to be offset toward higher radio luminosities for given X-ray luminosities when compared with the GB relation, although even in this sensitive data set most sources are too weak for the radio detections to provide information on the emission processes. The considerably improved sensitivity of the Expanded VLA will provide a better census of the YSO radio population as well as better constraints on the emission mechanisms.
C1 [Forbrich, Jan; Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Osten, Rachel A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Wolk, Scott/0000-0002-0826-9261
FU National Aeronautics and Space Administration [GO6-7015X, GO8-9017X,
NAS8-03060]
FX Support for this work was provided by the National Aeronautics and Space
Administration through Chandra Award Numbers GO6-7015X and GO8-9017X
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. S.J.W. is
supported by NASA contract NAS8-03060 (Chandra). The NRAO VLA data are
from programs S7874 (NGC1333) and S9056 (IC 348).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 25
DI 10.1088/0004-637X/736/1/25
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600025
ER
PT J
AU Krips, M
Martin, S
Eckart, A
Neri, R
Garcia-Burillo, S
Matsushita, S
Peck, A
Stoklasova, I
Petitpas, G
Usero, A
Combes, F
Schinnerer, E
Humphreys, L
Baker, AJ
AF Krips, M.
Martin, S.
Eckart, A.
Neri, R.
Garcia-Burillo, S.
Matsushita, S.
Peck, A.
Stoklasova, I.
Petitpas, G.
Usero, A.
Combes, F.
Schinnerer, E.
Humphreys, L.
Baker, A. J.
TI SUBMILLIMETER ARRAY/PLATEAU DE BURE INTERFEROMETER MULTIPLE LINE
OBSERVATIONS OF THE NEARBY SEYFERT 2 GALAXY NGC 1068: SHOCK-RELATED GAS
KINEMATICS AND HEATING IN THE CENTRAL 100 pc?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: individual (NGC 1068); galaxies: ISM;
galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: Seyfert;
radio continuum: galaxies; radio lines: galaxies; submillimeter:
galaxies
ID ACTIVE GALACTIC NUCLEUS; DENSE MOLECULAR GAS; STAR-FORMATION;
INTERSTELLAR-MEDIUM; STARBURST ENVIRONMENT; RADIO STRUCTURE; CENTRAL
ENGINE; NGC-1068; EMISSION; DISK
AB We present high angular resolution (0.'' 5-2.'' 0) observations of the millimeter continuum and the (CO)-C-12(J = 3-2), (CO)-C-13(J = 3-2), (CO)-C-13(J = 2-1), (CO)-O-18(J = 2-1), HCN(J = 3-2), HCO+(J = 4-3), and HCO+(J = 3-2) line emission in the circumnuclear disk (r less than or similar to 100 pc) of the prototypical Seyfert 2 galaxy NGC 1068, carried out with the Submillimeter Array. We also include in our analysis new (CO)-C-13(J = 1-0) and improved (CO)-C-12(J = 2-1) observations of NGC 1068 at high angular resolution (1.'' 0-2.'' 0) and sensitivity, conducted with the Institute de Radioastronomie Millimetrique Plateau de Bure Interferometer. Based on the complex dynamics of the molecular gas emission indicating non-circular motions in the central similar to 100 pc, we propose a scenario in which part of the molecular gas in the circumnuclear disk of NGC 1068 is blown radially outward as a result of shocks. This shock scenario is further supported by quite warm (T-kin >= 200 K) and dense (n(H-2) similar or equal to 10(4) cm(-3)) gas constrained from observed molecular line ratios. The HCN abundance in the circumnuclear disk is found to be [HCN]/[(CO)-C-12] approximate to 10(-3.5). This is slightly higher than the abundances derived for Galactic and extragalactic star-forming/starbursting regions. This result lends further support to X-ray-enhanced HCN formation in the circumnuclear disk of NGC 1068 as suggested by earlier studies. The HCO+ abundance ([HCO+]/[(CO)-C-12] approximate to 10(-5)) appears to be somewhat lower than that of Galactic and extragalactic star-forming/starbursting regions. When trying to fit the centimeter-to-millimeter continuum emission by different thermal and non-thermal processes, it appears that electron-scattered synchrotron emission yields the best results while thermal free-free emission seems to overpredict the millimeter continuum emission.
C1 [Krips, M.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Martin, S.] European So Observ, Santiago 19, Chile.
[Eckart, A.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
[Garcia-Burillo, S.; Usero, A.] Observ Madrid, OAN, Madrid 28014, Spain.
[Matsushita, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan.
[Matsushita, S.; Peck, A.] Joint ALMA Observ, Joint ALMA Off, Santiago 19, Chile.
[Peck, A.] NRAO, Charlottesville, VA 22903 USA.
[Stoklasova, I.] Acad Sci Czech Republic, Inst Astron, Vvi, Prague 14131, Czech Republic.
[Petitpas, G.] Harvard Smithsonian Ctr Astrophys, SMA Project, Cambridge, MA 02138 USA.
[Combes, F.] Observ Paris, LERMA, F-75014 Paris, France.
[Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
[Humphreys, L.] ESO, D-85748 Garching, Germany.
[Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
RP Krips, M (reprint author), Inst Radio Astron Millimetr, 300 Rue Piscine,Domaine Univ, F-38406 St Martin Dheres, France.
EM krips@iram.fr; smartin@eso.org; eckart@ph1.uni-koeln.de; neri@iram.fr;
s.gburillo@oan.es; apeck@alma.cl; satoki@asiaa.sinica.edu.tw;
gpetitpa@cfa.harvard.edu; a.usero@oan.es; francoise.combes@obspm.fr;
schinner@mpia.de; ehumphre@eso.org; ajbaker@physics.rutgers.edu
RI Orlitova, Ivana/G-6429-2014;
OI Orlitova, Ivana/0000-0002-9813-401X; Garcia-Burillo,
Santiago/0000-0003-0444-6897; Schinnerer, Eva/0000-0002-3933-7677;
Combes, Francoise/0000-0003-2658-7893
FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Smithsonian Institution;
Academia Sinica; Ministry of Education of the Czech Republic [LC06014];
National Radio Astronomy Observatory (NRAO); National Science Council
(NSC) of Taiwan [NSC 97-2112-M-001-021-MY3]
FX Based on observations carried out with the IRAM Plateau de Bure
Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany),
and IGN (Spain).; The 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 the anonymous referee for
a very careful and constructive report. We also thank Gaelle Dumas for a
very useful discussion on and help with the kinematic analysis of the
12CO data. I. S. acknowledges grant LC06014 of the Ministry
of Education of the Czech Republic. A. B. P. thanks the National Radio
Astronomy Observatory (NRAO) for support on this project. NRAO is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. S. M. is supported by the
National Science Council (NSC) of Taiwan, NSC 97-2112-M-001-021-MY3.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
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AR 37
DI 10.1088/0004-637X/736/1/37
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600037
ER
PT J
AU Offner, SSR
Mckee, CF
AF Offner, Stella S. R.
Mckee, Christopher F.
TI THE PROTOSTELLAR LUMINOSITY FUNCTION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: formation; stars: luminosity function, mass function
ID YOUNG STELLAR OBJECTS; INTERMEDIATE-MASS PROTOSTARS; AURIGA MOLECULAR
CLOUD; CLASS-I PROTOSTARS; STAR-FORMATION; EPISODIC ACCRETION;
TAURUS-AURIGA; DENSE CORES; EVOLUTIONARY SIGNATURES; RADIATIVE-TRANSFER
AB The protostellar luminosity function (PLF) is the present-day luminosity function of the protostars in a region of star formation. It is determined using the protostellar mass function in combination with a stellar evolutionary model that provides the luminosity as a function of instantaneous and final stellar mass. In 2010, McKee & Offner considered three main accretion models: the isothermal sphere (IS) model, the turbulent core (TC) model, and an approximation of the competitive accretion (CA) model. We also consider the effect of an accretion rate that tapers off linearly in time and an accelerating star formation rate. For each model, we characterize the luminosity distribution using the mean, median, maximum, ratio of the median to the mean, standard deviation of the logarithm of the luminosity, and the fraction of very low luminosity objects. We compare the models with bolometric luminosities observed in local star-forming regions and find that models with an approximately constant accretion time, such as the TC and CA models, appear to agree better with observation than those with a constant accretion rate, such as the IS model. We show that observations of the mean protostellar luminosity in these nearby regions of low-mass star formation suggest a mean star formation time of 0.3 +/- 0.1 Myr. Such a timescale, together with some accretion that occurs non-radiatively and some that occurs in high-accretion, episodic bursts, resolves the classical "luminosity problem" in low-mass star formation, in which observed protostellar luminosities are significantly less than predicted. An accelerating star formation rate is one possible way of reconciling the observed star formation time and mean luminosity. Future observations will place tighter constraints on the observed luminosities, star formation time, and episodic accretion, enabling better discrimination between star formation models and clarifying the influence of variable accretion on the PLF.
C1 [Offner, Stella S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mckee, Christopher F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Mckee, Christopher F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Offner, SSR (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
EM soffner@cfa.harvard.edu; cmckee@astro.berkeley.edu
FU NSF [AST-0908553, AST-0901055]
FX We thank Steven Stahler, Jean Francoise Lestrad, Mark Krumholz, Lee
Hartmann, Scott Kenyon, Joan Najita, Phil Myers, and an anonymous
referee for helpful comments. We thank Melissa Enoch, Neal Evans, and
Mike Dunham for useful discussions and clarifications of the
observational data. This research has been supported by NSF through
grants AST-0908553 (CFM) and AST-0901055 (SSRO).
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 53
DI 10.1088/0004-637X/736/1/53
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600053
ER
PT J
AU Rahoui, F
Lee, JC
Heinz, S
Hines, DC
Pottschmidt, K
Wilms, J
Grinberg, V
AF Rahoui, Farid
Lee, Julia C.
Heinz, Sebastian
Hines, Dean C.
Pottschmidt, Katja
Wilms, Joern
Grinberg, Victoria
TI A MULTIWAVELENGTH STUDY OF CYGNUS X-1: THE FIRST MID-INFRARED
SPECTROSCOPIC DETECTION OF COMPACT JETS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: close; dust, extinction; infrared: stars; stars: individual
(Cygnus X-1); X-rays: binaries
ID LONG-TERM VARIABILITY; RAY-TIMING-EXPLORER; EARLY-TYPE STARS;
SPITZER-SPACE-TELESCOPE; ACCRETING BLACK-HOLES; X-RAY; LOW/HARD STATE;
MASS-LOSS; GX 339-4; SYNCHROTRON EMISSION
AB We report on a Spitzer/InfraRed Spectrograph (mid-infrared), RXTE/PCA+HEXTE (X-ray), and Ryle (radio) simultaneous multiwavelength study of the microquasar Cygnus X-1, which aimed at an investigation of the origin of its mid-infrared emission. Compact jets were present in two out of three observations, and we show that they strongly contribute to the mid-infrared continuum. During the first observation, we detect the spectral break-where the transition from the optically thick to the optically thin regime takes place-at about 2.9x10(13) Hz. We then show that the jet's optically thin synchrotron emission accounts for Cygnus X-1's emission beyond 400 keV, although it cannot alone explain its 3-200 keV continuum. A compact jet was also present during the second observation, but we do not detect the break, since it has likely shifted to higher frequencies. In contrast, the compact jet was absent during the last observation, and we show that the 5-30 mu m mid-infrared continuum of Cygnus X-1 stems from the blue supergiant companion star HD 226868. Indeed, the emission can then be understood as the combination of the photospheric Rayleigh-Jeans tail and the bremsstrahlung from the expanding stellar wind. Moreover, the stellar wind is found to be clumpy, with a filling factor f(infinity) approximate to 0.09-0.10. Its bremsstrahlung emission is likely anti-correlated to the soft X-ray emission, suggesting an anti-correlation between the mass-loss and mass-accretion rates. Nevertheless, we do not detect any mid-infrared spectroscopic evidence of interaction between the jets and Cygnus X-1's environment and/or the companion star's stellar wind.
C1 [Rahoui, Farid; Lee, Julia C.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA.
[Rahoui, Farid; Lee, Julia C.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Heinz, Sebastian] Univ Wisconsin Madison, Dept Astron, Madison, WI 53706 USA.
[Hines, Dean C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Pottschmidt, Katja] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Pottschmidt, Katja] UMBC, CRESST, Greenbelt, MD 20771 USA.
[Wilms, Joern; Grinberg, Victoria] Univ Erlangen Nurnberg, Dr Karl Remeis Observ, D-96049 Bamberg, Germany.
[Wilms, Joern; Grinberg, Victoria] Univ Erlangen Nurnberg, ECAP, D-96049 Bamberg, Germany.
RP Rahoui, F (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA.
EM frahoui@cfa.harvard.edu; jclee@cfa.harvard.edu; heinzs@astro.wisc.edu;
hines@stsci.edu; katja@milkyway.gsfc.nasa.gov;
joern.wilms@sternwarte.uni-erlangen.de;
victoria.grinberg@sternwarte.uni-erlangen.de
RI Wilms, Joern/C-8116-2013; Lee, Julia/G-2381-2015;
OI Wilms, Joern/0000-0003-2065-5410; Lee, Julia/0000-0002-7336-3588; Heinz,
Sebastian/0000-0002-8433-8652
FU Harvard Faculty of Arts and Sciences and the Harvard College
Observatory; JPL-NASA [1292543]; Bundesministerium fur Wirtschaft und
Technologie through Deutsches Zentrum fur Luft- und Raumfahrt [50 OR
1007]; European Commission [ITN 215212]
FX We thank the anonymous referee for his/her useful comments. F.R. thanks
J. Rodriguez for providing the INTEGRAL/IBIS data. J.C.L. thanks the
Harvard Faculty of Arts and Sciences and the Harvard College
Observatory. S.H. acknowledges support from JPL-NASA contract no.
1292543. This work was partially funded by the Bundesministerium fur
Wirtschaft und Technologie through Deutsches Zentrum fur Luft- und
Raumfahrt grant 50 OR 1007 and by the European Commission through
contract ITN 215212 "Black Hole Universe." This research has made use of
NASA's Astrophysics Data System, of the SIMBAD, and VizieR databases
operated at CDS, Strasbourg, France.
NR 60
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2011
VL 736
IS 1
AR 63
DI 10.1088/0004-637X/736/1/63
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600063
ER
PT J
AU Shirokoff, E
Reichardt, CL
Shaw, L
Millea, M
Ade, PAR
Aird, KA
Benson, BA
Bleem, LE
Carlstrom, JE
Chang, CL
Cho, HM
Crawford, TM
Crites, AT
de Haan, T
Dobbs, MA
Dudley, J
George, EM
Halverson, NW
Holder, GP
Holzapfel, WL
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Padin, S
Plagge, T
Pryke, C
Ruhl, JE
Schaffer, KK
Spieler, HG
Staniszewski, Z
Stark, AA
Story, K
Vanderlinde, K
Vieira, JD
Williamson, R
Zahn, O
AF Shirokoff, E.
Reichardt, C. L.
Shaw, L.
Millea, M.
Ade, P. A. R.
Aird, K. A.
Benson, B. A.
Bleem, L. E.
Carlstrom, J. E.
Chang, C. L.
Cho, H. M.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Dobbs, M. A.
Dudley, J.
George, E. M.
Halverson, N. W.
Holder, G. P.
Holzapfel, W. L.
Hrubes, J. D.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Padin, S.
Plagge, T.
Pryke, C.
Ruhl, J. E.
Schaffer, K. K.
Spieler, H. G.
Staniszewski, Z.
Stark, A. A.
Story, K.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
Zahn, O.
TI IMPROVED CONSTRAINTS ON COSMIC MICROWAVE BACKGROUND SECONDARY
ANISOTROPIES FROM THE COMPLETE 2008 SOUTH POLE TELESCOPE DATA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic background radiation; cosmology: observations; large-scale
structure of universe
ID ZELDOVICH POWER SPECTRUM; ATACAMA COSMOLOGY TELESCOPE; STAR-FORMING
GALAXIES; INTRACLUSTER MEDIUM; DUST EMISSION; EXTRAGALACTIC SOURCES; GAS
MOTIONS; CLUSTERS; PROBE; SIMULATIONS
AB We report measurements of the cosmic microwave background (CMB) power spectrum from the complete 2008 South Pole Telescope (SPT) data set. We analyze twice as much data as the first SPT power spectrum analysis, using an improved cosmological parameter estimator which fits multi-frequency models to the SPT 150 and 220 GHz bandpowers. We find an excellent fit to the measured bandpowers with a model that includes lensed primary CMB anisotropy, secondary thermal (tSZ) and kinetic (kSZ) Sunyaev-Zel'dovich anisotropies, unclustered synchrotron point sources, and clustered dusty point sources. In addition to measuring the power spectrum of dusty galaxies at high signal-to-noise, the data primarily constrain a linear combination of the kSZ and tSZ anisotropy contributions at 150 GHz and l = 3000: D-3000(tSZ) + 0.5 D-3000(kSZ) = 4.5 +/- 1.0 mu K-2. The 95% confidence upper limits on secondary anisotropy power are D-3000(tSZ) < 5.3 mu K-2 and D-3000(kSZ) < 6.5 mu K-2. We also consider the potential correlation of dusty and tSZ sources and find it incapable of relaxing the tSZ upper limit. These results increase the significance of the lower than expected tSZ amplitude previously determined from SPT power spectrum measurements. We find that models including non-thermal pressure support in groups and clusters predict tSZ power in better agreement with the SPT data. Combining the tSZ power measurement with primary CMB data halves the statistical uncertainty on sigma(8). However, the preferred value of sigma(8) varies significantly between tSZ models. Improved constraints on cosmological parameters from tSZ power spectrum measurements require continued progress in the modeling of the tSZ power.
C1 [Shirokoff, E.; Reichardt, C. L.; Benson, B. A.; George, E. M.; Holzapfel, W. L.; Lee, A. T.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
[Millea, M.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
[Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA.
[de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA.
[Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA.
RP Shirokoff, E (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
EM shiro@berkeley.edu
RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015;
OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518;
Reichardt, Christian/0000-0003-2226-9169; Stark,
Antony/0000-0002-2718-9996
FU National Science Foundation [ANT-0638937, ANT-0130612, 0709498]; NSF
Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and
Betty Moore Foundation; National Sciences and Engineering Research
Council of Canada; Canada Research Chairs program; Canadian Institute
for Advanced Research; Alfred P. Sloan Research Fellowship; Yale
University; Office of Science of the U.S. Department of Energy
[DE-AC02-05CH11231]; NASA Office of Space Science
FX The South Pole Telescope is supported by the National Science Foundation
through grants ANT-0638937 and ANT-0130612. Partial support is also
provided by the NSF Physics Frontier Center grant PHY-0114422 to the
Kavli Institute of Cosmological Physics at the University of Chicago,
the Kavli Foundation and the Gordon and Betty Moore Foundation. The
McGill group acknowledges funding from the National Sciences and
Engineering Research Council of Canada, Canada Research Chairs program,
and the Canadian Institute for Advanced Research. M. Dobbs acknowledges
support from an Alfred P. Sloan Research Fellowship. L. Shaw
acknowledges the support of Yale University and NSF grant AST-1009811.
M. Millea and L. Knox acknowledge the support of NSF grant 0709498. This
research used resources of the National Energy Research Scientific
Computing Center, which is supported by the Office of Science of the
U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Some of
the results in this paper have been derived using the HEALPix (Gorski et
al. 2005) package. We acknowledge the use of the Legacy Archive for
Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is
provided by the NASA Office of Space Science.
NR 54
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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 2011
VL 736
IS 1
AR 61
DI 10.1088/0004-637X/736/1/61
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600061
ER
PT J
AU van Ballegooijen, AA
Asgari-Targhi, M
Cranmer, SR
DeLuca, EE
AF van Ballegooijen, A. A.
Asgari-Targhi, M.
Cranmer, S. R.
DeLuca, E. E.
TI HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVEN WAVE TURBULENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetohydrodynamics (MHD); Sun: chromosphere; Sun: corona; Sun:
granulation; Sun: surface magnetism; turbulence
ID MAGNETIC-FLUX TUBES; LOW-FREQUENCY WAVES; RAY TELESCOPE XRT;
MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; ACTIVE-REGION;
QUIET-SUN; REDUCED MAGNETOHYDRODYNAMICS; RESONANT ABSORPTION; MHD
TURBULENCE
AB A three-dimensional magnetohydrodynamic (MHD) model for the propagation and dissipation of Alfven waves in a coronal loop is developed. The model includes the lower atmospheres at the two ends of the loop. The waves originate on small spatial scales (less than 100 km) inside the kilogauss flux elements in the photosphere. The model describes the nonlinear interactions between Alfven waves using the reduced MHD approximation. The increase of Alfven speed with height in the chromosphere and transition region (TR) causes strong wave reflection, which leads to counter-propagating waves and turbulence in the photospheric and chromospheric parts of the flux tube. Part of the wave energy is transmitted through the TR and produces turbulence in the corona. We find that the hot coronal loops typically found in active regions can be explained in terms of Alfven wave turbulence, provided that the small-scale footpoint motions have velocities of 1-2 km s(-1) and timescales of 60-200 s. The heating rate per unit volume in the chromosphere is two to three orders of magnitude larger than that in the corona. We construct a series of models with different values of the model parameters, and find that the coronal heating rate increases with coronal field strength and decreases with loop length. We conclude that coronal loops and the underlying chromosphere may both be heated by Alfvenic turbulence.
C1 [van Ballegooijen, A. A.; Cranmer, S. R.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Asgari-Targhi, M.] UCL, Dept Math, London WC1E 6BT, England.
RP van Ballegooijen, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA.
RI DeLuca, Edward/L-7534-2013;
OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen,
Adriaan/0000-0002-5622-3540
FU NASA [NNM07AB07C]
FX We thank the anonymous referee for many useful comments which helped to
improve this paper. We also thank B. Chandran for discussions on
nonlinear effects in Alfvenic turbulence. Hinode is a Japanese mission
developed and launched by ISAS/JAXA, with NAOJ as domestic partner and
NASA and STFC (UK) as international partners. It is operated by these
agencies in cooperation with ESA and NSC (Norway). This work was
supported by NASA contract NNM07AB07C (NASA Solar-B X-Ray Telescope
Phase-E). This research has made use of NASA's Astrophysics Data System.
NR 143
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U2 11
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 2011
VL 736
IS 1
AR 3
DI 10.1088/0004-637X/736/1/3
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600003
ER
PT J
AU Vieregg, AG
Palladino, K
Allison, P
Baughman, BM
Beatty, JJ
Belov, K
Besson, DZ
Bevan, S
Binns, WR
Chen, C
Chen, P
Clem, JM
Connolly, A
Detrixhe, M
De Marco, D
Dowkontt, PF
DuVernois, M
Gorham, PW
Grashorn, EW
Hill, B
Hoover, S
Huang, M
Israel, MH
Javaid, A
Liewer, KM
Matsuno, S
Mercurio, BC
Miki, C
Mottram, M
Nam, J
Nichol, RJ
Romero-Wolf, A
Ruckman, L
Saltzberg, D
Seckel, D
Varner, GS
Wang, Y
AF Vieregg, A. G.
Palladino, K.
Allison, P.
Baughman, B. M.
Beatty, J. J.
Belov, K.
Besson, D. Z.
Bevan, S.
Binns, W. R.
Chen, C.
Chen, P.
Clem, J. M.
Connolly, A.
Detrixhe, M.
De Marco, D.
Dowkontt, P. F.
DuVernois, M.
Gorham, P. W.
Grashorn, E. W.
Hill, B.
Hoover, S.
Huang, M.
Israel, M. H.
Javaid, A.
Liewer, K. M.
Matsuno, S.
Mercurio, B. C.
Miki, C.
Mottram, M.
Nam, J.
Nichol, R. J.
Romero-Wolf, A.
Ruckman, L.
Saltzberg, D.
Seckel, D.
Varner, G. S.
Wang, Y.
TI THE FIRST LIMITS ON THE ULTRA-HIGH ENERGY NEUTRINO FLUENCE FROM
GAMMA-RAY BURSTS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma-ray burst: general; neutrinos
ID COSMIC-RAYS; AFTERGLOW; FIREBALLS
AB We set the first limits on the ultra-high energy (UHE) neutrino fluence at energies greater than 10(9) GeV from gamma-ray bursts (GRBs) based on data from the second flight of the Antarctic Impulsive Transient Antenna (ANITA). During the 31 day flight of ANITA-II, 26 GRBs were recorded by Swift or Fermi. Of these, we analyzed the 12 GRBs which occurred during quiet periods when the payload was away from anthropogenic activity. In a blind analysis, we observe 0 events on a total background of 0.0044 events in the combined prompt window for all 12 low-background bursts. We also observe 0 events from the remaining 14 bursts. We place a 90% confidence level limit on the E-4 prompt neutrino fluence between 10(8) GeV < E < 10(12) GeV of E-4 Phi = 2.5 x 10(17) GeV3 cm(-2) from GRB090107A. This is the first reported limit on the UHE neutrino fluence from GRBs above 10(9) GeV, and the strongest limit above 10(8) GeV.
C1 [Palladino, K.; Allison, P.; Baughman, B. M.; Beatty, J. J.; Connolly, A.; Grashorn, E. W.; Mercurio, B. C.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA.
[Besson, D. Z.; Detrixhe, M.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
[Bevan, S.; Mottram, M.; Nichol, R. J.] UCL, Dept Phys & Astron, London, England.
[Binns, W. R.; Dowkontt, P. F.; Israel, M. H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA.
[Chen, C.; Chen, P.; Huang, M.; Nam, J.; Wang, Y.] Natl Taiwan Univ, Dept Phys, Taipei, Taiwan.
[Clem, J. M.; De Marco, D.; Javaid, A.; Seckel, D.] Univ Delaware, Dept Phys, Newark, DE 19716 USA.
[DuVernois, M.; Gorham, P. W.; Hill, B.; Matsuno, S.; Miki, C.; Romero-Wolf, A.; Ruckman, L.; Varner, G. S.] Univ Hawaii Manoa, Dept Phys & Astron, Honolulu, HI 96822 USA.
[Liewer, K. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Vieregg, A. G.; Belov, K.; Hoover, S.; Saltzberg, D.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA.
RP Vieregg, AG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM avieregg@cfa.harvard.edu
RI Vieregg, Abigail/D-2287-2012; Belov, Konstantin/D-2520-2013; Connolly,
Amy/J-3958-2013; Beatty, James/D-9310-2011
OI Beatty, James/0000-0003-0481-4952
NR 22
TC 11
Z9 11
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 JUL 20
PY 2011
VL 736
IS 1
AR 50
DI 10.1088/0004-637X/736/1/50
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600050
ER
PT J
AU Wang, JF
Fabbiano, G
Elvis, M
Risaliti, G
Mundell, CG
Karovska, M
Zezas, A
AF Wang, Junfeng
Fabbiano, Giuseppina
Elvis, Martin
Risaliti, Guido
Mundell, Carole G.
Karovska, Margarita
Zezas, Andreas
TI A DEEP CHANDRA ACIS STUDY OF NGC 4151. II. THE INNERMOST EMISSION LINE
REGION AND STRONG EVIDENCE FOR RADIO JET-NLR CLOUD COLLISION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (NGC 4151); galaxies: jets; galaxies: Seyfert;
X-rays: galaxies
ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-4151; SOFT-X-RAY;
HUBBLE-SPACE-TELESCOPE; H-I; CIRCUMNUCLEAR REGION; NUMERICAL-SIMULATION;
EXTENDED EMISSION; VLA OBSERVATIONS; GEMINI NIFS
AB We have studied the X-ray emission within the inner similar to 150 pc radius of NGC 4151 by constructing high spatial resolution emission line images of blended O VII, OVIII, and Ne IX. These maps show extended structures that are spatially correlated with the radio outflow and optical [O III] emission. We find strong evidence for jet-gas cloud interaction, including morphological correspondences with regions of X-ray enhancement, peaks of near-infrared [Fe II] emission, and optical clouds. In these regions, moreover, we find evidence of elevated Ne IX/O VII ratios; the X-ray emission of these regions also exceeds that expected from nuclear photoionization. Spectral fitting reveals the presence of a collisionally ionized component. The thermal energy of the hot gas suggests that greater than or similar to 0.1% of the estimated jet power is deposited into the host interstellar medium through interaction between the radio jet and the dense medium of the circumnuclear region. We find possible pressure equilibrium between the collisionally ionized hot gas and the photoionized line-emitting cool clouds. We also obtain constraints on the extended iron and silicon fluorescent emission. Both lines are spatially unresolved. The upper limit on the contribution of an extended emission region to the Fe K alpha emission is less than or similar to 5% of the total, in disagreement with a previous claim that 65% of the Fe K alpha emission originates in the extended narrow line region.
C1 [Wang, Junfeng; Fabbiano, Giuseppina; Elvis, Martin; Risaliti, Guido; Karovska, Margarita; Zezas, Andreas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy.
[Mundell, Carole G.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
[Zezas, Andreas] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece.
RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM juwang@cfa.harvard.edu
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X
FU NASA [GO8-9101X, GO1-12009X, NAS8-03060]; CXC; Royal Society; Research
Councils, UK
FX We thank the anonymous referee for helpful suggestions. This work is
supported by NASA grant GO8-9101X (PI: Fabbiano) and grant GO1-12009X
(PI: Wang). We acknowledge support from the CXC, which is operated by
the Smithsonian Astrophysical Observatory (SAO) for and on behalf of
NASA under Contract NAS8-03060. C.G.M. acknowledges financial support
from the Royal Society and Research Councils, UK. J.W. thanks G.
Ferland, T. Kallman, S. Bianchi, A. Marinucci, and S. Chakravorty for
extensive advices on photoionization modeling, P. Nulsen for jet power
discussion, and T. Storchi-Bergmann and R. Riffel for providing the
Gemini NIFS maps. This research has made use of data obtained from the
Chandra Data Archive, and software provided by the CXC in the
application packages CIAO and Sherpa.
NR 72
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U1 0
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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 2011
VL 736
IS 1
AR 62
DI 10.1088/0004-637X/736/1/62
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 791EB
UT WOS:000292645600062
ER
PT J
AU Kocsis, B
Yunes, N
Loeb, A
AF Kocsis, Bence
Yunes, Nicolas
Loeb, Abraham
TI Observable signatures of extreme mass-ratio inspiral black hole binaries
embedded in thin accretion disks
SO PHYSICAL REVIEW D
LA English
DT Article
ID ACTIVE GALACTIC NUCLEI; ANGULAR-MOMENTUM TRANSPORT; I PLANETARY
MIGRATION; WAVE STANDARD SIRENS; GRAVITATIONAL-RADIATION; DYNAMICAL
FRICTION; MAGNETOHYDRODYNAMIC SIMULATIONS; 3-DIMENSIONAL SIMULATIONS;
PROTOSTELLAR DISKS; ORBITAL MIGRATION
AB We examine the electromagnetic and gravitational wave (GW) signatures of stellar-mass compact objects (COs) spiraling into a supermassive black hole (extreme mass-ratio inspirals), embedded in a thin, radiation-pressure dominated, accretion disk. At large separations, the tidal effect of the secondary CO clears a gap. We derive the conditions necessary for gap opening in a radiation-pressure dominated disk and show that the gap refills during the late GW-driven phase of the inspiral, leading to a sudden electromagnetic brightening of the source. The accretion disk leaves an imprint on the GW through its angular momentum exchange with the binary, the mass increase of the binary members due to accretion, and its gravity. We compute the disk-modified GWs both in an analytical Newtonian approximation and in a numerical effective-one-body approach. We find that disk-induced migration provides the dominant perturbation to the inspiral, with weaker effects from the mass accretion onto the CO and hydrodynamic drag. Depending on whether a gap is present, the perturbation of the GW phase is between 10 and 1000 rad per year, detectable with the future Laser Interferometer Space Antenna at high significance. The perturbation is significant for disk models with an effective viscosity proportional to gas pressure but much less so if proportional to the total pressure. The Fourier transform of the disk-modified GW in the stationary phase approximation is sensitive to disk parameters with a frequency trend different from postNewtonian vacuum corrections. Our results suggest that observations of extreme mass-ratio inspirals may place new sensitive constraints on the physics of accretion disks.
C1 [Kocsis, Bence; Yunes, Nicolas; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Yunes, Nicolas] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Yunes, Nicolas] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA.
RP Kocsis, B (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.
RI Kocsis, Bence/C-3061-2013
OI Kocsis, Bence/0000-0002-4865-7517
FU NASA [PF9-00063, PF0-110080, NNX08AL43G, NNA09DB30A]; National
Aeronautics Space Administration [NAS8-03060]; OTKA [68228]; NSF
[AST-0907890]
FX We are grateful to Cole Miller, Ramesh Narayan, Shane Davis, Scott
Hughes, Zoltan Haiman, and Jon McKinney for useful comments and
suggestions. B. K. and N. Y. acknowledge support from the NASA through
Einstein Postdoctoral Fellowship Award Nos. PF9-00063 and PF0-110080
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. B. K.
acknowledges partial support by OTKA Grant No. 68228. A. L. acknowledges
support from NSF Grant No. AST-0907890 and NASA Grants No. NNX08AL43G
and No. NNA09DB30A.
NR 179
TC 35
Z9 35
U1 0
U2 2
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 JUL 19
PY 2011
VL 84
IS 2
AR 024032
DI 10.1103/PhysRevD.84.024032
PG 41
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 794DL
UT WOS:000292875600002
ER
PT J
AU Covington, AM
Aguilar, A
Covington, IR
Hinojosa, G
Shirley, CA
Phaneuf, RA
Alvarez, I
Cisneros, C
Dominguez-Lopez, I
Sant'Anna, MM
Schlachter, AS
Ballance, CP
McLaughlin, BM
AF Covington, A. M.
Aguilar, A.
Covington, I. R.
Hinojosa, G.
Shirley, C. A.
Phaneuf, R. A.
Alvarez, I.
Cisneros, C.
Dominguez-Lopez, I.
Sant'Anna, M. M.
Schlachter, A. S.
Ballance, C. P.
McLaughlin, B. M.
TI Valence-shell photoionization of chlorinelike Ar+ ions
SO PHYSICAL REVIEW A
LA English
DT Article
ID DOUBLY-EXCITED RESONANCES; R-MATRIX THEORY; CROSS-SECTIONS; ORION
ASSOCIATION; ATOMIC IONS; C2+ IONS; ABSOLUTE; SPECTRUM; C+; SPECTROSCOPY
AB Absolute cross-section measurements for valence-shell photoionization of Ar+ ions are reported for photon energies ranging from 27.4 to 60.0 eV. The data, taken by merging beams of ions and synchrotron radiation at a photon energy resolution of 10 meV, indicate that the primary ion beam was a statistically weighted mixture of the P-2(3/2)o ground state and the P-2(1/2)o metastable state of Ar+. Photoionization of this Cl-like ion is characterized by multiple Rydberg series of autoionizing resonances superimposed on a direct photoionization continuum. Observed resonance line shapes indicate interference between indirect and direct photoionization channels. Resonance features are spectroscopically assigned and their energies and quantum defects are tabulated. The measurements are satisfactorily reproduced by theoretical calculations based on an intermediate coupling semirelativistic Breit-Pauli approximation.
C1 [Covington, A. M.; Aguilar, A.; Covington, I. R.; Hinojosa, G.; Shirley, C. A.; Phaneuf, R. A.] Univ Nevada, Dept Phys, Reno, NV 89557 USA.
[Alvarez, I.; Cisneros, C.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, Cuernavaca 62131, Morelos, Mexico.
[Dominguez-Lopez, I.; Sant'Anna, M. M.; Schlachter, A. S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Ballance, C. P.] Auburn Univ, Dept Phys, Auburn, AL 36840 USA.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Covington, AM (reprint author), Univ Nevada, Dept Phys, MS 220, Reno, NV 89557 USA.
RI Sant'Anna, Marcelo/B-9355-2013; Dominguez-Lopez, Ivan/B-6072-2016
OI Sant'Anna, Marcelo/0000-0001-5342-5799; Dominguez-Lopez,
Ivan/0000-0001-8084-8711
FU Office of Basic Energy Sciences, Chemical Sciences, Geosciences and
Energy Biosciences Division, of the US Department of Energy
[DE-FG03-00ER14787, DE-FG02-03ER15424]; University of Nevada, Reno;
Nevada DOE/EPSCoR; CONACyT through CCF-UNAM, Cuernavaca, Mexico;
DGAPA-UNAM-IN (Mexico) [113010]; CNPq (Brazil); US Department of Energy
through Auburn University; US National Science Foundation; Smithsonian
Astrophysical Observatory; Institute for Theoretical Atomic and
Molecular Physics (ITAMP)
FX The experimental work was supported by the Office of Basic Energy
Sciences, Chemical Sciences, Geosciences and Energy Biosciences
Division, of the US Department of Energy under Grants No.
DE-FG03-00ER14787 and No. DE-FG02-03ER15424 with the University of
Nevada, Reno; by the Nevada DOE/EPSCoR Program in Chemical Physics and
by CONACyT through the CCF-UNAM, Cuernavaca, Mexico. A. A. and M.M.S'A.
acknowledge support from DGAPA-UNAM-IN 113010 (Mexico) and CNPq
(Brazil), respectively. C. P. B. was supported by US Department of
Energy grants through Auburn University. B.M.McL. thanks the Institute
for Theoretical Atomic and Molecular Physics (ITAMP) for their
hospitality and support under the visitors program. ITAMP is supported
by a grant from the US National Science Foundation to Harvard University
and the Smithsonian Astrophysical Observatory. The computational work
was carried out at the National Energy Research Scientific Computing
Center in Oakland, CA, and on the Tera-grid at the National Institute
for Computational Sciences in Knoxville, Tennessee, which is supported
in part by the US National Science Foundation.
NR 46
TC 17
Z9 17
U1 2
U2 7
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 18
PY 2011
VL 84
IS 1
AR 013413
DI 10.1103/PhysRevA.84.013413
PG 11
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 793LH
UT WOS:000292823300012
ER
PT J
AU Lopano, CL
Heaney, PJ
Bandstra, JZ
Post, JE
Brantley, SL
AF Lopano, Christina L.
Heaney, Peter J.
Bandstra, Joel Z.
Post, Jeffrey E.
Brantley, Susan L.
TI Kinetic analysis of cation exchange in birnessite using time-resolved
synchrotron X-ray diffraction
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID ION-EXCHANGE; POWDER DIFFRACTION; RIETVELD REFINEMENT;
CRYSTAL-STRUCTURES; MANGANIC ACID; ALKALI; SELECTIVITY; MINERALS; PHASE;
RADII
AB In this study, we applied time-resolved synchrotron X-ray diffraction (TRXRD) to develop kinetic models that test a proposed two-stage reaction pathway for cation exchange in birnessite. These represent the first rate equations calculated for cation exchange in layered manganates. Our previous work has shown that the substitution of K, Cs, and Ba for interlayer Na in synthetic triclinic birnessite induces measurable changes in unit-cell parameters. New kinetic modeling of this crystallographic data supports our previously postulated two-stage reaction pathway for cation exchange, and we can correlate the kinetic steps with changes in crystal structure. In addition, the initial rates of cation exchange, R (angstrom(3) min(-1)), were determined from changes in unit-cell volume to follow these rate laws: R = 1.75[K(+) ((aq))](0.56), R = 41.1[Cs(+) ((aq))](1.10), R = 1.15[Ba(2+) ((aq))](0.50). Thus,the exchange rates for Na in triclinic birnessite decreased in the order: Cs >> K > Ba. These results are likely a function of hydration energy differences of the cations and the preference of the solution phase for the more readily hydrated cation. Published by Elsevier Ltd.
C1 [Lopano, Christina L.; Heaney, Peter J.; Bandstra, Joel Z.; Brantley, Susan L.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
[Lopano, Christina L.; Heaney, Peter J.; Bandstra, Joel Z.; Brantley, Susan L.] Penn State Univ, CEKA, University Pk, PA 16802 USA.
[Post, Jeffrey E.] Smithsonian NMNH, Dept Mineral Sci, Washington, DC 20013 USA.
[Brantley, Susan L.] Penn State Univ, Earth & Environm Syst Inst, University Pk, PA 16802 USA.
RP Lopano, CL (reprint author), US DOE, Natl Energy Technol Lab, 626 Cochrans Mill Rd,POB 10940, Pittsburgh, PA 15236 USA.
EM Christina.Lopano@netl.doe.gov
FU NSF [EAR04-17741, EAR07-45374]; Center for Environmental Kinetics
Analysis (CEKA); DOE [NSF CHE-0431328]; U.S. Department of Energy,
Division of Materials Sciences and Division of Chemical Sciences
[DE-AC02-98CH10886]
FX Funding for this research was provided by NSF grants EAR04-17741,
EAR07-45374, and the Center for Environmental Kinetics Analysis (CEKA),
an NSF-and DOE-sponsored Environmental Molecular Science Institute (NSF
CHE-0431328). 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. This
manuscript benefited greatly from the thoughtful feedback of three
anonymous reviewers, the associate editor, Dr. Peggy O'Day, and Ms.
Claire Fleeger at Penn State University.
NR 42
TC 10
Z9 11
U1 4
U2 31
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 JUL 15
PY 2011
VL 75
IS 14
BP 3973
EP 3981
DI 10.1016/j.gca.2011.04.021
PG 9
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 796YT
UT WOS:000293090100006
ER
PT J
AU Bovino, S
Zhang, P
Kharchenko, V
Dalgarno, A
AF Bovino, S.
Zhang, P.
Kharchenko, V.
Dalgarno, A.
TI Relaxation of energetic S(D-1) atoms in Xe gas: Comparison of ab initio
calculations with experimental data
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID CONSISTENT BASIS-SETS; FAST NITROGEN-ATOMS; JUPITERS ATMOSPHERE;
THERMALIZATION; COLLISIONS; AR; DISTRIBUTIONS
AB In this paper, we report our investigation of the translational energy relaxation of fast S(D-1) atoms in a Xe thermal bath. The interaction potential of Xe-S was constructed using ab initio methods. Total and differential cross sections were then calculated. The latter have been incorporated into the construction of the kernel of the Boltzmann equation describing the energy relaxation process. The solution of the Boltzmann equation was obtained and results were compared with those reported in experiments [G. Nan, and P. L. Houston, J. Chem. Phys. 97, 7865 (1992)]. Good agreement with the measured time-dependent relative velocity of fast S(D-1) atoms was obtained except at long relaxation times. The discrepancy may be due to the error accumulation caused by the use of hard sphere approximation and the Monte Carlo analysis of the experimental data. Our accurate description of the energy relaxation process led to an increase in the number of collisions required to achieve equilibrium by an order of magnitude compared to the number given by the hard-sphere approximation. (C) 2011 American Institute of Physics. [doi: 10.1063/1.3600352]
C1 [Zhang, P.; Kharchenko, V.; Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
[Bovino, S.] Univ Roma La Sapienza, Dept Chem, I-00185 Rome, Italy.
[Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
RP Dalgarno, A (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
EM adalgarno@cfa.harvard.edu
FU Chemical Science, Geoscience, and Bioscience Division of the Office of
Basic Energy Science, Office of Science, (U.S.) Department of Energy
(DOE); NASA [NNX10AB88G, NNX09AF13G]
FX This research of A.D. and P.Z. 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 (DOE) and of
V.K. by NASA Grant Nos. NNX10AB88G and NNX09AF13G. S.B. thanks ITAMP and
the Harvard-Smithsonian Center for Astrophysics for his participation in
their exchange visitor program.
NR 33
TC 3
Z9 3
U1 1
U2 11
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 JUL 14
PY 2011
VL 135
IS 2
AR 024304
DI 10.1063/1.3600352
PG 7
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 792UN
UT WOS:000292776000024
PM 21766939
ER
PT J
AU Mazur, JE
Crain, WR
Looper, MD
Mabry, DJ
Blake, JB
Case, AW
Golightly, MJ
Kasper, JC
Spence, HE
AF Mazur, J. E.
Crain, W. R.
Looper, M. D.
Mabry, D. J.
Blake, J. B.
Case, A. W.
Golightly, M. J.
Kasper, J. C.
Spence, H. E.
TI New measurements of total ionizing dose in the lunar environment
SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS
LA English
DT Article
ID SOLAR-WIND
AB We report new measurements of solar minimum ionizing radiation dose at the Moon onboard the Lunar Reconnaissance Orbiter (LRO) from June 2009 through May 2010. The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument on LRO houses a compact and highly precise microdosimeter whose design allows measurements of dose rates below 1 micro-Rad per second in silicon achieved with minimal resources (20 g, similar to 250 milliwatts, and similar to 3 bits/second). We envision the use of such a small yet accurate dosimeter in many future spaceflight applications where volume, mass, and power are highly constrained. As this was the first operation of the microdosimeter in a space environment, the goal of this study is to verify its response by using simultaneous measurements of the galactic cosmic ray ionizing environment at LRO, at L1, and with other concurrent dosimeter measurements and model predictions. The microdosimeter measured the same short timescale modulations in the galactic cosmic rays as the other independent measurements, thus verifying its response to a known source of minimum-ionizing particles. The total dose for the LRO mission over the first 333 days was only 12.2 Rads behind similar to 130 mils of aluminum because of the delayed rise of solar activity in solar cycle 24 and the corresponding lack of intense solar energetic particle events. The dose rate in a 50 km lunar orbit was about 30 percent lower than the interplanetary rate, as one would expect from lunar obstruction of the visible sky.
C1 [Mazur, J. E.] Aerosp Corp, Chantilly, VA 20151 USA.
[Crain, W. R.; Looper, M. D.; Mabry, D. J.; Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA.
[Case, A. W.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Golightly, M. J.; Spence, H. E.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA.
RP Mazur, JE (reprint author), Aerosp Corp, 15049 Conf Ctr Dr, Chantilly, VA 20151 USA.
EM joseph.mazur@aero.org
RI Kasper, Justin/D-1152-2010; Spence, Harlan/A-1942-2011;
OI Kasper, Justin/0000-0002-7077-930X; Spence, Harlan/0000-0002-2526-2205
NR 16
TC 19
Z9 19
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 1542-7390
J9 SPACE WEATHER
JI Space Weather
PD JUL 14
PY 2011
VL 9
AR S07002
DI 10.1029/2010SW000641
PG 12
WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology &
Atmospheric Sciences
GA 793QM
UT WOS:000292838200002
ER
PT J
AU Willis, EL
Kersey, DC
Durrant, BS
Kouba, AJ
AF Willis, Erin L.
Kersey, David C.
Durrant, Barbara S.
Kouba, Andrew J.
TI The Acute Phase Protein Ceruloplasmin as a Non-Invasive Marker of
Pseudopregnancy, Pregnancy, and Pregnancy Loss in the Giant Panda
SO PLOS ONE
LA English
DT Article
ID AILUROPODA-MELANOLEUCA; OXIDASE ACTIVITY; STEROID METABOLITES;
ENZYME-IMMUNOASSAY; PRE-ECLAMPSIA; HUMAN SERUM; COPPER;
IMMUNOPOTENTIATION; HETEROGENEITY; HYPERTENSION
AB After ovulation, non-pregnant female giant pandas experience pseudopregnancy. During pseudopregnancy, non-pregnant females exhibit physiological and behavioral changes similar to pregnancy. Monitoring hormonal patterns that are usually different in pregnant mammals are not effective at determining pregnancy status in many animals that undergo pseudopregnancy, including the giant panda. Therefore, a physiological test to distinguish between pregnancy and pseudopregnancy in pandas has eluded scientists for decades. We examined other potential markers of pregnancy and found that activity of the acute phase protein ceruloplasmin increases in urine of giant pandas in response to pregnancy. Results indicate that in term pregnancies, levels of active urinary ceruloplasmin were elevated the first week of pregnancy and remain elevated until 20-24 days prior to parturition, while no increase was observed during the luteal phase in known pseudopregnancies. Active ceruloplasmin also increased during ultrasound-confirmed lost pregnancies; however, the pattern was different compared to term pregnancies, particularly during the late luteal phase. In four out of the five additional reproductive cycles included in the current study where females were bred but no birth occurred, active ceruloplasmin in urine increased during the luteal phase. Similar to the known lost pregnancies, the temporal pattern of change in urinary ceruloplasmin during the luteal phase deviated from the term pregnancies suggesting that these cycles may have also been lost pregnancies. Among giant pandas in captivity, it has been presumed that there is a high rate of pregnancy loss and our results are the first to provide evidence supporting this notion.
C1 [Willis, Erin L.; Kouba, Andrew J.] Memphis Zool Soc, Dept Conservat & Res, Memphis, TN USA.
[Kersey, David C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Dept Reprod Sci, Ctr Species Survival, Front Royal, VA USA.
[Durrant, Barbara S.] San Diego Zoo Global, Inst Conservat Res, Reprod Physiol Div, Escondido, CA USA.
RP Willis, EL (reprint author), Memphis Zool Soc, Dept Conservat & Res, Memphis, TN USA.
EM ewillis@memphiszoo.org
FU Memphis Zoo Department of Conservation and Research
FX Support for this work was provided by the Memphis Zoo Department of
Conservation and Research's TM Giant Panda Physiology and Nutrition
Research Program. The director of the Memphis Zoo's Department of
Conservation and Research partipated in the decision to fund the
project, and in the preparation of and decision to publish the
manuscript.
NR 52
TC 11
Z9 11
U1 2
U2 26
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 JUL 13
PY 2011
VL 6
IS 7
AR e21159
DI 10.1371/journal.pone.0021159
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 792WQ
UT WOS:000292781500003
PM 21765892
ER
PT J
AU Lamata, L
Leibrandt, DR
Chuang, IL
Cirac, JI
Lukin, MD
Vuletic, V
Yelin, SF
AF Lamata, L.
Leibrandt, D. R.
Chuang, I. L.
Cirac, J. I.
Lukin, M. D.
Vuletic, V.
Yelin, S. F.
TI Ion Crystal Transducer for Strong Coupling between Single Ions and
Single Photons
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID QUANTUM STATE TRANSFER; ATOMIC ENSEMBLES; OPTICAL CAVITY; TRAPPED IONS;
COMMUNICATION; ENTANGLEMENT; COMPUTATION
AB A new approach for the realization of a quantum interface between single photons and single ions in an ion crystal is proposed and analyzed. In our approach the coupling between a single photon and a single ion is enhanced via the collective degrees of freedom of the ion crystal. Applications including single-photon generation, a memory for a quantum repeater, and a deterministic photon-photon, photon-phonon, or photon-ion entangler are discussed.
C1 [Lamata, L.; Cirac, J. I.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany.
[Leibrandt, D. R.; Chuang, I. L.; Vuletic, V.] MIT, Dept Phys, Ctr Ultracold Atoms, Cambridge, MA 02139 USA.
[Lukin, M. D.; Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
[Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA.
RP Lamata, L (reprint author), Max Planck Inst Quantum Opt, Hans Kopfermann Str 1, D-85748 Garching, Germany.
EM lucas.lamata@mpq.mpg.de
RI Lamata, Lucas/B-2439-2009
OI Lamata, Lucas/0000-0002-9504-8685
FU EU; DFG Forschergruppe [635]; NSF CUA; DARPA QUEST; AFOSR MURI; Packard
Foundation; NSF [PHY-0970055]
FX We thank M. C. Banuls, A. V. Gorshkov, O. Romero-Isart, T. Schatz, and
H. Schwager for fruitful discussions. We acknowledge funding from EU
projects AQUTE and COMPAS, from DFG Forschergruppe 635, from the NSF
CUA, DARPA QUEST, AFOSR MURI, and the Packard Foundation. S. F. Y.
acknowledges funding from NSF through Grant No. PHY-0970055.
NR 29
TC 15
Z9 15
U1 0
U2 10
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 11
PY 2011
VL 107
IS 3
AR 030501
DI 10.1103/PhysRevLett.107.030501
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 790OA
UT WOS:000292597400003
PM 21838337
ER
PT J
AU Sant'Anna, MM
Schlachter, AS
Ohrwall, G
Stolte, WC
Lindle, DW
McLaughlin, BM
AF Sant'Anna, M. M.
Schlachter, A. S.
Oehrwall, G.
Stolte, W. C.
Lindle, D. W.
McLaughlin, B. M.
TI K-Shell X-Ray Spectroscopy of Atomic Nitrogen
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID PHOTOIONIZATION CROSS-SECTIONS; PHOTOABSORPTION; OXYGEN; IONS;
SCATTERING; MOLECULE; Z=1-92; N-2
AB Absolute K-shell photoionization cross sections for atomic nitrogen have been obtained from both experiment and state-of-the-art theoretical techniques. Because of the difficulty of creating a target of neutral atomic nitrogen, no high-resolution K-edge spectroscopy measurements have been reported for this important atom. Interplay between theory and experiment enabled identification and characterization of the strong 1s -> np resonance features throughout the threshold region. An experimental value of 409.64 +/- 0.02 eV was determined for the K-shell binding energy.
C1 [Sant'Anna, M. M.; Schlachter, A. S.] Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
[Oehrwall, G.; Stolte, W. C.; Lindle, D. W.] Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
[McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
RP Sant'Anna, MM (reprint author), Univ Fed Rio de Janeiro, Inst Fis, Caixa Postal 68528, BR-21941972 Rio De Janeiro, Brazil.
RI Sant'Anna, Marcelo/B-9355-2013
OI Sant'Anna, Marcelo/0000-0001-5342-5799
FU NSF; DOE; DOE Facilities Initiative; Nevada DOE EPSCoR; CNPq (Brazil);
NASA
FX The experiments were supported by NSF, DOE, the DOE Facilities
Initiative, Nevada DOE EPSCoR, and CNPq (Brazil). The theoretical work
was supported by NSF and NASA grants to ITAMP at the Harvard-Smithsonian
Center for Astrophysics and the Smithsonian Astrophysical Observatory.
The computational work was done at the National Energy Research
Scientific Computing Center in Oakland, CA and on the Tera-grid at the
National Institute for Computational Sciences (NICS), in Knoxville, TN,
which is supported in part by NSF.
NR 34
TC 12
Z9 12
U1 2
U2 7
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 11
PY 2011
VL 107
IS 3
AR 033001
DI 10.1103/PhysRevLett.107.033001
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 790OA
UT WOS:000292597400007
PM 21838354
ER
PT J
AU Story, K
Aird, KA
Andersson, K
Armstrong, R
Bazin, G
Benson, BA
Bleem, LE
Bonamente, M
Brodwin, M
Carlstrom, JE
Chang, CL
Clocchiatti, A
Crawford, TM
Crites, AT
de Haan, T
Desai, S
Dobbs, MA
Dudley, JP
Foley, RJ
George, EM
Gladders, MD
Gonzalez, AH
Halverson, NW
High, FW
Holder, GP
Holzapfel, WL
Hoover, S
Hrubes, JD
Joy, M
Keisler, R
Knox, L
Lee, AT
Leitch, EM
Lueker, M
Luong-Van, D
Marrone, DP
McMahon, JJ
Mehl, J
Meyer, SS
Mohr, JJ
Montroy, TE
Padin, S
Plagge, T
Pryke, C
Reichardt, CL
Rest, A
Ruel, J
Ruhl, JE
Saliwanchik, BR
Saro, A
Schaffer, KK
Shaw, L
Shirokoff, E
Song, J
Spieler, HG
Stalder, B
Staniszewski, Z
Stark, AA
Stubbs, CW
Vanderlinde, K
Vieira, JD
Williamson, R
Zenteno, A
AF Story, K.
Aird, K. A.
Andersson, K.
Armstrong, R.
Bazin, G.
Benson, B. A.
Bleem, L. E.
Bonamente, M.
Brodwin, M.
Carlstrom, J. E.
Chang, C. L.
Clocchiatti, A.
Crawford, T. M.
Crites, A. T.
de Haan, T.
Desai, S.
Dobbs, M. A.
Dudley, J. P.
Foley, R. J.
George, E. M.
Gladders, M. D.
Gonzalez, A. H.
Halverson, N. W.
High, F. W.
Holder, G. P.
Holzapfel, W. L.
Hoover, S.
Hrubes, J. D.
Joy, M.
Keisler, R.
Knox, L.
Lee, A. T.
Leitch, E. M.
Lueker, M.
Luong-Van, D.
Marrone, D. P.
McMahon, J. J.
Mehl, J.
Meyer, S. S.
Mohr, J. J.
Montroy, T. E.
Padin, S.
Plagge, T.
Pryke, C.
Reichardt, C. L.
Rest, A.
Ruel, J.
Ruhl, J. E.
Saliwanchik, B. R.
Saro, A.
Schaffer, K. K.
Shaw, L.
Shirokoff, E.
Song, J.
Spieler, H. G.
Stalder, B.
Staniszewski, Z.
Stark, A. A.
Stubbs, C. W.
Vanderlinde, K.
Vieira, J. D.
Williamson, R.
Zenteno, A.
TI SOUTH POLE TELESCOPE DETECTIONS OF THE PREVIOUSLY UNCONFIRMED PLANCK
EARLY SUNYAEV-ZEL'DOVICH CLUSTERS IN THE SOUTHERN HEMISPHERE
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: clusters: individual (PLCKESZ
G255.62-46.16, PLCKESZ G225.92-19.99, PLCKESZ G264.41+19.48, PLCKESZ
G283.16-29.93, PLCKESZ G304.84-41.42)
ID SOURCE CATALOG; COSMOLOGY; SKY
AB We present South Pole Telescope (SPT) observations of the five galaxy cluster candidates in the southern hemisphere which were reported as unconfirmed in the Planck Early Sunyaev-Zel'dovich (ESZ) sample. One cluster candidate, PLCKESZ G255.62-46.16, is located in the 2500 deg(2) SPT SZ survey region and was reported previously as SPT-CL J0411-4819. For the remaining four candidates, which are located outside of the SPT SZ survey region, we performed short, dedicated SPT observations. Each of these four candidates was strongly detected in maps made from these observations, with signal-to-noise ratios ranging from 6.3 to 13.8. We have observed these four candidates on theMagellan-Baade telescope and used these data to estimate cluster redshifts from the red sequence. Resulting redshifts range from 0.24 to 0.46. We report measurements of Y(0'.75), the integrated Comptonization within a 0'.75 radius, for all five candidates. We also report X-ray luminosities calculated from ROSAT All-Sky Survey catalog counts, as well as optical and improved SZ coordinates for each candidate. The combination of SPT SZ measurements, optical red-sequence measurements, and X-ray luminosity estimates demonstrates that these five Planck ESZ cluster candidates do indeed correspond to real galaxy clusters with redshifts and observable properties consistent with the rest of the ESZ sample.
C1 [Story, K.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.
[Story, K.; Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA.
[Andersson, K.; Bazin, G.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany.
[Andersson, K.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Armstrong, R.; Desai, S.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA.
[Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany.
[Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[Bonamente, M.] Univ Alabama, Dept Phys, Huntsville, AL 35812 USA.
[Brodwin, M.; Foley, R. J.; Stalder, B.; Stark, A. A.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
[Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, HEP Div, Argonne, IL 60439 USA.
[Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
[de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
[Desai, S.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
[Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA.
[Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA.
[Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, VP62, Huntsville, AL 35812 USA.
[Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA.
[Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA.
[Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA.
[Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA.
[Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA.
[Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA.
[Rest, A.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.
[Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA.
[Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA.
RP Story, K (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
EM kstory@uchicago.edu
RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015;
Holzapfel, William/I-4836-2015;
OI Stubbs, Christopher/0000-0003-0347-1724; Williamson,
Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird,
Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169;
Stark, Antony/0000-0002-2718-9996
FU NSF [ANT-0638937, PHY-0114422, AST-1009012, AST-1009649, MRI-0723073];
Kavli Foundation; Gordon and Betty Moore Foundation; NSERC of Canada;
Quebec Fonds de recherche sur la nature et les technologies; CIAR; KICP;
CONICYT [Basal CATA PFB 06/09, 15010003]
FX The SPT is supported by NSF grant ANT-0638937. Partial support is also
provided by NSF grant PHY-0114422, the Kavli Foundation, and the Gordon
and Betty Moore Foundation. The McGill group acknowledges funding from
the NSERC of Canada, the Quebec Fonds de recherche sur la nature et les
technologies, and the CIAR. Galaxy cluster research is supported at
Harvard by NSF grant AST-1009012 and at SAO by NSF grants AST-1009649
and MRI-0723073. Benson acknowledges support from a KICP Fellowship, M.
Brodwin from the W. M. Keck Foundation, A. Clocchiatti from CONICYT
grants Basal CATA PFB 06/09 and FONDAP No. 15010003, R. J. Foley from a
Clay Fellowship, R. Keisler from NASA Hubble Fellowship grant
HF-51275.01, and B. Stalder from the Brinson Foundation.
NR 18
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U1 1
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PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 10
PY 2011
VL 735
IS 2
AR L36
DI 10.1088/2041-8205/735/2/L36
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OU
UT WOS:000293138000012
ER
PT J
AU Alatalo, K
Blitz, L
Young, LM
Davis, TA
Bureau, M
Lopez, LA
Cappellari, M
Scott, N
Shapiro, KL
Crocker, AF
Martin, S
Bois, M
Bournaud, F
Davies, RL
de Zeeuw, PT
Duc, PA
Emsellem, E
Falcon-Barroso, J
Khochfar, S
Krajnovic, D
Kuntschner, H
Lablanche, PY
McDermid, RM
Morganti, R
Naab, T
Oosterloo, T
Sarzi, M
Serra, P
Weijmans, A
AF Alatalo, K.
Blitz, L.
Young, L. M.
Davis, T. A.
Bureau, M.
Lopez, L. A.
Cappellari, M.
Scott, N.
Shapiro, K. L.
Crocker, A. F.
Martin, S.
Bois, M.
Bournaud, F.
Davies, R. L.
de Zeeuw, P. T.
Duc, P. -A.
Emsellem, E.
Falcon-Barroso, J.
Khochfar, S.
Krajnovic, D.
Kuntschner, H.
Lablanche, P. -Y.
McDermid, R. M.
Morganti, R.
Naab, T.
Oosterloo, T.
Sarzi, M.
Serra, P.
Weijmans, A.
TI DISCOVERY OF AN ACTIVE GALACTIC NUCLEUS DRIVEN MOLECULAR OUTFLOW IN THE
LOCAL EARLY-TYPE GALAXY NGC 1266
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: ISM; galaxies: kinematics and dynamics;
ISM: jets and outflows
ID MULTI-GAUSSIAN EXPANSION; STAR-FORMING GALAXIES; NEARBY GALAXIES;
BLACK-HOLES; ELLIPTIC GALAXIES; RADIO GALAXIES; SAURON PROJECT; IC 5063;
GAS; SPITZER
AB We report the discovery of a powerful molecular wind from the nucleus of the non-interacting nearby S0 field galaxy NGC 1266. The single-dish CO profile exhibits emission to +/- 400 km s(-1) and requires a nested Gaussian fit to be properly described. Interferometric observations reveal a massive, centrally concentrated molecular component with a mass of 1.1 x 10(9) M-circle dot and a molecular outflow with a molecular mass of approximate to 2.4 x 10(7) M-circle dot. The molecular gas close to the systemic velocity consists of a rotating, compact nucleus with a mass of about 4.1 x 10(8) M-circle dot within a radius of approximate to 60 pc. This compact molecular nucleus has a surface density of approximate to 2.7 x 10(4) M-circle dot pc(-2), more than two orders of magnitude larger than that of giant molecular clouds in the disk of the Milky Way, and it appears to sit on the Kennicutt-Schmidt relation despite its extreme kinematics and energetic activity. We interpret this nucleus as a disk that confines the outflowing wind. A mass outflow rate of approximate to 13 M-circle dot yr(-1) leads to a depletion timescale of less than or similar to 85 Myr. The star formation in NGC 1266 is insufficient to drive the outflow, and thus it is likely driven by the active galactic nucleus. The concentration of the majority of the molecular gas in the central 100 pc requires an extraordinary loss of angular momentum, but no obvious companion or interacting galaxy is present to enable the transfer. NGC 1266 is the first known outflowing molecular system that does not show any evidence of a recent interaction.
C1 [Alatalo, K.; Blitz, L.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Young, L. M.] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA.
[Davis, T. A.; Bureau, M.; Cappellari, M.; Scott, N.; Davies, R. L.] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England.
[Lopez, L. A.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Shapiro, K. L.; Lablanche, P. -Y.] Northrop Grumman Aerosp Syst, Aerosp Res Labs, Redondo Beach, CA 90278 USA.
[Crocker, A. F.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
[Martin, S.] European So Observ, Santiago 19, Chile.
[Martin, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Bois, M.; Emsellem, E.] Observ Paris, LERMA, F-75014 Paris, France.
[Bois, M.; Emsellem, E.] CNRS, F-75014 Paris, France.
[Bois, M.; Emsellem, E.] Univ Lyon 1, Observ Lyon, Ctr Rech Astrophys Lyon, F-69230 St Genis Laval, France.
[Bois, M.; Emsellem, E.] Ecole Normale Super Lyon, F-69230 St Genis Laval, France.
[Bournaud, F.; Duc, P. -A.] Univ Paris Diderot, CEA Saclay, Lab AIM, DSM,IRFU,SAp CNRS, F-91191 Gif Sur Yvette, France.
[de Zeeuw, P. T.; Emsellem, E.; Krajnovic, D.; Kuntschner, H.] European So Observ, D-85748 Garching, Germany.
[de Zeeuw, P. T.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Falcon-Barroso, J.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain.
[Falcon-Barroso, J.] ULL, Dept Astrofis, E-38206 Tenerife, Spain.
[Khochfar, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
[McDermid, R. M.] N Operat Ctr, Gemini Observ, Hilo, HI 96720 USA.
[Morganti, R.; Oosterloo, T.; Serra, P.] ASTRON, NL-7990 AA Dwingeloo, Netherlands.
[Morganti, R.; Oosterloo, T.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Naab, T.] Max Planck Inst Astrophys, D-85741 Garching, Germany.
[Sarzi, M.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL1 09AB, Herts, England.
[Weijmans, A.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
RP Alatalo, K (reprint author), Univ Calif Berkeley, Dept Astron, Campbell Hall, Berkeley, CA 94720 USA.
RI Bournaud, Frederic/K-1263-2013;
OI Davis, Timothy/0000-0003-4932-9379; Kuntschner,
Harald/0000-0002-2768-1198; Alatalo, Katherine/0000-0002-4261-2326;
Scott, Nicholas/0000-0001-8495-8547; Cappellari,
Michele/0000-0002-1283-8420
FU NSF [AST-0838258]; UK Research Councils [PP/E001114/1, ST/H002456/1];
Christ Church, Oxford; Royal Society [502011.K502/jd]; DFG; National
Aeronautics and Space Administration [11700538, NAS8-03060]; state of
California; state of Illinois; state of Maryland; Gordon and Betty Moore
Foundation; Kenneth T. and Eileen L. Norris Foundation; Associates of
the California Institute of Technology; National Science Foundation;
CARMA partner universities; Smithsonian Institution; Academia Sinica;
INSU/CNRS (France); MPG (Germany); ING (Spain); STFC [PP/D005574/1];
Gemini Observatory
FX K.A. thanks P. Chang, C. Heiles, N. Murray, and R. Plambeck for useful
ideas and conversations. K. A. also thanks A. Chung, M. Yun, C.
Feruglio, and the referee for their helpful discussions. The research of
K. Alatalo is supported by the NSF grant AST-0838258. R. L. D. is
supported by the rolling grants "Astrophysics at Oxford" PP/E001114/1
and ST/H002456/1 from the UK Research Councils. R. L. D. acknowledges
travel and computer grants from Christ Church, Oxford and support from
the Royal Society in the form of a Wolfson Merit Award 502011.K502/jd.
T. N. acknowledges support from the DFG Cluster of Excellence: "Origin
and Structure of the Universe." Support for this work was provided by
the National Aeronautics and Space Administration through Chandra Award
Number 11700538 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. Support for CARMA construction was derived from the states
of California, Illinois, and Maryland, the Gordon and Betty Moore
Foundation, the Kenneth T. and Eileen L. Norris Foundation, the
Associates of the California Institute of Technology, and the National
Science Foundation. Ongoing CARMA development and operations are
supported by the National Science Foundation under a cooperative
agreement, and by the CARMA partner universities. 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 data obtained from the
Chandra Data Archive and the Chandra Source Catalog, and software
provided by the Chandra X-ray Center (CXC) in the application packages
CIAO, ChIPS, and Sherpa. The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc. This paper is partly based on
observations carried out with the IRAM 30 m telescope. IRAM is supported
by INSU/CNRS (France), MPG (Germany), and ING (Spain). We acknowledge
use of the HYPERLEDA database (http://leda.univ-lyon1.fr) 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. M. C.
acknowledges support from a STFC Advanced Fellowship (PP/D005574/1) and
a Royal Society University Research Fellowship. RMcD is supported by the
Gemini Observatory, which is operated by the Association of Universities
for Research in Astronomy, Inc., on behalf of the international Gemini
partnership of Argentina, Australia, Brazil, Canada, Chile, the United
Kingdom, and the United States of America.
NR 67
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 88
DI 10.1088/0004-637X/735/2/88
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700021
ER
PT J
AU Coomber, G
Heinke, CO
Cohn, HN
Lugger, PM
Grindlay, JE
AF Coomber, G.
Heinke, C. O.
Cohn, H. N.
Lugger, P. M.
Grindlay, J. E.
TI THE UNUSUAL X-RAY BINARIES OF THE GLOBULAR CLUSTER NGC 6652
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE globular clusters: individual (NGC 6652); novae, cataclysmic variables;
stars: neutron; X-rays: binaries
ID XMM-NEWTON OBSERVATIONS; NEUTRON-STAR; GALACTIC-CENTER; CATACLYSMIC
VARIABLES; GLOBULAR-CLUSTER-47 TUCANAE; OPTICAL COUNTERPART; NGC-6652;
QUIESCENCE; EMISSION; ASCA
AB Our 5 ks Chandra ACIS-S observation of the globular cluster NGC 6652 detected seven X-ray sources, three of which were previously unidentified. This cluster hosts a well-known bright low-mass X-ray binary, source A (or XB1832-330). Source B shows unusual rapid flaring variability, with an average L-X(0.5-10 keV) similar to 2 x 10(34) erg s(-1), but with minutes-long flares up to L-X = 9 x 10(34) erg s(-1). Its spectrum can be fit by an absorbed power law of photon index Gamma similar to 1.24 and hardens as the count rate decreases. This suggests that part or all of the variation might be due to obscuration by the rim of a highly inclined accretion disk. Sources C and D, with L-X similar to 10(33) erg s(-1), have soft and unusual spectra. Source C requires a very soft component, with a spectrum peaking at 0.5 keV, which might be the hot polar cap of a magnetically accreting polar cataclysmic variable. Source D shows a soft spectrum (fit by a power law of photon index similar to 2.3) with marginal evidence for an emission line around 1 keV; its nature is unclear. The faint new sources E, F, and G have luminosities of 1-2 x 10(32) erg s(-1), if associated with the cluster (which is likely). E and F have relatively hard spectra (consistent with power laws with photon index similar to 1.5). G lacks soft photons, suggesting absorption with N-H > 10(22) cm(-2).
C1 [Coomber, G.; Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada.
[Cohn, H. N.; Lugger, P. M.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA.
[Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Coomber, G (reprint author), Univ Alberta, Dept Phys, 11322-89 Ave, Edmonton, AB T6G 2G7, Canada.
EM heinke@ualberta.ca
OI Heinke, Craig/0000-0003-3944-6109
FU NASA; NSERC; Alberta
FX We acknowledge support from NASA Chandra grants, an NSERC Discovery
Grant, and an Alberta Ingenuity New Faculty Award. We thank M. Muno for
his assistance in obtaining these observations.
NR 51
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 95
DI 10.1088/0004-637X/735/2/95
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700028
ER
PT J
AU Johnson, H
Raymond, JC
Murphy, NA
Giordano, S
Ko, YK
Ciaravella, A
Suleiman, R
AF Johnson, H.
Raymond, J. C.
Murphy, N. A.
Giordano, S.
Ko, Y. -K.
Ciaravella, A.
Suleiman, R.
TI TRANSITION REGION EMISSION FROM SOLAR FLARES DURING THE IMPULSIVE PHASE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun:
flares; Sun: UV radiation
ID CORONAL MASS EJECTION; 2002 JULY 23; HARD X-RAY; CHROMOSPHERIC
EVAPORATION; WHITE-LIGHT; SOHO OBSERVATIONS; ATOMIC DATABASE; SOURCE
MOTIONS; RHESSI; PLASMA
AB There are relatively few observations of UV emission during the impulsive phases of solar flares, so the nature of that emission is poorly known. Photons produced by solar flares can resonantly scatter off atoms and ions in the corona. Based on off-limb measurements by the Solar and Heliospheric Observatory/Ultraviolet Coronagraph Spectrometer, we derive the O VI lambda 1032 luminosities for 29 flares during the impulsive phase and the Ly alpha luminosities of 5 flares, and we compare them with X-ray luminosities from GOES measurements. The upper transition region and lower transition region luminosities of the events observed are comparable. They are also comparable to the luminosity of the X-ray emitting gas at the beginning of the flare, but after 10-15 minutes the X-ray luminosity usually dominates. In some cases, we can use Doppler dimming to estimate flow speeds of the O VI emitting gas, and five events show speeds in the 40-80 km s(-1) range. The O VI emission could originate in gas evaporating to fill the X-ray flare loops, in heated chromospheric gas at the footpoints, or in heated prominence material in the coronal mass ejection. All three sources may contribute in different events or even in a single event, and the relative timing of UV and X-ray brightness peaks, the flow speeds, and the total O VI luminosity favor each source in one or more events.
C1 [Johnson, H.; Raymond, J. C.; Murphy, N. A.; Suleiman, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Johnson, H.] Northeastern Univ, Dept Phys, Dana Res Ctr 111, Boston, MA 02115 USA.
[Giordano, S.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
[Ko, Y. -K.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA.
[Ciaravella, A.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy.
RP Johnson, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Ciaravella, Angela/0000-0002-3127-8078; Murphy,
Nicholas/0000-0001-6628-8033; Giordano, Silvio/0000-0002-3468-8566
FU NASA [NNG06GG78G, NNX09AB17G-R]
FX This work was supported by NASA grants NNG06GG78G and NNX09AB17G-R to
the Smithsonian Astrophysical Observatory. SOHO is a project of
international cooperation between ESA and NASA.
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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 2011
VL 735
IS 2
AR 70
DI 10.1088/0004-637X/735/2/70
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700003
ER
PT J
AU Kim, DW
Protopapas, P
Byun, YI
Alcock, C
Khardon, R
Trichas, M
AF Kim, Dae-Won
Protopapas, Pavlos
Byun, Yong-Ik
Alcock, Charles
Khardon, Roni
Trichas, Markos
TI QUASI-STELLAR OBJECT SELECTION ALGORITHM USING TIME VARIABILITY AND
MACHINE LEARNING: SELECTION OF 1620 QUASI-STELLAR OBJECT CANDIDATES FROM
MACHO LARGE MAGELLANIC CLOUD DATABASE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Magellanic Clouds; methods: data analysis; quasars: general
ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; DIFFERENCE IMAGE-ANALYSIS;
GRAVITATIONAL LENSING EXPERIMENT; TERM OPTICAL VARIABILITY; SUPPORT
VECTOR MACHINES; HERBIG-AE/BE STARS; X-RAY SOURCES; II BULGE DATA;
VARIABLE-STARS
AB We present a new quasi-stellar object (QSO) selection algorithm using a Support Vector Machine, a supervised classification method, on a set of extracted time series features including period, amplitude, color, and autocorrelation value. We train a model that separates QSOs from variable stars, non-variable stars, and microlensing events using 58 known QSOs, 1629 variable stars, and 4288 non-variables in the MAssive Compact Halo Object (MACHO) database as a training set. To estimate the efficiency and the accuracy of the model, we perform a cross-validation test using the training set. The test shows that the model correctly identifies similar to 80% of known QSOs with a 25% false-positive rate. The majority of the false positives are Be stars. We applied the trained model to the MACHO Large Magellanic Cloud (LMC) data set, which consists of 40 million light curves, and found 1620 QSO candidates. During the selection none of the 33,242 known MACHO variables were misclassified as QSO candidates. In order to estimate the true false-positive rate, we crossmatched the candidates with astronomical catalogs including the Spitzer Surveying the Agents of a Galaxy's Evolution LMC catalog and a few X-ray catalogs. The results further suggest that the majority of the candidates, more than 70%, are QSOs.
C1 [Kim, Dae-Won; Protopapas, Pavlos; Alcock, Charles; Trichas, Markos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kim, Dae-Won; Byun, Yong-Ik] Yonsei Univ, Dept Astron, Seoul 120749, South Korea.
[Byun, Yong-Ik] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea.
[Kim, Dae-Won; Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA.
[Khardon, Roni] Tufts Univ, Dept Comp Sci, Medford, MA 02155 USA.
RP Kim, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU FAS Research Computing Group at Harvard; NSF [IIS-0803409]; Korea
Astronomy and Space Science Institute
FX We thank M.-S. Shin, J. D. Hartman, P. J. Green, and R. Reid for
comments and helpful advice. The analysis in this paper has been done
using the Odyssey cluster supported by the FAS Research Computing Group
at Harvard. This work has been supported by NSF grant IIS-0803409. This
research has made use of the SIMBAD database, operated at CDS,
Strasbourg, France. Y.-I. Byun acknowledges the support of the
KASI-Yonsei Joint Research for the Frontiers of Astronomy and Space
Science' program 2011 funded by Korea Astronomy and Space Science
Institute.
NR 107
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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 2011
VL 735
IS 2
AR 68
DI 10.1088/0004-637X/735/2/68
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700001
ER
PT J
AU Myers, PC
AF Myers, Philip C.
TI FILAMENTARY CONDENSATIONS IN A YOUNG CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; stars: formation
ID MAGNETIZED MOLECULAR CLOUDS; MASSIVE STAR-FORMATION; GOULD BELT SURVEY;
DENSE CORES; STELLAR CLUSTERS; LARGE-SCALE; GRAVITATIONAL COLLAPSE;
INITIAL CONDITIONS; SCUBA SURVEY; FRAGMENTATION
AB New models are presented for star-forming condensations in clusters. In each model, the condensation mass increases linearly with radius on small scales, and more rapidly on large scales, as in "thermal-nonthermal" models. Spherical condensations with this structure form protostars which match the initial mass function if their infall is subject to equally likely stopping. However, such spherical models do not match the filamentary nature of cluster gas, and they are too extended to form protostars having high mass and short spacing. Two hybrid models are presented, which are spherical on small scales and filamentary on large scales. In and around clusters, cores embedded in linear filaments match the elongation of cluster gas, and the central concentration of low-mass stars. In cluster centers, condensations require a low volume-filling factor to produce massive stars with short spacing. These may have stellate shape, where cores are nodes of filamentary networks, as seen in some simulations of colliding flows and collapsing turbulent clumps. A dense configuration of such stellate condensations may be indistinguishable from a clump forming multiple protostars via filamentary flow paths.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM pmyers@cfa.harvard.edu
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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 2011
VL 735
IS 2
AR 82
DI 10.1088/0004-637X/735/2/82
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700015
ER
PT J
AU Skillman, SW
Hallman, EJ
O'Shea, BW
Burns, JO
Smith, BD
Turk, MJ
AF Skillman, Samuel W.
Hallman, Eric J.
O'Shea, Brian W.
Burns, Jack O.
Smith, Britton D.
Turk, Matthew J.
TI GALAXY CLUSTER RADIO RELICS IN ADAPTIVE MESH REFINEMENT COSMOLOGICAL
SIMULATIONS: RELIC PROPERTIES AND SCALING RELATIONSHIPS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; cosmology: theory; hydrodynamics; methods: numerical;
radiation mechanisms: non-thermal
ID RADIATION MAGNETOHYDRODYNAMICS CODE; PIECEWISE PARABOLIC METHOD; N-BODY
SIMULATIONS; 2 SPACE DIMENSIONS; X-RAY-EMISSION; SHOCK-WAVES;
COSMIC-RAYS; DARK-MATTER; PARTICLE-ACCELERATION; ASTROPHYSICAL SHOCKS
AB Cosmological shocks are a critical part of large-scale structure formation, and are responsible for heating the intracluster medium in galaxy clusters. In addition, they are capable of accelerating non-thermal electrons and protons. In this work, we focus on the acceleration of electrons at shock fronts, which is thought to be responsible for radio relics-extended radio features in the vicinity of merging galaxy clusters. By combining high-resolution adaptive mesh refinement/N-body cosmological simulations with an accurate shock-finding algorithm and a model for electron acceleration, we calculate the expected synchrotron emission resulting from cosmological structure formation. We produce synthetic radio maps of a large sample of galaxy clusters and present luminosity functions and scaling relationships. With upcoming long-wavelength radio telescopes, we expect to see an abundance of radio emission associated with merger shocks in the intracluster medium. By producing observationally motivated statistics, we provide predictions that can be compared with observations to further improve our understanding of magnetic fields and electron shock acceleration.
C1 [Skillman, Samuel W.; Hallman, Eric J.; Burns, Jack O.; Smith, Britton D.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Hallman, Eric J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[O'Shea, Brian W.; Smith, Britton D.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA.
[O'Shea, Brian W.] Michigan State Univ, Lyman Briggs Coll, E Lansing, MI 48824 USA.
[O'Shea, Brian W.] Michigan State Univ, Inst Cyber Enabled Res, E Lansing, MI 48824 USA.
[Burns, Jack O.] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94035 USA.
[Turk, Matthew J.] Columbia Univ, Dept Astron, New York, NY 10025 USA.
RP Skillman, SW (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
EM samuel.skillman@colorado.edu
FU US National Science Foundation [AST-0807215]; DOE [DE-FG02-97ER25308];
NASA [NNX09AD80G, NNZ07-AG77G]; NSF AAPF [AST 07-02923]; NSF
[AST0707474]
FX S. W. S. thanks Matthias Hoeft and Marcus Bruggen for making their radio
emission model available. S. W. S. and B.W.O. thank Megan Donahue and
Mark Voit for useful conversations and comments. We also thank an
anonymous referee for very helpful comments and suggestions. Computing
time was provided by NRAC allocations TG-AST090040 and TG-AST090095. S.
W. S., E.J.H., and J.O.B. have been supported in part by a grant from
the US National Science Foundation (AST-0807215). S. W. S. has been
supported by a DOE Computational Science Graduate Fellowship under grant
number DE-FG02-97ER25308. B.W.O. has been supported in part by a grant
from the NASA ATFP program (NNX09AD80G). E.J.H. also acknowledges
support from NSF AAPF AST 07-02923. B. D. S. has been supported by NASA
grant NNZ07-AG77G and NSF AST0707474. Computations described in this
work were performed using the Enzo code developed by the Laboratory for
Computational Astrophysics at the University of California in San Diego
(http://lca.ucsd.edu) and by a community of independent developers from
numerous other institutions. The yt analysis toolkit was developed
primarily by Matthew Turk with contributions from many other developers,
to whom we are very grateful. The LUNAR Consortium
(http://lunar.colorado.edu), headquartered at the University of
Colorado, is funded by the NASA Lunar Science Institute (via cooperative
Agreement NNA09DB30A). The authors acknowledge the Texas Advanced
Computing Center (TACC) at The University of Texas at Austin for
providing HPC resources that have contributed to the research results
reported within this paper. URL:http://www.tacc.utexas.edu. Some
computations were also performed on Kraken (a Cray XT5) at the National
Institute for Computational Sciences (http://www.nics.tennessee.edu/).
NR 62
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PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 96
DI 10.1088/0004-637X/735/2/96
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700029
ER
PT J
AU Volk, K
Hrivnak, BJ
Matsuura, M
Bernard-Salas, J
Szczerba, R
Sloan, GC
Kraemer, KE
van Loon, JT
Kemper, F
Woods, PM
Zijlstra, AA
Sahai, R
Meixner, M
Gordon, KD
Gruendl, RA
Tielens, AGGM
Indebetouw, R
Marengo, M
AF Volk, Kevin
Hrivnak, Bruce J.
Matsuura, Mikako
Bernard-Salas, Jeronimo
Szczerba, Ryszard
Sloan, G. C.
Kraemer, Kathleen E.
van Loon, Jacco Th.
Kemper, F.
Woods, Paul M.
Zijlstra, Albert A.
Sahai, Raghvendra
Meixner, Margaret
Gordon, Karl D.
Gruendl, Robert A.
Tielens, Alexander G. G. M.
Indebetouw, Remy
Marengo, Massimo
TI DISCOVERY AND ANALYSIS OF 21 mu m FEATURE SOURCES IN THE MAGELLANIC
CLOUDS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; galaxies: individual (LMC, SMC); stars: AGB and
post-AGB; stars: evolution
ID GIANT BRANCH STARS; RICH PROTOPLANETARY NEBULAE;
SPITZER-SPACE-TELESCOPE; POST-AGB STARS; M EMISSION FEATURE;
PLANETARY-NEBULAE; INFRARED SPECTROGRAPH; EVOLVED STARS; MAGNESIUM
SULFIDE; LEGACY PROGRAM
AB Spitzer Space Telescope mid-infrared spectroscopy has been obtained for 15 carbon-rich protoplanetary nebulae (PPNe) in the Large Magellanic Cloud (LMC) and for two other such stars in the Small Magellanic Cloud (SMC). Of these 17 PPNe, the unidentified 21 mu m feature is strong in 7 spectra, weak in 2 spectra, and very weak or questionable in 4 spectra. Two of the four spectra without the 21 mu m feature have a very strong feature near 11 mu m, similar to a feature observed in some carbon-rich planetary nebulae (PNe) in the LMC. We attribute this feature to unusual SiC dust, although the feature-to-continuum ratio is much larger than for SiC features in Galactic or Magellanic Cloud carbon star spectra. The remaining two objects show typical carbon-rich PPNe spectra with no 21 mu m features. One of the LMC objects that lacks the 21 mu m feature and one SMC object with a questionable 21 mu m detection may have mixed dust chemistries based upon their spectral similarity to Galactic [WC] PNe. The 13 objects that either definitely or may show the 21 mu m feature have distinct dust shell properties compared to the Galactic 21 mu m objects-the 21 mu m features are weaker, the estimated dust temperatures are significantly higher, the unidentified infrared (UIR) bands are stronger, and the UIRs show more structure. Four of the 21 mu m objects appear to show normal SiC emission features in their spectra. Many of the PPNe show strong 30 mu m features, although this feature carries less of the total mid-infrared emission than is normally the case for the Galactic 21 mu m PPNe. The LMC objects are in the LMC halo rather than in the LMC bar. The estimated luminosities of these PPNe vary from 4700 to 12,500L(circle dot).
C1 [Volk, Kevin; Meixner, Margaret; Gordon, Karl D.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Hrivnak, Bruce J.] Valparaiso Univ, Dept Phys & Astron, Valparaiso, IN 46383 USA.
[Hrivnak, Bruce J.] UCL, Inst Origins, Dept Phys & Astron, London WC1E 6BT, England.
[Bernard-Salas, Jeronimo] Univ Paris 11, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France.
[Szczerba, Ryszard] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland.
[Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[Kraemer, Kathleen E.] USAF, Res Lab, RVBYB, Hanscom AFB, MA 01731 USA.
[van Loon, Jacco Th.] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England.
[Kemper, F.; Woods, Paul M.; Zijlstra, Albert A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England.
[Sahai, Raghvendra] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Gruendl, Robert A.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Tielens, Alexander G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands.
[Indebetouw, Remy] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Marengo, Massimo] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
[Matsuura, Mikako] Univ Coll London, Mullard Space Sci Lab, Inst Origins, Dorking RH5 6NT, Surrey, England.
[Kemper, F.] Acad Sinica, Inst Astron & Astrophys, Taipei 10647, Taiwan.
[Indebetouw, Remy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Marengo, Massimo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Volk, K (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
EM volk@stsci.edu
RI Kemper, Francisca/D-8688-2011
OI Kemper, Francisca/0000-0003-2743-8240
FU NASA [1378453]; Polish MNiSW [N203 511838]
FX This work is primarily 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 research was provided by NASA through contract 1378453 issued
by JPL/Caltech. R.Sz. acknowledges support by grant N203 511838 from the
Polish MNiSW.
NR 84
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 127
DI 10.1088/0004-637X/735/2/127
PG 28
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700060
ER
PT J
AU Whitaker, KE
Labbe, I
van Dokkum, PG
Brammer, G
Kriek, M
Marchesini, D
Quadri, RF
Franx, M
Muzzin, A
Williams, RJ
Bezanson, R
Illingworth, GD
Lee, KS
Lundgren, B
Nelson, EJ
Rudnick, G
Tal, T
Wake, DA
AF Whitaker, Katherine E.
Labbe, Ivo
van Dokkum, Pieter G.
Brammer, Gabriel
Kriek, Mariska
Marchesini, Danilo
Quadri, Ryan F.
Franx, Marijn
Muzzin, Adam
Williams, Rik J.
Bezanson, Rachel
Illingworth, Garth D.
Lee, Kyoung-Soo
Lundgren, Britt
Nelson, Erica J.
Rudnick, Gregory
Tal, Tomer
Wake, David A.
TI THE NEWFIRM MEDIUM-BAND SURVEY: PHOTOMETRIC CATALOGS, REDSHIFTS, AND THE
BIMODAL COLOR DISTRIBUTION OF GALAXIES OUT TO z similar to 3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies: distances and redshifts; galaxies: high-redshift;
surveys
ID LYMAN-BREAK GALAXIES; DEEP-FIELD-SOUTH; INFRARED SPECTROSCOPIC SURVEY;
STAR-FORMATION HISTORIES; COSMIC EVOLUTION SURVEY; STELLAR MASS
FUNCTION; K-SELECTED GALAXIES; YALE-CHILE MUSYC; POPULATION SYNTHESIS;
MULTIWAVELENGTH SURVEY
AB We present deep near-IR (NIR) medium-bandwidth photometry over the wavelength range 1-1.8 mu m in the All-wavelength Extended Groth strip International Survey (AEGIS) and Cosmic Evolution Survey (COSMOS) fields. The observations were carried out using the NOAO Extremely Wide-Field Infrared Imager (NEWFIRM) on the Mayall 4 m Telescope on Kitt Peak as part of the NEWFIRM Medium-Band Survey (NMBS), an NOAO survey program. In this paper, we describe the full details of the observations, data reduction, and photometry for the survey. We also present a public K-selected photometric catalog, along with accurate photometric redshifts. The redshifts are computed with 37 (20) filters in the COSMOS (AEGIS) fields, combining the NIR medium-bandwidth data with existing UV (Galaxy Evolution Explorer), visible and NIR (Canada-France-Hawaii Telescope and Subaru Telescope), and mid-IR (Spitzer/IRAC) imaging. We find excellent agreement with publicly available spectroscopic redshifts, with sigma(z)/(1 + z) similar to 1%-2% for similar to 4000 galaxies at z = 0-3. The NMBS catalogs contain similar to 13,000 galaxies at z > 1.5 with accurate photometric redshifts and rest-frame colors. Due to the increased spectral resolution obtained with the five NIR medium-band filters, the median 68% confidence intervals of the photometric redshifts of both quiescent and star-forming galaxies are a factor of about two times smaller when comparing catalogs with medium-band NIR photometry to NIR broadband photometry. We show evidence for a clear bimodal color distribution between quiescent and star-forming galaxies that persists to z similar to 3, a higher redshift than has been probed so far.
C1 [Whitaker, Katherine E.; van Dokkum, Pieter G.; Brammer, Gabriel; Muzzin, Adam; Bezanson, Rachel; Lee, Kyoung-Soo; Lundgren, Britt; Nelson, Erica J.; Tal, Tomer; Wake, David A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Labbe, Ivo; Williams, Rik J.] Carnegie Observ, Pasadena, CA 91101 USA.
[Brammer, Gabriel] European So Observ, Santiago 19, Chile.
[Kriek, Mariska] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kriek, Mariska] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Marchesini, Danilo] Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
[Quadri, Ryan F.; Franx, Marijn] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
[Illingworth, Garth D.] UCO Lick Observ, Pasadena, CA 91101 USA.
[Rudnick, Gregory] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA.
RP Whitaker, KE (reprint author), Yale Univ, Dept Astron, New Haven, CT 06511 USA.
EM katherine.whitaker@yale.edu
FU NSF [AST-0807974]; NASA [NNX11AB08G]; STFC
FX We thank the anonymous referee for useful comments and a careful reading
of the paper. This paper is based partly on observations obtained with
MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, and WIRCam, a
joint project of CFHT, Taiwan, Korea, Canada, and France at the CFHT,
which is operated by the National Research Council (NRC) of Canada, the
Institut National des Science de l'Univers of the Centre National de la
Recherche Scientifique (CNRS) of France, and the University of Hawaii.
This work is based in part on data products produced at TERAPIX, the
WIRDS consortium, and the Canadian Astronomy Data Centre. We thank H.
Hildebrandt for providing the CARS-reduced CFHTLS images. This study
also makes use of data from AEGIS, a multiwavelength sky survey
conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru,
Palomar, Spitzer, VLA, and other telescopes and supported in part by the
NSF, NASA, and the STFC. Support from NSF grant AST-0807974 and NASA
grant NNX11AB08G is gratefully acknowledged.
NR 73
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 86
DI 10.1088/0004-637X/735/2/86
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700019
ER
PT J
AU Winter, HD
Martens, P
Reeves, KK
AF Winter, Henry D.
Martens, Petrus
Reeves, Katharine K.
TI SIMULATING THE EFFECTS OF INITIAL PITCH-ANGLE DISTRIBUTIONS ON SOLAR
FLARES
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods: numerical; Sun: corona; Sun: flares
ID RECONNECTING CURRENT SHEETS; X-RAY-EMISSION; 2002 APRIL 15;
PARTICLE-ACCELERATION; STOCHASTIC ACCELERATION; ELECTRON ACCELERATION;
TRANSITION REGION; ATOMIC DATABASE; ENERGY-BALANCE; CORONAL LOOPS
AB In this work, we model both the thermal and non-thermal components of solar flares. The model we use, HyLoop, combines a hydrodynamic equation solver with a non-thermal particle tracking code to simulate the thermal and non-thermal dynamics and emission of solar flares. In order to test the effects of pitch-angle distribution on flare dynamics and emission, a series of flares is simulated with non-thermal electron beams injected at the loop apex. The pitch-angle distribution of each beam is described by a single parameter and allowed to vary from flare to flare. We use the results of these simulations to generate synthetic hard and soft X-ray emissions (HXR and SXR). The light curves of the flares in Hinode's X-ray Telescope passbands show a distinct signal that is highly dependent on pitch-angle distribution. The simulated HXR emission in the 3-6 keV bandpass shows the formation and evolution of emission sources that correspond well to the observations of pre-impulsive flares. This ability to test theoretical models of thermal and non-thermal flare dynamics directly with observations allows for the investigation of a wide range of physical processes governing the evolution of solar flares. We find that the initial pitch-angle distribution of non-thermal particle populations has a profound effect on loop top HXR and SXR emission and that apparent motion of HXR is a natural consequence of non-thermal particle evolution in a magnetic trap.
C1 [Winter, Henry D.; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martens, Petrus] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA.
RP Winter, HD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA.
EM hwinter@cfa.harvard.edu
RI Reeves, Katharine/P-9163-2014
FU NASA [NNX09AB18G-R, NAG5-12820, NNM07AA02C]
FX H.D.W. and P.M. are supported by NASA grant NNX09AB18G-R. The original
development of HyLoop was supported by NASA grant NAG5-12820. K.K.R. is
supported by NASA grant NNM07AA02C to the Smithsonian Astrophysical
Observatory. Hinode is a Japanese mission developed and launched by
ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as
international partners. It is operated by these agencies in cooperation
with ESA and the NSC (Norway). H. D. W. thanks Drs. David McKenzie, Dana
Longcope, Charles Kankelborg, and Kelly Korreck for lively, informative,
and stimulating conversations that greatly aided in the production of
this work. The original MSULoop model that the current model is based on
was constructed by Charles Kankelborg with additional work done by
Rebecca McMullen in partial fulfilment of her Master's degree.
NR 51
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2011
VL 735
IS 2
AR 103
DI 10.1088/0004-637X/735/2/103
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 783NF
UT WOS:000292089700036
ER
PT J
AU Tscherbul, TV
Zhang, P
Sadeghpour, HR
Dalgarno, A
AF Tscherbul, T. V.
Zhang, P.
Sadeghpour, H. R.
Dalgarno, A.
TI Anisotropic Hyperfine Interactions Limit the Efficiency of Spin-Exchange
Optical Pumping of He-3 Nuclei
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID BASIS-SETS; RB ATOMS; GAS; RELAXATION
AB We use accurate ab initio and quantum scattering calculations to demonstrate that the maximum He-3 spin polarization that can be achieved in spin-exchange collisions with potassium (K-39) and silver (Ag-107) atoms is limited by the anisotropic hyperfine interaction. We find that spin exchange in Ag-He collisions occurs much faster than in K-He collisions over a wide range of temperatures (10-600 K). Our analysis indicates that measurements of trap loss rates of S-2 atoms in the presence of cold He-3 gas may be used to probe anisotropic spin-dependent interactions in atom-He collisions.
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, ITAMP, 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 NSF; Smithsonian Astrophysical Observatory
FX We thank T.G. Walker for encouraging discussions. This work was
supported by NSF grants to the Harvard-MIT CUA and ITAMP at Harvard
University and the Smithsonian Astrophysical Observatory.
NR 30
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PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
EI 1079-7114
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD JUL 8
PY 2011
VL 107
IS 2
AR 023204
DI 10.1103/PhysRevLett.107.023204
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 789VB
UT WOS:000292544000003
PM 21797604
ER
PT J
AU Turrisi, GF
Smith, DR
AF Turrisi, Giuseppe Fabrizio
Smith, David R.
TI Systematic revision and phylogeny of the endemic southeastern Asian
Pristaulacus comptipennis species group (Hymenoptera: Aulacidae)
SO ZOOTAXA
LA English
DT Article
DE Evanioidea; new species; southeastern Asia; systematic revision;
phylogeny; biogeography
ID AULACUS JURINE; MORPHOLOGICAL ADAPTATIONS; WASPS HYMENOPTERA; KIEFFER;
EVANIOIDEA; AMERICA; CHINA; WOOD
AB The endemic southeastern Asiatic Pristaulacus comptipennis species group is revised and illustrated. Twenty species are recognized: P. asiaticus Turrisi & Smith, sp. nov. (China), P. boninensis Konishi (Japan), P. comptipennis Enderlein (Japan, China, Taiwan, Laos), P. corellianus Turrisi & Smith, sp. nov. (Laos), P. dilleri Turrisi & Smith, sp. nov. (Laos), P. emarginaticeps Turner (Vietnam), P. excisus Turner (Vietnam), P. gusenleitneri Turrisi & Smith, sp. nov. (Thailand), P. insularis Konishi (Japan, South Korea), P. jenningsi Turrisi & Smith, sp. nov. (Laos), P. konishii Turrisi & Smith, sp. nov. (Thailand), P. lagrecai Turrisi & Smith, sp. nov. (Vietnam), P. nobilei Turrisi & Smith, sp. nov. (China), P. porcatus Sun & Sheng (China), P. sharkeyi Turrisi & Smith, sp. nov. (Thailand), P. thailandensis Turrisi & Smith, sp. nov. (Thailand), P. vietnamensis Turrisi & Smith, sp. nov. (Vietnam, Thailand), P. vilhelmseni Turrisi & Smith, sp. nov. (Laos), P. vivaldianus Turrisi & Smith, sp. nov. (Laos), P. watanabei Turrisi & Smith, sp. nov. (Thailand). Phylogenetic analyses are based on a previous set of 79 morphological characters. Of this data set, 28 informative including five newly added characters were analysed using TNT under different schemes (equal and implied weighting). All analyses support two large clades, the first with five species, and a more derived and diverse one containing 15 species. Other minor clades are identified and discussed. A key for identification of the species is provided.
C1 [Turrisi, Giuseppe Fabrizio] Univ Catania, CUTGANA, I-95027 Catania, Italy.
[Smith, David R.] Smithsonian Inst, Natl Museum Amer Hist, Systemat Entomol Lab, PSI,ARS,USDA, Washington, DC 20013 USA.
RP Turrisi, GF (reprint author), Univ Catania, CUTGANA, Via Terzora 8, I-95027 Catania, Italy.
EM turrisifabrizio@yahoo.it; dave.smith@ars.usda.gov
FU NSF [DEB-0542864]; European Commission [GB-TAF 390]
FX The Willi Hennig Society is kindly acknowledged for access to TNT
software. We also kindly thank Lars Vilhelmsen (Zoological Museum,
Copenhagen) for useful advice on TNT use. We are grateful to the
curators of Museums for providing us material for study, and especially
to Michael Sharkey (University of Kentucky, U. S. A.), for allowing
study of the material obtained through the "TIGER" project (Thailand
Inventory Group for Entomological Research), NSF Grant Number:
DEB-0542864. We are also grateful to Arkady Lelej (Russian Academy of
Sciences, Vladivostok, Russia) as subject editor, John Jennings
(University of Adelaide, Australia), Andrew Deans (North Carolina State
University, U. S. A.), and John Brown and Thomas Henry (Systematic
Entomology Laboratory, USDA, Washington, D. C., U. S. A.) as reviewers
for useful comments and criticisms on this paper. The senior author is
grateful to Suzanne Ryder and Gavin Broad for their assistance during
the revision of the Aulacidae stored in the Natural History Museum
(London) through the grant obtained under the European Commission's (FP
6) Integrated Infrastructure Initiative Programme Synthesys (GB-TAF
390). USDA is an equal opportunity provider and employer.
NR 55
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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 8
PY 2011
IS 2959
BP 1
EP 72
PG 72
WC Zoology
SC Zoology
GA 789HV
UT WOS:000292507200001
ER
PT J
AU Britz, R
Johnson, GD
AF Britz, Ralf
Johnson, G. David
TI Comments on the establishment of the one to one relationship between
characters as a prerequisite for homology assessment in phylogenetic
studies
SO ZOOTAXA
LA English
DT Editorial Material
ID MULTIPLE MOLECULAR PHYLOGENIES; OTOPHYSAN OSTARIOPHYSI; TELEOSTEI;
ONTOGENY; FISHES; CYPRINIFORMES; SYSTEMATICS; POSITION; CLADES; ARCH
C1 [Britz, Ralf] Nat Hist Museum, Dept Zool, London SW7 5BD, England.
[Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA.
RP Britz, R (reprint author), Nat Hist Museum, Dept Zool, Cromwell Rd, London SW7 5BD, England.
EM R.Britz@nhm.ac.uk; JOHN-SOND@si.edu
NR 49
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 JUL 8
PY 2011
IS 2946
SI SI
BP 65
EP 72
PG 8
WC Zoology
SC Zoology
GA 789GM
UT WOS:000292503300012
ER
PT J
AU Simberloff, D
Alexander, J
Allendorf, F
Aronson, J
Antunes, PM
Bacher, S
Bardgett, R
Bertolino, S
Bishop, M
Blackburn, TM
Blakeslee, A
Blumenthal, D
Bortolus, A
Buckley, R
Buckley, Y
Byers, J
Callaway, RM
Campbell, F
Campbell, K
Campbell, M
Carlton, JT
Cassey, P
Catford, J
Celesti-Grapow, L
Chapman, J
Clark, P
Clewell, A
Clode, JC
Chang, A
Chytry, M
Clout, M
Cohen, A
Cowan, P
Cowie, RH
Crall, AW
Crooks, J
Deveney, M
Dixon, K
Dobbs, FC
Duffy, DC
Duncan, R
Ehrlich, PR
Eldredge, L
Evenhuis, N
Fausch, KD
Feldhaar, H
Firn, J
Fowler, A
Galil, B
Garcia-Berthou, E
Geller, J
Genovesi, P
Gerber, E
Gherardi, F
Gollasch, S
Gordon, D
Graham, J
Gribben, P
Griffen, B
Grosholz, ED
Hewitt, C
Hierro, JL
Hulme, P
Hutchings, P
Jarosik, V
Jeschke, JM
Johnson, C
Johnson, L
Johnston, EL
Jones, CG
Keller, R
King, CM
Knols, BGJ
Kollmann, J
Kompas, T
Kotanen, PM
Kowarik, I
Kuhn, I
Kumschick, S
Leung, B
Liebhold, A
MacIsaac, H
Mack, R
McCullough, DG
McDonald, R
Merritt, DM
Meyerson, L
Minchin, D
Mooney, HA
Morisette, JT
Moyle, P
Heinz, MS
Murray, BR
Nehring, S
Nelson, W
Nentwig, W
Novak, SJ
Occhipinti, A
Ojaveer, H
Osborne, B
Ostfeld, RS
Parker, J
Pederson, J
Pergl, J
Phillips, ML
Pysek, P
Rejmanek, M
Ricciardi, A
Ricotta, C
Richardson, D
Rilov, G
Ritchie, E
Robertson, PA
Roman, J
Ruiz, G
Schaefer, H
Schaffelke, B
Schierenbeck, KA
Schmitz, DC
Schwindt, E
Seeb, J
Smith, LD
Smith, GF
Stohlgren, T
Strayer, DL
Strong, D
Sutherland, WJ
Therriault, T
Thuiller, W
Torchin, M
van der Putten, WH
Vila, M
Von Holle, B
Wallentinus, I
Wardle, D
Williamson, M
Wilson, J
Winter, M
Wolfe, LM
Wright, J
Wonham, M
Zabin, C
AF Simberloff, Daniel
Alexander, Jake
Allendorf, Fred
Aronson, James
Antunes, Pedro M.
Bacher, Sven
Bardgett, Richard
Bertolino, Sandro
Bishop, Melanie
Blackburn, Tim M.
Blakeslee, April
Blumenthal, Dana
Bortolus, Alejandro
Buckley, Ralf
Buckley, Yvonne
Byers, Jeb
Callaway, Ragan M.
Campbell, Faith
Campbell, Karl
Campbell, Marnie
Carlton, James T.
Cassey, Phillip
Catford, Jane
Celesti-Grapow, Laura
Chapman, John
Clark, Paul
Clewell, Andre
Clode, Joao Canning
Chang, Andrew
Chytry, Milan
Clout, Mick
Cohen, Andrew
Cowan, Phil
Cowie, Robert H.
Crall, Alycia W.
Crooks, Jeff
Deveney, Marty
Dixon, Kingsley
Dobbs, Fred C.
Duffy, David Cameron
Duncan, Richard
Ehrlich, Paul R.
Eldredge, Lucius
Evenhuis, Neal
Fausch, Kurt D.
Feldhaar, Heike
Firn, Jennifer
Fowler, Amy
Galil, Bella
Garcia-Berthou, Emili
Geller, Jonathan
Genovesi, Piero
Gerber, Esther
Gherardi, Francesca
Gollasch, Stephan
Gordon, Doria
Graham, Jim
Gribben, Paul
Griffen, Blaine
Grosholz, Edwin D.
Hewitt, Chad
Hierro, Jose L.
Hulme, Philip
Hutchings, Pat
Jarosik, Vojtech
Jeschke, Jonathan M.
Johnson, Chris
Johnson, Ladd
Johnston, Emma L.
Jones, Carl G.
Keller, Reuben
King, Carolyn M.
Knols, Bart G. J.
Kollmann, Johannes
Kompas, Thomas
Kotanen, Peter M.
Kowarik, Ingo
Kuehn, Ingolf
Kumschick, Sabrina
Leung, Brian
Liebhold, Andrew
MacIsaac, Hugh
Mack, Richard
McCullough, Deborah G.
McDonald, Robbie
Merritt, David M.
Meyerson, Laura
Minchin, Dan
Mooney, Harold A.
Morisette, Jeffrey T.
Moyle, Peter
Heinz, Mueller-Schaerer
Murray, Brad R.
Nehring, Stefan
Nelson, Wendy
Nentwig, Wolfgang
Novak, Stephen J.
Occhipinti, Anna
Ojaveer, Henn
Osborne, Bruce
Ostfeld, Richard S.
Parker, John
Pederson, Judith
Pergl, Jan
Phillips, Megan L.
Pysek, Petr
Rejmanek, Marcel
Ricciardi, Anthony
Ricotta, Carlo
Richardson, David
Rilov, Gil
Ritchie, Euan
Robertson, Peter A.
Roman, Joe
Ruiz, Gregory
Schaefer, Hanno
Schaffelke, Britta
Schierenbeck, Kristina A.
Schmitz, Don C.
Schwindt, Evangelina
Seeb, Jim
Smith, L. David
Smith, Gideon F.
Stohlgren, Thomas
Strayer, David L.
Strong, Donald
Sutherland, William J.
Therriault, Thomas
Thuiller, Wilfried
Torchin, Mark
van der Putten, Wim H.
Vila, Montserrat
Von Holle, Betsy
Wallentinus, Inger
Wardle, David
Williamson, Mark
Wilson, John
Winter, Marten
Wolfe, Lorne M.
Wright, Jeff
Wonham, Marjorie
Zabin, Chela
CA 141 Signatories
TI Non-natives: 141 scientists object
SO NATURE
LA English
DT Letter
C1 [Simberloff, Daniel] Univ Tennessee, Knoxville, TN 37996 USA.
[Alexander, Jake] Inst Integrat Biol, Zurich, Switzerland.
[Allendorf, Fred; Callaway, Ragan M.] Univ Montana, Missoula, MT USA.
[Aronson, James] CEFE CNRS, Montpellier, France.
[Antunes, Pedro M.] Algoma Univ, Sault Ste Marie, ON, Canada.
[Bacher, Sven; Heinz, Mueller-Schaerer] Univ Fribourg, Fribourg, Switzerland.
[Bardgett, Richard] Univ Lancaster, Lancaster, England.
[Bertolino, Sandro] Univ Turin, Grugliasco, Italy.
[Bishop, Melanie] Macquarie Univ, Sydney, NSW, Australia.
[Blackburn, Tim M.] Zool Soc London, London, England.
[Blakeslee, April; Clode, Joao Canning; Chang, Andrew; Fowler, Amy; Griffen, Blaine; Parker, John; Ruiz, Gregory; Zabin, Chela] Smithsonian Environm Res Ctr, Edgewater, MD USA.
[Blumenthal, Dana] USDA Agr Res Service, Ft Collins, CO USA.
[Bortolus, Alejandro; Schwindt, Evangelina] Ctr Nacl Patagonico CONICET, Puerto Madryn, Argentina.
[Buckley, Ralf] Griffith Univ, Southport, Qld, Australia.
[Buckley, Yvonne] CSIRO Ecosyst Sci, St Lucia, Qld, Australia.
[Buckley, Yvonne] Univ Queensland, ARC Ctr Excellence Environm Decis, St Lucia, Qld, Australia.
[Byers, Jeb] Univ Georgia, Athens, GA USA.
[Campbell, Faith] Nature Conservancy, Arlington, VA USA.
[Campbell, Karl] Island Conservat, Santa Cruz, CA USA.
[Campbell, Marnie; Hewitt, Chad] Cent Queensland Univ, Rockhampton, Qld 4702, Australia.
[Carlton, James T.] Williams Coll Mystic Seaport, Mystic, CT USA.
[Cassey, Phillip] Univ Adelaide, Adelaide, SA, Australia.
[Catford, Jane] Univ Melbourne, Melbourne, Vic, Australia.
[Celesti-Grapow, Laura; Ricotta, Carlo] Univ Roma La Sapienza, Rome, Italy.
[Chapman, John] Oregon State Univ, Hatfield Marine Sci Ctr, Newport, OR USA.
[Clark, Paul] Nat Hist Museum, London, England.
[Clewell, Andre] Tall Timbers Res Stn, Tallahassee, FL USA.
[Chytry, Milan] Masaryk Univ, Brno, Czech Republic.
[Clout, Mick] Univ Auckland, Auckland, New Zealand.
[Cohen, Andrew] Ctr Res Aquat Bioinvas, Richmond, CA USA.
[Cowan, Phil] Landcare Res, Palmerston North, New Zealand.
[Cowie, Robert H.; Duffy, David Cameron] Univ Hawaii, Honolulu, HI USA.
[Crall, Alycia W.; Fausch, Kurt D.; Graham, Jim; Kumschick, Sabrina; Stohlgren, Thomas] Colorado State Univ, Ft Collins, CO USA.
[Crooks, Jeff] Tijuana River Natl Estuarine Res Reserve, Imperial Beach, CA USA.
[Deveney, Marty] S Australian Aquat Sci Ctr, West Beach, Australia.
[Dixon, Kingsley] Kings Pk & Bot Gardens, Perth, WA 6005, Australia.
[Dobbs, Fred C.] Old Domin Univ, Norfolk, VA USA.
[Duncan, Richard; Hulme, Philip] Lincoln Univ, Lincoln, New Zealand.
[Ehrlich, Paul R.; Mooney, Harold A.] Stanford Univ, Stanford, CA USA.
[Eldredge, Lucius; Evenhuis, Neal] Bernice P Bishop Museum, Honolulu, HI USA.
[Feldhaar, Heike] Univ Osnabruck, Osnabruck, Germany.
[Firn, Jennifer] Queensland Univ Technol, Brisbane, Qld, Australia.
[Galil, Bella] Natl Inst Oceanog, Haifa, Israel.
[Garcia-Berthou, Emili] Univ Girona, Girona, Spain.
[Geller, Jonathan] Moss Landing Marine Labs, Moss Landing, CA USA.
[Genovesi, Piero] Italian Natl Inst Environm Protect & Res, Rome, Italy.
[Gerber, Esther] CABI Europe, Delemont, Switzerland.
[Gherardi, Francesca] Univ Florence, Florence, Italy.
[Gordon, Doria] Univ Florida, Gainesville, FL USA.
[Gribben, Paul; Murray, Brad R.; Phillips, Megan L.] Univ Technol Sydney, Sydney, NSW, Australia.
[Grosholz, Edwin D.; Moyle, Peter; Rejmanek, Marcel; Strong, Donald] Univ Calif Davis, Davis, CA USA.
[Hierro, Jose L.] Univ Nacl La Pampa, CONICET, La Pampa, Argentina.
[Hutchings, Pat] Australian Museum, Sydney, NSW, Australia.
[Jarosik, Vojtech] Charles Univ Prague, Prague, Czech Republic.
[Johnson, Chris] Univ Tasmania, Hobart, Tas, Australia.
[Johnson, Ladd] Univ Laval, Quebec City, PQ, Canada.
[Johnston, Emma L.] Univ New S Wales, Sydney, NSW, Australia.
[Jones, Carl G.] Durrell Wildlife Conservat Trust, Trinity, Jersey, England.
[Keller, Reuben] Univ Chicago, Chicago, IL USA.
[King, Carolyn M.] Univ Waikato, Hamilton, New Zealand.
[Knols, Bart G. J.] Acad Med Ctr, Amsterdam, Netherlands.
[Knols, Bart G. J.] K&S Consulting, Dodewaard, Netherlands.
[Jeschke, Jonathan M.; Kollmann, Johannes] Tech Univ Munich, Freising Weihenstephan, Germany.
[Kompas, Thomas] Australian Natl Univ, Canberra, ACT, Australia.
[Kotanen, Peter M.] Univ Toronto Mississauga, Mississauga, ON, Canada.
[Kowarik, Ingo] Tech Univ Berlin, Berlin, Germany.
[Kuehn, Ingolf; Winter, Marten] UFZ Helmholtz Ctr Environm Res, Halle, Germany.
[Leung, Brian; Ricciardi, Anthony] McGill Univ, Montreal, PQ, Canada.
[Liebhold, Andrew] USDA Forest Serv, Morgantown, WV USA.
[MacIsaac, Hugh] Univ Windsor, Windsor, ON, Canada.
[Mack, Richard] Washington State Univ, Pullman, WA USA.
[McCullough, Deborah G.] Michigan State Univ, E Lansing, MI USA.
[McDonald, Robbie] Food & Environm Res Agcy, Dept Environm Food & Rural Affairs, Stonehouse, England.
[Merritt, David M.] US Forest Serv, Ft Collins, CO USA.
[Meyerson, Laura] Univ Rhode Island, Kingston, RI USA.
[Minchin, Dan] Marine Organism Investigat, Killaloe, Ireland.
[Morisette, Jeffrey T.] US Geol Survey, Ft Collins Sci Ctr, Ft Collins, CO USA.
[Nehring, Stefan] Bundesamt Naturschutz, Bonn, Germany.
[Nelson, Wendy] Natl Inst Water & Atmospher Res, Wellington, New Zealand.
[Nentwig, Wolfgang] Univ Bern, Bern, Switzerland.
[Novak, Stephen J.] Boise State Univ, Boise, ID USA.
[Occhipinti, Anna] Univ Pavia, Pavia, Italy.
[Ojaveer, Henn] Univ Tartu, Parnu, Estonia.
[Osborne, Bruce] Univ Coll Dublin, Dublin, Ireland.
[Ostfeld, Richard S.; Strayer, David L.] Cary Inst Ecosyst Studies, Millbrook, NY USA.
[Pergl, Jan; Pysek, Petr] Acad Sci Czech Republic, Pruhonice, Czech Republic.
[Richardson, David; Wilson, John] Stellenbosch Univ, Matieland, South Africa.
[Rilov, Gil] Natl Inst Oceanog, Haifa, Israel.
[Ritchie, Euan] Deakin Univ, Burwood, Vic, Australia.
[Robertson, Peter A.] Food & Environm Res Agcy, York, N Yorkshire, England.
[Roman, Joe] Univ Vermont, Burlington, VT USA.
[Schaefer, Hanno] Harvard Univ, Cambridge, MA USA.
[Schaffelke, Britta] Australian Inst Marine Sci, Townsville, Qld, Australia.
[Schierenbeck, Kristina A.] Calif State Univ, Chico, CA USA.
[Schmitz, Don C.] Florida Fish & Wildlife Conservat Commiss, Tallahassee, FL USA.
[Seeb, Jim] Univ Washington, Seattle, WA USA.
[Smith, L. David] Smith Coll, Northampton, MA USA.
[Smith, Gideon F.] Univ Pretoria, Pretoria, South Africa.
[Sutherland, William J.] Univ Cambridge, Cambridge, England.
[Therriault, Thomas] Pacific Biol Stn, Nanaimo, BC, Canada.
[Thuiller, Wilfried] Univ Grenoble 1, Grenoble, France.
[Torchin, Mark] Smithsonian Trop Res Inst, Balboa, Panama.
[van der Putten, Wim H.] Netherlands Inst Ecol, Wageningen, Netherlands.
[Vila, Montserrat] Estac Biol Donana, Seville, Spain.
[Von Holle, Betsy] Univ Cent Florida, Orlando, FL USA.
[Wallentinus, Inger] Univ Gothenburg, Gothenburg, Sweden.
[Wardle, David] Swedish Univ Agr Sci, Umea, Sweden.
[Williamson, Mark] Univ York, York, N Yorkshire, England.
[Wolfe, Lorne M.] Georgia So Univ, Statesboro, GA USA.
[Wright, Jeff] Univ Tasmania, Launceston, Australia.
[Wonham, Marjorie] Quest Univ, Squamish, BC, Canada.
RP Simberloff, D (reprint author), Univ Tennessee, Knoxville, TN 37996 USA.
EM dsimberloff@utk.edu
RI Richardson, David/A-1495-2008; Wardle, David/F-6031-2011; Antunes,
Pedro/C-2949-2008; THUILLER, Wilfried/G-3283-2010; Nentwig,
Wolfgang/A-6624-2011; McDonald, Robbie/A-2931-2012; Wilson,
John/B-4101-2008; Jeschke, Jonathan/A-2707-2008; Pysek,
Petr/B-1957-2012; Liebhold, Andrew/C-1423-2008; van der Putten,
Wim/C-3707-2011; Garcia-Berthou, Emili/A-5392-2008; Canning Clode,
Joao/G-5142-2011; Hulme, Philip/F-7454-2011; Blumenthal,
Dana/J-3106-2012; Meyerson, Laura/K-9013-2012; Fausch, Kurt/A-8849-2010;
Sutherland, William/B-1291-2013; Buckley, Yvonne/B-1281-2008; Duncan,
Richard/E-7899-2013; Robertson, Peter/H-1614-2013; Meyerson,
Laura/D-4487-2013; Hewitt, Chad/C-4460-2008; Strayer, David/H-3788-2011;
Catford, Jane/B-9578-2012; Pergl, Jan/H-1071-2011; Johnston,
Emma/B-7210-2009; Mueller-Schaerer, Heinz/H-5277-2011; Bacher,
Sven/F-5431-2010; Ricciardi, Anthony/A-8536-2010; Vila,
Montserrat/D-9339-2013; Winter, Marten/E-7979-2011; Kollmann,
Johannes/B-4255-2012; CSIC, EBD Donana/C-4157-2011; Chang,
Andrew/J-8058-2016; Ojaveer, Henn/K-2160-2016; Chytry,
Milan/J-4954-2012; Celesti, Laura/R-3615-2016; Kuhn, Ingolf /B-9756-2009
OI Richardson, David/0000-0001-9574-8297; Wardle,
David/0000-0002-0476-7335; THUILLER, Wilfried/0000-0002-5388-5274;
McDonald, Robbie/0000-0002-6922-3195; Wilson, John/0000-0003-0174-3239;
Liebhold, Andrew/0000-0001-7427-6534; van der Putten,
Wim/0000-0002-9341-4442; Garcia-Berthou, Emili/0000-0001-8412-741X;
Canning Clode, Joao/0000-0003-2143-6535; Hulme,
Philip/0000-0001-5712-0474; Buckley, Yvonne/0000-0001-7599-3201; Duncan,
Richard/0000-0003-2295-449X; Robertson, Peter/0000-0003-1567-8677;
Hewitt, Chad/0000-0002-6859-6512; Catford, Jane/0000-0003-0582-5960;
Pergl, Jan/0000-0002-0045-1974; Johnston, Emma/0000-0002-2117-366X;
Bacher, Sven/0000-0001-5147-7165; Vila, Montserrat/0000-0003-3171-8261;
Winter, Marten/0000-0002-9593-7300; Kollmann,
Johannes/0000-0002-4990-3636; CSIC, EBD Donana/0000-0003-4318-6602;
Chang, Andrew/0000-0002-7870-285X; Ojaveer, Henn/0000-0003-2742-6063;
Chytry, Milan/0000-0002-8122-3075; Celesti, Laura/0000-0002-9533-6919;
Kuhn, Ingolf /0000-0003-1691-8249
NR 0
TC 74
Z9 76
U1 16
U2 444
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 7
PY 2011
VL 475
IS 7354
BP 36
EP 36
PG 1
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 788RE
UT WOS:000292461300028
PM 21734689
ER
PT J
AU Pyenson, ND
Lindberg, DR
AF Pyenson, Nicholas D.
Lindberg, David R.
TI What Happened to Gray Whales during the Pleistocene? The Ecological
Impact of Sea-Level Change on Benthic Feeding Areas in the North Pacific
Ocean
SO PLOS ONE
LA English
DT Article
ID SHIFTING BASE-LINE; ESCHRICHTIUS-ROBUSTUS; BERING-SEA; MARINE MAMMALS;
CHUKCHI SEAS; BRITISH-COLUMBIA; COMMUNITIES; SHELF; POPULATIONS;
CALIFORNIA
AB Background: Gray whales (Eschrichtius robustus) undertake long migrations, from Baja California to Alaska, to feed on seasonally productive benthos of the Bering and Chukchi seas. The invertebrates that form their primary prey are restricted to shallow water environments, but global sea-level changes during the Pleistocene eliminated or reduced this critical habitat multiple times. Because the fossil record of gray whales is coincident with the onset of Northern Hemisphere glaciation, gray whales survived these massive changes to their feeding habitat, but it is unclear how.
Methodology/Principal Findings: We reconstructed gray whale carrying capacity fluctuations during the past 120,000 years by quantifying gray whale feeding habitat availability using bathymetric data for the North Pacific Ocean, constrained by their maximum diving depth. We calculated carrying capacity based on modern estimates of metabolic demand, prey availability, and feeding duration; we also constrained our estimates to reflect current population size and account for glaciated and non-glaciated areas in the North Pacific. Our results show that key feeding areas eliminated by sea-level lowstands were not replaced by commensurate areas. Our reconstructions show that such reductions affected carrying capacity, and harmonic means of these fluctuations do not differ dramatically from genetic estimates of carrying capacity.
Conclusions/Significance: Assuming current carrying capacity estimates, Pleistocene glacial maxima may have created multiple, weak genetic bottlenecks, although the current temporal resolution of genetic datasets does not test for such signals. Our results do not, however, falsify molecular estimates of pre-whaling population size because those abundances would have been sufficient to survive the loss of major benthic feeding areas (i.e., the majority of the Bering Shelf) during glacial maxima. We propose that gray whales survived the disappearance of their primary feeding ground by employing generalist filter-feeding modes, similar to the resident gray whales found between northern Washington State and Vancouver Island.
C1 [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
[Pyenson, Nicholas D.] Univ Washington, Dept Mammal, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA.
[Pyenson, Nicholas D.] Univ Washington, Dept Paleontol, Burke Museum Nat Hist & Culture, Seattle, WA 98195 USA.
[Lindberg, David R.] Univ Calif Berkeley, Dept Integrat Biol, Ctr Computat Biol, Berkeley, CA 94720 USA.
[Lindberg, David R.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA.
RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA.
EM pyensonn@si.edu
RI Lindberg, David/D-8138-2011
FU Department of Integrative Biology; University of California Museum of
Paleontology at the University of California, Berkeley; National Science
Foundation; Natural Sciences and Engineering Research Council of Canada;
Smithsonian Institution; Biodiversity Synthesis Center at the Field
Museum, Chicago
FX This research was supported with funding from the Department of
Integrative Biology and the University of California Museum of
Paleontology at the University of California, Berkeley, to DRL. Funding
from a National Science Foundation Graduate Research Fellowship, a
Natural Sciences and Engineering Research Council of Canada postdoctoral
research fellowship and from the Smithsonian Institution supported NDP.
The funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.; For discussion
and constructive comments at various manuscript stages, we thank S. E.
Alter, P. K. Dayton, J. A. Estes, T. A. Demere, D. Jacobs, B. J. Le
Boeuf, S. R. Palumbi, M. Slatkin, and D. Strong. We sincerely appreciate
the perceptive and thorough comments from two anonymous reviewers, who
greatly improved the quality of this paper. We also thank B. Eakins for
assistance with the calculation of benthos area and E. B. Davis for help
with pilot analyses in the early stages of this project. This study also
benefited from valuable discussion at an Encyclopedia of Life synthesis
meeting on the evolution and diversity of marine tetrapods, funded by
the Biodiversity Synthesis Center at the Field Museum, Chicago, in 2009.
We also thank the conveners and participants of a symposium at the
Society of Vertebrate Paleontology's annual meeting on the physical
drivers and the evolution of marine tetrapods, in 2010. This paper is
University of California Museum of Paleontology contribution number
1982.
NR 115
TC 22
Z9 22
U1 3
U2 35
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUL 6
PY 2011
VL 6
IS 7
AR e21295
DI 10.1371/journal.pone.0021295
PG 14
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 791AK
UT WOS:000292632000008
PM 21754984
ER
PT J
AU Camera, S
Diaferio, A
Cardone, VF
AF Camera, Stefano
Diaferio, Antonaldo
Cardone, Vincenzo F.
TI Tomography from the next generation of cosmic shear experiments for
viable f(R) models
SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS
LA English
DT Article
DE modified gravity; power spectrum; cosmological parameters from LSS; weak
gravitational lensing
ID PROBE WMAP OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT
SUPERNOVAE; DARK ENERGY; COSMOLOGICAL PARAMETERS; POWER SPECTRUM;
MODIFIED GRAVITY; CURVATURE QUINTESSENCE; IA SUPERNOVAE; CONSTRAINTS
AB We present the cosmic shear signal predicted by two viable cosmological models in the framework of modified-action f(R) theories. We use f (R) models where the current accelerated expansion of the Universe is a direct consequence of the modified gravitational Lagrangian rather than Dark Energy (DE), either in the form of vacuum energy/cosmological constant or of a dynamical scalar field (e.g. quintessence). We choose Starobinsky's (St) and Hu & Sawicki's (HS) f(R) models, which are carefully designed to pass the Solar System gravity tests. In order to further support - or rule out - f(R) theories as alternative candidates to the DE hypothesis, we exploit the power of weak gravitational lensing, specifically of cosmic shear. We calculate the tomographic shear matrix as it would be measured by the upcoming ESA Cosmic Vision Euclid satellite. We find that in the St model the cosmic shear signal is almost completely degenerate with Lambda CDM but it is easily distinguishable in the HS model. Moreover, we compute the corresponding Fisher matrix for both the St and LIS models, thus obtaining forecasts for their cosmological parameters. Finally, we show that the Bayes factor for cosmic shear will definitely favour the HS model over Lambda CDM if Euclid measures a value larger than similar to 0.02 for the extra HS parameter n(HS).
C1 [Camera, Stefano; Diaferio, Antonaldo] Univ Turin, Dipartimento Fisiol Gen A Avogadro, I-10125 Turin, Italy.
[Camera, Stefano] Univ Turin, Dipartimento Fis Teor, I-10125 Turin, Italy.
[Camera, Stefano; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Cardone, Vincenzo F.] Osserv Astron Roma, Ist Nazl Astrofis INAF, I-00040 Monte Porzio Catone, Italy.
RP Camera, S (reprint author), Univ Turin, Dipartimento Fisiol Gen A Avogadro, Via P Giuria 1, I-10125 Turin, Italy.
EM camera@ph.unito.it; diaferio@ph.unito.it; winnyenodrac@gmail.com
RI Camera, Stefano/N-2456-2013
OI Camera, Stefano/0000-0003-3399-3574
FU INFN [PD51]; Minister dell'Istruzione, dell'Universita e della Ricerca
(MIUR); Universita degli Studi di Torino; Istituto Nazionale di Fisica
Nucleare (MIUR) [PRIN 2008NR3EBK]; Italian Space Agency
FX We thank the referee for providing very insightful comments. SC and AD
thank Bhuvnesh Jain for relevant suggestions on the use of cosmic shear
tomography. SC and AD gratefully acknowledge partial support from the
INFN grant PD51. SC acknowledges Research Grants funded jointly by
Minister dell'Istruzione, dell'Universita e della Ricerca (MIUR), by
Universita degli Studi di Torino and by Istituto Nazionale di Fisica
Nucleare within the Astroparticle Physics Project (MIUR contract number:
PRIN 2008NR3EBK). VFC is funded by Italian Space Agency. This research
has made use of NASA's Astrophysics Data System.
NR 90
TC 8
Z9 8
U1 0
U2 0
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 JUL
PY 2011
IS 7
AR 016
DI 10.1088/1475-7516/2011/07/016
PG 23
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 855CL
UT WOS:000297541000017
ER
PT J
AU Haggis, DC
Mook, MS
Fitzsimons, RD
Scarry, CM
Snyder, LM
AF Haggis, Donald C.
Mook, Margaret S.
Fitzsimons, Rodney D.
Scarry, C. Margaret
Snyder, Lynn M.
TI THE EXCAVATION OF ARCHAIC HOUSES AT AZORIA IN 2005-2006
SO HESPERIA
LA English
DT Article
ID ITANOS EASTERN CRETE; PART 1; COLLABORATION; DONE
AB This article reports on the excavation of Archaic houses (6th-early 5th century B.C.) in 2005 and 2006 at Azoria in eastern Crete. Five houses are discussed: four on the South Acropolis on the periphery of the civic center, and one on the North Acropolis. Well-preserved floor deposits provide evidence for room functions and permit a preliminary analysis of domestic space. The houses fill a lacuna in the published record of the 6th and early 5th centuries B.C. and contribute to our understanding of the form of Archaic houses in the Aegean and the integration of domestic space into an urban context.
C1 [Haggis, Donald C.] Univ N Carolina, Dept Class, Chapel Hill, NC 27599 USA.
[Mook, Margaret S.] Iowa State Univ, Class Studies Program Foreign Languages & Literat, Ames, IA 50011 USA.
[Fitzsimons, Rodney D.] Trent Univ, Dept Ancient Hist & Class, Peterborough, ON K9J 7B8, Canada.
[Scarry, C. Margaret] Univ N Carolina, Dept Anthropol, Chapel Hill, NC 27599 USA.
[Snyder, Lynn M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
RP Haggis, DC (reprint author), Univ N Carolina, Dept Class, 212 Murphey Hall,CB 3145, Chapel Hill, NC 27599 USA.
EM dchaggis@email.unc.edu; msmook@iastate.edu; rodneyfitzsimons@trentu.ca;
scarry@email.unc.edu; snyder.lynn@comcast.net
NR 45
TC 8
Z9 8
U1 0
U2 0
PU AMER SCHOOL CLASSICAL STUDIES AT ATHENS
PI PRINCETON
PA 6-8 CHARLTON STREET, PRINCETON, NJ 08540-5232 USA
SN 0018-098X
J9 HESPERIA
JI Hesperia
PD JUL-SEP
PY 2011
VL 80
IS 3
BP 431
EP 489
PG 59
WC Archaeology
SC Archaeology
GA 857IP
UT WOS:000297712000003
ER
PT J
AU Lasso-Alcala, O
Nunes, JLS
Lasso, C
Posada, J
Robertson, R
Piorski, NM
Van Tassell, J
Giarrizzo, T
Gondolo, G
AF Lasso-Alcala, Oscar
Nunes, Jorge L. S.
Lasso, Carlos
Posada, Juan
Robertson, Ross
Piorski, Nivaldo M.
Van Tassell, James
Giarrizzo, Tommaso
Gondolo, Guilherme
TI Invasion of the Indo-Pacific blenny Omobranchus punctatus (Perciformes:
Blenniidae) on the Atlantic Coast of Central and South America
SO NEOTROPICAL ICHTHYOLOGY
LA English
DT Article
DE Bio-invasions; Distributional data; Exotic marine fishes; New records
ID LIONFISH PTEROIS-VOLITANS; REEF FISHES; DISPERSAL; TELEOSTEI; PANAMA
AB We examined 308 specimens of the Indo-Pacific blenniid Omobranchus punctatus deposited in four museum collections, and analyzed data on their collection locations to assess its invasion on the Atlantic coast of Central and South America. This species occurs in shoreline estuarine and marine habitats in the Indo-West Pacific. Previous sampling and recent records in the Tropical West Atlantic from 1930 to 2004 produced 20 records for: Panama, Colombia, Venezuela, Trinidad and Brazil. In this work, we provide data on 17 new records for the Gulfs of Venezuela and Paria in Venezuela, as well as four records for Maranhao and Para states in NE Brazil. The temporal pattern of collections (1930 - 2009) and the proximity of most localities to ports and zones of ship traffic indicate that O. punctatus was initially introduced to the Atlantic by ships travelling from India to Trinidad. Within Brazil the introduction is linked to shipping connected to petroleum platforms. In Maranhao and Para the introduction may have occurred as a result of fish sheltering in fouling on hulls of ships moving between ports around the mouth of the Amazon River. Alternatively, the spread of this species along of the American coast may reflect the expansion of the range of O. puntactus through larval dispersal in northward flowing currents. We recommend monitoring of this introduced species, and studies of its ecology in West Atlantic areas.
C1 [Lasso-Alcala, Oscar] Fdn La Salle Ciencias Nat, Museo Hist Nat La Salle, Caracas 1010A, Venezuela.
[Nunes, Jorge L. S.] Univ Fed Maranhao, Lab Organismos Aquat, Ctr Ciencias Agr & Ambientais, Chapadinha, Maranhao, Brazil.
[Lasso, Carlos] Inst Alexander von Humboldt, Programa Biol Conservac & Uso Biodiversidad, Bogota, Colombia.
[Posada, Juan] Univ Simon Bolivar, Dept Biol Organismos, Caracas, Venezuela.
[Robertson, Ross] Smithsonian Trop Res Inst, Balboa, Panama.
[Piorski, Nivaldo M.] Univ Fed Maranhao, Dept Oceanog & Limnol, Sao Luis, Maranhao, Brazil.
[Van Tassell, James] Hofstra Univ, Hempstead, NY 11550 USA.
[Giarrizzo, Tommaso] Fed Univ Para, Lab Biol Pesqueira, BR-66059 Belem, Para, Brazil.
[Gondolo, Guilherme] Univ Estadual Piaui, Lab Ictiol, Campo Maior, Piaui, Brazil.
RP Lasso-Alcala, O (reprint author), Fdn La Salle Ciencias Nat, Museo Hist Nat La Salle, Apartado Postal 1930, Caracas 1010A, Venezuela.
EM oscar.lasso@fundacionlasalle.org.ve
RI Piorski, Nivaldo/M-3828-2014; Giarrizzo, Tommaso/G-8482-2016
OI Piorski, Nivaldo/0000-0001-6279-107X; Giarrizzo,
Tommaso/0000-0002-5116-5206
FU Fundacao de Amparo a Pesquisa do Estado do Para (FAPESPA) [137/2008 -
Universal]
FX The present paper represents part of the academic activities by the
first author in the Programa Integrado de Estudios de Postgrado en
Zoologia Agricola, Universidad Central de Venezuela. Thanks to Fernando
Cervigon (UMA), Arturo Acero (UNC-CECIMAR / INVEMAR), Maria Elisabeth de
Araujo (UFPE) and Jeff Williams (USNM) for the comments and suggestions
on the manuscript. Also to the directors and personnel from the fish
collections consulted for their cooperation with the revision of the
material and providing information over the records of the species: Juan
Carlos Capelo (MOBR-EDIMAR), Donald Taphorn (MCNG), Francisco Bisbal
(EBRG), Luz M. Mejia-Ladino, Gabriel Navas (INV - PEC), Mark Sabaj, John
Lundberg (ANSP), Jeffrey Williams, Richard Vari (USNM), Robert Robins,
George Burgess (UF), Philip Hastings (SIO), Sara LeCroy (GCRL), Scott
Schaefer (AMNH), Patrick Campbell and Oliver Crimmen (BMNH), Paulo
Buckup (MNRJ). The Instituto Socialista de Pesca y Acuicultura
(INSOPESCA) granted the scientific fishing permits required in
Venezuela. T. Giarrizzo acknowledges financial support by the Fundacao
de Amparo a Pesquisa do Estado do Para (FAPESPA) (Project number:
137/2008 - Universal).
NR 47
TC 1
Z9 2
U1 1
U2 10
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 2011
VL 9
IS 3
BP 571
EP 578
PG 8
WC Zoology
SC Zoology
GA 834KX
UT WOS:000295959300010
ER
PT J
AU Lang, SLC
Boness, DJ
Bowen, WD
Iverson, SJ
AF Lang, S. L. C.
Boness, D. J.
Bowen, W. D.
Iverson, S. J.
TI Primiparous females do not exhibit reduced maternal care in gray seals
(Halichoerus grypus)
SO MARINE MAMMAL SCIENCE
LA English
DT Article
DE gray seal; Halichoerus grypus; lactation; maternal behavior; milk energy
transfer; nursing; primiparous; reproductive experience
ID GREY SEALS; SABLE ISLAND; REPRODUCTIVE-PERFORMANCE; BREEDING COLONIES;
POPULATION GROWTH; NOVA-SCOTIA; PUP GROWTH; BEHAVIOR; AGE; SENESCENCE
AB We compared the behaviors of primiparous and multiparous gray seal (Halichoerus grypus) females over the course of lactation to examine whether poorly developed maternal behaviors may play a role in the reduced lactation performance observed in primiparous females. Overall, primiparous females spent as much time interacting with their pups as multiparous females. The proportion of time spent nursing their pup increased significantly between early and peak lactation in both primiparous and multiparous females. Although there was no significant difference in the duration of nursing bouts as a function of reproductive status, primiparous females nursed significantly more frequently (bouts/hour) and, therefore, spent a significantly greater proportion of time nursing than multiparous females throughout lactation. Primiparous gray seal females were also significantly more active than multiparous females, however, the difference in activity represented only a small proportion of the overall time budget. We conclude that poorly developed maternal behaviors resulting from a lack of prior reproductive experience are unlikely to account for lower levels of milk energy transfer to pups in primiparous gray seals.
C1 [Lang, S. L. C.; Iverson, S. J.] Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada.
[Boness, D. J.] Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA.
[Boness, D. J.] Univ Maine, Dept Wildlife Ecol, Orono, ME 04469 USA.
[Boness, D. J.] Univ Maine, Sch Marine Sci, Orono, ME 04469 USA.
[Bowen, W. D.] Bedford Inst Oceanog, Dartmouth, NS B2Y 4A2, Canada.
RP Lang, SLC (reprint author), Dalhousie Univ, Dept Biol, Halifax, NS B3H 4J1, Canada.
EM shelley.lang@dal.ca
RI Bowen, William/D-2758-2012
FU Canadian Department of Fisheries and Oceans; Natural Sciences and
Engineering Research Council (NSERC); Smithsonian Institution; Dalhousie
Graduate Studies Fellowship
FX We would like to thank J. McMillan, J. van Dommelen, J. Bryan, and G.
Breed for assistance with the field work. We also thank G. Forbes,
Officer in Charge of Main Station on Sable Island and the Canadian Coast
Guard for providing continuing logistic support. This research was
supported by the Canadian Department of Fisheries and Oceans, Natural
Sciences and Engineering Research Council (NSERC) grants to SJI and WDB,
Smithsonian Institution grants to DJB and a Dalhousie Graduate Studies
Fellowship to SLCL.
NR 37
TC 2
Z9 2
U1 2
U2 21
PU WILEY-BLACKWELL
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 2011
VL 27
IS 3
BP E153
EP E164
DI 10.1111/j.1748-7692.2010.00443.x
PG 12
WC Marine & Freshwater Biology; Zoology
SC Marine & Freshwater Biology; Zoology
GA 793LU
UT WOS:000292825200002
ER
PT J
AU Zhang, ZQ
Kress, WJ
Xie, WJ
Ren, PY
Gao, JY
Li, QJ
AF Zhang, Z. -Q.
Kress, W. J.
Xie, W. -J.
Ren, P. -Y.
Gao, J. -Y.
Li, Q. -J.
TI Reproductive biology of two Himalayan alpine gingers (Roscoea spp.,
Zingiberaceae) in China: pollination syndrome and compensatory floral
mechanisms
SO PLANT BIOLOGY
LA English
DT Article
DE Biodiversity hotspot; compensatory floral mechanism; conservation;
Hengduan Mountains; long-proboscid pollinator; pollination syndrome
ID BIODIVERSITY HOTSPOTS; FLOWERS; LONG; CONSERVATION; MUTUALISMS;
LONGEVITY; EVOLUTION; ASSURANCE; PATTERNS; SYSTEMS
AB According to the concept of pollination syndromes, floral traits reflect specialisation to a particular pollinator or set of pollinators. However, the reproductive biology of endemic, and often specialised, plants may require increased attention as climate change accelerates worldwide. Species of Roscoea endemic to the Himalayan region have striking orchid-like flowers with long corolla tubes, suggesting pollination by long-tongued insects. Until now, the reproductive biology of species of Roscoea has been poorly documented. We investigated the floral biology, breeding system and pollination ecology of R. cautleoides and R. humeana, from Hengduan Mountains, a global biodiversity hotspot in southwest China. We also tested whether floral longevity increases pollination success. Pollination experiments showed that the two species were self-compatible and depended on insects for fruit production. Over several flowering seasons we did not observe any potential pollinators with long tongues that matched the corolla tube visiting flowers in centres of distribution. The principal pollinators observed were pollen-collecting generalist bees, with low visitation frequencies. In general, members of the ginger family are characterised by short-lived (usually 1 day) flowers, but flowers of R. cautleoides and R. humeana last 8 and 6 days, respectively. Removing stigmas decreased fruit set in both study populations. Our results suggest that the original pollinators may have been long-tongued insects that are now absent from the Chinese Himalayas because habitats have responded to climate change. However, long-lived and self-compatible flowers, coupled with the presence of generalist pollinators, are traits that have allowed these gingers to reproduce and continue to persist in the alpine habitats.
C1 [Zhang, Z. -Q.; Kress, W. J.; Ren, P. -Y.; Gao, J. -Y.; Li, Q. -J.] Chinese Acad Sci, Key Lab Trop Forest Ecol, Xishuangbanna Trop Bot Garden, Xishuangbanna 666303, Yunnan, Peoples R China.
[Zhang, Z. -Q.] Chinese Acad Sci, Key Lab Biodivers & Biogeog, Kunming Inst Bot, Kunming 666303, Yunnan, Peoples R China.
[Kress, W. J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Xie, W. -J.] Yunnan Acad Agr Sci, Flower Res Inst, Kunming, Yunnan, Peoples R China.
RP Li, QJ (reprint author), Chinese Acad Sci, Key Lab Trop Forest Ecol, Xishuangbanna Trop Bot Garden, Xishuangbanna 666303, Yunnan, Peoples R China.
EM qjli@xtbg.ac.cn
RI Zhang, Zhi-Qiang/E-4819-2013
OI Zhang, Zhi-Qiang/0000-0002-6907-3481
FU National Basic Research Program of China (973 Program) [2007CB411603];
Chinese Academy of Sciences; China Postdoctoral Science Foundation
[20090461412]
FX We thank the editor and two anonymous reviewers for insightful comments
that have improved this manuscript; M. Liu M and G.-H. Liu for field
assistance; Prof. Y.-R. Wu (IOZ, CAS) for identifying insects; Drs W.-J.
Liao, X.-S. Chen and G.-Y. Hao for comments on earlier versions of the
manuscript. This work was supported by the National Basic Research
Program of China (973 Program) 2007CB411603, the CAS/SEFEA International
Partnership Program for Creative Research Teams, the Fund for Top One
Hundred Young Scientists of the Chinese Academy of Sciences, and a China
Postdoctoral Science Foundation funded project (20090461412).
NR 47
TC 13
Z9 14
U1 4
U2 28
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1435-8603
J9 PLANT BIOLOGY
JI Plant Biol.
PD JUL
PY 2011
VL 13
IS 4
BP 582
EP 589
DI 10.1111/j.1438-8677.2010.00423.x
PG 8
WC Plant Sciences
SC Plant Sciences
GA 778DF
UT WOS:000291679100004
PM 21668599
ER
PT J
AU Angelier, F
Tonra, CM
Holberton, RL
Marra, PP
AF Angelier, Frederic
Tonra, Christopher M.
Holberton, Rebecca L.
Marra, Peter P.
TI Short-term changes in body condition in relation to habitat and rainfall
abundance in American redstarts Setophaga ruticilla during the
non-breeding season
SO JOURNAL OF AVIAN BIOLOGY
LA English
DT Article
ID DISTANCE MIGRATORY BIRD; LONG-LIVED BIRD; REPRODUCTIVE SUCCESS;
NONBREEDING SEASON; ENVIRONMENTAL-CONDITIONS; MIGRANT BIRD; FOOD; AGE;
SELECTION; SURVIVAL
AB In migratory birds, environmental conditions during the stationary period of the non-breeding season are crucial to consider because they ultimately affect the fitness of individuals by influencing their subsequent migration, breeding success and survival. Although a few studies have investigated the influence of non-breeding habitat on the capacity of individuals to cope with long-term seasonal rainfall fluctuations, it remains unknown how habitat quality and variations in rainfall abundance-at a monthly scale-interact to affect non-breeding condition of migrating birds. In this study, we examined the influence of monthly changes in rainfall abundance on body condition of non-breeding female redstarts Setophaga ruticilla living either in a high quality habitat (mangrove) or in a low quality habitat (scrub). Body condition of both mangrove and scrub redstarts showed important variations over the study period, demonstrating for the first time that body condition of non-breeding female redstarts can change rapidly in response to short-term fluctuations in rainfall. Importantly, we found that female redstarts living in mangrove were usually in better condition during periods of low rainfall compared to females living in scrub. However, body condition did not differ between mangrove females and scrub females during an episode of frequent, heavy precipitation. Importantly, our study also demonstrated that the duration of a perturbation is an important determinant of body condition in redstarts since a prolonged drought resulted in similar low body condition for birds from both habitats. Age was not correlated with body condition whatever the habitat and the rainfall conditions. Our results demonstrate that high quality habitat can temporarily reduce the deleterious effect of a short-term drought on body condition, but also, that a habitat of low quality does not constrain individuals when climatic conditions are optimal.
C1 [Angelier, Frederic] CNRS, Ctr Etud Biol Chize, UPR 1934, FR-79360 Villiers En Bois, France.
[Tonra, Christopher M.; Holberton, Rebecca L.] Univ Maine, Sch Biol & Ecol, Lab Avian Biol, Orono, ME 04469 USA.
[Marra, Peter P.] Natl Zool Pk, Smithsonian Migr Bird Ctr, Washington, DC 20008 USA.
RP Angelier, F (reprint author), CNRS, Ctr Etud Biol Chize, UPR 1934, FR-79360 Villiers En Bois, France.
EM angelier@cebc.cnrs.fr
RI Tonra, Christopher/B-1620-2013
FU NSF [0649679, 0717338]; European Community [237034]
FX This study was supported by NSF grants (0649679 and 0717338) to PPM and
RLH. FA was supported by the 7th research program of the European
Community FP7/2007-2013 (Marie-Curie Fellowship, no 237034). We thank E.
Corliss, J. L. Dowling, J. H. Junda, S. R. Sult and M. A. Thomas for
their assistance in the field. We thank J. Perez-Tris for helpful
comments and suggestions. We thank the Petroleum Corporation of Jamaica
for permission to conduct this research at the Font Hill Nature
Preserve, and Yvette Strong and Andrea Donaldson of the Jamaica National
Environmental Planning Agency for their cooperation.
NR 43
TC 13
Z9 13
U1 1
U2 30
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0908-8857
J9 J AVIAN BIOL
JI J. Avian Biol.
PD JUL
PY 2011
VL 42
IS 4
BP 335
EP 341
DI 10.1111/j.1600-048X.2011.05369.x
PG 7
WC Ornithology
SC Zoology
GA 822MM
UT WOS:000295051800007
ER
PT J
AU Day, J
Goldstein, F
Nolan, J
AF Day, John
Goldstein, Fred
Nolan, John
TI THE LAST WALTZ AND MOVING BEYOND TCP/IP
SO JOURNAL OF THE INSTITUTE OF TELECOMMUNICATIONS PROFESSIONALS
LA English
DT Article
C1 [Day, John] Smithsonian, Washington, DC 20013 USA.
[Nolan, John] First Mile Networks, Mayfield, E Sussex, England.
[Goldstein, Fred] Northeastern Univ, Boston, MA USA.
[Goldstein, Fred] Natl Technol Univ, Buenos Aires, DF, Argentina.
[Nolan, John] Intercai Mondiale, Marlow, Bucks, England.
RP Day, J (reprint author), Smithsonian, Washington, DC 20013 USA.
EM jeanjour@comcast.net; fgoldstein@ionary.com;
john.nolan@firstmilenetworks.co.uk
NR 0
TC 0
Z9 0
U1 0
U2 1
PU ITP-INST TELECOMMUNICATIONS PROFESSIONALS
PI MIDDLESEX
PA SUNBURY TE, GREEN STREET, SUNBURY ON THAMES, MIDDLESEX, TW16 6QJ,
ENGLAND
SN 1755-9278
J9 J I TELECOMMUN PROF
JI J. Inst. Telecommun. Prof.
PD JUL-SEP
PY 2011
VL 5
BP 42
EP 50
PN 3
PG 9
WC Engineering, Electrical & Electronic; Telecommunications
SC Engineering; Telecommunications
GA 824GL
UT WOS:000295190300007
ER
PT J
AU Kokkin, DL
Reilly, NJ
McCarthy, MC
Stanton, JF
AF Kokkin, D. L.
Reilly, N. J.
McCarthy, M. C.
Stanton, J. F.
TI Experimental and theoretical investigation of the (B)over-tilde(1)A
'-(X)over-tilde(1)A ' electronic transition of CuSH
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
DE Electronic spectroscopy; Metal hydrosulfides; Equation-of-motion
coupled-cluster
ID MILLIMETER-WAVE SPECTRUM; PURE ROTATIONAL SPECTRUM; COUPLED-CLUSTER
METHOD; MILLIMETER/SUBMILLIMETER SPECTRUM; LABORATORY DETECTION; METAL
HYDROSULFIDES; ENERGY GRADIENTS; SPECTROSCOPY; HYDRODESULFURIZATION;
MOLECULE
AB By means of resonant two-color two-photon ionization time-of-flight mass spectroscopy, the jet-cooled spectrum of the (B) over tilde (1)A '-(X) over tilde (1)A ' transition of CuSH and CuSD, exhibiting an origin near 434 nm, has been measured. The carrier of the spectrum is confirmed to be CuSH, formed in a discharge between copper electrodes through H2S diluted in argon, on the basis of isotope analysis and comparison with ab initio calculations. Guided by coupled-cluster calculations of the (X) over tilde and (B) over tilde -states for both isotopologues, all of the observed bands are readily assigned to transitions involving the Cu-S stretch and Cu-S-H bend. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Kokkin, D. L.; Reilly, N. J.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Kokkin, D. L.; Reilly, N. J.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Stanton, J. F.] Univ Texas Austin, Dept Chem & Biochem, Austin, TX 78712 USA.
RP Reilly, NJ (reprint author), Harvard Univ, Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA.
EM nreilly@cfa.harvard.edu
FU NSF [CHE-0701204]; Robert A. Welch Foundation [F-1283]
FX The laboratory work in Cambridge was supported by the NSF Grant
CHE-0701204. JFS would like to thank the Robert A. Welch Foundation
(Grant F-1283) and the NSF for funding support.
NR 41
TC 5
Z9 5
U1 1
U2 5
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD JUL-AUG
PY 2011
VL 268
IS 1-2
SI SI
BP 23
EP 27
DI 10.1016/j.jms.2011.03.023
PG 5
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 819NH
UT WOS:000294833100005
ER
PT J
AU Nicole, S
Erickson, DL
Ambrosi, D
Bellucci, E
Lucchin, M
Papa, R
Kress, WJ
Barcaccia, G
AF Nicole, Silvia
Erickson, David L.
Ambrosi, Daria
Bellucci, Elise
Lucchin, Margherita
Papa, Roberto
Kress, W. John
Barcaccia, Gianni
TI Biodiversity studies in Phaseolus species by DNA barcoding
SO GENOME
LA English
DT Article
DE Phaseolus spp.; plastid DNA; internal transcribed spacers; DNA
barcoding; varietal groups; single-nucleotide polymorphisms
ID MULTILOCUS GENOTYPE DATA; LAND PLANTS; VULGARIS L.; GENETIC DIVERSITY;
CHLOROPLAST DNA; NONCODING REGIONS; SEQUENCES; IDENTIFICATION; TAXONOMY;
LANDRACES
AB The potential of DNA barcoding was tested as a system for studying genetic diversity and genetic traceability in bean germplasm. This technique was applied to several pure lines of Phaseolus vulgaris L. belonging to wild, domesticated, and cultivated common beans, along with some accessions of Phaseolus coccineus L., Phaseolus lunatus L., and Vigna unguiculata (L.) Walp. A multilocus approach was exploited using three chloroplast genic regions (rbcL, trnL, and matK), four intergenic spacers (rpoB-trnC, atpBrbcL, trnT-trnL, and psbA-trnH), and nuclear ITS1 and ITS2 rDNA sequences. Our main goals were to identify the markers and SNPs that show the best discriminant power at the variety level in common bean germplasm, to examine two methods (tree based versus character based) for biodiversity analysis and traceability assays, and to evaluate the overall utility of chloroplast DNA barcodes for reconstructing the origins of modern Italian varieties. Our results indicate that the neighbor-joining method is a powerful approach for comparing genetic diversity within plant species, but it is relatively uninformative for the genetic traceability of plant varieties. In contrast, the character-based method was able to identify several distinct haplotypes over all target regions corresponding to Mesoamerican or Andean accessions; Italian accessions originated from both gene pools. On the whole, our findings raise some concerns about the use of DNA barcoding for intraspecific genetic diversity studies in common beans and highlights its limitations for resolving genetic relationships between landraces and varieties.
C1 [Nicole, Silvia; Ambrosi, Daria; Lucchin, Margherita; Barcaccia, Gianni] Univ Padua, Dept Environm Agron & Crop Sci, I-35020 Padua, Italy.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20013 USA.
[Bellucci, Elise; Papa, Roberto] Univ Politecn Marche, Dept Environm Sci & Crop Prod, I-60131 Ancona, Italy.
[Papa, Roberto] Agr Res Council, Cereal Res Ctr, I-71122 Foggia, Italy.
RP Barcaccia, G (reprint author), Univ Padua, Dept Environm Agron & Crop Sci, Via Univ 16,Campus Agripolis, I-35020 Padua, Italy.
EM gianni.barcaccia@unipd.it
RI papa, roberto/F-9510-2014;
OI papa, roberto/0000-0001-9598-3131; Bellucci, Elisa/0000-0002-1636-0719
FU A. Gini Foundation (University of Padova, Italy); Smithsonian
Institution; Ministry of University, Research, Science, and Technology
(Italy); University of Padova [CPDA087818/08]
FX Thanks are due to the A. Gini Foundation (University of Padova, Italy)
to support S.N. during her internship at the Smithsonian Institution
(Washington DC). We also thank B. Campion, Agricultural Research
Council, Research Unit for Vegetable Crops (CRA-ORL; Montanaso Lombardo,
Italy), for supplying the Italian bean varieties. Funding for this
project was provided by the Smithsonian Institution, the Ministry of
University, Research, Science, and Technology (Italy), and the
University of Padova (project CPDA087818/08).
NR 60
TC 9
Z9 10
U1 2
U2 27
PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS
PI OTTAWA
PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA
SN 0831-2796
J9 GENOME
JI Genome
PD JUL
PY 2011
VL 54
IS 7
BP 529
EP 545
DI 10.1139/G11-018
PG 17
WC Biotechnology & Applied Microbiology; Genetics & Heredity
SC Biotechnology & Applied Microbiology; Genetics & Heredity
GA 818XB
UT WOS:000294788600001
PM 21777058
ER
PT J
AU Fromm, CM
Perucho, M
Ros, E
Savolainen, T
Lobanov, AP
Zensus, JA
Aller, MF
Aller, HD
Gurwell, MA
Lahteenmaki, A
AF Fromm, C. M.
Perucho, M.
Ros, E.
Savolainen, T.
Lobanov, A. P.
Zensus, J. A.
Aller, M. F.
Aller, H. D.
Gurwell, M. A.
Lahteenmaki, A.
TI Catching the radio flare in CTA102 I. Light curve analysis
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies: active; galaxies: jets; radiation mechanisms: non-thermal;
quasars: individual: CTA102
ID ACTIVE GALACTIC NUCLEI; RELATIVISTIC JETS; SPECTRAL EVOLUTION; 3C 345;
X-RAY; MODELS; QUASARS; CTA-102; OBJECTS; OUTBURSTS
AB Context. The blazar CTA102 (z = 1.037) underwent a historical radio outburst in April 2006. This event offered a unique chance to study the physical properties of the jet.
Aims. We used multifrequency radio and mm observations to analyze the evolution of the spectral parameters during the flare as a test of the shock-in-jet model under these extreme conditions.
Methods. For the analysis of the flare we took into account that the flaring spectrum is superimposed on a quiescent spectrum. We reconstructed the latter from archival data and fitted a synchrotron self-absorbed distribution of emission. The uncertainties of the derived spectral parameters were calculated using Monte Carlo simulations. The spectral evolution is modeled by the shock-in-jet model, and the derived results are discussed in the context of a geometrical model (varying viewing angle) and shock-shock interaction
Results. The evolution of the flare in the turnover frequency-turnover flux density (nu(m) - S(m)) plane shows a double peak structure. The nature of this evolution is dicussed in the frame of shock-in-jet models. We discard the generation of the double peak structure in the nu(m) - S(m) plane purely based on geometrical changes (variation of the Doppler factor). The detailed modeling of the spectral evolution favors a shock-shock interaction as a possible physical mechanism behind the deviations from the standard shock-in-jet model.
C1 [Fromm, C. M.; Ros, E.; Savolainen, T.; Lobanov, A. P.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany.
[Perucho, M.; Ros, E.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain.
[Perucho, M.] Univ Valencia, Dept Matemat Econ Empresa, Valencia 46022, Spain.
[Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland.
RP Fromm, CM (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany.
EM cfromm@mpifr.de
RI Lahteenmaki, Anne/L-5987-2013; Lobanov, Andrei/G-5891-2014; Perucho,
Manel/A-9528-2017;
OI Perucho, Manel/0000-0003-2784-0379; Ros, Eduardo/0000-0001-9503-4892;
Savolainen, Tuomas/0000-0001-6214-1085
FU International Max Planck Research School (IMPRS) for Astronomy and
Astrophysics at the Universities of Bonn and Cologne; COSTMP0905; Kolner
Gymnasial- und Studienstiftung; Spanish "Ministerio de Ciencia e
Innovacion" (MICINN) [AYA2010-21322-C03-01, AYA2010-21097-C03-01,
CONSOLIDER2007-00050, AYA2009-13036-C02-02]; Generalitat Valenciana
[PROMETEO-2009-103]; MICINN through Juan de la Cierva; NSF; university
of Michigan; Smithsonian Institution; Academia Sinica; Academy of
Finland
FX C.M.F. was supported for this research through a stipend from the
International Max Planck Research School (IMPRS) for Astronomy and
Astrophysics at the Universities of Bonn and Cologne. Part of this work
was supported by the COST Action MP0905 Black Hole in a violent
Universe. C. M. F. was supported during his Diploma Thesis by Kolner
Gymnasial- und Studienstiftung. C. M. F. thanks the Departament
d'Astronomia i Astrofisica of the University Valencia for its
hospitality. M. P. acknowledges financial support from the Spanish
"Ministerio de Ciencia e Innovacion" (MICINN) grants
AYA2010-21322-C03-01, AYA2010-21097-C03-01 and CONSOLIDER2007-00050, and
from the "Generalitat Valenciana" grant "PROMETEO-2009-103". M. P.
acknowledges support from MICINN through a "Juan de la Cierva" contract.
E. R. acknowledges partial support by the Spanish MICINN through grant
AYA2009-13036-C02-02. Part of this work was carried out while T. S. was
a research fellow of the Alexander von Humboldt Foundation. This work is
based on observations with the radio telescope of the university of
Michigan, MI, USA, the Metsahovi radio telescope of the university of
Helsinki, Finland and Submillimeter Array (SMA) of the Smithsonian
Astrophysical Observatory, Cambridge, MA, USA. The operation of UMRAO is
made possible by funds from the NSF and from the university of Michigan.
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 Metsahovi team acknowledges the support from the
Academy of Finland to our observing projects. We thank Maria Massi and
Petar Mimica for fruitful discussions and comments.
NR 38
TC 21
Z9 21
U1 0
U2 3
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2011
VL 531
AR A95
DI 10.1051/0004-6361/201116857
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795YZ
UT WOS:000293017700146
ER
PT J
AU Long, DM
Gallagher, PT
McAteer, RTJ
Bloomfield, DS
AF Long, D. M.
Gallagher, P. T.
McAteer, R. T. J.
Bloomfield, D. S.
TI Deceleration and dispersion of large-scale coronal bright fronts
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: UV
radiation; waves
ID SOLAR-FLARE WAVES; EIT WAVES; MORETON WAVES; MASS EJECTION; STEREO;
MULTIWAVELENGTH; REFLECTION; EVOLUTION; DIMMINGS; REGIONS
AB Context. One of the most dramatic manifestations of solar activity are large-scale coronal bright fronts (CBFs) observed in extreme ultraviolet (EUV) images of the solar atmosphere. To date, the energetics and kinematics of CBFs remain poorly understood, due to the low image cadence and sensitivity of previous EUV imagers and the limited methods used to extract the features.
Aims. In this paper, the trajectory and morphology of CBFs was determined in order to investigate the varying properties of a sample of CBFs, including their kinematics and pulse shape, dispersion, and dissipation.
Methods. We have developed a semi-automatic intensity profiling technique to extract the morphology and accurate positions of CBFs in 2.5-10 min cadence images from STEREO/EUVI. The technique was applied to sequences of 171 angstrom and 195 angstrom images from STEREO/EUVI in order to measure the wave properties of four separate CBF events.
Results. Following launch at velocities of similar to 240-450 km s(-1) each of the four events studied showed significant negative acceleration ranging from similar to-290 to -60 ms(-2). The CBF spatial and temporal widths were found to increase from similar to 50 Mm to similar to 200 Mm and similar to 100 s to similar to 1500 s respectively, suggesting that they are dispersive in nature. The variation in position-angle averaged pulse-integrated intensity with propagation shows no clear trend across the four events studied. These results are most consistent with CBFs being dispersive magnetoacoustic waves.
C1 [Long, D. M.; Gallagher, P. T.; McAteer, R. T. J.; Bloomfield, D. S.] Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
[Long, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[McAteer, R. T. J.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA.
RP Long, DM (reprint author), Trinity Coll Dublin, Astrophys Res Grp, Sch Phys, Dublin 2, Ireland.
EM longda@tcd.ie
RI Bloomfield, Shaun/G-5809-2011; Long, David/J-3227-2013; Gallagher,
Peter/C-7717-2011
OI Bloomfield, Shaun/0000-0002-4183-9895; Long, David/0000-0003-3137-0277;
Gallagher, Peter/0000-0001-9745-0400
FU Irish Research Council for Science, Engineering and Technology (IRCSET)
FX D.M.L. is a Government of Ireland Scholar supported by the Irish
Research Council for Science, Engineering and Technology (IRCSET),
R.T.J.McA. carried out this work as a Marie Curie Fellow under FP6, and
D.S.B. is a Marie Curie Fellow funded under FP7. We would like to thank
the STEREO/SECCHI consortium for providing open access to their data and
technical support as well as A. M. Veronig and I. W. Kienreich for
useful discussions
NR 36
TC 30
Z9 30
U1 0
U2 5
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2011
VL 531
DI 10.1051/0004-6361/201015879
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795YZ
UT WOS:000293017700024
ER
PT J
AU Neufeld, MJ
AF Neufeld, Michael J.
TI Continental Defense in the Eisenhower Era: Nuclear Antiaircraft Arms and
the Cold War
SO JOURNAL OF MILITARY HISTORY
LA English
DT Book Review
C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SOC MILITARY HISTORY
PI LEXINGTON
PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA
24450-1600 USA
SN 0899-3718
J9 J MILITARY HIST
JI J. Mil. Hist.
PD JUL
PY 2011
VL 75
IS 3
BP 971
EP 973
PG 3
WC History
SC History
GA 793VE
UT WOS:000292851200063
ER
PT J
AU Buffington, ML
AF Buffington, Matthew L.
TI DESCRIPTION, CIRCUMSCRIPTION AND PHYLOGENETICS OF THE DIGLYPHOSEMATINI
BELIZIN 1961, AND THE DESCRIPTION OF A NEW GENUS (HYMENOPTERA:
FIGITIDAE: EUCOILINAE)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Sinatra; revision; phylogeny
ID PHASEOLUS-VULGARIS; AGROMYZIDAE; LIRIOMYZA; CYNIPOIDEA; DIPTERA;
BUFFINGTON; WATERMELON
AB The genera comprising the Diglyphosematini Belizin (Hymenoptera: Figitidae: Eucoilinae) are redescribed, all of the valid species are cataloged, and a key to all Diglyphosematini genera is provided. To determine the monophyly of each of the included genera, a phylogenetic analysis of 1060 ribosomal characters, 392 mitochondrial characters, and 169 morphological/biological characters was conducted for 18 ingroup taxa in both a parsimony and Bayesian framework. Based on the results presented here and elsewhere, the Diglyphosematini are comprised of the following genera: Banacuniculus Buffington, Diglyphosema Forster, Disorygma Forster, Ealata Quinlan, Ganaspidium Weld, Gronotoma Forster, Microstilba Forster, Nordlanderia Quinlan, Paradiglyphosema Lin, and Tobiasiana Kovalev. Disorygma was not recovered as monophyletic; Sinatra Buffington, new genus, also included in Diglyphosematini, is described to accommodate S. pacifica (Yoshimoto). Nordlanderia, revised status, is removed from synonymy with Tobiasiana. Characters and character states applicable specifically to Diglyphosematini are defined and illustrated. Characters supporting the monophyly of each genus are discussed. All species of Diglyphosematini whose biology has been studied in depth are parasitoids of leaf-mining and stem-mining Agromyzidae (Diptera), or rarely, of fruit infesting Tephritidae (Diptera). New host records for Diglyphosema and Ealata, as well distributions and known type repositories for each species of Diglyphosematini, are reported.
C1 USDA, Systemat Entomol Lab, Smithsonian Inst, NMNH, Washington, DC 20013 USA.
RP Buffington, ML (reprint author), USDA, Systemat Entomol Lab, Smithsonian Inst, NMNH, 10th & Constitut Ave NW, Washington, DC 20013 USA.
EM matt.buffington@ars.usda.gov
FU National Science Foundation [DEB9712543]; Systematic Entomology
Laboratory, USDA/ARS
FX I thank Robert Wharton, James Woolley and John McEachran (Texas A&M
University, College Station, TX), Goran Nordlander (Swedish Agricultural
University, Uppsala, Sweden), and Fredrik Ronquist (Department of
Entomology, Swedish Museum of Natural History, Stockholm, Sweden) for
outstanding guidance and support throughout the early portions of this
project. Thanks also to: John LaSalle (CSIRO, Canberra, Australia) for
providing reared specimens and for allowing the use of their host data;
Andy Polaszek (BMNH, London) for assisting with deciphering D.J.
Greathead's handwritten labels. Smithsonian Institution interns
Stephanie Bailey and Jerrett McCormick assisted with the acquisition of
SEM's used in this project. I also thank the curators of the
institutions mentioned in the Materials and Methods section for
assisting me with loans of specimens. Dave Smith and Thomas Henry
(Systematic Entomology Laboratory, USDA/ARS, Washington, DC), Mattias
Forshage (Department of Entomology, Swedish Museum of Natural History,
Stockholm, Sweden), Jose-Luis Nieves Aldrey (Museo Nacional de Ciencas
Naturales, Madrid, Spain) and one anonymous reviewer improved the
quality of this paper immensely. This project was funded by the National
Science Foundation Partnerships for the Enhancement and Education in
Taxonomy (PEET) Grant, number DEB9712543 and the Systematic Entomology
Laboratory, USDA/ARS. Research was carried out at Texas A&M University,
College Station, TX, Uppsala University, Uppsala, Sweden, and the
National Museum of Natural History, Smithsonian Institution, Washington
DC. USDA is an equal opportunity employer.
NR 82
TC 6
Z9 6
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 2011
VL 113
IS 3
BP 239
EP 290
DI 10.4289/0013-8797.113.3.239
PG 52
WC Entomology
SC Entomology
GA 810RT
UT WOS:000294145500001
ER
PT J
AU Hoebeke, ER
Smith, DR
Goulet, H
AF Hoebeke, E. Richard
Smith, David R.
Goulet, Henri
TI ATHALIA CORNUBIAE BENSON (HYMENOPTERA: TENTHREDINIDAE: ALLANTINAE), A
SAWFLY GENUS AND SPECIES NEW TO NORTH AMERICA
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE adventive species; New York; Ontario
AB Athalia cornubiae Benson, an Old World species that feeds on Sedum (Crassulaceae), is reported from North America. It was collected in a Lindgren funnel trap in East Syracuse, Onondaga Co., New York, U.S.A. in 2007 and found in Malaise trap collections at a residence in Ottawa, Ontario, Canada, in 2010. This is the first record of both the genus and species in the Western Hemisphere.
C1 [Hoebeke, E. Richard] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA.
[Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
[Goulet, Henri] Cent Expt Farm, Ottawa, ON K1A 0C6, Canada.
RP Hoebeke, ER (reprint author), Cornell Univ, Dept Entomol, Comstock Hall, Ithaca, NY 14853 USA.
EM erh2@cornell.edu; dave.smith@ars.usda.gov; henri.goulet@agr.gc.ca
NR 22
TC 0
Z9 0
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 2011
VL 113
IS 3
BP 309
EP 314
DI 10.4289/0013-8797.113.3.309
PG 6
WC Entomology
SC Entomology
GA 810RT
UT WOS:000294145500004
ER
PT J
AU Bringel, JBD
Nakajima, JN
Robinson, H
AF de Azevedo Bringel, Joao Bernardo, Jr.
Nakajima, Jimi Naoki
Robinson, Harold
TI Allocephalus gamolepis, a New Genus and Species of Dipterocypselinae
(Vernonieae, Asteraceae) from Central Brazil
SO SYSTEMATIC BOTANY
LA English
DT Article
DE Dipterocypsela; Heterocypsela; Manyonia; Parana River Basin
ID MINAS-GERAIS
AB Allocephalus gamolepis is newly described here for the tribe Vernonieae (Compositae). The new genus, placed in subtribe Dypterocypselinae, is clearly distinct from other genera of subtribe by its capitula in axillary glomerules or spikelets, involucres with fused phyllaries and a biseriate pappus with an outer series of short setae and an inner series of longer flattened bristles. A key for the genera of Dypterocypselineae is provided.
C1 [de Azevedo Bringel, Joao Bernardo, Jr.] Jardim Bot Brasilia, Setor Mansoes Don Bosco, Brasilia, DF, Brazil.
[Nakajima, Jimi Naoki] Univ Fed Uberlandia, Inst Biol, Uberlandia, MG, Brazil.
[Robinson, Harold] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA.
RP Bringel, JBD (reprint author), Jardim Bot Brasilia, Setor Mansoes Don Bosco, Conjunto 12 Lago Sul, Brasilia, DF, Brazil.
EM jbbringel@gmail.com
RI Nakajima, Jimi/A-7718-2013
NR 15
TC 0
Z9 0
U1 0
U2 5
PU AMER SOC PLANT TAXONOMISTS
PI LARAMIE
PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071
USA
SN 0363-6445
J9 SYST BOT
JI Syst. Bot.
PD JUL-SEP
PY 2011
VL 36
IS 3
BP 785
EP 788
DI 10.1600/036364411X583736
PG 4
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 807WO
UT WOS:000293933900022
ER
PT J
AU Schroth, G
Faria, D
Araujo, M
Bede, L
Van Bael, SA
Cassano, CR
Oliveira, LC
Delabie, JHC
AF Schroth, Goetz
Faria, Deborah
Araujo, Marcelo
Bede, Lucio
Van Bael, Sunshine A.
Cassano, Camila R.
Oliveira, Leonardo C.
Delabie, Jacques H. C.
TI Conservation in tropical landscape mosaics: the case of the cacao
landscape of southern Bahia, Brazil
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE Agroforest; Atlantic Forest; Cabruca; Landscape scale conservation;
On-farm reserves; Theobroma cacao
ID 2 CONTRASTING LANDSCAPES; ATLANTIC FOREST TREES; BIODIVERSITY
CONSERVATION; AGROFORESTRY SYSTEMS; SPECIES RICHNESS; BIRD DIVERSITY;
SHADE COFFEE; RAIN-FOREST; COSTA-RICA; PLANTATIONS
AB A recent debate has contrasted two conservation strategies in agricultural landscapes; either "land sparing'' farm development combining intensive production practices with forest set-asides, or "wildlife-friendly'' farming with greater on-farm habitat value but lower yields. We argue that in established mosaic landscapes including old cacao production regions where natural forest has already been reduced to relatively small fragments, a combination of both strategies is needed to conserve biodiversity. After reviewing the evidence for the insufficiency of either strategy alone if applied to such landscapes, the paper focuses on the cacao production landscape of southern Bahia, Brazil, once the world's second largest cacao producer. Here, small remaining areas of Atlantic Forest are embedded in a matrix dominated by traditional cacao agroforests, resulting in a landscape mosaic that has proven favorable to the conservation of the region's high biodiversity. We show that current land use dynamics and public policies pose threats but also offer opportunities to conservation and describe a three- pronged landscape conservation strategy, consisting of (i) expansion of the protected areas system, (ii) promotion of productive yet biodiversity-friendly cacao farming practices, and (iii) assistance to land users to implement legally mandated on-farm reserves and voluntary private reserves. We discuss recent experiences concerning the implementation of this strategy, discuss likely future scenarios, and reflect on the applicability of the Bahian experience to biodiversity rich cacao production regions elsewhere in the tropics.
C1 [Schroth, Goetz] Mars Inc, BR-68109971 Santarem, Para, Brazil.
[Schroth, Goetz] Fed Univ Western Para, BR-68109971 Santarem, Para, Brazil.
[Faria, Deborah; Delabie, Jacques H. C.] Univ Estadual Santa Cruz, BR-45650000 Ilheus, BA, Brazil.
[Araujo, Marcelo; Cassano, Camila R.; Oliveira, Leonardo C.] IESB, BR-45653145 Ilheus, BA, Brazil.
[Bede, Lucio] Conservacao Int, BR-30112021 Belo Horizonte, MG, Brazil.
[Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Panama City, Panama.
[Cassano, Camila R.] Univ Sao Paulo, Dept Ecol, BR-05508090 Sao Paulo, Brazil.
[Oliveira, Leonardo C.] Univ Maryland, Dept Biol, College Pk, MD 20740 USA.
[Delabie, Jacques H. C.] CEPLAC, Ctr Pesquisa Cacau, BR-45600000 Itabuna, BA, Brazil.
RP Schroth, G (reprint author), Mars Inc, CP 513, BR-68109971 Santarem, Para, Brazil.
EM goetz.schroth@effem.com
RI Faria, Deborah/F-2879-2010; Delabie, Jacques/F-3405-2010; Cassano,
Camila/E-6761-2014; Oliveira, Leonardo/G-1290-2012
OI Delabie, Jacques/0000-0002-2695-1061; Oliveira,
Leonardo/0000-0002-1774-0713
FU Critical Ecosystem Partnership Fund (CEPF); European Union; SAVE
Brasil/BirdLife International; USAID; PPG7; Citibank; PDA Mata
Atlantica; PROBIO-PRONABIO/MMA-CNPq/BIRD-GEF; CNPq-Programa Nordeste;
PRONEX-CNPq/FAPESB; FAPESB; Gordon and Betty Moore Foundation; Seeds of
Change for Conservation International; CNPq
FX The work in Bahia reviewed in this paper has over the years received
support from various donors, including Critical Ecosystem Partnership
Fund (CEPF), European Union, SAVE Brasil/BirdLife International, USAID,
PPG7, Citibank, and PDA Mata Atlantica to IESB;
PROBIO-PRONABIO/MMA-CNPq/BIRD-GEF, CNPq-Programa Nordeste,
PRONEX-CNPq/FAPESB, and FAPESB to UESC; and the Gordon and Betty Moore
Foundation and Seeds of Change for Conservation International. DF and
JHCD also acknowledge their research grants from CNPq. Comments from
Luiz Paulo de Souza Pinto helped to improve the text.
NR 75
TC 42
Z9 43
U1 4
U2 68
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 JUL
PY 2011
VL 20
IS 8
BP 1635
EP 1654
DI 10.1007/s10531-011-0052-x
PG 20
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 799LH
UT WOS:000293287700003
ER
PT J
AU Moser, WE
Klemm, DJ
Phillips, AJ
Trauth, SE
Neal, RG
Stanley, JW
Connior, MB
Flotemersch, JE
AF Moser, William E.
Klemm, Donald J.
Phillips, Anna J.
Trauth, Stanley E.
Neal, Robert G.
Stanley, Jonathan W.
Connior, Matthew B.
Flotemersch, Joseph E.
TI Distribution of the Genus Philobdella (Macrobdellidae: Hirudinida),
Including New Locality Records from Arkansas and Oklahoma
SO COMPARATIVE PARASITOLOGY
LA English
DT Article
DE Philobdella gracilis; Philobdella floridana; Macrobdellidae; Hirudinida;
Hirudinea; Hirudinidae; leeches; Arkansas; Oklahoma
ID LEECH; FAMILY; WORLD
AB Philobdella gracilis Moore, 1901 (Macrobdellidae: Hirudinida) is reported from Arkansas and Oklahoma for the first time. Specimens were collected in creeks and ponds. The Mississippi drainage distribution of P. gracilis and eastern distribution Philobdella floridana were confirmed by reexamination of museum specimens.
C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA.
[Klemm, Donald J.; Flotemersch, Joseph E.] US EPA, Off Res & Dev, NERL, EERD,ERB, Cincinnati, OH 45268 USA.
[Phillips, Anna J.] CUNY, Grad Ctr, Dept Biol, New York, NY 10016 USA.
[Phillips, Anna J.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA.
[Trauth, Stanley E.; Neal, Robert G.; Stanley, Jonathan W.] Arkansas State Univ, Dept Biol Sci, State Univ, AR 72467 USA.
[Connior, Matthew B.] S Arkansas Community Coll, El Dorado, AR 71731 USA.
RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
EM moserw@si.edu; klemm.donald@epa.gov; ajphillips@amnh.org;
strauth@astate.edu; robert.neal@astate.edu;
jonathanw.stanley@smail.astate.edu; mconnior@southark.edu;
flotemersch.joseph@epa.gov
OI Phillips, Anna/0000-0003-4883-0022
NR 13
TC 1
Z9 2
U1 0
U2 3
PU HELMINTHOLOGICAL SOC WASHINGTON
PI LAWRENCE
PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS
66044 USA
SN 1525-2647
J9 COMP PARASITOL
JI Comp. Parasitol.
PD JUL
PY 2011
VL 78
IS 2
BP 387
EP 391
DI 10.1654/4507.1
PG 5
WC Parasitology; Zoology
SC Parasitology; Zoology
GA 803WH
UT WOS:000293612300023
ER
PT J
AU McAllister, CT
Moser, WE
Klemm, DJ
AF McAllister, Chris T.
Moser, William E.
Klemm, Donald J.
TI Actinobdella inequiannulata (Annelida: Hirudinida: Rhynchobdellida:
Glossiphoniidae) from White Crappie, Pomoxis annularis (Perciformes:
Centrarchidae), in Arkansas, USA
SO COMPARATIVE PARASITOLOGY
LA English
DT Article
DE white crappie; Pomoxis annularis; Catostomidae; Centrarchidae;
Actinobdella inequiannulata; Annelida; Hirudinea; Hirudinida;
Rhynchobdellida; Glossiphoniidae; leech; Arkansas; Ouachita River
ID FRESH-WATER LEECHES; RECORDS; MOORE
AB One of 4 (25%) white crappie, Pomoxis annularis, specimens from the Ouachita River, Dallas County, Arkansas, was found to be infested with 8 glossiphoniid leeches, Actinobdella inequiannulata Moore, 1901. Leeches were removed from within the operculum on gills and gill arches. This leech is generally thought to be uncommon but has been reported previously, mainly on members of the family Catostomidae from 21 states of the United States and 5 provinces of Canada. We report a new host record and the first report of A. inequiannulata from Arkansas.
C1 [McAllister, Chris T.] Eastern Oklahoma State Coll, Div Sci & Math, Idabel, OK 74745 USA.
[Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA.
[Klemm, Donald J.] US EPA, Off Res & Dev, NERL, EERD,ERB, Cincinnati, OH 45268 USA.
RP McAllister, CT (reprint author), Eastern Oklahoma State Coll, Div Sci & Math, 2805 NE Lincoln Rd, Idabel, OK 74745 USA.
EM cmcallister@se.edu; moserw@si.edu; klemm.donald@epa.gov
NR 28
TC 0
Z9 0
U1 1
U2 3
PU HELMINTHOLOGICAL SOC WASHINGTON
PI LAWRENCE
PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS
66044 USA
SN 1525-2647
EI 1938-2952
J9 COMP PARASITOL
JI Comp. Parasitol.
PD JUL
PY 2011
VL 78
IS 2
BP 392
EP 394
DI 10.1654/4503.1
PG 3
WC Parasitology; Zoology
SC Parasitology; Zoology
GA 803WH
UT WOS:000293612300024
ER
PT J
AU Barentsen, G
Vink, JS
Drew, JE
Greimel, R
Wright, NJ
Drake, JJ
Martin, EL
Valdivielso, L
Corradi, RLM
AF Barentsen, Geert
Vink, Jorick S.
Drew, J. E.
Greimel, R.
Wright, N. J.
Drake, J. J.
Martin, E. L.
Valdivielso, L.
Corradi, R. L. M.
TI T Tauri candidates and accretion rates using IPHAS: method and
application to IC 1396
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; stars: pre-main-sequence; stars: variables:
T Tauri, Herbig Ae/Be; open clusters and associations: individual:
IC1396
ID MAIN-SEQUENCE STARS; H-ALPHA-EMISSION; LOW-MASS STARS; NORTHERN GALACTIC
PLANE; RADIATION-DRIVEN IMPLOSION; ETA-CHAMAELEONTIS CLUSTER;
HUBBLE-SPACE-TELESCOPE; IRAS POINT SOURCES; BROWN DWARFS; DISK EVOLUTION
AB The Isaac Newton Telescope (INT) Photometric H-Alpha Survey (IPHAS) is a 1800 deg(2) survey of the Northern Galactic Plane, reaching down to r' similar to 21. We demonstrate how the survey can be used to (1) reliably select classical T Tauri star candidates and (2) constrain the mass accretion rates with an estimated relative uncertainty of 0.6 dex. IPHAS is a necessary addition to spectroscopic surveys because it allows large and uniform samples of accretion rates to be obtained with a precise handle on the selection effects.
We apply the method on a region of 7 deg(2) towards the H II region IC 1396 in Cepheus OB2 and identify 158 pre-main-sequence candidates with masses between 0.2 and 2.0 M-circle dot and accretion rates between 10(-9.2) and 10(-7.0) M-circle dot yr(-1). We find a power-law dependency between the stellar mass and the accretion rates with a slope of alpha = 1.1 +/- 0.2, which is less steep than indicated by previous studies. We discuss the influence of method-dependent systematic effects on the determination of this relationship.
The majority of our sample consists of faint, previously unknown, low-mass T Tauri candidates (56 per cent between 0.2 and 0.5 M-circle dot). Many candidates are clustered in front of three bright-rimmed molecular clouds, which are being ionized by the massive star HD206267 (O6.5V). We discover a spatio-temporal gradient of increasing accretion rates, increasing Spitzer infrared excess, and younger ages away from the ionizing star, providing a strong indication that the formation of these clusters has been sequentially triggered by HD206267 during the last similar to 1 Myr.
C1 [Barentsen, Geert; Vink, Jorick S.] Armagh Observ, Armagh BT61 9DG, North Ireland.
[Drew, J. E.] Univ Hertfordshire, Ctr Astron Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England.
[Greimel, R.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria.
[Wright, N. J.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Martin, E. L.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain.
[Valdivielso, L.; Corradi, R. L. M.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain.
[Corradi, R. L. M.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
RP Barentsen, G (reprint author), Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland.
EM gba@arm.ac.uk
OI Drew, Janet/0000-0003-1192-7082
FU Department of Culture, Arts and Leisure (DCAL) for Northern Ireland; UK
Science and Technology Facilities Council (STFC)
FX We thank the anonymous referee for providing useful comments which
helped us to improve the paper. We are also indebted to A.
Sicilia-Aguilar for providing helpful and constructive suggestions.
Armagh Observatory is funded by major grants from the Department of
Culture, Arts and Leisure (DCAL) for Northern Ireland and the UK Science
and Technology Facilities Council (STFC). The IPHAS survey is carried
out at the INT. The INT is operated on the island of La Palma by the
Isaac Newton Group in the Spanish Observatorio del Roque de los
Muchachos of the Instituto de Astrofisica de Canarias. All IPHAS data
are processed by the CASU, at the Institute of Astronomy in Cambridge.
Our work made extensive use of the TOPCAT (Taylor 2005), PYTHON, PYFITS
and POSTGRESQL software tools for data processing. The mosaics were
generated using the MONTAGE software maintained by NASA/IPAC.
NR 106
TC 42
Z9 42
U1 0
U2 3
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 JUL
PY 2011
VL 415
IS 1
BP 103
EP 132
DI 10.1111/j.1365-2966.2011.18674.x
PG 30
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000027
ER
PT J
AU Miller-Jones, JCA
Jonker, PG
Ratti, EM
Torres, MAP
Brocksopp, C
Yang, J
Morrell, NI
AF Miller-Jones, J. C. A.
Jonker, P. G.
Ratti, E. M.
Torres, M. A. P.
Brocksopp, C.
Yang, J.
Morrell, N. I.
TI An accurate position for the black hole candidate XTE J1752-223:
re-interpretation of the VLBI data
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE astrometry; stars: individual: XTE J1752-223; ISM: jets and outflows;
radio continuum: stars; X-rays: binaries
ID CALIBRATOR SURVEY; LARGE-SCALE; JETS; EVOLUTION; STATE; OUTBURST;
BINARIES; DISTANCE; MODEL; EVN
AB Using high-precision astrometric optical observations from the Walter Baade Magellan Telescope in conjunction with high-resolution very long baseline interferometric (VLBI) radio imaging with the Very Long Baseline Array (VLBA), we have located the core of the X-ray binary system XTE J1752-223. Compact radio emission from the core was detected following the state transition from the soft to the hard X-ray state. Its position to the south-east of all previously detected jet components mandated a re-analysis of the existing VLBI data. Our analysis suggests that the outburst comprised at least two ejection events prior to 2010 February 26. No radio-emitting components were detected to the south-east of the core at any epoch, suggesting that the receding jets were Doppler-deboosted below our sensitivity limit. From the ratio of the brightness of the detected components to the measured upper limits for the receding ejecta, we constrain the jet speed beta > 0.66 and the inclination angle to the line of sight theta < 49 degrees. Assuming that the initial ejection event occurred at the transition from the hard intermediate state to the soft intermediate state, an initial period of ballistic motion followed by a Sedov phase (i.e. self-similar adiabatic expansion) appears to fit the motion of the ejecta better than a uniform deceleration model. The accurate core location can provide a long time baseline for a future proper motion determination should the system show a second outburst, providing insights into the formation mechanism of the compact object.
C1 [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia.
[Jonker, P. G.; Ratti, E. M.; Torres, M. A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands.
[Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 AJ Nijmegen, Netherlands.
[Brocksopp, C.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England.
[Yang, J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands.
[Morrell, N. I.] Carnegie Observ, Las Campanas Observ, La Serena, Chile.
RP Miller-Jones, JCA (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia.
EM james.miller-jones@curtin.edu.au
RI Miller-Jones, James/B-2411-2013
OI Miller-Jones, James/0000-0003-3124-2814
FU Netherlands Organization for Scientific Research; Associated
Universities, Inc.
FX PGJ acknowledges support from the Netherlands Organization for
Scientific Research via a VIDI grant. The VLBA is operated by the
National Radio Astronomy Observatory, a facility of the National Science
Foundation operated under cooperative agreement by Associated
Universities, Inc. This paper includes data gathered with the 6.5-m
Magellan Telescopes located at the Las Campanas Observatory, Chile. This
research has made use of NASA's Astrophysics Data System.
NR 37
TC 15
Z9 15
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 JUL
PY 2011
VL 415
IS 1
BP 306
EP 312
DI 10.1111/j.1365-2966.2011.18704.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000044
ER
PT J
AU Kleiser, IKW
Poznanski, D
Kasen, D
Young, TR
Chornock, R
Filippenko, AV
Challis, P
Ganeshalingam, M
Kirshner, RP
Li, WD
Matheson, T
Nugent, PE
Silverman, JM
AF Kleiser, Io K. W.
Poznanski, Dovi
Kasen, Daniel
Young, Timothy R.
Chornock, Ryan
Filippenko, Alexei V.
Challis, Peter
Ganeshalingam, Mohan
Kirshner, Robert P.
Li, Weidong
Matheson, Thomas
Nugent, Peter E.
Silverman, Jeffrey M.
TI Peculiar Type II supernovae from blue supergiants
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE supernovae: general; supernovae: individual: SN 2000cb; supernovae:
individual: SN 1987A; supernovae: individual: SN 2005ci; supernovae:
individual: SN 1998A; supernovae: individual: SN 1999em
ID EXPANDING PHOTOSPHERE METHOD; CORE-COLLAPSE SUPERNOVAE; THEORETICAL
LIGHT-CURVE; P SUPERNOVAE; PLATEAU SUPERNOVAE; OBSERVATIONAL
CONSTRAINTS; UBVRI PHOTOMETRY; MAGELLANIC-CLOUD; IA SUPERNOVAE; MASSIVE
STARS
AB The vast majority of Type II supernovae (SNeII) are produced by red supergiants, but SN 1987A revealed that blue supergiants (BSGs) can produce members of this class as well, albeit with some peculiar properties. This best-studied event revolutionized our understanding of SNe and linking it to the bulk of Type II events is essential. We present here the optical photometry and spectroscopy gathered for SN 2000cb, which is clearly not a standard SNII and yet is not a SN 1987A analogue. The light curve of SN 2000cb is reminiscent of that of SN 1987A in shape, with a slow rise to a late optical peak, but on substantially different time-scales. Spectroscopically, SN 2000cb resembles a normal SNII, but with ejecta velocities that far exceed those measured for SN 1987A or normal SNeII, above 18 000 km s(-1) for H alpha at early times. The red colours, high velocities, late photometric peak and our modelling of this object all point towards a scenario involving the high-energy explosion of a small-radius star, most likely a BSG, producing 0.1 M-circle dot of Ni-56. Adding a similar object to the sample, SN 2005ci, we derive a rate of similar to 2 per cent of the core-collapse rate for this loosely defined class of BSG explosions.
C1 [Kleiser, Io K. W.; Poznanski, Dovi; Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Poznanski, Dovi; Kasen, Daniel; Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
[Kasen, Daniel] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA.
[Young, Timothy R.] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA.
[Chornock, Ryan; Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA.
RP Kleiser, IKW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM io.kleiser@berkeley.edu; dovi@berkeley.edu
FU Einstein Fellowship; US Department of Energy [DE-FG02-06ER06-04]; NSF
[AST-0908886, AST-0907903]; TABASGO Foundation; Sun Microsystems, Inc.;
Hewlett-Packard Company; AutoScope Corporation; Lick Observatory;
University of California; Sylvia & Jim Katzman Foundation
FX We thank Eddie Baron, Luc Dessart, Dan Maoz and the referee (Stephen
Smartt) for useful discussions and comments on this manuscript; Mario
Hamuy and Andrea Pastorello for sharing their data; and the following
for assistance with observations: Zoltan Balog, Perry Berlind, Alison
Coil, Douglas Leonard, Maryam Modjaz and Mark Phillips. DP acknowledges
support from an Einstein Fellowship and from the US Department of Energy
Scientific Discovery through Advanced Computing (SciDAC) programme under
contract DE-FG02-06ER06-04. AVF's SN group at UC Berkeley is supported
by the NSF grant AST-0908886 and by the TABASGO Foundation. The SN
research at the Harvard College Observatory is supported by NSF grant
AST-0907903. The construction and ongoing operation of the KAIT were
made possible by donations from the Sun Microsystems, Inc.,
Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, NSF,
University of California, Sylvia & Jim Katzman Foundation and TABASGO
Foundation. The Kast spectrograph at the Lick Observatory resulted from
a generous donation made by Bill and Marina Kast. We are grateful to the
dedicated staff at the Lick and F. L. Whipple Observatories.
NR 77
TC 32
Z9 32
U1 0
U2 3
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 JUL
PY 2011
VL 415
IS 1
BP 372
EP 382
DI 10.1111/j.1365-2966.2011.18708.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000049
ER
PT J
AU Camera, S
Kitching, TD
Heavens, AF
Bertacca, D
Diaferio, A
AF Camera, Stefano
Kitching, Thomas D.
Heavens, Alan F.
Bertacca, Daniele
Diaferio, Antonaldo
TI Measuring unified dark matter with 3D cosmic shear
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitation; cosmology: observations; cosmology: theory; dark energy;
dark matter; large-scale structure of Universe
ID HUBBLE-SPACE-TELESCOPE; K-ESSENCE; MICROWAVE-ANISOTROPY; POWER SPECTRA;
COSMOLOGICAL PARAMETERS; MODEL SELECTION; SCALAR FIELD; ENERGY;
CONSTRAINTS; QUINTESSENCE
AB We present parameter estimation forecasts for future 3D cosmic shear surveys for a class of Unified Dark Matter (UDM) models, where a single scalar field mimics both Dark Matter (DM) and Dark Energy (DE). These models have the advantage that they can describe the dynamics of the Universe with a single matter component providing an explanation for structure formation and cosmic acceleration. A crucial feature of the class of UDM models we use in this work is characterized by a parameter, c(infinity) (in units of the speed of light c = 1), that is the value of the sound speed at late times, and on which structure formation depends. We demonstrate that the properties of the DM-like behaviour of the scalar field can be estimated with very high precision with large-scale, fully 3D weak lensing surveys. We found that 3D weak lensing significantly constrains c(infinity), and we find minimal errors Delta c(infinity) = 3.0 x 10(-5), for the fiducial value c(infinity) = 1.0 x 10(-3) and Delta c(infinity) = 2.6 x 10(-5), for c(infinity) = 1.2 x 10(-2). Moreover, we compute the Bayesian evidence for UDM models over the Lambda CDM model as a function of c(infinity). For this purpose, we can consider the Lambda CDM model as a UDM model with c(infinity) = 0. We find that the expected evidence clearly shows that the survey data would unquestionably favour UDM models over the Lambda CDM model, for the values c(infinity) greater than or similar to 10(-3).
C1 [Camera, Stefano; Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, I-10125 Turin, Italy.
[Camera, Stefano] Univ Turin, Dipartimento Fis Teor, I-10125 Turin, Italy.
[Camera, Stefano; Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy.
[Kitching, Thomas D.; Heavens, Alan F.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland.
[Bertacca, Daniele] Univ Padua, Dipartimento Fis Galileo Galilei, I-35131 Padua, Italy.
[Bertacca, Daniele] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy.
[Bertacca, Daniele] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England.
[Diaferio, Antonaldo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Camera, S (reprint author), Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Via P Giuria 1, I-10125 Turin, Italy.
EM camera@ph.unito.it; tdk@roe.ac.uk; afh@roe.ac.uk; bertacca@pd.infn.it;
diaferio@ph.unito.it
RI Camera, Stefano/N-2456-2013;
OI Camera, Stefano/0000-0003-3399-3574; Bertacca,
Daniele/0000-0002-2490-7139
FU INFN [PD51]; Ministero dell'Istruzione, dell'Universita e della Ricerca
(MIUR); Universita di Torino; Istituto Nazionale di Fisica Nucleare
(MIUR) [PRIN 2008NR3EBK]; STFC [RA0888]; Fondazione Ing. Aldo Gini; ASI
[I/016/07/0]
FX We thank the referee for her/his useful comments which contributed to
remove some ambiguities in the presentation of our results. SC and AD
gratefully acknowledge partial support from the INFN grant PD51. SC
acknowledges Research Grants funded jointly by Ministero
dell'Istruzione, dell'Universita e della Ricerca (MIUR), by Universita
di Torino and by Istituto Nazionale di Fisica Nucleare within the
Astroparticle Physics Project (MIUR contract number: PRIN 2008NR3EBK).
SC also acknowledges partial support from the Institute for Astronomy,
University of Edinburgh and thanks it for the hospitality. TDK is
supported by the STFC Rolling Grant number RA0888. DB would like to
acknowledge the ICG Portsmouth for the hospitality during the
development of this project and the 'Fondazione Ing. Aldo Gini' for
support. DB research has been partly supported by ASI contract
I/016/07/0 'COFIS'.
NR 92
TC 13
Z9 13
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
PY 2011
VL 415
IS 1
BP 399
EP 409
DI 10.1111/j.1365-2966.2011.18712.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000051
ER
PT J
AU Nardini, E
Risaliti, G
AF Nardini, E.
Risaliti, G.
TI Compton-thick active galactic nuclei inside local ultraluminous infrared
galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies: active; galaxies: starburst; infrared: galaxies; X-rays:
galaxies
ID MU-M SPECTROSCOPY; SPECTRAL ENERGY-DISTRIBUTIONS; INTERSTELLAR
EXTINCTION LAW; SPITZER-SPACE-TELESCOPE; X-RAY SURVEY; XMM-NEWTON; IRAS
GALAXIES; BLACK-HOLES; SPECTROGRAPH IRS; ULIRG EVOLUTION
AB We present an X-ray analysis of the most luminous obscured active galactic nuclei (AGN) inside local ultraluminous infrared galaxies (ULIRGs). Our sample consists of 10 sources, harbouring AGN components with estimated luminosity in excess of similar to 10(12) L-circle dot and yet unidentified at optical wavelengths because of their large obscuration. According to the Chandra and XMM-Newton spectra, only in two cases out of 10 are clear AGN signatures detected at 2-10 keV in the shape of reflected emission. The X-ray flux from the starburst (SB) components, instead, is always broadly consistent with expectations based on their IR emission. The most convincing explanation for the missing AGN detections is therefore the Compton-thickness of the X-ray absorber. In general, the combination of our mid-IR and X-ray spectral analysis suggests that the environment surrounding the AGN component in ULIRGs is much richer in gas and dust than in ordinary active galaxies, and the degree of AGN absorption can be tentatively related to the starburst intensity, indicating a strong interaction between the two processes and supporting the ULIRG/quasar evolutionary scheme.
C1 [Nardini, E.] Univ Florence, Dipartimento Fis & Astron, Sez Astron, I-50125 Florence, Italy.
[Nardini, E.; Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
[Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Nardini, E (reprint author), Univ Florence, Dipartimento Fis & Astron, Sez Astron, Lgo E Fermi 2, I-50125 Florence, Italy.
EM nardini@arcetri.astro.it
OI Risaliti, Guido/0000-0002-3556-977X
FU NASA [NNX09AT10G, GO0-11017X]
FX This research has been partially supported by NASA grants NNX09AT10G and
GO0-11017X. We thank the anonymous referee for his/her constructive
comments which improved our work.
NR 67
TC 11
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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 JUL
PY 2011
VL 415
IS 1
BP 619
EP 628
DI 10.1111/j.1365-2966.2011.18732.x
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000070
ER
PT J
AU Steinhardt, CL
Elvis, M
Amarie, M
AF Steinhardt, Charles L.
Elvis, Martin
Amarie, Mihail
TI Evolutionary tracks of individual quasars in the mass-luminosity plane
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; black hole physics; galaxies: evolution;
galaxies: nuclei; quasars: general
ID BLACK-HOLE MASSES; ACTIVE GALACTIC NUCLEI; EDDINGTON RATIO; MODELS; SDSS
AB Previous work on the quasar mass-luminosity plane indicates the possibility that quasars of the same central black hole mass might follow a common evolutionary track, independent of the properties of the host galaxy. We consider two simple models for the evolution of individual quasars. Requiring these tracks to lie within the observed quasar locus at all redshifts strongly constrains the model parameters, but does allow some solutions. These solutions include a family of tracks with similar shape but different initial masses that might match the observed quasar distributions at all redshifts z < 2.0. This family of solutions is characterized by short (1-2 Gyr) lifetimes, a duty cycle in which the quasar is on at least 25 per cent of the time, and a rapid decline in Eddington ratio, perhaps with L(Edd) alpha t(-6) or steeper.
C1 [Steinhardt, Charles L.] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778583, Japan.
[Steinhardt, Charles L.; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Amarie, Mihail] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA.
RP Steinhardt, CL (reprint author), Univ Tokyo, Inst Phys & Math Universe, Kashiwanoha 5-1-5, Chiba 2778583, Japan.
EM charles.steinhardt@ipmu.jp
FU [G07-8136A]
FX The authors would like to thank Lars Hernquist and Norm Murray for
valuable comments. This work was supported in part by Chandra grant no.
G07-8136A.
NR 18
TC 3
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U1 0
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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 JUL
PY 2011
VL 415
IS 1
BP 732
EP 740
DI 10.1111/j.1365-2966.2011.18750.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000080
ER
PT J
AU McQuinn, M
Hernquist, L
Lidz, A
Zaldarriaga, M
AF McQuinn, Matthew
Hernquist, Lars
Lidz, Adam
Zaldarriaga, Matias
TI The signatures of large-scale temperature and intensity fluctuations in
the Lyman alpha forest
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE intergalactic medium; quasars: absorption lines; cosmology: theory;
large-scale structure of Universe
ID EQUATION-OF-STATE; PROBABILITY-DISTRIBUTION FUNCTION; INTERGALACTIC
MEDIUM-TEMPERATURE; IONIZING-RADIATION FLUCTUATIONS; HE II REIONIZATION;
DARK-MATTER MODEL; POWER SPECTRUM; DENSITY RELATION; HELIUM
REIONIZATION; FLUX DISTRIBUTION
AB It appears inevitable that reionization processes would have produced large-scale temperature fluctuations in the intergalactic medium. Using toy temperature models and detailed heating histories from cosmological simulations of He II reionization, we study the consequences of inhomogeneous heating for the Ly alpha forest. The impact of temperature fluctuations in physically well-motivated models can be surprisingly subtle. In fact, we show that temperature fluctuations at the level predicted by our reionization simulations do not give rise to detectable signatures in the types of statistics that have been employed previously. However, because of the aliasing of small-scale density power to larger scale modes in the line-of-sight Ly alpha forest power spectrum, earlier analyses were not sensitive to 3D modes with greater than or similar to 30 comoving Mpc wavelengths - scales where temperature fluctuations are likely to be relatively largest. The ongoing Baryon Oscillation Spectroscopic Survey ( BOSS) aims to measure the 3D power spectrum of the Ly alpha forest, P-F, from a large sample of quasars in order to avoid this aliasing. We find that physically motivated temperature models can alter P-F at an order unity level at k less than or similar to 0.1 comoving Mpc(-1), a magnitude that should be easily detectable with BOSS. Fluctuations in the intensity of the ultraviolet background can also alter P-F significantly. These signatures will make it possible for BOSS to study the thermal impact of He II reionization at 2 < z < 3 and to constrain models for the sources of the ionizing background. Future spectroscopic surveys could extend this measurement to even higher redshifts, potentially detecting the thermal imprint of hydrogen reionization.
C1 [McQuinn, Matthew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lidz, Adam] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
[Zaldarriaga, Matias] Inst Adv Study, Princeton, NJ 08540 USA.
RP McQuinn, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM mmcquinn@berkeley.edu
FU NASA
FX We would like to thank Steven Furlanetto, Shirley Ho, Avi Loeb and Nic
Ross for useful discussions, and Martin White for useful comments on the
manuscript. We thank Claude-Andre Faucher-Giguere for providing the
hydrodynamic simulations used in some of our calculations. MM is
supported by the NASA Einstein Fellowship.
NR 66
TC 23
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U1 0
U2 3
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUL
PY 2011
VL 415
IS 1
BP 977
EP 992
DI 10.1111/j.1365-2966.2011.18788.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 805UR
UT WOS:000293755000098
ER
PT J
AU Neufeld, MJ
AF Neufeld, Michael J.
TI Physics and Politics: Research and Research Support in Twentieth-Century
Germany in International Perspective.
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA.
RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
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 2011
VL 52
IS 3
BP 649
EP 650
PG 2
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 806KM
UT WOS:000293806400027
ER
PT J
AU Ashley, JW
Golombek, MP
Christensen, PR
Squyres, SW
McCoy, TJ
Schroder, C
Fleischer, I
Johnson, JR
Herkenhoff, KE
Parker, TJ
AF Ashley, J. W.
Golombek, M. P.
Christensen, P. R.
Squyres, S. W.
McCoy, T. J.
Schroeder, C.
Fleischer, I.
Johnson, J. R.
Herkenhoff, K. E.
Parker, T. J.
TI POST-FALL SURFACE MODIFICATION FEATURES OF IRON METEORITES FOUND BY THE
OPPORTUNITY ROVER AND THEIR IMPLICATIONS FOR MARTIAN WEATHERING
PROCESSES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbH, Royal Observ Greenwich
C1 [Ashley, J. W.; Christensen, P. R.] Arizona State Univ, Mars Space Flight Facil, Tempe, AZ 85287 USA.
[Golombek, M. P.; Parker, T. J.] CALTECH, Jet Prop Lab, Pasadena, CA USA.
[Squyres, S. W.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
[McCoy, T. J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Schroeder, C.] Univ Tubingen, Ctr Appl Geosci, Tubingen, Germany.
[Fleischer, I.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, Mainz, Germany.
[Johnson, J. R.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA.
EM james.ashley@ser.asu.edu
RI Johnson, Jeffrey/F-3972-2015; Schroder, Christian/B-3870-2009
OI Schroder, Christian/0000-0002-7935-6039
NR 3
TC 0
Z9 0
U1 1
U2 1
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2011
VL 46
SU 1
SI SI
BP A13
EP A13
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700022
ER
PT J
AU Bullock, ES
MacPherson, GJ
Krot, AN
Nagashima, K
Ushikubo, T
Kita, NT
AF Bullock, E. S.
MacPherson, G. J.
Krot, A. N.
Nagashima, K.
Ushikubo, T.
Kita, N. T.
TI OXYGEN ISOTOPES IN PYROXENES FROM TWO VIGARANO CAIs VARY INDEPENDENTLY
OF fO(2)
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbH, Royal Observ Greenwich
C1 [Bullock, E. S.] US Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[MacPherson, G. J.; Krot, A. N.; Nagashima, K.] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
[Ushikubo, T.; Kita, N. T.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA.
EM BullockE@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 2011
VL 46
SU 1
SI SI
BP A33
EP A33
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700062
ER
PT J
AU Corrigan, CM
McSween, HY
Scott, ERD
AF Corrigan, C. M.
McSween, H. Y., Jr.
Scott, E. R. D.
TI ELEMENTS MAGAZINE: A NEW FORM OF OUTREACH FOR THE METEORITICAL SOCIETY
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Corrigan, C. M.] Smithsonian Inst, NMNH, Washington, DC 20560 USA.
[McSween, H. Y., Jr.] Univ Tennessee, Knoxville, TN USA.
[Scott, E. R. D.] Univ Hawaii Manoa, HIGP, Honolulu, HI 96822 USA.
EM corriganc@si.edu
NR 13
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 2011
VL 46
SU 1
SI SI
BP A49
EP A49
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700094
ER
PT J
AU Corrigan, CM
Clarke, RS
Plotkin, H
McCoy, TJ
AF Corrigan, C. M.
Clarke, R. S., Jr.
Plotkin, H.
McCoy, T. J.
TI THE OLD WOMAN, CALIFORNIA, METEORITE
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Corrigan, C. M.; Clarke, R. S., Jr.; McCoy, T. J.] Smithsonian Inst, NMNH, Washington, DC 20013 USA.
[Plotkin, H.] Univ Western Ontario, London, ON, Canada.
EM corriganc@si.edu
NR 3
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 2011
VL 46
SU 1
SI SI
BP A48
EP A48
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700093
ER
PT J
AU Herd, CDK
Smith, CL
Grossman, JN
Weisberg, MK
Welzenbach, L
AF Herd, C. D. K.
Smith, C. L.
Grossman, J. N.
Weisberg, M. K.
Welzenbach, L.
TI NOMCOM REVIEW OF TYPE SPECIMEN REPOSITORIES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Herd, C. D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada.
[Smith, C. L.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England.
[Grossman, J. N.] NASA Headquarters, Washington, DC 20546 USA.
[Weisberg, M. K.] CUNY, Kingsborough Coll, Brooklyn, NY 11235 USA.
[Welzenbach, L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
EM herd@ualberta.ca
NR 1
TC 0
Z9 0
U1 0
U2 1
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 2011
VL 46
SU 1
SI SI
BP A92
EP A92
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700181
ER
PT J
AU Ivanova, MA
Krot, AN
Nagashima, K
MacPherson, GJ
AF Ivanova, M. A.
Krot, A. N.
Nagashima, K.
MacPherson, G. J.
TI FORMATION OF REFRACTORY INCLUSIONS FROM O-16-RICH AND O-16-POOR SOLIDS:
EVIDENCE FROM COMPLEX CAIS IN CV CHONDRITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbH, Royal Observ Greenwich
C1 [Ivanova, M. A.] Vernadsky Inst Geochem, Moscow 119991, Russia.
[Ivanova, M. A.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA.
[Krot, A. N.; Nagashima, K.] Univ Hawaii Manoa, Honolulu, HI 96822 USA.
EM meteorite2000@mail.ru
NR 6
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 2011
VL 46
SU 1
SI SI
BP A110
EP A110
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700217
ER
PT J
AU Marin-Carbonne, J
McKeegan, KD
Davis, AM
MacPherson, GJ
Mendybaev, RA
Richter, FM
AF Marin-Carbonne, J.
McKeegan, K. D.
Davis, A. M.
MacPherson, G. J.
Mendybaev, R. A.
Richter, F. M.
TI Mg AND Si ISOTOPIC COMPOSITIONS OF VIGARANO FUN INCLUSION 1623-5
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
ID EVAPORATION
C1 [Marin-Carbonne, J.; McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA.
[Davis, A. M.; Mendybaev, R. A.; Richter, F. M.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA.
[Davis, A. M.; Mendybaev, R. A.; Richter, F. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA.
[MacPherson, G. J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM jmarin@ess.ucla.edu
RI Marin-Carbonne, Johanna/E-5068-2015
OI Marin-Carbonne, Johanna/0000-0002-4265-1595
NR 6
TC 0
Z9 0
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 2011
VL 46
SU 1
SI SI
BP A147
EP A147
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700291
ER
PT J
AU Peplowski, PN
Hamara, DK
Lawrence, DJ
McCoy, TJ
Boynton, WV
Evans, LG
Rhodes, EA
Solomon, SC
Nittler, LR
Sprague, AL
AF Peplowski, P. N.
Hamara, D. K.
Lawrence, D. J.
McCoy, T. J.
Boynton, W. V.
Evans, L. G.
Rhodes, E. A.
Solomon, S. C.
Nittler, L. R.
Sprague, A. L.
TI ABUNDANCES OF RADIOACTIVE ELEMENTS ON THE SURFACE OF MERCURY: FIRST
RESULTS FROM THE MESSENGER GAMMA-RAY SPECTROMETER
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Peplowski, P. N.; Lawrence, D. J.; Rhodes, E. A.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[Hamara, D. K.; Boynton, W. V.; Sprague, A. L.] Univ Arizona, Tucson, AZ 85721 USA.
[McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA.
[Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Solomon, S. C.; Nittler, L. R.] Carnegie Inst Washington, Washington, DC 20015 USA.
RI Evans, Larry/F-7462-2012; Peplowski, Patrick/I-7254-2012; Lawrence,
David/E-7463-2015
OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence,
David/0000-0002-7696-6667
NR 5
TC 0
Z9 0
U1 0
U2 3
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 2011
VL 46
SU 1
SI SI
BP A185
EP A185
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700367
ER
PT J
AU Smith, SE
Mayne, RG
Corrigan, CM
AF Smith, S. E.
Mayne, R. G.
Corrigan, C. M.
TI USING PETROLOGY AND MINERALOGY TO UNDERSTAND THE SURFACE OF VESTA: A
COLLECTION OF FINE-GRAINED EUCRITES
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Smith, S. E.; Mayne, R. G.] Texas Christian Univ, Sch Geol Energy & Environm, Ft Worth, TX 76109 USA.
[Corrigan, C. M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM samantha.e.smith@tcu.edu
NR 3
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 2011
VL 46
SU 1
SI SI
BP A216
EP A216
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700428
ER
PT J
AU Weider, SZ
Nittler, LR
Starr, RD
Boynton, WV
Evans, LG
Goldsten, JO
McCoy, TJ
McNutt, RL
Schlemm, CE
Solomon, SC
Sprague, AL
AF Weider, S. Z.
Nittler, L. R.
Starr, R. D.
Boynton, W. V.
Evans, L. G.
Goldsten, J. O.
McCoy, T. J.
McNutt, R. L., Jr.
Schlemm, C. E., II
Solomon, S. C.
Sprague, A. L.
TI MAJOR-ELEMENT ABUNDANCES OF SURFACE MATERIALS ON MERCURY: FIRST RESULTS
FROM THE MESSENGER X-RAY SPECTROMETER
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
C1 [Weider, S. Z.; Nittler, L. R.; Solomon, S. C.] Carnegie Inst Washington, Washington, DC 20015 USA.
[Starr, R. D.] Catholic Univ, Washington, DC 20064 USA.
[Boynton, W. V.; Sprague, A. L.] Univ Arizona, Tucson, AZ 85721 USA.
[Evans, L. G.] Comp Sci Corp, Lanham, MD 20706 USA.
[Goldsten, J. O.; McNutt, R. L., Jr.; Schlemm, C. E., II] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA.
[McCoy, T. J.] Smithsonian Inst, Washington, DC 20013 USA.
EM sweider@ciw.edu
RI Evans, Larry/F-7462-2012; McNutt, Ralph/E-8006-2010
OI McNutt, Ralph/0000-0002-4722-9166
NR 7
TC 0
Z9 0
U1 0
U2 1
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 2011
VL 46
SU 1
SI SI
BP A248
EP A248
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700493
ER
PT J
AU Williams, CD
Wadhwa, M
Janney, PE
Hines, RR
Bullock, ES
MacPherson, GJ
AF Williams, C. D.
Wadhwa, M.
Janney, P. E.
Hines, R. R.
Bullock, E. S.
MacPherson, G. J.
TI ANALYSIS OF TITANIUM ISOTOPE RATIOS IN REFRACTORY INCLUSIONS BY
LA-MC-ICP-MS
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Meeting Abstract
CT 74th Annual Meeting of the Meteoritical-Society
CY AUG 08-12, 2011
CL London, ENGLAND
SP Meteorit Soc, Nat Hist Museum, Imperial Coll, Lunar & Planetary Inst, Natl Aeronaut & Space Adm, European Space Agcy, Barringer Crater Co, CAMECA Instruments, Bruker Nano GmbH, CEPSAR - Open Univ, Univ Leicester, Space Res Ctr, Univ Glasgow, Cambridge Univ Press, Sci (AAAS), WiTec GmbII, Royal Observ Greenwich
ID ANOMALIES; TI
C1 [Williams, C. D.; Wadhwa, M.; Janney, P. E.; Hines, R. R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA.
[Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, US Natl Museum Nat Hist, Washington, DC 20560 USA.
EM Curtis.Williams@asu.edu
RI Janney, Philip/K-2733-2013
OI Janney, Philip/0000-0001-5740-4266
NR 3
TC 0
Z9 0
U1 0
U2 1
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 2011
VL 46
SU 1
SI SI
BP A250
EP A250
PG 1
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 797AN
UT WOS:000293094700496
ER
PT J
AU Levin, NE
Brown, FH
Behrensmeyer, AK
Bobe, R
Cerling, TE
AF Levin, Naomi E.
Brown, Francis H.
Behrensmeyer, Anna K.
Bobe, Rene
Cerling, Thure E.
TI Paleosol carbonates from the Omo Group: Isotopic records of local and
regional environmental change in East Africa
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Pedogenic carbonate; Omo-Turkana Basin; East Africa; Pleistocene;
Pliocene; Carbon isotopes; Oxygen isotopes
ID KOOBI-FORA-FORMATION; TURKANA-BASIN; PEDOGENIC CARBONATE;
STABLE-ISOTOPES; HADAR FORMATION; HUMAN-EVOLUTION; NORTHERN KENYA;
HOMO-ERECTUS; PALEOENVIRONMENTAL INTERPRETATION;
DEPOSITIONAL-ENVIRONMENTS
AB Pliocene and Pleistocene sedimentary rocks from the Omo-Turkana Basin in East Africa are well known for fossil and archeological evidence of human evolution and provide a unique opportunity to study four million years of environmental change in a rift basin. This study uses carbon and oxygen isotope ratios of pedogenic carbonates to examine environmental variability across similar to 5000 km(2) within the Omo-Turkana Basin. An expanded isotopic dataset, including the first isotopic data on pedogenic carbonates from the Shungura Formation and new data from the Nachukui and Koobi Fora formations, is compared to published isotopic records from both the Omo-Turkana Basin and the lower Awash Basin, Ethiopia. Regionally, the carbon isotope record indicates a steady increase of C(4) vegetation in floodplain environments for the past 4 million years. The oxygen isotopic record indicates that the isotopic composition of rainfall was depleted in (18)O relative to today's waters and that both basins likely received more rainfall in the Pliocene than today. A shift to higher delta(18)O values in paleosol carbonate after 2 Ma in the Omo-Turkana Basin but not in the lower Awash Basin suggests that the ecology and hydrology in these two rift basins were influenced by different climatic regimes. In addition to regional trends, pedogenic carbonates sampled from different parts of the basin show that the distribution of C(4) vegetation and soil water delta(18)O values varied with proximity to the axial river system, and specifically that C(3) vegetation was more dominant in soils of the Shungura Formation compared with coeval sediments downstream in the Nachukui and Koobi Fora formations. This large isotopic dataset from pedogenic carbonates provides the opportunity to examine how terrestrial systems responded to global climate change during the last 4 million years, from both local and regional perspectives. The isotopic data indicate that local basin and climate dynamics strongly influenced the impact of large-scale environmental change in East African rift basins. 2011 Elsevier B.V. All rights reserved.
C1 [Levin, Naomi E.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA.
[Levin, Naomi E.; Brown, Francis H.; Cerling, Thure E.] Univ Utah, Dept Geol & Geophys, Salt Lake City, UT 84112 USA.
[Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Bobe, Rene] Univ Georgia, Dept Anthropol, Athens, GA 30602 USA.
RP Levin, NE (reprint author), Johns Hopkins Univ, Dept Earth & Planetary Sci, 3400 N Charles St,301 Olin Hall, Baltimore, MD 21218 USA.
EM nlevin3@jhu.edu
RI Levin, Naomi/B-4124-2010;
OI Levin, Naomi/0000-0001-5703-3717; Bobe, Rene/0000-0001-9059-2203
FU International Association of Sedimentologists; Leakey Foundation;
National Science Foundation [BCS0621542]
FX We thank Patrick Gathogo, Getachew Eshete, Tesfaye Kidane, and Kevin Uno
for their help in the field, and Kevin Uno and David Dettman for help in
the laboratory. Collection of samples from the Koobi Fora Formation was
in collaboration with David Braun, Christopher Campisano and Jack
Harris. We thank Jonathan Wynn and Rhonda Quinn for providing their
published data in tabulated form. The National Museums of Kenya were
critical for the export of samples. We thank Jay Quade for discussions
that sparked many of the ideas and data presented here. We are also
grateful to David Fox and an anonymous reviewer for their constructive
comments that improved the manuscript. This research was funded with
grants from the International Association of Sedimentologists, the
Leakey Foundation, and the National Science Foundation (BCS0621542).
NR 97
TC 49
Z9 49
U1 3
U2 32
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 JUL 1
PY 2011
VL 307
IS 1-4
BP 75
EP 89
DI 10.1016/j.palaeo.2011.04.026
PG 15
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 801FR
UT WOS:000293424300005
ER
PT J
AU Hearty, PJ
Olson, SL
AF Hearty, Paul J.
Olson, Storrs L.
TI PRESERVATION OF TRACE FOSSILS AND MOLDS OF TERRESTRIAL BIOTA BY INTENSE
STORMS IN MID-LAST INTERGLACIAL (MIS 5c) DUNES ON BERMUDA, WITH A MODEL
FOR DEVELOPMENT OF HYDROLOGICAL CONDUITS
SO PALAIOS
LA English
DT Article
ID SEA-LEVEL HIGHSTAND; SEDIMENTARY EVIDENCE; WESTERN-AUSTRALIA; ELEUTHERA
ISLAND; QUATERNARY; GEOCHRONOLOGY; STRATIGRAPHY; BAHAMAS; GEOLOGY;
HISTORY
AB We document massive deposition of carbonate sands along the south shore of Bermuda that were emplaced during one or two great storms during the last interglacial. As determined by their stratigraphic position and geochronological data, these deposits formed during marine isotope substage (MIS) 5c ca. 100 ka ago. Within a leeward set of eolian beds, evidence of a living landscape was preserved that includes delicate footprints of a shorebird (Scolopacidae, Catoptrophorus) preserved in frothy dune foreset beds. In the same stratigraphic unit, outlines of a standing forest of palm trees (Sabal bermudana), some evidently with fronds in place, were molded in the fine carbonate dune sand. All available evidence points to an MIS 5c sea level positioned several meters below the present datum, which would require great intensity of storms to transport such voluminous deposits well above present sea level. Waves and storm currents transported loose sediments from the shallow shelf onto the shore, where hurricane winds piled up sand sufficiently deep to bury established forests of 8- to 10-m-tall trees. Evidence of such powerful storms preserved in the rock record is a measure of the intensity of past hurricanes, and a possible bellwether of future storm events. Entombment of the trees involved rapid burial and cementation creating external molds in limestone, a process that is important in the development of vertical hydrological conduits commonly observed in eolianites.
C1 [Hearty, Paul J.] Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA.
[Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.
RP Hearty, PJ (reprint author), Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA.
EM heartyp@uncw.edu
NR 52
TC 8
Z9 8
U1 0
U2 2
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 JUL-AUG
PY 2011
VL 26
IS 7-8
BP 394
EP 405
DI 10.2110/palo.2010.p10-132r
PG 12
WC Geology; Paleontology
SC Geology; Paleontology
GA 797JL
UT WOS:000293120200002
ER
PT J
AU Neuhauser, R
Errmann, R
Berndt, A
Maciejewski, G
Takahashi, H
Chen, WP
Dimitrov, DP
Pribulla, T
Nikogossian, EH
Jensen, ELN
Marschall, L
Wu, ZY
Kellerer, A
Walter, FM
Briceno, C
Chini, R
Fernandez, M
Raetz, S
Torres, G
Latham, DW
Quinn, SN
Niedzielski, A
Bukowiecki, L
Nowak, G
Tomov, T
Tachihara, K
Hu, SCL
Hung, LW
Kjurkchieva, DP
Radeva, VS
Mihov, BM
Slavcheva-Mihova, L
Bozhinova, IN
Budaj, J
Vanko, M
Kundra, E
Hambalek, L
Krushevska, V
Movsessian, T
Harutyunyan, H
Downes, JJ
Hernandez, J
Hoffmeister, VH
Cohen, DH
Abel, I
Ahmad, R
Chapman, S
Eckert, S
Goodman, J
Guerard, A
Kim, HM
Koontharana, A
Sokol, J
Trinh, J
Wang, Y
Zhou, X
Redmer, R
Kramm, U
Nettelmann, N
Mugrauer, M
Schmidt, J
Moualla, M
Ginski, C
Marka, C
Adam, C
Seeliger, M
Baar, S
Roell, T
Schmidt, TOB
Trepl, L
Eisenbeiss, T
Fiedler, S
Tetzlaff, N
Schmidt, E
Hohle, MM
Kitze, M
Chakrova, N
Grafe, C
Schreyer, K
Hambaryan, VV
Broeg, CH
Koppenhoefer, J
Pandey, AK
AF Neuhaeuser, R.
Errmann, R.
Berndt, A.
Maciejewski, G.
Takahashi, H.
Chen, W. P.
Dimitrov, D. P.
Pribulla, T.
Nikogossian, E. H.
Jensen, E. L. N.
Marschall, L.
Wu, Z. -Y.
Kellerer, A.
Walter, F. M.
Briceno, C.
Chini, R.
Fernandez, M.
Raetz, St
Torres, G.
Latham, D. W.
Quinn, S. N.
Niedzielski, A.
Bukowiecki, L.
Nowak, G.
Tomov, T.
Tachihara, K.
Hu, S. C. -L.
Hung, L. W.
Kjurkchieva, D. P.
Radeva, V. S.
Mihov, B. M.
Slavcheva-Mihova, L.
Bozhinova, I. N.
Budaj, J.
Vanko, M.
Kundra, E.
Hambalek, L.
Krushevska, V.
Movsessian, T.
Harutyunyan, H.
Downes, J. J.
Hernandez, J.
Hoffmeister, V. H.
Cohen, D. H.
Abel, I.
Ahmad, R.
Chapman, S.
Eckert, S.
Goodman, J.
Guerard, A.
Kim, H. M.
Koontharana, A.
Sokol, J.
Trinh, J.
Wang, Y.
Zhou, X.
Redmer, R.
Kramm, U.
Nettelmann, N.
Mugrauer, M.
Schmidt, J.
Moualla, M.
Ginski, C.
Marka, C.
Adam, C.
Seeliger, M.
Baar, S.
Roell, T.
Schmidt, T. O. B.
Trepl, L.
Eisenbeiss, T.
Fiedler, S.
Tetzlaff, N.
Schmidt, E.
Hohle, M. M.
Kitze, M.
Chakrova, N.
Graefe, C.
Schreyer, K.
Hambaryan, V. V.
Broeg, C. H.
Koppenhoefer, J.
Pandey, A. K.
TI The Young Exoplanet Transit Initiative (YETI)
SO ASTRONOMISCHE NACHRICHTEN
LA English
DT Article
DE planetary systems; surveys; techniques: photometric; techniques:
spectroscopic
ID LOW-MASS STARS; UNIVERSITY OBSERVATORY JENA; EXTRASOLAR GIANT PLANETS;
SUB-STELLAR COMPANION; MONITOR PROJECT; BROWN DWARFS; HR 8799; OPEN
CLUSTERS; CEPHEUS OB2; CCD CAMERA
AB We present the Young Exoplanet Transit Initiative (YETI), in which we use several 0.2 to 2.6-m telescopes around the world to monitor continuously young (<= 100 Myr), nearby (<= 1 kpc) stellar clusters mainly to detect young transiting planets (and to study other variability phenomena on time-scales from minutes to years). The telescope network enables us to observe the targets continuously for several days in order not to miss any transit. The runs are typically one to two weeks long, about three runs per year per cluster in two or three subsequent years for about ten clusters. There are thousands of stars detectable in each field with several hundred known cluster members, e. g. in the first cluster observed, Tr-37, a typical cluster for the YETI survey, there are at least 469 known young stars detected in YETI data down to R = 16.5 mag with sufficient precision of 50 millimag rms (5 mmag rms down to R = 14.5 mag) to detect transits, so that we can expect at least about one young transiting object in this cluster. If we observe similar to 10 similar clusters, we can expect to detect similar to 10 young transiting planets with radius determinations. The precision given above is for a typical telescope of the YETI network, namely the 60/90-cm Jena telescope (similar brightness limit, namely within +/-1 mag, for the others) so that planetary transits can be detected. For targets with a periodic transit-like light curve, we obtain spectroscopy to ensure that the star is young and that the transiting object can be sub-stellar; then, we obtain Adaptive Optics infrared images and spectra, to exclude other bright eclipsing stars in the (larger) optical PSF; we carry out other observations as needed to rule out other false positive scenarios; finally, we also perform spectroscopy to determine the mass of the transiting companion. For planets with mass and radius determinations, we can calculate the mean density and probe the internal structure. We aim to constrain planet formation models and their time-scales by discovering planets younger than similar to 100 Myr and determining not only their orbital parameters, but also measuring their true masses and radii, which is possible so far only by the transit method. Here, we present an overview and first results. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim
C1 [Neuhaeuser, R.; Errmann, R.; Berndt, A.; Maciejewski, G.; Pribulla, T.; Raetz, St; Mugrauer, M.; Schmidt, J.; Moualla, M.; Ginski, C.; Marka, C.; Adam, C.; Seeliger, M.; Baar, S.; Roell, T.; Schmidt, T. O. B.; Trepl, L.; Eisenbeiss, T.; Fiedler, S.; Tetzlaff, N.; Schmidt, E.; Hohle, M. M.; Kitze, M.; Graefe, C.; Schreyer, K.; Hambaryan, V. V.] Inst Astrophys, D-07745 Jena, Germany.
[Neuhaeuser, R.; Errmann, R.; Berndt, A.; Maciejewski, G.; Pribulla, T.; Raetz, St; Mugrauer, M.; Schmidt, J.; Moualla, M.; Ginski, C.; Marka, C.; Adam, C.; Seeliger, M.; Baar, S.; Roell, T.; Schmidt, T. O. B.; Trepl, L.; Eisenbeiss, T.; Fiedler, S.; Tetzlaff, N.; Schmidt, E.; Hohle, M. M.; Kitze, M.; Graefe, C.; Schreyer, K.; Hambaryan, V. V.] Univ Sternwarte, FSU Jena, D-07745 Jena, Germany.
[Maciejewski, G.; Niedzielski, A.; Bukowiecki, L.; Nowak, G.; Tomov, T.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland.
[Takahashi, H.] Gunma Astron Observ, Takayama, Gunma 3770702, Japan.
[Chen, W. P.; Hu, S. C. -L.; Hung, L. W.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan.
[Dimitrov, D. P.; Mihov, B. M.; Slavcheva-Mihova, L.; Bozhinova, I. N.] Bulg Acad Sc, Inst Astron, Sofia 1784, Bulgaria.
[Pribulla, T.; Budaj, J.; Vanko, M.; Kundra, E.; Hambalek, L.; Krushevska, V.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia.
[Nikogossian, E. H.; Movsessian, T.; Harutyunyan, H.] Byurakan Astrophys Observ, Byurakan 378433, Armenia.
[Jensen, E. L. N.; Cohen, D. H.; Abel, I.; Ahmad, R.; Chapman, S.; Eckert, S.; Goodman, J.; Guerard, A.; Kim, H. M.; Koontharana, A.; Sokol, J.; Trinh, J.; Wang, Y.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA.
[Marschall, L.] Gettysburg Coll Observ, Dept Phys, Gettysburg, PA 17325 USA.
[Wu, Z. -Y.; Zhou, X.] Chinese Acad Sci, Key Lab Opt Astron, NAO, Beijing 100012, Peoples R China.
[Dimitrov, D. P.; Mihov, B. M.; Slavcheva-Mihova, L.; Bozhinova, I. N.] Bulg Acad Sc, NAO, Sofia 1784, Bulgaria.
[Kellerer, A.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
[Kellerer, A.] Big Bear Solar Observ, Big Bear City, CA 92314 USA.
[Walter, F. M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
[Briceno, C.; Downes, J. J.; Hernandez, J.] Ctr Invest Astron, Merida 5101, Venezuela.
[Chini, R.; Hoffmeister, V. H.] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany.
[Chini, R.] Univ Catolica Norte, Fac Ciencias, Antofagasta, Chile.
[Fernandez, M.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Torres, G.; Latham, D. W.; Quinn, S. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Tachihara, K.] Joint ALMA Observ, Santiago, Chile.
[Tachihara, K.] Natl Astron Observ Japan, ALMA Project Off, Tokyo 1818588, Japan.
[Kjurkchieva, D. P.; Radeva, V. S.] Univ Shumen, Shumen 9700, Bulgaria.
[Krushevska, V.] NAS Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine.
[Redmer, R.; Kramm, U.; Nettelmann, N.] Univ Rostock, Inst Phys, D-18051 Rostock, Germany.
[Hohle, M. M.; Koppenhoefer, J.] MPI Extraterr Phys, D-85740 Garching, Germany.
[Chakrova, N.] FSU Jena, Inst Appl Phys, D-07743 Jena, Germany.
[Graefe, C.] Univ Kiel, D-24098 Kiel, Germany.
[Broeg, C. H.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
[Koppenhoefer, J.] Univ Sternwarte, D-81679 Munich, Germany.
[Pandey, A. K.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, Uttarakhand, India.
RP Neuhauser, R (reprint author), Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany.
EM rne@astro.uni-jena.de
RI Redmer, Ronald/F-3046-2013; Maciejewski, Gracjan/D-6241-2014; Nowak,
Grzegorz/H-8234-2014; Dimitrov, Dinko/J-7682-2013;
OI Nowak, Grzegorz/0000-0002-7031-7754; Jensen, Eric/0000-0002-4625-7333
FU Thuringian government [B 515-07010]; DFG [SPP 1385, NE 515/34-1, NE
515/33-1, NE 515/35-1, NE 515/32-1, SFB-TR 7, SCHR 665/7-1, NE 515/30-1,
NE 515/36-1, NE 515/38-1, 39-1, NE 515/42-1]; European Union
[MTKD-CT-2006-042514]; State of Thuringia; DAAD PPP-MNiSW
[50724260-2010/2011]; Tishreen University in Lattakia, Syria; US
National Science Foundation [AST-0721386]; Nordrhein-Westfalische
Akademie der Wissenschaften und der Kunste in the framework of the
Federal Republic of Germany; state Nordrhein-Westfalen; National Natural
Science Foundation of China [10803007]; VEGA [2/0094/11, 2/0078/10,
2/0074/09]; National Science Foundation of the Bulgarian Ministry of
Education and Science [DO 02-362]
FX All the participating observatories appreciate the logistic and
financial support of their institutions and in particular their
technical workshops. We would like to thank F. Giessler, H. Gilbert, I.
Hausler, D. Keeley, and S. Fitzpatrick for participating in some of the
observations at the Jena telescope. RN would like to thank DLN for
long-term support and many good ideas and questions. RN would like to
acknowledge financial support from the Thuringian government (B
515-07010) for the STK CCD camera used in this project. RN would like to
thank the German National Science Foundation (Deutsche
Forschungsgemeinschaft, DFG) for general support in various projects.
RN, RE, SR, and CA would like to thank DFG for support in the Priority
Programme SPP 1385 on the "First Ten Million Years of the Solar System"
in projects NE 515/34-1, NE 515/33-1, and NE 515/35-1. RN, GM, TP, and
MV would like to thank the European Union in the Framework Programme FP6
Marie Curie Transfer of Knowledge project MTKD-CT-2006-042514 for
support. SF thanks the State of Thuringia for a scholarship. RN, GM, AN,
LB, TT, GN, MaMu, SR, and TP would like to thank DAAD PPP-MNiSW in
project no. 50724260-2010/2011 for support. RR and UK would like to
thank DFG for support in the Priority Programme SPP 1385 in project RE
882/12-1. AB would like to thank DFG for support in project NE 515/32-1.
MoMo would like to thank the Tishreen University in Lattakia, Syria for
a scholarship. TE, NT, MMH, LT, and VVH would like to thank the DFG for
support from the SFB-TR 7. TR would like to thank DFG for support in
project NE 515/33-1. CM and KS would like to thank DFG for support in
project SCHR 665/7-1. TOBS, ChGi, LT, TE, and TR would like to thank DFG
for support in project NE 515/30-1. MS would like to thank DFG for
support in project NE 515/36-1. NT would like to acknowledge a
scholarship. RN, RE, TP, TOBS, UK, and MS would like to thank DFG for
travel support to Calar Alto runs in projects NE 515/38-1 and 39-1. RN
and RE would like to thank DFG for financial support for a Keck run in
project NE 515/42-1. ELNJ and his colleagues from Swarthmore acknowledge
support from the US National Science Foundation grant, AST-0721386.
Osservatorio Cerro Armazones (OCA) is supported as a project of the
Nordrhein-Westfalische Akademie der Wissenschaften und der Kunste in the
framework of the academy program by the Federal Republic of Germany and
the state Nordrhein-Westfalen. ZYW is supported by the National Natural
Science Foundation of China, No. 10803007. JB, TP, and MV thank VEGA
grants 2/0094/11, 2/0078/10, 2/0074/09. DPD, DPK, and VSR would like to
acknowledge for financial support to the National Science Foundation of
the Bulgarian Ministry of Education and Science (project DO 02-362). We
used Simbad, ViziR, 2MASS, and WEBDA. We would like to thank an
anonymous referee for good suggestions.
NR 119
TC 21
Z9 21
U1 0
U2 9
PU WILEY-V C H VERLAG GMBH
PI WEINHEIM
PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY
SN 0004-6337
J9 ASTRON NACHR
JI Astro. Nachr.
PD JUL
PY 2011
VL 332
IS 6
BP 547
EP 561
DI 10.1002/asna.201111573
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 799FT
UT WOS:000293271400001
ER
PT J
AU Agudo, I
Marscher, AP
Jorstad, SG
Larionov, VM
Gomez, JL
Lahteenmaki, A
Smith, PS
Nilsson, K
Readhead, ACS
Aller, MF
Heidt, J
Gurwell, M
Thum, C
Wehrle, AE
Nikolashvili, MG
Aller, HD
Benitez, E
Blinov, DA
Hagen-Thorn, VA
Hiriart, D
Jannuzi, BT
Joshi, M
Kimeridze, GN
Kurtanidze, OM
Kurtanidze, SO
Lindfors, E
Molina, SN
Morozova, DA
Nieppola, E
Olmstead, AR
Reinthal, R
Roca-Sogorb, M
Schmidt, GD
Sigua, LA
Sillanpaa, A
Takalo, L
Taylor, B
Tornikoski, M
Troitsky, IS
Zook, AC
Wiesemeyer, H
AF Agudo, Ivan
Marscher, Alan P.
Jorstad, Svetlana G.
Larionov, Valeri M.
Gomez, Jose L.
Lahteenmaki, Anne
Smith, Paul S.
Nilsson, Kari
Readhead, Anthony C. S.
Aller, Margo F.
Heidt, Jochen
Gurwell, Mark
Thum, Clemens
Wehrle, Ann E.
Nikolashvili, Maria G.
Aller, Hugh D.
Benitez, Erika
Blinov, Dmitriy A.
Hagen-Thorn, Vladimir A.
Hiriart, David
Jannuzi, Buell T.
Joshi, Manasvita
Kimeridze, Givi N.
Kurtanidze, Omar M.
Kurtanidze, Sofia O.
Lindfors, Elina
Molina, Sol N.
Morozova, Daria A.
Nieppola, Elina
Olmstead, Alice R.
Reinthal, Riho
Roca-Sogorb, Mar
Schmidt, Gary D.
Sigua, Lorand A.
Sillanpaa, Aimo
Takalo, Leo
Taylor, Brian
Tornikoski, Merja
Troitsky, Ivan S.
Zook, Alma C.
Wiesemeyer, Helmut
TI ON THE LOCATION OF THE gamma-RAY OUTBURST EMISSION IN THE BL LACERTAE
OBJECT AO 0235+164 THROUGH OBSERVATIONS ACROSS THE ELECTROMAGNETIC
SPECTRUM
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE BL Lacertae objects: individual (AO 0235+164); galaxies: active;
galaxies: jets; gamma rays: general; polarization; radio continuum:
galaxies
ID ACTIVE GALACTIC NUCLEI; BASE-LINE ARRAY; POLARIMETRIC OBSERVATIONS;
RELATIVISTIC JETS; AMBIENT RADIATION; HIGH-FREQUENCIES; BRIGHT BLAZARS;
INNER JET; HOT DUST; 3C 454.3
AB We present observations of a major outburst at centimeter, millimeter, optical, X-ray, and gamma-ray wavelengths of the BL Lacertae object AO 0235+164. We analyze the timing of multi-waveband variations in the flux and linear polarization, as well as changes in Very Long Baseline Array images at lambda = 7 mm with similar to 0.15 milliarcsec resolution. The association of the events at different wavebands is confirmed at high statistical significance by probability arguments and Monte Carlo simulations. A series of sharp peaks in optical linear polarization, as well as a pronounced maximum in the 7 mm polarization of a superluminal jet knot, indicate rapid fluctuations in the degree of ordering of the magnetic field. These results lead us to conclude that the outburst occurred in the jet both in the quasi-stationary "core" and in the superluminal knot, both parsecs downstream of the supermassive black hole. We interpret the outburst as a consequence of the propagation of a disturbance, elongated along the line of sight by light-travel time delays, that passes through a standing recollimation shock in the core and propagates down the jet to create the superluminal knot. The multi-wavelength light curves vary together on long timescales (months/years), but the correspondence is poorer on shorter timescales. This, as well as the variability of the polarization and the dual location of the outburst, agrees with the expectations of a multi-zone emission model in which turbulence plays a major role in modulating the synchrotron and inverse Compton fluxes.
C1 [Agudo, Ivan; Gomez, Jose L.; Molina, Sol N.; Roca-Sogorb, Mar] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Agudo, Ivan; Marscher, Alan P.; Jorstad, Svetlana G.; Joshi, Manasvita; Olmstead, Alice R.; Taylor, Brian] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitriy A.; Hagen-Thorn, Vladimir A.; Morozova, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Larionov, Valeri M.; Blinov, Dmitriy A.; Hagen-Thorn, Vladimir A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia.
[Lahteenmaki, Anne; Nieppola, Elina; Tornikoski, Merja] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Nilsson, Kari; Nieppola, Elina] Univ Turku, Finnish Ctr Astron ESO FINCA, FIN-21500 Piikkio, Finland.
[Readhead, Anthony C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA.
[Aller, Margo F.; Aller, Hugh D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Heidt, Jochen] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany.
[Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Thum, Clemens] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France.
[Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA.
[Nikolashvili, Maria G.; Kimeridze, Givi N.; Kurtanidze, Omar M.; Kurtanidze, Sofia O.; Sigua, Lorand A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia.
[Benitez, Erika] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Hiriart, David] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 2280, Baja California, Mexico.
[Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA.
[Lindfors, Elina; Reinthal, Riho; Sillanpaa, Aimo; Takalo, Leo] Univ Turku, Tuorla Observ, FIN-21500 Piikkio, Finland.
[Schmidt, Gary D.] Natl Sci Fdn, Arlington, VA 22230 USA.
[Taylor, Brian] Lowell Observ, Flagstaff, AZ 86001 USA.
[Zook, Alma C.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA.
[Wiesemeyer, Helmut] Inst Radio Astron Millimetr, E-18012 Granada, Spain.
RP Agudo, I (reprint author), CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain.
EM iagudo@iaa.es
RI Larionov, Valeri/H-1349-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki,
Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Molina, Sol
Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Morozova,
Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad,
Svetlana/H-6913-2013; Hagen-Thorn, Vladimir/H-3983-2013
OI Larionov, Valeri/0000-0002-4640-4356; Blinov,
Dmitry/0000-0003-0611-5784; Molina, Sol Natalia/0000-0002-4112-2157;
Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804;
Troitskiy, Ivan/0000-0002-4218-0148; Jorstad,
Svetlana/0000-0001-9522-5453; Hagen-Thorn, Vladimir/0000-0002-6431-8590
FU NASA [NNX08AJ64G, NNX08AU02G, NNX08AV61G, NNX08AV65G, NNX08AW56S,
NNX09AU10G]; NSF [AST-0907893]; Boston University [GSSP07-0009]; RFBR
[09-02-00092]; MICIIN [AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784];
Academy of Finland; GNSF [ST08/4-404]; NSF, Boston University
FX We acknowledge the anonymous referee for constructive comments. This
research was funded by NASA grants NNX08AJ64G, NNX08AU02G, NNX08AV61G,
and NNX08AV65G, NSF grant AST-0907893, and NRAO award GSSP07-0009
(Boston University); RFBR grant 09-02-00092 (St. Petersburg State
University); MICIIN grant AYA2010-14844, and CEIC (Andalucia) grant
P09-FQM-4784 (IAA-CSIC); the Academy of Finland (Metsahovi); NASA grants
NNX08AW56S and NNX09AU10G (Steward Observatory); and GNSF grant
ST08/4-404 (Abastunami Observatory). The VLBA is an instrument of the
NRAO, a facility of the NSF under cooperative agreement by AUI. The
PRISM camera was developed by Janes et al. and funded by NSF, Boston
University, and Lowell Observatory. Calar Alto Observatory is operated
by MPIA and IAA-CSIC. The IRAM 30 m Telescope is supported by INSU/CNRS,
MPG, and IGN. The SMA is a joint project between the SAO and the
Academia Sinica.
NR 34
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Z9 55
U1 0
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2011
VL 735
IS 1
AR L10
DI 10.1088/2041-8205/735/1/L10
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OT
UT WOS:000293137900010
ER
PT J
AU Demory, BO
Seager, S
Madhusudhan, N
Kjeldsen, H
Christensen-Dalsgaard, J
Gillon, M
Rowe, JF
Welsh, WF
Adams, ER
Dupree, A
McCarthy, D
Kulesa, C
Borucki, WJ
Koch, DG
AF Demory, Brice-Olivier
Seager, Sara
Madhusudhan, Nikku
Kjeldsen, Hans
Christensen-Dalsgaard, Jorgen
Gillon, Michael
Rowe, Jason F.
Welsh, William F.
Adams, Elisabeth R.
Dupree, Andrea
McCarthy, Don
Kulesa, Craig
Borucki, William J.
Koch, David G.
TI THE HIGH ALBEDO OF THE HOT JUPITER KEPLER-7 b
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE planetary systems; stars: individual (Kepler-7, KIC 5780885, 2MASS
19141956+4105233); techniques: photometric
ID EXTRASOLAR GIANT PLANETS; LIGHT-CURVE PROJECT; TAU-BOOTIS-B; INITIAL
CHARACTERISTICS; REFLECTED STARLIGHT; THERMAL INVERSIONS; CADENCE DATA;
LOW-DENSITY; UPPER LIMIT; ATMOSPHERES
AB Hot Jupiters are expected to be dark from both observations (albedo upper limits) and theory (alkali metals and/or TiO and VO absorption). However, only a handful of hot Jupiters have been observed with high enough photometric precision at visible wavelengths to investigate these expectations. The NASA Kepler mission provides a means to widen the sample and to assess the extent to which hot Jupiter albedos are low. We present a global analysis of Kepler-7 b based on Q0-Q4 data, published radial velocities, and asteroseismology constraints. We measure an occultation depth in the Kepler bandpass of 44 +/- 5 ppm. If directly related to the albedo, this translates to a Kepler geometric albedo of 0.32 +/- 0.03, the most precise value measured so far for an exoplanet. We also characterize the planetary orbital phase light curve with an amplitude of 42 +/- 4 ppm. Using atmospheric models, we find it unlikely that the high albedo is due to a dominant thermal component and propose two solutions to explain the observed planetary flux. First, we interpret the Kepler-7 b albedo as resulting from an excess reflection over what can be explained solely by Rayleigh scattering, along with a nominal thermal component. This excess reflection might indicate the presence of a cloud or haze layer in the atmosphere, motivating new modeling and observational efforts. Alternatively, the albedo can be explained by Rayleigh scattering alone if Na and K are depleted in the atmosphere by a factor of 10-100 below solar abundances.
C1 [Demory, Brice-Olivier; Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
[Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Kjeldsen, Hans; Christensen-Dalsgaard, Jorgen] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark.
[Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, Liege 1, Belgium.
[Rowe, Jason F.; Borucki, William J.; Koch, David G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
[Adams, Elisabeth R.; Dupree, Andrea] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[McCarthy, Don; Kulesa, Craig] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Demory, BO (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.
EM demory@mit.edu
OI Demory, Brice-Olivier/0000-0002-9355-5165
FU Swiss NSF; NASA [NNX10AD67G]; NASA's Science Mission Directorate
FX Authors thank the Kepler Giant Planet Working Group, P.-O. Quirion, M.
Holman, D. Ragozzine, J. Jenkins, J.-M. Desert, B. Benneke, and D.
Latham for useful discussions. We thank E. Dunham, W. Cochran, and the
referee for helpful comments that improved the manuscript. B.-O.D.
acknowledges support from the Swiss NSF and thanks kindly R. Stewart, P.
L. Vidale, and A. Verhoef from the University of Reading (UK), where
part of this work has been carried out. M.G. is Belgian FNRS Research
Associate. We acknowledge support from NASA Kepler Participating Science
Program NNX10AD67G. Funding for this Discovery Mission is provided by
NASA's Science Mission Directorate.
NR 48
TC 47
Z9 48
U1 1
U2 9
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 JUL 1
PY 2011
VL 735
IS 1
AR L12
DI 10.1088/2041-8205/735/1/L12
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OT
UT WOS:000293137900012
ER
PT J
AU van Dokkum, PG
Conroy, C
AF van Dokkum, Pieter G.
Conroy, Charlie
TI CONFIRMATION OF ENHANCED DWARF-SENSITIVE ABSORPTION FEATURES IN THE
SPECTRA OF MASSIVE ELLIPTICAL GALAXIES: FURTHER EVIDENCE FOR A
NON-UNIVERSAL INITIAL MASS FUNCTION
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE cosmology: observations; galaxies: abundances; galaxies: evolution;
galaxies: stellar content; stars: luminosity function, mass function
ID FUNDAMENTAL PLANE; POPULATION PARAMETERS; STELLAR POPULATIONS;
LENTICULAR GALAXIES; GLOBULAR-CLUSTERS; LINE-STRENGTHS; EVOLUTION;
STARS; LIGHT; GROWTH
AB We recently found that massive cluster elliptical galaxies have strong Na I lambda 8183, 8195 and FeH lambda 9916 Wing-Ford band absorption, indicating the presence of a very large population of stars with masses less than or similar to 0.3 M(circle dot). Here we test this result by comparing the elliptical galaxy spectra to those of luminous globular clusters associated with M31. These globular clusters have similar metallicities, abundance ratios, and ages as massive elliptical galaxies but their low dynamical mass-to-light ratios rule out steep stellar initial mass functions (IMFs). From high-quality Keck spectra we find that the dwarf-sensitive absorption lines in globular clusters are significantly weaker than in elliptical galaxies and consistent with normal IMFs. The differences in the Na I and Wing-Ford indices are 0.027 +/- 0.007 mag and 0.017 +/- 0.006 mag, respectively. We directly compare the two classes of objects by subtracting the averaged globular cluster spectrum from the averaged elliptical galaxy spectrum. The difference spectrum is well fit by the difference between a stellar population synthesis model with a bottom-heavy IMF and one with a bottom-light IMF. We speculate that the slope of the IMF may vary with velocity dispersion, although it is not yet clear what physical mechanism would be responsible for such a relation.
C1 [van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA.
[Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP van Dokkum, PG (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA.
NR 39
TC 61
Z9 61
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUL 1
PY 2011
VL 735
IS 1
AR L13
DI 10.1088/2041-8205/735/1/L13
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797OT
UT WOS:000293137900013
ER
PT J
AU Ryder, TB
Fox, JW
Marra, PP
AF Ryder, Thomas B.
Fox, James W.
Marra, Peter P.
TI ESTIMATING MIGRATORY CONNECTIVITY OF GRAY CATBIRDS (DUMETELLA
CAROLINENSIS) USING GEOLOCATOR AND MARK-RECAPTURE DATA
SO AUK
LA English
DT Article
DE Dumetella carolinensis; geolocators; Gray Catbird; mark-recapture;
migratory connectivity
ID BIRD MIGRATION; SONGBIRD MIGRATION; POPULATIONS; ISOTOPES; MIGRANTS;
ACCURACY; TRACKING; GROUNDS; SUMMER; RANGES
AB Understanding the connectivity between breeding and nonbreeding populations of migratory birds is fundamental to our knowledge of biological phenomena such as population dynamics and dispersal. Moreover, our ability to quantify migratory connectivity has inevitable consequences for both conservation and management of species that utilize distinct geographic locations. Technology is rapidly advancing our ability to track birds throughout the annual cycle and to collect data on the degree of connectivity among breeding and nonbreeding populations. We combined two direct methods, mark recapture (n = 17) and geolocation (n = 6), to estimate the migratory connectivity of breeding and nonbreeding populations of Gray Catbirds (Dumetella carolinensis). Data from geolocators show that birds breeding in the Mid-Atlantic overwinter in both Cuba and southern Florida. Mark recapture data supported our geolocator results but also provided a broader spatial perspective by documenting that Mid-Atlantic and Midwestern populations occupy distinct geographic localities during the nonbreeding period. This research underscores the importance of geolocators, as well as other tools, to advance our understanding of migratory connectivity. Finally, our results highlight the potential value of U.S. Geological Survey (USGS) Bird Banding Laboratory mark recapture data, which are often underutilized in ornithological research. Received 6 January 2011, accepted 24 April 2011.
C1 [Ryder, Thomas B.; Marra, Peter P.] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA.
[Fox, James W.] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England.
RP Ryder, TB (reprint author), Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012-MRC5503, Washington, DC 20008 USA.
EM rydert@si.edu
NR 28
TC 31
Z9 33
U1 4
U2 43
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
EI 1938-4254
J9 AUK
JI AUK
PD JUL
PY 2011
VL 128
IS 3
BP 448
EP 453
DI 10.1525/auk.2011.11091
PG 6
WC Ornithology
SC Zoology
GA 799SV
UT WOS:000293307300002
ER
PT J
AU Vogelsberger, M
Mohayaee, R
White, SDM
AF Vogelsberger, Mark
Mohayaee, Roya
White, Simon D. M.
TI Non-spherical similarity solutions for dark halo formation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE dark matter
ID RADIAL ORBIT INSTABILITY; MATTER HALOES; SECONDARY INFALL; DENSITY
PROFILES; STELLAR-SYSTEMS; UNIVERSAL; STABILITY; GALAXIES; COLLAPSE;
SPECTRUM
AB We carry out fully three-dimensional simulations of evolution from self-similar, spherically symmetric linear perturbations of a cold dark matter (CDM)-dominated Einstein-de Sitter universe. As a result of the radial orbit instability, the haloes which grow from such initial conditions are triaxial with major-to-minor axial ratios of the order of 3:1. They nevertheless grow approximately self-similarly in time. In all cases, they have power-law density profiles and near-constant velocity anisotropy in their inner regions. Both the power-law index and the value of the velocity anisotropy depend on the similarity index of the initial conditions, the former as expected from simple scaling arguments. Halo structure is thus not 'universal' but remembers the initial conditions. On larger scales the density and anisotropy profiles show two characteristic scales, corresponding to particles at the first pericentre and at the first apocentre after infall. They are well approximated by the Navarro-Frenk-White model only for one value of the similarity index. In contrast, at all radii within the outer caustic the pseudo-phase-space density can be fitted by a single power law with an index which depends only very weakly on the similarity index of the initial conditions. This behaviour is very similar to that found for haloes formed from Lambda CDM initial conditions and so can be considered approximately universal.
C1 [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Mohayaee, Roya] UPMC, CNRS, Inst Astrophys Paris IAP, Paris, France.
[White, Simon D. M.] Max Planck Inst Astrophys, D-85748 Garching, Germany.
RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mvogelsberger@cfa.harvard.edu
FU French ANR OTARIE
FX Our simulations were carried out at the Computing Centre of the
Max-Planck-Society in Garching. RM thanks French ANR OTARIE for support.
We thank Niayesh Afshordi, Ed Bertschinger, James Binney, Jacques Colin,
Aaron Ludlow and Julio Navarro for useful discussions.
NR 33
TC 12
Z9 12
U1 2
U2 2
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 JUL
PY 2011
VL 414
IS 4
BP 3044
EP 3051
DI 10.1111/j.1365-2966.2011.18605.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 798CF
UT WOS:000293178600020
ER
PT J
AU Sijacki, D
Springel, V
Haehnelt, MG
AF Sijacki, Debora
Springel, Volker
Haehnelt, Martin G.
TI Gravitational recoils of supermassive black holes in hydrodynamical
simulations of gas-rich galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE black hole physics; methods: numerical; cosmology: theory
ID QUASAR SDSS J092712.65+294344.0; GALACTIC NUCLEI; COSMOLOGICAL
SIMULATIONS; DYNAMICAL FRICTION; RADIATION RECOIL; WAVE RECOIL; MERGER;
EVOLUTION; BINARIES; FEEDBACK
AB We study the evolution of gravitationally recoiled supermassive black holes (BHs) in massive gas-rich galaxies by means of high-resolution hydrodynamical simulations. We find that the presence of a massive gaseous disc allows recoiled BHs to return to the centre on a much shorter time-scale than for purely stellar discs. Also, BH accretion and feedback can strongly modify the orbit of recoiled BHs and hence their return time-scale, besides affecting the distribution of gas and stars in the galactic centre. However, the dynamical interaction of kicked BHs with the surrounding medium is in general complex and can facilitate both a fast return to the centre as well as a significant delay. The Bondi-Hoyle-Lyttleton accretion rates of the recoiling BHs in our simulated galaxies are favourably high for the detection of off-centred active galactic nuclei (AGN) if kicked into gas-rich discs - up to a few per cent of the Eddington accretion rate - and are highly variable on time-scales of a few 10(7) yr. In major merger simulations of gas-rich galaxies, we find that gravitational recoils increase the scatter in the BH mass-host galaxy relationships compared to simulations without kicks, with the BH mass being more sensitive to recoil kicks than the bulge mass. The BH mass can be lowered by a factor of a few due to a recoil, even for a relatively short return time-scale, but the exact magnitude of the effect depends strongly on the BH binary hardening time-scale and on the efficiency of star formation in the central regions. A generic result of our numerical models is that the clumpy massive discs suggested by recent high-redshift observations, as well as the remnants of gas-rich mergers, exhibit a gravitational potential that falls steeply in the central regions, due to the dissipative concentration of baryons. As a result, supermassive BHs should only rarely be able to escape from massive galaxies at high redshifts, which is the epoch where the bulk of BH recoils is expected to occur.
C1 [Sijacki, Debora; Haehnelt, Martin G.] Cambridge & Inst Astron, Kavli Inst Cosmol, Cambridge CB3 0HA, England.
[Sijacki, Debora] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany.
[Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany.
RP Sijacki, D (reprint author), Cambridge & Inst Astron, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England.
EM dsijacki@cfa.harvard.edu
OI Haehnelt, Martin/0000-0001-8443-2393
FU UK Science and Technology Funding Council (STFC); NASA
[HST-HF-51282.01-A]; STFC [LGAG 092/RG43335]
FX We would like to thank Jim Pringle for very useful discussions and
comments on the manuscript and Giuseppe Lodato for enthusiastic
discussions on the topic. DS acknowledges a Postdoctoral Fellowship from
the UK Science and Technology Funding Council (STFC) and NASA Hubble
Fellowship through grant HST-HF-51282.01-A. MGH was partially supported
by STFC grant LGAG 092/RG43335. Simulations were performed on the
Cambridge High Performance Computing Cluster DARWIN in Cambridge
(http://www.hpc.cam.ac.uk).
NR 46
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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 JUL
PY 2011
VL 414
IS 4
BP 3656
EP 3670
DI 10.1111/j.1365-2966.2011.18666.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 798CF
UT WOS:000293178600069
ER
PT J
AU Vann, R
Lang, M
AF Vann, Richard
Lang, Michael
TI Recreational diving fatalities
SO UNDERSEA & HYPERBARIC MEDICINE
LA English
DT Article
AB The risks of dying during recreational diving are small. The Divers Alert Network (DAN) held a workshop to consider whether the risks could be reduced further. Topics included investigation, surveillance, operational safety and cardiovascular disease. Investigation is essential to determine causes and involves on-scene inquiry, forensic examination of the deceased, and testing of life support equipment, but thorough investigations are unusual. Independent annual fatality rates were presented and reviewed for diving, jogging, and motor vehicle accidents and for divers in training. Common factors associated with diving fatalities included running out of gas, entrapment or entanglement, buoyancy control, equipment misuse, rough waters and emergency ascent. Asphyxia by drowning, air embolism and cardiac events were the principal injuries or causes of death. About one-quarter of the deaths were associated with cardiac events, mostly in older divers. Revised procedures were recommended for identifying occult cardiovascular disease in candidate divers who warrant further investigation, but older, previously certified divers may be at greatest risk.
C1 [Vann, Richard] Divers Alert Network, Durham, NC 27705 USA.
[Vann, Richard] Duke Univ, Ctr Hyperbar Med & Environm Physiol, Durham, NC USA.
[Lang, Michael] Smithsonian Inst, Washington, DC USA.
RP Vann, R (reprint author), Divers Alert Network, Durham, NC 27705 USA.
EM rvann@dan.org
NR 19
TC 11
Z9 11
U1 0
U2 2
PU UNDERSEA & HYPERBARIC MEDICAL SOC INC
PI DURHAM
PA 21 WEST COLONY PLACE, STE 280, DURHAM, NC 27705 USA
SN 1066-2936
J9 UNDERSEA HYPERBAR M
JI Undersea Hyperb. Med.
PD JUL-AUG
PY 2011
VL 38
IS 4
BP 257
EP 260
PG 4
WC Marine & Freshwater Biology; Medicine, Research & Experimental
SC Marine & Freshwater Biology; Research & Experimental Medicine
GA 799YA
UT WOS:000293321400006
PM 21877554
ER
PT J
AU Walke, JB
Harris, RN
Reinert, LK
Rollins-Smith, LA
Woodhams, DC
AF Walke, Jenifer B.
Harris, Reid N.
Reinert, Laura K.
Rollins-Smith, Louise A.
Woodhams, Douglas C.
TI Social Immunity in Amphibians: Evidence for Vertical Transmission of
Innate Defenses
SO BIOTROPICA
LA English
DT Article
DE antimicrobial peptide; Batrachochytrium dendrobatidis; disease ecology;
Hyalinobatrachium colymbiphyllum; Panama; skin defense; symbiotic
microbiota
ID EMERGING INFECTIOUS-DISEASE; ANTIFUNGAL SKIN BACTERIA; SYMBIOTIC
BACTERIA; BATRACHOCHYTRIUM-DENDROBATIDIS; CUTANEOUS BACTERIA; PEPTIDE
DEFENSES; 4-TOED SALAMANDERS; CHYTRIDIOMYCOSIS; EMBRYO; COMMON
AB Amphibian embryos are at risk of microbial infection. Here we find evidence that innate immune defenses, both antimicrobial skin peptides and mutualistic microbiota, of adult glass frogs, Hyalinobatrachium colymbiphyllum, can be transmitted to embryos deposited on leaves above rain forest streams in Panama and can inhibit the fungal pathogen Batrachochytrium dendrobatidis.
C1 [Rollins-Smith, Louise A.; Woodhams, Douglas C.] Smithsonian Trop Res Inst, Panama City, Panama.
[Walke, Jenifer B.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA.
[Harris, Reid N.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA.
[Reinert, Laura K.; Rollins-Smith, Louise A.] Vanderbilt Univ, Med Ctr, Dept Microbiol & Immunol, Nashville, TN 37232 USA.
[Rollins-Smith, Louise A.] Vanderbilt Univ, Med Ctr, Dept Pediat, Nashville, TN 37232 USA.
[Rollins-Smith, Louise A.] Vanderbilt Univ, Med Ctr, Dept Biol Sci, Nashville, TN 37232 USA.
[Woodhams, Douglas C.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland.
RP Woodhams, DC (reprint author), Smithsonian Trop Res Inst, Panama City, Panama.
EM dwoodhams@gmail.com
RI Woodhams, Douglas/B-1962-2012
FU U.S. National Science Foundation [IOS-0520847, IOS-0619536, IOS-0843207,
DEB-0640373]
FX We are grateful for the hospitality of Padre Pablo Kasuboski, and for
the field assistance of Arquimides Batista, Julie Ray, and Manuel
Rivera. Scientific collecting permits from the government of Panama
(Autoridad Nacional del Ambiente) were arranged with the assistance of
the Smithsonian Tropical Research Institute. We thank Brianna Lam of
James Madison University for laboratory assistance, and Eric Smith and
Denisa Olteanu of Virginia Tech for help with statistical analyses of
DGGE profiles. These studies were conducted with financial support from
the U.S. National Science Foundation (IOS-0520847, IOS-0619536 and
IOS-0843207 to LRS; and DEB-0640373 to RNH).
NR 45
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U2 41
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD JUL
PY 2011
VL 43
IS 4
BP 396
EP 400
DI 10.1111/j.1744-7429.2011.00787.x
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 793EV
UT WOS:000292804100002
ER
PT J
AU Mayne, RG
Sunshine, JM
McSween, HY
Bus, SJ
McCoy, TJ
AF Mayne, R. G.
Sunshine, J. M.
McSween, H. Y., Jr.
Bus, S. J.
McCoy, T. J.
TI The origin of Vesta's crust: Insights from spectroscopy of the Vestoids
SO ICARUS
LA English
DT Article
DE Asteroid Vesta; Asteroids, Surfaces; Asteroids, Composition;
Spectroscopy; Meteorites
ID ASTEROID 4 VESTA; MINERAL ABSORPTION FEATURES; MODIFIED GAUSSIAN MODEL;
REFLECTANCE SPECTRA; MAIN-BELT; BASALTIC ASTEROIDS; PARENT BODY;
METEORITES; PYROXENE; TEMPERATURE
AB High quality VNIR spectra of 15 Vestoids, small asteroids that are believed to originate from Vesta, were collected and compared to laboratory spectra and compositional data for selected HED meteorites. A combination of spectral parameters such as band centers, and factors derived from Modified Gaussian Model fits (band centers, band strengths, calculation of the low to high-Ca pyroxene ratio) were used to establish if each Vestoid appeared most like eucrite or diogenite material, or a mixture of the two (howardite). This resulted in the identification of the first asteroid with a ferroan diogenite composition, 2511 Patterson. This asteroid can be used to constrain the size of diogenite magma chambers within the crust of Vesta. The Vestoids indicate that both large-scale homogeneous units (>5 km) and smaller-scale heterogeneity (<1 km) exist on the surface of Vesta, as both monomineralogic (eucrite or diogenite material alone) and mixed (both eucrite and diogenite) spectra are observed. The small-scale of the variation observed within the Vestoid population is predicted by the partial melting model, which has multiple intrusions penetrating into the crust of Vesta. It is much more difficult to reconcile the observations here with the magma ocean model, which would predict much more homogeneous layers on a large-scale both at the surface and with depth. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Mayne, R. G.] Texas Christian Univ, Sch Geol Energy & Environm, Ft Worth, TX 76129 USA.
[Mayne, R. G.; McSween, H. Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA.
[Mayne, R. G.; McCoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA.
[Sunshine, J. M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Bus, S. J.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA.
RP Mayne, RG (reprint author), Texas Christian Univ, Sch Geol Energy & Environm, TCU Box 298830, Ft Worth, TX 76129 USA.
EM r.g.mayne@tcu.edu
FU PGG [NNX06AH69G]; NASA [NNG06GG36G]; UCLA [2090-S-JB694]
FX This work was supported by PGG Grant NNX06AH69G to J.M.S., a NASA
Cosmochemistry Grant NNG06GG36G to T.J.M. and UCLA subcontract
2090-S-JB694 for Dawn to H.Y.M. All meteorite spectra were collected at
Brown University's KECK/NASA Reflectance Experiment Laboratory (RELAB).
NR 61
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U1 1
U2 7
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 2011
VL 214
IS 1
BP 147
EP 160
DI 10.1016/j.icarus.2011.04.013
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 793WC
UT WOS:000292853600011
ER
PT J
AU Bernhardt, CE
Stanley, JD
Horton, BP
AF Bernhardt, Christopher E.
Stanley, Jean-Daniel
Horton, Benjamin P.
TI Wetland Vegetation in Manzala Lagoon, Nile Delta Coast, Egypt: Rapid
Responses of Pollen to Altered Nile Hydrology and Land Use
SO JOURNAL OF COASTAL RESEARCH
LA English
DT Article
DE Aswan; darns; delta wetlands; hydrologic changes; land use; Manzala
lagoon; Nile delta; Nile River; organics; pollen zones; pollutants
ID COMBINING ORGANIC PETROGRAPHY; ASSESS ANTHROPOGENIC IMPACTS; LAKE
MANZALA; EVERGLADES; PALYNOLOGY; PEATLANDS; ISLANDS; EXAMPLE; FLORIDA;
RIVER
AB The pollen record in a sediment core from Manzala lagoon on the Nile delta coastal margin of Egypt, deposited from ca. AD 1860 to 1990, indicates rapid coastal wetland vegetation responses to two primary periods of human activity. These are associated with artificially altered Nile hydrologic regimes in proximal areas and distal sectors located to similar to 1200 km south of Manzala. Freshwater wetland plants that were dominant, such as Typha and Phragmites, decreased rapidly, whereas in the early 1900s, brackish water wetland species (e.g., Amaranthaceae) increased. This change occurred after closure of the Aswan Low Dam in 1902. The second major modification in the pollen record occurred in the early 1970s, after Aswan High Dam closure from 1965 to 1970, when Typha pollen abundance increased rapidly. Massive population growth occurred along the Nile during the 130 years represented by the core section. During this time, the total volume of lagoon water decreased because of conversion of wetland areas to agricultural land, and input of organic-rich sediment, sewage (municipal, agricultural, industrial), and fertilizer in Manzala lagoon increased markedly. Although the wetland plant community has continued to respond to increasingly intensified and varied human-induced pressures in proximal sectors, the two most marked changes in Manzala pollen best correlate with distal events (i.e., closure of the two dams at Aswan). The study also shows that the two major vegetation changes in Manzala lagoon each occurred less than 10 years after closure upriver of the Low and High dams that markedly altered the Nile regime from Upper Egypt to the coast.
C1 [Bernhardt, Christopher E.] US Geol Survey, Reston, VA 20192 USA.
[Bernhardt, Christopher E.; Horton, Benjamin P.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
[Stanley, Jean-Daniel] Smithsonian Inst, Geoarchaeol Program, NMNH E 205, Washington, DC 20013 USA.
RP Bernhardt, CE (reprint author), US Geol Survey, Natl Ctr 926A, Reston, VA 20192 USA.
EM cbernhardt@usgs.gov
FU University of Pennsylvania; palynological laboratory at the U.S.
Geological Survey (USGS), Reston, VA
FX We thank the University of Pennsylvania for awarding a Paleobiology
Stipend (to CEB), and for support from the palynological laboratory at
the U.S. Geological Survey (USGS), Reston, VA. The Smithsonian
Institution's Delta-Global Change Program in Egypt authorized access to
core samples at the National Museum of Natural History. Drs. Debra
Willard and Lynn Wingard (USGS) and anonymous reviewers provided
insightful suggestions that significantly improved the original
manuscript.
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U1 0
U2 14
PU COASTAL EDUCATION & RESEARCH FOUNDATION
PI COCONUT CREEK
PA 5130 NW 54TH STREET, COCONUT CREEK, FL 33073 USA
SN 0749-0208
EI 1551-5036
J9 J COASTAL RES
JI J. Coast. Res.
PD JUL
PY 2011
VL 27
IS 4
BP 731
EP 737
DI 10.2112/10A-00001.1
PG 7
WC Environmental Sciences; Geography, Physical; Geosciences,
Multidisciplinary
SC Environmental Sciences & Ecology; Physical Geography; Geology
GA 795DL
UT WOS:000292951600013
ER
PT J
AU Winter, K
Garcia, M
Holtum, JAM
AF Winter, Klaus
Garcia, Milton
Holtum, Joseph A. M.
TI Drought-stress-induced up-regulation of CAM in seedlings of a tropical
cactus, Opuntia elatior, operating predominantly in the C-3 mode
SO JOURNAL OF EXPERIMENTAL BOTANY
LA English
DT Article
DE Carbon dioxide uptake; constitutive CAM; crassulacean acid metabolism;
C-3 photosynthesis; development; drought stress; environment;
facultative CAM; Opuntia
ID CRASSULACEAN-ACID-METABOLISM; CARBON-ISOTOPE COMPOSITION; FICUS-INDICA;
MESEMBRYANTHEMUM-CRYSTALLINUM; PHOTOSYNTHETIC METABOLISM; GAS-EXCHANGE;
PLANTS; CO2; ASSIMILATION; EXPRESSION
AB Immediately after unfolding, cotyledons of the tropical platyopuntoid cactus, Opuntia elatior Mill., exhibited a C-3-type diel CO2 exchange pattern characterized by net CO2 uptake in the light. Significant nocturnal increases in titratable acidity typical of crassulacean acid metabolism (CAM) were not detected at this early developmental stage. As cotyledons matured and the first cladode (flattened stem) developed, features of CAM were observed and the magnitude of CAM increased. Nonetheless, in well-watered seedlings up to 10 cm tall, C-3 photosynthetic CO2 fixation in the light remained the major pathway of carbon fixation. Reduced soil water availability led to an up-regulation of net dark CO2 fixation and greater nocturnal increases in tissue acidity, consistent with facultative CAM. These observations demonstrate that C-3 photosynthesis, drought-stress-related facultative CAM, and developmentally controlled constitutive CAM can all contribute to the early growth of O. elatior. The strong C-3 component and facultative CAM features expressed in young O. elatior contrast with mature plants in which obligate CAM is the major pathway of carbon acquisition.
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; Research ID, CTBCC /O-3564-2014
OI Holtum, Joseph/0000-0001-6568-8019;
FU Smithsonian Tropical Research Institute; JCU
FX The authors acknowledge the contribution of Aurelio Virgo who drew the
illustrations. The research was supported by funds from the Smithsonian
Tropical Research Institute. JAMH was supported by the JCU Special
Studies Programme.
NR 24
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U1 1
U2 40
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 2011
VL 62
IS 11
BP 4037
EP 4042
DI 10.1093/jxb/err106
PG 6
WC Plant Sciences
SC Plant Sciences
GA 793QR
UT WOS:000292838700029
PM 21504876
ER
PT J
AU Furlan, E
Luhman, KL
Espaillat, C
D'Alessio, P
Adame, L
Manoj, P
Kim, KH
Watson, DM
Forrest, WJ
McClure, MK
Calvet, N
Sargent, BA
Green, JD
Fischer, WJ
AF Furlan, E.
Luhman, K. L.
Espaillat, C.
D'Alessio, P.
Adame, L.
Manoj, P.
Kim, K. H.
Watson, Dan M.
Forrest, W. J.
McClure, M. K.
Calvet, N.
Sargent, B. A.
Green, J. D.
Fischer, W. J.
TI THE SPITZER INFRARED SPECTROGRAPH SURVEY OF T TAURI STARS IN TAURUS
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE circumstellar matter; protoplanetary disks; stars: formation; stars:
low-mass; stars: pre-main sequence
ID MAIN-SEQUENCE STARS; YOUNG STELLAR OBJECTS; LOW-MASS STARS; INTERSTELLAR
SILICATE MINERALOGY; AURIGA MOLECULAR CLOUD; HUBBLE-SPACE-TELESCOPE;
BROWN DWARF DISKS; PHOTOEVAPORATING PROTOPLANETARY DISCS; SPECTRAL
ENERGY-DISTRIBUTIONS; HERBIG AE/BE STARS
AB We present 161 Spitzer Infrared Spectrograph (IRS) spectra of T Tauri stars and young brown dwarfs in the Taurus star-forming region. All of the targets were selected based on their infrared excess and are therefore surrounded by protoplanetary disks; they form the complete sample of all available IRS spectra of T Tauri stars with infrared excesses in Taurus. We also present the IRS spectra of seven Class 0/I objects in Taurus to complete the sample of available IRS spectra of protostars in Taurus. We use spectral indices that are not significantly affected by extinction to distinguish between envelope-and disk-dominated objects. Together with data from the literature, we construct spectral energy distributions for all objects in our sample. With spectral indices derived from the IRS spectra we infer disk properties such as dust settling and the presence of inner disk holes and gaps. We find a transitional disk frequency, which is based on objects with unusually large 13-31 mu m spectral indices indicative of a wall surrounding an inner disk hole, of about 3%, and a frequency of about 20% for objects with unusually large 10 mu m features, which could indicate disk gaps. The shape and strength of the 10 mu m silicate emission feature suggests weaker 10 mu m emission and more processed dust for very low mass objects and brown dwarfs (spectral types M6-M9). These objects also display weaker infrared excess emission from their disks, but do not appear to have more settled disks than their higher-mass counterparts. We find no difference for the spectral indices and properties of the dust between single and multiple systems.
C1 [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
[Luhman, K. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
[Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA.
[Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico.
[Adame, L.; McClure, M. K.; Calvet, N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Manoj, P.; Kim, K. H.; Watson, Dan M.; Forrest, W. J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
[Sargent, B. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Green, J. D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Fischer, W. J.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA.
RP Furlan, E (reprint author), CALTECH, Jet Prop Lab, Mail Stop 264-723,4800 Oak Grove Dr, Pasadena, CA 91109 USA.
EM Elise.Furlan@jpl.nasa.gov; kluhman@astro.psu.edu;
cespaillat@cfa.harvard.edu; p.dalessio@crya.unam.mx; adamel@umich.edu;
manoj@pas.rochester.edu; khkim@pas.rochester.edu; dmw@pas.rochester.edu;
forrest@pas.rochester.edu; melisma@umich.edu; ncalvet@umich.edu;
sargent@stsci.edu; joel@astro.as.utexas.edu; wfische@utnet.utoledo.edu
OI Fischer, William J/0000-0002-3747-2496; McClure,
Melissa/0000-0003-1878-327X; Adame, Lucia/0000-0002-6328-6099; Furlan,
Elise/0000-0001-9800-6248
FU NASA; NASA through JPL/Caltech; NASA through the Spitzer Space
Telescope; National Science Foundation [AST-0544588, 0901947];
Pennsylvania State University; Eberly College of Science; Pennsylvania
Space Grant Consortium; NSF
FX This work is based on observations made with the Spitzer Space
Telescope, which is operated by the Jet Propulsion Laboratory (JPL),
California Institute of Technology (Caltech), under a contract with
NASA. Support for this work was provided by NASA through an award issued
by JPL/Caltech. E. F. was supported by NASA through the Spitzer Space
Telescope Fellowship Program, through a contract issued by JPL/Caltech
under a contract with NASA. K. L. was supported by grant AST-0544588
from the National Science Foundation. The Center for Exoplanets and
Habitable Worlds is supported by the Pennsylvania State University, the
Eberly College of Science, and the Pennsylvania Space Grant Consortium.
C. E. was supported by the National Science Foundation under Award No.
0901947. 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/Caltech,
funded by NASA and the NSF. It has also made use of the SIMBAD and
VizieR databases, operated at CDS (Strasbourg, France), NASA's
Astrophysics Data System Abstract Service, and of the NASA/IPAC Infrared
Science Archive operated by JPL, Caltech, under contract with NASA.
NR 212
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U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD JUL
PY 2011
VL 195
IS 1
AR 3
DI 10.1088/0067-0049/195/1/3
PG 45
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 790LT
UT WOS:000292590200003
ER
PT J
AU King, RS
Baker, ME
Kazyak, PF
Weller, DE
AF King, Ryan S.
Baker, Matthew E.
Kazyak, Paul F.
Weller, Donald E.
TI How novel is too novel? Stream community thresholds at exceptionally low
levels of catchment urbanization
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE aquatic biodiversity conservation; bioassessment; ecological thresholds;
indicator species; no-analog ecosystems; novel environmental gradients;
species sensitivity distribution; watershed classification
ID 9 METROPOLITAN-AREAS; NO-ANALOG FUTURE; LAND-USE; URBAN CATCHMENTS;
UNITED-STATES; BIODIVERSITY; ECOSYSTEMS; COVER; ECOLOGY; MANAGEMENT
AB Novel physical and chemical conditions of many modern ecosystems increasingly diverge from the environments known to have existed at any time in the history of Earth. The loss of natural land to urbanization is one of the most prevalent drivers of novel environments in freshwaters. However, current understanding of aquatic community response to urbanization is based heavily upon aggregate indicators of community structure and linear or wedge-shaped community response models that challenge ecological community theory. We applied a new analytical method, threshold indicator taxa analysis (TITAN), to a stream biomonitoring data set from Maryland to explicitly evaluate linear community response models to urbanization that implicitly assume individual taxa decline or increase at incrementally different levels of urbanization. We used TITAN (1) to identify the location and magnitude of greatest change in the frequency and abundance of individual taxa and (2) to assess synchrony in the location of change points as evidence for stream community thresholds in response to percent impervious cover in catchments. We documented clear and synchronous threshold declines of 110 of 238 macroinvertebrate taxa in response to low levels of impervious cover. Approximately 80% of the declining taxa did so between; similar to 0.5% and 2% impervious cover, whereas the last 20% declined sporadically from; similar to 2% to 25% impervious cover. Synchrony of individual responses resulted in distinct community-level thresholds ranging from <= 0.68% (mountains), 1.28% (piedmont), and 0.96% (coastal plain) impervious cover. Upper limits (95% confidence intervals) of community thresholds were <2% cover in all regions. Within distinct physiographic classes, higher-gradient, smaller catchments required less impervious cover than lower gradient, larger catchments to elicit community thresholds. Relatively few taxa showed positive responses to increasing impervious cover, and those that did gradually increased in frequency and abundance, approximating a linear cumulative distribution. The sharp, synchronous declines of numerous taxa established a consistent threshold response at exceptionally low levels of catchment urbanization, and uncertainty regarding the estimation of impervious cover from satellite data was mitigated by several corroborating lines of evidence. We suggest that threshold responses of communities to urban and other novel environmental gradients may be more prevalent than currently recognized.
C1 [King, Ryan S.] Baylor Univ, Ctr Reservoir & Aquat Syst Res, Dept Biol, Waco, TX 76798 USA.
[Baker, Matthew E.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA.
[Kazyak, Paul F.] Maryland Dept Nat Resources, Annapolis, MD 21401 USA.
[Weller, Donald E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP King, RS (reprint author), Baylor Univ, Ctr Reservoir & Aquat Syst Res, Dept Biol, 1 Bear Pl 97388, Waco, TX 76798 USA.
EM ryan_s_king@baylor.edu
RI Baker, Matthew/I-2839-2014;
OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437
FU U.S. EPA [R-82868401]; Baylor University; University of
Maryland-Baltimore County; U.S. EPA Region 6 [CP-966137-01]
FX We thank Ron Klauda, Scott Stranko, Tony Prochaska, Martin Hurd, Dan
Boward, and the entire MBSS team at the Maryland Department of Natural
Resources who contributed years of effort to the generation of the MBSS
data set, Dennis Whigham for his support of the SERC stream sampling,
Darrick Sparks for assistance in the field, Sean Sipple and Colleen
Roots for removal and enumeration of macroinvertebrates from samples,
Ellen Friedman at the Maryland DNR for identification of taxa from the
SERC stream samples, and Jeff Ostermiller for sharing the computer
program for standardizing macroinvertebrate counts among samples. R. S.
King and M. E. Baker conducted analyses and wrote the paper, P. F.
Kazyak led the collection of the MBSS data, and P. F. Kazyak and D. E.
Weller provided input on interpretation and helped edit the paper. R. S.
King and M. E. Baker were funded through a grant from U.S. EPA's STAR
program, agreement #R-82868401 to S. Prince and D. E. Weller, a grant
from U.S. EPA Region 6 to R. S. King, agreement #CP-966137-01, and
financial support from Baylor University to R. S. King and the
University of Maryland-Baltimore County to M. E. Baker. Although the
research described in this article has been funded in part by the United
States Environmental Protection Agency, it has not been subjected to the
Agency's required peer review and therefore does not necessarily reflect
the views of the Agency and no official endorsement should be inferred.
NR 78
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U1 7
U2 72
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD JUL
PY 2011
VL 21
IS 5
BP 1659
EP 1678
DI 10.1890/10-1357.1
PG 20
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 792RF
UT WOS:000292766100018
PM 21830709
ER
PT J
AU Weller, DE
Baker, ME
Jordan, TE
AF Weller, Donald E.
Baker, Matthew E.
Jordan, Thomas E.
TI Effects of riparian buffers on nitrate concentrations in watershed
discharges: new models and management implications
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE Chesapeake Bay watershed; collinearity; flow path analysis; land cover;
nitrate; nitrogen; nutrient discharges; riparian buffer; watershed
analysis; watershed management
ID EUROPEAN CLIMATIC GRADIENT; COASTAL-PLAIN WATERSHEDS; GULF-OF-MEXICO;
CHESAPEAKE BAY; LAND-COVER; AGRICULTURAL WATERSHEDS; NUTRIENT
INTERCEPTION; QUALITY FUNCTIONS; NITROGEN REMOVAL; TERRAIN ANALYSIS
AB Watershed analyses of nutrient removal in riparian buffers have been limited by the geographic methods used to map buffers and by the statistical models used to test and quantify buffer effects on stream nutrient levels. We combined geographic methods that account for buffer prevalence along flow paths connecting croplands to streams with improved statistical models to test for buffer effects on stream nitrate concentrations from 321 tributary watersheds to the Chesapeake Bay, USA. We developed statistical models that predict stream nitrate concentration from watershed land cover and physiographic province. We used information theoretic methods (AIC(c)) to compare models with and without buffer terms, and we demonstrate that models accounting for riparian buffers better explain stream nitrate concentrations than models using only land cover proportions. We analyzed the buffer model parameters to quantify differences within and among physiographic provinces in the potentials for nitrate loss from croplands and nitrate removal in buffers. On average, buffers in Coastal Plain study watersheds had a higher relative nitrate removal potential (95% of the inputs from cropland) than Piedmont buffers (35% of inputs). Buffers in Appalachian Mountain study watersheds were intermediate (retaining 39% of cropland inputs), but that percentage was uncertain. The absolute potential to reduce nitrate concentration was highest in the Piedmont study watersheds because of higher nitrate inputs from cropland. Model predictions for the study watersheds provided estimates of nitrate removals achieved with the existing cropland and buffer distributions. Compared to expected nitrate concentrations if buffers were removed, current buffers reduced average nitrate concentrations by 0.73 mg N/L (50% of their inputs from cropland) in the Coastal Plain study watersheds, 0.40 mg N/L (11%) in the Piedmont, and 0.08 mg N/L (5%) in the Appalachian Mountains. Restoration to close all buffer gaps downhill from croplands would further reduce nitrate concentrations by 0.66 mg N/L, 0.83 mg N/L, and 0.51 mg N/L, respectively, in the Coastal Plain, Piedmont, and Appalachian Mountain study watersheds. Aggregate nitrate removal by riparian buffers was less than suggested by many studies of field-to-stream transects, but buffer nitrate removal is significant, and restoration could achieve substantial additional removal.
C1 [Weller, Donald E.; Baker, Matthew E.; Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Weller, DE (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM wellerd@si.edu
RI Baker, Matthew/I-2839-2014;
OI Baker, Matthew/0000-0001-5069-0204; Weller, Donald/0000-0002-7629-5437
FU U.S. Environmental Protection Agency [R-82868401]; Watershed
Classification Program (USEPA) [R-831369]
FX Support for this research was provided in part by grants from the U.S.
Environmental Protection Agency's Science to Achieve Results (STAR)
Estuarine and Great Lakes (EaGLes) Program to the Atlantic Slope
Consortium (USEPA Agreement # R-82868401) and the Watershed
Classification Program (USEPA Agreement # R-831369). Although the
research described in this article has been funded by the U.S.
Environmental Protection Agency, it has not been subjected to the
Agency's required peer and policy review and therefore does not
necessarily reflect the views of the Agency, and no official endorsement
should be inferred. Further support was provided by CICEET, the
Cooperative Institute for Coastal and Estuarine Environmental
Technology. The stream data were collected with support from NSF
(BSR-89-05219, DEB-92-06811, and DEB-93-17968), NOAA (NA66RG0129), the
Governor's Research Council of Maryland, the government of Charles
County Maryland, and the Smithsonian Institution Environmental Sciences
Program. David L. Correll led the stream sampling program. We thank
Alison Baker, Kathy Boomer, Molly Van Appledorn, and Micah Ryder for
detailed feedback on early versions of the manuscript. Doug Call, James
Graves, Sal Orochena, Nancy Lee, Jennifer Bruggink, Carolyn Lieberman,
Kieren Tinning, and Michelle Coffee assembled spatial data used in some
of the analyses. D. E Weller and M. E. Baker are joint first authors.
NR 100
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U1 2
U2 57
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD JUL
PY 2011
VL 21
IS 5
BP 1679
EP 1695
PG 17
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 792RF
UT WOS:000292766100019
PM 21830710
ER
PT J
AU Kennedy, CM
Grant, EHC
Neel, MC
Fagan, WF
Marra, PP
AF Kennedy, Christina M.
Grant, Evan H. Campbell
Neel, Maile C.
Fagan, William F.
Marra, Peter P.
TI Landscape matrix mediates occupancy dynamics of Neotropical avian
insectivores
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE avian insectivores; Caribbean; colonization; extinction; Jamaica; matrix
effects; metapopulation; Neotropical birds; occupancy; tropical
conservation
ID AMAZONIAN FOREST FRAGMENTS; HABITAT FRAGMENTATION; PATCH SIZE;
METAPOPULATION DYNAMICS; BIRD ASSEMBLAGES; BOREAL FOREST; RESPONSES;
JAMAICA; MECHANISMS; DISPERSAL
AB In addition to patch-level attributes (i.e., area and isolation), the nature of land cover between habitat patches (the matrix) may drive colonization and extinction dynamics in fragmented landscapes. Despite a long-standing recognition of matrix effects in fragmented systems, an understanding of the relative impacts of different types of land cover on patterns and dynamics of species occurrence remains limited. We employed multi-season occupancy models to determine the relative influence of patch area, patch isolation, within-patch vegetation structure, and landscape matrix on occupancy dynamics of nine Neotropical insectivorous birds in 99 forest patches embedded in four matrix types (agriculture, suburban development, bauxite mining, and forest) in central Jamaica. We found that within-patch vegetation structure and the matrix type between patches were more important than patch area and patch isolation in determining local colonization and local extinction probabilities, and that the effects of patch area, isolation, and vegetation structure on occupancy dynamics tended to be matrix and species dependent. Across the avian community, the landscape matrix influenced local extinction more than local colonization, indicating that extinction processes, rather than movement, likely drive interspecific differences in occupancy dynamics. These findings lend crucial empirical support to the hypothesis that species occupancy dynamics in fragmented systems may depend greatly upon the landscape context.
C1 [Kennedy, Christina M.] Univ Maryland, Dept Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA.
[Grant, Evan H. Campbell] USGS Patuxent Wildlife Res Ctr, NE Amphibian Res & Monitoring Initiat, Laurel, MD 20708 USA.
[Neel, Maile C.] Univ Maryland, Dept Plant Sci & Landscape Architecture, College Pk, MD 20742 USA.
[Neel, Maile C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA.
[Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
RP Kennedy, CM (reprint author), Univ Maryland, Dept Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA.
EM cmk6@umd.edu
RI Grant, Evan/N-5160-2014
OI Grant, Evan/0000-0003-4401-6496
FU World Wildlife Fund; NASA; Fulbright U.S.; Washington Explorer's Club;
Cosmos Club Foundation; University of Maryland; Smithsonian Institution
(James Bond Trust); National Science Foundation
FX We thank A. Hayes-Sutton and O. Evelyn (Jamaica Forestry Department) for
sharing their knowledge of the study region and for providing logistical
field support; S. Schill (Nature Conservancy) for remote sensing data;
J. Hines and J. Nichols (USGS Patuxent Wildlife Research Center) for
statistical guidance and model programming; and T. Ricketts (World
Wildlife Fund) and two anonymous reviewers for constructive input on
previous drafts of the manuscript. Fieldwork was directed and conducted
by C. M. Kennedy with field assistance by H. Davis, C. Samuels, and M.
Beale. Research was made possible by the support of many Jamaican
researchers, nonprofit and governmental organizations, and individual
private land owners. Jamaica Forestry Department, Windalco, Alpart
Mining Venture, Jamalco bauxite mining companies, S&G Road Surfacing
Materials Ltd., and many private farmers and Mandeville citizens
permitted access to their lands. Funding was provided to C. M. Kennedy
by NASA Earth System Science Program, Fulbright U.S. Scholarship
Program, Washington Explorer's Club, Cosmos Club Foundation, and the
University of Maryland; to P. P. Marra and C. M. Kennedy by the
Smithsonian Institution (James Bond Trust); and to P. P. Marra by the
National Science Foundation.
NR 86
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U1 5
U2 66
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD JUL
PY 2011
VL 21
IS 5
BP 1837
EP 1850
PG 14
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 792RF
UT WOS:000292766100031
PM 21830722
ER
PT J
AU Moran, J
AF Moran, James
TI Donald Charles Backer obituary
SO PHYSICS TODAY
LA English
DT Biographical-Item
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Moran, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD JUL
PY 2011
VL 64
IS 7
BP 61
EP 62
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 789AE
UT WOS:000292484900024
ER
PT J
AU Songsasen, N
Woodruff, TK
Wildt, DE
AF Songsasen, N.
Woodruff, T. K.
Wildt, D. E.
TI In vitro growth and steroidogenesis of dog follicles are influenced by
the physical and hormonal microenvironment
SO REPRODUCTION
LA English
DT Article
ID PREANTRAL FOLLICULAR DEVELOPMENT; EARLY ANTRAL FOLLICLES; FREE
CULTURE-SYSTEM; STIMULATING-HORMONE; OVARIAN-FOLLICLES; PRIMORDIAL
FOLLICLES; LUTEINIZING-HORMONE; MOUSE OOCYTES; DEVELOPMENTAL COMPETENCE;
EXTRACELLULAR-MATRIX
AB The present study examined the influences of the physical and hormonal microenvironment on in vitro growth and steroidogenesis of dog follicles. Follicles were enzymatically isolated and individually encapsulated in 0.5% (w/v; n=17) or 1.5% (n=10) alginate and cultured with 0.5 IU/ml equine chorionic gonadotropin for 192 h. In a separate experiment, follicles were encapsulated in 0.5% alginate and cultured with 0 (n=22), 1 (n=23), 10 (n=20) or 100 (n=21) mu g/ml FSH for 240 h. Follicle diameter and steroid production were assessed every 48 h in both studies. Follicles encapsulated in the 0.5% alginate grew faster (P<0.05) than those cultured in the 1.5% concentration. Oestradiol (E(2)) and progesterone (P(4)) increased consistently (P<0.05) over time, and follicles in the 1.5% alginate produced more (P<0.05) P(4) than those in the 0.5% solution. Follicles cultured in the highest FSH concentration (100 mu g/ml) increased 100% in size after 240 h compared with 50 to 70% in lower dosages. E(2) concentration remained unchanged over time (P>0.05) across FSH dosages. However, P(4) increased (P<0.05) as culture progressed and with increasing FSH concentration. Results demonstrate that dog follicles cultured in alginate retain structural integrity, grow in size and are hormonally active. Lower alginate and increasing FSH concentrations promote in vitro follicle growth. However, the absence of an E(2) rise in follicles cultured in FSH alone suggests the need for LH supplementation to support theca cell differentiation and granulosa cell function. Reproduction (2011) 142 113-122
C1 [Songsasen, N.; Wildt, D. E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA.
[Woodruff, T. K.] Northwestern Univ, Feinberg Sch Med, Dept Obstet & Gynecol, Chicago, IL 60611 USA.
RP Songsasen, N (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Dept Reprod Sci, 1500 Remount Rd, Front Royal, VA 22630 USA.
EM songsasenn@si.edu
FU National Institutes of Health [KO1RR020564]
FX This research was supported by the National Institutes of Health
(KO1RR020564).
NR 78
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Z9 23
U1 0
U2 3
PU BIOSCIENTIFICA LTD
PI BRISTOL
PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT,
ENGLAND
SN 1470-1626
J9 REPRODUCTION
JI Reproduction
PD JUL
PY 2011
VL 142
IS 1
BP 113
EP 122
DI 10.1530/REP-10-0442
PG 10
WC Developmental Biology; Reproductive Biology
SC Developmental Biology; Reproductive Biology
GA 792HC
UT WOS:000292731400010
PM 21502334
ER
PT J
AU Rosindell, J
Hubbell, SP
Etienne, RS
AF Rosindell, James
Hubbell, Stephen P.
Etienne, Rampal S.
TI The Unified Neutral Theory of Biodiversity and Biogeography at Age Ten
SO TRENDS IN ECOLOGY & EVOLUTION
LA English
DT Review
ID RELATIVE SPECIES ABUNDANCE; LONG-DISTANCE DISPERSAL; ZERO-SUM
ASSUMPTION; TROPICAL FORESTS; DENSITY-DEPENDENCE; AREA RELATIONSHIPS;
MULTIPLE SAMPLES; RAIN-FORESTS; NUMBERS ADD; CORAL-REEFS
AB A decade has now passed since Hubbell published The Unified Neutral Theory of Biodiversity and Biogeography. Neutral theory highlights the importance of dispersal limitation, speciation and ecological drift in the natural world and provides quantitative null models for assessing the role of adaptation and natural selection. Significant advances have been made in providing methods for understanding neutral predictions and comparing them with empirical data. In this review, we describe the current state-of-the-art techniques and ideas in neutral theory and how these are of relevance to ecology. The future of neutral theory is promising, but its concepts must be applied more broadly beyond the current focus on species-abundance distributions.
C1 [Rosindell, James] Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England.
[Rosindell, James] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Apo Aa 340020948, Panama.
[Etienne, Rampal S.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands.
[Etienne, Rampal S.] Lincoln Univ, Fac Agr & Life Sci, Dept Soil & Phys Sci, Christchurch, New Zealand.
RP Rosindell, J (reprint author), Univ Leeds, Inst Integrat & Comparat Biol, Leeds LS2 9JT, W Yorkshire, England.
EM James@Rosindell.org
RI Etienne, Rampal/F-5835-2012;
OI Etienne, Rampal/0000-0003-2142-7612; Rosindell,
James/0000-0002-5060-9346
FU EPSRC [EP/F043112/1]; NWO
FX We thank the editor Paul Craze and two anonymous reviewers for their
helpful comments and suggestions. We also thank Bart Haegeman, David
Alonso, Egbert Leigh, Jr., Evan Economo, Fangliang He, Jonathan Eastman,
Luke Harmon, Matt Pennell, Stephen Cornell and members of the Harmon and
Rosenblum lab groups for their useful comments and discussions on the
paper. JR was funded by the EPSRC (grant EP/F043112/1); RSE acknowledges
financial support from NWO.
NR 100
TC 157
Z9 161
U1 53
U2 398
PU ELSEVIER SCIENCE LONDON
PI LONDON
PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND
SN 0169-5347
J9 TRENDS ECOL EVOL
JI Trends Ecol. Evol.
PD JUL
PY 2011
VL 26
IS 7
BP 340
EP 348
DI 10.1016/j.tree.2011.03.024
PG 9
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 791PF
UT WOS:000292676400008
PM 21561679
ER
PT J
AU Pabst, S
Zack, T
Savov, IP
Ludwig, T
Rost, D
Vicenzi, EP
AF Pabst, Sonja
Zack, Thomas
Savov, Ivan P.
Ludwig, Thomas
Rost, Detlef
Vicenzi, Edward P.
TI Evidence for boron incorporation into the serpentine crystal structure
SO AMERICAN MINERALOGIST
LA English
DT Article
DE Boron; lithium; serpentine; SIMS; ToF-SIMS; micro-Raman spectroscopy;
subduction; Mariana forearc
ID MARIANA FORE-ARC; DRILLING PROGRAM LEG-195; FLUID-MOBILE ELEMENTS; ION
MASS-SPECTROMETRY; SUBDUCTION ZONES; ISOTOPIC COMPOSITION;
VOLCANIC-ROCKS; OCEANIC PERIDOTITES; RAMAN-SPECTROSCOPY; MANTLE WEDGE
AB Serpentinite mud volcanoes from the Mariana forearc comprise B-rich mantle wedge peridotites serpentinized by slab fluids. The major component of these rocks are serpentine group minerals [Mg3Si2O5(OH)(4)], showing highly variable textural and geochemical features. Micro-Raman spectroscopy reveals that the serpentine minerals are well-crystallized lizardite and chrysotile. In situ SIMS spot analyses and element mapping via ToF-SIMS show that B is evenly distributed across serpentine grains, suggesting that serpentine, both lizardite and chrysotile in different textural regions, can host significant amounts of B (up to similar to 200 mu g/g) into its crystal structure. As such structurally bound B can only be released during recrystallization or serpentine breakdown, our results have implications for modeling of the efficiency of cross-arc fluid mobile element recycling in subduction zones and stress the importance of the hydrated forearc mantle as a reservoir for fluid mobile elements.
C1 [Pabst, Sonja; Ludwig, Thomas] Heidelberg Univ, Inst Geowissensch, D-69120 Heidelberg, Germany.
[Zack, Thomas] Johannes Gutenberg Univ Mainz, Inst Geowissensch, D-55099 Mainz, Germany.
[Savov, Ivan P.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England.
[Rost, Detlef; Vicenzi, Edward P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
RP Pabst, S (reprint author), Heidelberg Univ, Inst Geowissensch, D-69120 Heidelberg, Germany.
EM sonja.pabst@geow.uni-heidelberg.de
RI Zack, Thomas/C-6153-2009; Zack, Thomas/K-7228-2013
OI Zack, Thomas/0000-0003-4747-4134
FU Deutsche Forschungsgemeinschalt (DFG) [Za285/4]; B. Schmidt
(micro-Raman); H.-P. Meyer (EMP); U.S. National Science Foundation (NSF)
FX This study is part of the Ph.D. work of the first author, funded by
grants front the Deutsche Forschungsgemeinschalt (DFG, Za285/4).
Analytical work was expertly supported by B. Schmidt (micro-Raman) and
H.-P. Meyer (EMP). The manuscript has benefitted from the fruitful
discussions with E.S. Grew, J. Hopp, and G. Topuz and the scientific
support from P. Fryer and M. Mottl. We also thank P. Tomascak and A.
Brearley for helpful reviews of a first version of this manuscript. The
samples were allocated to I. Savoy by the Ocean Drilling Program (ODP
Leg 195, Site 1200). O.D.P. is sponsored by the U.S. National Science
Foundation (NSF) and participating countries under the management of
Joint Oceanographic Institutions (JOI), Inc.
NR 77
TC 15
Z9 15
U1 1
U2 26
PU MINERALOGICAL SOC AMER
PI CHANTILLY
PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA
SN 0003-004X
EI 1945-3027
J9 AM MINERAL
JI Am. Miner.
PD JUL
PY 2011
VL 96
IS 7
BP 1112
EP 1119
DI 10.2138/am.2011.3709
PG 8
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 787JM
UT WOS:000292372400017
ER
PT J
AU Harmon, RS
Shughrue, KM
Remus, JJ
Wise, MA
East, LJ
Hark, RR
AF Harmon, Russell S.
Shughrue, Katrina M.
Remus, Jeremiah J.
Wise, Michael A.
East, Lucille J.
Hark, Richard R.
TI Can the provenance of the conflict minerals columbite and tantalite be
ascertained by laser-induced breakdown spectroscopy?
SO ANALYTICAL AND BIOANALYTICAL CHEMISTRY
LA English
DT Article
DE Laser-induced breakdown spectroscopy; LIBS; Conflict minerals;
Columbite-tantalite; Coltan; PLSDA
ID GRANITIC PEGMATITES; CHEMISTRY; PROVINCE
AB Conflict minerals is a term applied to ores mined in conditions of armed conflict and human rights abuse. Niobium and tantalum are two rare metals whose primary natural occurrence is in the complex oxide minerals columbite and tantalite, the ore of which is commonly referred to as coltan. The illicit export of coltan ore from the Democratic Republic of the Congo is thought to be responsible for financing the ongoing civil conflicts in this region. Determining the chemical composition of an ore is one of the means of ascertaining its provenance. Laser-induced breakdown spectroscopy (LIBS) offers a means of rapidly distinguishing different geographic sources for a mineral because the LIBS plasma emission spectrum provides the complete chemical composition (i.e., "chemical fingerprint") of any material in real time. To test this idea for columbite-tantalite, three sample sets were analyzed. Partial least squares discriminant analysis (PLSDA) allows correct sample-level geographic discrimination at a success rate exceeding 90%.
C1 [Shughrue, Katrina M.; Hark, Richard R.] Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA.
[Harmon, Russell S.] ARL Army Res Off, Div Environm Sci, Durham, NC 27709 USA.
[Remus, Jeremiah J.] Clarkson Univ, Dept Elect & Comp Engn, Potsdam, NY 13699 USA.
[Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA.
[East, Lucille J.] Appl Spectra Inc, Fremont, CA 94538 USA.
RP Hark, RR (reprint author), Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA.
EM hark@juniata.edu
FU Army Research Laboratory; II-VI Foundation
FX This research was supported by Army Research Laboratory Fellow funding
to RSH and financial support to KMS from the II-VI Foundation and was
facilitated by technical support from Applied Spectra, Inc.
NR 21
TC 22
Z9 22
U1 3
U2 35
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 1618-2642
J9 ANAL BIOANAL CHEM
JI Anal. Bioanal. Chem.
PD JUL
PY 2011
VL 400
IS 10
BP 3377
EP 3382
DI 10.1007/s00216-011-5015-2
PG 6
WC Biochemical Research Methods; Chemistry, Analytical
SC Biochemistry & Molecular Biology; Chemistry
GA 789IE
UT WOS:000292508200020
PM 21537914
ER
PT J
AU Warkentin, KM
AF Warkentin, Karen M.
TI Environmentally Cued Hatching across Taxa: Embryos Respond to Risk and
Opportunity
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID PREDATION RISK; PHENOTYPIC PLASTICITY; ADAPTIVE PLASTICITY; NEURONS
MEDIATE; PARENTAL CARE; CHEMICAL CUES; EGGS; MECHANISMS; BIOLOGY; OXYGEN
AB Most animals begin life in eggs, protected and constrained by a capsule, shell, or other barrier. As embryos develop, their needs and abilities change, altering the costs and benefits of encapsulation, and the risks and opportunities of the outside world. When the cost/benefit ratio is better outside the egg, animals should hatch. Adaptive timing of hatching evolves in this context. However, many environmental variables affect the optimal timing of hatching so there is often no consistent best time. Across a broad range of animals, from flatworms and snails to frogs and birds, embryos hatch at different times or at different developmental stages in response to changing risks or opportunities. Embryos respond to many types of cues, assessed via different sensory modalities. Some responses appear simple. Others are surprisingly complex and sophisticated. Parents also manipulate the timing of hatching. The number and breadth of examples of cued hatching suggest that, in the absence of specific information, we should not assume that hatching timing is fixed. Our challenge now is to integrate information on the timing of hatching across taxa to better understand the diversity of patterns and how they are structured in relation to different types of environmental and developmental variation. As starting points for comparative studies, I: (1) suggest a framework based on heterokairy-individual, plastic variation in the rate, timing, or sequence of developmental events and processes-to describe patterns and mechanisms of variation in the timing of hatching; (2) briefly review the distribution of environmentally cued hatching across the three major clades of Bilateria, highlighting the diverse environmental factors and mechanisms involved; and (3) discuss factors that shape the diversity of plastic and fixed timing of hatching, drawing on evolutionary theory on phenotypic plasticity which directs our attention to fitness trade-offs, environmental heterogeneity, and predictive cues. Combining mechanistic and evolutionary perspectives is necessary because development changes organismal interactions with the environment. Integrative and comparative studies of the timing of hatching will improve our understanding of embryos as both evolving and developing organisms.
C1 [Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA.
EM kwarken@bu.edu
FU Society for Integrative and Comparative Biology; National Science
Foundation [IOS-1036933, HRD-0820175, DEB-0716923]; Smithsonian Tropical
Research Institute; Boston University
FX This symposium was supported by the Society for Integrative and
Comparative Biology and all of its divisions, the National Science
Foundation (IOS-1036933 to K. M., K. W., and R. S. and HRD-0820175 to
Boston University). The research was supported by a Smithsonian Tropical
Research Institute Senior Fellowship, Boston University, and the
National Science Foundation (DEB-0716923).
NR 87
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U1 2
U2 32
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD JUL
PY 2011
VL 51
IS 1
BP 14
EP 25
DI 10.1093/icb/icr017
PG 12
WC Zoology
SC Zoology
GA 786MY
UT WOS:000292313800002
PM 21705799
ER
PT J
AU Christy, JH
AF Christy, John H.
TI Timing of Hatching and Release of Larvae by Brachyuran Crabs: Patterns,
Adaptive Significance and Control
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID RHITHROPANOPEUS-HARRISII GOULD; ESTUARINE TERRESTRIAL CRAB; INTERTIDAL
CRABS; FIDDLER-CRABS; CHEMICAL CUES; UCA-THAYERI; REPRODUCTIVE
SYNCHRONY; EMBRYONIC-DEVELOPMENT; PLANKTIVOROUS FISHES; TIDAL REGIMES
AB Most semiterrestrial, intertidal and shallow subtidal brachyuran crabs that live in tropical and warm temperate estuaries, bays and protected coasts world-wide release their planktonic larvae near the times of nocturnal high tides on the larger amplitude tides in the biweekly or monthly cycles of tidal amplitude. Crab larvae usually emigrate quickly to the sea where they develop to return as postlarvae to settle in habitats suitable for their survival. Predators of larvae are more abundant where larvae are released than where they develop, suggesting that this migration from estuaries to the sea reduces predation on larvae. Crabs with larvae that are relatively well-protected by spines and cryptic colors do not emigrate and often lack strong reproductive cycles, lending support to this explanation. Adults control the timing of the release of larvae with respect to the biweekly and monthly cycles of tidal amplitude by controlling when they court and mate and females control when development begins by controlling when they ovulate and allow their eggs to be fertilized by stored sperm. By changing the time they breed, fiddler crabs (Uca terpsichores) compensate for the effects of spatial and temporal variation in incubation temperature on development rates so that embryos are ready to hatch at the appropriate time. Control of the diel and tidal timing of hatching and of release of larvae varies with where adults live. Females of the more terrestrial species often move from protected incubation sites, sometimes far from water, and they largely control the precise time, both, of hatching and of release of larvae. Females of intertidal species also may influence when embryos begin to hatch. Upon hatching, a chemical cue is released that stimulates the female to pump her abdomen, causing rapid hatching and release of all larvae in her clutch. Embryos, rather than females, largely control hatching in subtidal species, perhaps because females incubate their eggs where they release their larvae. Topics for further study include the mechanism whereby adults regulate the timing of breeding, the mechanisms by which females control development rates of embryos, the nature of communication between females and embryos that leads to precise and synchronous hatching by the number (often thousands) of embryos in a clutch, and the causes of selection for such precision. The timing of hatching and of release of larvae by cold-temperate, Arctic, and Antarctic species and by fully terrestrial and freshwater tropical species has received little attention.
C1 Smithsonian Trop Res Inst, Panama City, Panama.
RP Christy, JH (reprint author), Smithsonian Trop Res Inst, MRC 0580-08,Apartado 0843-03092, Panama City, Panama.
EM christyj@si.edu
FU Society for Integrative and Comparative Biology (SICB); Society for
Integrative and Comparative Biology (SICB), Division of Animal Behavior
(DAB); Society for Integrative and Comparative Biology (SICB), Division
of Comparative Physiology and Biochemistry (DCPB); Society for
Integrative and Comparative Biology (SICB), Division of Developmental
and Cellular Biology (DDCB); Society for Integrative and Comparative
Biology (SICB), Division of Evolutionary Developmental Biology (DEDB);
Society for Integrative and Comparative Biology (SICB), Division of
Invertebrate Zoology (DIZ); US National Science Foundation
[IOS-1036933]; Smithsonian Tropical Research Institute
FX Funding of this symposium and my participation in it was provided by the
Society for Integrative and Comparative Biology (SICB), and the
following Divisions within the Society: Animal Behavior (DAB),
Comparative Physiology and Biochemistry (DCPB), Developmental and
Cellular Biology (DDCB), Evolutionary Developmental Biology (DEDB), and
Invertebrate Zoology (DIZ), and by the US National Science Foundation
(IOS-1036933). The Smithsonian Tropical Research Institute supported my
research on the reproductive behavior and biology of the fiddler crabs
of Panama.
NR 70
TC 39
Z9 40
U1 0
U2 34
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
EI 1557-7023
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD JUL
PY 2011
VL 51
IS 1
BP 62
EP 72
DI 10.1093/icb/icr013
PG 11
WC Zoology
SC Zoology
GA 786MY
UT WOS:000292313800006
PM 21593141
ER
PT J
AU Warkentin, KM
AF Warkentin, Karen M.
TI Plasticity of Hatching in Amphibians: Evolution, Trade-Offs, Cues and
Mechanisms
SO INTEGRATIVE AND COMPARATIVE BIOLOGY
LA English
DT Article
ID RED-EYED TREEFROG; FROG PSEUDOPHRYNE-BIBRONI; PREDATION RISK; ADAPTIVE
PLASTICITY; AGALYCHNIS-CALLIDRYAS; EMBRYONIC-DEVELOPMENT; LIFE-HISTORY;
HYPEROLIUS-SPINIGULARIS; PHENOTYPIC PLASTICITY; SALAMANDER EGGS
AB Many species of frogs and salamanders, in at least 12 families, alter their timing of hatching in response to conditions affecting mortality of eggs or larvae. Some terrestrially laid or stranded embryos wait to hatch until they are submerged in water. Some embryos laid above water accelerate hatching if the eggs are dehydrating; others hatch early if flooded. Embryos can hatch early in response to predators and pathogens of eggs or delay hatching in response to predators of larvae; some species do both. The phylogenetic pattern of environmentally cued hatching suggests that similar responses have evolved convergently in multiple amphibian lineages. The use of similar cues, including hypoxia and physical disturbance, in multiple contexts suggests potential shared mechanisms underlying the capacity of embryos to respond to environmental conditions. Shifts in the timing of hatching often have clear benefits, but we know less about the trade-offs that favor plasticity, the mechanisms that enable it, and its evolutionary history. Some potentially important types of cued hatching, such as those involving embryo-parent interactions, are relatively unexplored. I discuss promising directions for research and the opportunities that the hatching of amphibians offers for integrative studies of the mechanisms, ecology and evolution of a critical transition between life-history stages.
C1 [Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA.
[Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City, Panama.
RP Warkentin, KM (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA.
EM kwarken@bu.edu
FU Society for Integrative and Comparative Biology and all its divisions;
National Science Foundation [IOS-1036933, HRD-0820175, DEB-0716923,
IBN-0234439]; Smithsonian Tropical Research Institute; Boston University
FX This symposium was supported by the Society for Integrative and
Comparative Biology and all its divisions, and the National Science
Foundation (IOS-1036933 to K. M., K. W. and R. S. and HRD-0820175 to
Boston University). This research was supported by a Smithsonian
Tropical Research Institute Senior Fellowship, Boston University, and
the National Science Foundation (DEB-0716923 and IBN-0234439).
NR 104
TC 44
Z9 45
U1 1
U2 52
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1540-7063
J9 INTEGR COMP BIOL
JI Integr. Comp. Biol.
PD JUL
PY 2011
VL 51
IS 1
BP 111
EP 127
DI 10.1093/icb/icr046
PG 17
WC Zoology
SC Zoology
GA 786MY
UT WOS:000292313800011
PM 21642239
ER
PT J
AU Visser, MD
Jongejans, E
van Breugel, M
Zuidema, PA
Chen, YY
Kassim, AR
de Kroon, H
AF Visser, Marco D.
Jongejans, Eelke
van Breugel, Michiel
Zuidema, Pieter A.
Chen, Yu-Yun
Kassim, Abdul Rahman
de Kroon, Hans
TI Strict mast fruiting for a tropical dipterocarp tree: a demographic
cost-benefit analysis of delayed reproduction and seed predation
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE delayed reproduction; demography; Dipterocarpaceae; elasticity;
life-history evolution; plant population and community dynamics;
predator satiation hypothesis; stochastic matrix model
ID RAIN-FOREST; EVOLUTIONARY ECOLOGY; SPATIAL-PATTERNS;
RESOURCE-ALLOCATION; WOODY-PLANTS; EL-NINO; RECRUITMENT; DISPERSAL;
DYNAMICS; IMPACT
AB 1. Masting, the production of large seed crops at intervals of several years, is a reproductive adaptation displayed by many tree species. The predator satiation hypothesis predicts that starvation of seed predators between mast years and satiation during mast years decreases seed predation and thus enhances tree regeneration.
2. Mast fruiting comes at demographic costs such as missed reproduction opportunities and increased density-dependence of recruits, but it remains unknown if predator satiation constitutes a sufficiently large benefit for masting to evolve as a viable life-history strategy. So far, no studies have quantified the net fitness consequences of masting.
3. Using a long-term demographic data set of the dipterocarp Shorea leprosula in a Malaysian forest, we constructed stochastic matrix population models and performed a demographic cost benefit analysis.
4. For observed values of mast frequency and seed predation rates, we show that strict masting strongly increases fitness compared with fruiting annually. Model results also show that the demographic costs of mast fruiting are very low compared to the demographic losses due to seed predation in a scenario of annual fruiting. Finally, we find that mast fruiting would still be selected for even at low levels of seed predation and when including additional costs such as decreased adult growth rates, limiting crop size and density-dependent seedling survival.
5. Synthesis. Our results are consistent with the predictions of the predator satiation hypothesis: mast fruiting increases fitness for a range of seed predation levels. Under seed predation pressure annually fruiting species are at a strong disadvantage and as a result a mast fruiting strategy may swiftly confer a fitness advantage. Our study shows that demographic modelling allows the weighing of fitness benefits and costs of life-history phenomena such as strict masting.
C1 [Visser, Marco D.; van Breugel, Michiel] Univ Wageningen & Res Ctr, NL-6880 GB Velp, Netherlands.
[Visser, Marco D.; Jongejans, Eelke; de Kroon, Hans] Radboud Univ Nijmegen, Inst Water & Wetland Res, Dept Expt Plant Ecol, NL-6525 AJ Nijmegen, Netherlands.
[van Breugel, Michiel] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Ancon, Panama.
[Zuidema, Pieter A.] Univ Utrecht, Inst Environm Biol Ecol & Biodivers, NL-3584 CH Utrecht, Netherlands.
[Chen, Yu-Yun] Natl Donghwa Univ, Dept Nat Resources & Environm Studies, Hualien 974, Taiwan.
[Kassim, Abdul Rahman] Forest Res Inst Malaysia, Nat Forest Div, Kuala Lumpur, Malaysia.
RP Visser, MD (reprint author), Univ Wageningen & Res Ctr, Van Hall Larenstein,Larensteinselaan 26A, NL-6880 GB Velp, Netherlands.
EM rn.visser@science.ru.nl
RI Zuidema, Pieter/C-8951-2009; de Kroon, Hans/B-3359-2009; Jongejans,
Eelke/B-4832-2008;
OI Zuidema, Pieter/0000-0001-8100-1168; de Kroon, Hans/0000-0001-6151-3561;
Jongejans, Eelke/0000-0003-1148-7419; van Breugel,
Michiel/0000-0003-2778-7803
FU Smithsonian Tropical Research Institute; Netherlands Organization for
Scientific Research (NWO) [863.08.006]; HSBC; ERC [242955]; US NSF
[DEB-0108388]; NSF [DEB-0075334]
FX We thank the Forest Research Institute Malaysia (FRIM) for logistical
support in the field. We are grateful for the helpful comments of four
anonymous reviewers. In addition, we thank W. van der Werf, P.A. Jansen
and S. Tuljapurkar for their comments and discussions. M.D.V.
acknowledges funding from the Smithsonian Tropical Research Institute
short-term fellowship program. E.J. acknowledges funding from the
Netherlands Organization for Scientific Research (NWO-veni grant,
863.08.006). M.v.B. acknowledges support from the HSBC Climate
Partnership. P.A.Z. was supported by ERC grant 242955. We acknowledge
S.P.Hubbell, S.J. Wright and I-Fang Sun for their effort to establish
the Pasoh forest dynamics plot seed and seedling monitoring project with
financial aid from US NSF (grant no.: DEB-0108388). The Pasoh forest
50-ha dynamics plot research was in part supported by NSF grant
DEB-0075334 to P.S. Ashton and S.J. Davies.
NR 97
TC 23
Z9 23
U1 2
U2 81
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD JUL
PY 2011
VL 99
IS 4
BP 1033
EP 1044
DI 10.1111/j.1365-2745.2011.01825.x
PG 12
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 788BG
UT WOS:000292419800016
ER
PT J
AU Hong, T
AF Hong, Terry
TI This Burns My Heart
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA.
RP Hong, T (reprint author), Smithsonian BookDragon, 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 2011
VL 136
IS 12
BP 73
EP 73
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 789BF
UT WOS:000292487600092
ER
PT J
AU Puillandre, N
Meyer, CP
Bouchet, P
Olivera, BM
AF Puillandre, Nicolas
Meyer, Christopher P.
Bouchet, Philippe
Olivera, Baldomero M.
TI Genetic divergence and geographical variation in the deep-water Conus
orbignyi complex (Mollusca: Conoidea)
SO ZOOLOGICA SCRIPTA
LA English
DT Article
ID SPECIES DELIMITATION; MOLECULAR PHYLOGENY; MITOCHONDRIAL-DNA; MARINE
GASTROPOD; DIFFERENTIATION; POPULATIONS; DIVERSITY; DISCOVERY; PEPTIDES;
PACIFIC
AB Puillandre, N., Meyer, C. P., Bouchet, P. & Olivera, B. M. (2011). Genetic divergence and geographical variation in the deep-water Conus orbignyi complex (Mollusca: Conoidea). - Zoologica Scripta, 40, 350-363.
The cone snails (family Conidae) are a hyperdiverse lineage of venomous gastropods. Two standard markers, COI and ITS2, were used to define six genetically divergent groups within a subclade of Conidae that includes Conus orbignyi; each of these was then evaluated based on their shell morphology. We conclude that three forms, previously regarded as subspecies of C. orbignyi are distinct species, now recognized as C. orbignyi, C. elokismenos and C. coriolisi. In addition, three additional species (C. pseudorbignyi, C. joliveti and C. comatosa) belong to this clade. Some of the proposed species (e. g. C. elokismenos) are possibly in turn complexes comprising multiple species. Groups such as Conidae illustrate the challenges generally faced in species delimitation in biodiverse lineages. In the case of C. orbignyi complex, they are not only definable, genetically divergent lineages, but also considerable geographical variation within each group. Our study suggests that an intensive analysis of multiple specimens within a single locality helps to minimize the confounding effects of geographical variation and can be a useful starting point for circumscribing different species within such a confusing complex.
C1 [Puillandre, Nicolas; Olivera, Baldomero M.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
[Puillandre, Nicolas; Bouchet, Philippe] Museum Natl Hist Nat, F-75005 Paris, France.
[Meyer, Christopher P.] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA.
RP Puillandre, N (reprint author), Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA.
EM puillandre@biology.utah.edu; MeyerC@si.edu; pbouchet@mnhn.fr;
olivera@biology.utah.edu
FU US National Institute of General Medical Sciences [GM48677]; Fogarty
Centre, NIH [1U01TW008163]; Lounsbery Foundation; Total Foundation;
Niarchos Foundation
FX This work was supported in part by Program grant GM48677 from the US
National Institute of General Medical Sciences (to BMO) and by ICBG
grant 1U01TW008163 from the Fogarty Centre, NIH, Margo Haygood,
Principal Investigator. Key material originates from the following
expeditions. (A) Philippines. The PANGLAO 2005 cruise on board M/V
DA-BFAR associated the USC, MNHN (co-PI Philippe Bouchet) and the
Philippines Bureau of Fisheries and Aquatic Research (BFAR; co-PI
Ludivina Labe). The AURORA 2007 cruise also on board M/V DA-BFAR
associated the National Museum of the Philippines (NMP, co-PI Marivene
Manuel), MNHN (co-PI Philippe Bouchet) and BFAR, and was made possible
through a grant from the Lounsbery Foundation. (B) Vanuatu. Material
originates from the MNHN-IRD-PNI Santo 2006 expedition, which was made
possible by grants, among others, from the Total Foundation and the
Niarchos Foundation. (C) Coral Sea and Solomon Islands. The EBISCO and
SALOMON cruises took place on board R/V Alis deployed from Noumea by the
Institut de Recherche pour le Developpement (IRD). Bertrand Richer de
Forges was cruise leader for the Solomons, Coral Sea and Vanuatu
expeditions. Ellen Strong and Yuri Kantor are thanked for their role in
molecular sampling during these expeditions. The authors thank Virginie
Heros for assistance in monitoring Aurora 2007 material and Hans-Jorg
Niederhofer (Staatliches Museum fur Naturkunde Stuttgart), Virginie
Heros (Museum National d'Histoire Naturelle, Paris) and Paul Callomon
(Academy of Natural Sciences, Philadelphia) for their help in providing
pictures of type specimens.
NR 56
TC 10
Z9 11
U1 1
U2 17
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0300-3256
J9 ZOOL SCR
JI Zool. Scr.
PD JUL
PY 2011
VL 40
IS 4
BP 350
EP 363
DI 10.1111/j.1463-6409.2011.00478.x
PG 14
WC Evolutionary Biology; Zoology
SC Evolutionary Biology; Zoology
GA 789VH
UT WOS:000292544800003
PM 21712968
ER
PT J
AU Broderick, AE
Loeb, A
Reid, MJ
AF Broderick, Avery E.
Loeb, Abraham
Reid, Mark J.
TI LOCALIZING SAGITTARIUS A* AND M87 ON MICROARCSECOND SCALES WITH
MILLIMETER VERY LONG BASELINE INTERFEROMETRY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; black hole physics; Galaxy: center; proper motions;
submillimeter: general; techniques: interferometric
ID ACTIVE GALACTIC NUCLEI; MASSIVE BLACK-HOLE; ALL-SKY SURVEY; SPECTRAL
ENERGY-DISTRIBUTIONS; GRAVITATIONAL-WAVE SOURCES; DISCRETE
RADIO-SOURCES; HIGH-FREQUENCY VLBI; SGR-A; STELLAR ORBITS; PROPER MOTION
AB With the advent of the Event Horizon Telescope (EHT), a millimeter/submillimeter very long baseline interferometer (VLBI), it has become possible to image a handful of black holes with sub-horizon resolutions. However, these images do not translate into microarcsecond absolute positions due to the lack of absolute phase information when an external phase reference is not used. Due to the short atmospheric coherence time at these wavelengths, nodding between the source and phase reference is impractical. However, here we suggest an alternative scheme which makes use of the fact that many of the VLBI stations within the EHT are arrays in their own right. With this we show that it should be possible to absolutely position the supermassive black holes at the centers of the Milky Way (Sgr A*) and M87 relative to nearby objects with precisions of roughly 1 mu as. This is sufficient to detect the perturbations to Sgr A*'s position resulting from interactions with the stars and stellar-mass black holes in the Galactic cusp on year timescales, and severely constrain the astrophysically relevant parameter space for an orbiting intermediate-mass black hole, implicated in some mechanisms for producing the young massive stars in the Galactic center. For M87, it allows the registering of millimeter images, in which the black hole may be identified by its silhouette against nearby emission, and existing larger-scale radio images, eliminating present ambiguities in the nature of the radio core and inclination, opening angle, and source of the radio jet.
C1 [Broderick, Avery E.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada.
[Loeb, Abraham] Harvard Univ, Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA.
[Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Broderick, AE (reprint author), Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada.
EM aeb@cita.utoronto.ca
FU National Aeronautics and Space Administration [NNX08AL43G, NNA09DB30A];
NSF [AST-0907890]; Beatrice D. Tremaine Fellowship
FX We thank Irwin Shapiro, Sheperd Doeleman, and Vincent Fish for
enlightening discussions and suggestions. 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
work was supported in part by NSF grant AST-0907890 and NASA grants
NNX08AL43G and NNA09DB30A. A.E.B. gratefully acknowledges the support of
the Beatrice D. Tremaine Fellowship.
NR 182
TC 14
Z9 14
U1 0
U2 6
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 57
DI 10.1088/0004-637X/735/1/57
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300057
ER
PT J
AU Bromley, BC
Kenyon, SJ
AF Bromley, Benjamin C.
Kenyon, Scott J.
TI MIGRATION OF PLANETS EMBEDDED IN A CIRCUMSTELLAR DISK
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; planet-disk interactions;
planets and satellites: formation
ID SPECTRAL ENERGY-DISTRIBUTIONS; BODY-COAGULATION CODE; GAS GIANT PLANETS;
LOW-MASS PLANETS; T-TAURI STARS; OLIGARCHIC GROWTH; DETERMINISTIC MODEL;
PLANETESIMAL DISKS; ORBITAL MIGRATION; TORQUE FORMULA
AB Planetary migration poses a serious challenge to theories of planet formation. In gaseous and planetesimal disks, migration can remove planets as quickly as they form. To explore migration in a planetesimal disk, we combine analytic and numerical approaches. After deriving general analytic migration rates for isolated planets, we use N-body simulations to confirm these results for fast and slow migration modes. Migration rates scale as m(-1) (for massive planets) and (1 + (e(H)/3)(3))(-1), where m is the mass of a planet and e(H) is the eccentricity of the background planetesimals in Hill units. When multiple planets stir the disk, our simulations yield the new result that large-scale migration ceases. Thus, growing planets do not migrate through planetesimal disks. To extend these results to migration in gaseous disks, we compare physical interactions and rates. Although migration through a gaseous disk is an important issue for the formation of gas giants, we conclude that migration has little impact on the formation of terrestrial planets.
C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA.
[Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA.
EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu
OI Kenyon, Scott/0000-0003-0214-609X
FU NASA [NNX10AF35G]
FX Advice and comments from M. Duncan, M. Geller, D. Kirsh, S. Tremaine, A.
Youdin, and the anonymous referee greatly improved our presentation.
Portions of this project were supported by NASA's Astrophysics Theory
Program, and the Origin of Solar Systems Program through grant
NNX10AF35G.
NR 121
TC 29
Z9 30
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 29
DI 10.1088/0004-637X/735/1/29
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300029
ER
PT J
AU Cannon, JM
Most, HP
Skillman, ED
Weisz, DR
Cook, D
Dolphin, AE
Kennicutt, RC
Lee, J
Seth, A
Walter, F
Warren, SR
AF Cannon, John M.
Most, Hans P.
Skillman, Evan D.
Weisz, Daniel R.
Cook, David
Dolphin, Andrew E.
Kennicutt, Robert C., Jr.
Lee, Janice
Seth, Anil
Walter, Fabian
Warren, Steven R.
TI THE M81 GROUP DWARF IRREGULAR GALAXY DDO 165. I. HIGH-VELOCITY NEUTRAL
GAS IN A POST-STARBURST SYSTEM
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: individual (DDO 165);
galaxies: irregular
ID STAR-FORMATION HISTORIES; H-I; INTERSTELLAR-MEDIUM; HOLMBERG-II;
SUPERGIANT SHELL; STELLAR FEEDBACK; NEARBY GALAXIES; NGC-5194 M51A;
FORMATION LAW; LOCAL VOLUME
AB We present new multi-configuration Very Large Array Hi spectral line observations of the M81 group dwarf irregular post-starburst galaxy DDO165. The Hi morphology is complex, with multiple column density peaks surrounding a large region of very low Hi surface density that is offset from the center of the stellar distribution. The bulk of the neutral gas is associated with the southern section of the galaxy; a secondary peak in the north contains similar to 15% of the total Hi mass. These components appear to be kinematically distinct, suggesting that either tidal processes or large-scale blowout have recently shaped the interstellar medium (ISM) of DDO165. Using spatially resolved position-velocity maps, we find multiple localized high-velocity gas features. Cross-correlating with radius-velocity analyses, we identify eight shell/hole structures in the ISM with a range of sizes (similar to 400-900 pc) and expansion velocities (similar to 7- 11 km s(-1)). These structures are compared with narrow- and broadband imaging from the Kitt Peak National Observatory and the Hubble Space Telescope (HST). Using the latter data, recent works have shown that DDO 165's previous "burst" phase was extended temporally (greater than or similar to 1 Gyr). We thus interpret the high-velocity gas features, Hi holes, and kinematically distinct components of the galaxy in the context of the immediate effects of "feedback" from recent star formation (SF). In addition to creating Hi holes and shells, extended SF events are capable of creating localized high-velocity motion of the surrounding interstellar material. A companion paper connects the energetics from the Hi and HST data.
C1 [Cannon, John M.; Most, Hans P.] Macalester Coll, Dept Phys & Astron, St Paul, MN 55105 USA.
[Skillman, Evan D.; Weisz, Daniel R.; Warren, Steven R.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Cook, David] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
[Kennicutt, Robert C., Jr.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Lee, Janice] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Seth, Anil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walter, Fabian] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Cannon, JM (reprint author), Macalester Coll, Dept Phys & Astron, 1600 Grand Ave, St Paul, MN 55105 USA.
EM jcannon@macalester.edu; skillman@astro.umn.edu; dweisz@astro.umn.edu;
dcook12@uwyo.edu; adolphin@raytheon.com; robk@ast.cam.ac.uk;
jlee@obs.carnegiescience.edu; aseth@cfa.harvard.edu; walter@mpia.de;
warren@astro.umn.edu
FU Space Telescope Science Institute, NASA [GO-10605]; National Aeronautics
and Space Administration [NAS5-26555]; Macalester College; Penrose
Fellowships; NASA's Astrophysics Data System
FX Partial support for this work was provided by NASA through grant
GO-10605 from the Space Telescope Science Institute, which is operated
by AURA, INC., under NASA contract NAS5-26555. J.M.C. and H.P.M. thank
Macalester College for research support. D.R.W. and S.R.W. are grateful
for support from Penrose Fellowships. This investigation 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.
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
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IS 1
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DI 10.1088/0004-637X/735/1/35
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WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300035
ER
PT J
AU Cannon, JM
Most, HP
Skillman, ED
Weisz, DR
Cook, D
Dolphin, AE
Kennicutt, RC
Lee, J
Seth, A
Walter, F
Warren, SR
AF Cannon, John M.
Most, Hans P.
Skillman, Evan D.
Weisz, Daniel R.
Cook, David
Dolphin, Andrew E.
Kennicutt, Robert C., Jr.
Lee, Janice
Seth, Anil
Walter, Fabian
Warren, Steven R.
TI THE M81 GROUP DWARF IRREGULAR GALAXY DDO 165. II. CONNECTING RECENT STAR
FORMATION WITH INTERSTELLAR MEDIUM STRUCTURES AND KINEMATICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: dwarf; galaxies: evolution; galaxies: individual (DDO 165);
galaxies: irregular
ID RED GIANT BRANCH; ELEMENTAL ABUNDANCE VARIATIONS;
SMALL-MAGELLANIC-CLOUD; CHEMICAL ENRICHMENT; NEARBY GALAXIES; MASSIVE
STARS; DISTANCE INDICATOR; RESOLVED GALAXIES; FORMATION HISTORY;
SUPERNOVA RATE
AB We compare the stellar populations and complex neutral gas dynamics of the M81 group dIrr galaxy DDO 165 using data from the Hubble Space Telescope and the Very Large Array. Cannon et al. in Paper I of this series identified two kinematically distinct Hi components, multiple localized high velocity gas features, and eight Hi holes and shells (the largest of which spans similar to 2.2 x 1.1 kpc). Using the spatial and temporal information from the stellar populations in DDO 165, we compare the patterns of star formation (SF) over the past 500 Myr with the Hi dynamics. We extract localized star formation histories within 6 of the 8 Hi holes identified in Paper I, as well as 23 other regions that sample a range of stellar densities and neutral gas properties. From population synthesis modeling, we derive the energy outputs (from stellar winds and supernovae) of the stellar populations within these regions over the last 100 Myr, and compare with refined estimates of the energies required to create the Hi holes. In all cases, we find that "feedback" is energetically capable of creating the observed structures in the interstellar medium (ISM). Numerous regions with significant energy inputs from feedback lack coherent Hi structures but show prominent localized high velocity gas features; this feedback signature is a natural product of temporally and spatially distributed SF. In DDO 165, the extended period of heightened SF activity (lasting more than 1 Gyr) is energetically capable of creating the observed holes and high velocity gas features in the neutral ISM.
C1 [Cannon, John M.; Most, Hans P.] Macalester Coll, Dept Phys & Astron, St Paul, MN 55105 USA.
[Skillman, Evan D.; Weisz, Daniel R.; Warren, Steven R.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Cook, David] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
[Kennicutt, Robert C., Jr.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
[Lee, Janice] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA.
[Seth, Anil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walter, Fabian] Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Cannon, JM (reprint author), Macalester Coll, Dept Phys & Astron, 1600 Grand Ave, St Paul, MN 55105 USA.
EM jcannon@macalester.edu; hmost@macalester.edu; skillman@astro.umn.edu;
dweisz@astro.umn.edu; dcook12@uwyo.edu; adolphin@raytheon.com;
robk@ast.cam.ac.uk; jlee@obs.carnegiescience.edu; aseth@cfa.harvard.edu;
walter@mpia.de; warren@astro.umn.edu
FU Space Telescope Science Institute, NASA [GO-10605]; National Aeronautics
and Space Administration [NAS5-26555]; Macalester College; Penrose
Fellowships; NASA's Astrophysics Data System
FX We thank an anonymous referee for an especially detailed, thorough, and
insightful report that helped to significantly strengthen this
manuscript. Support for this work was provided by NASA through grant
GO-10605 from the Space Telescope Science Institute, which is operated
by AURA, Inc., under NASA contract NAS5-26555. J.M.C. and H. P. M. thank
Macalester College for research support. D.R.W. and S.R.W. are grateful
for support from Penrose Fellowships. 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.
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SN 0004-637X
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JI Astrophys. J.
PD JUL 1
PY 2011
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DI 10.1088/0004-637X/735/1/36
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300036
ER
PT J
AU Chene, AN
Moffat, AFJ
Cameron, C
Fahed, R
Gamen, RC
Lefevre, L
Rowe, JF
St-Louis, N
Muntean, V
De La Chevrotiere, A
Guenther, DB
Kuschnig, R
Matthews, JM
Rucinski, SM
Sasselov, D
Weiss, WW
AF Chene, A. -N.
Moffat, A. F. J.
Cameron, C.
Fahed, R.
Gamen, R. C.
Lefevre, L.
Rowe, J. F.
St-Louis, N.
Muntean, V.
De La Chevrotiere, A.
Guenther, D. B.
Kuschnig, R.
Matthews, J. M.
Rucinski, S. M.
Sasselov, D.
Weiss, W. W.
TI WR 110: A SINGLE WOLF-RAYET STAR WITH COROTATING INTERACTION REGIONS IN
ITS WIND?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars: individual (WR 110); stars: rotation; stars: winds, outflows;
stars: Wolf-Rayet
ID PERIODIC VARIABILITY; WN STARS; EMISSION
AB A 30 day contiguous photometric run with the Microvariability and Oscillations of STars (MOST) satellite on the WN5-6b star WR 110 (HD 165688) reveals a fundamental periodicity of P = 4.08 +/- 0.55 days along with a number of harmonics at periods P/n, with n approximate to 2, 3, 4, 5, and 6, and a few other possible stray periodicities and/or stochastic variability on timescales longer than about a day. Spectroscopic radial velocity studies fail to reveal any plausible companion with a period in this range. Therefore, we conjecture that the observed light-curve cusps of amplitude similar to 0.01 mag that recur at a 4.08 day timescale may arise in the inner parts, or at the base, of a corotating interaction region (CIR) seen in emission as it rotates around with the star at constant angular velocity. The hard X-ray component seen in WR 110 could then be a result of a high velocity component of the CIR shock interacting with the ambient wind at several stellar radii. Given that most hot, luminous stars showing CIRs have two CIR arms, it is possible that either the fundamental period is 8.2 days or, more likely in the case of WR 110, there is indeed a second weaker CIR arm for P = 4.08 days, that occurs similar to two-thirds of a rotation period after the main CIR. If this interpretation is correct, WR 110 therefore joins the ranks with three other single WR stars, all WN, with confirmed CIR rotation periods (WR 1, WR 6, and WR 134), albeit with WR 110 having by far the lowest amplitude photometric modulation. This illustrates the power of being able to secure intense, continuous highprecision photometry from space-based platforms such as MOST. It also opens the door to revealing low-amplitude photometric variations in other WN stars, where previous attempts have failed. If all WN stars have CIRs at some level, this could be important for revealing sources of magnetism or pulsation in addition to rotation periods.
C1 [Chene, A. -N.] Herzberg Inst Astrophys, Canadian Gemini Off, Victoria, BC V9E 2E7, Canada.
[Chene, A. -N.] Univ Concepcion, Dept Astron, Concepcion, Chile.
[Chene, A. -N.] Univ Valparaiso, Fac Ciencias, Dept Fis & Astron, Valparaiso, Chile.
[Moffat, A. F. J.; Fahed, R.; St-Louis, N.; Muntean, V.; De La Chevrotiere, A.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
[Moffat, A. F. J.; Fahed, R.; St-Louis, N.; Muntean, V.; De La Chevrotiere, A.] Ctr Rech Astrophys Quebec, Quebec City, PQ, Canada.
[Cameron, C.; Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada.
[Gamen, R. C.] Univ Nacl La Plata, Inst Astrofis La Plata, CCT CONICET, RA-1900 La Plata, Argentina.
[Lefevre, L.] Observ Royal Belgique, B-1180 Brussels, Belgium.
[Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada.
[Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria.
[Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada.
[Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA.
RP Chene, AN (reprint author), Herzberg Inst Astrophys, Canadian Gemini Off, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada.
EM achene@astro-udec.cl; moffat@astro.umontreal.ca
RI Gamen, Roberto/A-1728-2015
FU Chilean Centro de Astrofisica FONDAP [15010003]; Chilean Centro de
Excelencia en Astrofisica y Tecnologias Afines (CATA); NSERC (Canada);
FQRNT (Quebec); Austrian Space Agency; Austrian Science Fund; Austrian
Fonds sur Forderung der wissenschaftlichen Forschung (FWF); Austrian
Academy of Sciences at the Institute of Astronomy of the University of
Vienna
FX A.N.C. gratefully acknowledges support from the Chilean Centro de
Astrofisica FONDAP No. 15010003 and the Chilean Centro de Excelencia en
Astrofisica y Tecnologias Afines (CATA). D.B.G., J.M.M., A.F.J.M.,
S.M.R., and N.S.L. are supported by NSERC (Canada), with additional
support to A.F.J.M. and N.S.L. from FQRNT (Quebec). R.K. and W.W.W. are
supported by the Austrian Space Agency and the Austrian Science Fund.
K.Z. acknowledges support from the Austrian Fonds sur Forderung der
wissenschaftlichen Forschung (FWF) and is recipient of an APART
fellowship of the Austrian Academy of Sciences at the Institute of
Astronomy of the University of Vienna. We thank the anonymous referee
for useful suggestions to improve the clarity of this work.
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
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JI Astrophys. J.
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PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300034
ER
PT J
AU Johnson, JA
Winn, JN
Bakos, GA
Hartman, JD
Morton, TD
Torres, G
Kovacs, G
Latham, DW
Noyes, RW
Sato, B
Esquerdo, GA
Fischer, DA
Marcy, GW
Howard, AW
Buchhave, LA
Furesz, G
Quinn, SN
Beky, B
Sasselov, DD
Stefanik, RP
Lazar, J
Papp, I
Sari, P
AF Johnson, John Asher
Winn, J. N.
Bakos, G. A.
Hartman, J. D.
Morton, T. D.
Torres, G.
Kovacs, Geza
Latham, D. W.
Noyes, R. W.
Sato, B.
Esquerdo, G. A.
Fischer, D. A.
Marcy, G. W.
Howard, A. W.
Buchhave, L. A.
Furesz, G.
Quinn, S. N.
Beky, B.
Sasselov, D. D.
Stefanik, R. P.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-30b: A TRANSITING HOT JUPITER ON A HIGHLY OBLIQUE ORBIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-30, GSC 0208-00722)
ID SPIN-ORBIT; PLANETARY SYSTEM; ECCENTRIC ORBIT; BRIGHT STAR; RETROGRADE;
FIELD; EXOPLANETS; ALIGNMENT; VELOCITY; SEARCH
AB We report the discovery of HAT-P-30b, a transiting exoplanet orbiting the V = 10.419 dwarf star GSC 0208-00722. The planet has a period P = 2.810595 +/- 0.000005 days, transit epoch T-c = 2455456.46561 +/- 0.00037 (BJD), and transit duration 0.0887 +/- 0.0015 days. The host star has a mass of 1.24 +/- 0.04 M-circle dot, radius of 1.21 +/- 0.05 R-circle dot, effective temperature of 6304 +/- 88 K, and metallicity [Fe/H] = +0.13 +/- 0.08. The planetary companion has a mass of 0.711 +/- 0.028 M-J and radius of 1.340 +/- 0.065 R-J yielding a mean density of 0.37 +/- 0.05 g cm(-3). We also present radial velocity measurements that were obtained throughout a transit that exhibit the Rossiter-McLaughlin effect. By modeling this effect, we measure an angle of lambda = 73 degrees.5 +/- 9 degrees.0 between the sky projections of the planet's orbit normal and the star's spin axis. HAT-P-30b represents another example of a close-in planet on a highly tilted orbit, and conforms to the previously noted pattern that tilted orbits are more common around stars with T-eff* greater than or similar to 6250 K.
C1 [Johnson, John Asher; Morton, T. D.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA.
[Johnson, John Asher; Morton, T. D.] CALTECH, NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA.
[Winn, J. N.] MIT, Dept Phys, Cambridge, MA 02139 USA.
[Winn, J. N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA.
[Bakos, G. A.; Hartman, J. D.; Torres, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Furesz, G.; Quinn, S. N.; Beky, B.; Sasselov, D. D.; Stefanik, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Johnson, JA (reprint author), CALTECH, Dept Astrophys, MC 249-17, Pasadena, CA 91125 USA.
EM gbakos@cfa.harvard.edu
RI Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars
A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166
FU NASA [N167Hr, NNG04GN74G, NNX08AF23G, NNX09AF59G]; SAO IRD; Kepler
Mission under NASA [NCC2-1390]; Hungarian Scientific Research Foundation
(OTKA) [K-81373]
FX Based in part on observations obtained at the W. M. Keck Observatory,
which is operated by the University of California and the California
Institute of Technology. Keck time has been granted by NASA (N167Hr).
Based in part on data collected at Subaru Telescope, which is operated
by the National Astronomical Observatory of Japan.; HATNet operations
have been funded by NASA grants NNG04GN74G and NNX08AF23G and SAO IR&D
grants. G. T. acknowledges partial support from NASA grant NNX09AF59G.
We acknowledge partial support also 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-81373. This research has made use of Keck telescope time granted
through NASA (N167Hr). Based in part on data collected at Subaru
Telescope, which is operated by the National Astronomical Observatory of
Japan.
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JI Astrophys. J.
PD JUL 1
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SC Astronomy & Astrophysics
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ER
PT J
AU Knutson, HA
Madhusudhan, N
Cowan, NB
Christiansen, JL
Agol, E
Deming, D
Desert, JM
Charbonneau, D
Henry, GW
Homeier, D
Langton, J
Laughlin, G
Seager, S
AF Knutson, Heather A.
Madhusudhan, Nikku
Cowan, Nicolas B.
Christiansen, Jessie L.
Agol, Eric
Deming, Drake
Desert, Jean-Michel
Charbonneau, David
Henry, Gregory W.
Homeier, Derek
Langton, Jonathan
Laughlin, Gregory
Seager, Sara
TI A SPITZER TRANSMISSION SPECTRUM FOR THE EXOPLANET GJ 436b, EVIDENCE FOR
STELLAR VARIABILITY, AND CONSTRAINTS ON DAYSIDE FLUX VARIATIONS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries: eclipsing; planetary systems; stars: activity; techniques:
photometric
ID NEPTUNE-MASS PLANET; SECONDARY ECLIPSE PHOTOMETRY; COLLISION-INDUCED
ABSORPTION; INFRARED-EMISSION SPECTRUM; NEXTGEN MODEL ATMOSPHERES;
TRANSITING HOT NEPTUNE; EARTH ORBITING GJ-436; LIGHT-CURVE PROJECT;
M-DWARF GJ-436; EXTRASOLAR PLANET
AB In this paper, we describe a uniform analysis of eight transits and eleven secondary eclipses of the extrasolar planet GJ 436b obtained in the 3.6, 4.5, and 8.0 mu m bands using the IRAC instrument on the Spitzer Space Telescope between UT 2007 June 29 and UT 2009 February 4. We find that the best-fit transit depths for visits in the same bandpass can vary by as much as 8% of the total (4.7 sigma significance) from one epoch to the next. Although we cannot entirely rule out residual detector effects or a time-varying, high-altitude cloud layer in the planet's atmosphere as the cause of these variations, we consider the occultation of active regions on the star in a subset of the transit observations to be the most likely explanation. We find that for the deepest 3.6 mu m transit the in-transit data have a higher standard deviation than the out-of-transit data, as would be expected if the planet occulted a star spot. We also compare all published transit observations for this object and find that transits observed in the infrared typically have smaller timing offsets than those observed in visible light. In this case, the three deepest Spitzer transits are all measured within a period of five days, consistent with a single epoch of increased stellar activity. We reconcile the presence of magnetically active regions with the lack of significant visible or infrared flux variations from the star by proposing that the star's spin axis is tilted with respect to our line of sight and that the planet's orbit is therefore likely to be misaligned. In contrast to the results reported by Beaulieu et al., we find no convincing evidence for methane absorption in the planet's transmission spectrum. If we exclude the transits that we believe to be most affected by stellar activity, we find that we prefer models with enhanced CO and reduced methane, consistent with GJ 436b's dayside composition from Stevenson et al. It is also possible that all transits are significantly affected by this activity, in which case it may not be feasible to characterize the planet's transmission spectrum using broadband photometry obtained over multiple epochs. These observations serve to illustrate the challenges associated with transmission spectroscopy of planets orbiting late-type stars; we expect that other systems, such as GJ 1214, may display comparably variable transit depths. We compare the limb-darkening coefficients predicted by PHOENIX and ATLAS stellar atmosphere models and discuss the effect that these coefficients have on the measured planet-star radius ratios given GJ 436b's near-grazing transit geometry. Our measured 8 mu m secondary eclipse depths are consistent with a constant value, and we place a 1 sigma upper limit of 17% on changes in the planet's dayside flux in this band. These results are consistent with predictions from general circulation models for this planet, which find that the planet's dayside flux varies by a few percent or less in the 8 mu m band. Averaging over the eleven visits gives us an improved estimate of 0.0452% +/- 0.0027% for the secondary eclipse depth; we also examine residuals from the eclipse ingress and egress and place an upper limit on deviations caused by a non-uniform surface brightness for GJ 436b. We combine timing information from our observations with previously published data to produce a refined orbital ephemeris and determine that the best-fit transit and eclipse times are consistent with a constant orbital period. We find that the secondary eclipse occurs at a phase of 0.58672 +/- 0.
00017, correponding to e cos(omega) = 0.13754 +/- 0.00027, where e is the planet's orbital eccentricity and omega is the longitude of pericenter. We also present improved estimates for other system parameters, including the orbital inclination, a/R-star, and the planet-star radius ratio.
C1 [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Madhusudhan, Nikku] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
[Cowan, Nicolas B.] Northwestern Univ, CIERA, Evanston, IL 60208 USA.
[Christiansen, Jessie L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
[Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA.
[Desert, Jean-Michel; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA.
[Homeier, Derek; Laughlin, Gregory] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany.
[Langton, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA.
[Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA.
[Seager, Sara] MIT, Dept Phys, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA.
RP Knutson, HA (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA.
EM hknutson@berkeley.edu
RI Agol, Eric/B-8775-2013;
OI Agol, Eric/0000-0002-0802-9145; Homeier, Derek/0000-0002-8546-9128;
Charbonneau, David/0000-0002-9003-484X
FU NASA; Miller Institute for Basic Research in Science; National Science
Foundation [0645416]
FX We thank the anonymous referee for a very thoughtful report, as well as
Jonathan Fortney, Megan Shabram, and Nikole Lewis for helpful
discussions on the implications of our data for their published models
of GJ 436b. We are also grateful to Eric Gaidos for his commentary on
the nature of activity on M dwarfs, and Josh Winn for helpful
discussions on spin-orbit alignment for GJ 436b. We also thank Howard
Isaacson for supplying the SHKvalues for our activity study
and acknowledge the Keck observers who obtained the HIRES spectra used
for these measurements, including Andrew Howard, John Johnson, Debra
Fischer, and Geoff Marcy. 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. H.A.K. was supported by a fellowship from the Miller
Institute for Basic Research in Science. E.A. was supported in part by
the National Science Foundation under CAREER Grant No. 0645416.
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JI Astrophys. J.
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SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300027
ER
PT J
AU Michel, M
Kirk, H
Myers, PC
AF Michel, Manon
Kirk, Helen
Myers, Philip C.
TI MASS DISTRIBUTIONS OF STARS AND CORES IN YOUNG GROUPS AND CLUSTERS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: clouds; stars: formation; stars: luminosity function, mass function
ID MOLECULAR CLOUDS; INITIAL CONDITIONS; FORMING REGION; DENSE CORES;
SUBMILLIMETER CONTINUUM; EVOLUTIONARY MODELS; CLUMP DISTRIBUTION;
STELLAR CLUSTERS; DISK POPULATION; SCUBA SURVEY
AB We investigate the relation of the stellar initial mass function and the dense core mass function (CMF), using stellar masses and positions in 14 well-studied young groups. Initial column density maps are computed by replacing each star with a model initial core having the same star formation efficiency (SFE). For each group the SFE, core model, and observational resolution are varied to produce a realistic range of initialmaps. A clump-finding algorithm parses each initial map into derived cores, derived core masses, and a derived CMF. The main result is that projected blending of initial cores causes derived cores to be too few and too massive. The number of derived cores is fewer than the number of initial cores by a mean factor of 1.4 in sparse groups and 5 in crowded groups. The mass at the peak of the derived CMF exceeds the mass at the peak of the initial CMF by a mean factor of 1.0 in sparse groups and 12.1 in crowded groups. These results imply that in crowded young groups and clusters, the mass distribution of observed cores may not reliably predict the mass distribution of protostars that will form in those cores.
C1 [Michel, Manon] Ecole Normale Super, Dept Phys, Format Interuniv Phys, F-75231 Paris 05, France.
[Kirk, Helen; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Michel, M (reprint author), Ecole Normale Super, Dept Phys, Format Interuniv Phys, 24 Rue Lhomond, F-75231 Paris 05, France.
EM manon.michel@ens.fr; hkirk@cfa.harvard.edu; pmyers@cfa.harvard.edu
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PY 2011
VL 735
IS 1
AR 51
DI 10.1088/0004-637X/735/1/51
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300051
ER
PT J
AU Murphy, NA
Raymond, JC
Korreck, KE
AF Murphy, N. A.
Raymond, J. C.
Korreck, K. E.
TI PLASMA HEATING DURING A CORONAL MASS EJECTION OBSERVED BY THE SOLAR AND
HELIOSPHERIC OBSERVATORY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE magnetic reconnection; Sun: activity; Sun: corona; Sun: coronal mass
ejections (CMEs); Sun: UV radiation; techniques: spectroscopic
ID CURRENT SHEET; MAGNETIC RECONNECTION; SOHO OBSERVATIONS; ENERGY
PARTITION; ATOMIC DATABASE; EMISSION-LINES; CHARGE STATES; ULTRAVIOLET;
ENERGETICS; ERUPTIONS
AB We perform a time-dependent ionization analysis to constrain plasma heating requirements during a fast partial halo coronal mass ejection (CME) observed on 2000 June 28 by the Ultraviolet Coronagraph Spectrometer (UVCS) aboard the Solar and Heliospheric Observatory (SOHO). We use two methods to derive densities from the UVCS measurements, including a density sensitive Ov line ratio at 1213.85 and 1218.35 angstrom, and radiative pumping of the OVI lambda lambda 1032, 1038 doublet by chromospheric emission lines. The most strongly constrained feature shows cumulative plasma heating comparable to or greater than the kinetic energy, while features observed earlier during the event show plasma heating of order or less than the kinetic energy. SOHO Michelson Doppler Imager observations are used to estimate the active region magnetic energy. We consider candidate plasma heating mechanisms and provide constraints when possible. Because this CME was associated with a relatively weak flare, the contribution from flare energy (e. g., through thermal conduction or energetic particles) is probably small; however, the flare may have been partially behind the limb. Wave heating by photospheric motions requires heating rates to be significantly larger than those previously inferred for coronal holes, but the eruption itself could drive waves that heat the plasma. Heating by small-scale reconnection in the flux rope or by the CME current sheet is not significantly constrained. UVCS line widths suggest that turbulence must be replenished continually and dissipated on timescales shorter than the propagation time in order to be an intermediate step in CME heating.
C1 [Murphy, N. A.; Raymond, J. C.; Korreck, K. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM namurphy@cfa.harvard.edu
OI Murphy, Nicholas/0000-0001-6628-8033
FU NASA [NNX09AB17G]
FX The authors acknowledge useful discussions with J.-Y. Lee, M. P.
Miralles, K. K. Reeves, S. Cranmer, J. Lin, A. Vourlidas, A. A. van
Ballegooijen, H. Johnson, E. G. Zweibel, T. G. Forbes, J. Chen, and E.
Robbrecht. We thank an anonymous referee for particularly insightful
comments which helped to improve this paper. This research is supported
by NASA grant NNX09AB17G to the Smithsonian Astrophysical Observatory.
SOHO is a project of international cooperation between ESA and NASA.
MLSO is a facility of the National Center for Atmospheric Research
operated by the High Altitude Observatory. Yohkoh is a project of the
Institute of Space and Astronautical Science of Japan. The LASCO CME
catalog is generated and maintained at the CDAW Data Center by NASA and
The Catholic University of America in cooperation with the Naval
Research Laboratory. This work has benefited from the use of NASA's
Astrophysics Data System.
NR 82
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U1 0
U2 8
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 17
DI 10.1088/0004-637X/735/1/17
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300017
ER
PT J
AU Ngoc, PB
Lee, CF
Ho, PTP
Tang, YW
AF Ngoc Phan-Bao
Lee, Chin-Fei
Ho, Paul T. P.
Tang, Ya-Wen
TI MOLECULAR OUTFLOWS IN THE SUBSTELLAR DOMAIN: MILLIMETER OBSERVATIONS OF
YOUNG VERY LOW MASS OBJECTS IN TAURUS AND rho OPHIUCHI
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE brown dwarfs; ISM: jets and outflows; stars: low-mass
ID BROWN DWARF DISKS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; DENSE
CLOUD CORES; INFRARED SPECTROGRAPH; SUBMILLIMETER ARRAY; T-TAURI;
ACCRETION; SEARCH; EVOLUTION
AB We report here our search for molecular outflows from young very low mass stars and brown dwarfs in Taurus and rho Ophiuchi. Using the Submillimeter Array and the Combined Array for Research in Millimeter-wave Astronomy, we have observed four targets at 1.3 mm wavelength (230 GHz) to search for CO J = 2 -> 1 outflows. A young very low mass star MHO 5 (in Taurus) with an estimated mass of 90 M-J, which is just above the hydrogen-burning limit, shows two gas lobes that are likely outflows. While the CO map of MHO 5 does not show a clear structure of outflow, possibly due to environment gas, its position-velocity diagram indicates two distinct blue-and redshifted components. We therefore conclude that they are components of a bipolar molecular outflow from MHO 5. We estimate an outflow mass of 7.0 x 10(-5) M-circle dot and a mass-loss rate of 9.0 x 10(-10) M-circle dot. These values are over two orders of magnitude smaller than the typical ones for T Tauri stars and somewhat weaker than those we have observed in the young brown dwarf ISO-Oph 102 of 60 M-J in rho Ophiuchi. This makes MHO 5 the first young very low mass star showing a bipolar molecular outflow in Taurus. The detection boosts the scenario that very low mass objects form like low-mass stars but in a version scaled down by a factor of over 100.
C1 [Ngoc Phan-Bao] HCMIU, Dept Phys, Linh Trung Ward, Ho Chi Minh City, Vietnam.
[Ngoc Phan-Bao; Lee, Chin-Fei; Ho, Paul T. P.; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
[Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ngoc, PB (reprint author), HCMIU, Dept Phys, Linh Trung Ward, Vietnam Natl Univ Adm Bldg,Block 6, Ho Chi Minh City, Vietnam.
EM pbngoc@hcmiu.edu.vn
FU VietNam NAFOSTED [103.08-2010.07]; National Science Council (NSC)
[97-2112-M-001-007-MY3]; Gordon and Betty Moore Foundation; Kenneth T.
and Eileen L. Norris Foundation; James S. McDonnell Foundation;
Associates of the California Institute of Technology; University of
Chicago; states of California, Illinois, and Maryland; National Science
Foundation
FX N.P.-B has been supported by VietNam NAFOSTED grant 103.08-2010.07. This
work was partly supported by the National Science Council (NSC) grant
97-2112-M-001-007-MY3 to P. T. P. H. Support for CARMA construction was
derived from the Gordon and Betty Moore Foundation, the Kenneth T. and
Eileen L. Norris Foundation, the James S. McDonnell Foundation, the
Associates of the California Institute of Technology, the University of
Chicago, the states of California, Illinois, and Maryland, and the
National Science Foundation. Ongoing CARMA development and operations
are supported by the National Science Foundation under a cooperative
agreement and by the CARMA partner universities. 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 work has made use of the
Centre de Donnees astronomiques de Strasbourg (CDS) database.
NR 41
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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 2011
VL 735
IS 1
AR 14
DI 10.1088/0004-637X/735/1/14
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300014
ER
PT J
AU O'Sullivan, E
Giacintucci, S
David, LP
Gitti, M
Vrtilek, JM
Raychaudhury, S
Ponman, TJ
AF O'Sullivan, E.
Giacintucci, S.
David, L. P.
Gitti, M.
Vrtilek, J. M.
Raychaudhury, S.
Ponman, T. J.
TI HEATING THE HOT ATMOSPHERES OF GALAXY GROUPS AND CLUSTERS WITH CAVITIES:
THE RELATIONSHIP BETWEEN JET POWER AND LOW-FREQUENCY RADIO EMISSION
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: clusters: general; galaxies: clusters:
intracluster medium; galaxies: groups: general; X-rays: galaxies:
clusters
ID ACTIVE GALACTIC NUCLEI; X-RAY CAVITIES; COOLING CLUSTERS; GAS ACCRETION;
FEEDBACK; BUBBLES; CHANDRA; SAMPLE; SPECTROSCOPY; MODELS
AB We present scaling relations between jet power and radio power measured using the Giant Metrewave Radio Telescope (GMRT), Chandra, and XMM-Newton, for a sample of nine galaxy groups combined with the Birzan et al. sample of clusters. Cavity power is used as a proxy for mechanical jet power. Radio power is measured at 235 MHz and 1.4 GHz, and the integrated 10 MHz-10 GHz radio luminosity is estimated from the GMRT 610-235 MHz spectral index. The use of consistently analyzed, high-resolution low-frequency radio data from a single observatory makes the radio powers for the groups more reliable than those used by previous studies, and the combined sample covers 6-7 decades in radio power and 5 decades in cavity power. We find a relation of the form P-jet proportional to L-radio(similar to 0.7) radio for integrated radio luminosity, with a total scatter of sigma(Lrad) = 0.63 and an intrinsic scatter of sigma(i,Lrad) = 0.59. A similar relation is found for 235 MHz power, but a slightly flatter relation with greater scatter is found for 1.4 GHz power, suggesting that low-frequency or broadband radio measurements are superior jet power indicators. We find our low-frequency relations to be in good agreement with previous observational results. Comparison with jet models shows reasonable agreement, which may be improved if radio sources have a significant low-energy electron population. We consider possible factors that could bias our results or render them more uncertain, and find that correcting for such factors in those groups we are able to study in detail leads to a flattening of the P-jet:L-radio relation.
C1 [O'Sullivan, E.; Raychaudhury, S.; Ponman, T. J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
[O'Sullivan, E.; Giacintucci, S.; David, L. P.; Gitti, M.; Vrtilek, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Giacintucci, S.; Gitti, M.] INAF Inst Radioastron, I-40129 Bologna, Italy.
[Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
[Gitti, M.] Osservatorio Astron Bologna INAF, I-40127 Bologna, Italy.
RP O'Sullivan, E (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
EM ejos@star.sr.bham.ac.uk
OI O'Sullivan, Ewan/0000-0002-5671-6900; Gitti, Myriam/0000-0002-0843-3009
FU Chandra [AR1-12014X, GO0-11136X]; NASA [ASI-INAFI/023/05/0, I/088/06/0]
FX We thank the anonymous referee for their useful suggestions. We thank
the staff of the GMRT for their help during observations. GMRT is run by
the National Centre for Radio Astrophysics of the Tata Institute of
Fundamental Research. We also acknowledge support from Chandra grant
AR1-12014X. E.J.O.S. thanks A.J.R. Sanderson for useful discussions and
acknowledges the support of the European Community under the Marie Curie
Research Training Network. S. G. acknowledges the support of NASA
through the award of an Einstein Postdoctoral Fellowship. M. G.
acknowledges the financial contribution from contracts
ASI-INAFI/023/05/0 and I/088/06/0 and Chandra grant GO0-11136X.
NR 38
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 11
DI 10.1088/0004-637X/735/1/11
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300011
ER
PT J
AU Palma, NI
Bottcher, M
de la Calle, I
Agudo, I
Aller, M
Aller, H
Bach, U
Benitez, E
Buemi, CS
Escande, L
Gomez, JL
Gurwell, MA
Heidt, J
Hiriart, D
Jorstad, SG
Joshi, M
Lahteenmaki, A
Larionov, VM
Leto, P
Li, Y
Lopez, JM
Lott, B
Madejski, G
Marscher, AP
Morozova, DA
Raiteri, CM
Roberts, V
Tornikoski, M
Trigilio, C
Umana, G
Villata, M
Wylezalek, D
AF Palma, N. I.
Boettcher, M.
de la Calle, I.
Agudo, I.
Aller, M.
Aller, H.
Bach, U.
Benitez, E.
Buemi, C. S.
Escande, L.
Gomez, J. L.
Gurwell, M. A.
Heidt, J.
Hiriart, D.
Jorstad, S. G.
Joshi, M.
Lahteenmaki, A.
Larionov, V. M.
Leto, P.
Li, Y.
Lopez, J. M.
Lott, B.
Madejski, G.
Marscher, A. P.
Morozova, D. A.
Raiteri, C. M.
Roberts, V.
Tornikoski, M.
Trigilio, C.
Umana, G.
Villata, M.
Wylezalek, D.
TI MULTIWAVELENGTH OBSERVATIONS OF THE GAMMA-RAY BLAZAR PKS 0528+134 IN
QUIESCENCE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: active; galaxies: jets; gamma rays: galaxies; polarization;
quasars: individual (PKS 0528+134); radiation mechanisms: non-thermal
ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS;
EXTRAGALACTIC RADIO-SOURCES; INTERNAL-SHOCK MODEL; BASE-LINE ARRAY;
EGRET OBSERVATIONS; MULTIFREQUENCY OBSERVATIONS; SHEAR ACCELERATION;
RELATIVISTIC JETS
AB We present multiwavelength observations of the ultraluminous blazar-type radio loud quasar PKS 0528+134 in quiescence during the period 2009 July-December. Four Target-of-Opportunity observations with the XMM-Newton satellite in the 0.2-10 keV range were supplemented with optical observations at the MDM Observatory, radio and optical data from the GLAST-AGILE Support Program of the Whole Earth Blazar Telescope and the Very Long Baseline Array, additional X-ray data from the Rossi X-ray Timing Explorer (2-10 keV) and from Suzaku (0.5-10 keV) as well as gamma-ray data from the Fermi Large Area Telescope in the 100 MeV-200 GeV range. In addition, publicly available data from the SMARTS blazar monitoring program and the University of Arizona/Steward Observatory Fermi Support program were included in our analysis. We found no evidence of significant flux or spectral variability in gamma-rays and most radio bands. However, significant flux variability on a timescale of several hours was found in the optical regime, accompanied by a weak trend of spectral softening with increasing flux. We suggest that this might be the signature of a contribution of unbeamed emission, possibly from the accretion disk, at the blue end of the optical spectrum. The optical flux is weakly polarized with rapid variations of the degree and direction of polarization, while the polarization of the 43 GHz radio core remains steady, perpendicular to the jet direction. Optical spectropolarimetry of the object in the quiescent state suggests a trend of increasing degree of polarization with increasing wavelength, providing additional evidence for an unpolarized emission component, possibly thermal emission from the accretion disk, contributing toward the blue end of the optical spectrum. Over an extended period of several months, PKS 0528+134 shows moderate (amplitude less than or similar to 50%) flux variability in the X-rays and most radio frequencies on similar to 1-2 week timescales. We constructed four spectral energy distributions (SEDs) corresponding to the times of the XMM-Newton observations. We find that even in the quiescent state, the bolometric luminosity of PKS 0528+134 is dominated by its gamma-ray emission. A leptonic single-zone jet model produced acceptable fits to the SEDs with contributions to the high-energy emission from both synchrotron self-Compton radiation and Comptonization of direct accretion disk emission. Fit parameters close to equipartition between the energy densities of the magnetic field and the relativistic electron population were obtained. The moderate variability on long timescales, compared to expected radiative cooling timescales, implies the existence of ongoing particle acceleration, while the observed optical polarization variability seems to point toward a turbulent acceleration process. Turbulent particle acceleration at stationary features along the jet therefore appears to be a viable possibility for the quiescent state of PKS 0528+134.
C1 [Palma, N. I.; Boettcher, M.; Li, Y.; Roberts, V.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA.
[Palma, N. I.] Univ Nacl Autonoma Honduras, Fac Ciencias Espaciales, Tegucigalpa Mdc, Honduras.
[de la Calle, I.] European Space Astron Ctr, Madrid 28691, Spain.
[Agudo, I.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
[Aller, M.; Aller, H.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Agudo, I.; Gomez, J. L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain.
[Bach, U.] Max Planck Inst Radioastron, D-53225 Bonn, Germany.
[Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
[Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy.
[Escande, L.; Lott, B.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France.
[Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Heidt, J.] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany.
[Hiriart, D.; Lopez, J. M.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico.
[Jorstad, S. G.; Larionov, V. M.; Morozova, D. A.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia.
[Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland.
[Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg 198504, Russia.
[Madejski, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA.
[Madejski, G.] Stanford Univ, SLAC Natl Acelerator Lab, Stanford, CA 94305 USA.
[Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy.
[Wylezalek, D.] Univ Cambridge, Cavendish Lab, Dept Phys, Cambridge CB3 0HE, England.
RP Palma, NI (reprint author), Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger 339, Athens, OH 45701 USA.
EM iagudo@bu.edu; jlgomez@iaa.es; jorstad@bu.edu; marscher@bu.edu
RI Larionov, Valeri/H-1349-2013; Lahteenmaki, Anne/L-5987-2013; Agudo,
Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Jorstad,
Svetlana/H-6913-2013; XRAY, SUZAKU/A-1808-2009;
OI Larionov, Valeri/0000-0002-4640-4356; Umana, Grazia/0000-0002-6972-8388;
Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804;
Jorstad, Svetlana/0000-0001-9522-5453; Buemi, Carla
Simona/0000-0002-7288-4613; Villata, Massimo/0000-0003-1743-6946; Leto,
Paolo/0000-0003-4864-2806; Raiteri, Claudia Maria/0000-0003-1784-2784
FU NASA [NNX08AD67G, NNX09AV45G, GO8-9100X, NNX09AT82G, NNX09AT99G,
NNX08AV65G, NNX09AU16G, NNX10AP16G, NNX08AZ89G, NNX08AW56G, NNX09AU10G];
MICIIN (Spain) [AYA2007-67267-C03-03, AYA2010-14844]; CEIC (Andalucia)
[P09-FQM-4784]; Smithsonian Institution; Academia Sinica; Academy of
Finland [212656, 210338]; NSF [AST-0907893, AST-0607523]; NSF, BU;
Lowell Observatory; Russian RFBR foundation [09-02-00092]; University of
Michigan
FX This work was supported by NASA through XMM-Newton Guest Observer
Program awards NNX08AD67G and NNX09AV45G, Chandra Guest Observer Program
award GO8-9100X, and Fermi Guest Investigator Program award NNX09AT82G.;
Acquisition of the MAPCAT data is supported in part by MICIIN (Spain)
grants AYA2007-67267-C03-03 and AYA2010-14844, and by CEIC (Andalucia)
grant P09-FQM-4784.; 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 Metsahovi team
acknowledges the support from the Academy of Finland to our observing
projects (numbers 212656, 210338, and others).; The research at Boston
University (BU) was funded in part by NASA Fermi Guest Investigator
grants NNX09AT99G and NNX08AV65G, and by the NSF through grant
AST-0907893. The PRISM camera at Lowell Observatory was developed by K.
Janes et al. at BU and Lowell Observatory, with funding from the NSF,
BU, and Lowell Observatory.; D.M. acknowledges support from Russian RFBR
foundation via grant 09-02-00092.; The research at UMRAO was funded in
part by NSF grant AST-0607523 and by NASA grants NNX09AU16G and
NNX10AP16G. The operation of UMRAO is made possible by funds from the
University of Michigan.; G.M. acknowledges support from NASA through
Suzaku Guest Observer grant NNX08AZ89G.; The Steward Observatory Fermi
Support Program is supported by NASA through Fermi Guest Investigator
Program grants NNX08AW56G and NNX09AU10G.
NR 70
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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 2011
VL 735
IS 1
AR 60
DI 10.1088/0004-637X/735/1/60
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300060
ER
PT J
AU Sell, PH
Pooley, D
Zezas, A
Heinz, S
Homan, J
Lewin, WHG
AF Sell, P. H.
Pooley, D.
Zezas, A.
Heinz, S.
Homan, J.
Lewin, W. H. G.
TI LUMINOSITY FUNCTIONS AND POINT-SOURCE PROPERTIES FROM MULTIPLE CHANDRA
OBSERVATIONS OF M81
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M81); X-rays: binaries; X-rays: galaxies
ID X-RAY BINARIES; ANTENNAE GALAXIES NGC-4038/4039; GLOBULAR CLUSTER
CONNECTION; STAR-FORMATION RATE; CONFIDENCE-LIMITS; ELLIPTIC GALAXIES;
SOURCE POPULATION; XMM-NEWTON; MULTIWAVELENGTH PROJECT; MONITORING
OBSERVATIONS
AB We present an analysis of 15 Chandra observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of similar to 10(37) erg s(-1). With these observations and one previous deeper Chandra observation, we compile a master source list of 265 point sources, extract and fit their spectra, and differentiate basic populations of sources through their colors. We also carry out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. We find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. We also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way.
C1 [Sell, P. H.; Pooley, D.; Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
[Pooley, D.] Eureka Sci, Oakland, CA USA.
[Zezas, A.] Univ Crete, Dept Phys, Iraklion, Greece.
[Zezas, A.] Fdn Res & Technol Hellas, IESL, Iraklion, Greece.
[Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Homan, J.; Lewin, W. H. G.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA USA.
RP Sell, PH (reprint author), Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RI Sell, Paul/B-1283-2017; Zezas, Andreas/C-7543-2011;
OI Sell, Paul/0000-0003-1771-5531; Zezas, Andreas/0000-0001-8952-676X;
Heinz, Sebastian/0000-0002-8433-8652
FU Chandra grant [GO5-6092]; UE IRG [224878]; EU [206469]
FX We thank Jay Gallagher and Christy Tremonti for helpful comments. D.P.
and P.S. gratefully acknowledge support from Chandra grant GO5-6092.
A.Z. acknowledges support by the UE IRG grant 224878. Space Astrophysics
at the University of Crete is supported by EU FP7-REGPOT grant 206469
(ASTROSPACE).
NR 72
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PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 26
DI 10.1088/0004-637X/735/1/26
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300026
ER
PT J
AU Shen, Y
Liu, X
Greene, JE
Strauss, MA
AF Shen, Yue
Liu, Xin
Greene, Jenny E.
Strauss, Michael A.
TI TYPE 2 ACTIVE GALACTIC NUCLEI WITH DOUBLE-PEAKED [O III] LINES. II.
SINGLE AGNs WITH COMPLEX NARROW-LINE REGION KINEMATICS ARE MORE COMMON
THAN BINARY AGNs
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: active; galaxies: interactions; galaxies:
nuclei; galaxies: Seyfert; quasars: general
ID DIGITAL-SKY-SURVEY; BLACK-HOLE SYSTEM; REDSHIFT SURVEY; GALAXIES;
SEYFERT; QUASARS; GAS; KPC; MARKARIAN-78; DISCOVERY
AB Approximately 1% of low-redshift (z less than or similar to 0.3) optically selected type 2 active galactic nuclei (AGNs) show a doublepeaked [O III] narrow emission line profile in their spatially integrated spectra. Such features are usually interpreted as either due to kinematics, such as biconical outflows and/or disk rotation of the narrow line region (NLR) around single black holes, or due to the relative motion of two distinct NLRs in a merging pair of AGNs. Here, we report follow-up near-infrared (NIR) imaging and optical slit spectroscopy of 31 double-peaked [O III] type 2 AGNs drawn from the Sloan Digital Sky Survey (SDSS) parent sample presented in Liu et al. The NIR imaging traces the old stellar population in each galaxy, while the optical slit spectroscopy traces the NLR gas. These data reveal a mixture of origins for the double-peaked feature. Roughly 10% of our objects are best explained by binary AGNs at (projected) kpc-scale separations, where two stellar components with spatially coincident NLRs are seen. similar to 50% of our objects have [O III] emission offset by a few kpc, corresponding to the two velocity components seen in the SDSS spectra, but there are no spatially coincident double stellar components seen in the NIR imaging. For those objects with sufficiently high-quality slit spectra, we see velocity and/or velocity dispersion gradients in [O III] emission, suggestive of the kinematic signatures of a single NLR. The remaining similar to 40% of our objects are ambiguous and will need higher spatial resolution observations to distinguish between the two scenarios. Our observations therefore favor the kinematics scenario with a single AGN for the majority of these double-peaked [O III] type 2 AGNs. We emphasize the importance of combining imaging and slit spectroscopy in identifying kpc-scale binary AGNs, i.e., in no cases does one of these alone allow an unambiguous identification. We estimate that similar to 0.5%-2.5% of the z less than or similar to 0.3 type 2 AGNs are kpc-scale binary AGNs of comparable luminosities, with a relative orbital velocity greater than or similar to 150 km s(-1).
C1 [Shen, Yue; Liu, Xin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Greene, Jenny E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
[Liu, Xin; Greene, Jenny E.; Strauss, Michael A.] Princeton Univ Observ, Princeton, NJ 08544 USA.
RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA.
FU Smithsonian Astrophysical Observatory; Chandra X-ray Center [PF0-110076,
NAS8-03060]; NSF [AST-0707266]; Chandra X-ray Observatory Center
[NAS8-03060, GO1-12127X]; Alfred P. Sloan Foundation; National Science
Foundation; U.S. Department of Energy; National Aeronautics and Space
Administration; Japanese Monbukagakusho; Max Planck Society; Higher
Education Funding Council for England
FX We thank Laura Blecha for useful discussions and comments on the draft.
Y.S. acknowledges support from a Clay Postdoctoral Fellowship through
the Smithsonian Astrophysical Observatory. Support for the work of X.L.
was provided by NASA through Einstein Postdoctoral Fellowship grant
number PF0-110076 awarded by the Chandra X-ray Center, which is operated
by the Smithsonian Astrophysical Observatory for NASA under contract
NAS8-03060. X.L. and M.A.S. acknowledge the support of NSF grant
AST-0707266. Support for this work was provided by the National
Aeronautics and Space Administration through Chandra Award Number
GO1-12127X issued by the Chandra X-ray Observatory Center, which is
operated by the Smithsonian Astrophysical Observatory for and on behalf
of the National Aeronautics and Space Administration under contract
NAS8-03060.; Funding for the SDSS and SDSS-II has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Science Foundation, the U.S. Department of Energy, the National
Aeronautics and Space Administration, the Japanese Monbukagakusho, the
Max Planck Society, and the Higher Education Funding Council for
England. The SDSS Web site is http://www.sdss.org/.
NR 45
TC 70
Z9 70
U1 1
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 JUL 1
PY 2011
VL 735
IS 1
AR 48
DI 10.1088/0004-637X/735/1/48
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300048
ER
PT J
AU Wang, K
Zhang, QZ
Wu, YF
Zhang, HW
AF Wang, Ke
Zhang, Qizhou
Wu, Yuefang
Zhang, Huawei
TI HIERARCHICAL FRAGMENTATION AND JET-LIKE OUTFLOWS IN IRDC G28.34+0.06: A
GROWING MASSIVE PROTOSTAR CLUSTER
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G28.34+0.06); ISM: jets and outflows; stars:
early-type; stars: formation
ID INFRARED-DARK CLOUDS; VELOCITY MOLECULAR OUTFLOWS; STAR-FORMATION; HOT
CORE; MULTIPLE OUTFLOWS; DENSITY STRUCTURE; DUST PROPERTIES; IRAS
20126+4104; FORMING REGION; WATER MASERS
AB We present Submillimeter Array (SMA) lambda = 0.88mm observations of an infrared dark cloud G28.34+0.06. Located in the quiescent southern part of the G28.34 cloud, the region of interest is a massive (>10(3) M-circle dot) molecular clump P1 with a luminosity of similar to 10(3) L-circle dot, where our previous SMA observations at 1.3 mm have revealed a string of five dust cores of 22-64 M-circle dot along the 1 pc IR-dark filament. The cores are well aligned at a position angle (P. A.) of 48 degrees and regularly spaced at an average projected separation of 0.16 pc. The new high-resolution, high-sensitivity 0.88 mm image further resolves the five cores into 10 compact condensations of 1.4-10.6 M-circle dot, with sizes of a few thousand AU. The spatial structure at clump (similar to 1 pc) and core (similar to 0.1 pc) scales indicates a hierarchical fragmentation. While the clump fragmentation is consistent with a cylindrical collapse, the observed fragment masses are much larger than the expected thermal Jeans masses. All the cores are driving CO (3-2) outflows up to 38 km s(-1), the majority of which are bipolar, jet-like outflows. The moderate luminosity of the P1 clump sets a limit on the mass of protostars of 3-7 M-circle dot. Because of the large reservoir of dense molecular gas in the immediate medium and ongoing accretion as evident by the jet-like outflows, we speculate that P1 will grow and eventually form a massive star cluster. This study provides a first glimpse of massive, clustered star formation that currently undergoes through an intermediate-mass stage.
C1 [Wang, Ke; Wu, Yuefang; Zhang, Huawei] Peking Univ, Dept Astron, Sch Phys, Beijing 100871, Peoples R China.
[Wang, Ke; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wang, K (reprint author), Peking Univ, Dept Astron, Sch Phys, Beijing 100871, Peoples R China.
EM kwang@cfa.harvard.edu; qzhang@cfa.harvard.edu
OI Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589
FU SMA; China Scholarship Council; Smithsonian Institution Endowment Funds;
NSFC [10873019, 11073003]
FX We appreciate an anonymous referee's valuable comments that helped
clarify the manuscript. K.W. acknowledges the support from the SMA
predoctoral fellowship and the China Scholarship Council. Q.Z.
acknowledges the support from the Smithsonian Institution Endowment
Funds. This research is funded in part by NSFC grants 10873019 and
11073003.
NR 71
TC 50
Z9 50
U1 1
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 64
DI 10.1088/0004-637X/735/1/64
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300064
ER
PT J
AU Williams, BF
Dalcanton, JJ
Gilbert, KM
Seth, AC
Weisz, DR
Skillman, ED
Dolphin, AE
AF Williams, Benjamin F.
Dalcanton, Julianne J.
Gilbert, Karoline M.
Seth, Anil C.
Weisz, Daniel R.
Skillman, Evan D.
Dolphin, Andrew E.
TI THE ACS NEARBY GALAXY SURVEY TREASURY. VII. THE NGC 4214 STARBURST AND
THE EFFECTS OF STAR FORMATION HISTORY ON DWARF MORPHOLOGY
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies: evolution; galaxies: individual (NGC-4214); galaxies: spiral;
galaxies: stellar content
ID HUBBLE-SPACE-TELESCOPE; YOUNG STELLAR POPULATION; IRREGULAR GALAXIES;
PHOTOMETRIC SYSTEMS; NGC-4214; DISK; ULTRAVIOLET; ISOCHRONES;
PARAMETERS; EVOLUTION
AB We present deep Hubble Space Telescope WFPC2 optical observations obtained as part of the ACS Nearby Galaxy Survey Treasury as well as early release Wide Field Camera 3 ultraviolet and infrared observations of the nearby dwarf starbursting galaxy NGC 4214. Our data provide a detailed example of how covering such a broad range in wavelength provides a powerful tool for constraining the physical properties of stellar populations. The deepest data reach the ancient red clump at M-F814W similar to -0.2. All of the optical data reach the main-sequence turnoff for stars younger than similar to 300 Myr and the blue He-burning sequence for stars younger than 500 Myr. The full color-magnitude diagram (CMD) fitting analysis shows that all three fields in our data set are consistent with similar to 75% of the stellar mass being older than 8 Gyr, in spite of showing a wide range in star formation rates at present. Thus, our results suggest that the scale length of NGC 4214 has remained relatively constant for many gigayears. As previously noted by others, we also find the galaxy has recently ramped up production consistent with its bright UV luminosity and its population of UV-bright massive stars. In the central field we find UV point sources with F336W magnitudes as bright as -9.9. These are as bright as stars with masses of at least 52-56 M-circle dot and ages near 4 Myr in stellar evolution models. Assuming a standard initial mass function, our CMD is well fitted by an increase in star formation rate beginning 100 Myr ago. The stellar populations of this late-type dwarf are compared with those of NGC 404, an early-type dwarf that is also the most massive galaxy in its local environment. The late-type dwarf appears to have a similar high fraction of ancient stars, suggesting that these dominant galaxies may form at early epochs even if they have low total mass and very different present-day morphologies.
C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Gilbert, Karoline M.; Weisz, Daniel R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA.
[Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Skillman, Evan D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
[Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA.
RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA.
EM ben@astro.washington.edu; jd@astro.washington.edu;
kgilbert@astro.washington.edu; aseth@cfa.harvard.edu;
dweisz@astro.washington.edu; skillman@astro.umn.edu;
adolphin@raytheon.com
FU Space Telescope Science Institute [GO-10915, GO-11719, GO-11986]; NASA
[NAS5-26555]
FX Support for this work was provided by NASA through grants GO-10915,
GO-11719, and GO-11986 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 37
TC 7
Z9 7
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2011
VL 735
IS 1
AR 22
DI 10.1088/0004-637X/735/1/22
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 779OM
UT WOS:000291788300022
ER
PT J
AU Akre, KL
Ryan, MJ
AF Akre, Karin L.
Ryan, Michael J.
TI Female tungara frogs elicit more complex mating signals from males
SO BEHAVIORAL ECOLOGY
LA English
DT Article
DE communication; display strategy; elicitation behavior; female choice;
proceptive behavior; sexual selection
ID PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; PREDATION RISK;
REPRODUCTIVE-BEHAVIOR; MALE COMPETITION; MALE COURTSHIP; FIDDLER-CRABS;
MATE CHOICE; COMMUNICATION; DISPLAYS
AB Sexual selection is responsible for the evolution of costly elaborate male traits. When male displays are dynamic, display strategy is sensitive to contextual cues that alter the relative costs and benefits of producing each signal in a male's repertoire. Because females often prefer more elaborate signals, males often respond to female presence by elaborating their display. When added elaboration increases assessment information or reproductive stimulation, females might benefit by extracting the maximum amount of signal elaboration from males. Thus, we expect that females could exaggerate their presence and cause males to produce even costlier and more attractive signals by exhibiting "elicitation" behaviors. We asked whether female tungara frogs elicit increased call complexity from prospective mates. In tungara frogs, adding complexity increases both attractiveness and predation risk. We found that females exhibit a repertoire of movements that function not in mate acquisition, per se, but in display manipulation, by eliciting increased complexity from calling males. The probability that males add complexity to their display increases when females produce these movements. Thus, females actively influence males to produce riskier signals.
C1 [Akre, Karin L.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA.
[Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Akre, KL (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn,C0930, Austin, TX 78712 USA.
EM kakre@mail.utexas.edu
FU National Science Foundation [NSF IBN 9816564]
FX A National Science Foundation Graduate Research Fellowship provided
funding to K.L.A. Other funding was provided by a National Science
Foundation grant to M.J.R. (NSF IBN 9816564).
NR 62
TC 19
Z9 19
U1 1
U2 25
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
J9 BEHAV ECOL
JI Behav. Ecol.
PD JUL-AUG
PY 2011
VL 22
IS 4
BP 846
EP 853
DI 10.1093/beheco/arr065
PG 8
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA 779AH
UT WOS:000291750000022
ER
PT J
AU Milian-Garcia, Y
Venegas-Anaya, M
Frias-Soler, R
Crawford, AJ
Ramos-Targarona, R
Rodriguez-Soberon, R
Alonso-Tabet, M
Thorbjarnarson, J
Sanjur, OI
Espinosa-Lopez, G
Bermingham, E
AF Milian-Garcia, Yoamel
Venegas-Anaya, Miryam
Frias-Soler, Roberto
Crawford, Andrew J.
Ramos-Targarona, Roberto
Rodriguez-Soberon, Roberto
Alonso-Tabet, Manuel
Thorbjarnarson, John
Sanjur, Oris I.
Espinosa-Lopez, Georgina
Bermingham, Eldredge
TI Evolutionary History of Cuban Crocodiles Crocodylus rhombifer and
Crocodylus acutus Inferred From Multilocus Markers
SO JOURNAL OF EXPERIMENTAL ZOOLOGY PART A-ECOLOGICAL GENETICS AND
PHYSIOLOGY
LA English
DT Article
ID BAYESIAN PHYLOGENETIC INFERENCE; LENGTH DIFFERENCE TEST;
MITOCHONDRIAL-DNA; MORELETS CROCODILE; POPULATION STATUS; MASS
MORTALITY; GENOTYPE DATA; HYBRIDIZATION; BIOGEOGRAPHY; TREES
AB Among crocodilians, Crocodylus rhombifer is one of the world's most endangered species with the smallest natural distribution. In Cuba, this endemic species coexists with the American crocodile (Crocodylus acutus). Hybridization between these two species is well known in captivity and might occur in the wild, but has never been demonstrated genetically. Here, we combined molecular data with environmental, geographic, and fossil data to infer the evolutionary history of Crocodylus in the Cuban Archipelago, and to evaluate genealogical support for species boundaries. We analyzed seven microsatellite loci plus DNA sequence data from nuclear (RAG-1) and mitochondrial (cytochrome b and cytochrome oxidase I) genes from 89 wild-caught individuals in Cuba, Grand Cayman Island, Jamaica, and Central America, and two samples from zoo collections. Microsatellites showed evidence of introgression, suggesting potential hybridization among Cuban groups. In Cuba, C. acutus contained one mitochondrial DNA (mtDNA) haplotype, whereas C. rhombifer contained two haplotypes. MtDNA data showed that C. acutus is paraphyletic with respect to C. rhombifer, revealing 1% sequence divergence between species within Cuba vs. 8% divergence between Cuban forms and mainland C. acutus. We suggest that hybridization has been a historical as well as a current phenomenon between C. acutus and C. rhombifer. These findings suggest that long-term conservation of crocodiles in Cuba will require identification of genetically pure and hybrid individuals, and a decrease in anthropogenic activities. We also recommend more extensive morphological and genetic analyses of Cuban population to establish clear boundaries of the hybrid zone between C. acutus and C. rhombifer. J. Exp. Zool. 315: 358-375, 2011. (C) 2011 Wiley-Liss, Inc.
C1 [Milian-Garcia, Yoamel; Frias-Soler, Roberto; Espinosa-Lopez, Georgina] Univ La Habana, Fac Biol, Havana, Cuba.
[Venegas-Anaya, Miryam; Crawford, Andrew J.; Sanjur, Oris I.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama.
[Venegas-Anaya, Miryam] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA.
[Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia.
[Ramos-Targarona, Roberto; Rodriguez-Soberon, Roberto; Alonso-Tabet, Manuel] Empresa Nacl Protecc Flora & Fauna, Havana, Cuba.
[Thorbjarnarson, John] Wildlife Conservat Soc, Gainesville, FL USA.
RP Espinosa-Lopez, G (reprint author), Univ Havana, Havana, Cuba.
EM georgina@fbio.uh.cu
OI Crawford, Andrew J./0000-0003-3153-6898
FU Smithsonian Tropical Research Institute; NSF [DEB04441333]
FX Grant Sponsors: Smithsonian Tropical Research Institute; NSF; Grant
number: DEB04441333.
NR 104
TC 20
Z9 20
U1 5
U2 32
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1932-5223
J9 J EXP ZOOL PART A
JI J. Exp. Zool. Part A
PD JUL 1
PY 2011
VL 315A
IS 6
BP 358
EP 375
DI 10.1002/jez.683
PG 18
WC Zoology
SC Zoology
GA 778IY
UT WOS:000291698600004
PM 21462351
ER
PT J
AU Balogh, AL
Ryder, TB
Marra, PP
AF Balogh, Anne L.
Ryder, Thomas B.
Marra, Peter P.
TI Population demography of Gray Catbirds in the suburban matrix: sources,
sinks and domestic cats
SO JOURNAL OF ORNITHOLOGY
LA English
DT Article
DE Cats; Nest survival; Post-fledging survival; Urbanization; Source-sink
dynamics
ID URBAN GRADIENT; NEST PREDATION; FELIS-CATUS; HOUSE CATS; POSTFLEDGING
MOVEMENTS; NEW-ZEALAND; HABITAT USE; SURVIVAL; BIRDS; LANDSCAPE
AB Understanding factors that limit the productivity and survival of birds in rapidly changing human-dominated landscapes are key to managing future population persistence. To date, few studies have quantified both nest success and post-fledging survival for birds breeding within the suburban matrix. Here, we estimated nest success and juvenile post-fledging survival for Gray Catbirds (Dumatella carolinensis) and used those site-specific parameters to model source-sink dynamics at three sites in suburban Washington DC (USA). Cumulative nest success probability varied substantially among suburban sites and indicated that in some cases suburban habitats may provide suitable breeding sites for passerine birds. In addition, we documented the effects of sex and brood size on post-fledging survival rates and determined the role of predation on dispersing fledglings. Like nest success, estimates of post-fledging juvenile survival also varied among sites and highlight the importance of site-specific demographic estimates in urban habitats. Predation accounted for 79% of all mortalities, with 47% of known predation events attributable to domestic cats (Felis catus). Our models of source-sink dynamics underscore the importance of seasonal recruitment parameters for calculating population growth rate and subsequent persistence. This study provides parameter estimates for two critical life history stages in the avian annual cycle in the suburban matrix and posits that predation drives differential nest and post-fledging survival within human-dominated environments.
C1 [Balogh, Anne L.; Ryder, Thomas B.; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA.
[Balogh, Anne L.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA.
RP Ryder, TB (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012,MRC 5503, Washington, DC 20013 USA.
EM rydert@si.edu
FU Mills Corporation; Smithsonian Endowment Funds
FX We thank N. Diggs, A. Struzinski and B. Johnson for dedicated
assistance. C. Studds for statistical help and L. S. Johnson for
invaluable editing and comments. The Mills Corporation and support from
the Smithsonian Endowment Funds supported this research. All research
was in compliance with Smithsonian IACUC protocols.
NR 64
TC 34
Z9 34
U1 8
U2 63
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 2011
VL 152
IS 3
BP 717
EP 726
DI 10.1007/s10336-011-0648-7
PG 10
WC Ornithology
SC Zoology
GA 777HB
UT WOS:000291605400022
ER
PT J
AU Li, G
Gordon, IE
Bernath, PF
Rothman, LS
AF Li, G.
Gordon, I. E.
Bernath, P. F.
Rothman, L. S.
TI Direct fit of experimental ro-vibrational intensities to the dipole
moment function: Application to HCl
SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER
LA English
DT Article
DE Hydrogen chloride; Dipole moment function; Intensity measurements;
Intensity calculations; Herman-Wallis coefficients
ID ROTATIONAL MATRIX-ELEMENTS; DIATOMIC-MOLECULES; INFRARED TRANSITIONS;
HYDROGEN-CHLORIDE; LINE INTENSITIES; OVERTONE BANDS; LASER; DCL;
COEFFICIENTS; STRENGTHS
AB A dipole moment function (DMF) for hydrogen chloride (HCl) has been obtained using a direct fit approach that fits the best available and appropriately weighted experimental data for individual ro-vibrational transitions. Combining wavefunctions derived from the Rydberg-Klein-Rees (RKR) numerical method and a semi-empirical DMF, line intensities were calculated numerically for bands with Delta v=0, 1, 2, 3, 4, 5, 6, 7 up to v'=7. The results have demonstrated the effectiveness of inclusion of rotational dipole moment matrix elements and appropriate weighting of the experimental data in the DMF fitting. The new method is shown to be superior to the common method of fitting only the rotationless dipole moment elements, while at the same time being simple to implement. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Gordon, I. E.; Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
[Li, G.; Bernath, P. F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM igordon@cfa.harvard.edu
RI Bernath, Peter/B-6567-2012; Li, Gang/P-2272-2015;
OI Bernath, Peter/0000-0002-1255-396X; Li, Gang/0000-0002-5605-7896;
Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847
FU NASA Planetary Atmospheres [NNX10AB94G]
FX We are very thankful to Professor R. J. Le Roy for advice on the use of
his invaluable programs such as LEVEL and RKR. We also thank Professors
J. Coxon and P. Hajigeorgiou for providing us the new H35Cl
potential prior to publication. This work has been supported by NASA
Planetary Atmospheres Grant NNX10AB94G.
NR 40
TC 16
Z9 16
U1 2
U2 27
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 JUL
PY 2011
VL 112
IS 10
BP 1543
EP 1550
DI 10.1016/j.jqsrt.2011.03.014
PG 8
WC Optics; Spectroscopy
SC Optics; Spectroscopy
GA 778OS
UT WOS:000291714600005
ER
PT J
AU Gould, L
Power, ML
Ellwanger, N
Rambeloarivony, H
AF Gould, Lisa
Power, Michael L.
Ellwanger, Nicholas
Rambeloarivony, Hajamanitra
TI Feeding Behavior and Nutrient Intake in Spiny Forest-Dwelling
Ring-Tailed Lemurs (Lemur catta) During Early Gestation and Early to
Mid-Lactation Periods: Compensating in a Harsh Environment
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Article
DE Lemur catta; nutrition; reproductive females; spiny forest
ID MAHAFALY SPECIAL RESERVE; PROSIMIAN PRIMATES; MILK-COMPOSITION; SOUTHERN
MADAGASCAR; BERENTY-RESERVE; CEBUS-CAPUCINUS; PATTERNS; EULEMUR; DIET;
REPRODUCTION
AB Strong resource seasonality in Madagascar has led to the evolution of female feeding priority and weaning synchrony in most lemur species. For these taxa, pregnancy/early lactation periods coincide with low food availability, and weaning of infants is timed with increased resources at the onset of the rainy season. Reproductive females experience high metabolic requirements, which they must accommodate, particularly when food resources are scarce. Female ring-tailed lemurs (Lemur catta) residing in spiny forest habitat must deal with resource scarcity, high temperatures (similar to 36-40 degrees C) and little shade in early to mid-lactation periods. Considered "income breeders," these females must use resources obtained from the environment instead of relying on fat stores; thus, we expected they would differ from same-sized males in time spent on feeding and in the intake of food and nutrients. We investigated these variables in two groups (N = 11 and 12) of Lemur catta residing in spiny forest habitat during early gestation and early to mid-lactation periods. Focal animal data and food plant samples were collected, and plants were analyzed for protein, kcal, and fiber. We found no sex differences for any feeding or nutrient intake variable for the top five food species consumed. Females in early gestation spent more time feeding compared with early/mid-lactation. Physiological compensation for spiny forest-dwelling females may be tied to greater time spent resting compared with gallery forest conspecifics, consuming foods high in protein, calories, and water, reduced home range defense in a sparsely populated habitat, and for Lemur catta females in general, production of relatively dilute milk compared with many strepsirrhines. Am J Phys Anthropol 145: 469-479, 2011. (C) 2011 Wiley-Liss, Inc.
C1 [Gould, Lisa] Univ Victoria, Dept Anthropol, Victoria, BC V8W 3P5, Canada.
[Power, Michael L.] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA.
[Ellwanger, Nicholas] Univ Texas San Antonio, Dept Anthropol, San Antonio, TX USA.
[Rambeloarivony, Hajamanitra] Oxford Brookes Univ, Dept Anthropol, Oxford OX3 0BP, England.
RP Gould, L (reprint author), Univ Victoria, Dept Anthropol, Victoria, BC V8W 3P5, Canada.
EM lgould@uvic.ca
OI Power, Michael/0000-0002-6120-3528
FU Natural Sciences and Engineering Research Council of Canada (NSERC)
FX Grant sponsor: Natural Sciences and Engineering Research Council of
Canada (NSERC).
NR 75
TC 12
Z9 14
U1 4
U2 71
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0002-9483
EI 1096-8644
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD JUL
PY 2011
VL 145
IS 3
BP 469
EP 479
DI 10.1002/ajpa.21530
PG 11
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 781QX
UT WOS:000291949700014
PM 21541932
ER
PT J
AU Werner, K
Rauch, T
Kruk, JW
Kurucz, RL
AF Werner, K.
Rauch, T.
Kruk, J. W.
Kurucz, R. L.
TI Iron abundance in the prototype PG1159 star, GW Vir pulsator PG1159-035,
and related objects
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars: abundances; stars: atmospheres; stars: evolution; stars: AGB and
post-AGB; white dwarfs
ID WHITE-DWARFS; ULTRAVIOLET SPECTROSCOPY; HOT; FUSE; HST; SUN
AB We performed an iron abundance determination of the hot, hydrogen deficient post-AGB star PG1159-035, which is the prototype of the PG1159 spectral class and the GW Vir pulsators, and of two related objects (PG1520+525, PG1144+005), based on the first detection of Fe VIII lines in stellar photospheres. In another PG1159 star, PG1424+535, we detect Fe VII lines. In all four stars, each within T-eff = 110 000-150 000 K, we find a solar iron abundance. This result agrees with our recent abundance analysis of the hottest PG1159 stars (T-eff = 150 000-200 000 K) that exhibit Fe x lines. On the whole, we find that the PG1159 stars are not significantly iron deficient, in contrast to previous notions.
C1 [Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany.
[Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Werner, K (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany.
EM werner@astro.uni-tuebingen.de
RI Kruk, Jeffrey/G-4047-2012
FU NASA [NAS5-32985, NAS5-26666, NAS5-26555]; German Aerospace Centre (DLR)
[05 OR0806]; NASA Office of Space Science [NNX09AF08G]
FX Based on observations made with the NASA-CNES-CSA Far Ultraviolet
Spectroscopic Explorer. FUSE was operated for NASA by the Johns Hopkins
University under NASA contract NAS5-32985. Based on observations with
the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
Science Institute, which is operated by the Association of Universities
for Research in Astronomy, Inc., under NASA contract NAS5-26666.; T.R.
is supported by the German Aerospace Centre (DLR) under grant 05 OR0806.
Some of the data presented in this paper were obtained from the
Multimission Archive at the Space Telescope Science Institute (MAST).
STScI is operated by the Association of Universities for Research in
Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for
non-HST data is provided by the NASA Office of Space Science via grant
NNX09AF08G and by other grants and contracts.
NR 19
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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 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2011
VL 531
AR A146
DI 10.1051/0004-6361/201116992
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795YZ
UT WOS:000293017700168
ER
PT J
AU Brown, JL
AF Brown, Janine L.
TI Lions, Tigers, Bears, and Elephants: Potential New Models for
Reproductive Endocrinology and Infertility.
SO BIOLOGY OF REPRODUCTION
LA English
DT Meeting Abstract
CT 44th Annual Meeting of the Society-for-the-Study-of-Reproduction (SSR)
CY 2011
CL Portland, OR
SP Soc Study Reproduct
C1 [Brown, Janine L.] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
NR 0
TC 0
Z9 0
U1 2
U2 9
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD JUL
PY 2011
VL 85
SI SI
MA 20
PG 2
WC Reproductive Biology
SC Reproductive Biology
GA 032VC
UT WOS:000310746200211
ER
PT J
AU Comizzoli, P
AF Comizzoli, Pierre
TI Building Bridges Between Wild Species and Human Reproductive Science
Through Fertility Preservation Studies.
SO BIOLOGY OF REPRODUCTION
LA English
DT Meeting Abstract
CT 44th Annual Meeting of the Society-for-the-Study-of-Reproduction (SSR)
CY 2011
CL Portland, OR
SP Soc Study Reproduct
C1 [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Washington, DC USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD JUL
PY 2011
VL 85
SI SI
MA 22
PG 2
WC Reproductive Biology
SC Reproductive Biology
GA 032VC
UT WOS:000310746200212
ER
PT J
AU Graves-Herring, JE
Wildt, DE
Comizzoli, P
AF Graves-Herring, Jennifer E.
Wildt, David E.
Comizzoli, Pierre
TI Protective Effect of Trehalose During Desiccation and Storage of
Oocytes: A Novel Approach to Preserve the Germinal Vesicle Using the Cat
Model
SO BIOLOGY OF REPRODUCTION
LA English
DT Meeting Abstract
CT 44th Annual Meeting of the Society-for-the-Study-of-Reproduction (SSR)
CY 2011
CL Portland, OR
SP Soc Study Reproduct
C1 [Graves-Herring, Jennifer E.; Wildt, David E.; Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
NR 0
TC 1
Z9 1
U1 0
U2 1
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD JUL
PY 2011
VL 85
SI SI
MA 321
PG 2
WC Reproductive Biology
SC Reproductive Biology
GA 032VC
UT WOS:000310746200333
ER
PT J
AU Hobbs, RJ
Comizzoli, P
Wildt, DE
Howard, J
AF Hobbs, Rebecca J.
Comizzoli, Pierre
Wildt, David E.
Howard, JoGayle
TI Developmental, but Not Meiotic, Competence of Cat Oocytes Is Affected by
Seasonal Anestrus
SO BIOLOGY OF REPRODUCTION
LA English
DT Meeting Abstract
CT 44th Annual Meeting of the Society-for-the-Study-of-Reproduction (SSR)
CY 2011
CL Portland, OR
SP Soc Study Reproduct
C1 [Hobbs, Rebecca J.; Comizzoli, Pierre; Wildt, David E.; Howard, JoGayle] Smithsonian Conservat Biol Inst, Front Royal, VA USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU SOC STUDY REPRODUCTION
PI MADISON
PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA
SN 0006-3363
J9 BIOL REPROD
JI Biol. Reprod.
PD JUL
PY 2011
VL 85
SI SI
MA 327
PG 2
WC Reproductive Biology
SC Reproductive Biology
GA 032VC
UT WOS:000310746200446
ER
PT J
AU Prado, A
Ledezma, J
Cubilla-Rios, L
Bede, JC
Windsor, DM
AF Prado, Alberto
Ledezma, Julieta
Cubilla-Rios, Luis
Bede, Jacqueline C.
Windsor, Donald M.
TI Two Genera of Aulacoscelinae Beetles Reflexively Bleed Azoxyglycosides
Found in Their Host Cycads
SO JOURNAL OF CHEMICAL ECOLOGY
LA English
DT Article
DE Aulacoscelinae; Aulacoscelis; Azoxyglycosides; Chrysomelidae;
Coleoptera; Dioon; Janbechynea; Reflex bleeding; Zamia; Zamiaceae
ID EUMAEUS-ATALA; CYCASIN; CHRYSOMELIDAE; METHYLAZOXYMETHANOL; COLEOPTERA;
EVOLUTION; DEFENSE
AB Aulacoscelinae beetles have an ancient relationship with cycads (Cycadophyta: Zamiaceae), which contain highly toxic azoxyglycoside (AZG) compounds. How these "primitive" leaf beetles deal with such host-derived compounds remains largely unknown. Collections were made of adult Aulacoscelis appendiculata from Zamia cf. elegantissima in Panama, A. vogti from Dioon edule in Mexico, and Janbechynea paradoxa from Zamia boliviana in Bolivia. Total AZG levels were quantified in both cycad leaves and adult beetles by high performance liquid chromatography (HPLC). On average, cycad leaves contained between 0.5-0.8% AZG (frozen weight, FW), while adult beetles feeding on the same leaves contained even higher levels of the compounds (average 0.9-1.5% FW). High AZG levels were isolated from reflex bleeding secreted at the leg joints when beetles were disturbed. Nuclear magnetic resonance and mass spectroscopy identified two AZGs, cycasin and macrozamin, in the reflex bleeding; this is the first account of potentially plant-derived compounds in secretions of the Aulacoscelinae. These data as well as the basal phylogenetic position of the Aulacoscelinae suggest that sequestration of plant secondary metabolites appeared early in leaf beetle evolution.
C1 [Prado, Alberto; Bede, Jacqueline C.] McGill Univ, Dept Plant Sci, Quebec City, PQ H9X 3V9, Canada.
[Ledezma, Julieta] Museo Hist Nat Noel Kempff Mercado, Santa Cruz, CA USA.
[Cubilla-Rios, Luis] Univ Panama, Fac Nat & Exact Sci & Technol, Panama City, Panama.
[Windsor, Donald M.] Smithsonian Trop Res Inst, Balboa, Panama.
RP Bede, JC (reprint author), McGill Univ, Dept Plant Sci, 21 111 Lakeshore, Quebec City, PQ H9X 3V9, Canada.
EM jacqueline.bede@mcgill.ca
FU McGill's Neotropical Environmental Option program; Smithsonian Tropical
Research Institute; Mexican government through CONACYT; NSERC
FX We are grateful to the following people for assistance; Laura Yanez
(Universidad Autonoma de San Luis Potosi) and Alberto S. Taylor
(Universidad de Panama) for advice and field information, Alejandro
Beqarano (Natural History Museum Noel Kempf Mercado) and Tony Bonasso
(Reserva Privada Patrimonio Natural - Potrerillos del Guenda), Santa
Cruz, Bolivia; Titto Varughese, Humberto Ortega, and Johannys Lakey
(Universidad de Panama) for assistance during AZG isolation, HPLC, and
NMR analysis and Alexandra Furtos-Matel (Universite de Montreal) for MS
analysis. As well, we thank two anonymous reviewers and Guillaume Dury
for insightful comments to an earlier version of the manuscript. This
research was funded by McGill's Neotropical Environmental Option
program, the Smithsonian Tropical Research Institute, the Mexican
government through CONACYT, and an NSERC operating grant to J.C.B. Leaf
and beetle collections in Panama were performed under Panama's Ministry
of the Environment (ANAM) permit numbers SE/AP-4-09, SE/AP-7-10).
NR 16
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U1 2
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PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0098-0331
J9 J CHEM ECOL
JI J. Chem. Ecol.
PD JUL
PY 2011
VL 37
IS 7
BP 736
EP 740
DI 10.1007/s10886-011-9977-5
PG 5
WC Biochemistry & Molecular Biology; Ecology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology
GA 785GM
UT WOS:000292215400010
PM 21656034
ER
PT J
AU Weigt, LA
AF Weigt, Lee A.
TI CONGEN-2010: A Semester in a Fortnight
SO JOURNAL OF HEREDITY
LA English
DT Editorial Material
C1 Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, Washington, DC 20250 USA.
RP Weigt, LA (reprint author), Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, MRC534, Washington, DC 20250 USA.
EM weigtl@si.edu
NR 0
TC 0
Z9 0
U1 0
U2 1
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-1503
J9 J HERED
JI J. Hered.
PD JUL-AUG
PY 2011
VL 102
IS 4
BP 494
EP 495
DI 10.1093/jhered/esr057
PG 2
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 784CI
UT WOS:000292130800014
PM 21670175
ER
PT J
AU Glynn, PW
Colley, SB
Guzman, HM
Enochs, IC
Cortes, J
Mate, JL
Feingold, JS
AF Glynn, P. W.
Colley, S. B.
Guzman, H. M.
Enochs, I. C.
Cortes, J.
Mate, J. L.
Feingold, J. S.
TI Reef coral reproduction in the eastern Pacific: Costa Rica, Panama, and
the Galapagos Islands (Ecuador). VI. Agariciidae, Pavona clavus
SO MARINE BIOLOGY
LA English
DT Article
ID SEA-SURFACE TEMPERATURE; GREAT-BARRIER-REEF; EL-NINO; OCEAN
ACIDIFICATION; THERMAL-STRESS; CLIMATE-CHANGE; RECOVERY; ECUADOR;
VARIABILITY; SCLERACTINIA
AB The reproductive ecology of the zooxanthellate reef coral Pavona clavus was investigated at several sites in Costa Rica, Panama, and the Galapagos Islands (Ecuador) over the period 1985-2009. Pavona clavus displayed stable gonochorism as only five hermaphrodites were found in 590 samples. At four of five locations, sex ratios were skewed toward female dominance; however, at Saboga Island (Panama) male colonies predominated. In Panama, sexual maturity was observed in an estimated eight-year-old female colony, and several colonies of 10-20 years of age demonstrated gametogenesis. Sexual activity was observed at all study sites, but gamete development occurred in only 14-31% of colonies sampled sporadically. Seasonality of gametogenic activity occurred predominantly during the warm/wet season, June to August, at mainland sites (Cao Island, Costa Rica, and Gulfs of Chiriqui and Panama, Panama). This pattern was repeated in the Galapagos Islands, but mainly from March to May when seasonally high sea temperatures and rainfall prevailed there. Histological sampling and field observations indicated that spawning was centered around the full moon, most frequently on lunar day 17, and near sunset (1,800 h). Mean fecundity (mature ova cm(-2) live tissue) estimates were significantly different for two sites and ranged from similar to 1,780 (Saboga Island, Gulf of Panama, seasonally upwelling) to similar to 4,280 (Uva Is, Gulf of Chiriqui, non-upwelling). Assuming three annual spawning events colony(-1) (August, September, October), extrapolation of minimum and maximum fecundities yield 5,340 and 12,840 ova cm(-2) year(-1). Seasonal, lunar, and diel spawning patterns in nine zooxanthellate species at Uva Island indicate asynchronous coral community spawning.
C1 [Glynn, P. W.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA.
[Colley, S. B.] PBS&J, Metairie, LA 70002 USA.
[Guzman, H. M.; Mate, J. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
[Enochs, I. C.] Univ Miami, Cooperat Inst Marine & Atmospher Sci, Rosenstiel Sch Marine & Atmospher Sci, Miami, FL 33149 USA.
[Cortes, J.] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica.
[Cortes, J.] Univ Costa Rica, Escuela Biol, San Jose 115012060, Costa Rica.
[Feingold, J. S.] Nova SE Univ Oceanog Ctr, Dania, FL 33004 USA.
RP Glynn, PW (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.
EM pglynn@rsmas.miami.edu
RI Enochs, Ian/B-8051-2014
OI Enochs, Ian/0000-0002-8867-0361
FU US National Science Foundation [OCE-0526361]
FX For help with collections, field observations, and laboratory work, we
thank Andrew Baker, Kathy Black, Celina Bourbonierre, Viktor
Brandtneris, Luis D'Croz, Peggy Fong, Erin Kapostasy, Priscilla
Martinez, Fernando Rivera, Tyler Smith, Lauren Toth, Anibal Velarde, and
Nancy Voss. Bernadette Bezy shared observations on spawning in Costa
Rica, and for this we are very grateful. Research support was provided
by the US National Science Foundation, Biological Oceanography Program,
grant OCE-0526361 and earlier awards. Thanks are due to the following
host-country institutions for facilitating this research: Costa Rica,
Centro de Investigaciones en Ciencias del Mar y Limnologia (CIMAR),
Universidad de Costa Rica, and Sistema Nacional de Areas de
Conservacion, Ministerio del Ambiente y Energia; Panama, Departamento de
Biologia Acuatica, Autoridad Nacional del Ambiente (ANAM), and
Smithsonian Tropical Research Institute; Ecuador, Charles Darwin
Research Station, and the Galapagos National Park Service. This is a
contribution from the University of Miami, Rosenstiel School of Marine
and Atmospheric Science.
NR 54
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U1 0
U2 31
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD JUL
PY 2011
VL 158
IS 7
BP 1601
EP 1617
DI 10.1007/s00227-011-1673-z
PG 17
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 781HT
UT WOS:000291922200013
ER
PT J
AU Chisholm, RA
Pacala, SW
AF Chisholm, Ryan A.
Pacala, S. W.
TI Independent species in independent niches behave neutrally: a response
SO OIKOS
LA English
DT Editorial Material
C1 [Pacala, S. W.] Princeton Univ, Dept Ecol & Evolut Biol, Princeton, NJ 08544 USA.
[Chisholm, Ryan A.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA.
RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, MRC0580-12,Unit 9100,Box 0948, Dpo, AA 34002 USA.
EM ryan.chis@gmail.com
RI Chisholm, Ryan/H-8033-2012
NR 4
TC 0
Z9 0
U1 0
U2 11
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 2011
VL 120
IS 7
BP 964
EP 965
DI 10.1111/j.1600-0706.2011.19880.x
PG 2
WC Ecology
SC Environmental Sciences & Ecology
GA 783WH
UT WOS:000292114300002
ER
PT J
AU Ruger, N
Huth, A
Hubbell, SP
Condit, R
AF Rueger, Nadja
Huth, Andreas
Hubbell, Stephen P.
Condit, Richard
TI Determinants of mortality across a tropical lowland rainforest community
SO OIKOS
LA English
DT Article
ID SEEDLING SURVIVAL; TREE MORTALITY; LIGHT GRADIENT; COSTA-RICA;
PHYSIOLOGICAL TRAITS; DIPTEROCARP FOREST; SHADE TOLERANCE; SEVERE
DROUGHT; LA-SELVA; GROWTH
AB Tree mortality is an important process determining forest dynamics. However, in species-rich tropical forests it is largely unknown, how species differ in their response of mortality to resource availability and individual condition. We use a hierarchical Bayesian approach to quantify the impact of light availability, tree size and past growth on mortality of 284 woody species in a 50-ha long-term forest census plot in Barro Colorado Island, Panama. Light reaching each individual tree was estimated from yearly vertical censuses of vegetation density. Across the community, 78% of the species showed increasing mortality with increasing light. Considering species individually, just 29 species showed a significant response to light, all with increasing mortality at high light. Past growth had a significant impact on all but three species, with higher growth leading to lower mortality. For the majority of species, mortality decreased sharply with diameter in saplings, then levelled off or increased slightly towards the maximum diameter of the species. Diameter had the biggest impact on mortality, followed by past growth and finally light availability. Our results challenge many previous reports of higher mortality in shade, and we suggest that it is crucial to control for size effects when assessing the impact of environmental conditions on mortality.
C1 [Rueger, Nadja; Huth, Andreas] UFZ Helmholtz Ctr Environm Res, UFZ, Dept Ecol Modelling, DE-04318 Leipzig, Germany.
[Condit, Richard] Natl Ctr Ecol Anal & Synth, Santa Barbara, CA 93101 USA.
[Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA.
[Hubbell, Stephen P.; Condit, Richard] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA.
RP Ruger, N (reprint author), Univ Leipzig, AG Spezielle Bot & Funkt Biodiversitat, Johannisallee 21-23, DE-04103 Leipzig, Germany.
EM nadja.rueger@uni-leipzig.de
RI Ruger, Nadja/J-6393-2015
OI Ruger, Nadja/0000-0003-2371-4172
FU Center for Tropical Forest Science; National Center for Ecological
Analysis and Synthesis (Santa Barbara, USA); US National Science
Foundation; John D. and Catherine D. McArthur Foundation; Smithsonian
Tropical Research Institute
FX We thank Helene Muller-Landau for providing the step width adjusting
routine of the Metropolis-Hastings algorithm and Jens Doleschal and the
Center for Information Services and High Performance Computing,
Technische Univ. Dresden, for the parallelisation of the R code and
computing resources. NR was supported by a research grant from the
Center for Tropical Forest Science, and RC by a fellowship from the
National Center for Ecological Analysis and Synthesis (Santa Barbara,
USA). The BCI plot has been made possible through the support of the US
National Science Foundation, the John D. and Catherine D. McArthur
Foundation, and the Smithsonian Tropical Research Institute. We thank
the dozens of field assistants and botanists who have collected data on
trees and carried out the canopy censuses in the BCI plot over the past
25 years.
NR 56
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U1 3
U2 42
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 2011
VL 120
IS 7
BP 1047
EP 1056
DI 10.1111/j.1600-0706.2010.19021.x
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 783WH
UT WOS:000292114300012
ER
PT J
AU Rick, TC
AF Rick, Torben C.
TI Weathering the storm: Coastal subsistence and ecological resilience on
Late Holocene Santa Rosa Island, California
SO QUATERNARY INTERNATIONAL
LA English
DT Article
ID NORTHERN CHANNEL-ISLANDS; SOUTHERN-CALIFORNIA; PREHISTORIC CALIFORNIA;
RESOURCE DEPRESSION; PACIFIC-NORTHWEST; HUNTER-GATHERERS; HUMAN IMPACTS;
MARINE; ARCHAEOLOGY; AMERICA
AB Archaeological research on California's Channel Islands has significantly enhanced understanding of the diversity and variability of coastal hunter-gatherers and the shell middens these people left behind. On the Channel Islands, the Late Holocene was a time of substantial population growth, territoriality, and the emergence of social hierarchies. The role of marine and terrestrial climate change, population growth, human environmental impacts, and other variables in driving Late Holocene cultural and ecological developments is a subject of considerable debate. Analysis of faunal remains (especially finfish and shellfish), complemented by human skeletal and stable isotope analyses, from a massive shell midden and village complex (CA-SRI-2) on Santa Rosa Island provides insight into Late Holocene human responses to coastal resource stress and environmental change. Despite significant population growth, the emergence of social stratification, and increased pressure on local resources and ecosystems, these data demonstrate that there is significant continuity in the coastal resources Channel Island peoples exploited through time. These results document the long-term resilience and adaptability of coastal hunter-gatherers, the marine resources they harvested, and Channel Island ecosystems. (C) 2010 Elsevier Ltd and INQUA. All rights reserved.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA.
RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA.
EM rickt@si.edu
FU National Science Foundation [BCS-0201668]; National Park Service
[1443CA8120-00-007]
FX This research was funded by a National Science Foundation Dissertation
Improvement Grant (BCS-0201668) and the National Park Service
(Cooperative Agreement 1443CA8120-00-007). I thank Ann Huston, Kelly
Minas, Don Morris, and Mark Senning of Channel Islands National Park for
supporting this research. I also thank my Ph.D. dissertation committee
members-Jon Erlandson, Mel Aikens, Doug Kennett, John Johnson, Madonna
Moss, and Cathy Whitlock-for helpful comments on this research. Jeanne
Arnold and Terry Jones also provided helpful comments on earlier work at
CA-SRI-2. Dan Guthrie helped analyze the bird remains and Ken Gobalet
helped with the analysis of small fish remains. I also thank the special
issue editors, Lynn Gamble, and an anonymous reviewer for comments
during the review process.
NR 74
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U1 1
U2 18
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 1040-6182
EI 1873-4553
J9 QUATERN INT
JI Quat. Int.
PD JUL 1
PY 2011
VL 239
BP 135
EP 146
DI 10.1016/j.quaint.2010.06.008
PG 12
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 784AF
UT WOS:000292125300013
ER
PT J
AU Owen, RB
Renaut, RW
Potts, R
Behrensmeyer, AK
AF Owen, R. B.
Renaut, R. W.
Potts, R.
Behrensmeyer, A. K.
TI Geochemical trends through time and lateral variability of diatom floras
in the Pleistocene Olorgesailie Formation, southern Kenya Rift Valley
SO QUATERNARY RESEARCH
LA English
DT Article
DE Diatoms; Geochemistry; Sedimentology; Weathering; REE data; Lakes;
Olorgesailie; East African Rift System
ID HUMAN-EVOLUTION; TRACE-ELEMENTS; LAKE; SEDIMENTS; HISTORY; CLIMATE;
OLDUVAI; TANZANIA; ENGLAND; AFRICA
AB The Olorgesailie Formation (1.2-0.49 Ma) consists of fluvial and lacustrine rift sediments that have yielded abundant Acheulean artifacts and a fossil hominin (Homo cf. erectus). In testing prior understandings of the paleoenvironmental context, we define nine new geochemical zones. A Chemical Index of Alteration suggests increased catchment weathering during deposition of Members 1, 2, 7, 11, and 13. Biophile elements (Br, S) peak in M8-9 and lower M13 possibly reflecting increased input from soil erosion. REE data show that the Magadi Trachytes supplied most siliciclastic grains. Sixteen diatom stages indicate conductivities of 200-16,000 mu S cm(-1) and pH of 7.5-9.5 for five deep-water lakes, ten shallow lakes and sixteen wetlands. These results are compared with diatom data from other sections in the basin and show aquatic spatial variability over km-scale distances. Similar floras are traceable over several kilometers for M2, M3 and M9, indicating broadly homogeneous lacustrine conditions during these times, but diatoms in other members imply variable conditions, some related to local tectonic controls. This lateral and temporal variability emphasizes the importance of carrying out stratigraphic sampling at multiple sites within a basin in efforts to define the environmental context relevant to human evolution. (C) 2011 University of Washington. Published by Elsevier Inc. All rights reserved.
C1 [Owen, R. B.] Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China.
[Renaut, R. W.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada.
[Potts, R.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA.
[Potts, R.] Natl Museums Kenya, Paleontol Sect, Dept Earth Sci, Nairobi, Kenya.
[Behrensmeyer, A. K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Owen, RB (reprint author), Hong Kong Baptist Univ, Dept Geog, Kowloon Tong, Hong Kong, Peoples R China.
EM owen@hkbu.edu.hk; robin.renaut@usask.ca; pottsr@si.edu; behrensa@si.edu
OI Owen, Richard Bernhart/0000-0001-5267-5366
FU National Museums of Kenya (NMK); NMK Paleontology Section (Earth
Sciences); Hong Kong Research Grants Council [201709]; Hong Kong Baptist
University [FRG/08-09/II-25]; NSERC [629-2008]; National Science
Foundation [0218511]; Peter Buck Fund for Research in Human Origins;
Smithsonian Human Origins Program
FX We thank the National Museums of Kenya (NMK) and the NMK Paleontology
Section (Earth Sciences), for support of the Olorgesailie project. Owen
was funded by the Hong Kong Research Grants Council (201709) and Hong
Kong Baptist University (FRG/08-09/II-25); Renaut was funded by an NSERC
Discovery Grant (629-2008). Fieldwork was supported by the National
Science Foundation (HOMINID grant 0218511), the Peter Buck Fund for
Research in Human Origins, and the Smithsonian Human Origins Program. We
thank Muteti Nume and Jennifer Clark for field support.
NR 46
TC 9
Z9 9
U1 1
U2 12
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0033-5894
EI 1096-0287
J9 QUATERNARY RES
JI Quat. Res.
PD JUL
PY 2011
VL 76
IS 1
BP 167
EP 179
DI 10.1016/j.yqres.2011.05.002
PG 13
WC Geography, Physical; Geosciences, Multidisciplinary
SC Physical Geography; Geology
GA 784RK
UT WOS:000292175700015
ER
PT J
AU Clough, GW
AF Clough, G. Wayne
TI A Better Space
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-AUG
PY 2011
VL 42
IS 4
BP 28
EP 28
PG 1
WC Humanities, Multidisciplinary
SC Arts & Humanities - Other Topics
GA 783ZB
UT WOS:000292122300011
ER
PT J
AU Strong, EE
AF Strong, Ellen E.
TI More than a gut feeling: utility of midgut anatomy in phylogeny of the
Cerithioidea (Mollusca: Caenogastropoda)
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE character evolution; feeding biology; homology; morphology; phylogenetic
utility
ID LAKE TANGANYIKA; MOLECULAR PHYLOGENY; ADAPTIVE RADIATION; EAST-AFRICA;
GASTROPOD; PROSOBRANCHIA; PACHYCHILIDAE; SYSTEMATICS; PALUDOMIDAE;
MORPHOLOGY
AB The Cerithioidea is a large and diverse superfamily of marine, brackish, and freshwater snails. The complexity and variety of midgut features within this group have long been known, but have been underutilized as a resource of characters for phylogenetic analysis. Consequently, this group is an ideal system for assessing the utility of midgut anatomy at lower systematic levels. Midgut anatomy of 46 cerithioidean gastropods and two outgroup taxa (Campanilidae, Plesiotrochidae) is described. A subset of these taxa, combined with published and unpublished descriptions for several additional species, were coded for 28 midgut characters. These characters were integrated with a large multi-organ system data set for 56 taxa, comprising 123 characters from the shell, radula, foregut, kidney, nerves, sperm ultrastructure, and reproductive system. The morphological matrix was analysed using parsimony, and was combined with a molecular data set of 16S and 28S rRNA sequences, and then analysed using parsimony and Bayesian methods. Optimization of midgut characters on the resulting cladograms indicates that midgut characters provide conservative and informative sources of variation at all hierarchical levels, from basal nodes to within family-level taxa. Exploratory analyses including and excluding midgut characters demonstrate the impact of midgut characters in elucidating phylogenetic relationships of cerithioideans, particularly among and within freshwater clades. Statistical analyses of retention index values for characters mapped on both the morphological and morphological plus molecular topologies confirm that midgut characters have significantly higher phylogenetic signals than other morphological characters. In the case of cerithioidean phylogeny, the importance of midgut data as a resource of characters cannot be overstated. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 162, 585-630. doi: 10.1111/j.1096-3642.2010.00687.x
C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
RP Strong, EE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA.
EM stronge@si.edu
OI Strong, Ellen/0000-0001-7181-4114
FU Deutscher Akademischer Austausch Dienst (DAAD)
FX I gratefully acknowledge the skill and patience of Marilyn Schotte
(USNM) in rendering the inked illustrations. I thank Matthias Glaubrecht
(ZMB) for providing logistical support during the initial part of this
work as a DAAD fellow in 1999. Financial support through a Deutscher
Akademischer Austausch Dienst (DAAD) Research Grant for Recent PhDs and
PhD Candidates is gratefully acknowledged. I am indebted to Winston
Ponder for routinely providing guidance, encouragement and feedback.
NR 92
TC 3
Z9 3
U1 3
U2 12
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0024-4082
J9 ZOOL J LINN SOC-LOND
JI Zool. J. Linn. Soc.
PD JUL
PY 2011
VL 162
IS 3
BP 585
EP 630
DI 10.1111/j.1096-3642.2010.00687.x
PG 46
WC Zoology
SC Zoology
GA 783TT
UT WOS:000292107600005
ER
PT J
AU Mah, C
Foltz, D
AF Mah, Christopher
Foltz, David
TI Molecular phylogeny of the Forcipulatacea (Asteroidea: Echinodermata):
systematics and biogeography
SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE Antarctica; deep-sea; echinoderms; Mesozoic; molecular systematics;
phylogenetic systematics; revision; Southern Hemisphere
ID SEA STARS LEPTASTERIAS; GULF-OF-MEXICO; ANTARCTIC PENINSULA;
FEEDING-BEHAVIOR; SOUTHERN-OCEAN; SEYMOUR ISLAND; CLIMATE-CHANGE;
CLASSIFICATION; GENUS; TAXA
AB We present a comprehensively sampled three-gene phylogeny of the monophyletic Forcipulatacea, one of three major lineages within the crown-group Asteroidea. We present substantially more Southern Hemisphere and deep-sea taxa than were sampled in previous molecular studies of this group. Morphologically distinct groups, such as the Brisingida and the Zoroasteridae, are upheld as monophyletic. Brisingida is supported as the derived sister group to the Asteriidae (restricted), rather than as a basal taxon. The Asteriidae is paraphyletic, and is broken up into the Stichasteridae and four primary asteriid clades: (1) a highly diverse boreal clade, containing members from the Arctic and sub-Arctic in the Northern Hemisphere; (2) the genus Sclerasterias; (3) and (4) two sister clades that contain asteriids from the Antarctic and pantropical regions. The Stichasteridae, which was regarded as a synonym of the Asteriidae, is resurrected by our results, and represents the most diverse Southern Hemisphere forcipulatacean clade (although two deep-sea stichasterid genera occur in the Northern Hemisphere). The Labidiasteridae is artificial, and should be synonymized into the Heliasteridae. The Pedicellasteridae is paraphyletic, with three separate clades containing pedicellasterid taxa emerging among the basal Forcipulatacea. Fossils and timing estimates from species-level phylogeographic studies are consistent with prior phylogenetic hypotheses for the Forcipulatacea, suggesting diversification of basal taxa in the early Mesozoic, with some evidence for more widely distributed ranges from Cretacous taxa. Our analysis suggests a hypothesis of an older fauna present in the Antarctic during the Eocene, which was succeeded by a modern Antarctic fauna that is represented by the recently derived Antarctic Asteriidae and other forcipulatacean lineages. (C) 2011 The Linnean Society of London, Zoological Journal of the Linnean Society, 2011, 162, 646-660. doi: 10.1111/j.1096-3642.2010.00688.x
C1 [Mah, Christopher] Smithsonian Inst, Washington, DC 20013 USA.
[Foltz, David] Louisiana State Univ Biol Sci, Baton Rouge, LA 70803 USA.
RP Mah, C (reprint author), Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA.
EM mahch@si.edu
FU NSF [OPP-0631245]; LSU
FX For providing specimens and facilitating specimen loans and materials,
we thank: Bob Carney, Louisiana State University; Cynthia Ahearn
(deceased), Tim Coffer, Paul Greenhall, and Dave Pawson, Smithsonian
Institution; Chrissy Piotrowski, Rich Mooi, Bob Van Syoc, and Susie
Lockhart, California Academy of Sciences; Tim O'Hara, Museum Victoria;
Martha Nizinski, National Marine Fisheries Service; Kate O'Neil and
Kareen Schnabel, National Institute of Water and Atmosphere (New
Zealand); and Marc Eleaume and Nadia Ameziane, Museum national
d'Histoire naturelle (Paris). The authors would also like to extend
special thanks to Mieko Komatsu for providing tissue from Plazaster.
John Pearse, UC Santa Cruz, Dan Blake, University of Illinois-Urbana
Champaign, and Lynn Parenti, Department of Ichthyology, Smithsonian
Institution, graciously read early drafts of the manuscript and
volunteered improvements. We are grateful to David Clague, Craig
MacClain, the personnel of the Monterey Bay Aquarium Research Institute
(MBARI), and the crew of the R/V Western Flyer for their efforts in
collecting material used herein. Thanks also to Sandra Brooke, Marine
Conservation Biology Institute (MCBI) for an image used in Fig. 1. This
research was supported by NSF-Polar Programs Postdoctoral Fellowship
OPP-0631245 to CM, and by an LSU Faculty Research Grant to DF.
NR 56
TC 11
Z9 11
U1 4
U2 17
PU WILEY-BLACKWELL
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 JUL
PY 2011
VL 162
IS 3
BP 646
EP 660
DI 10.1111/j.1096-3642.2010.00688.x
PG 15
WC Zoology
SC Zoology
GA 783TT
UT WOS:000292107600007
ER
PT J
AU Smith, HA
AF Smith, Howard A.
TI Alone in the Universe Despite the growing catalog of extrasolar planets,
data so far do not alter estimates that we are effectively on our own
SO AMERICAN SCIENTIST
LA English
DT Article
ID STARS
C1 [Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, MS-65,60 Garden St, Cambridge, MA 02138 USA.
EM hsmith@cfa.harvard.edu
NR 17
TC 5
Z9 5
U1 0
U2 3
PU SIGMA XI-SCI RES SOC
PI RES TRIANGLE PK
PA PO BOX 13975, RES TRIANGLE PK, NC 27709 USA
SN 0003-0996
J9 AM SCI
JI Am. Scientist
PD JUL-AUG
PY 2011
VL 99
IS 4
BP 320
EP 327
PG 8
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 776DH
UT WOS:000291514200022
ER
PT J
AU Strader, J
Caldwell, N
Seth, AC
AF Strader, Jay
Caldwell, Nelson
Seth, Anil C.
TI STAR CLUSTERS IN M31. V. INTERNAL DYNAMICAL TRENDS: SOME TROUBLESOME,
SOME REASSURING
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies: individual (M31); galaxies: star clusters: general; globular
clusters: general; stars: luminosity function, mass function
ID TO-LIGHT RATIOS; INITIAL MASS FUNCTION; GLOBULAR-CLUSTERS; FUNDAMENTAL
PLANE; STRUCTURAL PARAMETERS; POPULATION SYNTHESIS; MILKY-WAY; GALAXIES;
EVOLUTION; CATALOG
AB We present internal velocity dispersions and precise radial velocities for 200 globular clusters (GCs) in M31 that are derived using new high-resolution spectra from MMT/Hectochelle. Of these, 163 also have King model structural parameters that allow us to estimate their mass-to-light ratios. This is, by far, the largest such data set available for any galaxy, including the Milky Way. These data strongly confirm earlier suggestions that the optical and near-infrared mass-to-light ratios of M31 GCs decline with increasing metallicity. This behavior is the opposite of that predicted by stellar population models for a standard initial mass function. We show that this phenomenon does not appear to be caused by standard dynamical evolution. A shallower mass function for metal-rich GCs (with dN/dM proportional to M-0.8-M-1.3 below 1 M-circle dot) can explain the bulk of extant observations. We also observe a consistent, monotonic correlation between mass-to-light ratio and cluster mass. This correlation, in contrast to the correlation with metallicity, is well explained by the accepted model of dynamical evolution of GCs through mass segregation and the preferential loss of low-mass stars, and these data are among the best available to constrain this process.
C1 [Strader, Jay; Caldwell, Nelson; Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Strader, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jstrader@cfa.harvard.edu
FU NASA [NAS5-26555]; National Science Foundation [AST-0808099];
JPL/Caltech [1310512]
FX We thank Michele Cappellari, Charlie Conroy, Aaron Dotter, Diederick
Kruijssen, Soeren Larsen, Steinn Sigurdsson, and Graeme Smith for useful
comments and conversations; Susan Tokarz for help with the spectroscopic
data reduction; and Perry Berlind and Michael Calkins for help acquiring
the data. We thank the anonymous referee for a useful report. This work
was initiated while 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. Some of the
observations reported here were obtained at the MMT Observatory, a joint
facility of the Smithsonian Institution and the University of Arizona.
This paper uses data products produced by the OIR Telescope Data Center,
supported by the Smithsonian Astrophysical Observatory. Based on
observations made with the NASA/ESA Hubble Space Telescope and obtained
from the Hubble Legacy Archive, which is a collaboration between the
Space Telescope Science Institute (STScI/NASA), the Space Telescope
European Coordinating Facility (ST-ECF/ESA), and the Canadian Astronomy
Data Centre (CADC/NRC/CSA). This work was partially supported by the
National Science Foundation through grant AST-0808099. Partial support
for this work was provided by award 1310512, issued by JPL/Caltech.
NR 45
TC 60
Z9 60
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2011
VL 142
IS 1
AR 8
DI 10.1088/0004-6256/142/1/8
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 777AE
UT WOS:000291584200008
ER
PT J
AU Kiso, WK
Brown, JL
Siewerdt, F
Schmitt, DL
Olson, D
Crichton, EG
Pukazhenthi, BS
AF Kiso, Wendy K.
Brown, Janine L.
Siewerdt, Frank
Schmitt, Dennis L.
Olson, Deborah
Crichton, Elizabeth G.
Pukazhenthi, Budhan S.
TI Liquid Semen Storage in Elephants (Elephas maximus and Loxodonta
africana): Species Differences and Storage Optimization
SO JOURNAL OF ANDROLOGY
LA English
DT Article
DE Asian elephant; African elephant; spermatozoa; extender; temperature
ID ASIAN ELEPHANT; EGG-YOLK; MAMMALIAN SPERMATOZOA; ACROSOMAL INTEGRITY;
BOVINE SPERMATOZOA; SPERM MEMBRANES; RAM SPERMATOZOA; SEMINAL PLASMA;
NORTH-AMERICA; COLD-SHOCK
AB Artificial insemination plays a key role in the genetic management of elephants in zoos. Because freshly extended semen is typically used for artificial insemination in elephants, it has become imperative to optimize conditions for liquid storage and semen transport. The objectives of this study were to examine the interactions between different extenders and storage temperatures on sperm total motility, progressive motility, and acrosomal integrity in Asian (Elephas maximus) and African (Loxodonta africana) elephants. Ejaculates were collected by rectal massage, diluted using a split-sample technique in 5 semen extenders: TL-Hepes (HEP), Modena (MOD), Biladyl (BIL), TEST refrigeration medium (TES), and INRA96 (INR), maintained at 35 degrees C, 22 degrees C, or 4 degrees C. At 0, 4, 6, 12, and 24 hours, aliquots were removed and assessed for sperm total motility, progressive motility, and acrosomal integrity. After 24 hours of storage, African elephant spermatozoa exhibited greater longevity and higher values in sperm quality parameters compared with those of Asian elephants. In both species, semen storage at 35 degrees C resulted in a sharp decline in all sperm quality parameters after 4 hours of storage, whereas storage at 22 degrees C and 4 degrees C facilitated sperm survival. In Asian elephants, MOD and HEP were most detrimental, whereas BIL, TES, and INR maintained motility up to 12 hours when spermatozoa were cooled to 22 degrees C or 4 degrees C. In African elephants, there were no differences among extenders. All media maintained good sperm quality parameters at 22 degrees C or 4 degrees C. However, although MOD, BIL, and INR were most effective at lower temperatures, HEP and TES maintained sperm motility at all storage temperatures. This study demonstrated sperm sensitivity to components of various semen extenders and storage temperatures and offers recommendations for semen extender choices for liquid semen storage for both Asian and African elephants.
C1 [Kiso, Wendy K.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC 20008 USA.
[Brown, Janine L.; Pukazhenthi, Budhan S.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA.
[Siewerdt, Frank] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA.
[Schmitt, Dennis L.] Missouri State Univ, William H Darr Sch Agr, Springfield, MO USA.
[Schmitt, Dennis L.] Ringling Bros Ctr Elephant Conservat, Polk City, FL USA.
[Olson, Deborah] Int Elephant Fdn, Azle, TX USA.
[Olson, Deborah] Indianapolis Zoo, Indianapolis, IN USA.
[Crichton, Elizabeth G.] XY Inc, Navasota, TX USA.
RP Kiso, WK (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zoological Pk,POB 37012,MRC 5502, Washington, DC 20008 USA.
EM kisow@si.edu
RI Siewerdt, Frank/D-8523-2011
FU Bros Center for Elephant Conservation, International Elephant
Foundation; Association of Zoos and Aquariums, Indianapolis Zoo; Feld
Entertainment Inc.
FX Supported by Ringling Bros Center for Elephant Conservation,
International Elephant Foundation, Association of Zoos and Aquariums
Conservation Endowment Fund, Indianapolis Zoo, and Friends of the
National Zoo. Wendy K. Kiso was supported by a grant from Feld
Entertainment Inc.
NR 63
TC 15
Z9 15
U1 0
U2 10
PU AMER SOC ANDROLOGY, INC
PI LAWRENCE
PA C/O ALLEN PRESS, INC PO BOX 368, LAWRENCE, KS 66044 USA
SN 0196-3635
J9 J ANDROL
JI J. Androl.
PD JUL-AUG
PY 2011
VL 32
IS 4
BP 420
EP 431
DI 10.2164/jandrol.110.011460
PG 12
WC Andrology
SC Endocrinology & Metabolism
GA 773EG
UT WOS:000291289200012
PM 21127305
ER
PT J
AU Willyard, A
Wallace, LE
Wagner, WL
Weller, SG
Sakai, AK
Nepokroeff, M
AF Willyard, Ann
Wallace, Lisa E.
Wagner, Warren L.
Weller, Stephen G.
Sakai, Ann K.
Nepokroeff, Molly
TI Estimating the species tree for Hawaiian Schiedea (Caryophyllaceae) from
multiple loci in the presence of reticulate evolution
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
DE Hawai'i; Species trees; Reticulate evolution; Schiedea; Caryophyllaceae;
Low-copy nuclear loci
ID ADAPTIVE RADIATION; ALSINIDENDRON CARYOPHYLLACEAE; PHYLOGENETIC
ANALYSIS; MITOCHONDRIAL-DNA; CHLOROPLAST DNA; GENE TREES; SALICARIA
CARYOPHYLLACEAE; INBREEDING DEPRESSION; ADAMANTIS CARYOPHYLLACEAE;
LYDGATEI CARYOPHYLLACEAE
AB Schiedea (Caryophyllaceae) is a monophyletic genus of 34 species, all endemic to the Hawaiian Islands, that arose from a single colonization, providing one of the best examples of adaptive radiation in Hawaii. Species utilize a range of habitats and exhibit a variety of growth forms and transitions in breeding systems from hermaphroditism toward dimorphism or autogamy. Our study included the most thorough sampling to date: 2-5 individuals per species and 4 independent genetic partitions: eight plastid and three low-copy nuclear loci (9217 bps), allowing a three-locus BEST species tree. Despite incomplete resolution at the tips, our results support monophyly for each extant species. Gene trees revealed several clear cases of cytonuclear incongruence, likely created by interspecific introgression. Conflict occurs at the divergence of section Alphaschiedea as well as at the tips. Ages inferred from a BEAST analysis allow an original colonization onto either Nihoa or Kauai and inform some aspects of inter-island migrations. We suggest that several hard polytomies on the species tree are biologically realistic, signifying either nearly simultaneous speciation or historical introgressive hybridization. Based on inferred node ages that exceed expected coalescent times, we propose that undetected nuclear introgression may play a larger role than incomplete lineage sorting in sections Schiedea and Mononeura. (C) 2011 Elsevier Inc. All rights reserved.
C1 [Willyard, Ann; Nepokroeff, Molly] Univ S Dakota, Dept Biol, Vermillion, SD 57069 USA.
[Wallace, Lisa E.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA.
[Wagner, Warren L.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA.
[Weller, Stephen G.; Sakai, Ann K.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA.
RP Willyard, A (reprint author), Hendrix Coll, Dept Biol, 1600 Washington Ave, Conway, AR 72032 USA.
EM willyard@hendrix.edu; lisawallace@biology.msstate.edu; wagnerw@si.edu;
sgweller@uci.edu; aksakai@uci.edu; Molly.Nepokroeff@USD.edu
FU National Science Foundation [DEB-0445410]; National Tropical Botanical
Gardens McBryde Senior Research program
FX This research was supported by a Grant from the National Science
Foundation (DEB-0445410). The authors thank the National Tropical
Botanical Gardens McBryde Senior Research program for support to MN;
Douglas Jennewein and Joe Reynoldson for computing support; Tim Flynn,
Joel Lau, John Obata, Steve Perlman, Wayne Takeuchi, and Ken Wood for
field collections; Tina Clausen, Jeff Engeman, Bridget Jacobs, Calvin
Krogman, and Robynn Shannon for laboratory and herbarium work; L. Lacey
Knowles, Laura Kubatko and the participants in the Estimating Species
Trees workshop for inspiration; Adam Bazinet and Liang Liu for helpful
suggestions on software implementation.
NR 116
TC 22
Z9 22
U1 2
U2 19
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 JUL
PY 2011
VL 60
IS 1
BP 29
EP 48
DI 10.1016/j.ympev.2011.04.001
PG 20
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 775LD
UT WOS:000291459900004
PM 21511045
ER
PT J
AU Sutton-Grier, AE
Keller, JK
Koch, R
Gilmour, C
Megonigal, JP
AF Sutton-Grier, Ariana. E.
Keller, Jason K.
Koch, Rachel
Gilmour, Cynthia
Megonigal, J. Patrick
TI Electron donors and acceptors influence anaerobic soil organic matter
mineralization in tidal marshes
SO SOIL BIOLOGY & BIOCHEMISTRY
LA English
DT Article
DE Terminal electron acceptors (TEAs); Methane (CH(4)); Fe(III); SO(4)(2-);
Microbial respiration; Carbon quality; Maryland; Chesapeake Bay; Organic
carbon mineralization
ID METHANE PRODUCTION; SULFATE REDUCTION; WETLAND SOILS; RIPARIAN WETLAND;
FERRIC IRON; SALT-MARSH; DECOMPOSITION; SEDIMENTS; FRESH;
DENITRIFICATION
AB Anaerobic decomposition in wetland soils is carried out by several interacting microbial processes that influence carbon storage and greenhouse gas emissions. To understand the role of wetlands in the global carbon cycle, it is critical to understand how differences in both electron donor (i.e., organic carbon) and terminal electron acceptor (TEA) availability influence anaerobic mineralization of soil organic matter. In this study we manipulated electron donors and acceptors to examine how these factors influence total rates of carbon mineralization and the pathways of microbial respiration (e.g., sulfate reduction versus methanogenesis). Using a field-based reciprocal transplant of soils from brackish and freshwater tidal marshes, in conjunction with laboratory amendments of TEAs, we examined how rates of organic carbon mineralization changed when soils with different carbon contents were exposed to different TEAs. Total mineralization (the sum of CO(2) + CH(4) produced) on a per gram soil basis was greater in the brackish marsh soils, which had higher soil organic matter content: however, on a per gram carbon basis, mineralization was greater in the freshwater soils, suggesting that the quality of carbon inputs from the freshwater plants was higher. Overall anaerobic metabolism was higher for both soil types incubated at the brackish site where SO(4)(2-) was the dominant TEA. When soils were amended with TEAs in the laboratory, more thermodynamically favorable respiration pathways typically resulted in greater organic matter mineralization (Fe(III) respiration > SO(4)(2-) reduction > methanogenesis). These results suggest that both electron donors and acceptors play important roles in regulating anaerobic microbial mineralization of soil organic matter. (C) 2011 Elsevier Ltd. All rights reserved.
C1 [Sutton-Grier, Ariana. E.; Keller, Jason K.; Koch, Rachel; Gilmour, Cynthia; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Sutton-Grier, AE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM ariana.suttongrier@gmail.com
RI Gilmour, Cynthia/G-1784-2010;
OI Gilmour, Cynthia/0000-0002-1720-9498; Sutton-Grier,
Ariana/0000-0002-1242-7728
FU NSF [DEB-0516400]; Smithsonian Fellowship
FX We thank Allyson Bullock for help with sampling, Jim Duls and Liam
Megonigal for help in the field, and Tyler Bell and Joe Miklas for help
with laboratory work. This work was funded by NSF Grant DEB-0516400 to
P. Megonigal and a Smithsonian Fellowship to J. Keller. Thomas Jordan
provided valuable insights into the reciprocal transplant experimental
design. Thoughtful comments from two anonymous reviewers greatly
improved this manuscript.
NR 47
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U1 4
U2 74
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 2011
VL 43
IS 7
BP 1576
EP 1583
DI 10.1016/j.soilbio.2011.04.008
PG 8
WC Soil Science
SC Agriculture
GA 776YI
UT WOS:000291576800023
ER
PT J
AU Sjogersten, S
Cheesman, AW
Lopez, O
Turner, BL
AF Sjoegersten, Sofie
Cheesman, Alexander W.
Lopez, Omar
Turner, Benjamin L.
TI Biogeochemical processes along a nutrient gradient in a tropical
ombrotrophic peatland
SO BIOGEOCHEMISTRY
LA English
DT Article
DE Carbon; Enzymes; Forest diversity; Methane; Microbial biomass; Nitrogen;
Peat; Phosphorus; Soil respiration; Tropical wetland
ID SWAMP FOREST; MICROBIAL BIOMASS; COSTA-RICA; SPECIES-DIVERSITY;
EXTRACTION METHOD; COASTAL-PLAIN; 3 ECOSYSTEMS; LAND-USE; SOIL; WETLANDS
AB Biogeochemical properties, including nutrient concentrations, carbon gas fluxes, microbial biomass, and hydrolytic enzyme activities, were determined along a strong nutrient gradient in an ombrotrophic peatland in the Republic of Panama. Total phosphorus in surface peat decreased markedly along a 2.7 km transect from the marginal Raphia taedigera swamp to the interior sawgrass swamp, with similar trends in total nitrogen and potassium. There were parallel changes in the forest structure: basal area decreased dramatically from the margins to the interior, while tree diversity was greatest at sites with extremely low concentrations of readily-exchangeable phosphate. Soil microbial biomass concentrations declined in parallel with nutrient concentrations, although microbes consistently contained a large proportion (up to 47%) of the total soil phosphorus. Microbial C:P and N:P ratios and hydrolytic enzyme activities, including those involved in the cycles of carbon, nitrogen, and phosphorus, increased towards the nutrient-poor wetland interior, indicating strong below-ground nutrient limitation. Soil CO(2) fluxes and CH(4) fluxes did not vary systematically along the nutrient gradient, although potential soil respiration determined on drained soils was lower from nutrient-poor sites. Soil respiration responded strongly to drainage and increased temperature. Taken together, our results demonstrate that nutrient status exerts a strong control on above and below-ground processes in tropical peatlands with implications for carbon dynamics and hence long term development of such ecosystems.
C1 [Sjoegersten, Sofie] Univ Nottingham, Div Agr & Environm Sci, Sch Biosci, Nottingham NG7 2RD, England.
[Cheesman, Alexander W.] Univ Florida, Dept Soil & Water Sci, Gainesville, FL 32611 USA.
[Lopez, Omar; Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Sjogersten, S (reprint author), Univ Nottingham, Div Agr & Environm Sci, Sch Biosci, Univ Pk, Nottingham NG7 2RD, England.
EM sofie.sjogersten@nottingham.ac.uk
RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013
OI Turner, Benjamin/0000-0002-6585-0722; Cheesman,
Alexander/0000-0003-3931-5766
FU University of Nottingham; National Secretariat for Science and
Technology of the Republic of Panama [270-2006-87]; USDA-CREES National
Research Initiative [2004-35107-14918]
FX We thank Tania Romero for laboratory assistance, Eric Brown for field
support, Emma Wright and Jodie Hartill for assistance in collecting and
compiling the potential respiration data, and staff at the Smithsonian
Tropical Research Institute station in Bocas del Toro for logistical
support. Funding from the University of Nottingham supported this
project. Omar R. Lopez was funded by a postdoctoral research fellowship
by the National Secretariat for Science and Technology of the Republic
of Panama (No. 270-2006-87). Alexander Cheesman was funded by a grant
from the USDA-CREES National Research Initiative (No. 2004-35107-14918).
NR 70
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U1 11
U2 73
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD JUL
PY 2011
VL 104
IS 1-3
BP 147
EP 163
DI 10.1007/s10533-010-9493-7
PG 17
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 771OA
UT WOS:000291168900012
ER
PT J
AU Stanley, AA
Graham, AM
Wagner, RH
Morton, ES
Schug, MD
AF Stanley, Abby A.
Graham, Allie M.
Wagner, Richard H.
Morton, Eugene S.
Schug, Malcolm D.
TI Characterization of 10 polymorphic microsatellite markers for the purple
martin, Progne subis
SO CONSERVATION GENETICS RESOURCES
LA English
DT Article
DE Purple martin; Progne subis; Microsatellite; Genetic marker; Genetic
variation
ID PATERNITY; SUCCESS
AB The purple martin is a large North American swallow that suffered a severe population crash in the 20th century due to nesting competition from invasive species. We screened an enriched DNA library for microsatellites from purple martins (Progne subis subis). Ten loci consistently amplified and were polymorphic with an allele range of 2-19 and observed heterozygosity ranged from 0.31 to 0.93. Two loci are sex-linked, and two additional loci failed to meet Hardy-Weinberg expectations likely due to the presence of null alleles. These polymorphic microsatellite loci can be used for studies of genetic diversity, population structure, and relatedness, all of which have been suggested to determine the impact of substantial regional declines in population density.
C1 [Stanley, Abby A.; Graham, Allie M.; Schug, Malcolm D.] Univ N Carolina Greensboro, Dept Biol, Greensboro, NC 27402 USA.
[Wagner, Richard H.] Austrian Acad Sci, Konrad Lorenz Inst Ethol, A-1160 Vienna, Austria.
[Morton, Eugene S.] Smithsonian Inst, Washington, DC 20008 USA.
RP Schug, MD (reprint author), Univ N Carolina Greensboro, Dept Biol, 301 Eberhart Bldg, Greensboro, NC 27402 USA.
EM mdschug@uncg.edu
OI Graham, Allie/0000-0001-7404-168X
NR 16
TC 1
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U1 0
U2 8
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1877-7252
J9 CONSERV GENET RESOUR
JI Conserv. Genet. Resour.
PD JUL
PY 2011
VL 3
IS 3
BP 577
EP 579
DI 10.1007/s12686-011-9408-5
PG 3
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 771OG
UT WOS:000291169700041
ER
PT J
AU Welch, AJ
Fleischer, RC
AF Welch, Andreanna J.
Fleischer, Robert C.
TI Polymorphic microsatellite markers for the endangered Hawaiian petrel
(Pterodroma sandwichensis)
SO CONSERVATION GENETICS RESOURCES
LA English
DT Article
DE Microsatellite; Primers; Procellariidae; Pterodroma; Seabirds
ID AMPLIFICATION; POPULATION; SHEARWATER; SOFTWARE; LOCI
AB The endemic and endangered Hawaiian petrel (Pterodroma sandwichensis) breeds on four of the Hawaiian Islands, however the levels of gene flow between islands remain unclear. We describe 10 novel polymorphic microsatellite loci isolated from this species, and characterize 10 additional previously published primer sets in 40 individuals from the island of Maui. Loci exhibited between 3 and 14 alleles (mean 6.85), and observed heterozygosity ranged from 0.150 to 0.825 (mean 0.540). Four loci showed evidence for null alleles, although only one locus had significant deviation from Hardy-Weinberg equilibrium after Bonferonni correction. Two primer pairs showed significant gametic disequilibrium. The loci described here should provide a useful toolset for investigations of population connectivity.
C1 [Welch, Andreanna J.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA.
[Welch, Andreanna J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA.
RP Welch, AJ (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk,POB 37012,MRC 5513, Washington, DC 20013 USA.
EM WelchA@si.edu
FU Smithsonian's Office; Smithsonian Walcott Fund; NSF [DEB-0745604]
FX We are grateful to Josh Adams, David Anderson, Fern Duvall, Nick Holmes,
Jay Penniman, Helen James, Peggy Ostrom, Anne Wiley, Christina Gebhard,
Megan Spitzer, Hawaii Volcanoes National Park, and the University of
Washington Burke Museum for assistance obtaining samples. We also thank
Frank Hailer, Nancy Rotzel, Michelle Haynie, Colleen Cotton, and the
members of the CCEG lab group. Funding was provided by the Smithsonian's
Office of Fellowships, the Smithsonian Walcott Fund, and the NSF (grant
DEB-0745604).
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U1 0
U2 4
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 1877-7252
J9 CONSERV GENET RESOUR
JI Conserv. Genet. Resour.
PD JUL
PY 2011
VL 3
IS 3
BP 581
EP 584
DI 10.1007/s12686-011-9409-4
PG 4
WC Biodiversity Conservation; Genetics & Heredity
SC Biodiversity & Conservation; Genetics & Heredity
GA 771OG
UT WOS:000291169700042
ER
PT J
AU Hauber, DP
Saltonstall, K
White, DA
Hood, CS
AF Hauber, Donald P.
Saltonstall, Kristin
White, David A.
Hood, Craig S.
TI Genetic Variation in the Common Reed, Phragmites australis, in the
Mississippi River Delta Marshes: Evidence for Multiple Introductions
SO ESTUARIES AND COASTS
LA English
DT Article
DE Microsatellite; Haplotype; Invasive species; Genetic variation
ID MULTILOCUS GENOTYPE DATA; NORTH-AMERICA; CHESAPEAKE BAY; NONCODING
REGIONS; ISOZYME VARIATION; CHLOROPLAST DNA; TIDAL MARSHES; DIVERSITY;
POPULATIONS; INVASIONS
AB Multiple introductions are believed to play an important role in increasing genetic diversity and adaptability of invasive species, but there are few well-documented examples. The common reed, Phragmites australis, has dramatically increased in tidal wetlands throughout the USA in the past century due primarily to the introduction of a Eurasian lineage. In the Mississippi River "Balize" delta, P. australis is the dominant vegetation where monotypic stands of an introduced form blanket the outer marshes. The delta's interior marshes, on the other hand, are more vegetatively diverse, serving as important waterfowl foraging habitat. Recent encroachment by various phenotypic forms of P. australis into the interior marshes led to this study examining genetic variation in these stands. Our results revealed four chloroplast DNA haplotypes that also segregate based on microsatellite variation. Three of these are closely related and introduced, but differ relative to time and likely mode of introduction. The "Delta" type (haplotype M1), which is unique to the region and the most common lineage, displays considerable microsatellite diversity. The Eurasian introduced lineage of P. australis (haplotype M), which is invasive elsewhere in North America, is increasing its distribution in the delta. A novel haplotype, AD, was also identified which is phenotypically and genetically similar to haplotype M. Despite the close relatedness, we found no evidence for inter-haplotype gene exchange at the nuclear level, suggesting that intraspecific hybridization is not a contributing factor to these invasions. The site provides a unique opportunity for researchers to understand the dynamics of multiple P. australis invasions.
C1 [Hauber, Donald P.; White, David A.; Hood, Craig S.] Loyola Univ, Dept Biol Sci, New Orleans, LA 70118 USA.
[Saltonstall, Kristin] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama.
RP Hauber, DP (reprint author), Loyola Univ, Dept Biol Sci, New Orleans, LA 70118 USA.
EM hauber@loyno.edu
FU Loyola University; Leaves Committee; Faculty Development Grant; Rev.
J.H. Mullahy Fund; Coastal Restoration and Enhancement through Science
and Technology (CREST) program; Louisiana Board of Regents
[LEQSF(2007-12)-ENH-PKSFI-PES-03]
FX We wish to thank Dr. E. Bermingham for financial support (KS) and use of
his laboratory facilities (DH, KS); the U.S Fish & Wildlife Service for
access to the DNWR; Loyola University Grants & Leaves Committee Research
Grant (2006, 2007), Faculty Development Grant (2007) and Sabbatical
Leave (2008) (DH); Rev. J.H. Mullahy Fund (DH, DW, and CH); the Coastal
Restoration and Enhancement through Science and Technology (CREST)
program for financial support (DH, DW, and CH); the Louisiana Board of
Regents grant LEQSF(2007-12)-ENH-PKSFI-PES-03 to Frank Jordan and Loyola
University; Charlie Troxel and Carrie Owens for guidance on use of the
LI-COR 4300; Frank Jordan for collections; two anonymous reviewers and
Cori Richards-Zawacki, Michael Blum, and others from the SE Louisiana
EEB Journal Club for comments on early drafts; and J.A. Englert, Truc
Le, John Nguyen, and Hans Brix for technical assistance.
NR 65
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U1 2
U2 39
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 1559-2723
J9 ESTUAR COAST
JI Estuaries Coasts
PD JUL
PY 2011
VL 34
IS 4
BP 851
EP 862
DI 10.1007/s12237-011-9391-9
PG 12
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 772TO
UT WOS:000291259800017
ER
PT J
AU Kaspari, M
Powell, S
Lattke, J
O'Donnell, S
AF Kaspari, Michael
Powell, Scott
Lattke, John
O'Donnell, Sean
TI Predation and patchiness in the tropical litter: do swarm-raiding army
ants skim the cream or drain the bottle?
SO JOURNAL OF ANIMAL ECOLOGY
LA English
DT Article
DE brown food webs; density dependence; invertebrates; predation; prey
choice; tropical rainforest
ID SIZE-GRAIN HYPOTHESIS; COMMUNITY STRUCTURE; HYMENOPTERA; FORMICIDAE;
FOREST; RESOURCES; BIODIVERSITY; COMPETITION; PHYLOGENY; DYNAMICS
AB P>1. Swarm-raiding army ants have long been considered as episodic, catastrophic agents of disturbance in the tropical litter, but few quantitative data exist on their diets, preferences, and, critically, their ability to deplete prey.
2. Here, we provide such data for two common species of swarm raiders broadly sympatric throughout the Neotropics: the iconic Eciton burchellii and the more secretive, less studied Labidus praedator. In Ecuador, Costa Rica, Venezuela and Panama, patches of forest floor were sampled for litter invertebrates immediately before and after army ant raids. These invertebrates have been shown to regulate decomposition and vary 100-fold in local densities across the forest floor.
3. Contrary to Eciton's popular image, only Labidus consistently reduced the biomass of litter invertebrates and only then by an average of 25%. Eciton's impacts were concentrated on rich patches of invertebrates, while Labidus prey depletion showed no such density dependence. Labidus reduced the biomass of some invertebrates-isopods, larviforms and coleoptera-by up to 75%; Eciton showed no such prey preferences.
4. Our results suggest that Eciton specializes on high biomass patches, while Labidus feeds profitably from any litter patch. Combined, these swarm raiders sum to be chronic, but not catastrophic, predators of common litter invertebrates of the brown food web.
C1 [Kaspari, Michael] Univ Oklahoma, Dept Zool, EEB Grad Program, Norman, OK 73019 USA.
[Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama.
[Powell, Scott] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England.
[Lattke, John] Cent Univ Venezuela, Museo Inst Zool Agr, Maracay 2101A, Venezuela.
[O'Donnell, Sean] Univ Washington, Dept Psychol, Anim Behaviour Program, Seattle, WA 98195 USA.
RP Kaspari, M (reprint author), Univ Oklahoma, Dept Zool, EEB Grad Program, Norman, OK 73019 USA.
EM mkaspari@ou.edu
RI Lattke, John/K-2934-2015;
OI Lattke, John/0000-0002-6793-3003; Kaspari, Michael/0000-0002-9717-5768
FU National Science Foundation [DEB 0842038]; National Geographic Society;
Natural Environment Research Council, U.K. [NER/S/A/2001/05997]
FX This paper is dedicated to Carl Rettenmeyer, a colleague and mentor who
contributed greatly to our knowledge of army ant ecology. Special thanks
to Greg Crutsinger and Beatriz Baker for their work at La Selva and
Barro Colorado Island. Tom Valone greatly improved an earlier draft.
This project was funded by the National Science Foundation under grant
number DEB 0842038, and by the National Geographic Society, to M.
Kaspari. S. P. had additional support from a CASE Studentship from the
Natural Environment Research Council (NER/S/A/2001/05997), U.K., and the
CASE partner, the Smithsonian Tropical Research Institute, Panama.
NR 52
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U1 2
U2 34
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0021-8790
J9 J ANIM ECOL
JI J. Anim. Ecol.
PD JUL
PY 2011
VL 80
IS 4
BP 818
EP 823
DI 10.1111/j.1365-2656.2011.01826.x
PG 6
WC Ecology; Zoology
SC Environmental Sciences & Ecology; Zoology
GA 773LT
UT WOS:000291309500011
PM 21388371
ER
PT J
AU Wilson, S
Martin, K
AF Wilson, Scott
Martin, Kathy
TI Life-history and demographic variation in an alpine specialist at the
latitudinal extremes of the range
SO POPULATION ECOLOGY
LA English
DT Article
DE Lagopus leucura; Population growth; Reproductive ecology; Seasonality;
Survival; White-tailed ptarmigan
ID WHITE-TAILED PTARMIGAN; CLUTCH-SIZE VARIATION; EGG SIZE; WILLOW
PTARMIGAN; POPULATION-DYNAMICS; REPRODUCTIVE COSTS; BREEDING SUCCESS;
CHICK SURVIVAL; CLIMATE-CHANGE; NEST SURVIVAL
AB Alpine environments are unique systems to examine variation in life-history strategies because temperature and seasonality are similar across broad latitudinal gradients. We studied the life-history strategies, demography and population growth of white-tailed ptarmigan Lagopus leucura, an alpine specialist, at the latitudinal extremes of the range in the Yukon (YK, studied from 2004 to 2008) and Colorado (CO, 1987-1996). The two populations were separated by 2,400 km of latitude, and the Yukon site was approximately 2,000 m lower in elevation than the Colorado site. Yukon females bred on average 9 days earlier than those in Colorado, but the latter study was conducted 15 years earlier and breeding dates may have advanced over this period. The length of the breeding season was similar between the two populations, and females had comparable probabilities of re-nesting after failure. The two populations differed in how they allocated effort to the first clutch as Yukon females laid larger clutches (7.1 vs. 5.9 eggs) but smaller eggs (18.8 vs. 20.5 g) than those in Colorado. Demographic rates also differed; nest survival was higher in the Yukon (0.40) than in Colorado (0.24), and the resultant annual fecundity was nearly twice as high in the Yukon (3.92 vs. 1.77 chicks/female). In contrast, annual adult survival was higher in Colorado although the confidence intervals overlapped (females: YK = 0.35, CO = 0.44; males: YK = 0.48, CO = 0.59). Estimates of annual population growth (lambda) indicated both populations were declining, especially in Colorado (lambda (YK) = 0.83, lambda (CO) = 0.66), and thus, dispersal movements are likely key to long-term persistence in both cases. Our findings suggest that breeding-season temperature and seasonality affect measures related to timing of reproduction, but not the costs and benefits of clutch and egg size.
C1 [Wilson, Scott] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
[Martin, Kathy] Univ British Columbia, Dept Forest Sci, Vancouver, BC V6T 1Z4, Canada.
[Martin, Kathy] Environm Canada, Delta, BC V4K 3N2, Canada.
RP Wilson, S (reprint author), Canadian Wildlife Serv, 115 Perimeter Rd, Saskatoon, SK S7N 0X4, Canada.
EM scottd.wilson@ec.gc.ca
FU Natural Sciences and Engineering Research Council of Canada (NSERC);
Environment Canada; Northern Scientific Training Program; British
Columbia Upland Birds Society; Calgary Bird Banding Society; UBC
Department of Forestry; Izaak Walton Killam and University
FX We thank the many able field assistants who helped collect data in the
field during these two studies, including D. Chalmers, A. Clason, S.
Nouvet, G. Pelchat, A. Wilson and M. Wong for the Yukon study, and T.
Artiss, L. Robb, K. Wiebe and many undergraduates for the Colorado
study. We thank D. S. Hik, A. and S. Williams, and L. Goodwin for
providing logistical support at Pika Camp and the Arctic Institute of
North America at Kluane Lake, YK, Canada. C. E. Braun, Colorado Division
of Wildlife (Fort Collins, CO, USA) provided critical logistical
assistance for the duration of the Colorado study, and M. Mossop and L.
Robb provided able technical assistance. Funding for the research on
both sites was provided by Natural Sciences and Engineering Research
Council of Canada (NSERC; Discovery Grant, Northern Research Supplement,
International Polar Year) and Environment Canada support to KM, and
NSERC Postgraduate Scholarship, Northern Scientific Training Program,
British Columbia Upland Birds Society, Calgary Bird Banding Society, UBC
Department of Forestry, and Izaak Walton Killam and University Graduate
Fellowships to SW. We thank Cameron Aldridge and an anonymous reviewer
for helpful comments in revising this manuscript.
NR 72
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U1 2
U2 28
PU SPRINGER JAPAN KK
PI TOKYO
PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065,
JAPAN
SN 1438-3896
EI 1438-390X
J9 POPUL ECOL
JI Popul. Ecol.
PD JUL
PY 2011
VL 53
IS 3
BP 459
EP 471
DI 10.1007/s10144-011-0261-x
PG 13
WC Ecology
SC Environmental Sciences & Ecology
GA 774NL
UT WOS:000291393200005
ER
PT J
AU Kathilankal, JC
Mozdzer, TJ
Fuentes, JD
McGlathery, KJ
D'Odorico, P
Zieman, JC
AF Kathilankal, James C.
Mozdzer, Thomas J.
Fuentes, Jose D.
McGlathery, Karen J.
D'Odorico, Paolo
Zieman, Jay C.
TI Physiological responses of Spartina alterniflora to varying
environmental conditions in Virginia marshes
SO HYDROBIOLOGIA
LA English
DT Article
DE Salt marshes; Carbon cycling; Photosynthesis; Stomatal conductance;
Environmental change; Sea level rise; Atmospheric warming; Stable carbon
isotopes
ID WATER-VAPOR EXCHANGE; PHOTON FLUX-DENSITY; ENGLAND SALT-MARSH; STOMATAL
CONDUCTANCE; ELEVATED CO2; CHLOROPHYLL FLUORESCENCE; LEAF ANATOMY;
SEA-LEVEL; PHOSPHOENOLPYRUVATE CARBOXYLASE; CARBON ASSIMILATION
AB Physiological measurements were used to investigate the dependence of photosynthesis on light, temperature, and intercellular carbon dioxide (CO2) levels in the C-4 marsh grass Spartina alterniflora. Functional relationships between these environmental variables and S. alterniflora physiological responses were then used to improve C-4-leaf photosynthesis models. Field studies were conducted in monocultures of S. alterniflora in Virginia, USA. On average, S. alterniflora exhibited lower light saturation values (similar to 1000 mu mol m(-2) s(-1)) than observed in other C-4 plants. Maximum carbon assimilation rates and stomatal conductance to water vapor diffusion were 36 mu mol (CO2) m(-2) s(-1) and 200 mmol (H2O) m(-2) s(-1), respectively. Analysis of assimilation-intercellular CO2 and light response relationships were used to determine Arrhenius-type temperature functions for maximum rate of carboxylation (V (cmax)), phosphoenolpyruvate carboxylase activity (V (pmax)), and maximum electron transport rate (J (max)). Maximum V (cmax) values of 105 mu mol m(-2) s(-1) were observed at the leaf temperature of 311 K. Optimum V (pmax) values (80.6 mu mol m(-2) s(-1)) were observed at the foliage temperature of 308 K. The observed V (pmax) values were lower than those in other C-4 plants, whereas V (cmax) values were higher, and more representative of C-3 plants. Optimum J (max) values reached 138 mu mol (electrons) m(-2) s(-1) at the foliage temperature of 305 K. In addition, the estimated CO2 compensation points were in the range of C-3 or C-3-C-4 intermediate plants, not those typical of C-4 plants. The present results indicate the possibility of a C-3-C-4 intermediate or C-4-like photosynthetic mechanism rather than the expected C-4-biochemical pathway in S. alterniflora under field conditions. In a scenario of atmospheric warming and increased atmospheric CO2 concentrations, S. alterniflora will likely respond positively to both changes. Such responses will result in increased S. alterniflora productivity, which is uncharacteristic of C-4 plants.
C1 [Fuentes, Jose D.] Penn State Univ, Dept Meteorol, University Pk, PA 16802 USA.
[Kathilankal, James C.] Li Cor Inc, Biosci Div, Lincoln, NE USA.
[Mozdzer, Thomas J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[McGlathery, Karen J.; D'Odorico, Paolo; Zieman, Jay C.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA.
RP Fuentes, JD (reprint author), Penn State Univ, Dept Meteorol, 503 Walker Bldg, University Pk, PA 16802 USA.
EM jdfuentes@psu.edu
RI Mozdzer, Thomas/G-4372-2011; D'Odorico, Paolo/A-5836-2008; Mozdzer,
Thomas/A-3599-2014
OI Mozdzer, Thomas/0000-0002-1053-0967
FU U.S. National Science Foundation [DEB-0621014]
FX The U.S. National Science Foundation provided support to carry out this
research as part of the VCR LTER research activities (grant number
DEB-0621014). Two reviewers provided excellent comments to improve the
manuscript.
NR 82
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U1 0
U2 29
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0018-8158
J9 HYDROBIOLOGIA
JI Hydrobiologia
PD JUL
PY 2011
VL 669
IS 1
BP 167
EP 181
DI 10.1007/s10750-011-0681-9
PG 15
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 765BO
UT WOS:000290678600012
ER
PT J
AU Peterson, PM
Giraldo-Canas, D
AF Peterson, Paul M.
Giraldo-Canas, Diego
TI The species of Muhlenbergia (Poaceae: Chloridoideae) from Argentina
SO CALDASIA
LA Spanish
DT Article
DE Muhlenbergia; Chloridoideae; Poaceae; Neotropical grasses; Flora of
Argentina
ID CYNODONTEAE MUHLENBERGIINAE; CLASSIFICATION; ANATOMY; GENUS
AB A taxonomic study of the Argentinian native species of the genus Muhlenbergia is presented, based on the study of specimens deposited in 48 herbaria. Different aspects related to the classification, nomenclature, and morphological variations are discussed. Muhlenbergia is represented in Argentina by 18 native species; identification keys, descriptions, synonyms, illustrations, geographical distribution, and some morphological and ecological observations are also provided. Muhlenbergia breviaristata (Hack.) Parodi and Muhlenbergia holwayorum Hitchc. are reduced as synonym of the hybrid Muhlenbergia angustata (J. Presp Kunth x M rigida (Kunth) Kunth. Muhlenbergia diversiglumis Trin. is recorded for the first time for Argentina. Muhlenbergia tenella (Kunth) Trin. and Muhlenbergia tenuissima (J. Presl) Kunth are excluded from the Argentinian Flora.
C1 [Peterson, Paul M.] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Giraldo-Canas, Diego] Univ Nacl Colombia, Fac Ciencias, Inst Ciencias Nat, Bogota, Colombia.
RP Peterson, PM (reprint author), Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA.
EM peterson@si.edu; dagiraldoc@unal.edu.co
NR 17
TC 0
Z9 2
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 2011
VL 33
IS 1
BP 21
EP 54
PG 34
WC Plant Sciences; Multidisciplinary Sciences; Zoology
SC Plant Sciences; Science & Technology - Other Topics; Zoology
GA 824JJ
UT WOS:000295197900002
ER
PT J
AU Cooper, M
Martin, RV
Sauvage, B
Boone, CD
Walker, KA
Bernath, PF
McLinden, CA
Degenstein, DA
Volz-Thomas, A
Wespes, C
AF Cooper, Matthew
Martin, Randall V.
Sauvage, Bastien
Boone, Chris D.
Walker, Kaley A.
Bernath, Peter F.
McLinden, Chris A.
Degenstein, Doug A.
Volz-Thomas, Andreas
Wespes, Catherine
TI Evaluation of ACE-FTS and OSIRIS Satellite retrievals of ozone and
nitric acid in the tropical upper troposphere: Application to ozone
production efficiency
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
ID CHEMISTRY EXPERIMENT ACE; MOZAIC AIRBORNE PROGRAM; PACIFIC EXPLORATORY
MISSION; IN-SERVICE AIRCRAFT; STRATOSPHERIC OZONE; GLOBAL-MODEL;
PEM-TROPICS; DISTRIBUTIONS; NOY; CLIMATOLOGY
AB We evaluate climatologies of upper tropospheric ozone and nitric acid retrieved from two satellite instruments (ACE-FTS and OSIRIS) with long-term in situ measurements from aircraft (MOZAIC, CR-AVE, PRE-AVE, PEM Tropics, and TC4) and ozonesondes. A global chemical transport model (GEOS-Chem) is used to guide the evaluation and to relate sparse in situ measurements with the satellite retrievals. Both satellite retrievals generally reproduce broad ozone features in the upper troposphere such as summer enhancements in the northern subtropics and larger concentrations over the tropical Atlantic versus the tropical Pacific. These comparisons indicate biases in annual, tropical mean ozone concentrations from both ACE-FTS (10-13%) and OSIRIS (5%) relative to aircraft and ozonesonde observations. More uncertain evidence suggests that nitric acid from ACE-FTS has a positive mean bias of 15%. We demonstrate that an upper limit on the ozone production efficiency in the upper troposphere can be determined using ACE-FTS satellite measurements of O-3 and HNO3. The resulting value of 196 (+34, -61) mol/mol is in broad agreement with model simulations. Higher OPE values inferred from ACE-FTS over the tropical Pacific (249 (+21, -68) mol/mol) than the tropical Atlantic (146 (+16, -41) mol/mol) reflect increasing ozone production efficiency with decreasing pollution. This analysis indicates a new capability of satellite observations to provide insight into ozone production in the tropical troposphere.
C1 [Cooper, Matthew; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
[Boone, Chris D.; Walker, Kaley A.; Bernath, Peter F.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada.
[Degenstein, Doug A.] Univ Saskatchewan, Inst Space & Atmospher Sci, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada.
[Sauvage, Bastien] Univ Toulouse 3, CNRS, Lab Aerol, F-31062 Toulouse, France.
[McLinden, Chris A.] Environm Canada, Toronto, ON M2H 5T4, Canada.
[Volz-Thomas, Andreas] Forschungszentrum Julich, Inst Energie & Klimaforsch Troposphare 8, DE-52425 Julich, Germany.
[Wespes, Catherine] Univ Libre Bruxelles, B-1050 Brussels, Belgium.
[Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada.
[Bernath, Peter F.] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England.
RP Cooper, M (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada.
EM cooperm2@dal.ca
RI Bernath, Peter/B-6567-2012; Volz-Thomas, Andreas/J-7223-2012; Martin,
Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Bernath, Peter/0000-0002-1255-396X; Volz-Thomas,
Andreas/0000-0003-3700-1667; Martin, Randall/0000-0003-2632-8402;
FU Canadian Foundation for Climate and Atmospheric Science (CFCAS);
Canadian Space Agency (CSA); Natural Sciences and Engineering Research
Council of Canada (NSERC); UK Natural Environment Research Council
(NERC); INSU-CNRS (France), Meteo-France; Forschungszentrum (FZJ,
Julich, Germany)
FX This research was supported by the Canadian Foundation for Climate and
Atmospheric Science (CFCAS) and by the Canadian Space Agency (CSA). The
ACE mission is funded primarily by the CSA and the Natural Sciences and
Engineering Research Council of Canada (NSERC). Some funding was also
provided by the UK Natural Environment Research Council (NERC). The
authors acknowledge the strong support of the European Commission,
Airbus, and the airlines (Lufthansa, Austrian, Air France) who have
carried the MOZAIC equipment and performed maintenance free of charge
since 1994. MOZAIC is presently funded by INSU-CNRS (France),
Meteo-France, and Forschungszentrum (FZJ, Julich, Germany). The MOZAIC
database is supported by ETHER (CNES and INSU-CNRS). Ozonesonde data
available from WOUDC are provided by the India Meteorological Department
(IMD), Japan Meteorological Agency (JMA), Hong Kong Observatory (HKO),
University of Alabama at Huntsville (UAH), and the National Institute of
Meteorology of Spain-Izana Observatory (INME-IZO).
NR 64
TC 11
Z9 11
U1 1
U2 22
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD JUN 29
PY 2011
VL 116
AR D12306
DI 10.1029/2010JD015056
PG 12
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 787MK
UT WOS:000292380500001
ER
PT J
AU Cardoso, P
Pekar, S
Jocque, R
Coddington, JA
AF Cardoso, Pedro
Pekar, Stano
Jocque, Rudy
Coddington, Jonathan A.
TI Global Patterns of Guild Composition and Functional Diversity of Spiders
SO PLOS ONE
LA English
DT Article
ID SPECIES RICHNESS; ECOLOGICAL COMMUNITIES; BIODIVERSITY; ARANEAE; FOREST;
DISTURBANCE; ECOSYSTEMS; VEGETATION; GRADIENTS
AB The objectives of this work are: (1) to define spider guilds for all extant families worldwide; (2) test if guilds defined at family level are good surrogates of species guilds; (3) compare the taxonomic and guild composition of spider assemblages from different parts of the world; (4) compare the taxonomic and functional diversity of spider assemblages and; (5) relate functional diversity with habitat structure. Data on foraging strategy, prey range, vertical stratification and circadian activity was collected for 108 families. Spider guilds were defined by hierarchical clustering. We searched for inconsistencies between family guild placement and the known guild of each species. Richness and abundance per guild before and after correcting guild placement were compared, as were the proportions of each guild and family between all possible pairs of sites. Functional diversity per site was calculated based on hierarchical clustering. Eight guilds were discriminated: (1) sensing, (2) sheet, (3) space, and (4) orb web weavers; (5) specialists; (6) ambush, (7) ground, and (8) other hunters. Sixteen percent of the species richness corresponding to 11% of all captured individuals was incorrectly attributed to a guild by family surrogacy; however, the correlation of uncorrected vs. corrected guilds was invariably high. The correlation of guild richness or abundances was generally higher than the correlation of family richness or abundances. Functional diversity was not always higher in the tropics than in temperate regions. Families may potentially serve as ecological surrogates for species. Different families may present similar roles in the ecosystems, with replacement of some taxa by other within the same guild. Spiders in tropical regions seem to have higher redundancy of functional roles and/or finer resource partitioning than in temperate regions. Although species and family diversity were higher in the tropics, functional diversity seems to be also influenced by altitude and habitat structure.
C1 [Cardoso, Pedro; Coddington, Jonathan A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Cardoso, Pedro] Univ Acores, Azorean Biodivers Grp, CITA A, Angra Do Heroismo, Portugal.
[Pekar, Stano] Masaryk Univ, Fac Sci, Dept Bot & Zool, CS-61137 Brno, Czech Republic.
[Jocque, Rudy] Musee Royal Afr Cent, Tervuren, Belgium.
RP Cardoso, P (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM pcardoso@ennor.org
RI Cardoso, Pedro/A-8820-2008;
OI Cardoso, Pedro/0000-0001-8119-9960; Pekar, Stano/0000-0002-0197-5040
FU Fundacao para a Ciencia e Tecnologia [SFRH/BPD/40688/2007]; Ministry of
Education, Youth and Sports of the Czech Republic [0021622416];
Smithsonian Institution; Carlsberg Foundation; NSF [EAR-0228699,
DEB-9707744, DEB-9712353]
FX PC was supported by Fundacao para a Ciencia e Tecnologia
(SFRH/BPD/40688/2007). SP was supported by project no. 0021622416 of the
Ministry of Education, Youth and Sports of the Czech Republic. JAC was
supported by various grants from the Neotropical Lowlands, Biodiversity
of the Guianas, and Scholarly Studies Programs of the Smithsonian
Institution, the Carlsberg Foundation, and NSF grants EAR-0228699,
DEB-9707744, and DEB-9712353. The funders had no role in study design,
data collection and analysis, decision to publish, or preparation of the
manuscript.
NR 57
TC 62
Z9 69
U1 5
U2 76
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 JUN 29
PY 2011
VL 6
IS 6
AR e21710
DI 10.1371/journal.pone.0021710
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 786FZ
UT WOS:000292290100058
PM 21738772
ER
PT J
AU Indriati, E
Swisher, CC
Lepre, C
Quinn, RL
Suriyanto, RA
Hascaryo, AT
Grun, R
Feibel, CS
Pobiner, BL
Aubert, M
Lees, W
Anton, SC
AF Indriati, Etty
Swisher, Carl C., III
Lepre, Christopher
Quinn, Rhonda L.
Suriyanto, Rusyad A.
Hascaryo, Agus T.
Gruen, Rainer
Feibel, Craig S.
Pobiner, Briana L.
Aubert, Maxime
Lees, Wendy
Anton, Susan C.
TI The Age of the 20 Meter Solo River Terrace, Java, Indonesia and the
Survival of Homo erectus in Asia
SO PLOS ONE
LA English
DT Article
ID ELECTRON-SPIN-RESONANCE; TOOTH ENAMEL; COSMIC-RAY; U-UPTAKE; NGANDONG;
GEOCHRONOLOGY; PLEISTOCENE; AFFINITIES; HOMININ; SAPIENS
AB Homo erectus was the first human lineage to disperse widely throughout the Old World, the only hominin in Asia through much of the Pleistocene, and was likely ancestral to H. sapiens. The demise of this taxon remains obscure because of uncertainties regarding the geological age of its youngest populations. In 1996, some of us co-published electron spin resonance (ESR) and uranium series (U-series) results indicating an age as young as 35-50 ka for the late H. erectus sites of Ngandong and Sambungmacan and the faunal site of Jigar (Indonesia). If correct, these ages favor an African origin for recent humans who would overlap with H. erectus in time and space. Here, we report (40)Ar/(39)Ar incremental heating analyses and new ESR/U-series age estimates from the "20 m terrace'' at Ngandong and Jigar. Both data sets are internally consistent and provide no evidence for reworking, yet they are inconsistent with one another. The (40)Ar/(39)Ar analyses give an average age of 546 +/- 12 ka (sd +/- 5 se) for both sites, the first reliable radiometric indications of a middle Pleistocene component for the terrace. Given the technical accuracy and consistency of the analyses, the argon ages represent either the actual age or the maximum age for the terrace and are significantly older than previous estimates. Most of the ESR/U-series results are older as well, but the oldest that meets all modeling criteria is 143 ka+20/-17. Most samples indicated leaching of uranium and likely represent either the actual or the minimum age of the terrace. Given known sources of error, the U-series results could be consistent with a middle Pleistocene age. However, the ESR and (40)Ar/(39)Ar ages preclude one another. Regardless, the age of the sites and hominins is at least bracketed between these estimates and is older than currently accepted.
C1 [Indriati, Etty; Suriyanto, Rusyad A.; Hascaryo, Agus T.] Gadjah Mada Univ, Fac Med, Lab Bio & Paleoanthropol, Yogyakarta, Indonesia.
[Swisher, Carl C., III; Lepre, Christopher; Quinn, Rhonda L.; Feibel, Craig S.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ USA.
[Lepre, Christopher] Columbia Univ, Lamont Doherty Earth Observ Palisades, New York, NY USA.
[Quinn, Rhonda L.] Loyola Univ Chicago, Dept Anthropol, Chicago, IL USA.
[Gruen, Rainer; Aubert, Maxime; Lees, Wendy] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia.
[Pobiner, Briana L.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
[Anton, Susan C.] NYU, Dept Anthropol, Ctr Study Human Origins, New York, NY 10003 USA.
RP Indriati, E (reprint author), Gadjah Mada Univ, Fac Med, Lab Bio & Paleoanthropol, Yogyakarta, Indonesia.
EM cswish@rci.rutgers.edu; susan.anton@nyu.edu
RI Grun, Rainer/A-1437-2012
OI Grun, Rainer/0000-0003-1366-3674
FU U.S. NSF [BCS 0317292]; AAAS WISC program; UGM
FX The project was funded by the U.S. NSF BCS 0317292 to SCA, an AAAS WISC
program grant to EI and SCA, and a UGM sabbatical grant to EI. The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 51
TC 28
Z9 30
U1 0
U2 23
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUN 29
PY 2011
VL 6
IS 6
AR e21562
DI 10.1371/journal.pone.0021562
PG 10
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 786FZ
UT WOS:000292290100039
PM 21738710
ER
PT J
AU Lovelock, CE
Ruess, RW
Feller, IC
AF Lovelock, Catherine E.
Ruess, Roger W.
Feller, Ilka C.
TI CO2 Efflux from Cleared Mangrove Peat
SO PLOS ONE
LA English
DT Article
ID SHRIMP PONDS; LAND-USE; FORESTS; SEQUESTRATION; RESPIRATION; SEDIMENTS;
COLLAPSE; FUTURE
AB Background: CO2 emissions from cleared mangrove areas may be substantial, increasing the costs of continued losses of these ecosystems, particularly in mangroves that have highly organic soils.
Methodology/Principal Findings: We measured CO2 efflux from mangrove soils that had been cleared for up to 20 years on the islands of Twin Cays, Belize. We also disturbed these cleared peat soils to assess what disturbance of soils after clearing may have on CO2 efflux. CO2 efflux from soils declines from time of clearing from similar to 10 600 tonnes km 22 year 21 in the first year to 3000 tonnes km(2) year(-1) after 20 years since clearing. Disturbing peat leads to short term increases in CO2 efflux (27 umol m(-2)s(-1)), but this had returned to baseline levels within 2 days.
Conclusions/Significance: Deforesting mangroves that grow on peat soils results in CO2 emissions that are comparable to rates estimated for peat collapse in other tropical ecosystems. Preventing deforestation presents an opportunity for countries to benefit from carbon payments for preservation of threatened carbon stocks.
C1 [Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld, Australia.
[Ruess, Roger W.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK USA.
[Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Lovelock, CE (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld, Australia.
EM c.lovelock@uq.edu.au
RI Lovelock, Catherine/G-7370-2012
OI Lovelock, Catherine/0000-0002-2219-6855
FU Smithsonian Marine Science Network; National Science Foundation
[DEB-9981535]
FX This work was supported by the Smithsonian Marine Science Network and a
National Science Foundation Biocomplexity award (DEB-9981535). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 34
TC 35
Z9 37
U1 6
U2 66
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 JUN 29
PY 2011
VL 6
IS 6
AR e21279
DI 10.1371/journal.pone.0021279
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 786FZ
UT WOS:000292290100016
PM 21738628
ER
PT J
AU Loeuille, B
Robinson, H
Semir, J
AF Loeuille, Benoit
Robinson, Harold
Semir, Joao
TI Minasia ramosa (Asteraceae: Vernonieae), a new species from the Serra do
Cabral, Minas Gerais, Brazil
SO PHYTOTAXA
LA English
DT Article
DE Lychnophorinae; Espinhaco Range; Compositae; campos rupestres
AB Minasia ramosa, a new species from Brazil, is here described and illustrated. The species is endemic to the campos rupestres of the Serra do Cabral, a western extension of the Espinhaco Range in Minas Gerais. Minasia ramosa is characterized by its narrow ensiform leaves, paniculate inflorescence and totally setuliferous cypselae. The affinities of this species are discussed.
C1 [Loeuille, Benoit] Univ Sao Paulo, Inst Biociencias, Dept Bot, BR-05508090 Sao Paulo, Brazil.
[Robinson, Harold] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA.
[Semir, Joao] Univ Estadual Campinas, Dept Bot, Inst Biol, Campinas, SP, Brazil.
RP Loeuille, B (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Bot, Rua Matao 277, BR-05508090 Sao Paulo, Brazil.
EM benoit_loeuille@yahoo.fr; robinsoh@si.edu
FU CNPq (Brazil); Cuatrecasas Travel Award Committee
FX Thanks are due to Leonardo M. Borges for the line illustrations, to CNPq
(Brazil) and the Cuatrecasas Travel Award Committee for the fellowships
awarded to first author. The authors would like to thank the curators of
all the herbaria listed in the text for loaning the specimens, D.J.N.
Hind, M. Dematteis and an anonymous reviewer are thanked for their
comments on the manuscript.
NR 11
TC 1
Z9 1
U1 3
U2 7
PU MAGNOLIA PRESS
PI AUCKLAND
PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND
SN 1179-3155
J9 PHYTOTAXA
JI Phytotaxa
PD JUN 28
PY 2011
VL 25
BP 18
EP 22
PG 5
WC Plant Sciences
SC Plant Sciences
GA 814FJ
UT WOS:000294432900002
ER
PT J
AU Parenti, LR
Hartel, KE
AF Parenti, Lynne R.
Hartel, Karsten E.
TI Osteology Identifies Fundulus capensis Garman, 1895 as a Killifish in
the Family Fundulidae (Atherinomorpha: Cyprinodontiformes)
SO COPEIA
LA English
DT Article
ID TELEOSTEI; CARTILAGE; FISHES
AB Fundulus capensis Garman, 1895 was described from the unique holotype said to be from False Bay, Cape of Good Hope, South Africa. Largely ignored by killifish taxonomists, its classification has remained ambiguous for over a century. Radiography and computed tomography of the holotype reveal skeletal details that have been used in modern phylogenetic hypotheses of cyprinodontiform lineages. Osteological synapomorphies confirm it is a cyprinodontiform killifish and allow us to identify it to species. The first pleural rib on the second vertebra and a symmetrical caudal fin with hypural elements fused into a fan-shaped hypural plate corroborate its classification in the cyprinodontiform suborder Cyprinodontoidel. The twisted maxilla with an anterior hook and the premaxilla with an elongate ascending process both place it in the family Fundulidae. The pointed neurapophyses of the first vertebra that do not meet in the midline and do not form a spine exclude it from the family Poeciliidae. Presence of discrete exoccipital condyles excludes it from the subfamily Poeciliinae. Overall shape, position of fins, and meristic data agree well with those of the well-known North American killifish, F. heteroclitus. Fundulus capensis Garman, 1895, redescribed herein, is considered a subjective synonym of Fundulus heteroclitus (Linnaeus, 1766). Provenance of the specimen remains a mystery.
C1 [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
[Hartel, Karsten E.] Harvard Univ, Museum Comparat Zool, Dept Ichthyol, Cambridge, MA 02138 USA.
RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,NHB MRC 159, Washington, DC 20013 USA.
EM parentil@si.edu; hartel@oeb.harvard.edu
FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the
Division of Fishes (USNM)
FX K. Lazara informed us that F. capensis had been considered by R.
Griffith in his dissertation and also that it was listed in early
editions of the Killifish Master Index. S. Raredon (USNM) prepared the
radiographs. J. Mounts (USNM) aided with figure preparation. A.
Williston (MCZ) prepared the CT micrographs and photographed the
holotype (Fig 1); the original photography is President and Fellows of
Harvard College. B. Collette (National Marine Fisheries Service) read
and provided helpful comments on a draft of the manuscript. K. Cole
(University of Hawaii) kindly identified the False Bay gobiid and T.
Munroe (National Marine Fisheries Service) provided detailed comments on
the identification of the False Bay flatfish. Preparation and
publication of the manuscript was supported by the Herbert R. and Evelyn
Axelrod Chair in Systematic Ichthyology in the Division of Fishes
(USNM).
NR 31
TC 1
Z9 1
U1 1
U2 4
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 28
PY 2011
IS 2
BP 242
EP 250
DI 10.1643/CI-10-146
PG 9
WC Zoology
SC Zoology
GA 790JJ
UT WOS:000292584000006
ER
PT J
AU Hilton, EJ
Johnson, GD
Houde, ED
Latour, RJ
AF Hilton, Eric J.
Johnson, G. David
Houde, Edward D.
Latour, Robert J.
TI John Edward Olney, Sr. (1947-2010) OBITUARY
SO COPEIA
LA English
DT Biographical-Item
C1 [Hilton, Eric J.; Latour, Robert J.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
[Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Zool, Washington, DC 20013 USA.
[Houde, Edward D.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA.
RP Hilton, EJ (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA.
EM ehilton@vims.edu; johnsond@si.edu; ehoude@umces.edu; latour@vims.edu
RI Houde, Edward/D-8498-2012
NR 1
TC 0
Z9 0
U1 0
U2 2
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 28
PY 2011
IS 2
BP 332
EP 341
DI 10.1643/OT-11-004
PG 10
WC Zoology
SC Zoology
GA 790JJ
UT WOS:000292584000018
ER
PT J
AU Kawahara, AY
Ohshima, I
Kawakita, A
Regier, JC
Mitter, C
Cummings, MP
Davis, DR
Wagner, DL
De Prins, J
Lopez-Vaamonde, C
AF Kawahara, Akito Y.
Ohshima, Issei
Kawakita, Atsushi
Regier, Jerome C.
Mitter, Charles
Cummings, Michael P.
Davis, Donald R.
Wagner, David L.
De Prins, Jurate
Lopez-Vaamonde, Carlos
TI Increased gene sampling strengthens support for higher-level groups
within leaf-mining moths and relatives (Lepidoptera: Gracillariidae)
SO BMC EVOLUTIONARY BIOLOGY
LA English
DT Article
ID OBLIGATE POLLINATION MUTUALISM; PHYLOGENETIC TREE SELECTION;
MAXIMUM-LIKELIHOOD; EVOLUTIONARY TREES; NUCLEAR GENE; COMPOSITIONAL
HETEROGENEITY; MOLECULAR PHYLOGENIES; SEQUENCE EVOLUTION; EPICEPHALA
MOTHS; GLOCHIDION TREES
AB Background: Researchers conducting molecular phylogenetic studies are frequently faced with the decision of what to do when weak branch support is obtained for key nodes of importance. As one solution, the researcher may choose to sequence additional orthologous genes of appropriate evolutionary rate for the taxa in the study. However, generating large, complete data matrices can become increasingly difficult as the number of characters increases. A few empirical studies have shown that augmenting genes even for a subset of taxa can improve branch support. However, because each study differs in the number of characters and taxa, there is still a need for additional studies that examine whether incomplete sampling designs are likely to aid at increasing deep node resolution. We target Gracillariidae, a Cretaceous-age (similar to 100 Ma) group of leaf-mining moths to test whether the strategy of adding genes for a subset of taxa can improve branch support for deep nodes. We initially sequenced ten genes (8,418 bp) for 57 taxa that represent the major lineages of Gracillariidae plus outgroups. After finding that many deep divergences remained weakly supported, we sequenced eleven additional genes (6,375 bp) for a 27-taxon subset. We then compared results from different data sets to assess whether one sampling design can be favored over another. The concatenated data set comprising all genes and all taxa and three other data sets of different taxon and gene sub-sampling design were analyzed with maximum likelihood. Each data set was subject to five different models and partitioning schemes of non-synonymous and synonymous changes. Statistical significance of non-monophyly was examined with the Approximately Unbiased (AU) test.
Results: Partial augmentation of genes led to high support for deep divergences, especially when non-synonymous changes were analyzed alone. Increasing the number of taxa without an increase in number of characters led to lower bootstrap support; increasing the number of characters without increasing the number of taxa generally increased bootstrap support. More than three-quarters of nodes were supported with bootstrap values greater than 80% when all taxa and genes were combined. Gracillariidae, Lithocolletinae + Leucanthiza, and Acrocercops and Parectopa groups were strongly supported in nearly every analysis. Gracillaria group was well supported in some analyses, but less so in others. We find strong evidence for the exclusion of Douglasiidae from Gracillarioidea sensu Davis and Robinson (1998). Our results strongly support the monophyly of a G.B.R.Y. clade, a group comprised of Gracillariidae + Bucculatricidae + Roeslerstammiidae + Yponomeutidae, when analyzed with non-synonymous changes only, but this group was frequently split when synonymous and non-synonymous substitutions were analyzed together.
Conclusions: 1) Partially or fully augmenting a data set with more characters increased bootstrap support for particular deep nodes, and this increase was dramatic when non-synonymous changes were analyzed alone. Thus, the addition of sites that have low levels of saturation and compositional heterogeneity can greatly improve results. 2) Gracillarioidea, as defined by Davis and Robinson (1998), clearly do not include Douglasiidae, and changes to current classification will be required. 3) Gracillariidae were monophyletic in all analyses conducted, and nearly all species can be placed into one of six strongly supported clades though relationships among these remain unclear. 4) The difficulty in determining the phylogenetic placement of Bucculatricidae is probably attributable to compositional heterogeneity at the third codon position. From our tests for compositional heterogeneity and strong bootstrap values obtained when synonymous changes are excluded, we tentatively conclude that Bucculatricidae is closely related to Gracillariidae + Roeslerstammiidae + Yponomeutidae.
C1 [Kawahara, Akito Y.; Mitter, Charles] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Ohshima, Issei] Natl Inst Basic Biol, Div Evolutionary Biol, Okazaki, Aichi 444, Japan.
[Kawakita, Atsushi] Kyoto Univ, Ctr Ecol Res, Kyoto, Japan.
[Regier, Jerome C.] Univ Maryland, Inst Biosci & Biotechnol Res, College Pk, MD 20742 USA.
[Cummings, Michael P.] Univ Maryland, Lab Mol Evolut, Ctr Bioinformat & Computat Biol, College Pk, MD 20742 USA.
[Davis, Donald R.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA.
[Wagner, David L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT 06269 USA.
[De Prins, Jurate] Royal Museum Cent Afr, Tervuren, Belgium.
[Lopez-Vaamonde, Carlos] INRA, Zool Forestiere UR0633, F-45000 Orleans, France.
RP Kawahara, AY (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
EM kawahara@flmnh.ufl.edu
RI Lopez-Vaamonde, Carlos/A-5548-2009
OI Lopez-Vaamonde, Carlos/0000-0003-2278-2368
FU Federal Scientific Institutions [MO/37/022]; Japan Society for the
Promotion of Science (JSPS) [20-5555, 20870021]
FX We thank Andreas Zwick (State Museum of Natural History, Stuttgart) for
continuous support, critical comments and advice, and Tosio Kumata
(Hokkaido University) for many insights into the systematics of
Gracillariidae. Zaile Du and Anamika Verma assisted with sequencing.
Adam Bazinet (University of Maryland) was instrumental in helping access
and utilize The Lattice Grid. Joaquin Baixeras (University of Valencia),
Soowon Cho (Chungbuk National University), Terry Harrison (University of
Illinois), Kenji Nishida (University of Costa Rica), Jae-Cheon Sohn
(University of Maryland), and Kazuhiro Sugisima (Okayama City, Japan)
provided some important taxa used in this study. We also thank Rodolphe
Rougerie (Canadian Centre for DNA Barcoding) for sending valuable
extracts, and Kim Mitter (University of Maryland) for assisting with the
preparation of samples. Jean-Francois Landry (Canadian National
Collection) helped clarify taxonomic inconsistencies related to some
taxa in the study. Julie Byrd (University of Maryland) and two anonymous
reviewers provided comments that improved the quality Federal Scientific
Institutions, project number MO/37/022; The Research Fellowships of the
Japan Society for the Promotion of Science (JSPS) for Young Scientists
(award 20-5555); and a Grant-in Aid from JSPS (20870021).
NR 90
TC 35
Z9 37
U1 1
U2 18
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 24
PY 2011
VL 11
AR 182
DI 10.1186/1471-2148-11-182
PG 14
WC Evolutionary Biology; Genetics & Heredity
SC Evolutionary Biology; Genetics & Heredity
GA 798PB
UT WOS:000293221600001
PM 21702958
ER
PT J
AU Graves, GR
Prys-Jones, RP
AF Graves, Gary R.
Prys-Jones, Robert P.
TI Rediscovery of the holotype of Trochilus maria Gosse, 1849 (Aves:
Apodiformes: Trochilidae)
SO ZOOTAXA
LA English
DT Letter
C1 [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA.
[Prys-Jones, Robert P.] Nat Hist Museum, Dept Zool, Bird Grp, Tring HP23 6AP, Herts, England.
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; R.Prys-Jones@nhm.ac.uk
NR 19
TC 1
Z9 1
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 JUN 24
PY 2011
IS 2929
BP 59
EP 63
PG 5
WC Zoology
SC Zoology
GA 783NJ
UT WOS:000292090100006
ER
PT J
AU Neill, JL
Steber, AL
Muckle, MT
Zaleski, DP
Lattanzi, V
Spezzano, S
McCarthy, MC
Remijan, AJ
Friedel, DN
Weaver, SLW
Pate, BH
AF Neill, Justin L.
Steber, Amanda L.
Muckle, Matt T.
Zaleski, Daniel P.
Lattanzi, Valerio
Spezzano, Silvia
McCarthy, Michael C.
Remijan, Anthony J.
Friedel, Douglas N.
Weaver, Susanna L. Widicus
Pate, Brooks H.
TI Spatial Distributions and Interstellar Reaction Processes
SO JOURNAL OF PHYSICAL CHEMISTRY A
LA English
DT Article
ID ION-MOLECULE REACTIONS; PRESSURE ASSOCIATION REACTIONS; PROTON-TRANSFER
REACTIONS; STAR-FORMING REGIONS; ORION KLEINMANN-LOW; GAS-PHASE; METHYL
FORMATE; DISSOCIATIVE RECOMBINATION; DIMETHYL ETHER; AB-INITIO
AB Methyl formate presents a challenge for the conventional chemical mechanisms assumed to guide interstellar organic chemistry. Previous studies of potential formation pathways for methyl formate in interstellar clouds ruled out gas-phase chemistry as a major production route, and more recent chemical kinetics models indicate that it may form efficiently from radical-radical chemistry on ice surfaces. Yet, recent chemical imaging studies of methyl formate and molecules potentially related to its formation suggest that it may form through previously unexplored gas-phase chemistry. Motivated by these findings, two new gas-phase ion-molecule formation routes are proposed and characterized using electronic structure theory with conformational specificity. The proposed reactions, acid-catalyzed Fisher esterification and methyl cation transfer, both produce the less stable trans-conformational isomer of protonated methyl formate in relatively high abundance under the kinetically controlled conditions relevant to interstellar chemistry. Gas-phase neutral methyl formate can be produced from its protonated counterpart through either a dissociative electron recombination reaction or a proton transfer reaction to a molecule with larger proton affinity. Retention (or partial retention) of the conformation in these neutralization reactions would yield trans-methyl formate in an abundance that exceeds predictions under thermodynamic equilibrium at typical interstellar temperatures of <= 100 K. For this reason, this conformer may prove to be an excellent probe of gas-phase chemistry in interstellar clouds. Motivated by new theoretical predictions, the rotational spectrum of trans-methyl formate has been measured for the first time in the laboratory, and seven lines have now been detected in the interstellar medium using the publicly available PRIMOS survey from the NRAO Green Bank Telescope.
C1 [Neill, Justin L.; Steber, Amanda L.; Muckle, Matt T.; Zaleski, Daniel P.; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA.
[Lattanzi, Valerio; Spezzano, Silvia; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Lattanzi, Valerio; Spezzano, Silvia; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.
[Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
[Friedel, Douglas N.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
[Weaver, Susanna L. Widicus] Emory Univ, Dept Chem, Atlanta, GA 30322 USA.
RP Pate, BH (reprint author), Univ Virginia, Dept Chem, McCormick Rd,POB 400319, Charlottesville, VA 22904 USA.
EM brookspate@virginia.edu
OI McCarthy, Michael/0000-0001-9142-0008; Zaleski,
Daniel/0000-0003-0153-9158; Steber, Amanda/0000-0002-8203-2174
FU NSF Centers for Chemical Innovation [CHE-0847919]; National Science
Foundation
FX The authors acknowledge support from the NSF Centers for Chemical
Innovation (CHE-0847919). The authors also thank Eric Herbst for
fruitful discussions regarding organic reactions in interstellar
chemistry and Kevin Lehmann for assistance with the temperature
determination in the Orion Compact Ridge. Support for CARMA construction
was derived from the states of California, Illinois, and Maryland, the
James S. McDonnell Foundation, the Gordon and Betty Moore Foundation,
the Kenneth T. and Eileen L. Norris Foundation, the University of
Chicago, the Associates of the California Institute of Technology, and
the National Science Foundation. Ongoing CARMA development and
operations are supported by the National Science Foundation under a
cooperative agreement and by the CARMA partner universities. The
National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc.
NR 74
TC 20
Z9 20
U1 3
U2 22
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 1089-5639
J9 J PHYS CHEM A
JI J. Phys. Chem. A
PD JUN 23
PY 2011
VL 115
IS 24
BP 6472
EP 6480
DI 10.1021/jp200539b
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 778MU
UT WOS:000291709400018
PM 21591798
ER
PT J
AU Larsson, J
Fransson, C
Ostlin, G
Groningsson, P
Jerkstrand, A
Kozma, C
Sollerman, J
Challis, P
Kirshner, RP
Chevalier, RA
Heng, K
McCray, R
Suntzeff, NB
Bouchet, P
Crotts, A
Danziger, J
Dwek, E
France, K
Garnavich, PM
Lawrence, SS
Leibundgut, B
Lundqvist, P
Panagia, N
Pun, CSJ
Smith, N
Sonneborn, G
Wang, L
Wheeler, JC
AF Larsson, J.
Fransson, C.
Ostlin, G.
Groningsson, P.
Jerkstrand, A.
Kozma, C.
Sollerman, J.
Challis, P.
Kirshner, R. P.
Chevalier, R. A.
Heng, K.
McCray, R.
Suntzeff, N. B.
Bouchet, P.
Crotts, A.
Danziger, J.
Dwek, E.
France, K.
Garnavich, P. M.
Lawrence, S. S.
Leibundgut, B.
Lundqvist, P.
Panagia, N.
Pun, C. S. J.
Smith, N.
Sonneborn, G.
Wang, L.
Wheeler, J. C.
TI X-ray illumination of the ejecta of supernova 1987A
SO NATURE
LA English
DT Article
ID HUBBLE-SPACE-TELESCOPE; SN 1987A; REVERSE SHOCK; LINE EMISSION;
LIGHT-CURVE; EVOLUTION; RING; SN-1987A; REMNANT; STARS
AB When a massive star explodes as a supernova, substantial amounts of radioactive elements-primarily (56)Ni, (57)Ni and (44)Ti-are produced(1). After the initial flash of light from shock heating, the fading light emitted by the supernova is due to the decay of these elements(2). However, after decades, the energy powering a supernova remnant comes from the shock interaction between the ejecta and the surrounding medium(3). The transition to this phase has hitherto not been observed: supernovae occur too infrequently in the Milky Way to provide a young example, and extragalactic supernovae are generally too faint and too small. Here we report observations that show this transition in the supernova SN 1987A in the Large Magellanic Cloud. From 1994 to 2001, the ejecta faded owing to radioactive decay of (44)Ti as predicted. Then the flux started to increase, more than doubling by the end of 2009. We show that this increase is the result of heat deposited by X-rays produced as the ejecta interacts with the surrounding material. In time, the X-rays will penetrate farther into the ejecta, enabling us to analyse the structure and chemistry of the vanished star.
C1 [Larsson, J.; Fransson, C.; Ostlin, G.; Groningsson, P.; Jerkstrand, A.; Kozma, C.; Sollerman, J.; Lundqvist, P.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
[Challis, P.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Chevalier, R. A.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
[Heng, K.] Eidgenossische Tech Hsch, Inst Astron, CH-8093 Zurich, Switzerland.
[McCray, R.] Univ Colorado, JILA, Boulder, CO USA.
[Suntzeff, N. B.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA.
[Bouchet, P.] DSM IRFU Serv Astrophys Commissariat Energie Alte, FR-91191 Gif Sur Yvette, France.
[Crotts, A.] Columbia Univ, Dept Astron, New York, NY 10027 USA.
[Dwek, E.; Sonneborn, G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Danziger, J.] Osserv Astron Trieste, I-34131 Trieste, Italy.
[France, K.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
[Garnavich, P. M.] Univ Notre Dame, Notre Dame, IN 46556 USA.
[Lawrence, S. S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA.
[Leibundgut, B.] ESO, D-85748 Garching, Germany.
[Panagia, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA.
[Panagia, N.] Osserv Astrofis Catania, INAF CT, I-95123 Catania, Italy.
[Pun, C. S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China.
[Smith, N.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
[Wheeler, J. C.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA.
RP Larsson, J (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden.
EM josefin.larsson@astro.su.se; claes@astro.su.se
RI Dwek, Eli/C-3995-2012; Sonneborn, George/D-5255-2012; Jerkstrand,
Anders/K-9648-2015;
OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman,
Jesper/0000-0003-1546-6615; /0000-0003-0065-2933
FU Swedish Research Council; Swedish National Space Board; Space Telescope
Science Institute
FX This work was supported by the Swedish Research Council and the Swedish
National Space Board. Support for the HST observing programme was
provided by NASA through a grant from the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc.
NR 24
TC 35
Z9 35
U1 0
U2 9
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 23
PY 2011
VL 474
IS 7352
BP 484
EP 486
DI 10.1038/nature10090
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 781NJ
UT WOS:000291939700042
PM 21654749
ER
PT J
AU Jordano, P
Forget, PM
Lambert, JE
Bohning-Gaese, K
Traveset, A
Wright, SJ
AF Jordano, Pedro
Forget, Pierre-Michel
Lambert, Joanna E.
Boehning-Gaese, Katrin
Traveset, Anna
Wright, S. Joseph
TI Frugivores and seed dispersal: mechanisms and consequences for
biodiversity of a key ecological interaction
SO BIOLOGY LETTERS
LA English
DT Editorial Material
DE conservation biology; dispersal; fragmentation; frugivory; hunting;
movement ecology
AB The 5th Symposium on Frugivores and Seed Dispersal, held in Montpellier (France), 13-18 June 2010, brought together more than 220 researchers exemplifying a wide diversity of approaches to the study of frugivory and dispersal of seeds. Following Ted Fleming and Alejandro Estrada's initiative in 1985, this event was a celebration of the 25th anniversary of the first meeting in Veracruz, Mexico. Frugivory and seed dispersal are active research areas that have diversified in multiple directions since 1985 to include evolution (e.g. phylogenetic diversity and dispersal adaptations), physiology (e.g. sensory cues and digestion), landscape ecology (movement patterns), molecular ecology (e.g. gene flow, genetic diversity and structure), community ecology (e.g. mutualistic interaction networks) and conservation biology (effects of hunting, fragmentation, invasion and extinction), among others. This meeting provided an opportunity to assess conceptual and methodological progress, to present ever more sophisticated insights into frugivory in animals and dispersal patterns in plants, and to report the advances made in examining the mechanisms and consequences of seed dispersal for plants and frugivores.
C1 [Jordano, Pedro] CSIC, Integrat Ecol Grp, Estac Biol Donana, E-41092 Seville, Spain.
[Forget, Pierre-Michel] Museum Natl Hist Nat, UMR 7179, F-91800 Brunoy, France.
[Lambert, Joanna E.] Univ Texas San Antonio, Dept Ecol Anthropol, San Antonio, TX 78249 USA.
[Boehning-Gaese, Katrin] Goethe Univ Frankfurt, Dept Biol Sci, D-60323 Frankfurt, Germany.
[Boehning-Gaese, Katrin] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany.
[Traveset, Anna] Inst Mediterrani Estudis Avancats CSIC UIB, Esporles Mallorca 07190, Illes Balears, Spain.
[Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Jordano, P (reprint author), CSIC, Integrat Ecol Grp, Estac Biol Donana, Avda Amer Vespucio S-N, E-41092 Seville, Spain.
EM jordano@ebd.csic.es
RI Biodiversity & Climate Res Ctr, BiK-F/C-4266-2012; Jordano,
Pedro/A-5162-2008; Forget, Pierre-Michel/B-4355-2009; Wright,
Stuart/M-3311-2013; CSIC, EBD Donana/C-4157-2011
OI Jordano, Pedro/0000-0003-2142-9116; Forget,
Pierre-Michel/0000-0002-9252-974X; Wright, Stuart/0000-0003-4260-5676;
CSIC, EBD Donana/0000-0003-4318-6602
NR 11
TC 26
Z9 29
U1 4
U2 67
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 JUN 23
PY 2011
VL 7
IS 3
BP 321
EP 323
DI 10.1098/rsbl.2010.0986
PG 3
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 762XI
UT WOS:000290515100001
PM 21084336
ER
PT J
AU Stoinski, TS
Drayton, LA
Price, EE
AF Stoinski, T. S.
Drayton, L. A.
Price, E. E.
TI Evidence of social learning in black-and-white ruffed lemurs (Varecia
variegata)
SO BIOLOGY LETTERS
LA English
DT Article
DE behavioural traditions; culture; two-action method
ID PROSIMIAN PRIMATES; BEHAVIOR; CATTA; CHIMPANZEES; CULTURES; FULVUS; TASK
AB Although many studies have examined social learning capabilities in apes and monkeys, experiments involving prosimians remain largely absent. We investigated the potential for social learning in black-and-white ruffed lemurs using a two-action foraging task. Eight individuals were divided into two experimental groups and exposed to conspecifics using one of two techniques to access food. Subjects were then given access to the apparatus and their retrieval techniques were recorded and compared. All subjects made their first retrieval using the technique they observed being demonstrated, and there were significant differences between the two groups in their overall response patterns. These results suggest that prosimians are capable of social learning and that additional long-term field studies may reveal the presence of behavioural traditions similar to those found in other primates.
C1 [Stoinski, T. S.; Drayton, L. A.] Zoo Atlanta, Atlanta, GA 30315 USA.
[Price, E. E.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA.
RP Stoinski, TS (reprint author), Zoo Atlanta, 800 Cherokee Ave, Atlanta, GA 30315 USA.
EM tstoinski@zooatlanta.org
NR 18
TC 8
Z9 8
U1 7
U2 59
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 JUN 23
PY 2011
VL 7
IS 3
BP 376
EP 379
DI 10.1098/rsbl.2010.1070
PG 4
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 762XI
UT WOS:000290515100018
PM 21227976
ER
PT J
AU Stouffer, PC
Johnson, EI
Bierregaard, RO
Lovejoy, TE
AF Stouffer, Philip C.
Johnson, Erik I.
Bierregaard, Richard O., Jr.
Lovejoy, Thomas E.
TI Understory Bird Communities in Amazonian Rainforest Fragments: Species
Turnover through 25 Years Post-Isolation in Recovering Landscapes
SO PLOS ONE
LA English
DT Article
ID HABITAT FRAGMENTATION; INSECTIVOROUS BIRDS; ANIMAL COMMUNITIES;
SECONDARY FORESTS; COSTA-RICA; EXTINCTION; RATES; DEFORESTATION;
DYNAMICS; COLONIZATION
AB Inferences about species loss following habitat conversion are typically drawn from short-term surveys, which cannot reconstruct long-term temporal dynamics of extinction and colonization. A long-term view can be critical, however, to determine the stability of communities within fragments. Likewise, landscape dynamics must be considered, as second growth structure and overall forest cover contribute to processes in fragments. Here we examine bird communities in 11 Amazonian rainforest fragments of 1-100 ha, beginning before the fragments were isolated in the 1980s, and continuing through 2007. Using a method that accounts for imperfect detection, we estimated extinction and colonization based on standardized mist-net surveys within discreet time intervals (1-2 preisolation samples and 4-5 post-isolation samples). Between preisolation and 2007, all fragments lost species in an area-dependent fashion, with loss of as few as,10% of preisolation species from 100-ha fragments, but up to 70% in 1-ha fragments. Analysis of individual time intervals revealed that the 2007 result was not due to gradual species loss beginning at isolation; both extinction and colonization occurred in every time interval. In the last two samples, 2000 and 2007, extinction and colonization were approximately balanced. Further, 97 of 101 species netted before isolation were detected in at least one fragment in 2007. Although a small subset of species is extremely vulnerable to fragmentation, and predictably goes extinct in fragments, developing second growth in the matrix around fragments encourages recolonization in our landscapes. Species richness in these fragments now reflects local turnover, not long-term attrition of species. We expect that similar processes could be operating in other fragmented systems that show unexpectedly low extinction.
C1 [Stouffer, Philip C.; Johnson, Erik I.] Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
[Bierregaard, Richard O., Jr.] Univ N Carolina, Dept Biol, Charlotte, NC 28223 USA.
[Lovejoy, Thomas E.] Heinz Ctr, Washington, DC USA.
[Stouffer, Philip C.; Johnson, Erik I.; Bierregaard, Richard O., Jr.; Lovejoy, Thomas E.] Inst Nacl de Pesquisas da Amazonia, Projeto Dinam Fragmentos Florestais, Manaus, Amazonas, Brazil.
[Stouffer, Philip C.; Johnson, Erik I.; Bierregaard, Richard O., Jr.; Lovejoy, Thomas E.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil.
RP Stouffer, PC (reprint author), Louisiana State Univ, Ctr Agr, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA.
EM pstouffer@lsu.edu
FU National Institute for Amazonian Research (INPA); World Wildlife
Fund-US; Smithsonian Institution; MacArthur Foundation; U.S. National
Science Foundation [DEB 0545491]; United States Agency for International
Development; Mellon Foundation
FX The National Institute for Amazonian Research (INPA), World Wildlife
Fund-US, Smithsonian Institution, MacArthur Foundation, U.S. National
Science Foundation (DEB 0545491), United States Agency for International
Development, Mellon Foundation, and other organizations generously
supported this work and the Biological Dynamics of Forest Fragments
Project. The funders had no role in study design, data collection and
analysis, decision to publish, or preparation of the manuscript.
NR 71
TC 25
Z9 25
U1 5
U2 45
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 JUN 22
PY 2011
VL 6
IS 6
AR e20543
DI 10.1371/journal.pone.0020543
PG 11
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 782TF
UT WOS:000292033700009
PM 21731616
ER
PT J
AU Anker, A
Nizinski, M
AF Anker, Arthur
Nizinski, Martha
TI Description of a new deep-water species of Alpheus Fabricius, 1798 from
the Gulf of Mexico (Crustacea, Decapoda, Alpheidae)
SO ZOOTAXA
LA English
DT Article
DE Caridea; Alpheidae; Alpheus; Gulf of Mexico; western Atlantic;
deep-water reefs; new species
AB A new deep-water species of the snapping shrimp genus Alpheus Fabricius, 1798 is described from two offshore localities in the northern Gulf of Mexico, south of Louisiana. Alpheus lentiginosus n. sp. belongs to the A. macrocheles (Hailstone, 1835) species group and is most closely related to the western Atlantic A. pouang Christoffersen, 1979 and A. amblyonyx Chace 1972, the eastern Atlantic A. platydactylus Coutiere, 1897 and A. macrocheles (Hailstone, 1835), and perhaps also to the eastern Pacific A. exilis Kim & Abele, 1988. The new species is associated with deep-water soft sediments adjacent to clusters of Lophelia pertusa (L.) (Scleractinia) or mud-covered rocks and cobble, at a depth range of 336-438 m, thus representing the deepest-known record of the Alpheidae in the Gulf of Mexico and the entire western Atlantic.
C1 [Anker, Arthur] Univ Fed Ceara, Inst Ciencias Mar Labomar, Fortaleza, Ceara, Brazil.
[Nizinski, Martha] Smithsonian Inst, NOAA NMFS Natl Systemat Lab, Washington, DC 20560 USA.
RP Anker, A (reprint author), Univ Fed Ceara, Inst Ciencias Mar Labomar, Fortaleza, Ceara, Brazil.
EM arthuranker7@yahoo.com; nizinski@si.edu
FU US Geological Survey
FX The science parties, the crew of the R/V Seward Johnson and the pilots
of the Johnson Sea Link are gratefully acknowledged for their assistance
with collection of the above-reported material. Funding support for
expeditions to the Gulf of Mexico was provided by US Geological Survey
Deepwater Program (K.J. Sulak, lead PI in 2004; S. W. Ross, lead PI in
2009). Karen Reed (USNM) informed MN about AA visiting the USNM
collections thus initiating this study and also arranged loan of
specimens. Linda Ward (USNM) and Cheryl Ames (UNCW, NOAA) provided
curatorial assistance; Cheryl Morrison (USGS) provided colour
photographs; William Moser (USNM) helped with station data. Kristin
Hultgren (USNM) and an anonymous reviewer kindly reviewed the
manuscript.
NR 20
TC 3
Z9 5
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 JUN 21
PY 2011
IS 2925
BP 49
EP 56
PG 8
WC Zoology
SC Zoology
GA 782HF
UT WOS:000291998400005
ER
PT J
AU Croston, JH
Hardcastle, MJ
Mingo, B
Evans, DA
Dicken, D
Morganti, R
Tadhunter, CN
AF Croston, J. H.
Hardcastle, M. J.
Mingo, B.
Evans, D. A.
Dicken, D.
Morganti, R.
Tadhunter, C. N.
TI A LARGE-SCALE SHOCK SURROUNDING A POWERFUL RADIO GALAXY?
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE galaxies: active; galaxies: jets
ID X-RAY-EMISSION; MAGNETIC-FIELD STRENGTHS; JET POWER; CLUSTER; SAMPLE;
LOBES; CENTAURUS; NUCLEI; MODELS
AB We report Chandra evidence for a 200 kpc scale shock in the cluster surrounding the powerful radio galaxy 3C 444. Our 20 ks observation allows us to identify a clear surface brightness drop around the outer edge of the radio galaxy, which is likely to correspond to a spheroidal shock propagating into the intracluster medium. We measure a temperature jump across this drop of a factor similar to 1.7, which corresponds to a Mach number of similar to 1.7. This is likely to be an underestimate due to the need to average over fairly large regions. We also detect clear cavities corresponding to the positions of the radio lobes, which is only the second such detection associated with an FRII radio galaxy. We estimate that the total energy transferred to the environment is >8.2 x 10(60) erg, corresponding to a jet power >2.9 x 10(45) erg s(-1). Our results suggest that energy input from FRII radio galaxies is likely to exceed substantially estimates based on cluster cavity scaling relations.
C1 [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
[Hardcastle, M. J.; Mingo, B.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England.
[Evans, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Evans, D. A.] Elon Univ, Dept Phys, Elon, NC 27244 USA.
[Dicken, D.] Rochester Inst Technol, Dept Phys & Astron, Rochester, NY 14623 USA.
[Morganti, R.] Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands.
[Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands.
[Tadhunter, C. N.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
RP Croston, JH (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England.
EM J.Croston@soton.ac.uk
RI Hardcastle, Martin/E-2264-2012
OI Hardcastle, Martin/0000-0003-4223-1117
FU South-East Physics Network (SEPnet); Royal Society
FX J.H.C. acknowledges support from the South-East Physics Network
(SEPnet). M.J.H. thanks the Royal Society for support via a University
Research Fellowship. We thank the anonymous referee for useful comments
that have enabled us to improve the Letter.
NR 30
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U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 20
PY 2011
VL 734
IS 2
AR L28
DI 10.1088/2041-8205/734/2/L28
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797NX
UT WOS:000293135700003
ER
PT J
AU Barnard, R
Garcia, M
Li, Z
Primini, F
Murray, SS
AF Barnard, R.
Garcia, M.
Li, Z.
Primini, F.
Murray, S. S.
TI FOUR NEW BLACK HOLE CANDIDATES IDENTIFIED IN M31 GLOBULAR CLUSTERS WITH
CHANDRA AND XMM-NEWTON
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies: individual (M31); globular clusters:
general; X-rays: binaries; X-rays: general
ID X-RAY BINARIES; STAR-CLUSTERS; SPECTRAL TRANSITIONS; UPDATED SURVEY;
NEUTRON-STAR; NGC 4472; O-III; MASS; EMISSION; BRIGHT
AB We have identified four new black hole candidates (BHCs) in M31 globular clusters (GCs) using 123 Chandra and 4 XMM-Newton observations of the M31 central region. The X-ray source associated with Bo 163 (XB163) is a recurrent transient with the highest observed luminosity, similar to 1.4x10(38) erg s(-1), considerably brighter than any outbursts from neutron star transients Aql X-1 or 4U 1608-452; the outburst apparently started similar to 45 days earlier than the observed peak, and hence the luminosity may have been considerably higher. We identified XB082, XB153, and XB185 as BHCs by observing "low state" emission spectra at luminosities that exceed the threshold for neutron star binaries. The probability that these are neutron star systems with anisotropic emission beamed toward us is less than or similar to 4 x 10(-4), and their variability suggests emission from a single source. We therefore conclude that these systems likely contain black holes rather than neutron stars. We have now identified four persistently bright BHCs in the region; the probability that these are all background active galactic nuclei is less than or similar to 1x10(-20). According to theory, the donors could be tidally captured main-sequence stars or white dwarfs in ultracompact binaries. We find that GCs that are particularly massive (XB082) or metal-rich (XB144) can host bright X-ray sources in addition to GCs that are both (XB163). Our method may reveal BHCs in other bright X-ray sources.
C1 [Barnard, R.; Garcia, M.; Li, Z.; Primini, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Primini, Francis/0000-0002-6077-0643
FU ESA; USA (NASA); NASA [NAS-03060]; [GO9-0100X]; [GO-11013]
FX We thank the referees for their insightful comments; this work was
significantly improved as a result. This research has made use of data
obtained from the Chandra data archive, and software provided by the
Chandra X-ray Center (CXC). This work also used observations made by
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA member states and the USA (NASA). R. B. is funded
by Chandra grant GO9-0100X and HST grant GO-11013. M. R. G. is partially
supported by NASA grant NAS-03060. We thank Andrew King for useful
discussions.
NR 46
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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 20
PY 2011
VL 734
IS 2
AR 79
DI 10.1088/0004-637X/734/2/79
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500007
ER
PT J
AU Beky, B
Bakos, GA
Hartman, J
Torres, G
Latham, DW
Jordan, A
Arriagada, P
Bayliss, D
Kiss, LL
Kovacs, G
Quinn, SN
Marcy, GW
Howard, AW
Fischer, DA
Johnson, JA
Esquerdo, GA
Noyes, RW
Buchhave, LA
Sasselov, DD
Stefanik, RP
Perumpilly, G
Lazar, J
Papp, I
Sari, P
AF Beky, B.
Bakos, G. A.
Hartman, J.
Torres, G.
Latham, D. W.
Jordan, A.
Arriagada, P.
Bayliss, D.
Kiss, L. L.
Kovacs, Geza
Quinn, S. N.
Marcy, G. W.
Howard, A. W.
Fischer, D. A.
Johnson, J. A.
Esquerdo, G. A.
Noyes, R. W.
Buchhave, L. A.
Sasselov, D. D.
Stefanik, R. P.
Perumpilly, G.
Lazar, J.
Papp, I.
Sari, P.
TI HAT-P-27b: A HOT JUPITER TRANSITING A G STAR ON A 3 DAY ORBIT
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary systems; stars: individual (HAT-P-27, GSC 0333-00351);
techniques: photometric; techniques: spectroscopic
ID SHORT-PERIOD PLANETS; LOW-DENSITY PLANET; SOLAR-TYPE STAR; SPECTROSCOPIC
BINARIES; DETERMINISTIC MODEL; EXTRASOLAR PLANETS; ECCENTRIC ORBIT;
GIANT PLANETS; BRIGHT STAR; K-DWARF
AB We report the discovery of HAT-P-27b, an exoplanet transiting the moderately bright G8 dwarf star GSC 0333-00351 (V = 12.214). The orbital period is 3.039586 +/- 0.000012 days, the reference epoch of transit is 2455186.01879 +/- 0.00054 (BJD), and the transit duration is 0.0705 +/- 0.0019 days. The host star with its effective temperature 5300 +/- 90 K is somewhat cooler than the Sun and is more metal-rich with a metallicity of +0.29 +/- 0.10. Its mass is 0.94 +/- 0.04 M-circle dot and radius is 0.90(-0.04)(+0.05) R-circle dot. For the planetary companion we determine a mass of 0.660 +/- 0.033 M-J and radius of 1.038(-0.058)(+0.077) R-J. For the 30 known transiting exoplanets between 0.3 M-J and 0.8 M-J, a negative correlation between host star metallicity and planetary radius and an additional dependence of planetary radius on equilibrium temperature are confirmed at a high level of statistical significance.
C1 [Beky, B.; Bakos, G. A.; Hartman, J.; Torres, G.; Latham, D. W.; Jordan, A.; Quinn, S. N.; Esquerdo, G. A.; Noyes, R. W.; Buchhave, L. A.; Sasselov, D. D.; Stefanik, R. P.; Perumpilly, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Jordan, A.; Arriagada, P.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile.
[Bayliss, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT, Australia.
[Kiss, L. L.; Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary.
[Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
[Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA.
[Johnson, J. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA.
[Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark.
[Perumpilly, G.] Univ S Dakota, Dept Phys, Vermillion, SD 57069 USA.
[Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary.
RP Beky, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM bbeky@cfa.harvard.edu
RI Bayliss, Daniel/I-4635-2012; Howard, Andrew/D-4148-2015;
OI Howard, Andrew/0000-0001-8638-0320; Jordan, Andres/0000-0002-5389-3944;
Buchhave, Lars A./0000-0003-1605-5666; Hartman,
Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861
FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G]; SAO IRD grants; NSF
[AST-0702843]; Fondecyt [1095213, BASAL CATA PFB-06, FONDAP CFA
15010003, MIDE-PLAN ICM Nucleus P07-021-F, Anillo ACT-086]; Hungarian
Scientific Research Foundation (OTKA) [K-81373]; Hungarian Academy of
Sciences; Hungarian OTKA [K76816, K83790, MB08C 81013]; Kepler Mission
under NASA [NCC2-1390]
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. G. T. acknowledges partial support from NASA grant
NNX09AF59G. A.J. acknowledges support from Fondecyt project 1095213,
BASAL CATA PFB-06, FONDAP CFA 15010003, MIDE-PLAN ICM Nucleus P07-021-F,
and Anillo ACT-086. G. K. thanks the Hungarian Scientific Research
Foundation (OTKA) for support through grant K-81373. L. L. K. is
supported by the "Lendulet" Young Researchers Program of the Hungarian
Academy of Sciences and the Hungarian OTKA grants K76816, K83790 and
MB08C 81013. Tamas Szalai (University of Szeged) is acknowledged for his
assistance during the ANU 2.3 m observations. We also acknowledge
partial support from the Kepler Mission under NASA Cooperative Agreement
NCC2-1390 (D.W.L., PI). This research has made use of Keck telescope
time granted through NOAO (A201Hr) and NASA (N018Hr, N167Hr). We also
thank Mount Stromlo Observatory and Siding Spring Observatory for the
ANU 2.3 m telescope time.
NR 79
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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 JUN 20
PY 2011
VL 734
IS 2
AR 109
DI 10.1088/0004-637X/734/2/109
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500037
ER
PT J
AU Castro, D
Slane, PO
Gaensler, BM
Hughes, JP
Patnaude, DJ
AF Castro, D.
Slane, P. O.
Gaensler, B. M.
Hughes, J. P.
Patnaude, D. J.
TI AN XMM-NEWTON STUDY OF THE BRIGHT, NEARBY SUPERNOVA REMNANT G296.1-0.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM: individual objects (G296.1-0.5); ISM: supernova remnants; X-rays:
individual (G296.1-0.5, 2XMMi J115004.8-622442)
ID WOLF-RAYET STARS; X-RAY; NOVA REMNANT; WIND; CATALOG; GALAXY; CRUX;
EVOLUTION; EMISSION; NEBULAE
AB We present a detailed study of the supernova remnant (SNR) G296.1-0.5, performed using observations with the European Photon Imaging Camera (EPIC) and Reflection Grating Spectrometer instruments of the XMM-Newton satellite. G296.1-0.5 is a bright remnant that displays an incomplete multiple-shell morphology in both its radio and X-ray images. We use a set of observations toward G296.1-0.5, from three distinct pointings of EPIC, in order to perform a thorough spatial and spectral analysis of this remnant, and hence determine what type of progenitor gave rise to the supernova explosion, and describe the evolutionary state of the SNR. Our XMM-Newton observations establish that the spectral characteristics are consistent across the X-ray bright regions of the object and are best described by a model of the emission from a nonequilibrium ionization collisional plasma. The study reveals that the emission from the shell is characterized by an excess of N and an underabundance of O, which is typical of wind material from red supergiant and Wolf-Rayet stars. Additionally, we have detected transient X-ray source 2XMMi J115004.8-622442 at the edge of the SNR whose properties suggest that it is the result of stellar flare, and we discuss its nature in more detail.
C1 [Castro, D.; Slane, P. O.; Patnaude, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Castro, D.] Univ Simon Bolivar, Dept Fis, Caracas 1080A, Venezuela.
[Gaensler, B. M.] Univ Sydney, Sch Phys A29, Sydney Inst Astron, Sydney, NSW 2006, Australia.
[Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
RP Castro, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Gaensler, Bryan/F-8655-2010;
OI Gaensler, Bryan/0000-0002-3382-9558
FU NASA [NNX07AQ61G, NAS8-03060, NNX08AX55G, NNX08AX72G, NNX09AAP40G];
Australian Research Council [FF0561298]; Australian Research Council;
School of Physics of the University of Sydney; National Aeronautics and
Space Administration; National Science Foundation
FX The authors wish to thank Tea Temim, Jeremy Drake, Joseph Neilsen, Hans
Moritz Gunther, and Jeff McClintock for several helpful discussions.
This work was supported in part by NASA grant NNX07AQ61G. P.O.S.
acknowledges support from NASA contract NAS8-03060. B. M. G.
acknowledges the support of a Federation Fellowship from the Australian
Research Council through grant FF0561298. Financial support for XMM
research by J.P.H. at Rutgers is provided by NASA grants NNX08AX55G,
NNX08AX72G, and NNX09AAP40G. The MOST is operated with the support of
the Australian Research Council and the School of Physics of the
University of Sydney. 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 47
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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 20
PY 2011
VL 734
IS 2
AR 86
DI 10.1088/0004-637X/734/2/86
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500014
ER
PT J
AU Castro, D
Slane, P
Patnaude, DJ
Ellison, DC
AF Castro, Daniel
Slane, Patrick
Patnaude, Daniel J.
Ellison, Donald C.
TI THE IMPACT OF EFFICIENT PARTICLE ACCELERATION ON THE EVOLUTION OF
SUPERNOVA REMNANTS IN THE SEDOV-TAYLOR PHASE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; magnetohydrodynamics (MHD); ISM: supernova remnants
ID DIFFUSIVE SHOCK ACCELERATION; CHANDRA X-RAY; NONEQUILIBRIUM IONIZATION;
COSMIC-RAYS; SHELL; SPECTRA; WAVES; DISCOVERY; EMISSION; MODELS
AB We investigate the effects of the efficient production of cosmic rays (CRs) on the evolution of supernova remnants (SNRs) in the adiabatic Sedov-Taylor phase. We model the SNR by coupling the hydrodynamic evolution with nonlinear diffusive shock acceleration (DSA) and track self-consistently the ionization state of the shock-heated plasma. Using a plasma emissivity code and the results of the model, we predict the thermal X-ray emission and combine it with the non-thermal component in order to obtain the complete spectrum in this energy range. Hence, we study how the interpretation of thermal X-ray observations is affected by the efficiency of the DSA process, and find that, compared to test particle cases, the efficient DSA example yields a smaller shock radius and speed, a larger compression ratio, and lower intensity X-ray thermal emission. We also find that a model where the shock is not assumed to produce CRs can fit the X-ray observational properties of an example with efficient particle acceleration, with a different set of input parameters, and in particular a much lower explosion energy. Additionally, we model the broadband non-thermal emission and investigate what signatures result from the acceleration of particles.
C1 [Castro, Daniel; Slane, Patrick; Patnaude, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Castro, Daniel] Univ Simon Bolivar, Dept Fis, Caracas 1080A, Venezuela.
[Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
RP Castro, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU NASA [NAS8-03060, NNH04Zss001N-LTSA, 06-ATP06-21]; [NNX09AT68G]
FX The authors thank the referees for their insightful comments. This work
was carried out with partial support from Fermi Grant NNX09AT68G. P. S.
and D.J.P. acknowledge support from NASA Contract NAS8-03060. D. C. E.
acknowledges support through NASA grants NNH04Zss001N-LTSA and
06-ATP06-21.
NR 36
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U2 4
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2011
VL 734
IS 2
AR 85
DI 10.1088/0004-637X/734/2/85
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500013
ER
PT J
AU Davis, SW
Narayan, R
Zhu, YC
Barret, D
Farrell, SA
Godet, O
Servillat, M
Webb, NA
AF Davis, Shane W.
Narayan, Ramesh
Zhu, Yucong
Barret, Didier
Farrell, Sean A.
Godet, Olivier
Servillat, Mathieu
Webb, Natalie A.
TI THE COOL ACCRETION DISK IN ESO 243-49 HLX-1: FURTHER EVIDENCE OF AN
INTERMEDIATE-MASS BLACK HOLE
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; X-rays: binaries;
X-rays: individual (ESO 243-49 HLX-1)
ID X-RAY SOURCES; VERTICAL STRUCTURE; SPECTRA; BINARIES; STATE; SPIN;
MODELS; INCLINATION; CONTINUUM; GALAXIES
AB With an inferred bolometric luminosity exceeding 10(42) erg s(-1), HLX-1 in ESO 243-49 is the most luminous of ultraluminous X-ray sources and provides one of the strongest cases for the existence of intermediate-mass black holes. We obtain good fits to disk-dominated observations of the source with BHSPEC, a fully relativistic black hole accretion disk spectral model. Due to degeneracies in the model arising from the lack of independent constraints on inclination and black hole spin, there is a factor of 100 uncertainty in the best-fit black hole mass M. Nevertheless, spectral fitting of XMM-Newton observations provides robust lower and upper limits with 3000 M-circle dot less than or similar to M less than or similar to 3 x 10(5) M-circle dot, at 90% confidence, placing HLX-1 firmly in the intermediate-mass regime. The lower bound on M is entirely determined by matching the shape and peak energy of the thermal component in the spectrum. This bound is consistent with (but independent of) arguments based solely on the Eddington limit. Joint spectral modeling of the XMM-Newton data with more luminous Swift and Chandra observations increases the lower bound to 6000 M-circle dot, but this tighter constraint is not independent of the Eddington limit. The upper bound on M is sensitive to the maximum allowed inclination i, and is reduced to M less than or similar to 10(5) M-circle dot if we limit i less than or similar to 75 degrees.
C1 [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada.
[Narayan, Ramesh; Zhu, Yucong; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Barret, Didier; Godet, Olivier; Webb, Natalie A.] Univ Toulouse 3, Univ Toulouse, Observ Midi Pyrenees, IRAP, F-31062 Toulouse, France.
[Barret, Didier; Godet, Olivier; Webb, Natalie A.] CNRS, IRAP, F-31028 Toulouse 4, France.
[Farrell, Sean A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
[Farrell, Sean A.] Univ Sydney, Sydney Inst Astron, Sch Phys A29, Sydney, NSW 2006, Australia.
RP Davis, SW (reprint author), Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada.
OI Narayan, Ramesh/0000-0002-1919-2730
FU NSERC of Canada; UK Science and Technology Research Council; Australian
Research Council; NASA [NNX11AE16G]; NASA/Chandra grant [DD0-11050X];
NSF [AST-0909073]; ESA Member States
FX We thank the anonymous referee for useful comments that improved the
paper. S. W. D. is supported in part through NSERC of Canada. S. A. F.
gratefully acknowledges funding from the UK Science and Technology
Research Council and the Australian Research Council. R.N. acknowledges
support from NASA grant NNX11AE16G. M. S. acknowledges supports from
NASA/Chandra grant DD0-11050X and NSF grant AST-0909073. This research
has made use of data obtained from the Chandra Data Archive and software
provided by the Chandra X-ray Center. Based on observations from
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA.
NR 52
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PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2011
VL 734
IS 2
AR 111
DI 10.1088/0004-637X/734/2/111
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500039
ER
PT J
AU Oberg, KI
Qi, CH
Fogel, JKJ
Bergin, EA
Andrews, SM
Espaillat, C
Wilner, DJ
Pascucci, I
Kastner, JH
AF Oeberg, Karin I.
Qi, Chunhua
Fogel, Jeffrey K. J.
Bergin, Edwin A.
Andrews, Sean M.
Espaillat, Catherine
Wilner, David J.
Pascucci, Ilaria
Kastner, Joel H.
TI DISK IMAGING SURVEY OF CHEMISTRY WITH SMA. II. SOUTHERN SKY
PROTOPLANETARY DISK DATA AND FULL SAMPLE STATISTICS
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM;
stars: formation; techniques: high angular resolution
ID MAIN-SEQUENCE STARS; HERBIG-AE STARS; TWIN YOUNG SUNS; T-TAURI STARS;
DM-TAURI; SURROUNDING HD-142527; MOLECULAR-EMISSION; COMPLEX CHEMISTRY;
ACCRETION RATES; IM-LUPI
AB This is the second in a series of papers based on data from DISCS, a Submillimeter Array observing program aimed at spatially and spectrally resolving the chemical composition of 12 protoplanetary disks. We present data on six Southern sky sources-IM Lup, SAO 206462 (HD 135344b), HD 142527, AS 209, AS 205, and V4046 Sgr-which complement the six sources in the Taurus star-forming region reported previously. CO 2-1 and IICO+ 3-2 emission are detected and resolved in all disks and show velocity patterns consistent with Keplerian rotation. Where detected, the emission from DCO+ 3-2, N2H+ 3-2, H2CO 3(0 3) - 2(0 2) and 4(1 4) - 3(1 3,) HCN 3-2, and CN 2(3 3/4/2) - 1(2 2/3/1) are also generally spatially resolved. The detection rates are highest toward the M and K stars, while the F star SAO 206462 has only weak CN and HCN emission, and H2CO alone is detected toward HD 142527. These findings together with the statistics from the previous Taurus disks support the hypothesis that high detection rates of many small molecules depend on the presence of a cold and protected disk midplane, which is less common around F and A stars compared to M and K stars. Disk-averaged variations in the proposed radiation tracer CN/HCN are found to be small, despite a two orders of magnitude range of spectral types and accretion rates. In contrast, the resolved images suggest that the CN/HCN emission ratio varies with disk radius in at least two of the systems. There are no clear observational differences in the disk chemistry between the classical/full T Tauri disks and transitional disks. Furthermore, the observed line emission does not depend on the measured accretion luminosities or the number of infrared lines detected, which suggests that the chemistry outside of 100 AU is not coupled to the physical processes that drive the chemistry in the innermost few AU.
C1 [Oeberg, Karin I.; Qi, Chunhua; Andrews, Sean M.; Espaillat, Catherine; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
[Fogel, Jeffrey K. J.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
[Pascucci, Ilaria] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
[Kastner, Joel H.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
FU Smithsonian Institution; Academia Sinica; NASA through Space Telescope
Science Institute [NAS 5-26555]; National Science Foundation [0901947]
FX This work has benefited from discussions with Ewine van Dishoeck and
Michiel Hogerheijde and helpful suggestions from the anonymous referee.
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. Support for K.I.O. is provided by NASA through a Hubble
Fellowship grant awarded by the Space Telescope Science Institute, which
is operated by the Association of Universities for Research in
Astronomy, Inc., for NASA, under contract NAS 5-26555. C.E. was
supported by the National Science Foundation under Award No. 0901947.
NR 60
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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 JUN 20
PY 2011
VL 734
IS 2
AR 98
DI 10.1088/0004-637X/734/2/98
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500026
ER
PT J
AU Pasachoff, JM
Rusin, V
Druckmullerova, H
Saniga, M
Lu, M
Malamut, C
Seaton, DB
Golub, L
Engell, AJ
Hill, SW
Lucas, R
AF Pasachoff, J. M.
Rusin, V.
Druckmuellerova, H.
Saniga, M.
Lu, M.
Malamut, C.
Seaton, D. B.
Golub, L.
Engell, A. J.
Hill, S. W.
Lucas, R.
TI STRUCTURE AND DYNAMICS OF THE 2010 JULY 11 ECLIPSE WHITE-LIGHT CORONA
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE eclipses; Sun: chromosphere; Sun: corona; Sun: coronal mass ejections
(CMEs); Sun: magnetic topology; Sun: UV radiation
ID SOLAR CORONA; MASS EJECTIONS; PROMINENCE; CYCLE
AB The white-light corona (WLC) during the total solar eclipse on 2010 July 11 was observed by several teams in the Moon's shadow stretching across the Pacific Ocean and a number of isolated islands. We present a comparison of the WLC as observed by eclipse teams located on the Tatakoto Atoll in French Polynesia and on Easter Island, 83 minutes later, combined with near-simultaneous space observations. The eclipse was observed at the beginning of the solar cycle, not long after solar minimum. Nevertheless, the solar corona shows a plethora of different features (coronal holes, helmet streamers, polar rays, very faint loops and radial-oriented thin streamers, a coronal mass ejection, and a puzzling "curtain-like" object above the north pole). Comparing the observations from the two sites enables us to detect some dynamic phenomena. The eclipse observations are further compared with a hairy-ball model of the magnetic field and near-simultaneous images from the Atmospheric Imaging Assembly on NASA's Solar Dynamics Observatory, the Extreme Ultraviolet Imager on NASA's Solar Terrestrial Relations Observatory, the Sun Watcher, using Active Pixel System Detector and Image Processing on ESA's PRoject for Onboard Autonomy, and the Naval Research Laboratory's Large Angle and Spectrometric Coronagraph on ESA's Solar and Heliospheric Observatory. The Ludendorff flattening coefficient is 0.156, matching the expected ellipticity of coronal isophotes at 2 R-circle dot, for this rising phase of the solar-activity cycle.
C1 [Pasachoff, J. M.] Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA.
[Rusin, V.; Saniga, M.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia.
[Druckmuellerova, H.] Brno Univ Technol, Brno 61669, Czech Republic.
[Lu, M.; Malamut, C.] Williams Coll, Dept Astron, Williamstown, MA 01267 USA.
[Malamut, C.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA.
[Seaton, D. B.] Royal Observ Belgium, SIDC, B-1180 Brussels, Belgium.
[Golub, L.; Engell, A. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
[Hill, S. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
[Lucas, R.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
RP Pasachoff, JM (reprint author), Williams Coll, Hopkins Observ, Williamstown, MA 01267 USA.
EM eclipse@williams.edu; vrusin@ta3.sk; hanadruck@seznam.cz;
msaniga@ta3.sk; muzhou.lu@williams.edu; cmalamut@wesleyan.edu;
dseaton@oma.be; golub@cfa.harvard.edu; aengell@cfa.harvard.edu;
steele.w.hill@nasa.gov; lucas@physics.usyd.edu.au
RI Saniga, Metod/F-6200-2012;
OI Saniga, Metod/0000-0001-9642-5879; SEATON, DANIEL/0000-0002-0494-2025
FU VEGA (Slovak Academy of Sciences) [2/0098/10]; Czech Science Foundation
[205/09/1469]; National Science Foundation [AGS-1047726, AST-1005024];
Williams College; NASA's Marshall Space Flight Center [NNX10AK47A]; U.S.
Department of Defense; European Commission [218816]; Centre Spatial de
Liege; BELSPO; Lockheed Martin
FX The work of V. R. and M. S. was partially supported by the VEGA grant
agency project 2/0098/10 (Slovak Academy of Sciences) and that of H. D.
by grant 205/09/1469 of the Czech Science Foundation. V. R. also
cordially thanks Shadia Habbal for partial financial support, the
ASTELCO for providing the mount, and Heifara Lanteires for hospitality
during his stay at Tatakoto. J.M.P.'s eclipse research is supported in
part by the Solar Terrestrial Program of the National Science Foundation
through grant AGS-1047726; the 2010 expedition received additional
support from the Brandi Fund and Science Center funds from Williams
College. J.M.P.'s solar research is also supported in part by grant
NNX10AK47A from NASA's Marshall Space Flight Center. C. M. was a Keck
Northeast Astronomy Consortium Summer Fellow, supported at Williams
College by the Research Experiences for Undergraduates program of the
National Science Foundation under grant AST-1005024. Partial support for
this work was provided by the U.S. Department of Defense's Awards to
Stimulate and Support Undergraduate Research Education (ASSURE) program
in collaboration with the National Science Foundation's Research
Experiences for Undergraduates program. For the Easter Island
expedition, we thank Jonathan Kern of the Carnegie Observatories, Nikon
Professional Services, Williams College's Equipment Loan Office/James
Lillie, and the Photographic Department of the National Geographic
Society for providing equipment. For the Tatakoto expedition, we thank
ASTELCO Systems GmbH (Germany). J.M.P. thanks the Planetary Sciences
Department of the California Institute of Technology for hospitality
during the preparation of this paper. Support for D. B. S. and SWAP came
from PRODEX grant C90345 managed by the European Space Agency in
collaboration with the Belgian Federal Science Policy Office (BELSPO) in
support of the PROBA2/SWAP mission, and from the European Commission's
Seventh Framework Programme (FP7/2007-2013) under the grant agreement
no. 218816 (SOTERIA project, www.soteria-space.eu). SWAP is a project of
the Centre Spatial de Liege and the Royal Observatory of Belgium funded
by BELSPO. A. E. and L. G. were supported by a contract from Lockheed
Martin. We thank the referee, Y.-M. Wang of NRL, for valuable comments
and for providing the PFSS figure.
NR 38
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U1 0
U2 4
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2011
VL 734
IS 2
AR 114
DI 10.1088/0004-637X/734/2/114
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 774LD
UT WOS:000291386500042
ER
PT J
AU Pei, NC
Lian, JY
Erickson, DL
Swenson, NG
Kress, WJ
Ye, WH
Ge, XJ
AF Pei, Nancai
Lian, Ju-Yu
Erickson, David L.
Swenson, Nathan G.
Kress, W. John
Ye, Wan-Hui
Ge, Xue-Jun
TI Exploring Tree-Habitat Associations in a Chinese Subtropical Forest Plot
Using a Molecular Phylogeny Generated from DNA Barcode Loci
SO PLOS ONE
LA English
DT Article
ID COMMUNITY ECOLOGY; SPATIAL DISTRIBUTIONS; DIVERSITY; OVERDISPERSION;
BIODIVERSITY; PATTERNS; TRAIT; SCALE; SIZE
AB Elucidating the ecological mechanisms underlying community assembly in subtropical forests remains a central challenge for ecologists. The assembly of species into communities can be due to interspecific differences in habitat associations, and there is increasing evidence that these associations may have an underlying phylogenetic structure in contemporary terrestrial communities. In other words, by examining the degree to which closely related species prefer similar habitats and the degree to which they co-occur, ecologists are able to infer the mechanisms underlying community assembly. Here we implement this approach in a diverse subtropical tree community in China using a long-term forest dynamics plot and a molecular phylogeny generated from three DNA barcode loci. We find that there is phylogenetic signal in plant-habitat associations (i.e. closely related species tend to prefer similar habitats) and that patterns of co-occurrence within habitats are typically non-random with respect to phylogeny. In particular, we found phylogenetic clustering in valley and low-slope habitats in this forest, indicating a filtering of lineages plays a dominant role in structuring communities in these habitats and we found evidence of phylogenetic overdispersion in high-slope, ridge-top and high-gully habitats, indicating that distantly related species tended to co-occur in these high elevation habitats and that lineage filtering is less important in structuring these communities. Thus we infer that non-neutral niche-based processes acting upon evolutionarily conserved habitat preferences explain the assembly of local scale communities in the forest studied.
C1 [Pei, Nancai; Lian, Ju-Yu; Ye, Wan-Hui; Ge, Xue-Jun] Chinese Acad Sci, S China Bot Garden, Key Lab Plant Resource Conservat & Sustainable Ut, Guangzhou, Guangdong, Peoples R China.
[Pei, Nancai] Chinese Acad Sci, Grad Univ, Beijing, Peoples R China.
[Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA.
[Swenson, Nathan G.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA.
RP Pei, NC (reprint author), Chinese Acad Sci, S China Bot Garden, Key Lab Plant Resource Conservat & Sustainable Ut, Guangzhou, Guangdong, Peoples R China.
EM why@scbg.ac.cn; xjge@scbg.ac.cn
RI Swenson, Nathan/A-3514-2012
OI Swenson, Nathan/0000-0003-3819-9767
FU National Basic Research Program of China (973 Program) [2007CB411600];
China National Program for R & D Infrastructure and Facility Development
[2008BAC39B02]; Chinese Academy of Sciences [2009-LSF-GBOWS-01,
KSCX2-YW-N-0807, KZCX2-YW-430]
FX This study was financially supported by National Basic Research Program
of China (973 Program) (2007CB411600), China National Program for R & D
Infrastructure and Facility Development (2008BAC39B02), the Research
Fund for the Large-Scale Scientific Facilities of the Chinese Academy of
Sciences (2009-LSF-GBOWS-01), Major Innovation Program of CAS
(KSCX2-YW-N-0807) and Key Innovation Project of CAS (KZCX2-YW-430). The
funders had no role in study design, data collection and analysis,
decision to publish, or preparation of the manuscript.
NR 41
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Z9 44
U1 6
U2 40
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUN 20
PY 2011
VL 6
IS 6
AR e21273
DI 10.1371/journal.pone.0021273
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 782BY
UT WOS:000291983800037
PM 21701680
ER
PT J
AU Hagedorn, M
Carter, VL
AF Hagedorn, Mary
Carter, Virginia L.
TI Zebrafish Reproduction: Revisiting In Vitro Fertilization to Increase
Sperm Cryopreservation Success
SO PLOS ONE
LA English
DT Article
ID SWORDTAIL XIPHOPHORUS-HELLERI; REFRIGERATED STORAGE; HIGH-THROUGHPUT;
DANIO-RERIO; FISH; SPERMATOZOA; DILUTION; OOCYTES; EGGS; DRUM
AB Although conventional cryopreservation is a proven method for long-term, safe storage of genetic material, protocols used by the zebrafish community are not standardized and yield inconsistent results, thereby putting the security of many genotypes in individual laboratories and stock centers at risk. An important challenge for a successful zebrafish sperm cryopreservation program is the large variability in the post-thaw in vitro fertilization success (0 to 80%). But how much of this variability was due to the reproductive traits of the in vitro fertilization process, and not due to the cryopreservation process? These experiments only assessed the in vitro process with fresh sperm, but yielded the basic metrics needed for successful in vitro fertilization using cryopreserved sperm, as well. We analyzed the reproductive traits for zebrafish males with a strict body condition range. It did not correlate with sperm volume, or motility (P > 0.05), but it did correlate with sperm concentration. Younger males produced more concentrated sperm (P < 0.05). To minimize the wastage of sperm during the in vitro fertilization process, 10 6 cells/ml was the minimum sperm concentration needed to achieve an in vitro fertilization success of >= 70%. During the in vitro process, pooling sperm did not reduce fertilization success (P > 0.05), but pooling eggs reduced it by approximately 30 to 50% (P < 0.05). This reduction in fertilization success was due not to the pooling of the females' eggs, but to the type of tools used to handle the eggs. Recommendations to enhance the in vitro process for zebrafish include: 1) using males of a body condition closer to 1.5 for maximal sperm concentration; 2) minimizing sperm wastage by using a working sperm concentration of 10(6) motile cells/ml for in vitro fertilization; and 3) never using metal or sharp-edged tools to handle eggs prior to fertilization.
C1 [Hagedorn, Mary; Carter, Virginia L.] Smithsonian Conservat Biol Inst, Washington, DC USA.
[Hagedorn, Mary; Carter, Virginia L.] Univ Hawaii, Hawaii Inst Marine Biol, Kaneohe, HI USA.
RP Hagedorn, M (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Natl Zool Pk, Washington, DC USA.
EM hagedornm@si.edu
FU National Institutes of Health, National Center for Research Resources
[5R24RR023998]
FX This work was supported by the National Institutes of Health, National
Center for Research Resources (Grant # 5R24RR023998). The funders had no
role in study design, data collection and analysis, decision to publish,
or preparation of the manuscript.
NR 25
TC 7
Z9 7
U1 1
U2 23
PU PUBLIC LIBRARY SCIENCE
PI SAN FRANCISCO
PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA
SN 1932-6203
J9 PLOS ONE
JI PLoS One
PD JUN 16
PY 2011
VL 6
IS 6
AR e21059
DI 10.1371/journal.pone.0021059
PG 9
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 778UW
UT WOS:000291734100048
PM 21698162
ER
PT J
AU Vikhlinin, A
AF Vikhlinin, Alexey
TI ASTROPHYSICS Early black holes uncovered
SO NATURE
LA English
DT Editorial Material
ID QUASARS
C1 Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA 02138 USA.
RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, Div High Energy Astrophys, Cambridge, MA 02138 USA.
EM avikhlinin@cfa.harvard.edu
NR 8
TC 1
Z9 1
U1 0
U2 0
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUN 16
PY 2011
VL 474
IS 7351
BP 293
EP 294
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 777TD
UT WOS:000291647100031
PM 21677743
ER
PT J
AU Ferreira, PSF
Henry, TJ
AF Fiuza Ferreira, Paulo Sergio
Henry, Thomas J.
TI Synopsis and keys to the tribes, genera, and species of Miridae
(Hemiptera: Heteroptera) of Minas Gerais, Brazil Part I: Bryocorinae
SO ZOOTAXA
LA English
DT Article
DE Hemiptera; Heteroptera; Miridae; Bryocorinae; Brazil; Minas Gerais;
diagnoses; distribution; host plants; keys
ID INSECT ORDER HETEROPTERA; NEOTROPICAL MIRIDAE; JANUARY 1985;
DEPOSITORIES; PLANT
AB This paper begins a series of synoptic taxonomic treatments on the Miridae known from Minas Gerais, Brazil, by subfamily, beginning with the Bryocorinae. We provide diagnoses, host-plant information, distribution data, and illustrated keys to four tribes, 24 genera, and 56 species. For most species, illustrations of the adults, selected morphological characters, and male genitalia are provided to facilitate identification.
C1 [Fiuza Ferreira, Paulo Sergio] Univ Fed Vicosa, Dept Biol Anim, Museu Entomol, BR-36570000 Vicosa, MG, Brazil.
[Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA.
RP Ferreira, PSF (reprint author), Univ Fed Vicosa, Dept Biol Anim, Museu Entomol, BR-36570000 Vicosa, MG, Brazil.
EM pfiuza@ufv.br; thomas.henry@ars.usda.gov
FU FAPEMIG [CBS 288/97]
FX We thank Jose Lino Neto (Department of General Biology, Federal
University of Vicosa, MG, Brazil) for his photographs (Figs. 4, 14, 26,
35, 48), Evaldo Martins Pires (graduate student) for his dorsal habitus
illustration (Fig. 45), Livia Aguiar Coelho (graduate student) for the
useful suggestions (Department of Animal Biology, Federal University of
Vicosa, MG, Brazil). The following editors kindly gave permission to
reproduce figures previously published in their journals (citations for
each are given in the figure captions): Sionei R. Bonatto (Revista
Brazileira de Zoologia [now Zoologia (An International Journal of
Zoology)]); Alexander W. A. Kellner (Anais da Academia Brasileira de
Ciencias); Wanda I. Lugo (University of Puerto Rico, Agricultural
Experiment Station Technical Paper series); Raisla Magalhaes (Revista
Ceres); and Takako Matsumura Tundisi (Revista Brasileira de Biologia
[now Brazilian Journal of Biology]). The first author (PSFF) is grateful
to FAPEMIG for funding Project CBS 288/97. Finally, we thank John W.
Brown (Systematic Entomology Laboratory [SEL], ARS, USDA, c/o USNM,
Washington, DC), Michael W. Gates (SEL), and M. D. Schwartz (Division of
Invertebrate Zoology, American Museum of Natural History, New York, NY)
for their constructive reviews of the manuscript.
NR 130
TC 6
Z9 7
U1 1
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 JUN 16
PY 2011
IS 2920
BP 1
EP 41
PG 41
WC Zoology
SC Zoology
GA 782FP
UT WOS:000291994200001
ER
PT J
AU D'Rozario, A
Labandeira, C
Guo, WY
Yao, YF
Li, CS
AF D'Rozario, Ashalata
Labandeira, Conrad
Guo, Wen-Yi
Yao, Yi-Feng
Li, Cheng-Sen
TI Spatiotemporal extension of the Euramerican Psaronius component
community to the Late Permian of Cathaysia: In situ coprolites in a P.
housuoensis stem from Yunnan Province, southwest China
SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY
LA English
DT Article
DE Coprolites; Psaronius housuoensis; Plant-arthropod association; Late
Permian; South China Block; Insect
ID PENNSYLVANIAN TREE FERNS; NORTH-CENTRAL TEXAS; PLANT ASSEMBLAGE; EARLY
HISTORY; ASSOCIATIONS; ARTHROPOD; USA; HOLOMETABOLA; HYMENOPTERA; FLORAS
AB We report well-preserved coprolites in the ground tissue of the permineralized stem of Psaronius housuoensis D'Rozario et al., from the Upper Permian deposits of Yunnan Province, southwest China. The distinctive coprolites are circular to oval in shape, ranging on average from 944 x 1190 mu m to 1065 x 1120 mu m, and contain histologically identifiable tracheids, parenchyma, gum sac cells, spores and fungal remains. Several lines of evidence indicate that this association was detritivorous, represented a pith boring, and was made by a diplopod or more likely an insect. This discovery extends the temporal duration of the food web of Psaronius plant-arthropod associations from the late Middle Pennsylvanian to now the Late Permian, and extends the biogeographic range from the equatorial wetlands of the Illinois, Northern Appalachian, and German Erzgebirge Basins of Euramerica to now the South China Block of Cathaysia. The Psaronius-arthropod-fungi component community is spatiotemporally the most persistent of documented Paleozoic associations in the fossil record. (C) 2011 Elsevier B.V. All rights reserved.
C1 [D'Rozario, Ashalata] Narasinha Dutt Coll, Dept Bot, Howrah 711101, India.
[Labandeira, Conrad] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
[Labandeira, Conrad] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
[Labandeira, Conrad] Univ Maryland, BEES Program, College Pk, MD 20742 USA.
[Guo, Wen-Yi; Yao, Yi-Feng; Li, Cheng-Sen] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China.
[Guo, Wen-Yi] 2 Xiamen Environm Protect Res Inst, Xiamen 361006, Peoples R China.
RP D'Rozario, A (reprint author), Narasinha Dutt Coll, Dept Bot, 129 Bellilious Rd, Howrah 711101, India.
EM ashalatandc@gmail.com
FU Chinese Academy of Sciences (CAS)-TWAS; academy of sciences for the
developing world at the State Key Laboratory of Systematic and
Evolutionary Botany, Institute of Botany, Chinese Academy of Sciences,
Beijing
FX This research work was supported by the Chinese Academy of Sciences
(CAS)-TWAS, the academy of sciences for the developing world Visiting
Scholar Fellowship award (2006, 2009) to ADR at the State Key Laboratory
of Systematic and Evolutionary Botany, Institute of Botany, Chinese
Academy of Sciences, Beijing. Thanks are due to Bin Sun and Finnegan
Marsh for preparing and formatting the images of the photographic plate.
The constructive suggestions and comments by three reviewers are
gratefully acknowledged. This is contribution 180 of the Evolution of
Terrestrial Ecosystems consortium at the National Museum of Natural
History, in Washington, DC.
NR 84
TC 22
Z9 22
U1 1
U2 5
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0031-0182
EI 1872-616X
J9 PALAEOGEOGR PALAEOCL
JI Paleogeogr. Paleoclimatol. Paleoecol.
PD JUN 15
PY 2011
VL 306
IS 3-4
BP 127
EP 133
DI 10.1016/j.palaeo.2011.04.009
PG 7
WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology
SC Physical Geography; Geology; Paleontology
GA 787XN
UT WOS:000292410100003
ER
PT J
AU Johnson, EG
Young, AC
Hines, AH
Kramer, MA
Bademan, M
Goodison, MR
Aguilar, R
AF Johnson, Eric G.
Young, Alicia C.
Hines, Anson H.
Kramer, Margaret A.
Bademan, Martha
Goodison, Michael R.
Aguilar, Robert
TI Field comparison of survival and growth of hatchery-reared versus wild
blue crabs, Callinectes sapidus Rathbun
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Blue crab; Callinectes sapidus; Growth; Restocking; Survival
ID LOBSTERS HOMARUS-GAMMARUS; SALT-MARSH NURSERIES; CHESAPEAKE-BAY; STOCK
ENHANCEMENT; RELEASE STRATEGIES; COASTAL FISHERIES; BEHAVIOR; REFUGE;
SIZE; RESTOCKING
AB The efficacy of restocking as a fisheries management tool depends upon the ability of hatchery-reared juveniles to survive, grow and reproduce in the wild following release. However, hatchery-reared animals may be maladapted to the natural environment as a result of morphological, physiological, or behavioral deficiencies acquired during the hatchery phase. To assess the competency of hatchery-reared blue crabs Callinectes sapidus Rathbun, a species under consideration for restocking in Chesapeake Bay, we compared survival and growth of hatchery-reared and wild juveniles using complementary field tethering experiments and small-scale field releases in shallow blue crab nursery habitats of the upper Chesapeake Bay. We observed no difference in the survival rates of hatchery-reared and wild crabs in either tethering experiments or paired field releases. Hatchery-reared and wild juveniles also exhibited similar growth rates and levels of growth variability. The results indicate that hatchery-reared juveniles are competent and likely not disadvantaged relative to wild conspecifics, and that poor performance of hatchery-reared individuals following release is not a significant barrier to restocking for this species in Chesapeake Bay. Further, our study highlights the potential utility of release experiments with hatchery-reared animals to provide key biological data for stock assessments and fishery management. (C) 2011 Elsevier B.V. All rights reserved.
C1 [Johnson, Eric G.; Young, Alicia C.; Hines, Anson H.; Kramer, Margaret A.; Bademan, Martha; Goodison, Michael R.; Aguilar, Robert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
[Bademan, Martha] Florida Fish & Wildlife Conservat Commiss, Div Marine Fisheries Management, Tallahassee, FL 32399 USA.
RP Johnson, EG (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM johnsoneg@si.edu
RI Aguilar, Robert/O-2480-2016
OI Aguilar, Robert/0000-0001-8732-5382
FU NOM Chesapeake Bay Office; Phillips Seafood, Inc.; Maryland Sea Grant
Program; Smithsonian Institution Women's Committee; Smithsoniain Marine
Science Network; Smithsonian Environmental Studies Program; Smithsonian
Environmental Research Center (SERC); U.S. Senator Barbara Mikulski from
Maryland
FX Funding for this research was provided by the NOM Chesapeake Bay Office,
Phillips Seafood, Inc., Maryland Sea Grant Program, the Smithsonian
Institution Women's Committee, the Smithsoniain Marine Science Network,
the Smithsonian Environmental Studies Program, and the Fellowship
Program of the Smithsonian Environmental Research Center (SERC). We
thank the numerous undergraduate student interns, summer technicians,
and volunteers that assisted with the field sampling and tagging
juvenile blue crabs. In particular, we thank Jana L. D. Davis for her
efforts and support of the project in the early years and for conducting
the field release in 2003, and Paige Roberts who has overseen the field
aspects and data management of the project since 2008. We also thank the
many researchers and technicians at COMB for raising the hatchery crabs
used in this study without whom this research would not be possible. We
are especially grateful to U.S. Senator Barbara Mikulski from Maryland
for her support of the Blue Crab Advanced Research Consortium. [RH]
NR 74
TC 4
Z9 4
U1 0
U2 25
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 JUN 15
PY 2011
VL 402
IS 1-2
BP 35
EP 42
DI 10.1016/j.jembe.2011.03.013
PG 8
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 774GY
UT WOS:000291374900005
ER
PT J
AU Kline, DI
Vollmer, SV
AF Kline, David I.
Vollmer, Steven V.
TI White Band Disease (type I) of Endangered Caribbean Acroporid Corals is
Caused by Pathogenic Bacteria
SO SCIENTIFIC REPORTS
LA English
DT Article
ID ELKHORN CORAL; INDO-PACIFIC; REEF CORALS; ASSOCIATION; CAUSATION;
MORTALITY; PALMATA; ENVIRONMENT; ECOSYSTEMS; HEALTHY
AB Diseases affecting coral reefs have increased exponentially over the last three decades and contributed to their decline, particularly in the Caribbean. In most cases, the responsible pathogens have not been isolated, often due to the difficulty in isolating and culturing marine bacteria. White Band Disease (WBD) has caused unprecedented declines in the Caribbean acroporid corals, resulting in their listings as threatened on the US Threatened and Endangered Species List and critically endangered on the IUCN Red List. Yet, despite the importance of WBD, the probable pathogen(s) have not yet been determined. Here we present in situ transmission data from a series of filtrate and antibiotic treatments of disease tissue that indicate that WBD is contagious and caused by bacterial pathogen(s). Additionally our data suggest that Ampicillin could be considered as a treatment for WBD (type I).
C1 [Kline, David I.] Univ Queensland, Coral Reef Ecosyst Lab, St Lucia, Qld 4072, Australia.
[Kline, David I.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia.
[Kline, David I.; Vollmer, Steven V.] Smithsonian Trop Res Inst, Balboa, Panama.
[Vollmer, Steven V.] Northeastern Univ, Ctr Marine Sci, Nahant, MA 01908 USA.
RP Kline, DI (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Scripps Photobiol Grp, 9500 Gilman Dr, La Jolla, CA 92093 USA.
EM dkline0@gmail.com
FU Smithsonian Marine Science Network
FX We thank the staff of the STRI Bocas del Toro research station and the
STRI research staff in Panama City for their assistance throughout our
research project. We also wish to thank Nancy Knowlton and Paul Muir for
critically reviewing and greatly improving this manuscript. This work
was funded by a Smithsonian Marine Science Network postdoctoral
fellowship to DIK & SVV. This is contribution #4 of the Caribbean Future
Reef Project.
NR 57
TC 18
Z9 18
U1 1
U2 29
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 2045-2322
J9 SCI REP-UK
JI Sci Rep
PD JUN 14
PY 2011
VL 1
AR 7
DI 10.1038/srep00007
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 835OR
UT WOS:000296046200007
PM 22355526
ER
PT J
AU Dame, TM
Thaddeus, P
AF Dame, T. M.
Thaddeus, P.
TI A MOLECULAR SPIRAL ARM IN THE FAR OUTER GALAXY
SO ASTROPHYSICAL JOURNAL LETTERS
LA English
DT Article
DE Galaxy: structure; ISM: molecules; radio lines: ISM
ID COMPLETE CO SURVEY; MILKY-WAY; VERTICAL STRUCTURE; CLOUDS; DISK; HI
AB We have identified a spiral arm lying beyond the Outer Arm in the first Galactic quadrant similar to 15 kpc from the Galactic center. After tracing the arm in existing 21 cm surveys, we searched for molecular gas using the CfA 1.2 m telescope and detected CO at 10 of 220 positions. The detections are distributed along the arm from l = 13 degrees, v = -21 km s(-1) to l = 55 degrees, v = -84 km s(-1) and coincide with most of the main Hi concentrations. One of the detections was fully mapped to reveal a large molecular cloud with a radius of 47 pc and a molecular mass of similar to 50,000 M(circle dot). At a mean distance of 21 kpc, the molecular gas in this arm is the most distant yet detected in the Milky Way. The new arm appears to be the continuation of the Scutum-Centaurus Arm in the outer Galaxy, as a symmetric counterpart of the nearby Perseus Arm.
C1 [Dame, T. M.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Dame, TM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM tdame@cfa.harvard.edu; pthaddeus@cfa.harvard.edu
NR 15
TC 43
Z9 43
U1 0
U2 5
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 2041-8205
J9 ASTROPHYS J LETT
JI Astrophys. J. Lett.
PD JUN 10
PY 2011
VL 734
IS 1
AR L24
DI 10.1088/2041-8205/734/1/L24
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 797NV
UT WOS:000293135500024
ER
EF