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).
NR 80
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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 AUG 1
PY 2011
VL 736
IS 2
AR 133
DI 10.1088/0004-637X/736/2/133
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795MD
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.
NR 74
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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 1
PY 2011
VL 736
IS 2
AR 129
DI 10.1088/0004-637X/736/2/129
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 795MD
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).
NR 85
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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 AUG 1
PY 2011
VL 736
IS 2
AR 146
DI 10.1088/0004-637X/736/2/146
PG 17
WC Astronomy & Astrophysics
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, al