FN Thomson Reuters Web of Science™
VR 1.0
PT J
AU Stauffer, JR
Jones, BF
Backman, D
Hartmann, LW
Navascues, DBY
Pinsonneault, MH
Terndrup, DM
Muench, AA
AF Stauffer, JR
Jones, BF
Backman, D
Hartmann, LW
Navascues, DBY
Pinsonneault, MH
Terndrup, DM
Muench, AA
TI Why are the K dwarfs in the Pleiades so blue?
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE open clusters and associations : individual (Pleiades); stars : low
mass, brown dwarfs
ID LOW-MASS STARS; PRE-MAIN-SEQUENCE; OPEN CLUSTER NGC-2516;
H-BETA-PHOTOMETRY; COLOR-MAGNITUDE DIAGRAMS; ALPHA-PERSEI CLUSTERS;
T-TAURI STARS; ROTATIONAL VELOCITIES; CHEMICAL-COMPOSITION; GALACTIC
CLUSTERS
AB The K dwarfs in the Pleiades fall nearly 1/2 mag below a main-sequence isochrone when plotted in a color-magnitude diagram utilizing V magnitude as the luminosity index and B-V as the color index. This peculiarity has been known for 40 years but has gone unexplained and mostly ignored. When compared to Praesepe members, the Pleiades K dwarfs again are subluminous (or blue) in a color-magnitude diagram using B-V as the color index. However, using V-I as the color index, stars in the two clusters are coincident to M(V) similar to 10; using V-K as the color index, Pleiades late K and M stars fall above the main-sequence locus defined by Praesepe members. We believe that the anomalous spectral energy distributions for the Pleiades K dwarfs, as compared to older clusters, are a consequence of rapid stellar rotation and may be primarily due to spottedness. If so, the required areal filling factor for the cool component has to be very large (greater than or equal to50%). Weak-lined T Tauri stars have similar color anomalies, and we suspect that this is a common feature of all very young K dwarfs (spectral type >K3). The peculiar spectral energy distribution needs to be considered in deriving accurate pre-main-sequence isochrone-fitting ages for clusters like the Pleiades, since the age derived will depend on the temperature index used.
C1 CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA.
Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA.
Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
Lab Astrofis Espacial & Fis Fundamental, Madrid 28080, Spain.
Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
RP Stauffer, JR (reprint author), CALTECH, SIRTF Sci Ctr, Mail Code 314-6,1200 E Calif Blvd, Pasadena, CA 91125 USA.
RI Barrado Navascues, David/C-1439-2017
OI Barrado Navascues, David/0000-0002-5971-9242
NR 85
TC 73
Z9 73
U1 0
U2 1
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 AUG
PY 2003
VL 126
IS 2
BP 833
EP 847
DI 10.1086/376739
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706GU
UT WOS:000184446600019
ER
PT J
AU Cohen, M
Wheaton, WA
Megeath, ST
AF Cohen, M
Wheaton, WA
Megeath, ST
TI Spectral irradiance calibration in the infrared. XIV. The absolute
calibration of 2MASS
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared radiation; surveys
ID STARS
AB Element by element, we have combined the optical components in the three cameras of the Two Micron All Sky Survey (2MASS), and incorporated detector quantum efficiency curves and site-specific atmospheric transmissions, to create three relative spectral response curves (RSRs). We provide the absolute 2MASS attributes associated with "zero magnitude'' in the JHKs bands so that these RSRs may be used for synthetic photometry. The RSRs tie 2MASS to the "Cohen-Walker-Witteborn'' framework of absolute photometry and stellar spectra for the purpose of using 2MASS data to support the development of absolute calibrators for the Infrared Array Camera and pairwise cross-calibrators between all three SIRTF instruments. We examine the robustness of these RSRs to changes in water vapor within a night. We compare the observed 2MASS magnitudes of 33 stars ( converted from the precision optical calibrators of Landolt and Carter-Meadows into absolute infrared calibrators from 1.2 to 35 mum) with our predictions, thereby deriving 2MASS "zero-point offsets'' from the ensemble. These offsets are the final ingredients essential to merge 2MASS JHKs data with our other absolutely calibrated bands and stellar spectra, and to support the creation of faint calibration stars for SIRTF.
C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Cohen, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA.
NR 11
TC 433
Z9 435
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD AUG
PY 2003
VL 126
IS 2
BP 1090
EP 1096
DI 10.1086/376474
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 706GU
UT WOS:000184446600038
ER
PT J
AU Rodriguez, J
Tomsick, JA
Foschini, L
Walter, R
Goldwurm, A
Corbel, S
Kaaret, P
AF Rodriguez, J
Tomsick, JA
Foschini, L
Walter, R
Goldwurm, A
Corbel, S
Kaaret, P
TI An XMM-Newton observation of IGR J16320-4751 = AX J1631.9-4752
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion disk; stars : individual : IGR J16320-4751; X-rays
: binaries; X-rays : general
ID PHOTON IMAGING CAMERA; X-RAY-SPECTRA; NEUTRON-STARS; NOVAE
AB The hard X-ray sensitivity and arcminute position accuracy of the recently launched International Gamma-Ray Laboratory (INTEGRAL) has lead to the (re-)discovery of a class of heavily absorbed hard X-ray sources lying in the Galactic plane. We report on the analysis of an XMM observation of such a source IGR J16320-4751 = AX J1631.9-4752. Our analysis allowed us to obtain the most accurate X-ray position to date (Rodriguez et al. 2003), and to identify a likely infrared counterpart (Tomsick et al. 2003). We present the detailed analysis of the IGR J16320-4751 XMM spectra. The PN spectrum can be well represented by a single powerlaw or a comptonized spectrum with a high equivalent absorption column density of similar to2 x 10(23) cm(-2). The current analysis and the comparison with the properties of other sources favor the possibility that the source is a Galactic X-Ray Binary (XRB). The identification of two candidate IR counterparts is in good agreement with this identification. The hard spectrum previously seen with ASCA, and the brightness of the candidate counterparts indicate that IGR J16320-4751 is most probably a highly absorbed High Mass X-ray Binary, hosting a neutron star.
C1 CEA Saclay, DSM DAPNIA SAp, CNRS, FRE 2591, F-91191 Gif Sur Yvette, France.
Integral Sci Data Ctr, CH-1290 Versoix, Switzerland.
Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
IASF CNR, Sez Bologna, I-40129 Bologna, Italy.
Univ Paris 07, Federat APC, F-75251 Paris 05, France.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Rodriguez, J (reprint author), CEA Saclay, DSM DAPNIA SAp, CNRS, FRE 2591, F-91191 Gif Sur Yvette, France.
RI Foschini, Luigi/H-3833-2012
OI Foschini, Luigi/0000-0001-8678-0324
NR 25
TC 45
Z9 45
U1 0
U2 1
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2003
VL 407
IS 2
BP L41
EP L45
DI 10.1051/0004-6361:20031093
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 708CV
UT WOS:000184550300006
ER
PT J
AU Boonman, AMS
Doty, SD
van Dishoeck, EF
Bergin, EA
Melnick, GJ
Wright, CM
Stark, R
AF Boonman, AMS
Doty, SD
van Dishoeck, EF
Bergin, EA
Melnick, GJ
Wright, CM
Stark, R
TI Modeling gas-phase H2O between 5 mu m and 540 mu m toward massive
protostars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM : abundances; ISM : molecules; infrared : ISM; ISM : lines and
bands; molecular processes
ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; MAGNETOHYDRODYNAMIC
SHOCK-WAVES; MOLECULAR CLOUD CORES; ISO-SWS OBSERVATIONS; WATER-VAPOR;
ABSORPTION FEATURES; ASTRONOMY-SATELLITE; INTERSTELLAR WATER;
RADIATIVE-TRANSFER
AB We present models and observations of gas-phase H2O lines between 5 and 540 mum toward deeply embedded massive protostars, involving both pure rotational and ro-vibrational transitions. The data have been obtained for 6 sources with both the Short and Long Wavelength Spectrometers (SWS and LWS) on board the Infrared Space Observatory (ISO) and with the Submillimeter Wave Astronomy Satellite (SWAS). For comparison, CO J = 7-6 spectra have been observed with the MPIfR/SRON 800 GHz heterodyne spectrometer at the James Clerk Maxwell Telescope (JCMT). A radiative transfer model in combination with different physical/chemical scenarios has been used to model these H2O lines for 4 sources to probe the chemical structure of these massive protostars. The results indicate that pure gas-phase production of H2O cannot explain the observed spectra. Ice evaporation in the warm inner envelope and freeze-out in the cold outer part are important for most of our sources and occur at T similar to 90-110 K. The ISO-SWS data are particularly sensitive to ice evaporation in the inner part whereas the ISO-LWS data are good diagnostics of freeze-out in the outer region. The modeling suggests that the 557 GHz SWAS line includes contributions from both the cold and the warm H2O gas. The SWAS line profiles indicate that for some of the sources a fraction of up to 50% of the total flux may originate in the outflow. Shocks do not seem to contribute significantly to the observed emission in other H2O lines, however, in contrast with the case for Orion. The results show that three of the observed and modeled H2O lines, the 3(03)-2(12), 2(12)-1(01), and 1(10)-1(01) lines, are good candidates to observe with the Herschel Space Observatory in order to further investigate the physical and chemical conditions in massive star-forming regions.
C1 Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Boonman, AMS (reprint author), Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands.
NR 58
TC 47
Z9 47
U1 0
U2 2
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2003
VL 406
IS 3
BP 937
EP 955
DI 10.1051/0004-6361:20030765
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704BL
UT WOS:000184317800018
ER
PT J
AU Hempelmann, A
Schmitt, JHMM
Baliunas, SL
Donahue, RA
AF Hempelmann, A
Schmitt, JHMM
Baliunas, SL
Donahue, RA
TI Evidence for coronal activity cycles on 61 Cygni A and B
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars : late-type; stars : activity; stars : coronae; stars :
chromospheres
ID X-RAY-EMISSION; MAIN-SEQUENCE STARS; CHROMOSPHERIC VARIATIONS
AB We investigate a four-and-one-half year time-series of ROSAT HRI pointed observations of 61 Cyg A and B and compare the X-ray light curves with the chromospheric Ca HK variability. The ROSAT sampling rate was two pointings per year and typical errors lie in the range of 5-10%. The chromospheric cycles are well-known for both stars from the Mt. Wilson Ca HK survey. Although the time basis of our ROSAT observations is shorter than the 7-and 12-year cycles of components A and B, respectively, we find the long-term trend of coronal activity in close correlation with the chromospheric activity during the observation period, between 1993 and 1998. The chromospheric activity increased through maximum activity down to a minimum for component A, and from maximum to minimum activity for component B. The same behaviour is observed for the X-ray light curves but with much higher amplitudes by factors 2.5-3. The remaining scatter observed around low-order regression curves of coronal activity is small. We conclude that both stars do show coronal cycles and that coronal cycles are the dominant source of variability for 61 Cygni.
C1 Univ Hamburg, D-21029 Hamburg, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hempelmann, A (reprint author), Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany.
NR 12
TC 13
Z9 14
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD AUG
PY 2003
VL 406
IS 2
BP L39
EP L42
DI 10.1051/0004-6361:20030882
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 702KC
UT WOS:000184222200003
ER
PT J
AU Yoshida, N
Abel, T
Hernquist, L
Sugiyama, N
AF Yoshida, N
Abel, T
Hernquist, L
Sugiyama, N
TI Simulations of early structure formation: Primordial gas clouds
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology : theory; early universe; galaxies : formation; stars :
formation
ID COLD DARK-MATTER; POPULATION-III STARS; PARTICLE HYDRODYNAMICS
SIMULATIONS; FIRST COSMOLOGICAL OBJECTS; 1ST STARS; RADIATIVE FEEDBACK;
ANGULAR-MOMENTUM; GALAXY FORMATION; HIGH-REDSHIFT; MASS FUNCTION
AB We use cosmological simulations to study the origin of primordial star-forming clouds in a LambdaCDM universe, by following the formation of dark matter halos and the cooling of gas within them. To model the physics of chemically pristine gas, we employ a nonequilibrium treatment of the chemistry of nine species (e(-), H, H(+), He, He(+), He(++), H(2), H(2)(+), H(-)) and include cooling by molecular hydrogen. By considering cosmological volumes, we are able to study the statistical properties of primordial halos, and the high resolution of our simulations enables us to examine these objects in detail. In particular, we explore the hierarchical growth of bound structures forming at redshifts z approximate to 25-30 with total masses in the range approximate to10(5)-10(6) M(.). We find that when the amount of molecular hydrogen in these objects reaches a critical level, cooling by rotational line emission is efficient, and dense clumps of cold gas form. We identify these "gas clouds'' as sites for primordial star formation. In our simulations, the threshold for gas cloud formation by molecular cooling corresponds to a critical halo mass of approximate to5 x 10(5) h(-1) M(.), in agreement with earlier estimates, but with a weak dependence on redshift in the range z > 16. The complex interplay between the gravitational formation of dark halos and the thermodynamic and chemical evolution of the gas clouds compromises analytic estimates of the critical H(2) fraction. Dynamical heating from mass accretion and mergers opposes relatively inefficient cooling by molecular hydrogen, delaying the production of star-forming clouds in rapidly growing halos. We also investigate the effect of photodissociating ultraviolet radiation on the formation of primordial gas clouds. We consider two extreme cases, first by including a uniform radiation field in the optically thin limit and second by accounting for the maximum effect of gas self-shielding in virialized regions. For radiation with Lyman-Werner band flux J > 10(-23) ergs s(-1) cm(-2) Hz(-1) sr(-1), hydrogen molecules are rapidly dissociated, rendering gas cooling inefficient. In both the cases we consider, the overall effect can be described by computing an equilibrium H(2) abundance for the radiation flux and defining an effective shielding factor. Based on our numerical results, we develop a semianalytic model of the formation of the first stars and demonstrate how it can be coupled with large N-body simulations to predict the star formation rate in the early universe.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA.
Natl Astron Observ Japan, Tokyo 1818588, Japan.
RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Yoshida, Naoki/A-4305-2011
NR 66
TC 337
Z9 338
U1 3
U2 7
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 645
EP 663
DI 10.1086/375810
PN 1
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100001
ER
PT J
AU Aldcroft, TL
Green, PJ
AF Aldcroft, TL
Green, PJ
TI Lens or binary? Chandra observations of the wide-separation broad
absorption line quasar pair UM 425
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing; quasars : absorption lines; quasars : individual
(UM Q2345, 425+007); X-rays : general
ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; EARLY DATA RELEASE;
X-RAY-EMISSION; STELLAR OBJECTS; ULTRAVIOLET-ABSORPTION; INTRACLUSTER
MEDIUM; OPTICAL-PROPERTIES; CANDIDATE UM-425; TIME-DELAY
AB We have obtained a 110 ks Chandra ACIS-S exposure of UM 425, a pair of QSOs at z = 1.47 separated by 6."5, which show remarkably similar emission and broad absorption line (BAL) profiles in the optical/UV. Our 5000 count X-ray spectrum of UM 425A ( the brighter component) is well fitted with a power law (photon spectral index Gamma = 2.0) partially covered by a hydrogen column of 3.8 x 10(22) cm(-2). The underlying power-law slope for this object and for other recent samples of BALQSOs is typical of radio-quiet quasars, lending credence to the hypothesis that BALs exist in every quasar. Assuming the same Gamma for the much fainter image of UM 425B, we detect an obscuring column 5 times larger. We search for evidence of an appropriately large lensing mass in our Chandra image and find weak diffuse emission near the quasar pair, with an X-ray flux typical of a group of galaxies at redshift z similar to 0.6. From our analysis of archival HST WFPC2 and NICMOS images, we find no evidence for a luminous lensing galaxy, but note a 3 sigma excess of galaxies in the UM 425 field with plausible magnitudes for a z = 0.6 galaxy group. However, the associated X-ray emission does not imply sufficient mass to produce the observed image splitting. The lens scenario thus requires a dark (high M/L ratio) lens or a fortuitous configuration of masses along the line of sight. UM425 may instead be a close binary pair of BALQSOs, which would boost arguments that interactions and mergers increase nuclear activity and outflows.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Aldcroft, TL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 72
TC 13
Z9 13
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 710
EP 720
DI 10.1086/375863
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100006
ER
PT J
AU Gilli, R
Cimatti, A
Daddi, E
Hasinger, G
Rosati, P
Szokoly, G
Tozzi, P
Bergeron, J
Borgani, S
Giacconi, R
Kewley, L
Mainieri, V
Mignoli, M
Nonino, M
Norman, C
Wang, J
Zamorani, G
Zheng, W
Zirm, A
AF Gilli, R
Cimatti, A
Daddi, E
Hasinger, G
Rosati, P
Szokoly, G
Tozzi, P
Bergeron, J
Borgani, S
Giacconi, R
Kewley, L
Mainieri, V
Mignoli, M
Nonino, M
Norman, C
Wang, J
Zamorani, G
Zheng, W
Zirm, A
TI Tracing the large-scale structure in the Chandra Deep Field South
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : clusters : general; galaxies : high-redshift; large-scale
structure of universe; X-rays : general
ID ACTIVE GALACTIC NUCLEI; ESO IMAGING SURVEY; X-RAY; REDSHIFT SURVEY;
ANGULAR-CORRELATION; SOURCE CATALOG; OPTICAL SURVEY; QSOS; GALAXIES;
EVOLUTION
AB We report the discovery of large-scale structures of X-ray sources in the 1 Ms observation of the Chandra Deep Field South. Two main structures appear as narrow (Deltaz less than or similar to 0.02) spikes in the source redshift distribution at z = 0.67 and 0.73, respectively. Their angular distribution spans a region at least similar to17' wide, corresponding to a physical size of 7.3 h(70)(-1) Mpc at a redshift of z 0.7 (Omega(m) = 0.3, Omega(Lambda) = 0.7). These spikes are populated by 19 sources each, which are mainly identified as active galactic nuclei (AGNs). Two sources in each spike are extended in X-rays, corresponding to galaxy groups/clusters embedded in larger structures. The X-ray source redshift distribution shows other spikes, the most remarkable at z = 1.04, 1.62, and 2.57. This is one of the first evidences for large-scale structure traced by X-ray sources and for spatial clustering of X-ray-selected AGNs. The X-ray data have been complemented with the spectroscopic data from the K20 near-infrared survey (Cimatti et al.), which covers similar to1/10 of the X-ray field. In this survey, too, the source redshift distribution shows several spikes. Two narrow structures at z = 0.67 and 0.73 (again with Deltaz similar to 0.02) are the most significant features, containing 24 and 47 galaxies, respectively. While the K20 structure at z = 0.73 is dominated by a standard galaxy cluster with a significant concentration around a central cD galaxy and morphological segregation, the galaxies at z = 0.67 constitute a loose structure rather uniformly distributed along the K20 field. Moreover, we find a very good correlation (almost one-to-one) between less prominent peaks detected in the redshift distributions of X-ray and K20 sources. In particular, at z < 1.3 we find that five out of the six more significant K20 peaks have a corresponding peak in the X-ray-selected sources and, similarly, all five X-ray peaks below that redshift have a corresponding K20 peak. Since the K20 survey sensitivity drops beyond z &SIM; 1.3, structures at higher redshift are traced only by the X-ray sources. This correlation suggests that AGNs ( from the X-ray data) and (early-type) galaxies ( from the K20 survey) are tracing the same underlying structures. We also compared the X-ray and K-band catalogs to search for enhanced X-ray activity in the sources in the two main redshift spikes. While in the structure at z = 0.73 the fraction of X-ray sources is the same as in the field, in the structure at z = 0.67 it is higher by a factor of &SIM;2, suggesting that X-ray activity may be triggered preferentially in the structure at z = 0.67. Given the limited statistics, this result is significant only at the &SIM;2σ level.
C1 INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
Johns Hopkins Univ, Baltimore, MD 21218 USA.
European So Observ, D-85748 Garching, Germany.
Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy.
CNRS, Inst Astrophys Paris, F-75014 Paris, France.
Univ Trieste, Dipartimento Astron, Ist Nazl Fis Nucl, I-34131 Trieste, Italy.
Associated Univ Inc, Washington, DC 20036 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Gilli, R (reprint author), INAF, Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy.
RI Daddi, Emanuele/D-1649-2012; Mignoli, Marco/O-9426-2015; Gilli,
Roberto/P-1110-2015;
OI Daddi, Emanuele/0000-0002-3331-9590; Mignoli, Marco/0000-0002-9087-2835;
Gilli, Roberto/0000-0001-8121-6177; Nonino, Mario/0000-0001-6342-9662;
Borgani, Stefano/0000-0001-6151-6439; Zamorani,
Giovanni/0000-0002-2318-301X
NR 29
TC 124
Z9 124
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 721
EP 727
DI 10.1086/375777
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100007
ER
PT J
AU Steidel, CC
Adelberger, KL
Shapley, AE
Pettini, M
Dickinson, M
Giavalisco, M
AF Steidel, CC
Adelberger, KL
Shapley, AE
Pettini, M
Dickinson, M
Giavalisco, M
TI Lyman break galaxies at redshift z similar to 3: Survey description and
full data set
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE catalogs; galaxies : evolution; galaxies : high-redshift
ID HUBBLE DEEP FIELD; RESOLUTION IMAGING SPECTROMETER; RADIO-QUIET GALAXY;
C-IV ABSORPTION; STAR-FORMATION; PRIMEVAL GALAXIES; QSO FIELDS;
ULTRAVIOLET LUMINOSITY; KECK SPECTROSCOPY; MS 1512-CB58
AB We present the basic data for a large ground-based spectroscopic survey for z similar to 3 Lyman break galaxies (LBGs), photometrically selected using rest-UV colors from very deep images in 17 high Galactic latitude fields. The total survey covers an area of 0.38 deg(2) and includes 2347 photometrically selected candidate LBGs to an apparent R-AB magnitude limit of 25.5. Approximately half of these objects have been observed spectroscopically using the Keck telescopes, yielding 940 redshifts with (z) = 2.96 +/- 0.29. We discuss the images, photometry, target selection, and spectroscopic program in some detail and present catalogs of the photometric and spectroscopic data, made available in electronic form. We discuss the general utility of conducting nearly volume-limited redshift surveys in prescribed redshift intervals using judicious application of photometric preselection.
C1 CALTECH, Pasadena, CA 91125 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP CALTECH, MS 105-24, Pasadena, CA 91125 USA.
NR 73
TC 526
Z9 527
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 728
EP 754
DI 10.1086/375772
PN 1
PG 27
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100008
ER
PT J
AU Di Stefano, R
Kong, AKH
AF Di Stefano, R
Kong, AKH
TI Luminous supersoft X-ray sources in external galaxies
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (M51, M83, M101, NGC 4697); methods : data
analysis; supernova remnants; white dwarfs; X-rays : binaries; X-rays :
galaxies
ID CHANDRA; DISCOVERY; EMISSION; NUCLEUS; M101; POPULATION; DISTANCES;
M-83; MASS
AB We use a set of conservative criteria to identify luminous supersoft X-ray sources (SSSs) in external galaxies. We test this approach on blackbody models and then apply it to Chandra data from four galaxies: an elliptical galaxy (NGC 4967), two face-on spiral galaxies (M101 and M83), and an interacting galaxy (M51). We find SSSs in every galaxy and estimate that the total SSS population of sources with L > 10(37) ergs s(-1) in each galaxy is at least several hundred and could be significantly larger. In addition, we discover two intriguing features of galactic populations of SSSs. First, there are significant subpopulations of high-luminosity sources; the bolometric luminosities can exceed 10(39) ergs s(-1). Second, in the spiral galaxies M101, M83, and M51, SSSs appear to be associated with the spiral arms. This may indicate that some SSSs are young systems, possibly younger than 10(8) yr.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 29
TC 64
Z9 64
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 884
EP 899
DI 10.1086/375858
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100017
ER
PT J
AU De Pasquale, M
Piro, L
Perna, R
Costa, E
Feroci, M
Gandolfi, G
In't Zand, J
Nicastro, L
Frontera, F
Antonelli, LA
Fiore, F
Stratta, G
AF De Pasquale, M
Piro, L
Perna, R
Costa, E
Feroci, M
Gandolfi, G
In't Zand, J
Nicastro, L
Frontera, F
Antonelli, LA
Fiore, F
Stratta, G
TI A comparative study of the X-ray afterglow properties of optically
bright and dark gamma-ray bursts
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays : bursts
ID HOST GALAXY; UNIVERSE; DUST; REIONIZATION; DESTRUCTION; COUNTERPART;
GRB-970828; EMISSION; LINE
AB We have examined the complete set of X-ray afterglow observations of dark and optically bright gamma-ray bursts (GRBs) performed by BeppoSAX through 2001 February. X-ray afterglows are detected in similar to90% of the cases. We do not find significant differences in the X-ray spectral shape, in particular no increased X-ray absorption in GRBs without optical transient (dark GRBs) compared to GRBs with optical transient (OTGRBs). Rather, we find that the 1.6-10 keV flux of OTGRBs is on average about 5 times larger than that of the dark GRBs. A Kolmogorov-Smirnov test shows that this difference is significant at 99.8% probability. Under the assumption that dark and OTGRBs have similar spectra, this could suggest that the first are uncaught in the optical band because they are just faint sources. In order to test this hypothesis, we have determined the optical-to-X-ray flux ratios of the sample. OTGRBs show a remarkably narrow distribution of flux ratios, which corresponds to an average optical-to-X-ray spectral index (α) over bar (OT)(ox) = 0.794 +/- 0.054. We find that, while 75% of dark GRBs have flux ratio upper limits still consistent with those of OT GRBs, the remaining 25% are 4-10 times weaker in optical than in X-rays. The significance of this result is greater than or equal to2.6 sigma. If this subpopulation of dark GRBs were constituted by objects assimilable to OTGRBs, they should have shown optical fluxes higher than upper limits actually found. We discuss the possible causes of their behavior, including a possible occurrence in high-density clouds or origin at very high redshift and a connection with ancient, Population III stars.
C1 CNR, IASF, I-00133 Rome, Italy.
Univ Roma La Sapienza, I-00185 Rome, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Space Res Org Netherlands, NL-3584 CA Utrecht, Netherlands.
CNR, IASF, I-90146 Palermo, Italy.
CNR, IASF, I-40129 Bologna, Italy.
Univ Ferrara, Dept Phys, I-44100 Ferrara, Italy.
Rome Astron Observ, I-00044 Frascati, Italy.
RP De Pasquale, M (reprint author), CNR, IASF, Via Fosso Del Cavaliere 100, I-00133 Rome, Italy.
RI PIRO, LUIGI/E-4954-2013; Nicastro, Luciano/F-5866-2015; Stratta, Maria
Giuliana/L-3045-2016;
OI PIRO, LUIGI/0000-0003-4159-3984; Nicastro, Luciano/0000-0001-8534-6788;
Stratta, Maria Giuliana/0000-0003-1055-7980; Costa,
Enrico/0000-0003-4925-8523; Feroci, Marco/0000-0002-7617-3421; Fiore,
Fabrizio/0000-0002-4031-4157
NR 47
TC 75
Z9 75
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 1018
EP 1024
DI 10.1086/375854
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100028
ER
PT J
AU Igumenshchev, IV
Narayan, R
Abramowicz, MA
AF Igumenshchev, IV
Narayan, R
Abramowicz, MA
TI Three-dimensional magnetohydrodynamic simulations of radiatively
inefficient accretion flows
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; convection; MHD;
turbulence
ID ADVECTION-DOMINATED ACCRETION; ANGULAR-MOMENTUM TRANSPORT; BLACK-HOLES;
3 DIMENSIONS; RADIO JETS; DISKS; CONVECTION; TRANSITIONS; MODELS; STARS
AB We present three-dimensional MHD simulations of rotating radiatively inefficient accretion flows onto black holes. We continuously inject magnetized matter into the computational domain near the outer boundary and run the calculations long enough for the resulting accretion flow to reach a quasi-steady state. We have studied two limiting cases for the geometry of the injected magnetic field: pure toroidal field and pure poloidal field. In the case of toroidal field injection, the accreting matter forms a nearly axisymmetric, geometrically thick, turbulent accretion disk. The disk resembles in many respects the convection-dominated accretion flows found in previous numerical and analytical investigations of viscous hydrodynamic flows. Models with poloidal field injection evolve through two distinct phases. In an initial transient phase, the flow forms a relatively flattened, quasi-Keplerian disk with a hot corona and a bipolar outflow. However, when the flow later achieves steady state, it changes in character completely. The magnetized accreting gas becomes two-phase, with most of the volume being dominated by a strong dipolar magnetic field from which a thermal low-density wind flows out. Accretion occurs mainly via narrow slowly rotating radial streams that "diffuse'' through the magnetic field with the help of magnetic reconnection events.
C1 Univ Rochester, Laser Energet Lab, Rochester, NY 14623 USA.
Harvard Smithsonian Ctr Astrophys, Dept Astron, Cambridge, MA 02138 USA.
Gothenburg Univ, Dept Astron & Astrophys, S-41296 Gothenburg, Sweden.
Chalmers Univ Technol, S-41296 Gothenburg, Sweden.
RP Igumenshchev, IV (reprint author), Univ Rochester, Laser Energet Lab, 250 E River Rd, Rochester, NY 14623 USA.
OI Narayan, Ramesh/0000-0002-1919-2730
NR 56
TC 206
Z9 206
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 1042
EP 1059
DI 10.1086/375769
PN 1
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100031
ER
PT J
AU Tomsick, JA
Kalemci, E
Corbel, S
Kaaret, P
AF Tomsick, JA
Kalemci, E
Corbel, S
Kaaret, P
TI X-ray flares and oscillations from the black hole candidate X-ray
transient XTE J1650-500 at low luminosity
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; stars : individual (XTE
J1650-500); X-rays : stars
ID ADVECTION-DOMINATED ACCRETION; SAGITTARIUS-A-ASTERISK; SYNCHROTRON
EMISSION; TIMING EXPLORER; GALACTIC-CENTER; XTE J1650-500; GRO J0422+32;
ENERGY; OUTBURST; STATES
AB We report on X-ray observations made with the Rossi X-Ray Timing Explorer of the black hole candidate (BHC) transient XTE J1650-500 at the end of its first, and currently only, outburst. By monitoring the source at low luminosities over several months, we found six bright similar to100 s X-ray flares and long timescale oscillations of the X-ray flux. The oscillations are aperiodic with a characteristic timescale of 14.2 days and an order of magnitude variation in the 2.8-20 keV flux. The oscillations may be related to optical "mini-outbursts'' that have been observed at the ends of outbursts for other short orbital period BHC transients. The X-ray flares have durations between 62 and 215 s and peak fluxes that are 5-24 times higher than the persistent flux. The. ares have nonthermal energy spectra and occur when the persistent luminosity is near 3 x 10(34) (d/4 kpc)(2) ergs s(-1) (2.8-20 keV). The rise time for the brightest. are demonstrates that physical models for BHC systems must be able to account for the situation where the X-ray flux increases by a factor of up to 24 on a timescale of seconds. We discuss the. ares in the context of observations and theory of Galactic BHCs and compare the. ares to those detected from Sgr A*, the supermassive black hole at the Galactic center. We also compare the. ares to X-ray bursts that are seen in neutron star systems. While some of the. are light curves are similar to those of neutron star bursts, the. ares have nonthermal energy spectra in contrast to the blackbody spectra exhibited in bursts. This indicates that X-ray bursts should not be taken as evidence that a given system contains a neutron star unless the presence of a blackbody component in the burst spectrum can be demonstrated.
C1 Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA.
Univ Calif Berkeley, Space Sci Lab, Berkeley, CA USA.
CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France.
Univ Paris 07, F-91191 Gif Sur Yvette, France.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Tomsick, JA (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, Code 0424, La Jolla, CA 92093 USA.
NR 63
TC 25
Z9 25
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP 1100
EP 1109
DI 10.1086/375811
PN 1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RG
UT WOS:000184408100035
ER
PT J
AU Habbal, SR
Arndt, MB
Nayfeh, MH
Arnaud, J
Johnson, J
Hegwer, S
Woo, R
Ene, A
Habbal, F
AF Habbal, SR
Arndt, MB
Nayfeh, MH
Arnaud, J
Johnson, J
Hegwer, S
Woo, R
Ene, A
Habbal, F
TI On the detection of the signature of silicon nanoparticle dust grains in
coronal holes
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; eclipses; polarization; Sun : corona; Sun : infrared;
Sun : magnetic fields
ID 1991 SOLAR ECLIPSE; INTERPLANETARY DUST; INFRARED OBSERVATIONS; THERMAL
RADIATION; CIRCUMSOLAR DUST; MAGNETIC-FIELD; EMISSION-LINE; POLARIZATION
AB We report on polarization measurements in the Fe XIII line at 1074.7 nm made during the total solar eclipse of 2001 June 21, which yielded the first signature of interplanetary dust in the inner corona. In the first-ever images at this wavelength, the signature of dust appears as a tangentially polarized emission in the radial extension of the low-temperature and low-density coronal holes as opposed to a predominantly radial polarization direction in the rest of the corona. The observed emission and polarization are attributed to fluorescence from silicon nanoparticle dust grains in the inner corona.
C1 Univ Coll Wales, Dept Phys, Aberystwyth SY23 3BZ, Dyfed, Wales.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Bridgewater State Coll, Dept Phys, Bridgewater, MA 02325 USA.
Univ Illinois, Dept Phys, Urbana, IL 61801 USA.
Observ Midi Pyrenees, F-31400 Toulouse, France.
Electricon, Boulder, CO 80304 USA.
Natl Solar Observ, Sunspot, NM 88349 USA.
CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
Stanford Univ, Dept Phys, Stanford, CA 94305 USA.
Univ Texas, Dept Mech Engn, Austin, TX 78712 USA.
RP Habbal, SR (reprint author), Univ Coll Wales, Dept Phys, Aberystwyth SY23 3BZ, Dyfed, Wales.
NR 21
TC 17
Z9 17
U1 1
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP L87
EP L90
DI 10.1086/377678
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RJ
UT WOS:000184408300009
ER
PT J
AU McCarthy, MC
Thaddeus, P
AF McCarthy, MC
Thaddeus, P
TI The radio spectrum of Si-3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : molecules; line : identification; molecular data; molecular
processes; radio lines : ISM
ID GROUND-STATE; CLUSTERS
AB The silicon trimer Si-3 and several of its rare isotopic species have been detected in the laboratory, and the frequencies of 66 rotational transitions in the range 5 - 42 GHz have been measured to a few parts in 10(7). The most intense radio lines can be calculated from the derived spectroscopic constants to better than 3 km s(-1) in equivalent radial velocity up to frequencies of 50 GHz, adequate for a deep search in the best astronomical sources; above that frequency the uncertainties increase to of the order of 20 km s(-1) at 160 GHz, which is still sufficient for a deep search in a wide-line source such as IRC + 10216.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 12
TC 3
Z9 3
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD AUG 1
PY 2003
VL 592
IS 2
BP L91
EP L93
DI 10.1086/375728
PN 2
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 705RJ
UT WOS:000184408300010
ER
PT J
AU Liu, X
Newchurch, MJ
Kim, JH
AF Liu, X
Newchurch, MJ
Kim, JH
TI Occurrence of ozone anomalies over cloudy areas in TOMS version-7
level-2 data
SO ATMOSPHERIC CHEMISTRY AND PHYSICS
LA English
DT Article
ID TROPICAL TROPOSPHERIC OZONE; MAPPING SPECTROMETER; COLUMN OZONE;
STRATOSPHERIC AEROSOL; SOUTH-AMERICA; TRACE-A; CLIMATOLOGY;
REFLECTIVITY; ABSORPTION; RADIATION
AB This study investigates anomalous ozone distributions over cloudy areas in Nimbus-7 (N7) and Earth-Probe (EP) TOMS version-7 data and analyzes the causes for ozone anomaly formation. A 5degrees-longitude by 5degrees-latitude region is defined to contain a Positive Ozone Anomaly (POA) or Negative Ozone Anomaly (NOA) if the correlation coefficient between total ozone and reflectivity is greater than or equal to0.5 or less than or equal to0.5. The average fractions of ozone anomalies among all cloud fields are 31.8+/-7.7% and 35.8+/-7.7% in the N7 and EP TOMS data, respectively. Some ozone anomalies are caused by ozone retrieval errors, and others are caused by actual geophysical phenomena. Large cloud-height errors are found in the TOMS version-7 algorithm in comparison to the Temperature Humidity Infrared Radiometer (THIR) cloud data. On average, cloud-top pressures are overestimated by similar to200 hPa (THIR cloud-top pressure less than or equal to200 hPa) for high-altitude clouds and underestimated by similar to150 hPa for low-altitude clouds ( THIR cloud-top pressure greater than or equal to750 hPa). Most tropical NOAs result from negative errors induced by large cloud-height errors, and most tropical POAs are caused by positive errors due to intra-cloud ozone absorption enhancement. However, positive and negative errors offset each other, reducing the ozone anomaly occurrence in TOMS data. Large ozone/reflectivity slopes for mid-latitude POAs show seasonal variation consistent with total ozone fluctuation, indicating that they result mainly from synoptic and planetary wave disturbances. POAs with an occurrence fraction of 30-60% occur in regions of marine stratocumulus off the west coast of South Africa and off the west coast of South America. Both fractions and ozone/reflectivity slopes of these POAs show seasonal variations consistent with that in the tropospheric ozone. About half the ozone/reflectivity slope can be explained by ozone retrieval errors over clear and cloudy areas. The remaining slope may result from there being more ozone production because of rich ozone precursors and higher photolysis rates over high-frequency, low-altitude clouds than in clear areas. Ozone anomalies due to ozone retrieval errors have important implications in TOMS applications such as tropospheric ozone derivation and analysis of ozone seasonal variation.
C1 Univ Alabama, Dept Atmospher Sci, Huntsville, AL 35899 USA.
Pusan Natl Univ, Dept Atmospher Sci, Pusan, South Korea.
RP Liu, X (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RI Liu, Xiong/P-7186-2014
OI Liu, Xiong/0000-0003-2939-574X
NR 50
TC 10
Z9 11
U1 0
U2 1
PU EUROPEAN GEOPHYSICAL SOC
PI KATLENBURG-LINDAU
PA MAX-PLANCK-STR 13, 37191 KATLENBURG-LINDAU, GERMANY
SN 1680-7324
J9 ATMOS CHEM PHYS
JI Atmos. Chem. Phys.
PD AUG 01
PY 2003
VL 3
BP 1113
EP 1129
PG 17
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 707KD
UT WOS:000184509100002
ER
PT J
AU Sumner, S
Hughes, WOH
Boomsma, JJ
AF Sumner, S
Hughes, WOH
Boomsma, JJ
TI Evidence for differential selection and potential adaptive evolution in
the worker caste of an inquiline social parasite
SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY
LA English
DT Article
DE inquilinism; metapleural gland; disease resistance; Metarhizium;
leaf-cutting ant
ID LEAF-CUTTING ANTS; METAPLEURAL GLANDS; ACROMYRMEX-OCTOSPINOSUS;
SYMPATRIC SPECIATION; ATTA-SEXDENS; HYMENOPTERA; FORMICIDAE; INSINUATOR;
SECRETION; SIZE
AB Social parasites exploit the socially managed resources of social insect colonies in order to maximise their own fitness. The inquilines are among the most specialised social parasites, because they are dependent on being fully integrated into their host's colony throughout their lives. They are usually relatives of their host and so share ancestral characteristics (Emery's rule). Closely related inquiline-host combinations offer a rare opportunity to study trade-offs in natural selection. This is because ancestral adaptations to a free-living state (e.g. the production of a worker caste) become redundant and may be replaced by novel, parasitic traits as the inquiline becomes more specialised. The dynamics of such processes are, however, unknown as virtually all extant inquiline social parasites have completely lost their worker caste. An exception is Acromyrmex insinuator, an incipient permanent social parasite of the leaf-cutting ant Acromyrmex echinatior. In the present study, we document the size distribution of parasite and host workers and infer how selection has acted on A. insinuator to reduce, but not eliminate, its investment in a worker caste. We show that the antibiotic producing metapleural glands of these parasite workers are significantly smaller than in their host counterparts and we deduce that the metapleural gland size in the host represents the ancestral state. We further show experimentally that social parasite workers are more vulnerable to the general insect pathogenic fungus Metarhizium than are host workers. Our findings suggest that costly disease resistance mechanisms are likely to have been lost early in inquiline evolution, possibly because active selection for maintaining these traits became less when parasite workers had evolved the ability to exploit the collective immune system of their host societies.
C1 Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen, Denmark.
RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Gamboa POB 2072, Balboa, Panama.
EM sumners@naos.si.edu
RI Sumner, Seirian/E-6611-2011; Hughes, William/A-6957-2014; Boomsma,
Jacobus/M-2785-2014
OI Hughes, William/0000-0003-0951-9768; Boomsma,
Jacobus/0000-0002-3598-1609
NR 41
TC 23
Z9 23
U1 1
U2 7
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0340-5443
J9 BEHAV ECOL SOCIOBIOL
JI Behav. Ecol. Sociobiol.
PD AUG
PY 2003
VL 54
IS 3
BP 256
EP 263
DI 10.1007/s00265-003-0633-0
PG 8
WC Behavioral Sciences; Ecology; Zoology
SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology
GA 711RM
UT WOS:000184754900008
ER
PT J
AU Kursar, TA
Coley, PD
AF Kursar, TA
Coley, PD
TI Convergence in defense syndromes of young leaves in tropical rainforests
SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY
LA English
DT Article; Proceedings Paper
CT 4th International Legume Conference
CY JUL 02-06, 2001
CL CANBERRA, AUSTRALIA
DE herbivory; rainforest; Barro Colorado Island; young leaves; phenolics;
leaf expansion; pathogens; bioassays; toughness; delayed greening; Inga
ID LEAF DEVELOPMENT; HERBIVORY; TREE; COEVOLUTION; CONSEQUENCES; EXPANSION;
TOXICITY; INSECTS
AB In tropical forests, the majority of damage by herbivores or pathogens occurs on young leaves, yet the patterns of damage and the factors that influence them are poorly known. By measuring damage throughout leaf development and maturation for five. species in a Panamanian forest, we showed that leaf toughening, which only occurs over a few days once the leaf is fully expanded, is the main factor decreasing damage in mature leaves. Although rates of damage to young leaves are, on average, orders of magnitude greater than on mature leaves, there is significant interspecific variation in young leaf defenses and in damage rates. In a survey of 55 species of shade-tolerant plants, we found that each species only invested in a subset of the,potential defensive mechanisms for young leaves. We measured rates of young leaf expansion, nitrogen content, delayed chloroplast development, synchrony of leaf production and rates of damage in the field. On a subset of 24 species, we also measured phenolic compounds, checked for the presence of saponins and alkaloids, and conducted bioassays using lepidopteran, coleopteran and orthopteran herbivores and. four fungal pathogens to test for toxicity of young leaf extracts. Certain combinations,of traits repeatedly co-occurred across unrelated species suggesting convergent evolution. We argue that selection has repeatedly led to tradeoffs among defenses such that species fall along an escape/defense continuum. At one extreme are species with a 'defense' strategy, which includes effective chemical defense, slow leaf expansion, normal greening and low rates of damage (less than 20% of the leaf area lost). At the other extreme are 'escape' species which have ineffective chemical defenses and, as a consequence, have high rates of leaf damage, >60% of leaf area lost during expansion. In partial compensation for ineffective chemical defense, these species have very rapid leaf expansion (doubling in area every day) which minimizes the window of vulnerability, delayed chloroplast development (white young leaves) which contain fewer resources, and synchronous leaf production to satiate herbivores. Thus, interspecific variation in young leaf damage rates is explained by differences in defense combinations along this escape/defense continuum. Because apparently beneficial traits such as effective chemical defense and rapid leaf expansion do not occur in the same species, we suggest that physiological constraints limit the defense combinations of any one species to a restricted subset of those observed. However, the defense and escape strategies do not represent different tradeoffs that have equal fitness, as species with the escape syndrome suffer much higher rates of damage. We hypothesize that the escape syndrome arose over evolutionary time among plants that failed to evolve effective secondary metabolites while herbivores succeeded in evolving adaptations to the chemistry of their host plant. Hence the defense syndrome should provide the greatest fitness, whereas the escape syndrome minimizes damage given the failure of the plant's secondary metabolites to provide protection. (C) 2003 Elsevier Science Ltd. All rights reserved.
C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
Smithsonian Trop Res Inst, Balboa, Panama.
RP Kursar, TA (reprint author), Univ Utah, Dept Biol, 257 South 1400 East, Salt Lake City, UT 84112 USA.
NR 52
TC 146
Z9 159
U1 5
U2 72
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0305-1978
J9 BIOCHEM SYST ECOL
JI Biochem. Syst. Ecol.
PD AUG
PY 2003
VL 31
IS 8
BP 929
EP 949
DI 10.1016/S0305-1978(03)00087-5
PG 21
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 696TH
UT WOS:000183903000008
ER
PT J
AU Zigler, KS
Lessios, HA
AF Zigler, KS
Lessios, HA
TI 250 million years of bindin evolution
SO BIOLOGICAL BULLETIN
LA English
DT Article
ID POSITIVE DARWINIAN SELECTION; ABALONE SPERM LYSIN; SEA-URCHIN EGGS;
STRONGYLOCENTROTUS-FRANCISCANUS; MOLECULAR EVOLUTION; MITOCHONDRIAL-DNA;
MEMBRANE-FUSION; RAPID EVOLUTION; PROTEIN BINDIN; SEQUENCE
AB Bindin plays a central role in sperm-egg attachment and fusion in sea urchins (echinoids). Previous studies determined the DNA sequence of bindin in two orders of the class Echinoidea, representing 10% of all echinoid species. We report sequences of mature bindin from five additional genera, representing four new orders, including the distantly related sand dollars, heart urchins, and pencil urchins. The six orders in which bindin is now known include 70% of all echinoids, and indicate that bindin was present in the common ancestor of all extant sea urchins more than 250 million years ago. Over this span of evolutionary time there has been (1) remarkable conservation in the core region of bindin, particularly in a stretch of 29 amino acids that has not changed at all; (2) conservation of a motif of basic amino acids at the cleavage site between preprobindin and mature bindin; (3) more than a twofold change in length of mature bindin; and (4) emergence of high variation in the sequences outside the core, including the insertion of glycine-rich repeats in the bindins of some orders, but not others.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Duke Univ, Dept Biol, Durham, NC USA.
RP Zigler, KS (reprint author), Univ Washington, Friday Harbor Labs, 620 Univ Rd, Friday Harbor, WA 98250 USA.
NR 45
TC 37
Z9 38
U1 2
U2 7
PU MARINE BIOLOGICAL LABORATORY
PI WOODS HOLE
PA 7 MBL ST, WOODS HOLE, MA 02543 USA
SN 0006-3185
J9 BIOL BULL-US
JI Biol. Bull.
PD AUG
PY 2003
VL 205
IS 1
BP 8
EP 15
DI 10.2307/1543440
PG 8
WC Biology; Marine & Freshwater Biology
SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology
GA 714ZJ
UT WOS:000184945300002
PM 12917217
ER
PT J
AU Larson, SR
Jones, TA
McCracken, CL
Jensen, KB
AF Larson, SR
Jones, TA
McCracken, CL
Jensen, KB
TI Amplified fragment length polymorphism in Elymus elymoides, Elymus
multisetus, and other Elymus taxa
SO CANADIAN JOURNAL OF BOTANY-REVUE CANADIENNE DE BOTANIQUE
LA English
DT Article
DE AFLP; Elymus; nucleotide diversity; squirreltail
ID NEEDLEGRASS NASSELLA-PULCHRA; NORTH-AMERICAN ELYMUS; PERENNIAL
TRITICEAE; SYNTHETIC HYBRIDS; GENETIC-VARIATION; SITANION HYSTRIX; AFLP;
GENERA; REGRESSION; CANADENSIS
AB The geographic and phylogenetic significance of amplified fragment length polymorphism within and among 22 Elymus elymoides (Raf.) Swezey subsp. elymoides, 24 E. elymoides subsp. brevifolius (J.G. Sm.) Barkworth, and 13 Elymus multisetus (J.G. Sm.) Burtt-Davy squirreltail accessions was assessed relative to six other North American and three Eurasian Elymus taxa. Elymus elymoides and E. multisetus, comprising Elymus sect. Sitanion (Raf.) A. Love, were both monophyletic and closely related compared with other congeners. The monophyly of subsp. elymoides was also supported; subsp. brevifolius, however, was paraphyletic and separated into four genetically distinct groups. Estimates of nucleotide divergence among the five E. elymoides groups range from 0.0194 to 0.0288, with approximately 0.0329 differences per site between E. elymoides and E. multisetus. Corresponding estimates of nucleotide divergence range from 0.0243 to 0.0387 among North American taxa and from 0.0337 to 0.0455 between North American and Eurasian taxa. DNA polymorphism among E. elymoides accessions was correlated with geographic provenance and previously reported quantitative traits. Distinct genetic groups of E. elymoides generally correspond to different geographic regions, whereas divergent E. multisetus and E. elymoides accessions are sympatric. Thus, taxonomic ranks of E. multisetus and E. elymoides were supported and geographic groups within E. elymoides were distinguished.
C1 Utah State Univ, USDA ARS, Forage & Range Res Lab, Logan, UT 84341 USA.
Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA.
RP Larson, SR (reprint author), Utah State Univ, USDA ARS, Forage & Range Res Lab, Logan, UT 84341 USA.
OI McCracken, Carrie/0000-0002-8038-9727
NR 49
TC 21
Z9 23
U1 1
U2 3
PU NATL RESEARCH COUNCIL CANADA
PI OTTAWA
PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA
SN 0008-4026
J9 CAN J BOT
JI Can. J. Bot.-Rev. Can. Bot.
PD AUG
PY 2003
VL 81
IS 8
BP 789
EP 804
DI 10.1139/B03-077
PG 16
WC Plant Sciences
SC Plant Sciences
GA 727DJ
UT WOS:000185641100004
ER
PT J
AU Grosholz, ED
Ruiz, GM
AF Grosholz, ED
Ruiz, GM
TI Biological invasions drive size increases in marine and estuarine
invertebrates
SO ECOLOGY LETTERS
LA English
DT Article
DE biological invasions; body size; climate change; extinction; fossil
record; introduced species; marine invertebrates; range expansion
ID CHARACTER DISPLACEMENT; SEXUAL DIMORPHISM; ANOLIS LIZARDS; BODY-SIZE;
EVOLUTION; ISLANDS; PLANTS; DIFFERENTIATION; CONSEQUENCES; BIODIVERSITY
AB Ecologists have long been fascinated by the morphological changes that species frequently undergo when introduced into new regions. In this study an unusual pattern of size change associated with the invasion of 19 species of marine and estuarine invertebrates is reported. The results show that the majority of species are significantly larger in the introduced range compared with the native range with little evidence for any decrease in size following invasion. This invasion-driven increase in body size sharply contrasts with the pattern observed in many other taxa including plants, mammals and lizards, where invaders frequently exhibit post-invasion decreases and increases in size. These size changes were not influenced by differences in latitude, sample size or length of time since invasion. Although several mechanisms, may explain the results, none have been demonstrated.
C1 Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Grosholz, ED (reprint author), Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA.
RI Ross, Donald/F-7607-2012;
OI Ross, Donald/0000-0002-8659-3833; Ruiz, Gregory/0000-0003-2499-441X
NR 36
TC 49
Z9 53
U1 3
U2 30
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 1461-023X
J9 ECOL LETT
JI Ecol. Lett.
PD AUG
PY 2003
VL 6
IS 8
BP 700
EP 705
DI 10.1046/j.1461-0248.2003.00495.x
PG 6
WC Ecology
SC Environmental Sciences & Ecology
GA 710QA
UT WOS:000184689900005
ER
PT J
AU Langley, JA
Dijkstra, P
Drake, BG
Hungate, BA
AF Langley, JA
Dijkstra, P
Drake, BG
Hungate, BA
TI Ectomycorrhizal colonization, biomass, and production in a regenerating
scrub oak forest in response to elevated CO2
SO ECOSYSTEMS
LA English
DT Article
DE ectomycorrhizae; fine roots; ingrowth bags; production; turnover;
Quercus
ID ATMOSPHERIC CARBON-DIOXIDE; MYCORRHIZAL COLONIZATION; ROOT PRODUCTION;
QUERCUS-ALBA; ECOSYSTEM; GROWTH; SOIL; DECOMPOSITION; GRASSLANDS; FUNGI
AB The effects of CO2 elevation on the dynamics of fine root (FR) mass and ectomycorrhizal (EM) mass and colonization were studied in situ in a Florida scrub oak system over four years of postfire regeneration. Soil cores were taken at five dates and sorted to assess the standing crop of ectomycorrhizal and fine roots. We used ingrowth bags to estimate the effects of elevated CO2 on production of EM roots and fine roots. Elevated CO2 tended to increase EM colonization frequency but did not affect EM mass nor FR mass in soil cores (standing mass). However, elevated CO2 strongly increased EM mass and FR mass in ingrowth bags (production), but it did not affect the EM colonization frequency therein. An increase in belowground production with unchanged biomass indicates that elevated CO2 may stimulate root turnover. The CO2-stimulated increase of belowground production was initially larger than that of aboveground production. The oaks may allocate a larger portion of resources to root/mycorrhizal production in this system in elevated rather than ambient CO2.
C1 No Arizona Univ, Dept Biol Sci, Merriam Powell Ctr Environm Res, Flagstaff, AZ 86011 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Langley, JA (reprint author), No Arizona Univ, Dept Biol Sci, Merriam Powell Ctr Environm Res, Box 5640, Flagstaff, AZ 86011 USA.
RI Hungate, Bruce/F-8991-2011
OI Hungate, Bruce/0000-0002-7337-1887
NR 36
TC 11
Z9 12
U1 2
U2 17
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 1432-9840
J9 ECOSYSTEMS
JI Ecosystems
PD AUG
PY 2003
VL 6
IS 5
BP 424
EP 430
DI 10.1007/s10021-002-0194-5
PG 7
WC Ecology
SC Environmental Sciences & Ecology
GA 720HU
UT WOS:000185256000002
ER
PT J
AU Meyerson, LA
Reaser, JK
AF Meyerson, LA
Reaser, JK
TI Bioinvasions, bioterrorism, and biosecurity
SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT
LA English
DT Review
ID INFECTIOUS-DISEASES; UNITED-STATES; BIODIVERSITY; AGRICULTURE; THREATS;
IMPACT; MEXICO; HEALTH; TRENDS
AB Despite their high profile and potentially devastating consequences, bioterrorist acts are relatively unpredictable, rare, and thus far small-scale events. In contrast, biological invasions are occurring daily in the US and have significant impacts on human health, agriculture, infrastructure, and the environment, yet they receive far less attention and fewer resources. Scientists and the US government must work together to implement a comprehensive approach to biosecurity that addresses not only bioterrorism, but also the more common incursions of invasive alien species. This approach should also address the potential for the deliberate use of invasive alien species as agents of bioterrorism. To achieve these goals, it will be necessary for the relevant government institutions to acknowledge and include prevention, early detection, and rapid response to species incursions as central mission themes. In addition, the scientific community, industry, and the public must work together to ensure that the necessary technology and information systems are readily available.
C1 US EPA, Amer Assoc Adv Sci Fellow, Natl Ctr Environm Assessment, Washington, DC 20460 USA.
Ecos Syst Inst, Springfield, VA 22150 USA.
Museum Natl Hist Nat, Smithsonian Inst, Washington, DC 20560 USA.
RP Meyerson, LA (reprint author), US EPA, Amer Assoc Adv Sci Fellow, Natl Ctr Environm Assessment, Washington, DC 20460 USA.
EM meyerson.laura@nmnh.si.edu
RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013
NR 50
TC 32
Z9 34
U1 2
U2 14
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA
SN 1540-9295
J9 FRONT ECOL ENVIRON
JI Front. Ecol. Environ.
PD AUG
PY 2003
VL 1
IS 6
BP 307
EP 314
DI 10.2307/3868091
PG 8
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 825WZ
UT WOS:000221790800019
ER
PT J
AU Wehncke, EV
Hubbell, SP
Foster, RB
Dalling, JW
AF Wehncke, EV
Hubbell, SP
Foster, RB
Dalling, JW
TI Seed dispersal patterns produced by white-faced monkeys: implications
for the dispersal limitation of neotropical tree species
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE Cebus capucinus; dispersal effectiveness; primate dispersal; recruitment
limitation; seed dispersal
ID TROPICAL RAIN-FOREST; BROWN CAPUCHIN MONKEYS; INDIVIDUAL SPATIAL CHOICE;
CEBUS-APELLA; RECRUITMENT LIMITATION; FORAGING GROUPS; FRENCH-GUIANA;
HOME-RANGE; DIVERSITY; CONSEQUENCES
AB 1 Primate frugivores are important seed dispersers for a large fraction of tree species in many tropical forests. The movement, diet preferences and defecation patterns produced by primates may therefore strongly influence seed dispersion patterns and seedling recruitment success. Here we examine the pattern of seed dispersal generated by white-faced monkeys (Cebus capucinus ) in relation to adult tree distribution in the 50-ha plot on Barro Colorado Island (BCI), Panama.
2 Diet breadth of Cebus was remarkably wide. Over four months they consumed fruits of 95 out of an estimated 240 species available. Seeds of 67 species passed intact through the gut and 28 were spat out.
3 Dispersal effectiveness of Cebus was also high. Two Cebus groups on average spent < 10 min feeding in individual trees, had large home ranges (> 150 ha), travelled 1-3 km day(-1) and defecated seeds in small clumps throughout the day.
4 Mean dispersal distance of ingested seeds was 216 m (range 20-844 m), with the highest probability of dispersal 100-200 m from the parent plant. For six of nine species studied, the distance between defecation sites and nearest conspecific adults of seeds in faeces was not significantly different from random expectations.
5 The scattered dispersal pattern produced by Cebus suggests that this species contributes relatively little to dispersal limitation (sensu Nathan & Muller-Landau 2000) compared to other dispersers in the community. Long-distance dispersal by Cebus resulted in substantial movement of seeds in and out of the 50 ha plot, and suggests that inverse modelling procedures to estimate dispersal functions from trap data may not adequately describe dispersal patterns generated by this primate.
C1 Univ Nacl Autonoma Mexico, Lab Interac Planta Anim, Dept Ecol Evolut, Mexico City 04510, DF, Mexico.
Smithsonian Trop Res Inst, Balboa, Panama.
Univ Georgia, Dept Bot, Athens, GA 30602 USA.
Field Museum, Dept Bot, Chicago, IL 60605 USA.
Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
RP Wehncke, EV (reprint author), Univ Nacl Autonoma Mexico, Lab Interac Planta Anim, Dept Ecol Evolut, Apartado 70-275,Ciudad Univ,Circuito Rxterior, Mexico City 04510, DF, Mexico.
NR 79
TC 75
Z9 81
U1 2
U2 38
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD AUG
PY 2003
VL 91
IS 4
BP 677
EP 685
DI 10.1046/j.1365-2745.2003.00798.x
PG 9
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 703FA
UT WOS:000184268300015
ER
PT J
AU Woodman, N
Cuartas-Calle, CA
Delgado, CA
AF Woodman, N
Cuartas-Calle, CA
Delgado, CA
TI The humerus of Cryptotis colombiana and its bearing on the species'
phylogenetic relationships (Soricomorpha : Soricidae)
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE anatomy; Cryptotis; Insectivora; morphology; osteology
ID SMALL-EARED SHREW; MAMMALIA; INSECTIVORA
AB The Colombian small-eared shrew, Cryptotis colombiana Woodman and Timm, was described from the Colombian Andes in 1993. Its original allocation to the C. nigrescens group recently was questioned based on several cranial characters the species appeared to share with some members of the C. thomasi group. We review characteristics of the C. nigrescens and C. thomasi groups, and we describe the humerus of C. colombiana and the humerus and manus of C. medellinia. The morphology of the humerus joins the suite of characters that supports the hypotheses that C. colombiana is not a member of the C. thomasi group and that all remaining South American species form a cohesive, definable set that is probably monophyletic.
C1 Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, MRC 111, Washington, DC 20013 USA.
Univ Antioquia, Inst Biol, Medellin 1226, Colombia.
RP Woodman, N (reprint author), Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, MRC 111, POB 37012, Washington, DC 20013 USA.
EM woodman.neal@nmnh.si.edu
OI Woodman, Neal/0000-0003-2689-7373
NR 12
TC 9
Z9 13
U1 0
U2 2
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD AUG
PY 2003
VL 84
IS 3
BP 832
EP 839
DI 10.1644/BME-007
PG 8
WC Zoology
SC Zoology
GA 718MC
UT WOS:000185149300004
ER
PT J
AU Jakab, PL
AF Jakab, PL
TI First to fly: North Carolina and the beginnings of aviation.
SO JOURNAL OF SOUTHERN HISTORY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Jakab, PL (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SOUTHERN HISTORICAL ASSOC
PI ATHENS
PA UNIV GEORGIA, HISTORY DEPT, ATHENS, GA 30602 USA
SN 0022-4642
J9 J SOUTHERN HIST
JI J. South. Hist.
PD AUG
PY 2003
VL 69
IS 3
BP 729
EP 730
PG 2
WC History
SC History
GA 708YG
UT WOS:000184597500065
ER
PT J
AU Kensley, B
Cartes, JE
AF Kensley, B
Cartes, JE
TI Records and distribution of Syscenus infelix in the deep Mediterranean
(Crustacea : Isopoda : Aegidae)
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
ID FISHES
AB The parasitic isopod Syscenus infelix is recorded from the Mediterranean, based on 19 specimens from a depth range of 375-2071 m. The first ovigerous female of the species is also recorded. Patterns of possible parasitism were suggested based on the depth distribution of S. infelix, and their possible host macrourid fish below 900 m depth in the Catalano-Balearic basin.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA.
CSIC, Inst Ciencies Mar Barcelona, Barcelona 080003, Spain.
RP Kensley, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA.
NR 8
TC 3
Z9 4
U1 1
U2 4
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD AUG
PY 2003
VL 83
IS 4
BP 775
EP 777
DI 10.1017/S002531540300777Xh
PG 3
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 719KM
UT WOS:000185202300015
ER
PT J
AU Endo, H
Sasaki, M
Narushima, E
Komiya, T
Hayashida, A
Hayashi, Y
Stafford, BJ
AF Endo, H
Sasaki, M
Narushima, E
Komiya, T
Hayashida, A
Hayashi, Y
Stafford, BJ
TI Macroscopic study of the functional significance of the forearm muscles
in the giant panda
SO JOURNAL OF VETERINARY MEDICAL SCIENCE
LA English
DT Article
DE accessory carpal bone; forearm; giant panda; radial sesamoid bone
ID RADIAL SESAMOID BONE; AILUROPODA-MELANOLEUCA; ANATOMY
AB The extensor and flexor group muscles and their related muscles were functional-morphologically observed in the dead body of the giant panda to clarify the action of the forearm and the palm in the manipulation of the species. The Musculus flexor carpi ulnaris had two developed heads, however, we can conclude that the contraction of this muscle slightly changes the angle of the accessory carpal bone to the ulna. The data pointed out that the accessory carpal bone acts as a supporting post, when the giant panda seizes the object. The M. abductor digiti I longus possessed the well-developed origin in both ulna and radius. These findings suggest that this muscle may function as a supinator of the forearm. We also suggest that the well-developed M. pronator quadratus and M. pronator teres, and the proximal part of the M. abductor digiti I longus and the M. supinator may efficiently contribute to the pronator-spinator action of the forearm, when the giant panda brings the food to its mouth using the manipulation system equipped in the palm region.
C1 Natl Sci Museum, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan.
Obihiro Univ Agr & Vet Med, Dept Vet Anat, Obihiro, Hokkaido 0108666, Japan.
Ueno Zool Gardens, Tokyo 1108701, Japan.
Rakuno Gakuen Univ, Fac Med Vet, Dept Toxicol, Ebetsu, Hokkaido 0698501, Japan.
Univ Tokyo, Grad Sch Agr & Life Sci, Dept Vet Anat, Tokyo 1138567, Japan.
Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA.
Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA.
RP Endo, H (reprint author), Natl Sci Museum, Dept Zool, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan.
NR 17
TC 2
Z9 3
U1 0
U2 3
PU JAPAN SOC VET SCI
PI TOKYO
PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN
SN 0916-7250
J9 J VET MED SCI
JI J. Vet. Med. Sci.
PD AUG
PY 2003
VL 65
IS 8
BP 839
EP 843
PG 5
WC Veterinary Sciences
SC Veterinary Sciences
GA 719PR
UT WOS:000185212700003
PM 12951414
ER
PT J
AU Endo, H
Hikida, T
Motokawa, M
Chou, LM
Fukuta, K
Stafford, BJ
AF Endo, H
Hikida, T
Motokawa, M
Chou, LM
Fukuta, K
Stafford, BJ
TI Morphological adaptation of the skull for various behaviors in the tree
shrews
SO JOURNAL OF VETERINARY MEDICAL SCIENCE
LA English
DT Article
DE adaptation; behavior; osteometry; skull; Tupaiidae
ID TUPAIA-GLIS; THAILAND
AB Skull size and shape were examined among 14 species of the tree shrews (Tupaia montana, T. picta, T. splendidula, T. mulleri, T. longipes, T. glis, T. javanica, T. minor, T. gracilis, T. dorsalis, T. tana, Dendrogale melanura, D. murina, and Ptilocercus lowii). The bones of face were rostro-caudally longer in T. tana and T. dorsalis, contrasting with T. minor and T. gracilis, D. melanura, D. murina and P. lowii which have smaller facial length ratios. The arbo-terrestrial species (T. longipes and T. glis) were similar to terrestrial species in length ratios of bones of face unlike the other arbo-terrestrial species (T. montana., T. picta, T. splendidula, and T. mulleri). We propose that T. longipes and T. glis have adapted to foraging for termites and ants as have T. tana and T dorsalis. Additionally small body size in T. javanica may be the result of being isolated in Java. We separated the species into 5 groups from the measurment values of skulls: 1) Terrestrial species; T. tana and T dorsalis, 2) Arboreal species; T. minor and T. gracilis, 3) Arbo-terrestrial species group 1: T. montana. T. splendidula, T. picta and T. mulleri, and T. javanica, 4) Arbo-terrestrial species group 2: T. glis and T longipes, 5) Arboreal species of Dendrogale and Ptilocercus. Principal component analysis separated species into 8 clusters as follows: 1) T. tana, 2) T. dorsalis, 3) T. montana, T. splendidula, T. picta and T. mulleri, 4) T. glis and T. longipes, 5) T. javanica, 6) T. minor and T. gracilis, 7) D. melanura and D. murina, and 8) P. lowii. We suggest that these clusters correspond to behavioral strategies and peculiarities observed in foraging, feeding and locomotion in each species.
C1 Natl Sci Museum, Dept Zool, Shinjuku Ku, Tokyo 1690073, Japan.
Kyoto Univ, Fac Sci, Dept Zool, Kyoto 6068501, Japan.
Kyoto Univ, Univ Museum, Kyoto 6068501, Japan.
Natl Univ Singapore, Raffles Museum Biodivers Res, Singapore 117548, Singapore.
Nagoya Univ, Grad Sch Bioagr Sci, Lab Anim Morphol & Funct, Nagoya, Aichi 4648601, Japan.
Smithsonian Inst, Natl Museum Nat Hist, Div Mammal, Washington, DC 20560 USA.
Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA.
RP Endo, H (reprint author), Natl Sci Museum, Dept Zool, Shinjuku Ku, 3-23-1 Hyakunin Cho, Tokyo 1690073, Japan.
RI Chou, Loke Ming/I-2951-2012
NR 25
TC 4
Z9 5
U1 0
U2 8
PU JAPAN SOC VET SCI
PI TOKYO
PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN
SN 0916-7250
J9 J VET MED SCI
JI J. Vet. Med. Sci.
PD AUG
PY 2003
VL 65
IS 8
BP 873
EP 879
PG 7
WC Veterinary Sciences
SC Veterinary Sciences
GA 719PR
UT WOS:000185212700008
PM 12951419
ER
PT J
AU Hutchinson, A
AF Hutchinson, A
TI Bear in mind: The California grizzly.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Lib, Washington, DC 20560 USA.
RP Hutchinson, A (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD AUG
PY 2003
VL 128
IS 13
BP 124
EP 124
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 710VG
UT WOS:000184703100284
ER
PT J
AU Riley, S
AF Riley, S
TI Present value.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Riley, S (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD AUG
PY 2003
VL 128
IS 13
BP 137
EP 137
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 710VG
UT WOS:000184703100367
ER
PT J
AU Grapes, RH
Wysoczanski, RJ
Hoskin, PWO
AF Grapes, RH
Wysoczanski, RJ
Hoskin, PWO
TI Rhonite paragenesis in pyroxenite xenoliths, Mount Sidley volcano, Marie
Byrd Land, West Antarctica
SO MINERALOGICAL MAGAZINE
LA English
DT Article
DE rhonote; pyroxenite xenoliths; Mount Sidney; volcano; Antarctica;
kaersutite
ID AMPHIBOLE; OCCURRENCES; PETROLOGY; LAVAS
AB Rhonite occurs in lower crustal pyroxenite xenoliths erupted in phonolite from the Mount Sidley composite volcano, Marie Byrd Land, Antarctica, as a localized breakdown product, with plagioclase, clinopyroxene, +/- olivine +/- Ti-magnetite + melt, of kaersutite, and as rnicrophenocrysts (with olivine, plagioclase, clinopyroxene) in pockets of basanitic melt. Rhonite after kaersutite has a more NaSi-rich/ CaAl-poor composition, lower Ti, and formed at higher oxidation (similar toNNO) conditions than rhonite Occurring as microphenocrysts in basanite. Comparison with experimentally deterinined rhonite stability in understaturated alkali basalt and as a reaction product after Ti-amphibole indicates that the Mount Sidley rhonite (and associated minerals) formed between 1090 and 1190 degreesC at <0.5 kbar, presumably during temporary residence of the xenoliths in a shallow magma chamber below the volcanic edifice.
C1 Univ Freiburg, Inst Mineral Petr & Geochem, D-79104 Freiburg, Germany.
Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA.
RP Grapes, RH (reprint author), Univ Freiburg, Inst Mineral Petr & Geochem, Hugstetter Str 55, D-79104 Freiburg, Germany.
RI Wysoczanski, Richard/C-2930-2009; Wysoczanski, Richard/I-7730-2012
NR 31
TC 11
Z9 14
U1 0
U2 1
PU MINERALOGICAL SOCIETY
PI LONDON
PA 41 QUEENS GATE, LONDON SW7 5HR, ENGLAND
SN 0026-461X
J9 MINERAL MAG
JI Mineral. Mag.
PD AUG
PY 2003
VL 67
IS 4
BP 639
EP 651
DI 10.1180/0026461036740123
PG 13
WC Mineralogy
SC Mineralogy
GA 722GB
UT WOS:000185366100006
ER
PT J
AU Songsasen, N
Yu, I
Gomez, M
Leibo, SP
AF Songsasen, N
Yu, I
Gomez, M
Leibo, SP
TI Effects of meiosis-inhibiting agents and equine chorionic gonadotropin
on nuclear maturation of canine oocytes
SO MOLECULAR REPRODUCTION AND DEVELOPMENT
LA English
DT Article
DE canine oocytes; nuclear maturation; dbcAMP; roscovitine; equine
chorionic gonadotropin
ID IN-VITRO MATURATION; HIGH DEVELOPMENTAL COMPETENCE; PREPUBERTAL GOAT
OOCYTES; MEIOTIC COMPETENCE; BOVINE OOCYTES; BUTYROLACTONE-I; PIG
OOCYTES; GERMINAL VESICLE; ANTRAL FOLLICLES; BITCH OOCYTES
AB Experiments were conducted to determine the effects of meiosis-inhibiting-agents and gonadotropins on nuclear maturation of canine oocytes. The culture medium was TCM199 + 10 ng/ml epidermal growth factor supplemented with 25 muM beta-mercapto-ethanol, 0.25 mM pyruvate, and 1.0 mM L-glutamine (Basal TCM). Initially, oocytes were cultured in Basal TCM alone or in Basal TCM + dibutylryl cyclic adenosine monophosphate (0.5, 1, 5, or 10 mM dbcAMP) for 24 hr. Dibutylryl cAMP inhibited resumption of meiosis in a dose-dependent manner; 60% of oocytes remained at the germinal vesicle (GV) stage after being cultured for 24 hr in 5 mM dbcAMP. The meiosis-inhibitory effect of dbcAMP appeared to be reversible, as the oocytes resumed meiosis and completed nuclear maturation after being cultured for an additional 48 hr in its absence. Oocytes were then cultured in Basal TCM alone or in Basal TCM + roscovitine (12.5, 25, or 50 muM) for 24 hr. Although similar to60% of oocytes cultured in 25 muM roscovitine remained at the GV stage, this percentage was not significantly different from the 48% that also remained at the GV stage when cultured in its absence. Oocytes were cultured in Basal TCM + 25 1.0 roscovitine for 17 hr, exposed briefly to equine chorionic gonadotropin (eCG), and then cultured in Basal TCM for 48 hr. Short exposure of oocytes to eCG was beneficial, as it significantly increased the proportion of oocytes developing beyond germinal vesicle breakdown (P < 0.05) with similar to20-30% of these were metaphase I (MI) oocytes. Study of the kinetics of nuclear maturation demonstrated that large numbers of oocytes remained at MI even after being cultured for 52 hr following brief exposure to eCG. This study showed that in vitro maturation of canine oocytes can be somewhat improved by short exposure of oocytes to eCG. However, further studies are still required to derive effective methods to mature canine oocytes in vitro. (C) 2003 Wiley-Liss, Inc.
C1 Univ New Orleans, Dept Sci Biol, New Orleans, LA USA.
Audubon Ctr Res Endangered Species, New Orleans, LA USA.
Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA.
RP Songsasen, N (reprint author), Smithsonian Natl Zool Pk, Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA.
NR 73
TC 19
Z9 24
U1 0
U2 1
PU WILEY-LISS
PI NEW YORK
PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA
SN 1040-452X
J9 MOL REPROD DEV
JI Mol. Reprod. Dev.
PD AUG
PY 2003
VL 65
IS 4
BP 435
EP 445
DI 10.1002/mrd.10321
PG 11
WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology;
Reproductive Biology
SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology;
Reproductive Biology
GA 700QK
UT WOS:000184122500011
PM 12840817
ER
PT J
AU Jones, LR
Ponman, TJ
Horton, A
Babul, A
Ebeling, H
Burke, DJ
AF Jones, LR
Ponman, TJ
Horton, A
Babul, A
Ebeling, H
Burke, DJ
TI The nature and space density of fossil groups of galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies : clusters : general; galaxies : elliptical and lenticular, cD;
galaxies : general; X-rays : galaxies : clusters
ID BRIGHTEST CLUSTER GALAXIES; X-RAY-CLUSTERS; N-BODY SIMULATIONS; POOR
CLUSTERS; WARPS SURVEY; HIERARCHICAL-MODELS; LUMINOSITY FUNCTION; MERGER
RATES; CD GALAXIES; EVOLUTION
AB We describe the properties of a sample of galaxy groups with very unusual distributions of galaxy luminosities. The most extreme example has an X-ray luminosity similar to that of the Virgo cluster but has a very low richness, with only one galaxy brighter than L *, compared with six in Virgo. That one galaxy, however, is optically more luminous than any galaxy in Virgo and has an optical luminosity as bright as many of the central cD galaxies in rich Abell clusters.
The characteristic feature of the fossil groups we study is that most of the light arises from one dominant, central galaxy. We define a fossil system and, based on this definition, construct a small X-ray-selected, flux-limited sample of fossil groups with well-known selection criteria. We confirm that these systems are indeed groups of galaxies, but dominated by one central luminous giant elliptical galaxy and with few, or no, L * galaxies. We find that fossil systems represent 8-20 per cent of all systems of the same X-ray luminosity. Fossil groups are at least as numerous as all poor and rich clusters combined, and are thus a possible site for the formation of luminous central cluster galaxies before infall into clusters occurs. The fossil systems in our sample have significantly higher X-ray luminosities than normal groups of similar total optical luminosities (or similar X-ray temperature, where the latter can be measured). These enhanced X-ray luminosities may be due to relatively cool gas in the innermost regions or due to a low central gas entropy. We interpret fossil groups as old, undisturbed systems which have avoided infall into clusters, but where galaxy merging of most of the L * galaxies has occurred. An early formation epoch, before that of most groups, could explain low central gas entropies and high X-ray luminosities.
C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada.
Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Jones, LR (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
NR 76
TC 187
Z9 188
U1 0
U2 2
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD AUG 1
PY 2003
VL 343
IS 2
BP 627
EP 638
DI 10.1046/j.1365-8711.2003.06702.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704HT
UT WOS:000184334600031
ER
PT J
AU Erhardt, D
AF Erhardt, D
TI Not-so-new technology
SO NATURE MATERIALS
LA English
DT News Item
C1 Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, Suitland, MD 20746 USA.
RP Erhardt, D (reprint author), Smithsonian Inst, Museum Support Ctr, Smithsonian Ctr Mat Res & Educ, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
NR 0
TC 7
Z9 8
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 1476-1122
J9 NAT MATER
JI Nat. Mater.
PD AUG
PY 2003
VL 2
IS 8
BP 509
EP 510
DI 10.1038/nmat951
PG 2
WC Chemistry, Physical; Materials Science, Multidisciplinary; Physics,
Applied; Physics, Condensed Matter
SC Chemistry; Materials Science; Physics
GA 710NW
UT WOS:000184687200006
PM 12894257
ER
PT J
AU Engelbrecht, BMJ
Kursar, TA
AF Engelbrecht, BMJ
Kursar, TA
TI Comparative drought-resistance of seedlings of 28 species of
co-occurring tropical woody plants
SO OECOLOGIA
LA English
DT Article
DE growth; irrigation; soil moisture; survival; tropical moist forest
ID EL-NINO DROUGHT; RAIN-FOREST; TREE SEEDLINGS; MOIST FOREST; HABITAT
ASSOCIATIONS; VIROLA-SURINAMENSIS; WATER RELATIONS; GROWTH; SURVIVAL;
TOLERANCE
AB Quantifying plant drought resistance is important for understanding plant species' association to microhabitats with different soil moisture availability and their distribution along rainfall gradients, as well as for understanding the role of underlying morphological and physiological mechanisms. The effect of dry season drought on survival and leaf-area change of first year seedlings of 28 species of co-occurring woody tropical plants was experimentally quantified in the understory of a tropical moist forest. The seedlings were subjected to a drought or an irrigation treatment in the forest for 22 weeks during the dry season. Drought decreased survival and growth (assessed as leaf-area change) in almost all of the species. Both survival and leaf-area change in the dry treatment ranged fairly evenly from 0% to about 100% of that in the irrigated treatment. In 43% of the species the difference between treatments in survival was not significant even after 22 weeks. In contrast, only three species showed no significant effect of drought on leaf-area change. The effects of drought on species' survival and growth were not correlated with each other, reflecting different strategies in response to drought. Seedling size at the onset of the dry season had no significant effect on species' drought response. Our study is the first to comparatively assess seedling drought resistance in the habitat for a large number of tropical species, and underlines the importance of drought for plant population dynamics in tropical forests.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
RP Engelbrecht, BMJ (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama.
RI Engelbrecht, Bettina/E-9914-2012
NR 64
TC 126
Z9 137
U1 5
U2 54
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD AUG
PY 2003
VL 136
IS 3
BP 383
EP 393
DI 10.1007/s00442-003-1290-8
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 711RZ
UT WOS:000184756000007
PM 12811534
ER
PT J
AU Torres, DF
Romero, GE
Dame, TM
Combi, JA
Butt, YM
AF Torres, DF
Romero, GE
Dame, TM
Combi, JA
Butt, YM
TI Supernova remnants and gamma-ray sources
SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS
LA English
DT Review
DE gamma-rays; observations; gamma-rays; theory; ISM; supernova remnants;
ISM; clouds; cosmic rays
ID UNIDENTIFIED EGRET SOURCES; GALACTIC PLANE SURVEY; HIGH-ENERGY EMISSION;
ACCELERATED COSMIC-RAYS; RADIO-CONTINUUM SURVEY; PULSAR SAX J0635+0533;
ACCRETING BLACK-HOLE; AIR-SHOWER ARRAY; EARLY-TYPE STARS; X-RAY
AB A review of the possible relationship between x-ray sources and supernova remnants (SNRs) is presented. Particular emphasis is given to the analysis of the observational status of the problem of cosmic ray acceleration at SNR shock fronts. All positional coincidences between SNRs and unidentified gamma-ray sources listed in the Third EGRET Catalog at low Galactic latitudes are discussed on a case by case basis. For several coincidences of particular interest, new CO(J = 1 - 0) and radio continuum maps are shown, and the mass content of the SNR surroundings is determined. The contribution to the T-ray flux observed that might come from cosmic ray particles (particularly nuclei) locally accelerated at the SNR shock fronts is evaluated. We discuss the prospects for future research in this field and remark on the possibilities for observations with forthcoming gamma-ray instruments. (C) 2003 Published by Elsevier B.V.
C1 Lawrence Livermore Lab, Livermore, CA 94550 USA.
Inst Argentino Radioastron, Buenos Aires, DF, Argentina.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lawrence Livermore Lab, 7000 E Ave,L-413, Livermore, CA 94550 USA.
EM dtorres@igpp.uclln1.org
RI Torres, Diego/O-9422-2016
OI Torres, Diego/0000-0002-1522-9065
NR 293
TC 104
Z9 104
U1 1
U2 2
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0370-1573
EI 1873-6270
J9 PHYS REP
JI Phys. Rep.-Rev. Sec. Phys. Lett.
PD AUG
PY 2003
VL 382
IS 6
BP 303
EP 380
DI 10.1016/S0370-1573(03)00201-1
PG 78
WC Physics, Multidisciplinary
SC Physics
GA 703RG
UT WOS:000184294300001
ER
PT J
AU Hanson, DT
Franklin, LA
Samuelsson, G
Badger, MR
AF Hanson, DT
Franklin, LA
Samuelsson, G
Badger, MR
TI The Chlamydomonas reinhardtii cia3 mutant lacking a thylakoid
lumen-localized carbonic anhydrase is limited by CO2 supply to rubisco
and not photosystem II function in vivo
SO PLANT PHYSIOLOGY
LA English
DT Article
ID INORGANIC CARBON; CONCENTRATING MECHANISM; CO2-CONCENTRATING MECHANISMS;
DEFICIENT MUTANTS; QUANTUM YIELD; PHOTOSYNTHESIS; EXCHANGE; OXYGEN;
ALGAE; TRANSPORT
AB The Chlamydomonas reinhardtii cia3 mutant has a phenotype indicating that it requires high-CO2 levels for effective photosynthesis and growth. It was initially proposed that this mutant was defective in a carbonic anhydrase (CA) that was a key component of the photosynthetic CO2-concentrating mechanism (CCM). However, more recent identification of the genetic lesion as a defect in a lumenal CA associated with photosystem II (PSII) has raised questions about the role of this CA in either the CCM or PSII function. To resolve the role of this lumenal CA, we re-examined the physiology of the cia3 mutant. We confirmed and extended previous gas exchange analyses by using membrane-inlet mass spectrometry to monitor O-16(2), O-18(2), and CO2 fluxes in vivo. The results demonstrate that PSII electron transport is not limited in the cia3 mutant at low inorganic carbon (Ci). We also measured metabolite pools sizes and showed that the RuBP pool does not fall to abnormally low levels at low Ci as might be expected by a photosynthetic electron transport or ATP generation limitation. Overall, the results demonstrate that under low Ci conditions, the mutant lacks the ability to supply Rubisco with adequate CO2 for effective CO2 fixation and is not limited directly by any aspect of PSII function. We conclude that the thylakoid CA is primarily required for the proper functioning of the CCM at low Ci by providing an ample supply of CO2 for Rubisco.
C1 Australian Natl Univ, Res Sch Biol Sci, Mol Plant Physiol Grp, Canberra, ACT 2601, Australia.
Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Umea Univ, Dept Plant Physiol, Umea Plant Sci Ctr, S-90187 Umea, Sweden.
RP Badger, MR (reprint author), Australian Natl Univ, Res Sch Biol Sci, Mol Plant Physiol Grp, GPO Box 475, Canberra, ACT 2601, Australia.
RI Hanson, David/J-8034-2012; Samuelsson, Goran/E-1824-2015; Badger,
Murray/C-8153-2009
NR 43
TC 44
Z9 47
U1 0
U2 7
PU AMER SOC PLANT BIOLOGISTS
PI ROCKVILLE
PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA
SN 0032-0889
J9 PLANT PHYSIOL
JI Plant Physiol.
PD AUG
PY 2003
VL 132
IS 4
BP 2267
EP 2275
DI 10.1104/pp.103.023481
PG 9
WC Plant Sciences
SC Plant Sciences
GA 710ZV
UT WOS:000184713400053
PM 12913181
ER
PT J
AU Kim, HG
Funk, VA
Vlasak, A
Zimmer, EA
AF Kim, HG
Funk, VA
Vlasak, A
Zimmer, EA
TI A phylogeny of the Munnoziinae (Asteraceae, Liabeae): circumscription of
Munnozia and a new placement of M-perfoliata
SO PLANT SYSTEMATICS AND EVOLUTION
LA English
DT Article
DE Asteraceae; Cichorioideae; Liabeae; Munnoziinae; Liabinae;
Paranepheliinae; Phylogeny; internal transcribed spacer (ITS); parsimony
and maximum likelihood analyses; monophyly; paraphyly; biogeography
ID NUCLEAR RIBOSOMAL DNA; TRANSCRIBED SPACER SEQUENCES; MOLECULAR EVIDENCE;
DATA SETS; EVOLUTION; GENUS; BIOGEOGRAPHY; CONFIDENCE; COMPOSITAE;
ORIGIN
AB The tribe Liabeae (Compositae, Cichorioideae) comprises three subtribes, Liabinae, Munnoziinae, and Paranepheliinae. For one of these, the Munnoziinae, which contains the genera Munnozia, Chrysactinium, Erato, and Philoglossa, the nuclear ITS (internal transcribed spacer) region was sequenced to examine the monophyly of the subtribe and the core genus Munnozia within it. Thirty-six samples representing four currently recognized genera of Munnoziinae and two outgroups were included in this study. Molecular phylogenetic analyses confirm the close relationship of Munnozia with Chrysactinium, and Erato with Philoglossa. However, the monophyly of the Munnoziinae and Munnozia is not supported, in disagreement with the current morphological findings. The discrepancies were attributed to the placements of Munnozia perfoliata outside the Munnoziinae and Munnozia, and Chrysactinium within Munnozia. The resulting tree indicates that first, M. perfoliata needs to be moved out of the munnoziinae and second, Chrysactinium originated from within Munnozia. For the first finding, morphological and palynological reevaluation of this species with allegedly related species reveals additional support in agreement with molecular data. Therefore we propose that the genus Munnozia be re-delimited to the members having black or dark brown anther theca and sordid or reddish pappus and re-organized.
C1 Smithsonian Inst, Museum Support Ctr, Labs Analyt Biol, Suitland, MD 20746 USA.
Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Div Bot, Washington, DC 20560 USA.
RP Kim, HG (reprint author), Univ Texas, Dept Biol Sci, Sect Integrat Biol, Austin, TX 78713 USA.
RI Zimmer, Elizabeth/G-3890-2011
NR 51
TC 8
Z9 10
U1 0
U2 1
PU SPRINGER-VERLAG WIEN
PI VIENNA
PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 VIENNA, AUSTRIA
SN 0378-2697
J9 PLANT SYST EVOL
JI Plant Syst. Evol.
PD AUG
PY 2003
VL 239
IS 3-4
BP 171
EP 185
DI 10.1007/s00606-003-0003-4
PG 15
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 719KE
UT WOS:000185201600001
ER
PT J
AU Kennicutt, RC
Armus, L
Bendo, G
Calzetti, D
Dale, DA
Draine, BT
Engelbracht, CW
Gordon, KD
Grauer, AD
Helou, G
Hollenbach, DJ
Jarrett, TH
Kewley, LJ
Leitherer, C
Li, A
Malhotra, S
Regan, MW
Rieke, GH
Rieke, MJ
Roussel, H
Smith, JDT
Thornley, MD
Walter, F
AF Kennicutt, RC
Armus, L
Bendo, G
Calzetti, D
Dale, DA
Draine, BT
Engelbracht, CW
Gordon, KD
Grauer, AD
Helou, G
Hollenbach, DJ
Jarrett, TH
Kewley, LJ
Leitherer, C
Li, A
Malhotra, S
Regan, MW
Rieke, GH
Rieke, MJ
Roussel, H
Smith, JDT
Thornley, MD
Walter, F
TI SINGS: The SIRTF nearby galaxies survey
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Review
ID STAR-FORMING GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; SPACE-OBSERVATORY
ATLAS; VIRGO CLUSTER GALAXIES; BRIGHT SPIRAL GALAXIES; SHORT-WAVELENGTH
SPECTROMETER; FABRY-PEROT OBSERVATIONS; CLERK-MAXWELL-TELESCOPE;
WESTERBORK HI SURVEY; INTERSTELLAR-MEDIUM
AB The SIRTF Nearby Galaxy Survey is a comprehensive infrared imaging and spectroscopic survey of 75 nearby galaxies. Its primary goal is to characterize the infrared emission of galaxies and their principal infrared-emitting components, across a broad range of galaxy properties and star formation environments. SINGS will provide new insights into the physical processes connecting star formation to the interstellar medium properties of galaxies and provide a vital foundation for understanding infrared observations of the distant universe and ultraluminous and active galaxies. The galaxy sample and observing strategy have been designed to maximize the scientific and archival value of the data set for the SIRTF user community at large. The SIRTF images and spectra will be supplemented by a comprehensive multiwavelength library of ancillary and complementary observations, including radio continuum, H I, CO, submillimeter, BVRIJHK, Halpha, Paalpha, ultraviolet, and X-ray data. This paper describes the main astrophysical issues to be addressed by SINGS, the galaxy sample and the observing strategy, and the SIRTF and other ancillary data products.
C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA.
Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA.
CALTECH, Pasadena, CA 91101 USA.
Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA.
NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Kennicutt, RC (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
OI Draine, Bruce/0000-0002-0846-936X
NR 106
TC 776
Z9 779
U1 1
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2003
VL 115
IS 810
BP 928
EP 952
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704DK
UT WOS:000184322400002
ER
PT J
AU Evans, NJ
Allen, LE
Blake, GA
Boogert, ACA
Bourke, T
Harvey, PM
Kessler, JE
Koerner, DW
Lee, CW
Mundy, LG
Myers, PC
Padgett, DL
Pontoppidan, K
Sargent, AI
Stapelfeldt, KR
van Dishoeck, EF
Young, CH
Young, KE
AF Evans, NJ
Allen, LE
Blake, GA
Boogert, ACA
Bourke, T
Harvey, PM
Kessler, JE
Koerner, DW
Lee, CW
Mundy, LG
Myers, PC
Padgett, DL
Pontoppidan, K
Sargent, AI
Stapelfeldt, KR
van Dishoeck, EF
Young, CH
Young, KE
TI From molecular cores to planet-forming disks: An SIRTF legacy program
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID TELESCOPE-FACILITY SIRTF; INTERMEDIATE-MASS STARS; MAIN-SEQUENCE STARS;
CIRCUMSTELLAR DISKS; ISO SPECTROSCOPY; BROWN DWARFS; SPECTRAL ENERGY;
TAURUS-AURIGA; DENSE CORES; DARK CLOUD
AB Crucial steps in the formation of stars and planets can be studied only at mid- to far-infrared wavelengths, where the Space Infrared Telescope (SIRTF) provides an unprecedented improvement in sensitivity. We will use all three SIRTF instruments ( Infrared Array Camera [IRAC], Multiband Imaging Photometer for SIRTF [MIPS], and Infrared Spectrograph [IRS]) to observe sources that span the evolutionary sequence from molecular cores to protoplanetary disks, encompassing a wide range of cloud masses, stellar masses, and star-forming environments. In addition to targeting about 150 known compact cores, we will survey with IRAC and MIPS (3.6 - 70 mum) the entire areas of five of the nearest large molecular clouds for new candidate protostars and substellar objects as faint as 0.001 solar luminosities. We will also observe with IRAC and MIPS about 190 systems likely to be in the early stages of planetary system formation ( ages up to about 10 Myr), probing the evolution of the circumstellar dust, the raw material for planetary cores. Candidate planet-forming disks as small as 0.1 lunar masses will be detectable. Spectroscopy with IRS of new objects found in the surveys and of a select group of known objects will add vital information on the changing chemical and physical conditions in the disks and envelopes. The resulting data products will include catalogs of thousands of previously unknown sources, multiwavelength maps of about 20 deg(2) of molecular clouds, photometry of about 190 known young stars, spectra of at least 170 sources, ancillary data from ground-based telescopes, and new tools for analysis and modeling. These products will constitute the foundations for many follow-up studies with ground-based telescopes, as well as with SIRTF itself and other space missions such as SIM, JWST, Herschel, and TPF/ Darwin.
C1 Univ Texas, Dept Astron, Austin, TX 78712 USA.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA.
CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA.
No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA.
Korea Astron Observ, Taeduk Radio Astron Observ, Taejon 305348, South Korea.
Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
SIRTF Sci Ctr, Pasadena, CA 91125 USA.
Leiden Observ, NL-2300 RA Leiden, Netherlands.
CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Evans, NJ (reprint author), Univ Texas, Dept Astron, 1 Univ Stn C1400, Austin, TX 78712 USA.
RI Stapelfeldt, Karl/D-2721-2012
NR 58
TC 354
Z9 355
U1 0
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2003
VL 115
IS 810
BP 965
EP 980
DI 10.1086/376697
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704DK
UT WOS:000184322400004
ER
PT J
AU Maness, H
Vrtilek, SD
AF Maness, H
Vrtilek, SD
TI Nebular versus stellar wind abundances in NGC 6543
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID ABSORPTION CROSS-SECTIONS; PLANETARY-NEBULAE
AB An early analysis of Chandra observations of the planetary nebula NGC 6543 suggested that the location and the derived temperature for the X-ray-emitting region are inconsistent with the abundances measured for this object. We revisit Chandra observations of this source ( following significant updates to both the reprocessing and extraction software) in order to propose a resolution to this apparent anomaly. Our reanalysis using abundances found from observations in the infrared, optical, and ultraviolet suggests that the location and temperature of the X-ray emission from NGC 6543 is consistent with nebular abundances expected for the source.
C1 Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Maness, H (reprint author), Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
NR 12
TC 5
Z9 5
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD AUG
PY 2003
VL 115
IS 810
BP 1002
EP 1005
DI 10.1086/376573
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704DK
UT WOS:000184322400007
ER
PT J
AU Launius, RD
AF Launius, RD
TI Public opinion polls and perceptions of US human spaceflight
SO SPACE POLICY
LA English
DT Article; Proceedings Paper
CT World Space Congress
CY OCT 10-19, 2002
CL HOUSTON, TEXAS
SP Comm Space Res
DE spaceflight; public opinion; human exploration of space; project Apollo
ID SPACE
AB A belief exists in the United States about public support for NASA's human spaceflight activities. Many hold that NASA and the cause of the human exploration of space enjoyed outstanding public support and confidence in the 1960s during the era of Apollo and that public support waned in the post-Apollo era, only to sink to quite low depths in the decade of the 1990s. These beliefs are predicated on anecdotal evidence that should not be discounted, but empirical evidence gleaned from public opinion polling data suggests that some of these conceptions are totally incorrect and others are either incomplete or more nuanced than previously believed. This article explores the evolution of public support for space exploration since the 1960s. Using polling data from a variety of sources it presents trends over time and offers comments on the meaning of public perceptions for the evolution of space policy and the development of space exploration in the United States. Published by Elsevier Ltd.
C1 Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, Washington, DC 20013 USA.
RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Div Space Hist, POB 37012,NASM Room 3550,MRC 311, Washington, DC 20013 USA.
OI Launius, Roger/0000-0003-1633-1253
NR 30
TC 19
Z9 19
U1 0
U2 5
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0265-9646
J9 SPACE POLICY
JI Space Policy
PD AUG
PY 2003
VL 19
IS 3
BP 163
EP 175
DI 10.1016/S0265-9646(03)00039-0
PG 13
WC International Relations; Social Sciences, Interdisciplinary
SC International Relations; Social Sciences - Other Topics
GA 714AD
UT WOS:000184889400002
ER
PT J
AU Fiore, AM
Jacob, DJ
Mathur, R
Martin, RV
AF Fiore, AM
Jacob, DJ
Mathur, R
Martin, RV
TI Application of empirical orthogonal functions to evaluate ozone
simulations with regional and global models
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE empirical orthogonal functions; principal components; air pollution;
ozone; regional modeling; global modeling
ID EASTERN UNITED-STATES; SURFACE OZONE; NORTH-AMERICA; TRANSPORT;
POLLUTION; SYSTEMS; PREDICTIONS/; PERFORMANCE; CHEMISTRY; MECHANISM
AB Empirical orthogonal functions are used together with standard statistical metrics to evaluate the ability of models with different spatial resolutions to reproduce observed patterns of surface ozone (O-3) in the eastern United States in the summer of 1995. We examine simulations with the regional Multiscale Air Quality Simulation Platform model (horizontal resolution of 36 km(2)) and the global GEOS-CHEM model (2degrees x 2.5degrees and 4degrees x 5degrees). As the model resolution coarsens, the ability to resolve local O-3 maxima (O-3 greater than or equal to 90 ppbv) is compromised, but the spatial correlation improves. This result shows that synoptic-scale processes modulating O-3 concentrations are easier to capture in models than processes occurring on smaller scales. Empirical orthogonal functions (EOFs) derived from the observed O-3 fields reveal similar modes of variability when averaged onto the three model horizontal resolutions. The EOFs appear to represent (1) an east-west pattern associated with frontal passages, (2) a midwest-northeast pattern associated with migratory high-pressure systems, and (3) a southeast stagnation pattern linked to westward extension of the Bermuda High. All models capture the east-west and southeast EOFs, but the midwest-northeast EOF is misplaced in GEOS-CHEM. GEOS-CHEM captures the principal components of the observational EOFs when the model fields are projected onto these EOFs, implying that it can resolve the contribution of the EOFs to the observed variance. We conclude that coarse-resolution global models can successfully simulate the synoptic conditions leading to high-O-3 episodes in the eastern United States.
C1 Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
MCNC, Environm Modeling Ctr, Res Triangle Pk, NC 27709 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Fiore, AM (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 12 Oxford St, Cambridge, MA 02138 USA.
EM afiore@post.harvard.edu
RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem,
GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
NR 39
TC 43
Z9 43
U1 0
U2 20
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 JUL 31
PY 2003
VL 108
IS D19
AR 4431
DI 10.1029/2002JD003151
PG 15
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 710WZ
UT WOS:000184707000007
ER
PT J
AU Losos, JB
Leal, M
Glor, RE
de Queiroz, K
Hertz, PE
Schettino, LR
Lara, AC
Jackman, TR
Larson, A
AF Losos, JB
Leal, M
Glor, RE
de Queiroz, K
Hertz, PE
Schettino, LR
Lara, AC
Jackman, TR
Larson, A
TI Niche lability in the evolution of a Caribbean lizard community
SO NATURE
LA English
DT Article
ID ANOLIS LIZARDS; PHYLOGENETIC-RELATIONSHIPS; ECOLOGY; SYSTEMS; MODEL
AB Niche conservatism-the tendency for closely related species to be ecologically similar - is widespread(1-3). However, most studies compare closely related taxa that occur in allopatry(3); in sympatry, the stabilizing forces that promote niche conservatism(4,5), and thus inhibit niche shifts, may be countered by natural selection favouring ecological divergence to minimize the intensity of interspecific interactions(6,7). Consequently, the relative importance of niche conservatism versus niche divergence in determining community structure has received little attention(7). Here, we examine a tropical lizard community in which species have a long evolutionary history of ecological interaction. We find that evolutionary divergence overcomes niche conservatism: closely related species are no more ecologically similar than expected by random divergence and some distantly related species are ecologically similar, leading to a community in which the relationship between ecological similarity and phylogenetic relatedness is very weak. Despite this lack of niche conservatism, the ecological structuring of the community has a phylogenetic component: niche complementarity only occurs among distantly related species, which suggests that the strength of ecological interactions among species may be related to phylogeny, but it is not necessarily the most closely related species that interact most strongly.
C1 Washington Univ, Dept Biol, St Louis, MO 63130 USA.
Union Coll, Dept Biol Sci, Schenectady, NY 12308 USA.
Smithsonian Inst, Natl Museum Amer Hist, Div Amphibians & Reptiles, Washington, DC 20560 USA.
Columbia Univ Barnard Coll, Dept Biol, New York, NY 10027 USA.
CITGMA, Inst Ecol & Sistemat, Havana 10800, Cuba.
Villanova Univ, Dept Biol, Villanova, PA 19085 USA.
RP Losos, JB (reprint author), Washington Univ, Dept Biol, Campus Box 1137, St Louis, MO 63130 USA.
RI Leal, Manuel/A-7220-2010; Glor, Richard/N-4656-2013;
OI Glor, Richard/0000-0002-3359-1631; Jackman, Todd/0000-0002-5391-8136
NR 30
TC 181
Z9 188
U1 2
U2 73
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD JUL 31
PY 2003
VL 424
IS 6948
BP 542
EP 545
DI 10.1038/nature01814
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 706LG
UT WOS:000184454700040
PM 12891355
ER
PT J
AU Olshanii, M
Dunjko, V
AF Olshanii, M
Dunjko, V
TI The short-distance first-order correlation function of the interacting
one-dimensional Bose gas
SO NEW JOURNAL OF PHYSICS
LA English
DT Article
ID IMPENETRABLE BOSONS; QUANTUM FLUIDS; DENSITY-MATRIX; GROUND STATE;
TEMPERATURE; CONFINEMENT; MODELS; TIME
AB We derive exact closed-form expressions for the first few terms of the short-distance Taylor expansion of the one-body correlation function of the Lieb-Liniger gas.
C1 Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Olshanii, M (reprint author), Univ So Calif, Dept Phys & Astron, Los Angeles, CA 90089 USA.
RI Olshanii, Maxim/M-2830-2013
OI Olshanii, Maxim/0000-0003-3629-6002
NR 19
TC 6
Z9 6
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 1367-2630
J9 NEW J PHYS
JI New J. Phys.
PD JUL 28
PY 2003
VL 5
AR 98
DI 10.1088/1367-2630/5/1/398
PG 5
WC Physics, Multidisciplinary
SC Physics
GA 706RG
UT WOS:000184466900002
ER
PT J
AU Chatterjee, P
Hernquist, L
Loeb, A
AF Chatterjee, P
Hernquist, L
Loeb, A
TI Effects of wandering on the coalescence of black hole binaries in
galactic centers
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; galaxies : kinematics and dynamics; galaxies :
nuclei; methods : n-body simulations; stellar dynamics
ID EARLY-TYPE GALAXIES; DYNAMICAL EVOLUTION; ELLIPTIC GALAXIES; MASSIVE
BINARY; HST; SYSTEM; MOTION; NUCLEI
AB We examine whether massive binary black holes in spherically symmetric bulges of galaxies can achieve coalescence through the emission of gravitational radiation under the action of stellar dynamical processes alone. In particular, we address the importance of the Brownian motion of a binary's center of mass to its continued interaction with stellar orbits that allows it to keep hardening. We use an analytical model and N-body simulations to calculate the time required to reach the gravitational radiation-dominated stage. We find that a substantial fraction of all massive binaries in galaxies can coalesce within a Hubble time.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Chatterjee, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 31
TC 28
Z9 28
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 32
EP 41
DI 10.1086/375552
PN 1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600004
ER
PT J
AU Kraft, RP
Vazquez, SE
Forman, WR
Jones, C
Murray, SS
Hardcastle, MJ
Worrall, DM
Churazov, E
AF Kraft, RP
Vazquez, SE
Forman, WR
Jones, C
Murray, SS
Hardcastle, MJ
Worrall, DM
Churazov, E
TI X-ray emission from the hot interstellar medium and southwest radio lobe
of the nearby radio galaxy Centaurus A
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies : active; galaxies : individual (Centaurus A, NGC 5128);
galaxies : ISM; galaxies : jets; radio continuum : galaxies; X-rays :
galaxies
ID MAGNETIC-FIELD STRENGTHS; ACTIVE GALACTIC NUCLEI; COOLING FLOWS; CHANDRA
OBSERVATIONS; ELLIPTIC GALAXY; EMITTING GAS; HYDRA-A; INTRACLUSTER
MEDIUM; HIGH-RESOLUTION; INTERGALACTIC MEDIUM
AB We present results from two Chandra/ACIS-I observations and one XMM-Newton observation of X-ray emission from the interstellar medium (ISM) and the inner radio lobes of the nearby radio galaxy Centaurus A. The ISM has an average radial surface brightness pro. le that is well described by a beta-model pro. le with index beta = 0.40 +/- 0.04 and a temperature of k(B)T(ISM) similar to 0.29 keV beyond 2 kpc from the nucleus. We. nd that diffuse X-ray emission is coincident with the outer half of the southwest radio lobe, and a bright X-ray enhancement is detected along the edge of the lobe. On the basis of energetic and lifetime arguments, we reject a nonthermal explanation for this emission. We model this emission as a thin, hot shell or cap of X-ray emitting plasma surrounding the radio lobe that was created by the supersonic inflation of the lobe. This plasma shell is both hotter than (k(B)T(SH) similar to 2.9 keV) and greatly overpressurized relative to the ambient ISM, indicating supersonic expansion. We estimate that the lobe is expanding into the ISM at approximately Mach 8.5, or 2400 km s(-1). We are not directly observing the bow shock, but rather the cooler, denser material that is accumulating ahead of the contact discontinuity. The thermal energy in the shell is a significant fraction of the thermal energy of the hot ISM, demonstrating the possibility that the hot ISM of early galaxies can be reenergized by outflows from nuclear activity. Interestingly, no similarly bright X-ray emission is detected in or along the edge of the northeast lobe, implying that there are differences in the dynamics and evolution of the kiloparsec-scale radio components.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England.
Moscow Space Res Inst, Moscow 117810, Russia.
Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-31, Cambridge, MA 02138 USA.
RI Hardcastle, Martin/E-2264-2012; Churazov, Eugene/A-7783-2013
OI Hardcastle, Martin/0000-0003-4223-1117;
NR 112
TC 118
Z9 118
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 129
EP 146
DI 10.1086/375533
PN 1
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600010
ER
PT J
AU Muzerolle, J
Hillenbrand, L
Calvet, N
Briceno, C
Hartmann, L
AF Muzerolle, J
Hillenbrand, L
Calvet, N
Briceno, C
Hartmann, L
TI Accretion in young stellar/substellar objects
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; circumstellar matter; stars : emission-line,
Be; stars : low-mass, brown dwarfs; stars : pre-main-sequence
ID T-TAURI STARS; LOW-MASS STARS; ORION-NEBULA-CLUSTER; EMISSION-LINE
DIAGNOSTICS; MAIN-SEQUENCE EVOLUTION; AURIGA MOLECULAR CLOUD; X-RAY
IONIZATION; DISK ACCRETION; BROWN DWARFS; MAGNETOSPHERIC ACCRETION
AB We present a study of accretion in a sample of 45 young, low-mass objects in a variety of star-forming regions and young associations, about half of which are likely substellar. Based primarily on the presence of broad, asymmetric Halpha emission, we have identified 13 objects (similar to30% of our sample) that are strong candidates for ongoing accretion. At least three of these are substellar. We do not detect significant continuum veiling in most of the accretors with late spectral types (M5-M7). Accretion shock models show that lack of measurable veiling allows us to place an upper limit to the mass accretion rates of less than or similar to10(-10) M-circle dot yr(-1). Using magnetospheric accretion models with appropriate ( sub) stellar parameters, we can successfully explain the accretor Halpha emission-line profiles and derive quantitative estimates of accretion rates in the range 10(-12) M-circle dot yr(-1) < (M)over dot < 10(-9) M-circle dot yr(-1). There is a clear trend of decreasing accretion rate with stellar mass, with mean accretion rates declining by 3-4 orders of magnitude over similar to1-0.05 M-circle dot.
C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
CALTECH, Dept Astron, Pasadena, CA 91125 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Ctr Invest Astron, Merida 5010A, Venezuela.
RP Muzerolle, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
NR 78
TC 258
Z9 259
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 266
EP 281
DI 10.1086/375704
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600021
ER
PT J
AU Jayawardhana, R
Mohanty, S
Basri, G
AF Jayawardhana, R
Mohanty, S
Basri, G
TI Evidence for a T Tauri phase in young brown dwarfs
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; planetary systems; stars : formation; stars :
low-mass, brown dwarfs; stars : pre-main-sequence; techniques :
spectroscopic
ID LOW-MASS STARS; EMISSION-LINE DIAGNOSTICS; MAGNETOSPHERIC ACCRETION;
CIRCUMSTELLAR DISKS; FORMING REGION; ASSOCIATION; ROTATION; CLUSTER;
MEMBERS; MODELS
AB As part of a multifaceted program to investigate the origin and early evolution of substellar objects, we present high-resolution Keck optical spectra of 14 very low mass sources in the IC 348 young cluster and the Taurus star-forming cloud. All of our targets, which span a range of spectral types from M5 to M8, exhibit moderate to very strong Halpha emission. In half of the IC 348 objects, the Halpha profiles are broad and asymmetric, indicative of ongoing accretion. Of these, IC 348-355 ( M8) is the lowest mass object to date to show accretion-like Halpha. Three of our similar toM6IC 348 targets with broad Halpha also harbor broad O I (8446 Angstrom) and Ca II (8662 Angstrom) emission, and one shows broad He I (6678 Angstrom) emission; these features are usually seen in strongly accreting classical T Tauri stars. We find that in very low mass accretors, the Halpha profile may be somewhat narrower than that in higher mass stars. We propose that low accretion rates combined with small infall velocities at very low masses can conspire to produce this effect. In the nonaccretors in our sample, Halpha emission is commensurate with, or higher than, saturated levels in field M dwarfs of similar spectral type. Our results constitute the most compelling evidence to date that young brown dwarfs undergo a T Tauri-like accretion phase similar to that in stars. This is consistent with a common origin for most low-mass stars, brown dwarfs, and isolated planetary mass objects.
C1 Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Jayawardhana, R (reprint author), Univ Michigan, Dept Astron, 830 Dennison, Ann Arbor, MI 48109 USA.
NR 31
TC 126
Z9 126
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 282
EP 287
DI 10.1086/375573
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600022
ER
PT J
AU Rho, JH
Reynolds, SP
Reach, WT
Jarrett, TH
Allen, GE
AF Rho, JH
Reynolds, SP
Reach, WT
Jarrett, TH
Allen, GE
TI Near-infrared synchrotron emission from Cassiopeia A
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE acceleration of particles; ISM : individual (Cassiopeia A); supernova
remnants
ID SHOCK-ACCELERATED ELECTRONS; KEPLER SUPERNOVA-REMNANTS; GAMMA-RAY
EMISSION; NONTHERMAL X-RAYS; MAXIMUM ENERGIES; RICH EJECTA; SHELL;
DISCOVERY; RADIO; DUST
AB Recent high-energy observations of Cassiopeia A suggest the presence of synchrotron radiation, implying acceleration of cosmic rays by young supernova remnants. We detect synchrotron emission from Cas A in the near-infrared using Two Micron All-Sky Survey (2MASS) and Palomar 200 inch (5.1 m) PFIRCAM observations. The remnant is detected in the J, H, and K(s) bands using 2MASS: the K(s) band is the brightest, H is moderate, and J is faint. In the J and H bands, bright [Fe II] lines (1.24 and 1.64 mum) are detected spectroscopically. The Palomar observations include K(s)-continuum, narrowband 1.64 mum (centered on [Fe II]) and 2.12 mum [centered on H(2) (1-0)] images. While the narrowband 1.64 mum image shows filamentary and knotty structures, similar to the optical image, the K(s) image shows a relatively smooth, diffuse shell, remarkably similar to the radio image. The H(2) image is identical to the K(s)-continuum image, with surface brightness reduced as expected for the ratio of filter bandwidths, showing no contribution of H(2) lines to the K(s)-band image. The broadband near-infrared fluxes of Cas A are generally consistent with, but a few tens of percent higher than, an extrapolation of the radio fluxes. The hardening to higher frequencies is possibly due to nonlinear shock acceleration and/or spectral index variation across the remnant. We show evidence of spectral index variation across Cas A using the "spectral tomography" technique. The presence of near-infrared synchrotron radiation requires the rolloff frequency to be higher than 1.5 x 10(14) Hz, implying that electrons are accelerated to energies of at least E = 0.3B(mG)(-1/2) ergs, or 0.2 TeV. The morphological similarity in diffuse emission between the radio and K(s)-band images implies that synchrotron losses are not dominant, or we would expect to see a greater concentration in knots. We also show that dust continuum is not significant in the near-infrared emission of Cas A. Our observations show unambiguous evidence that the near-infrared K(s)-band emission of Cas A is from synchrotron emission by accelerated cosmic-ray electrons.
C1 CALTECH, SIRTF Sci Ctr, IPAC, Pasadena, CA 91125 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
Cornell Univ, Ithaca, NY 14853 USA.
N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
RP Rho, JH (reprint author), CALTECH, SIRTF Sci Ctr, IPAC, MS 220-6, Pasadena, CA 91125 USA.
EM rho@ipac.caltech.edu
OI Reach, William/0000-0001-8362-4094
NR 52
TC 20
Z9 20
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 299
EP 310
DI 10.1086/375564
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600024
ER
PT J
AU Heyl, JS
AF Heyl, JS
TI The synoptic swift synergy - Catching gamma-ray bursts before they fly
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gamma rays : bursts
ID OPTICAL AFTERGLOW; SUPERNOVA; GRB-021004
AB The advent of large panoramic photometric surveys of the sky offers the possibly of exploring the association of gamma-ray bursts (GRBs) with supernovae. To date, a few GRBs have been connected possibly with supernovae: GRB 980425-SN 1998bw, GRB 011121-SN 2001ke, GRB 970228, and GRB 980326. A combination of a large detection rate of GRBs and rapid coverage of a large portion of the sky to faint magnitude limits offers the possibility of detecting a supernova preceding an associated GRB or at least placing limits on the rate of association between these two phenomena and the time delay between them. This would provide important constraints on theoretical models for GRBs.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Heyl, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 18
TC 3
Z9 3
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 401
EP 403
DI 10.1086/375699
PN 1
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600033
ER
PT J
AU Boroson, B
Vrtilek, SD
Kallman, T
Corcoran, M
AF Boroson, B
Vrtilek, SD
Kallman, T
Corcoran, M
TI Chandra grating spectroscopy of the X-ray binary 4U 1700-37 in a flaring
state
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : close; stars : individual (4U 1700-37); X-rays : binaries;
X-rays : individual ( 4U 1700-37)
ID QUASI-PERIODIC OSCILLATIONS; STELLAR WIND; VELA X-1; APERIODIC
VARIABILITY; LMC X-4; 4U-1700-37; SPECTRUM; LINES; COMPTONIZATION;
HERCULES-X-1
AB Chandra X-Ray Observatory grating spectra of the supergiant X-ray binary 4U 1700-37 reveal emission lines from hydrogen- and helium-like S, Si, Mg, and Ne in the 4 - 13 Angstrom range. The spectrum also shows fluorescent lines from S and Si and a prominent Fe Kalpha line at 1.94 Angstrom. The lines contribute to the previously unaccounted "soft excess'' in the flux in this range at orbital phi approximate to 0.7. The X-ray source was observed during intermittent flaring, and the strengths of the lines vary with the source state. The widths of the lines (FWHM approximate to 1000 2000 km s(-1)) can result from either Compton scattering or Doppler shifts. Power spectra of the hard X- rays show red noise, and the soft X- rays and lines show in addition quasi-periodic oscillations and a power spectral break. Helium-like triplets of Si and Mg suggest that the gas is not in a pure photoionization equilibrium. We discuss whether resonant scattering could affect the line ratios or whether a portion of the wind may be heated to temperatures T similar to 10(6) K.
C1 MIT, Space Res Ctr, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Boroson, B (reprint author), MIT, Space Res Ctr, Cambridge, MA 02138 USA.
NR 61
TC 26
Z9 27
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP 516
EP 531
DI 10.1086/375636
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EA
UT WOS:000184098600042
ER
PT J
AU Park, S
Hughes, JP
Slane, PO
Burrows, DN
Warren, JS
Garmire, GP
Nousek, JA
AF Park, S
Hughes, JP
Slane, PO
Burrows, DN
Warren, JS
Garmire, GP
Nousek, JA
TI Detection of magnesium-rich ejecta in the middle-aged supernova remnant
N49B
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : individual (N49B); supernova remnants; X-rays : ISM
ID LARGE-MAGELLANIC-CLOUD; CCD IMAGING SPECTROMETER; CHARGE-TRANSFER
INEFFICIENCY; X-RAY-EMISSION; ABUNDANCES; SPECTROSCOPY; ELEMENTS
AB The middle-aged supernova remnant (SNR) N49B in the Large Magellanic Cloud has been observed with the Chandra X-Ray Observatory. The superb angular resolution of Chandra resolves the complex structure of X-ray-emitting filaments across the SNR. All observed features are soft (E < 3 keV), and we find no evidence of either pointlike or extended hard emission within the SNR. Spectral lines from O, Ne, Mg, Si, S, and Fe are present. Equivalent width images for the detected elemental species and spatially resolved spectral analysis reveal the presence of Mg-rich ejecta within the SNR. We find no such enrichment in O or Ne, which may reflect details of the nucleosynthesis process or the heating and cooling of the ejecta as it evolved. The bright circumferential filaments are emission from the shocked dense interstellar medium (ISM). We detect faint diffuse X-ray emission that extends beyond the X-ray-bright filaments toward the west and southeast. These features appear to be the blast wave shock front expanding into lower density portions of the ISM seen in projection. We set an upper limit of &SIM;2 x 10(33) ergs s(-1) on the 0.5-5 keV band X-ray luminosity of any embedded compact object.
C1 Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Park, S (reprint author), Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
NR 22
TC 26
Z9 26
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 20
PY 2003
VL 592
IS 1
BP L41
EP L44
DI 10.1086/377507
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700ED
UT WOS:000184098900011
ER
PT J
AU Li, LX
AF Li, LX
TI Disk accretion flow driven by large-scale magnetic fields: Solutions
with constant specific energy
SO PHYSICAL REVIEW D
LA English
DT Article
ID 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; BLACK-HOLE MAGNETOSPHERE;
ACTIVE GALACTIC NUCLEI; DOMINATED ACCRETION; ANGULAR-MOMENTUM; DYNAMO
ACTION; MHD; INSTABILITY; EXTRACTION; CONVECTION
AB We study the dynamical evolution of a stationary, axisymmetric, and perfectly conducting cold accretion disk containing a large-scale magnetic field around a Kerr black hole, trying to understand the relation between accretion and the transportation of angular momentum and energy. A one-dimensional radial momentum equation is derived near the equatorial plane, which has one intrinsic singularity at the fast critical point. We solve the radial momentum equation for solutions corresponding to an accretion flow that starts from a subsonic state at infinity, smoothly passes the fast critical point, then supersonically falls into the horizon of the black hole. The solutions always have the following features: (1) The specific energy of fluid particles remains constant but the specific angular momentum is effectively removed by the magnetic field. (2) At large radii, where the disk motion is dominantly rotational, the energy density of the magnetic field is equipartitioned with the rotational energy density of the disk. (3) Inside the fast critical point, where radial motion becomes important, the ratio of the electromagnetic energy density to the kinetic energy density drops quickly. The results indicate that: (1) disk accretion does not necessarily imply energy dissipation since magnetic fields do not have to transport or dissipate a lot of energy as they effectively transport angular momentum and (2) when resistivity is small, the large-scale magnetic field is amplified by the shearing rotation of the disk until the magnetic energy density is equipartitioned with the rotational energy density, ending up with a geometrically thick disk. This is in contrast to the evolution of small-scale magnetic fields where if the resistivity is nonzero the magnetic energy density is likely to be equipartitioned with the kinetic energy density associated with local random motions (e.g., turbulence), making a thin Keplerian disk possible.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 54
TC 3
Z9 3
U1 0
U2 0
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2470-0010
EI 2470-0029
J9 PHYS REV D
JI Phys. Rev. D
PD JUL 15
PY 2003
VL 68
IS 2
AR 024022
DI 10.1103/PhysRevD.68.024022
PG 23
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 719XA
UT WOS:000185229300055
ER
PT J
AU Ozanne, CMP
Anhuf, D
Boulter, SL
Keller, M
Kitching, RL
Korner, C
Meinzer, FC
Mitchell, AW
Nakashizuka, T
Dias, PLS
Stork, NE
Wright, SJ
Yoshimura, M
AF Ozanne, CMP
Anhuf, D
Boulter, SL
Keller, M
Kitching, RL
Korner, C
Meinzer, FC
Mitchell, AW
Nakashizuka, T
Dias, PLS
Stork, NE
Wright, SJ
Yoshimura, M
TI Biodiversity meets the atmosphere: A global view of forest canopies
SO SCIENCE
LA English
DT Review
ID TROPICAL FOREST; ELEVATED CO2; HERBIVOROUS INSECTS; TREES; PLANTS;
DIVERSITY; RESPONSES; PATTERNS; ECOLOGY; GROWTH
AB The forest canopy is the functional interface between 90% of Earth's terrestrial biomass and the atmosphere. Multidisciplinary research in the canopy has expanded concepts of global species richness, physiological processes, and the provision of ecosystem services. Trees respond in a species-specific manner to elevated carbon dioxide levels, while climate change threatens plant-animal interactions in the canopy and will likely alter the production of biogenic aerosols that affect cloud formation and atmospheric chemistry.
C1 Univ Surrey Roehampton, Sch Life & Sport Sci, Ctr Res Ecol & Environm, London SW15 3SN, England.
Univ Sao Paulo, Inst Estudos Avancados, BR-05508900 Sao Paulo, Brazil.
Griffith Univ, Environm Sci & Rainforest Cooperat Res Ctr, Nathan, Qld 4111, Australia.
US Forest Serv, Int Inst Trop Forestry, USDA, San Juan, PR 00926 USA.
Univ Basel, Inst Bot, CH-4056 Basel, Switzerland.
US Forest Serv, USDA, Pacific NW Res Stn, Corvallis, OR 97331 USA.
Univ Oxford, Global Canopy Programme, Oxford OX1 3UB, England.
Res Inst Human & Nat, Kamigyo Ku, Kyoto 6020878, Japan.
Japan Sci & Technol Corp, Core Res Evolut Sci & Technol, Osaka, Japan.
Univ Sao Paulo, Inst Astron & Geofis, BR-05508900 Sao Paulo, Brazil.
James Cook Univ N Queensland, Rainforest Cooperat Res Ctr, Cairns, Qld 4870, Australia.
Smithsonian Trop Res Inst, Balboa, Panama.
RP Ozanne, CMP (reprint author), Univ Surrey Roehampton, Sch Life & Sport Sci, Ctr Res Ecol & Environm, West Hill, London SW15 3SN, England.
RI Kitching, Roger/C-5102-2009; Keller, Michael/A-8976-2012; Korner,
Christian/B-6592-2014; Meinzer, Frederick/C-3496-2012; Wright,
Stuart/M-3311-2013; Leite da Silva Dias, Pedro/H-1183-2016
OI Keller, Michael/0000-0002-0253-3359; Wright, Stuart/0000-0003-4260-5676;
Leite da Silva Dias, Pedro/0000-0002-4051-2962
NR 71
TC 139
Z9 165
U1 7
U2 88
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 JUL 11
PY 2003
VL 301
IS 5630
BP 183
EP 186
DI 10.1126/science.1084507
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 699KN
UT WOS:000184056200032
PM 12855799
ER
PT J
AU Fabbiano, G
King, AR
Zezas, A
Ponman, TJ
Rots, A
Schweizer, F
AF Fabbiano, G
King, AR
Zezas, A
Ponman, TJ
Rots, A
Schweizer, F
TI A variable ultraluminous supersoft X-ray source in ''the antennae'':
Stellar-mass black hole or white dwarf?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 4038/4039); galaxies : interactions; galaxies
: peculiar; X-rays : binaries; X-rays : galaxies
ID CHANDRA OBSERVATIONS; GALAXIES NGC-4038/4039; DISCOVERY; BINARIES; M101;
M81
AB The Chandra monitoring observations of "The Antennae'' (NGC 4038/4039) have led to the discovery of a variable, luminous, supersoft source (SSS). This source is detected only at energies below 2 keV and, in 2002 May, reached count rates comparable to those of the nine ultraluminous X-ray sources (ULXs) detected in these galaxies. Spectral fits of the SSS data give acceptable results only for a similar to90 - 100 eV blackbody spectrum with an intrinsic absorption column of N-H similar to (2-3) x 10(21) cm(-2). For a distance of 19 Mpc, the best-fit observed luminosity increases from 1.7 x 10(38) ergs s(-1) in 1999 December to 8.0 x 10(38) ergs s(-1) in 2002 May. The intrinsic, absorption-corrected, best-fit luminosity reaches 1.4 x 10(40) ergs s(-1) in 2002 May. The assumption of unbeamed emission would suggest a black hole of greater than or similar to 100M(.). However, if the emission is blackbody at all times, as suggested by the steep soft spectrum, the radiating area would have to vary by a factor of similar to10(3), inconsistent with gravitational energy release from within a few Schwarzschild radii of a black hole. Viable explanations for the observed properties of the SSS are provided by anisotropic emission from either an accreting nuclear-burning white dwarf or an accreting stellar-mass black hole.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England.
Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Rots, Arnold/0000-0003-2377-2356
NR 25
TC 49
Z9 49
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP 843
EP 849
DI 10.1086/375441
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UF
UT WOS:000184016700024
ER
PT J
AU Bensch, F
Leuenhagen, U
Stutzki, J
Schieder, R
AF Bensch, F
Leuenhagen, U
Stutzki, J
Schieder, R
TI [C I] 492 GHz mapping observations of the high-latitude translucent
cloud MCLD 123.5+24.9
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrochemistry; ISM : abundances; ISM : clouds; ISM : individual (MCLD
123.5+24.9); radio lines : ISM
ID A MOLECULAR CLOUD; ATOMIC CARBON; PHOTODISSOCIATION REGIONS;
INTERSTELLAR CLOUDS; ORION-A; NEUTRAL CARBON; CIRRUS CLOUD; DARK CLOUD;
EMISSION; SUBMILLIMETER
AB We present the first map of the [C I] P-3(1) --> P-3(0) fine-structure transition of neutral carbon made toward a translucent molecular cloud (MCLD 123.5+ 24.9, located in the Polaris Flare). The [C I] observations were made with the Submillimeter Wave Astronomy Satellite and are supplemented by ground-based observations of (CO)-C-12 and (CO)-C-13 rotational transitions. We find that the [C I] emission is spatially extended following the region bright in (CO)-C-12. The [C I] to CO line ratios observed throughout the MCLD 123.5+ 24.9 cloud are relatively low, and the [C I] line flux density is only similar to50% of the emission by the three lowest CO rotational transitions. However, the ratios are still within the range observed along selected lines of sight toward other diffuse and translucent molecular clouds. Assuming LTE conditions for the neutral atomic carbon with an excitation temperature of 8 K derived from the (CO)-C-12 spectra, we derive a total carbon column density of (0.25-1) x 10(17) cm(-2) and a C to CO column density ratio between 0.2 and 1.1. Comparison with a photon-dominated region model shows that the model consistently would require uncomfortably high values for the gas volume density in order to reproduce the low [C I] to CO line ratios observed (n > 10(5) cm(-3)), unless we assume that the line-emitting clumps are embedded in an interclump medium with a density of n < 10(3) cm(-3). The low-density interclump medium does not significantly contribute to the observed [C I] and CO line emission, but the molecular hydrogen in the gas provides an effective shielding for the CO in the embedded clumps by blocking the FUV photons at the frequencies of CO line transition to the predissociation states. This reduces the photodissociation of CO and, thus, the abundance of neutral and ionized carbon in the denser clumps.
C1 Univ Cologne, Inst Phys, D-50937 Cologne, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
LB Kiel, D-24103 Kiel, Germany.
RP Bensch, F (reprint author), Univ Cologne, Inst Phys, Zulpicher Str 77, D-50937 Cologne, Germany.
NR 48
TC 23
Z9 23
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP 1013
EP 1024
DI 10.1086/375393
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UF
UT WOS:000184016700036
ER
PT J
AU Bergin, E
Calvet, N
D'Alessio, P
Herczeg, GJ
AF Bergin, E
Calvet, N
D'Alessio, P
Herczeg, GJ
TI The effects of UV continuum and Ly alpha radiation on the chemical
equilibrium of T Tauri disks
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; astrobiology; astrochemistry; circumstellar
matter; stars : pre-main-sequence; ultraviolet : stars
ID AURIGA MOLECULAR CLOUD; MAIN-SEQUENCE STARS; PROTOPLANETARY DISKS;
ACCRETION DISKS; 2-DIMENSIONAL DISTRIBUTIONS; OSCILLATOR-STRENGTHS;
GASEOUS MOLECULES; COLUMN DENSITIES; YOUNG OBJECTS; X-RAY
AB We show in this Letter that the spectral details of the far-ultraviolet (FUV) radiation fields have a large impact on the chemistry of protoplanetary disks surrounding T Tauri stars. We show that the strength of a realistic stellar FUV field is significantly lower than typically assumed in chemical calculations and that the radiation field is dominated by strong line emission, most notably Lyalpha radiation. The effects of the strong Lyalpha emission on the chemical equilibrium in protoplanetary disks have previously been unrecognized. We discuss the impact of this radiation on molecular observations in the context of a radiative transfer model that includes both direct attenuation and scattering. In particular, Lya radiation will directly dissociate water vapor and may contribute to the observed enhancements of CN/HCN in disks.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58089, Michoacan, Mexico.
Univ Colorado, Joint Inst Lab Astrophys, UCB 440, Boulder, CO 80309 USA.
RP Bergin, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 42
TC 90
Z9 90
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP L159
EP L162
DI 10.1086/377148
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UJ
UT WOS:000184017100022
ER
PT J
AU Bonanos, AZ
Stanek, KZ
AF Bonanos, AZ
Stanek, KZ
TI Reanalysis of Very Large Telescope data for M83 with image subtraction -
Ninefold increase in number of cepheids
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Cepheids; distance scale; galaxies : individual (M83)
ID DETACHED ECLIPSING BINARIES; DIRECT DISTANCES; ADDITIONAL VARIABLES; M31
AB We apply the image-subtraction method in order to reanalyze the ESO Very Large Telescope data on M83 (NGC 5236), obtained and analyzed by Thim et al. Whereas Thim et al. found 12 Cepheids with periods between 12 and 55 days, we find 112 Cepheids with periods ranging from 7 to 91 days as well as similar to60 other variables. These include two candidate eclipsing binaries, which, if confirmed, would be the first optically discovered outside the Local Group. We thus demonstrate that the image-subtraction method is much more powerful for detecting variability, especially in crowded fields. However, Hubble Space Telescope observations are necessary to obtain a Cepheid period-luminosity distance not dominated by blending and crowding. We propose a "hybrid" approach, in which numerous Cepheids are discovered and characterized using large ground-based telescopes and then followed up with the Hubble Space Telescope to obtain precise distances.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Bonanos, Alceste/K-5392-2013
OI Bonanos, Alceste/0000-0003-2851-1905
NR 14
TC 9
Z9 9
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP L111
EP L114
DI 10.1086/377073
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UJ
UT WOS:000184017100010
ER
PT J
AU Hughes, JP
Slane, PO
Park, S
Roming, PWA
Burrows, DN
AF Hughes, JP
Slane, PO
Park, S
Roming, PWA
Burrows, DN
TI An X-ray pulsar in the oxygen-rich supernova remnant G292.0+1.8
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : individual (G292.0+1.8, MSH 11-54); pulsars : individual (PSR
J1124-5916) stars : neutron; supernova remnants; X-rays : individual
(CXOU J112439.1-591620)
ID CASSIOPEIA-A; WIND
AB We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period (P = 0.13530915 s) is consistent with the extrapolation of the radio pulse period of PSR J1124-5916 for a spin-down rate of (P) over dot = 7.6 x 10(-13) s s(-1). The X-ray pulse is single-peaked and broad, with an FWHM width of 0.23P (83degrees). The pulse-averaged X-ray spectral properties of the pulsar are well described by a featureless power-law model with an absorbing column density N(H) = 3.1 x 10(21) cm(-2), a photon index Gamma = 1.6, and an unabsorbed 0.3-10 keV band luminosity L(x) = 7.2 x 10(32) ergs s(-1). We plausibly identify the location of the pulsar's termination shock. Pressure balance between the pulsar wind nebula and the larger synchrotron nebula, as well as lifetime issues for the X-ray-emitting electrons, argue for a particle-dominated pulsar wind nebula that is far from the minimum-energy condition. Upper limits on the surface temperature of the neutron star are at, or slightly below, values expected from "standard" cooling curves. There is no optical counterpart to the new pulsar; its optical luminosity is at least a factor of 5 below that of the Crab pulsar.
C1 Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA.
RP Hughes, JP (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA.
EM jph@physics.rutgers.edu; slane@head-cfa.harvard.edu
NR 19
TC 42
Z9 43
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP L139
EP L142
DI 10.1086/377072
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UJ
UT WOS:000184017100017
ER
PT J
AU Pooley, D
Lewin, WHG
Anderson, SF
Baumgardt, H
Filippenko, AV
Gaensler, BM
Homer, L
Hut, P
Kaspi, VM
Makino, J
Margon, B
McMillan, S
Portegies Zwart, S
van der Klis, M
Verbunt, F
AF Pooley, D
Lewin, WHG
Anderson, SF
Baumgardt, H
Filippenko, AV
Gaensler, BM
Homer, L
Hut, P
Kaspi, VM
Makino, J
Margon, B
McMillan, S
Portegies Zwart, S
van der Klis, M
Verbunt, F
TI Dynamical formation of close binary systems in globular clusters
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : close; globular clusters : general; X-rays : binaries
ID X-RAY SOURCES; NEUTRON-STAR; LUMINOSITY FUNCTIONS; STELLAR DYNAMICS;
EVOLUTION; DISCOVERY; CATALOG; CORE; M15
AB We know from observations that globular clusters are very efficient catalysts in forming unusual short-period binary systems or their offspring, such as low-mass X-ray binaries (LMXBs; neutron stars accreting matter from low-mass stellar companions), cataclysmic variables ( white dwarfs accreting matter from stellar companions), and millisecond pulsars ( rotating neutron stars with spin periods of a few milliseconds). Although there has been little direct evidence, the overabundance of these objects in globular clusters has been attributed by numerous authors to the high densities in the cores, which leads to an increase in the formation rate of exotic binary systems through close stellar encounters. Many such close binary systems emit X-radiation at low luminosities (L-x less than or similar to 10(34) ergs s(-1)) and are being found in large numbers through observations with the Chandra X-Ray Observatory. Here we present conclusive observational evidence of a link between the number of close binaries observed in X-rays in a globular cluster and the stellar encounter rate of the cluster. We also make an estimate of the total number of LMXBs in globular clusters in our Galaxy.
C1 MIT, Ctr Space Res, Cambridge, MA 02139 USA.
Univ Washington, Dept Astron, Seattle, WA 98195 USA.
Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Adv Study, Princeton, NJ 08540 USA.
McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA.
Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands.
RP Pooley, D (reprint author), MIT, Ctr Space Res, 70 Vassar St, Cambridge, MA 02139 USA.
EM dave@mit.edu; lewin@space.mit.edu; anderson@astro.washington.edu;
holger@astron.s.u-tokyo.ac.jp; alex@astron.berkeley.edu;
bgaensler@cfa.harvard.edu; homer@astro.washington.edu; piet@ias.edu;
vkaspi@hep.physics.mcgill.ca; makino@astron.s.u-tokyo.ac.jp;
margon@stsci.edu; steve@kepler.physics.drexel.edu; spz@science.uva.nl;
michiel@astro.uva.nl; f.w.m.verbunt@astro.uu.nl
RI Gaensler, Bryan/F-8655-2010; Baumgardt, Holger/A-5444-2012; Margon,
Bruce/B-5913-2012; Makino, Junichiro/A-9525-2014;
OI Gaensler, Bryan/0000-0002-3382-9558
NR 37
TC 134
Z9 134
U1 0
U2 3
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 10
PY 2003
VL 591
IS 2
BP L131
EP L134
DI 10.1086/377074
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 698UJ
UT WOS:000184017100015
ER
PT J
AU Van Bael, SA
Brawn, JD
Robinson, SK
AF Van Bael, SA
Brawn, JD
Robinson, SK
TI Birds defend trees from herbivores in a Neotropical forest canopy
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
ID TROPHIC CASCADES; FOOD-WEB; IMPACT; DAMAGE; INSECTS; TOP
AB Most forest birds include arthropods in their diet, sometimes specializing on arthropods that consume plant foliage. Experimental tests of whether bird predation on arthropods can reduce plant damage, however, are few and restricted to relatively low-diversity systems. Here, we describe an experimental test in a diverse tropical forest of whether birds indirectly defend foliage from arthropod herbivores. We also compare how the indirect effects of bird predation vary with different levels of foliage productivity in the canopy vs. the understory. For three Neotropical tree species, we observed that birds decreased local arthropod densities on canopy branches and reduced consequent damage to leaves. In contrast, we observed no evidence of bird-arthropod limitation on conspecific saplings in the less productive understory of the same forest. Our results support theory that predicts trophic cascades where productivity is high and suggest that birds play an important role in Neotropical communities by means of their indirect defense of some canopy tree species.
C1 Univ Illinois, Dept Anim Biol, Champaign, IL 61820 USA.
Univ Illinois, Dept Nat Resources & Environm Sci, Champaign, IL 61820 USA.
RP Van Bael, SA (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama.
NR 32
TC 107
Z9 111
U1 1
U2 24
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD JUL 8
PY 2003
VL 100
IS 14
BP 8304
EP 8307
DI 10.1073/pnas.1431621100
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 702KF
UT WOS:000184222500049
PM 12832618
ER
PT J
AU Simkin, T
Fiske, RS
AF Simkin, T
Fiske, RS
TI Krakatoa - The day the world exploded: August 27, 1883
SO SCIENCE
LA English
DT Book Review
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
RP Simkin, T (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA.
NR 6
TC 0
Z9 1
U1 3
U2 11
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 JUL 4
PY 2003
VL 301
IS 5629
BP 50
EP 51
DI 10.1126/science.1086522
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 696YG
UT WOS:000183914700022
ER
PT J
AU Ewe, SML
Sternberg, LD
AF Ewe, SML
Sternberg, LD
TI Seasonal gas exchange characteristics of Schinus terebinthifolius in a
native and disturbed upland community in Everglades National Park,
Florida
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE invasive exotic; everglades; photosynthesis
ID NITROGEN-USE EFFICIENCY; WATER-USE EFFICIENCY; CARBON ISOTOPE
DISCRIMINATION; PHOTOSYNTHETIC CAPACITY; GROWTH; HAWAII; ALLOCATION;
INCREASE; PATTERNS; DECLINE
AB Schinus terebinthifolius Raddi (Schinus) is an invasive exotic plant widely found in Florida and Hawaii. This species is found from the upland pinelands to the mangrove forests of Florida. Dense Schinus infestations have the capacity to displace native species, reduce species diversity and been shown to reduce faunal use of the community.
The purpose of this study was to determine if gas exchange patterns of Schinus were significantly different from native species. This work was part of a larger study to determine if the exotic's physiology contributed to its presence in two upland communities of South Florida. The first was an endemic rock pineland community and the second, a disturbed previously farmed area where Schinus was the canopy dominant. Schinus gas exchange, leaf nitrogen and carbon stable isotope contents were contrasted with four native species for one wet and dry season.
Schinus tended to have higher assimilation (A), mesophyll conductance (g(m)), intrinsic water-use efficiency (WUE) and photosynthetic nitrogen-use efficiency (PNUE) than native species in the pineland site during the wet season but these differences were not statistically significant. There were also no significant differences in conspecific plant responses between the two communities. Seasonal differences were, however, significant for most of the gas exchange parameters at either one or both of the study sites. Wet season A, g(m), nitrogen concentration ([N]), intrinsic WUE, PNUE and carbon stable isotope signatures (delta(13)C) were higher than the dry season, most likely a consequence of greater water availability within the substrate.
Although differences in gas exchange could contribute to the invasiveness of Schinus into native pineland and disturbed upland areas, other aspects of its autoecology also play an important role. (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
Smithsonian Marine Stn, Ft Pierce, FL USA.
RP Ewe, SML (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33124 USA.
NR 45
TC 27
Z9 33
U1 2
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD JUL 3
PY 2003
VL 179
IS 1-3
BP 27
EP 36
AR PII S0378-1127(02)00531-5
DI 10.1016/S0378-1127(02)00531-5
PG 10
WC Forestry
SC Forestry
GA 695ND
UT WOS:000183836300003
ER
PT J
AU Ott, JD
Oran, ES
Anderson, JD
AF Ott, JD
Oran, ES
Anderson, JD
TI A mechanism for flame acceleration in narrow tubes
SO AIAA JOURNAL
LA English
DT Article
ID TO-DETONATION TRANSITION; NUMERICAL-SIMULATION; BOUNDARY-CONDITIONS;
SHOCK; PROPAGATION
C1 Combust Res & Flow Technol, Dublin, PA 18917 USA.
USN, Res Lab, Computat Phys & Fluid Dynam Lab, Washington, DC 20375 USA.
Smithsonian Inst, Natl Air & Space Museum, Aeronaut Div, Washington, DC 20560 USA.
RP Ott, JD (reprint author), Combust Res & Flow Technol, 174 N Main St,Bldg 3,POB 1150, Dublin, PA 18917 USA.
NR 22
TC 36
Z9 40
U1 0
U2 2
PU AMER INST AERONAUT ASTRONAUT
PI RESTON
PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA
SN 0001-1452
J9 AIAA J
JI AIAA J.
PD JUL
PY 2003
VL 41
IS 7
BP 1391
EP 1396
DI 10.2514/2.2088
PG 6
WC Engineering, Aerospace
SC Engineering
GA 698GR
UT WOS:000183990800022
ER
PT J
AU Lellinger, DB
AF Lellinger, DB
TI Nomenclatural and taxonomic notes on the pteridophytes of Costa Rica,
Panama, and Colombia, III
SO AMERICAN FERN JOURNAL
LA English
DT Article
AB The new species Hypolepis rubginopilosula and Polypodium chirripoense are described, the new combinations Blechnum loxense var. stenophyllum, B. l'herminieri subsp. lehmannii, Diplazium ribae, Lastreopsis squamifera, Lomariopsis salicifolia, Pteridium caudatum subsp. arachnoideum, and Tectaria xmicheleriana are made, and three lectotypes are chosen for tropical American ferns.
C1 Natl Museum Nat Hist, Smithsonian Inst, Bot Sect, Washington, DC 20560 USA.
RP Lellinger, DB (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Bot Sect, Washington, DC 20560 USA.
NR 5
TC 5
Z9 8
U1 0
U2 0
PU AMER FERN SOC INC
PI WASHINGTON
PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC
20560 USA
SN 0002-8444
J9 AM FERN J
JI Am. Fern J.
PD JUL-SEP
PY 2003
VL 93
IS 3
BP 146
EP 151
DI 10.1640/0002-8444(2003)093[0146:NATNOT]2.0.CO;2
PG 6
WC Plant Sciences
SC Plant Sciences
GA 726CK
UT WOS:000185580400005
ER
PT J
AU Herken, G
AF Herken, G
TI Comment on book review of "brotherhood of the bomb: The tangled lives
and loyalties of Robert Oppenheimer, Ernest Lawrence, and Edward
Teller," by Gregg Herken [Am. J. Phys. 71(4),411-415 (2003)]
SO AMERICAN JOURNAL OF PHYSICS
LA English
DT Letter
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Herken, G (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER ASSOC PHYSICS TEACHERS AMER INST PHYSICS
PI MELVILLE
PA STE 1 NO 1, 2 HUNTINGTON QUADRANGLE, MELVILLE, NY 11747-4502 USA
SN 0002-9505
J9 AM J PHYS
JI Am. J. Phys.
PD JUL
PY 2003
VL 71
IS 7
BP 647
EP 648
DI 10.1119/1.1579499
PG 2
WC Education, Scientific Disciplines; Physics, Multidisciplinary
SC Education & Educational Research; Physics
GA 692KR
UT WOS:000183660700001
ER
PT J
AU Christy, JH
Baum, JK
Backwell, PRY
AF Christy, JH
Baum, JK
Backwell, PRY
TI Attractiveness of sand hoods built by courting male fiddler crabs, Uca
musica: test of a sensory trap hypothesis
SO ANIMAL BEHAVIOUR
LA English
DT Article
ID SEXUAL SELECTION; CHOICE
AB Courting male fiddler crabs, Uca musica, sometimes build sand hoods at the entrances of their burrows to which they attract females for mating. On average, females visit 17 males in as many minutes before they choose a mate, and they preferentially visit males with hoods. When moving between burrows, fiddler crabs of both sexes sometimes approach and temporarily hide against objects on the surface. Hence, mate-searching females may approach hoods because they resemble (mimic) other objects that crabs approach to reduce their predation risk. We conducted two experiments to test this sensory trap hypothesis. First, we determined whether sexually receptive and nonreceptive female U. musica and nonreceptive female U. stenodactylus, a species that does not build structures, spontaneously approach hoods (replicas), stones, pieces of wood and shells. As predicted by the sensory trap hypothesis, both species, irrespective of sexual receptivity, approached these objects and neither preferred hoods. Second, to determine whether female U. musica show a preference for hoods when they search for a mate, we recorded the frequency with which females approached males with natural hoods, hood replicas, wood, stones and shells. Again as expected, females approached males with these different structures at the same rates. We conclude that hoods are effective mimics of objects that females approach for safety whether they are searching for a mate or not. Males benefit by using this sensory trap because hoods make them more attractive, and receptive females may benefit when they approach hoods because they reduce their mate-search risk. (C) 2003 Published by Elsevier Ltd on behalf of The Association for the Study of Animal Behaviour.
C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama.
RI Baum, Julia/A-4693-2008; Backwell, Patricia/C-8883-2009
NR 21
TC 48
Z9 50
U1 2
U2 10
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
J9 ANIM BEHAV
JI Anim. Behav.
PD JUL
PY 2003
VL 66
BP 89
EP 94
DI 10.1006/anbe.2003.2196
PN 1
PG 6
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA 707CN
UT WOS:000184492000008
ER
PT J
AU Endo, H
Watanabe, K
Hayashi, Y
Matsuzaki, M
Sakai, T
Itoh, T
Koie, H
Kimura, J
Stafford, BL
AF Endo, H
Watanabe, K
Hayashi, Y
Matsuzaki, M
Sakai, T
Itoh, T
Koie, H
Kimura, J
Stafford, BL
TI Three-dimensional CT image analysis of the digging system in the
aardvark
SO ANNALS OF ANATOMY-ANATOMISCHER ANZEIGER
LA English
DT Article
DE aardvark; CT; digging; metacarpal; metatarsal
ID PANDA AILUROPODA-MELANOLEUCA
AB We examined the bone movement in the forepaw and hind paw in the aardvark (Orycteropus afer) by using three-dimensional (3D)-computed tomography (CT) techniques and osteometrical methods to confirm the functional adaptation of the extremities as a digging system. The four metacarpal bones could be strongly bent from the distal carpal bones. The distal end of the second and third metacarpal bones possessed enlarged smooth articulation surfaces that allowed the proximal phalanx to bend at a sharp angle. However, the articulation surface was not well-developed in the distal end of the fourth and fifth metacarpal bones and the proximal phalanx could bend at smaller angle in these two lateral digits. The proximal phalanges sharply crook from the metatarsal in the first, second, third and fourth digits in the hind paw. We suggest that the medial two digits in the forepaw directly contribute to the crushing, when these proximal phalanges crook in the phase of power stroke. In contrast the lateral third and fourth digits may act as sweeper of the crushed soil. These suggestions regarding the different functional adaptation between medial two digits and lateral two digits are consistent with the anatomical data of the forearm musculature. In the hind paw, we suggest that the second, third and fourth digits are functionally similar and that the hind paw may not act as a crushing apparatus but as a running motor or soil-sweeper similarly using these main three digits.
C1 Museum Nat Sci, Dept Zool, Tokyo 1690073, Japan.
Univ Tokyo, Fac Agr, Dept Vet Anat, Tokyo 113, Japan.
Nihon Univ, Coll Bioresources Sci, Dept Prevent Vet Med & Anim Hlth, Kanagawa, Japan.
Nihon Univ, Coll Bioresources Sci, Lab Comprehens Vet Clin Studies, Kanagawa, Japan.
Nihon Univ, Coll Bioresources Sci, Dept Vet Anat, Kanagawa, Japan.
Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA.
Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA.
RP Endo, H (reprint author), Museum Nat Sci, Dept Zool, Tokyo 1690073, Japan.
RI Itou, Takuya/H-7406-2013
NR 10
TC 4
Z9 4
U1 3
U2 13
PU URBAN & FISCHER VERLAG
PI JENA
PA BRANCH OFFICE JENA, P O BOX 100537, D-07705 JENA, GERMANY
SN 0940-9602
J9 ANN ANAT
JI Ann. Anat.-Anat. Anz.
PD JUL
PY 2003
VL 185
IS 4
BP 367
EP 372
DI 10.1016/S0940-9602(03)80063-8
PG 6
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 709TL
UT WOS:000184640400012
PM 12924475
ER
PT J
AU Bonanos, AZ
Stanek, KZ
Sasselov, DD
Mochejska, BJ
Macri, LM
Kaluzny, J
AF Bonanos, AZ
Stanek, KZ
Sasselov, DD
Mochejska, BJ
Macri, LM
Kaluzny, J
TI Direct distances to nearby galaxies using detached eclipsing binaries
and Cepheids. IX. Variables in the field M31Y discovered with image
subtraction
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries : eclipsing; Cepheids; distance scale; galaxies : individual
(M31); stars : variables : other
ID ANDROMEDA GALAXY; MAGELLANIC-CLOUD; STARS; RADII; M-31; IV
AB The DIRECT Project aims to obtain direct distances to two Local Group galaxies, M31 and M33, which occupy a crucial position near the base of the cosmological distance ladder. The first step is to search for detached eclipsing binaries (DEBs) and Cepheids using 1 m class telescopes to select good candidates, which will be followed up spectroscopically on 6.5-10 m class telescopes. In this ninth paper, we present a catalog of variable stars discovered with image subtraction in field M31Y (alpha = 10.degrees97, delta = 41.degrees69; J2000.0). The data were obtained with the Fred Lawrence Whipple Observatory 1.2 m telescope on 25 nights, over a period of 6 months. In our search covering 22' x 22', we discovered 41 eclipsing binaries, 126 Cepheids, and 97 other periodic or nonperiodic variables, including a luminous blue variable candidate, a nova, and a Galactic cataclysmic variable. The catalog of variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Opt Astron Observ, Tucson, AZ 85719 USA.
Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
RP Bonanos, AZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Bonanos, Alceste/K-5392-2013;
OI Bonanos, Alceste/0000-0003-2851-1905; Macri, Lucas/0000-0002-1775-4859
NR 28
TC 39
Z9 39
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2003
VL 126
IS 1
BP 175
EP 186
DI 10.1086/375762
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 696UG
UT WOS:000183905500017
ER
PT J
AU Ridge, NA
Wilson, TL
Megeath, ST
Allen, LE
Myers, PC
AF Ridge, NA
Wilson, TL
Megeath, ST
Allen, LE
Myers, PC
TI A (CO)-C-13 and (CO)-O-18 survey of the molecular gas around young
stellar clusters within 1 kiloparsec of the Sun
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM : clouds; radio emission lines; stars :
formation
ID HERBIG-AE/BE STARS; RADIATION-DRIVEN IMPLOSION; BRIGHT-RIMMED CLOUDS; IR
IMAGING PHOTOMETRY; H-II REGIONS; DENSE CORES; FORMING REGIONS; UNBIASED
SURVEY; HARO OBJECTS; CEPHEUS-A
AB As the first step of a multiwavelength investigation into the relationship between young stellar clusters and their environment, we present fully sampled maps in the J = 1 - 0 lines of (CO)-C-13 and (CO)-O-18 and the J = 2 - 1 line of (CO)-O-18 for a selected group of 30 young stellar groups and clusters within 1 kpc of the Sun. This is the first systematic survey of these regions to date. The clusters range in size from several stars to a few hundred stars. Thirty fields ranging in size from 8' x 8' to 30' x 60' were mapped with 47" resolution simultaneously in the two J = 1 - 0 lines at the Five College Radio Astronomy Observatory. Seventeen sources were mapped over fields ranging in size from 3' x 3' to 13' x 13' in the J = 2 - 1 line with 35" resolution at the Submillimeter Telescope Observatory. We compare the cloud properties derived from each of the three tracers in order to better understand systematic uncertainties in determining masses and line widths. Cloud masses are determined independently using the (CO)-C-13 and (CO)-O-18 transitions; these masses range from 30 to 4000 M-.. Finally, we present a simple morphological classification scheme, which may serve as a rough indicator of cloud evolution.
C1 Univ Massachusetts, Five Coll Radio Astron Observ, Dept Astron, Amherst, MA 01003 USA.
Univ Arizona, Submillimeter Telescope Observ, Tucson, AZ 85721 USA.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ridge, NA (reprint author), Univ Massachusetts, Five Coll Radio Astron Observ, Dept Astron, Amherst, MA 01003 USA.
NR 95
TC 64
Z9 64
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUL
PY 2003
VL 126
IS 1
BP 286
EP 310
DI 10.1086/375455
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 696UG
UT WOS:000183905500026
ER
PT J
AU Malizia, A
Bassani, L
Capalbi, M
Fabian, AC
Fiore, F
Nicastro, F
AF Malizia, A
Bassani, L
Capalbi, M
Fabian, AC
Fiore, F
Nicastro, F
TI A BeppoSAX observation of MKN6
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays : galaxies; galaxies : Seyfert; galaxies : individual : MKN6
ID X-RAY ABSORPTION; GALAXIES; REGIONS; NUCLEUS
AB We have used the BeppoSAX satellite to study the broad band (0.5-100 keV) X-ray spectrum of the Seyfert 1.5 galaxy MKN6. The source is characterized by a power law of Gamma = 1.7(-0.07)(+0.08) and there is no strong evidence for either a reflection bump or a high energy cut-off. We have detected a narrow iron line at 6.4 keV ( rest frame) with an equivalent width of 98(-35+33) eV. MKN6 also exhibits strong and complex absorption. At least two components (N-H1 = 1.34(-0.4)(+0.4) x 10(22) cm(-2) and N-H2 = 4.18(-1.3)(+2.2) x 10(22) cm(-2)) are present and they both partially cover the source with covering fractions of similar to90% and similar to50% respectively. Comparison with a previous ASCA observation indicates that in both absorbing columns the N-H is variable over a 2 year timescale, while the covering fractions are constant over the same amount of time. The state of each absorber is cold or mildly photoionized. The Broad Line Region (BLR) is suggested as the possible location for this complex absorption.
C1 CNR, IASF, I-40129 Bologna, Italy.
ESA, ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Osserv Astron Roma, INAF, I-00044 Monte Porzio Catone, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Malizia, A (reprint author), CNR, IASF, Via Piero Gobetti 101, I-40129 Bologna, Italy.
OI Fiore, Fabrizio/0000-0002-4031-4157; Malizia,
Angela/0000-0002-6558-1163; Nicastro, Fabrizio/0000-0002-6896-1364;
Bassani, Loredana/0000-0003-4858-6963
NR 14
TC 12
Z9 12
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2003
VL 406
IS 1
BP 105
EP 109
DI 10.1051/0004-6361:20030743
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 700EJ
UT WOS:000184099400018
ER
PT J
AU Morales-Rueda, L
Marsh, TR
Steeghs, D
Unda-Sanzana, E
Wood, JH
North, RC
AF Morales-Rueda, L
Marsh, TR
Steeghs, D
Unda-Sanzana, E
Wood, JH
North, RC
TI New results on GP Com
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE accretion, accretion discs; binaries : spectroscopic; line : profiles;
stars : mass-loss; stars : novae, cataclysmic variables; stars :
individual : GP Com
ID DB-WHITE-DWARFS; CATACLYSMIC VARIABLES; FORBIDDEN COMPONENTS; NEUTRAL
HELIUM; STARS; SECONDARIES; SPECTRUM; BINARIES; G61-29; SEARCH
AB We present high resolution optical and UV spectra of the 46 min orbital period, helium binary, GP Com. Our data contains simultaneous photometric correction which confirms the flaring behaviour observed in previous optical and UV data. In this system all lines show a triple peaked structure where the outer two peaks are associated with the accretion disc around the compact object. The main aim of this paper is to constrain the origin of the central peak, also called "central spike". We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-wave is similar to10 km s(-1) indicating that its origin is near the centre of mass of the system, which in this case lies very close to the white dwarf. Our resolution is higher than that of previous data which allows us to resolve structure in the central peak of the line. The central spike in three of the He. lines shows another peak blueshifted with respect to the main peak. We propose that one of the peaks is a neutral helium forbidden transition excited in a high electron density region. This forbidden transition is associated with the permitted one ( the stronger peak in two of the lines). The presence of a high electron density region again favours the white dwarf as their origin. We compute Doppler maps for the emission lines which show three emission regions: an accretion disc, a bright spot and an unidentified low velocity emission region associated with the central spike. We obtain modulation Doppler tomograms for some of the emission lines that map the anisotropic emission from the bright spot region. The HST UV spectra also show a strong flare component and confirm the under abundance of silicon in GP Com.
C1 Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02318 USA.
Univ Keele, Sch Chem & Phys, Astrophys Grp, Keele ST5 5BG, Staffs, England.
Met Off, Bracknell RG12 2SZ, Berks, England.
RP Morales-Rueda, L (reprint author), Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England.
RI Unda-Sanzana, Eduardo/K-3592-2012; Steeghs, Danny/C-5468-2009
OI Unda-Sanzana, Eduardo/0000-0002-7514-8312; Steeghs,
Danny/0000-0003-0771-4746
NR 29
TC 32
Z9 32
U1 0
U2 2
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2003
VL 405
IS 1
BP 249
EP 261
DI 10.1051/0004-6361:20030552
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 689RV
UT WOS:000183507500027
ER
PT J
AU Pirogov, L
Zinchenko, I
Caselli, P
Johansson, LEB
Myers, PC
AF Pirogov, L
Zinchenko, I
Caselli, P
Johansson, LEB
Myers, PC
TI N2H+(1-0) survey of massive molecular cloud cores
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars : formation; ISM : clouds; ISM : molecules; radio lines : ISM
ID H-II REGIONS; YOUNG STELLAR OBJECTS; FAR-INFRARED SOURCES; SOUTHERN H2O
MASERS; STAR-FORMATION; DENSE CORES; DUST CONTINUUM; OUTER GALAXY;
HYPERFINE-STRUCTURE; DARK CLOUDS
AB We present the results of N2H+(1-0) observations of 35 dense molecular cloud cores from the northern and southern hemispheres where massive stars and star clusters are formed. Line emission has been detected in 33 sources, for 28 sources detailed maps have been obtained. Peak N2H+ column densities lie in the range: 3.6 x 10(12)-1.5 x 10(14) cm(-2). Intensity ratios of (01-12) to (23-12) hyperfine components are slightly higher than the LTE value. The optical depth of (23-12) component toward peak intensity positions of 10 sources is similar to0.2-1. In many cases the cores have elongated or more complex structures with several emission peaks. In total, 47 clumps have been revealed in 26 sources. Their sizes lie in the range 0.3-2.1 pc, the range of virial masses is similar to30-3000 M-circle dot. Mean N2H+ abundance for 36 clumps is 5 x 10-10. Integrated intensity maps with axial ratios <2 have been fitted with a power-law radial distribution &SIM;r(-p) convolved with the telescope beam. Mean power-law index for 25 clumps is close to 1.3. For reduced maps where positions of low intensity are rejected mean power-law index is close to unity corresponding to the &SIM;r(-2) density profile provided N2H+ excitation conditions do not vary inside these regions. In those cases where we have relatively extensive and high quality maps, line widths of the cores either decrease or stay constant with distance from the center, implying an enhanced dynamical activity in the center. There is a correlation between total velocity gradient direction and elongation angle of the cores. However, the ratio of rotational to gravitational energy is too low (4 x 10(-4)-7.1 x 10(-2)) for rotation to play a significant role in the dynamics of the cores. A correlation between mean line widths and sizes of clumps has been found. A comparison with physical parameters of low-mass cores is given.
C1 Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod 603950, Russia.
Nizhny Novgorod Univ, Nizhnii Novgorod 603950, Russia.
Univ Helsinki, Helsinki Univ Observ, FIN-00014 Helsinki, Finland.
Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
Onsala Space Observ, S-43992 Onsala, Sweden.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Pirogov, L (reprint author), Russian Acad Sci, Inst Appl Phys, Ulyanova 46, Nizhnii Novgorod 603950, Russia.
OI Zinchenko, Igor/0000-0003-2793-8229
NR 52
TC 62
Z9 63
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUL
PY 2003
VL 405
IS 2
BP 639
EP 654
DI 10.1051/0004-6361:20030659
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691PY
UT WOS:000183615700028
ER
PT J
AU Krivonos, RA
Vikhlinin, AA
Markevitch, ML
Pavlinsky, MN
AF Krivonos, RA
Vikhlinin, AA
Markevitch, ML
Pavlinsky, MN
TI A possible shock wave in the intergalactic medium of the cluster of
galaxies A754
SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS
LA English
DT Article
DE clusters of galaxies; shock waves
ID PHYSICS; A3667
AB observations show the nonequilibrium state of the central part of the cluster, in which a cloud of cold plasma similar to500 kpc in size was identified amid the hotter cluster gas. The X-ray image of A754 exhibits a brightness discontinuity, which can be interpreted as a shock wave in front of a moving cloud of dense gas. The shock parameters are determined from the jump in intergalactic gas density using the ROSAT image. The estimated Mach number is M-1 = 1.71(-0.24)(+0.45) at a 68% confidence level. (C) 2003 MAIK "Nauka/Interperiodica". kalInterperiodica".
C1 Russian Acad Sci, Space Res Inst, Moscow 117810, Russia.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Krivonos, RA (reprint author), Russian Acad Sci, Space Res Inst, Profsoyuznaya Ul 84-32, Moscow 117810, Russia.
NR 12
TC 15
Z9 15
U1 0
U2 1
PU MAIK NAUKA/INTERPERIODICA PUBL
PI MELVILLE
PA C/O AMERICAN INST PHYSICS, 2 HUNTINGTON QUANDRANGLE, STE 1NO1, MELVILLE,
NY 11747-4502 USA
SN 1063-7737
J9 ASTRON LETT+
JI Astron. Lett.-J. Astron. Space Astrophys.
PD JUL
PY 2003
VL 29
IS 7
BP 425
EP 428
DI 10.1134/1.1589859
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 704VF
UT WOS:000184360800001
ER
PT J
AU Erb, DK
Shapley, AE
Steidel, CC
Pettini, M
Adelberger, KL
Hunt, MP
Moorwood, AFM
Cuby, JG
AF Erb, DK
Shapley, AE
Steidel, CC
Pettini, M
Adelberger, KL
Hunt, MP
Moorwood, AFM
Cuby, JG
TI H alpha spectroscopy of galaxies at z > 2: Kinematics and star formation
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : evolution; galaxies : high-redshift; galaxies : kinematics
and dynamics stars : formation
ID LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; LUMINOSITY FUNCTION;
STARBURST GALAXIES; FORMING GALAXIES; FIELD GALAXIES; ULTRAVIOLET
LUMINOSITY; STELLAR POPULATIONS; BRIGHT STARBURST; QSO FIELDS
AB We present near-infrared spectroscopy of Halpha emission lines in a sample of 16 star-forming galaxies at redshifts 2.0 < z < 2.6. Our targets are drawn from a large sample of galaxies photometrically selected and spectroscopically confirmed to lie in this redshift range. We have obtained this large sample with an extension of the broadband U(n)GR color criteria used to identify Lyman break galaxies at z similar to 3. The primary selection criterion for IR spectroscopic observation was proximity to a QSO sight line; we therefore expect the galaxies presented here to be representative of the sample as a whole. Six of the galaxies exhibit spatially extended, tilted Halpha emission lines; rotation curves for these objects reach mean velocities of similar to150 km s(-1) at radii of similar to6 kpc, without corrections for inclination or any other observational effect. The velocities and radii give a mean dynamical mass of (M) greater than or equal to 4 x 10(10) M(circle dot). We have obtained archival Hubble Space Telescope images for two of these galaxies; they are morphologically irregular. One-dimensional velocity dispersions for the 16 galaxies range from similar to50 to similar to260 km s(-1), and in cases in which we have both virial masses implied by the velocity dispersions and dynamical masses derived from the spatially extended emission lines, they are in rough agreement. We compare our kinematic results with similar measurements made at z similar to 3 and find that both the observed rotational velocities and velocity dispersions tend to be larger at z similar to 2 than at z similar to 3. We also calculate star formation rates (SFRs) from the Halpha luminosities and compare them with SFRs calculated from the UV continuum luminosity. We find a mean SFR(Halpha) of 16 M(circle dot) yr(-1) and an average SFR(Halpha)/SFR(UV) ratio of 2.4, without correcting for extinction. We see moderate evidence for an inverse correlation between the UV continuum luminosity and the ratio SFR(Halpha)/SFR(UV), such as might be observed if the UV-faint galaxies suffered greater extinction. We discuss the effects of dust and star formation history on the SFRs and conclude that extinction is the most likely explanation for the discrepancy between the two SFRs.
C1 CALTECH, Dept Astron, Pasadena, CA 91125 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
European So Observ, D-85748 Garching, Germany.
European So Observ, Santiago 19, Chile.
RP Erb, DK (reprint author), CALTECH, Dept Astron, MS 105-24, Pasadena, CA 91125 USA.
EM dke@astro.caltech.edu
NR 59
TC 164
Z9 164
U1 1
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP 101
EP 118
DI 10.1086/375316
PN 1
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QR
UT WOS:000183617400007
ER
PT J
AU McDowell, JC
Clements, DL
Lamb, SA
Shaked, S
Hearn, NC
Colina, L
Mundell, C
Borne, K
Baker, AC
Arribas, S
AF McDowell, JC
Clements, DL
Lamb, SA
Shaked, S
Hearn, NC
Colina, L
Mundell, C
Borne, K
Baker, AC
Arribas, S
TI Chandra observations of extended X-ray emission in Arp 220
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (Arp 220); galaxies : interactions; galaxies :
starburst; X-rays : galaxies
ID ULTRALUMINOUS IRAS GALAXIES; ARP 220; INFRARED GALAXIES; STARBURST
GALAXY; STAR-FORMATION; RING GALAXIES; IC 4553; H-I; MARKARIAN-231;
MORPHOLOGIES
AB We resolve the extended X-ray emission from the prototypical ultraluminous infrared galaxy Arp 220. Extended, faint, edge-brightened, soft X-ray lobes outside the optical galaxy are observed to a distance of 10-15 kpc on each side of the nuclear region. Bright plumes inside the optical isophotes coincide with the optical line emission and extend 11 kpc from end to end across the nucleus. The data for the plumes cannot be fitted by a single-temperature plasma and display a range of temperatures from 0.2 to 1 keV. The plumes emerge from bright, diffuse circumnuclear emission in the inner 3 kpc centered on the Halpha peak, which is displaced from the radio nuclei. There is a close morphological correspondence between the Halpha and soft X-ray emission on all spatial scales. We interpret the plumes as a starburst-driven superwind and discuss two interpretations of the emission from the lobes in the context of simulations of the merger dynamics of Arp 220.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2BW, England.
Univ Illinois, Ctr Theoret Astrophys, Dept Phys, Loomis Lab Phys, Urbana, IL 61801 USA.
Univ Illinois, Ctr Theoret Astrophys, Dept Astron, Loomis Lab Phys, Urbana, IL 61801 USA.
Univ Arizona, Dept Astron, Tucson, AZ 85721 USA.
CSIC, Inst Estructura Mat, E-28006 Madrid, Spain.
Liverpool John Moores Univ, ARI, Wirral CH41 1LD, Cheshire, England.
NASA, Goddard Space Flight Ctr, Raytheon Informat Technol Serv, Greenbelt, MD 20771 USA.
NASA, Goddard Space Flight Ctr, Raytheon Sci Serv, Greenbelt, MD 20771 USA.
Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales.
Space Telescope Sci Inst, ESA Space Telescope Div, Baltimore, MD 21218 USA.
RP McDowell, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 45
TC 53
Z9 53
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP 154
EP 166
DI 10.1086/375289
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QR
UT WOS:000183617400011
ER
PT J
AU Saucedo, J
Calvet, N
Hartmann, L
Raymond, J
AF Saucedo, J
Calvet, N
Hartmann, L
Raymond, J
TI The spatial distribution of fluorescent H-2 emission near T Tauri
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars : formation; stars : individual (T Tauri); stars :
pre-main-sequence; stars : winds, outflows; ultraviolet : stars
ID HUBBLE-SPACE-TELESCOPE; HERBIG-HARO OBJECTS; BINARY-SYSTEM;
MOLECULAR-HYDROGEN; BURNHAMS NEBULA; YOUNG STARS; SPECTRA; CLOUD; JETS;
SPECTROSCOPY
AB New subarcsecond far-UV observations of T Tau with Hubble Space Telescope STIS show spatially resolved structures in the 2" x 2" area around the star. The structures are apparent in multiline emission of fluorescent H-2 pumped by Lyalpha. One emission structure follows the cavity walls observed around T Tau N in scattered light in the optical. A temperature of greater than or equal to1000 K is required to have a high enough population in the H-2 to produce the observed fluorescent lines; in the cool environment of the T Tau system, shock heating is required to achieve this temperature at distances of a few tens of AU. Fluorescent H-2 along the cavity wall represents the best evidence to date for the action of low-density, wide opening angle outflows driving cavities into the molecular medium at scales less than or equal to100 AU. A southern region of emission consists of two arcs, with shape and orientation similar to the arcs of H-2 2.12 mum and forbidden-line emission crossing the outflow associated with the embedded system T Tau S. This region is located near the centroid of forbidden-line emission at the blueshifted lobe of the north-south outflow.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
RP Saucedo, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 37
TC 31
Z9 31
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP 275
EP 282
DI 10.1086/374885
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QR
UT WOS:000183617400019
ER
PT J
AU Garcia, MR
Miller, JM
McClintock, JE
King, AR
Orosz, J
AF Garcia, MR
Miller, JM
McClintock, JE
King, AR
Orosz, J
TI Resolved jets and long-period black hole X-ray novae
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE novae, cataclysmic variables; X-rays : binaries
ID RXTE SPECTRAL OBSERVATIONS; MICROQUASAR XTE J1550-564; TRANSIENT GRO
J1655-40; RADIO-EMISSION; SUPERLUMINAL SOURCE; RELATIVISTIC JETS; SOURCE
A0620-00; ENERGY-SPECTRA; NEUTRON-STAR; LIGHT CURVES
AB In this brief note we point out that the four spatially resolved relativistic jets among the 14 dynamically confirmed black hole X-ray novae are all in systems with long orbital periods. Many shorter period systems show transient radio outbursts that are attributed to jets, but these jets have not been spatially resolved. Super-Eddington accretion has been suggested as a requirement for jet formation and may be consistent with our compilation of luminosities, but some super-Eddington outbursts did not form spatially resolved jets. We speculate that some as yet unknown process (or combination of processes) favors formation of substantially larger jets in long-period systems. Two short-period systems show evidence of being extended, but have not been resolved into multiple components, as the long-period systems have.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England.
San Diego State Univ, Dept Astron, San Diego, CA 92182 USA.
RP Garcia, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM garcia@cfa.harvard.edu; jmmiller@cfa.harvard.edu; jem@cfa.harvard.edu;
ark@astro.le.ac.uk; orosz@zwartgat.sdsu.edu
NR 107
TC 27
Z9 27
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP 388
EP 396
DI 10.1086/375218
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QR
UT WOS:000183617400029
ER
PT J
AU Goldberg, D
Mazeh, T
Latham, DW
AF Goldberg, D
Mazeh, T
Latham, DW
TI On the mass-ratio distribution of spectroscopic binaries
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : spectroscopic; Galaxy : halo; methods : statistical; stars :
formation; stars : fundamental parameters
ID PROPER-MOTION STARS; DA WHITE-DWARFS; SOLAR-TYPE STARS; ORBITAL
SOLUTIONS; SAMPLE; EVOLUTION; FRAGMENTATION; MULTIPLICITY; SECONDARIES;
PHOTOMETRY
AB In this paper we derive the mass-ratio and secondary-mass distributions of a large, well-defined, complete sample of 129 spectroscopic binaries with periods between 1 and 2500 days. The binaries, whose orbits were published recently, were detected by a systematic radial-velocity survey of a sample of more than 1400 large proper motion stars. Three features stand out in the mass-ratio distribution: a rise as the mass ratio goes down to q similar to 0.2, a sharp drop below q similar to 0.2, and a smaller peak at q similar to 0.8. Another way to characterize the results is to state that the distribution includes two "populations," one with a high asymmetric peak at q similar to 0.2 and another with a smaller peak at q similar to 0.8, while the minimum between the two populations is centered at q similar to 0.55. The size of the binary sample allows us to divide it into two subsamples and look for differences in the mass-ratio distributions of the two subsamples. We performed two different divisions: one into Galactic halo versus disk populations, and the other into high- and low-mass primary stars ( above and below 0.67 M-circle dot). The former division yields differences with moderate statistical significance of 88%, while the latter is more significant at a level of 97%. Our analysis suggests that the rise toward low mass ratios does not appear in the mass-ratio distribution of the halo binaries. The other separation shows a broad peak at mass ratio of q similar to 0.8-1 for the subsample of binaries with low-mass primaries but no corresponding peak in the subsample with high- mass primaries. We discuss our findings and their application to theories of binary formation.
C1 Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Goldberg, D (reprint author), Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel.
NR 67
TC 41
Z9 41
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP 397
EP 405
DI 10.1086/345990
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QR
UT WOS:000183617400030
ER
PT J
AU Grav, T
Holman, MJ
Kavelaars, JJ
AF Grav, T
Holman, MJ
Kavelaars, JJ
TI The short rotation period of Nereid
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planets and satellites : individual (Nereid)
ID CHAOTIC ROTATION; HYPERION; NEPTUNE; SATELLITES; PHOTOMETRY; DYNAMICS
AB We determine the period, p = 11.52 +/- 0.14 hr, and a light-curve peak-to-peak amplitude, a = 0.029 +/- 0.003 mag, of the Neptunian irregular satellite Nereid. If the light-curve variation is due to albedo variations across the surface, rather than solely to the shape of Nereid variations, the rotation period would be a factor of 2 shorter. In either case, such a rotation period and light-curve amplitude, together with Nereid's orbital period, p = 360.14 days, imply that Nereid is almost certainly in a regular rotation state, rather than the chaotic rotation state suggested in work of Schaefer & Schaefer and of Dobrovolskis. Assuming that Nereid is perfectly spherical, the albedo variation is 3% across the observed surface. Assuming a uniform geometric albedo, the observed cross-sectional area varies by 3%. We caution that the light curve found in this Letter only sets limits on the combination of albedo and physical irregularity and that we cannot determine the orientation of Nereid's spin axis from our data.
C1 Univ Oslo, Inst Theoret Astrophys, N-0359 Oslo, Norway.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Res Council Canada, Victoria, BC V9E 2E7, Canada.
RP Grav, T (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0359 Oslo, Norway.
EM tommy.grav@astro.uio.no; mholman@cfa.harvard.edu;
jj.kavelaars@nrc-cnrc.gc.ca
NR 24
TC 14
Z9 15
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP L71
EP L74
DI 10.1086/377067
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QZ
UT WOS:000183618100018
ER
PT J
AU Kastner, JH
Balick, B
Blackman, EG
Frank, A
Soker, N
Vrtilek, SD
Li, JQ
AF Kastner, JH
Balick, B
Blackman, EG
Frank, A
Soker, N
Vrtilek, SD
Li, JQ
TI A compact X-ray source and possible X-ray jets within the planetary
nebula Menzel 3
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : jets and outflows; planetary nebulae : individual (Menzel 3);
stars : AGB and post-AGB; stars : mass loss; stars : winds, outflows
ID PREPLANETARY NEBULAE; BINARY-SYSTEMS; R-AQUARII; EMISSION; STARS; MZ-3;
DISCOVERY; NGC-7027; OUTFLOW; WINDS
AB We report the discovery, by the Chandra X-Ray Observatory, of X-ray emission from the bipolar planetary nebula Menzel 3. In Chandra CCD imaging, Mz 3 displays hot [similar to(3-6) x 10(6) K] gas within its twin, coaxial bubbles of optical nebulosity as well as a compact X-ray source at the position of its central star(s). The brightest diffuse X-ray emission lies along the polar axis of the optical nebula, suggesting a jetlike configuration. The observed combination of an X-ray-emitting point source and possible X-ray jet(s) is consistent with models in which accretion disks and, potentially, magnetic fields shape bipolar planetary nebulae via the generation of fast, collimated outflows.
C1 Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA.
Univ Washington, Dept Astron, Seattle, WA 98195 USA.
Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
Dept Phys, IL-36006 Oranim, Tivon, Israel.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kastner, JH (reprint author), Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA.
NR 37
TC 51
Z9 51
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP L37
EP L40
DI 10.1086/376979
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QZ
UT WOS:000183618100010
ER
PT J
AU Stanek, KZ
Matheson, T
Garnavich, PM
Martini, P
Berlind, P
Caldwell, N
Challis, P
Brown, WR
Schild, R
Krisciunas, K
Calkins, ML
Lee, JC
Hathi, N
Jansen, RA
Windhorst, R
Echevarria, L
Eisenstein, DJ
Pindor, B
Olszewski, EW
Harding, P
Holland, ST
Bersier, D
AF Stanek, KZ
Matheson, T
Garnavich, PM
Martini, P
Berlind, P
Caldwell, N
Challis, P
Brown, WR
Schild, R
Krisciunas, K
Calkins, ML
Lee, JC
Hathi, N
Jansen, RA
Windhorst, R
Echevarria, L
Eisenstein, DJ
Pindor, B
Olszewski, EW
Harding, P
Holland, ST
Bersier, D
TI Spectroscopic discovery of the supernova 2003dh associated with GRB
030329
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : distances and redshifts; gamma rays : bursts; supernovae :
general; supernovae : individual (SN 2003dh)
ID GAMMA-RAY BURST; OPTICAL AFTERGLOW; STANDARD STARS; SN 1998BW;
FOLLOW-UP; SPECTROPHOTOMETRY; SPECTROGRAPH; GRB-011121; HYPERNOVA;
TELESCOPE
AB We present early observations of the afterglow of GRB 030329 and the spectroscopic discovery of its associated supernova SN 2003dh. We obtained spectra of the afterglow of GRB 030329 each night from March 30.12 (0.6 days after the burst) to April 8.13 (UT) (9.6 days after the burst). The spectra cover a wavelength range of 350-850 nm. The early spectra consist of a power-law continuum (F-v proportional to v(-0.9)) with narrow emission lines originating from H II regions in the host galaxy, indicating a low redshift of. However, our spectra taken z = 0.1687 after 2003 April 5 show broad peaks in flux characteristic of a supernova. Correcting for the afterglow emission, we find that the spectrum of the supernova is remarkably similar to the Type Ic "hypernova" SN 1998bw. While the presence of supernovae has been inferred from the light curves and colors of gamma-ray burst afterglows in the past, this is the first direct, spectroscopic confirmation that a subset of classical gamma-ray bursts originate from supernovae.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA.
Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
Smithsonian Inst, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA.
Campanas Observ, La Serena, Chile.
Cerro Tololo Interamer Observ, La Serena, Chile.
Univ Arizona, Steward Observ, Tucson, AZ 85718 USA.
Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA.
Princeton Univ Observ, Princeton, NJ 08544 USA.
Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA.
RP Stanek, KZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Hathi, Nimish/J-7092-2014
OI Hathi, Nimish/0000-0001-6145-5090
NR 45
TC 842
Z9 850
U1 2
U2 10
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP L17
EP L20
DI 10.1086/376976
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QZ
UT WOS:000183618100005
ER
PT J
AU Yoshida, N
Sokasian, A
Hernquist, L
Springel, V
AF Yoshida, N
Sokasian, A
Hernquist, L
Springel, V
TI Early structure formation and reionization in a warm dark matter
cosmology
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology : theory; dark matter; early universe; stars : formation
ID NUMERICAL COSMOLOGY; 1ST STARS; UNIVERSE; CONSTRAINTS
AB We study the first structure formations in Lambda-dominated universes using large cosmological N-body/smoothed particle hydrodynamics simulations. We consider a standard Lambda cold dark matter (CDM) model and a Lambda warm dark matter (WDM) model in which the mass of the dark matter particles is taken to be m(X) = 10 keV. The linear power spectrum for the LambdaWDM model has a characteristic cutoff at a wavenumber k = 200 Mpc(-1), suppressing the formation of low- mass (<10(6) M-circle dot) nonlinear objects early on. The absence of low- mass halos in the WDM model makes the formation of primordial gas clouds with molecular hydrogen very inefficient at high redshifts. The first star-forming gas clouds form at z approximate to 21 in the WDM model, considerably later than in the CDM counterpart, and the abundance of these gas clouds differs by an order of magnitude between the two models. We carry out radiative transfer calculations by embedding massive Population III stars in the gas clouds. We show that the volume fraction of ionized gas rises up close to 100% by z = 18 in the CDM case, whereas that of the WDM model remains extremely small at a level of a few percent. Thus, the WDM model with m(X) = 10 keV is strongly inconsistent with the high optical depth observed by the Wilkinson Microwave Anisotropy Probe satellite.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Astrophys, D-85741 Garching, Germany.
RP Yoshida, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Yoshida, Naoki/A-4305-2011
NR 25
TC 92
Z9 92
U1 1
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUL 1
PY 2003
VL 591
IS 1
BP L1
EP L4
DI 10.1086/376963
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 691QZ
UT WOS:000183618100001
ER
PT J
AU Beadell, JS
Schreiber, EA
Schreiber, RW
Schenk, GA
Doherty, PF
AF Beadell, JS
Schreiber, EA
Schreiber, RW
Schenk, GA
Doherty, PF
TI Survival of Brown Boobies (Sula leucogaster) at Johnston Atoll: A
long-term study
SO AUK
LA English
DT Article
ID NINO-SOUTHERN OSCILLATION; EL-NINO; MARKED ANIMALS; BREEDING
PROBABILITIES; POPULATIONS; VARIABILITY; SEABIRDS; PACIFIC
AB Survival of Brown Boobies (Sula leucogaster) at Johnston Atoll was examined over a 17-year period using capture-mark-recapture analysis. Annual adult survival was estimated to be 0.90 +/- 0.01 (SE). Variation in survival did not correspond to either local environmental fluctuation or more widespread disturbances associated with El Nino-Southern Oscillation events, and a time-invariant model of survival was best supported by our data. Absence of major oceanographic anomalies in the immediate vicinity of Johnston Atoll may contribute to relatively high and invariant survival in Brown Boobies.
C1 Natl Museum Nat Hist, Bird Dept, Washington, DC 20560 USA.
Smithsonian Inst, Genet Program, Washington, DC 20008 USA.
Museum Hist Nat, Los Angeles, CA 90007 USA.
Colorado State Univ, Dept Fishery & Wildlife Biol, Ft Collins, CO 80512 USA.
RP Schreiber, EA (reprint author), Natl Museum Nat Hist, Bird Dept, E 607 MRC 116, Washington, DC 20560 USA.
NR 41
TC 11
Z9 11
U1 1
U2 7
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
J9 AUK
JI AUK
PD JUL
PY 2003
VL 120
IS 3
BP 811
EP 817
DI 10.1642/0004-8038(2003)120[0811:SOBBSL]2.0.CO;2
PG 7
WC Ornithology
SC Zoology
GA 713AB
UT WOS:000184830800022
ER
PT J
AU Meese, RJ
Neronov, VM
Alestchenko, GM
Ruggiero, M
AF Meese, RJ
Neronov, VM
Alestchenko, GM
Ruggiero, M
TI Rapid acquisition and dissemination of standardized biological
inventories from Russian Biosphere Reserves
SO BIODIVERSITY AND CONSERVATION
LA English
DT Article
DE biodiversity; biological inventory; biosphere reserve; nomenclature;
Russia; systematics; zapovednik
ID WESTERN
AB We accumulate, standardize, and disseminate the results of biological inventories of 21 protected areas in the Russian Federation; each of these areas has been recognized by UNESCO's Man and the Biosphere (MAB) program as a Biosphere Reserve. These inventories, comprising 4702 species of plants and 1094 species of vertebrate animals of the breadth of Russia, represent 20% of the vascular flora and 73% of the vertebrate fauna of Russia and are made widely available for the first time. We describe an approach to the development and Internet availability of large databases of species inventories which were produced through the provision of custom biological inventory software supported by training, cost-free distribution, and a modest amount of taxonomic support. Our experiences also highlight the essential role of an active national office in a system of protected areas. Our approach overcomes many of the obstacles inherent in previous and existing attempts to assemble the results of biological inventories derived from a variety of sources. We suggest a similar application of biological inventory software, supported by national coordination, as an effective means to provide access to species inventories of a system of protected areas. Standardized, taxonomically current species inventories are essential components of regional and global conservation efforts.
C1 Univ Calif Davis, Informat Ctr Environm, Dept Environm Sci & Policy, Davis, CA 95616 USA.
Russian MAB Comm, Moscow, Russia.
Natl Museum Nat Hist, Smithsonian Inst, Biodivers Programs ITIS, Washington, DC 20560 USA.
RP Meese, RJ (reprint author), Univ Calif Davis, Informat Ctr Environm, Dept Environm Sci & Policy, Davis, CA 95616 USA.
RI Neronov, Valery/C-3959-2014
NR 17
TC 0
Z9 0
U1 1
U2 3
PU KLUWER ACADEMIC PUBL
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0960-3115
J9 BIODIVERS CONSERV
JI Biodivers. Conserv.
PD JUL
PY 2003
VL 12
IS 7
BP 1421
EP 1429
DI 10.1023/A:1023685928666
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 675WZ
UT WOS:000182721700007
ER
PT J
AU Rehse, T
Kress, WJ
AF Rehse, T
Kress, WJ
TI Distichochlamys rubrostriata (Zingiberaceae), a new species from
northern Vietnam
SO BRITTONIA
LA English
DT Article
DE Distichochlamys; Zingiberaceae; Zingibereae; Scaphochlamys; Vietnam;
southeast Asia
AB A third species of the until recently monotypic genus Distichochlamys (Zingiberaceae) is described from living and preserved material collected in northern Vietnam. Distichochlamys rubrostriata is distinguished from the original species, D. citrea, and the recently described D. orlowii, on the basis of leaf, inflorescence bract, lateral staminode, and labellum characters.
C1 Duke Univ, Dept Biol, Durham, NC 27708 USA.
Natl Museum Nat Hist, Smithsonian Inst, US Natl Herbarium, Washington, DC 20560 USA.
RP Rehse, T (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA.
NR 9
TC 1
Z9 2
U1 0
U2 0
PU NEW YORK BOTANICAL GARDEN
PI BRONX
PA PUBLICATIONS DEPT, BRONX, NY 10458 USA
SN 0007-196X
J9 BRITTONIA
JI Brittonia
PD JUL-AUG
PY 2003
VL 55
IS 3
BP 205
EP 208
DI 10.1663/0007-196X(2003)055[0205:DRZANS]2.0.CO;2
PG 4
WC Plant Sciences
SC Plant Sciences
GA 703YD
UT WOS:000184309800001
ER
PT J
AU Eberhard, WG
AF Eberhard, WG
TI Sexual behavior and morphology of Themira minor (Diptera : Sepsidae)
males and the evolution of male sternal lobes and genitalic surstyli
SO CANADIAN ENTOMOLOGIST
LA English
DT Article
ID FUNCTIONAL-MORPHOLOGY; FLIES DIPTERA; COURTSHIP; MICROSEPSIS;
COPULATION; CYNIPSEA
AB Probable ancestral types of courtship behavior for most sepsid flies were deduced from the behavior and morphology of a species in the relatively basal genus Themira. At least three of the five behavior patterns used by Themira minor (Haliday) males to court females prior to and during copulation are shared with other, more derived groups. During copulation the male's sternal lobes were rotated so that their brushes of long setae were fanned apart and may tap the female. The morphology of the tips of the male's genitalic surstyli and the muscles attached to them indicate that they are also moveable. This trait, which occurs in several other distantly related species, probably serves to squeeze the female during copulation. Thus, contrary to the impression from previous studies, elaborate courtship before and during copulation may be widespread among sepsids.
C1 Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad, Costa Rica.
Ciudad Sanitaria & Univ Vall Hebron, Escuela Biol, Ciudad, Costa Rica.
RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, Ciudad, Costa Rica.
NR 22
TC 15
Z9 15
U1 1
U2 9
PU ENTOMOL SOC CANADA
PI OTTAWA
PA 393 WINSTON AVE, OTTAWA, ONTARIO K2A 1Y8, CANADA
SN 0008-347X
J9 CAN ENTOMOL
JI Can. Entomol.
PD JUL-AUG
PY 2003
VL 135
IS 4
BP 569
EP 581
PG 13
WC Entomology
SC Entomology
GA 700YU
UT WOS:000184139400005
ER
PT J
AU Klemm, DJ
Daniels, BA
Moser, WE
Lester, RJG
AF Klemm, DJ
Daniels, BA
Moser, WE
Lester, RJG
TI Biology of the leech Actinobdella inequiannulata Moore, 1901 (Annelida :
Hirudinea : Rhynchobdellida : Glossiphoniidae), parasitic on the white
sucker, Catostomus commersoni Lacepede, 1803, and the longnose sucker,
Catostomus catostomus Forster, 1773, in Algonquin Provincial Park,
Ontario, Canada
SO COMPARATIVE PARASITOLOGY
LA English
DT Article
DE benthic invertebrate; freshwater annelid; feeding behavior; fish
parasite; leech; parasitism; Actinobdella annectens; Actinobdella
inequiannulata; Actinobdella pediculata; Actinobdella triannulata;
Myzobdella lugubris; white sucker; Catostomus commersoni; longnose
sucker; Catostomus catostomus; Algonquin Provincial Park; Ontario;
Canada
ID HELOBDELLA-STAGNALIS L; FRESH-WATER LEECHES; LIFE-HISTORY; SOUTH-WALES;
POPULATION; RECORDS; RIVER; CYCLE; LAKE
AB Actinobdella inequiannulata was found on the white sucker. Catostomus commersoni, and less frequently on the longnose sucker, Catostomus catostomus, in Algonquin Provincial Park, Ontario, Canada. Catostomus commersoni parasitized with Act. inequiannulata was collected from July to October 1973 and May to October 1974. In May and October, less than 3% of the fish carried leeches. In July, 80% of the fish were parasitized with an average of 1.5 leeches/fish. Observations on leech weight suggest that young leeches attach to fish from May to September, some mature in July, and a second generation of leeches reparasitize the fish in August and September. The mean size of leeches on suckers increased from May until July, after which the size remained relatively constant. Leeches produced characteristic lesions on the opercula of suckers. Fully developed lesions on fish opercula produced by aggregated leeches had varying amounts of central erosion, extravasation, dermal and epidermal hyperplasia, and necrosis.
C1 US EPA, Off Res & Dev, Natl Exposure Res Lab, Ecosyst Res Branch,Ecol Exposure Res Div, Cincinnati, OH 45268 USA.
Smithsonian Inst, Natl Museum Nat Hist, ADP Off, Washington, DC 20560 USA.
Univ Queensland, Dept Microbiol & Parasitol, Brisbane, Qld 4072, Australia.
RP Klemm, DJ (reprint author), US EPA, Off Res & Dev, Natl Exposure Res Lab, Ecosyst Res Branch,Ecol Exposure Res Div, Cincinnati, OH 45268 USA.
EM klemm.Donald@epa.gov; daniels.bruce@nmnh.si.edu;
moser.William@nmnh.si.edu; r.lester@mail.box.uq
NR 40
TC 4
Z9 4
U1 3
U2 7
PU HELMINTHOLOGICAL SOC WASHINGTON
PI LAWRENCE
PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS
66044 USA
SN 1525-2647
EI 1938-2952
J9 COMP PARASITOL
JI Comp. Parasitol.
PD JUL
PY 2003
VL 70
IS 2
BP 120
EP 127
DI 10.1654/4064
PG 8
WC Parasitology; Zoology
SC Parasitology; Zoology
GA 701XH
UT WOS:000184193900003
ER
PT J
AU Dupuis, AP
Marra, PP
Kramer, LD
AF Dupuis, AP
Marra, PP
Kramer, LD
TI Serologic evidence of West Nile virus transmission, Jamaica, West Indies
SO EMERGING INFECTIOUS DISEASES
LA English
DT Article
ID CROSS-NEUTRALIZATION; BIRDS; ARBOVIRUSES; FLAVIVIRUSES; INFECTION
AB In spring 2002, an intensive avian serosurvey was initiated in Jamaica, Puerto Rico, and Mexico. We collected >1,600 specimens from resident and nonresident neotropical migratory birds before their northerly migrations. Plaque reduction neutralization test results indicated specific neutralizing antibodies to West Nile virus in 11 resident species from Jamaica.
C1 New York State Dept Hlth, Slingerlands, NY USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Dupuis, AP (reprint author), Griffin Lab, 5668 State Farm Rd, Slingerlands, NY 12159 USA.
FU ODCDC CDC HHS [U50/CCU320544-01]
NR 18
TC 90
Z9 102
U1 0
U2 5
PU CENTER DISEASE CONTROL
PI ATLANTA
PA ATLANTA, GA 30333 USA
SN 1080-6040
J9 EMERG INFECT DIS
JI Emerg. Infect. Dis
PD JUL
PY 2003
VL 9
IS 7
BP 860
EP 863
PG 4
WC Immunology; Infectious Diseases
SC Immunology; Infectious Diseases
GA 698WL
UT WOS:000184022300017
PM 12890329
ER
PT J
AU de Oliveira, CR
Ruiz-Miranda, CR
Kleiman, DG
Beck, BB
AF de Oliveira, CR
Ruiz-Miranda, CR
Kleiman, DG
Beck, BB
TI Play behavior in juvenile golden lion tamarins (Callitrichidae :
Primates): Organization in relation to costs
SO ETHOLOGY
LA English
DT Article
ID COTTON-TOP TAMARINS; SOCIAL PLAY; LEONTOPITHECUS-ROSALIA;
SQUIRREL-MONKEYS; HABITAT QUALITY; GELADA BABOONS; MACACA-MULATTA;
VIGILANCE; ECOLOGY; VOCALIZATIONS
AB Play is a complex behavior that is widespread among vertebrates. Despite the potential benefits for the development of social, cognitive and motor skills, play behavior has costs: energy expenditure, and the risks of injury and predation. As the fitness benefits of play are presumably to be gained as adults, we expect young animals to minimize its immediate costs. Here, we describe play behavior in golden lion tamarins (GLTs) (Leontopithecus rosalia ) and test cost-minimizing hypotheses. We collected data on play behavior and adult vigilance in nine groups (four wild and five supplemented, the latter deriving from a reintroduction) of wild-living lion tamarins (16 infants) in Brazil. Results showed that play occupied 3.8% of the activity budget, occurred during the hottest times of the day, and was characterized by being mainly social, involving partners of different ages, and sometimes different species. We found no differences in playing time between wild and supplemented groups. The lion tamarins played less in 'dangerous' substrates (canopy branches and forest floor), and more in 'safe' substrates (large branches and vine tangles), and favored playing in the center of the group over the periphery. The reproductive animals were vigilant during 78% of the time the infants were playing, and were mostly oriented away from the playing animals. The observed organization of play behavior suggests that juvenile GLTs minimize the risk of predation and accidental injuries, but do not seem to minimize energy expenditure and the risks of social injuries. The social-cognitive benefits acquired from experience of older partners during play may overcome the costs of the latter behavior, and because little time was spent in play, the energetic costs may be inconsequential.
C1 Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, CBB, BR-28015620 Campos Dos Goytacazes, RJ, Brazil.
Univ Sao Paulo, Dept Psicobiol, BR-14049 Ribeirao Preto, Brazil.
Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA.
RP Ruiz-Miranda, CR (reprint author), Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, CBB, Av Alberto Lamego 2000, BR-28015620 Campos Dos Goytacazes, RJ, Brazil.
RI Ruiz-Miranda, Carlos/A-4719-2008; Ruiz-Miranda, Carlos/H-7308-2015;
Ruiz, Carlos/I-4446-2016
OI Ruiz-Miranda, Carlos/0000-0001-9786-5315; Ruiz-Miranda,
Carlos/0000-0001-7360-0304;
NR 85
TC 17
Z9 17
U1 6
U2 49
PU BLACKWELL VERLAG GMBH
PI BERLIN
PA KURFURSTENDAMM 57, D-10707 BERLIN, GERMANY
SN 0179-1613
J9 ETHOLOGY
JI Ethology
PD JUL
PY 2003
VL 109
IS 7
BP 593
EP 612
DI 10.1046/j.1439-0310.2003.00901.x
PG 20
WC Psychology, Biological; Behavioral Sciences; Zoology
SC Psychology; Behavioral Sciences; Zoology
GA 697TK
UT WOS:000183959200005
ER
PT J
AU Dudar, JC
Waye, JS
Saunders, SR
AF Dudar, JC
Waye, JS
Saunders, SR
TI Determination of a kinship system using ancient DNA, mortuary practice,
and historic records in an Upper Canadian pioneer cemetery
SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY
LA English
DT Article
DE ancient DNA; kinship system; mortuary practice; historic cemetery; Upper
Canadian history
ID TANDEM REPEAT LOCI; 19TH-CENTURY CANADA; SKELETAL REMAINS; STR LOCI;
POPULATION; IDENTIFICATION; AMPLIFICATION; PATTERNS; FAMILY; BONE
AB Recovered and amplified ancient DNA (aDNA), from a historically documented 19th century Upper Canadian pioneer cemetery produced genotypes that were used to infer a past societal kinship system. While the results from multiplex short tandem repeat (STR) amplifications showed an unreliable polymerase chain reaction (PCR) product, a single locus HUMTH01 analysis yielded reproducible data and an allelic frequency pattern not statistically different from modern populations. Mitochondrial (mt) DNA HVR II data showed that a combined cemetery database exhibited reduced haplotype diversity indicators, as well as clusters of probable maternally related burials, The chronological persistence and replacement of mtDNA clusters approximately every two generations suggests a patrilineal/patrilocal kinship structure from a virilocal burial program for the Harmony Road cemetery. Through the integration of the aDNA analysis with archaeological material culture, historic records, and other ethnohistoric sources of information, this conclusion is supported. In this study persisting patrilineally inherited surnames act as a surrogate for aDNA Y-chromosome haplotype analysis. These results suggest that aDNA applications on aggregate skeletal collections where sparse, or no ethnological or historical documentation exists, may result in incorrect population history inferences if the presence of a kinship interment bias is not considered. Copyright (C) 2003 John Wiley Sons, Ltd.
C1 Natl Museum Nat Hist, Smithsonian Inst, Repatriat Off, Washington, DC USA.
McMaster Univ, Dept Pathol & Mol Med, Hamilton, ON, Canada.
McMaster Univ, Dept Anthropol, Hamilton, ON, Canada.
RP Dudar, JC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Repatriat Off, POB 37012,MRC 138, Washington, DC USA.
NR 68
TC 15
Z9 16
U1 0
U2 10
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 1047-482X
J9 INT J OSTEOARCHAEOL
JI Int. J. Osteoarchaeol.
PD JUL-AUG
PY 2003
VL 13
IS 4
BP 232
EP 246
DI 10.1002/oa.680
PG 15
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 713BT
UT WOS:000184836100006
ER
PT J
AU Cabrera-Asencio, I
Santiago-Blay, JA
Velez, AL
AF Cabrera-Asencio, I
Santiago-Blay, JA
Velez, AL
TI Epitragus aurulentus (Kirsch) (Coleoptera : Tenebrionidae): A new record
and report for Puerto Rico
SO JOURNAL OF AGRICULTURE OF THE UNIVERSITY OF PUERTO RICO
LA English
DT Article
C1 Dept Crop Protect, Juana Diaz, PR 00795 USA.
Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA.
Natl Museum Nat Hist, Dept Systemat Biol Entomol, Smithsonian Inst, Washington, DC 20013 USA.
Univ Puerto Rico, Coll Agr Sci, Agr Expt Stn, Rio Piedras, PR 00928 USA.
RP Cabrera-Asencio, I (reprint author), Dept Crop Protect, HC-04,Box 7115, Juana Diaz, PR 00795 USA.
NR 15
TC 0
Z9 0
U1 1
U2 1
PU COLL AGRICULTURAL SCI, AGRICULTURAL EXPERIMENT STN
PI RIO PIEDRAS
PA UNIV PUERTO RICO, MAYAGUEZ CAMPUS, RIO PIEDRAS, PR 00928 USA
SN 0041-994X
J9 J AGR U PUERTO RICO
JI J. Agric. Univ. P. R.
PD JUL-OCT
PY 2003
VL 87
IS 3-4
BP 161
EP 164
PG 4
WC Agriculture, Multidisciplinary
SC Agriculture
GA 875UB
UT WOS:000225446200008
ER
PT J
AU Piperno, DR
AF Piperno, DR
TI A few kernels short of a cob: on the Staller and Thompson late entry
scenario for the introduction of maize into northern South America
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE Zea mays; Ecuador; phytolith analysis; multiproxy data collection
ID ARCHAEOLOGICAL SITE; TROPICAL FOREST; COASTAL ECUADOR; AGRICULTURE;
ANCIENT; EVOLUTION; AMAZON; DOMESTICATION; PHYTOLITHS; LOWLANDS
AB In recent JAS articles, Staller and Thompson (J. Archaeol. Sci. 29 (2002) 33) and Staller (2002) claim that phytoliths recovered in food residues from the Late Valdivia site of La Emerenciana represent the earliest remains of maize in Ecuador. These authors also dispute the utility of a technique developed by Pearsall and this author which identifies the remains of vegetative structures of maize retrieved from archaeological and paleoecological sediments. Staller and Thompson, in arguing that maize phytoliths occur only in the latest sherds recovered from La Emerenciana, ignore evidence strongly suggesting that maize is also present in the earliest ceramics at the site, despite the very small sample of pottery sherds from this time period that was analyzed. Their criticisms of the corpus of evidence identifying maize use during the late preceramic and early ceramic periods in northern South America, remains of which age they did not study, are based on inaccurate depictions of the methodology and interpretations relating to these accumulated data, and on unsupported assumptions concerning the integrity of this well-dated, multiproxy collection of information. (C) 2003 Elsevier Science Ltd. All rights reserved.
C1 Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
Smithsonian Trop Res Inst, Unit 0948, Balboa, Panama.
RP Piperno, DR (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
NR 41
TC 12
Z9 13
U1 0
U2 5
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0305-4403
J9 J ARCHAEOL SCI
JI J. Archaeol. Sci.
PD JUL
PY 2003
VL 30
IS 7
BP 831
EP 836
DI 10.1016/S0305-4403(02)00255-8
PG 6
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 682LB
UT WOS:000183092200004
ER
PT J
AU Puyravaud, JP
Dufour, C
Aravajy, S
AF Puyravaud, JP
Dufour, C
Aravajy, S
TI Rain forest expansion mediated by successional processes in vegetation
thickets in the Western Ghats of India
SO JOURNAL OF BIOGEOGRAPHY
LA English
DT Article
DE rainforest; disturbance; succession; India; thickets; nestedness
ID SOUTHERN INDIA; SAVANNA; REGENERATION; MANAGEMENT; DISPERSAL; DYNAMICS;
PATTERNS; SUBSETS; HABITAT; MATTER
AB Aim The objective of this study was to document succession from grassland thickets to rain forest, and to provide evidence for their potential as restoration tools.
Location The Linganamakki region (State of Karnataka) of the Central Western Ghats of India.
Method We selected thirty vegetation thickets ranging from 4 to 439 m(2) in area in the vicinity of rain forest. The area of each small thicket was estimated as an oval using its maximum length and its maximum width. When the shape was irregular (mostly in large thickets) the limits of the thicket were mapped and the area calculated from the map. Plant species were identified, the number of individuals was estimated and their heights measured.
Results There was a progression in the thickets from early to late successional species. Small thickets were characterized by ecotone species and savanna trees such as Catunaregam dumetorum . Savanna trees served as a nucleus for thicket formation. Colonizing species were mostly bird-dispersed. As succession proceeded in larger thickets, the proportion of evergreen, late-successional rain forest trees increased. The species composition of the large thickets differed depending on the species composition of reproductive adults in the nearby forested areas. The species within small thickets were also found in the large thickets. The nestedness in species composition suggested that species turnover was deterministic based on thicket size. Human disturbance (leaf and wood collection by the local populations) affected the species composition and the species-area relationship of thickets.
Main conclusions Vegetation thickets are nodal centres for rain forest colonization within grasslands. They expand and replace savanna. Early successional bird-dispersed species established around savanna trees followed by late-successional rain forest trees dispersed from the nearby forest by birds. Restoration programmes that reproduce natural successional processes such as those observed in thickets will be more successful and less expensive than the methods currently being employed, where trees are individually planted in grassland. Wood harvesting is the only factor that prevents thicket growth and coalescence and hampers forest expansion.
C1 French Inst Pondicherry, Pondicherry, India.
RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama.
EM puyravaudj@tivoli.si.edu
NR 59
TC 32
Z9 32
U1 2
U2 9
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0305-0270
J9 J BIOGEOGR
JI J. Biogeogr.
PD JUL
PY 2003
VL 30
IS 7
BP 1067
EP 1080
PG 14
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 694DT
UT WOS:000183759100009
ER
PT J
AU Swider, JR
Hackley, VA
Winter, J
AF Swider, JR
Hackley, VA
Winter, J
TI Characterization of Chinese ink in size and surface
SO JOURNAL OF CULTURAL HERITAGE
LA English
DT Article
DE soot; animal glue; sol; electrophoresis; scanning electron microscopy
(SEM); photon correlation spectroscopy (PCS); laser Doppler
electrophoresis (LDE); isoelectric point (IEP)
ID CARBON; SOOT
AB Chinese ink, a mixture of soot and animal glue, has been used in East Asia for centuries as the sole black paint of choice. The combination of animal glue and soot particles create a distinctive dispersion system giving Chinese ink its unique properties among paints and inks. Photon correlation spectroscopy (PCS) size measurements and scanning electron microscopy (SEM) imaging revealed subtle differences in particle size and aggregation among inks of different soot origin. Surface chemistry of the particles was examined using laser Doppler electrophoresis (LDE) for determination of the isoelectric point (IEP). The IEPs of different inks were not distinct, but reflected the presence of the collagen-based glue on the particles' surface. The IEP and size dropped significantly when inks were treated with collagenase and when soot and carbon blacks alone were measured, pointing to the important role of animal glue in this dispersion system. (C) 2003 Editions scientifiques et medicales Elsevier SAS. All rights reserved.
C1 Smithsonian Inst, Freer Gallery Art, Dept Conservat & Sci Res, Washington, DC 20560 USA.
Smithsonian Inst, Arthur M Sackler Gallery, Dept Conservat & Sci Res, Washington, DC 20560 USA.
NIST, Mat Sci & Engn Lab, Gaithersburg, MD 20899 USA.
RP Swider, JR (reprint author), Smithsonian Inst, Freer Gallery Art, Dept Conservat & Sci Res, Washington, DC 20560 USA.
EM joseph.swider@asia.si.edu
OI Hackley, Vincent/0000-0003-4166-2724
NR 33
TC 15
Z9 15
U1 5
U2 22
PU EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER
PI PARIS
PA 23 RUE LINOIS, 75724 PARIS, FRANCE
SN 1296-2074
J9 J CULT HERIT
JI J. Cult. Herit.
PD JUL-SEP
PY 2003
VL 4
IS 3
BP 175
EP 186
DI 10.1016/S1296-2074(03)00044-X
PG 12
WC Archaeology; Art; Chemistry, Analytical; Geosciences, Multidisciplinary;
Materials Science, Multidisciplinary; Spectroscopy
SC Archaeology; Art; Chemistry; Geology; Materials Science; Spectroscopy
GA 738NF
UT WOS:000186294200003
ER
PT J
AU Jordan, TE
Whigham, DF
Hofmockel, KH
Pittek, MA
AF Jordan, TE
Whigham, DF
Hofmockel, KH
Pittek, MA
TI Nutrient and sediment removal by a restored wetland receiving
agricultural runoff
SO JOURNAL OF ENVIRONMENTAL QUALITY
LA English
DT Article
ID PARTIALLY STRATIFIED ESTUARY; SMALL CONSTRUCTED WETLANDS;
NONPOINT-SOURCE POLLUTION; CHESAPEAKE BAY; COASTAL-PLAIN; PHOSPHORUS
RETENTION; REDUCING NITROGEN; TILE DRAINAGE; WATER-QUALITY;
PHYTOPLANKTON
AB Few studies have measured removal of pollutants by restored wetlands that receive highly variable inflows. We used automated flow-proportional sampling to monitor the removal of nutrients and sus? ended solids by a 1.3-ha restored wetland receiving unregulated inflows from a 14-ha agricultural watershed in Maryland, USA. Water entered the wetland mainly in brief pulses of runoff, which sometimes exceeded the 2500-m(3) water holding capacity of the wetland. Half of the total water inflow occurred in only 24 days scattered throughout the two-year study. Measured annual water gains were within 5% of balancing water losses. Annual removal of nutrients differed greatly between the two years of the study. The most removal occurred in the first year, which included a three-month period of decreasing water level in the wetland. In that year, the wetland removed 59% of the total P, 38% of the total N, and 41% of the total organic C it received. However, in the second year, which lacked a drying period, there was no significant (p > 0.05) net removal of total N or P, although 30% of the total organic C input was removed. For the entire two-year period, the wetland removed 25% of the ammonium, 52% of the nitrate, and 34% of the organic C it received, but there was no significant net removal of total suspended solids (TSS) or other forms of N and P. Although the variability of inflow may have decreased the capacity of the wetland to remove materials, the wetland still reduced nonpoint-source pollution.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Duke Univ, Dept Biol, Durham, NC 27708 USA.
Univ Maryland, Dept Biol Resources Engn, College Pk, MD 20742 USA.
RP Jordan, TE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM jordanth@si.edu
OI Whigham, Dennis/0000-0003-1488-820X
NR 62
TC 104
Z9 115
U1 5
U2 66
PU AMER SOC AGRONOMY
PI MADISON
PA 677 S SEGOE RD, MADISON, WI 53711 USA
SN 0047-2425
J9 J ENVIRON QUAL
JI J. Environ. Qual.
PD JUL-AUG
PY 2003
VL 32
IS 4
BP 1534
EP 1547
PG 14
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 700EN
UT WOS:000184099800042
PM 12931911
ER
PT J
AU Coxall, HK
Huber, BT
Pearson, PN
AF Coxall, HK
Huber, BT
Pearson, PN
TI Origin and morphology of the Eocene planktonic foraminifer Hantkenina
SO JOURNAL OF FORAMINIFERAL RESEARCH
LA English
DT Article
ID MOLECULAR EVIDENCE; EVOLUTION; STRATIGRAPHY; SPECIATION; TRENDS; OCEAN
AB Study of the origin and early evolution of the tubulospine-bearing planktonic foraminiferal genus Hantkenina reveals that it evolved gradually from the clavate species Clavigerinella eocanica in the earliest middle Eocene and is unrelated to the genus Pseudohastigerina. Clavigerinella eocanica and the lower middle Eocene species Hantkenina nuttalli share many morphologic features and show similar developmental patterns but differ significantly in these aspects from P. micra. Rare, transitional Clavigerinella-Hantkenina forms from the Helvetikum section of Austria bridge the gap between clavate and tubulospinose morphologies, providing direct, stratigraphically-ordered evidence of the evolutionary transition between Hantkenina and Clavigerinella. Clavigerinellid ancestry is traced to a previously undescribed low-trochospiral species, Parasubbotina eoclava sp. nov., at Ocean Drilling Program Site 865.
We speculate that Hantkenina originated through competition for limited food resources in a deep, oxygen-deficient habitat below the thermocline. The tubulospines may represent a structural adaptation to this new trophic strategy, allowing the organism to harvest a greater volume of water at minimal metabolic cost. The abrupt occurrence of Hantkenina in pelagic sediment cores from the central Pacific and other regions of the world ocean may represent immigration into these areas following speciation within the hydrographically evolving Tethys Seaway. Alternatively, cladogenesis may have occurred over a wider area, but due to a contemporaneous global hiatus the fossil record of this bioevent is poorly preserved.
C1 Sch Ocean & Earth Sci, Southampton Oceanog Ctr, Southampton SO14 3ZH, Hants, England.
Smithsonian Inst, Natl Museum Nat Hist, MRC 121, Dept Paleobiol, Washington, DC 20560 USA.
Univ Bristol, Dept Earth Sci, Bristol BS8 1RJ, Avon, England.
RP Coxall, HK (reprint author), Sch Ocean & Earth Sci, Southampton Oceanog Ctr, European Way, Southampton SO14 3ZH, Hants, England.
RI Pearson, Paul/B-2276-2009
OI Pearson, Paul/0000-0003-4628-9818
NR 88
TC 13
Z9 15
U1 0
U2 3
PU CUSHMAN FOUNDATION FORAMINIFERAL RES
PI CAMBRIDGE
PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST,
HARVARD UNIV, CAMBRIDGE, MA 02138 USA
SN 0096-1191
J9 J FORAMIN RES
JI J. Foraminifer. Res.
PD JUL
PY 2003
VL 33
IS 3
BP 237
EP 261
DI 10.2113/33.3.237
PG 25
WC Paleontology
SC Paleontology
GA 723GH
UT WOS:000185424000005
ER
PT J
AU Ceruzzi, PE
AF Ceruzzi, PE
TI Strategic computing: DARPA and the quest for machine intelligence,
1983-1993.
SO JOURNAL OF MILITARY HISTORY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU SOC MILITARY HISTORY
PI LEXINGTON
PA C/O VIRGINIA MILITARY INST, GEORGE C MARSHALL LIBRARY, LEXINGTON, VA
24450-1600 USA
SN 0899-3718
J9 J MILITARY HIST
JI J. Mil. Hist.
PD JUL
PY 2003
VL 67
IS 3
BP 994
EP 996
DI 10.1353/jmh.2003.0207
PG 3
WC History
SC History
GA 697CU
UT WOS:000183925300065
ER
PT J
AU Zu, L
Hamilton, PA
Chance, KV
Davies, PB
AF Zu, L
Hamilton, PA
Chance, KV
Davies, PB
TI Pressure broadening of the lowest rotational transition of (HCl)-Cl-35
by N-2 and O-2
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
ID HCL; SPECTRUM; LINE
AB The nitrogen and oxygen pressure broadening coefficients of the J = 1 <-- 0 transition of (HCl)-Cl-35 at 626 GHz (21 cm(-1)) have been measured using a high resolution tunable far infrared sideband spectrometer. The profiles of the three Cl-35 hyperfine components of the transition were separately fitted to Voigt line shapes and the Lorentzian widths determined over a range of broadening gas pressures up to 1.1 Torr for nitrogen and 1 Torr for oxygen. The room temperature pressure broadening coefficient for nitrogen was derived as 3.46(6) MHz/Torr and for oxygen as 2.70(5) MHz/Torr. (C) 2003 Elsevier Science (USA). All rights reserved.
C1 Univ Cambridge, Dept Chem, Cambridge CB2 1EW, England.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Ohio State Univ, Dept Chem, 100 W 8th Av, Columbus, OH 43210 USA.
EM pbd2@cus.cam.ac.uk
OI Chance, Kelly/0000-0002-7339-7577
NR 14
TC 3
Z9 3
U1 0
U2 7
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
EI 1096-083X
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD JUL
PY 2003
VL 220
IS 1
BP 107
EP 112
DI 10.1016/S0022-2852(03)00096-1
PG 6
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 699VM
UT WOS:000184076700011
ER
PT J
AU Mendoza, DT
Gonzalez, LDU
Ortega-Barria, E
Capson, TL
Rios, LC
AF Mendoza, DT
Gonzalez, LDU
Ortega-Barria, E
Capson, TL
Rios, LC
TI Five new cassane diterpenes from Myrospermum frutescens with activity
against Trypanosoma cruzi
SO JOURNAL OF NATURAL PRODUCTS
LA English
DT Article
ID DERIVATIVES; ACID
AB Five novel cassane diterpenes (1-5) with activity against Trypanosoma cruzi were isolated from leaves of Myrospermum frutescens. The structures were determined as 18-hydroxycassan-13,15-diene (1), 6beta,18-dihydroxycassan-13,15-diene (2), 6beta-hydroxy-18-acetoxycassan-13,15-diene (3),18-acetoxy-13,15-diene-19-cassanoic acid (4), and 6beta,13beta-dihydroxy-18-acetoxycassan-14(17),15-diene (5). Structures were elucidated by spectroscopic analysis (NMR and HRCIMS) and by the synthesis of derivatives 2a and 2b. Compounds 3 and 5 were more active against the extracellular form of the parasite (11 and 16 muM, respectively) than the intracellular forms, while compounds 1 and 2 were more active against the more clinically relevant intracellular forms of the parasite (17 muM). Compounds 1 and 2 were approximately 9-fold more toxic toward T. cruzi than toward human fibroblasts, the cell type that serves as the parasite's mammalian host cell.
C1 Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Panama City, Panama.
Florida State Univ, Inst Trop Med & Hlth Sci, Panama City, Panama.
Smithsonian Trop Res Inst, Panama City, Panama.
RP Rios, LC (reprint author), Univ Panama, Fac Nat & Exact Sci & Technol, Lab Nat Prod, Apartado 0824, Panama City, Panama.
EM lucr@ancon.up.ac.pa
OI Torres-Mendoza, Daniel/0000-0002-3540-4238
NR 15
TC 18
Z9 19
U1 0
U2 0
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0163-3864
J9 J NAT PROD
JI J. Nat. Prod.
PD JUL
PY 2003
VL 66
IS 7
BP 928
EP 932
DI 10.1021/np030010o
PG 5
WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy
SC Plant Sciences; Pharmacology & Pharmacy
GA 705UE
UT WOS:000184412800005
PM 12880308
ER
PT J
AU Pojeta, J
Eernisse, DJ
Hoare, RD
Henderson, MD
AF Pojeta, J
Eernisse, DJ
Hoare, RD
Henderson, MD
TI Echinochiton dufoei: A new spiny Ordovician chiton
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID WIWAXIA-CORRUGATA MATTHEW; BURGESS SHALE; MOLLUSK; FOSSIL
AB Echinochiton dufoei new genus and species is described from the Ordovician age Forreston Member, Grand Detour Formation (Blackriveran) near Beloit, Wisconsin. For a variety of reasons, we regard E. dufoei as a chiton; the species is known from four articulated or partially articulated specimens, one of which has eight plates and two of which have a mucro on the tail plate. Echinochiton dufoei differs from other chitons in having large hollow spines that project from each of the known plates. In plate shape and position, E. dufoei is much like the Upper Cambrian species Matthevia variabilis Walcott, 1885, and the Lower Ordovician species Chelodes whitehousei Runnegar, Pojeta, Taylor, and Collins (1979).
C1 Smithsonian Inst, Museum Hist Nat, US Geol Survey, Washington, DC 20560 USA.
Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92834 USA.
Bowling Green State Univ, Dept Geol, Bowling Green, OH 43403 USA.
Burpee Museum Nat Hist, Rockford, IL 61103 USA.
RP Pojeta, J (reprint author), Smithsonian Inst, Museum Hist Nat, US Geol Survey, Washington, DC 20560 USA.
RI Eernisse, Douglas/B-5016-2011
NR 20
TC 21
Z9 24
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 JUL
PY 2003
VL 77
IS 4
BP 646
EP 654
DI 10.1666/0022-3360(2003)077<0646:EDANSO>2.0.CO;2
PG 9
WC Paleontology
SC Paleontology
GA 704RZ
UT WOS:000184354900003
ER
PT J
AU Rogalla, NS
Carter, JG
Pojeta, J
AF Rogalla, NS
Carter, JG
Pojeta, J
TI Shell microstructure of the Late Carboniferous rostroconch mollusc
Apotocardium lanterna (Branson, 1965)
SO JOURNAL OF PALEONTOLOGY
LA English
DT Article
ID CAMBRIAN MOLLUSKS; BIVALVIA; ORIGIN; WATSONELLA; EVOLUTION
AB The Late Carboniferous bransoniid conocardioidean Apotocardium lanterna (Branson, 1965) had an entirely aragonitic shell with a finely prismatic outer shell layer, a predominantly crossed lamellar to complex crossed lamellar middle shell layer, and an "inner" shell layer of finely textured porcelaneous and/or matted structure. This "inner" layer is probably homologous with the inner part of the middle shell layer and the inner layer sensu stricto of bivalved molluscs. Shell morphological and microstructural convergences between conocardioids and living heart cockles suggest that at least some conocardioids may have farmed algal endosymbionts in their posterior mantle margins. This symbiosis may have helped conocardioids compete with the biomechanically more efficient bivalves during the latter part of the Paleozoic.
C1 Univ Marburg, Inst Geol & Palaeontol, D-35032 Marburg, Germany.
Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
Smithsonian Inst, Natl Museum Nat Hist, US Geol Survey, Washington, DC 20013 USA.
RP Rogalla, NS (reprint author), Univ Marburg, Inst Geol & Palaeontol, Hans Meerwein Str, D-35032 Marburg, Germany.
NR 52
TC 8
Z9 8
U1 0
U2 4
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 JUL
PY 2003
VL 77
IS 4
BP 655
EP 673
DI 10.1666/0022-3360(2003)077<0655:SMOTLC>2.0.CO;2
PG 19
WC Paleontology
SC Paleontology
GA 704RZ
UT WOS:000184354900004
ER
PT J
AU Emmons, LH
Dubois, MA
AF Emmons, LH
Dubois, MA
TI Leaf-area index change across river-beach successional transects in
south-eastern Peru
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE ecotone; Leaf Area Index; Peru; plant succession; rain forest
ID FOREST/
C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA.
CEA Saclay, Serv Phys Etat Condense, F-91191 Gif Sur Yvette, France.
RP Emmons, LH (reprint author), Smithsonian Inst, Dept Systemat Biol, NHB 390,MRC 108,POB 37012, Washington, DC 20013 USA.
NR 12
TC 5
Z9 6
U1 0
U2 3
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD JUL
PY 2003
VL 19
BP 473
EP 477
DI 10.1017/S0266467403003523
PN 4
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 709WZ
UT WOS:000184650700013
ER
PT J
AU Way, T
AF Way, T
TI Grounds for pleasure: Four centuries of the American garden
SO LANDSCAPE ARCHITECTURE
LA English
DT Book Review
C1 Cornell Univ, Ithaca, NY 14853 USA.
Smithsonian Inst, Washington, DC 20560 USA.
RP Way, T (reprint author), Cornell Univ, Ithaca, NY 14853 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER SOC LANDSCAPE ARCHITECTS
PI WASHINGTON
PA 636 EYE ST, NW, WASHINGTON, DC 20001-3736 USA
SN 0023-8031
J9 LANDSCAPE ARCHIT
JI Landsc. Archit.
PD JUL
PY 2003
VL 93
IS 7
BP 96
EP 96
PG 1
WC Architecture
SC Architecture
GA 692JX
UT WOS:000183658900019
ER
PT J
AU Kalfatovic, MR
AF Kalfatovic, MR
TI Il Gigante: Michelangelo, Florence, and the David, 1492-1504.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst, Lib, Washington, DC 20560 USA.
RP Kalfatovic, MR (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUL
PY 2003
VL 128
IS 12
BP 75
EP 76
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA 696VL
UT WOS:000183908200051
ER
PT J
AU Schroll, S
AF Schroll, S
TI John Currin.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst, Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 1
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUL
PY 2003
VL 128
IS 12
BP 75
EP 75
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 696VL
UT WOS:000183908200049
ER
PT J
AU Reimold, WU
Koeberl, C
Hough, RM
McDonald, I
Bevan, A
Amare, K
French, BM
AF Reimold, WU
Koeberl, C
Hough, RM
McDonald, I
Bevan, A
Amare, K
French, BM
TI Woodleigh impact structure, Australia: Shock petrography and geochemical
studies
SO METEORITICS & PLANETARY SCIENCE
LA English
DT Article
ID PLATINUM-GROUP ELEMENTS; SOUTHERN CARNARVON BASIN; SMALL SAMPLE
ANALYSIS; LATE DEVONIAN AGE; MORY,A.J. ET-AL.; K-AR EVIDENCE;
WESTERN-AUSTRALIA; SUEVITE BRECCIA; ILLITIC CLAYS; CRATER
AB The large, complex Woodleigh structure in the Carnarvon basin of Western Australia has recently been added to the terrestrial impact crater record. Many aspects of this structure are, however, still uncertain. This work provides a detailed petrographic assessment of a suite of representative drill core samples from the borehole Woodleigh I that penetrated uplifted basement rocks of the central part of this structure. Fundamental rock and mineral deformation data and high-precision chemical data, including results of PGE and oxygen isotopic analysis, are presented. The sampled interval displays likely impact-produced macrodeformation in the form of fracturing and breccia veining at the microscopic scale. Contrary to earlier reports that these breccias represent pseudotachylite (friction melt) or even shock/shear-produced pseudotachylitic melt breccia cannot be confirmed due to pervasive post-impact alteration. Abundant planar deformation features (PDFs) in quartz, in addition to diaplectic glass and partial isotropization, are the main shock deformation effects observed, confirming that Woodleigh is of impact origin. Over the investigated depth interval, the statistics of quartz grains with a variable number of sets of PDFs does not change significantly, and the patterns of crystallographic orientations of PDFs in randomly selected quartz grains does not indicate a change in absolute shock pressure with depth either. The value of oxygen isotopes for the recognition of meteoritic contamination, as proposed by earlier Woodleigh workers, is critically assessed. Neither INA nor PGE analyses of our samples support the presence of a meteoritic component within this basement section, as had been claimed in earlier work.
C1 Univ Witwatersrand, Sch Geosci, Impact Cratering Res Grp, Johannesburg, South Africa.
Univ Vienna, Dept Geosci, A-1090 Vienna, Austria.
Western Australian Museum, Dept Earth & Planetary Sci, Perth, WA, Australia.
Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England.
Cardiff Univ, Dept Earth Sci, Cardiff CF10 3YE, S Glam, Wales.
Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
RP Reimold, WU (reprint author), Univ Witwatersrand, Sch Geosci, Impact Cratering Res Grp, POB 2050, Johannesburg, South Africa.
OI McDonald, Iain/0000-0001-9066-7244
NR 53
TC 15
Z9 16
U1 1
U2 1
PU METEORITICAL SOC
PI FAYETTEVILLE
PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA
SN 1086-9379
J9 METEORIT PLANET SCI
JI Meteorit. Planet. Sci.
PD JUL
PY 2003
VL 38
IS 7
BP 1109
EP 1130
PG 22
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 738UJ
UT WOS:000186306000011
ER
PT J
AU Weldon, PJ
Aldrich, JR
Klun, JA
Oliver, JE
Debboun, M
AF Weldon, PJ
Aldrich, JR
Klun, JA
Oliver, JE
Debboun, M
TI Benzoquinones from millipedes deter mosquitoes and elicit self-anointing
in capuchin monkeys (Cebus spp.)
SO NATURWISSENSCHAFTEN
LA English
DT Article
ID INSECTS
AB Neotropical monkeys of the genus Cebus anoint themselves by rubbing arthropods and plants against their pelage. A recent study has shown that free-ranging wedge-capped capuchin monkeys (C. olivaceus) in Venezuela self-anoint with a benzoquinone-secreting millipede, an activity by which they are hypothesized to appropriate chemical deterrents of mosquitoes. To evaluate the plausibility of this hypothesis, female yellow fever mosquitoes (Aedes aegypti) were presented with two millipede secretory compounds, 2-methyl-1,4-benzoquinone and 2-methoxy-3-methyl-1,4-benzoquinone, on nylon-reinforced silicone membranes placed over wells filled with human blood, a highly preferred food. Mosquitoes exhibited fewer landings, fed less frequently, and flew more frequently (a possible indication of repellency) in the presence of membranes treated with benzoquinones than with controls. These compounds also elicit self-anointing in captive male and female tufted (C. apella) and white-faced (C. capucinus) capuchin monkeys.
C1 ARS, Chem Affecting Insect Behav Lab, USDA, Beltsville, MD 20705 USA.
Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA.
Walter Reed Army Med Ctr, Walter Reed Army Inst Res, Dept Entomol, Div Communicable Dis & Immunol, Washington, DC 20307 USA.
RP Aldrich, JR (reprint author), ARS, Chem Affecting Insect Behav Lab, USDA, Beltsville, MD 20705 USA.
NR 25
TC 39
Z9 41
U1 0
U2 14
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0028-1042
J9 NATURWISSENSCHAFTEN
JI Naturwissenschaften
PD JUL
PY 2003
VL 90
IS 7
BP 301
EP 304
DI 10.1007/s00114-003-0427-2
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 703UC
UT WOS:000184298500002
PM 12883771
ER
PT J
AU Nagamine, K
Loeb, A
AF Nagamine, K
Loeb, A
TI Future evolution of nearby large-scale structures in a universe
dominated by a cosmological constant
SO NEW ASTRONOMY
LA English
DT Article
DE cosmology : theory; large-scale structure of Universe; Local Group;
methods : numerical
ID PECULIAR VELOCITY ANALYSIS; GALAXY REDSHIFT SURVEY; DISTANCE DATA; LOCAL
GROUP; MASS; HALO; SPECTROSCOPY; CALIBRATION; SIMULATIONS; ANISOTROPY
AB We simulate the future evolution of the observed inhomogeneities in the local universe assuming that the global expansion rate is dominated by a cosmological constant. We find that within two Hubble times (similar to30 billion years) from the present epoch, large-scale structures will freeze in co-moving coordinates and the mass distribution of bound objects will stop evolving. The Local Group will get somewhat closer to the Virgo cluster in co-moving coordinates, but will be pulled away from the Virgo in physical coordinates due to the accelerated expansion of the Universe. In the distant future there will only be one massive galaxy within our event horizon, namely the merger product of the Andromeda and the Milky Way galaxies. All galaxies that are not gravitationally bound to the Local Group will recede away from us and eventually exit from our event horizon. More generally, we identify the critical interior overdensity above which a shell of matter around an object will remain bound to it at late times. (C) 2003 Elsevier B.V. All rights reserved.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Nagamine, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA.
EM knagamin@cfa.harvard.edu; aloeb@cfa.harvard.edu
NR 36
TC 50
Z9 50
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 1384-1076
EI 1384-1092
J9 NEW ASTRON
JI New Astron.
PD JUL
PY 2003
VL 8
IS 5
BP 439
EP 448
DI 10.1016/S1384-1076(02)00234-8
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 710CD
UT WOS:000184662500006
ER
PT J
AU Dalal, N
Kochanek, CS
AF Dalal, N
Kochanek, CS
TI Detection of CDM substructure
SO NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS
LA English
DT Article; Proceedings Paper
CT 5th International UCLA Symposium on Sources and Detection of Dark Matter
and Dark Energy in the Universe
CY FEB 20-22, 2002
CL MARINA DEL REY, CALIFORNIA
ID DARK-MATTER SUBSTRUCTURE; GALACTIC SATELLITES; GALAXIES; MODELS; POWER;
LENS
AB The properties of multiple image gravitational lenses require a fractional surface mass density in satellites of f(sat) = 0.02 (0.006 less than or similar to f(sat) less than or similar to 0.07 at 90% confidence) that is consistent with the expectations for CDM. The characteristic satellite mass scale, 10(6)-10(9) M-circle dot, is also consistent with the expectations for CDM. The agreement between the observed and expected density of CDM substructure supports the basic CDM paradigm, and disfavors modifications to the CDM theory such as self-interacting dark matter or a warm dark matter component.
C1 Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02420 USA.
RP Dalal, N (reprint author), Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA.
NR 16
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0920-5632
J9 NUCL PHYS B-PROC SUP
JI Nucl. Phys. B-Proc. Suppl.
PD JUL
PY 2003
VL 124
BP 144
EP 147
DI 10.1016/S0920-5632(03)02094-2
PG 4
WC Physics, Particles & Fields
SC Physics
GA 703UE
UT WOS:000184298700025
ER
PT J
AU Lopez, OR
Kursar, TA
AF Lopez, OR
Kursar, TA
TI Does flood tolerance explain tree species distribution in tropical
seasonally flooded habitats?
SO OECOLOGIA
LA English
DT Article
DE Panama; root growth; seasonality; stomatal conductance; swamps
ID NEOTROPICAL FOREST; CENTRAL AMAZONIA; VARZEA FORESTS; RAIN-FORESTS;
GROWTH; DROUGHT; RESPONSES; SEEDLINGS; PATTERNS; STRESS
AB In the tropics, seasonally flooded forests (SFF) harbor fewer tree species than terra firme (i.e. non-flooded) forests. The low species diversity of tropical flooded forests has been ascribed to the paucity of species with adaptations to tolerate flooding. To test the hypothesis that flooding is the only factor restricting most species from SFF, we compared plant morphological and physiological responses to flooding in 2-month old seedlings of 6 species common to SFF and 12 species common to terra firme forests. Although flooding impaired growth, total biomass, maximum root length and stomatal conductance in most species, responses varied greatly and were species-specific. For example, after 90 days, flooding reduced leaf area growth by 10-50% in all species, except in Tabebuia, a common species from non-flooded habitats. Similarly, flooding had a 5-45% negative effect on total biomass for all species, except in 1 SFF and 1 terra firme species both of which had more biomass under flooding. A principal component analysis, using the above responses to flooding, provided no evidence that SFF and terra firme species differed in their responses to flooding. Flooding also caused reductions in root growth for most species. Rooting depth and root: shoot ratios were significantly less affected by flooding in SFF than in terra firme species. Although flood tolerance is critical for survival in flooded habitats, we hypothesize that responses to post-flooding events such as drought might be equally important in seasonal habitats. Therefore, we suggest that the ability to grow roots under anoxia might be critical in predicting success in inundated habitats that also experience a strong dry season.
C1 Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Lopez, OR (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA.
NR 57
TC 35
Z9 37
U1 0
U2 19
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD JUL
PY 2003
VL 136
IS 2
BP 193
EP 204
DI 10.1007/s00442-003-1259-7
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 700BJ
UT WOS:000184092500004
PM 12743794
ER
PT J
AU Harrington, GJ
AF Harrington, GJ
TI Wasatchian (Early Eocene) pollen floras from the Red Hot Truck Stop,
Mississippi, USA
SO PALAEONTOLOGY
LA English
DT Article
DE Red Hot Truck Stop; US Gulf Coast; palynology; Palaeocene; Eocene
ID PALEOCENE THERMAL MAXIMUM; NORTH-AMERICA; BIGHORN BASIN; MARINE;
DIVERSITY; EVOLUTION; TERRESTRIAL; BOUNDARY; TURNOVER; RECORDS
AB Sediments at the Red Hot Truck Stop (RUTS), Mississippi, USA are important because they contain the lowest latitude record of both the earliest known Eocene plant and mammal fossils in North America. The RHTS contains the uppermost Tuscahoma Formation and the lowermost part of the basal Bashi and Hatchetigbee formations. The Tuscahoma Formation is composed of glauconitic sands and silts that represent estuarine to shallow marine sediments. Faunal remains indicate that the RHTS section belongs to the Wasatchian North American land mammal age and specifically to the lower Graybullian subdivision. Pollen and spore floras from the RHTS are moderately diverse (113 taxa) and contain families that today are associated with warm-adapted vegetation types such as Annonaceae, Bombacaceae, Burseraceae and palms. Eocene first occurrences are represented by Brosipollis sp., Celtispollenites sp., Interpollis microsupplingensis, cf. Nuxpollenites psilatus, Platycarya spp., Retistephanocolporites sp. and Symplocos? contracta and by one genus of pteridophyte spore (Granulatisporites sp.). The overall composition and within-sample diversity of the sporomorph flora is more similar to the Hatchetigbee Formation (early Eocene) than to the middle Tuscahoma Formation (late Palaeocene) but among-sample diversity remains unchanged across the Palaeocene/Eocene boundary. The distinct composition of the RUTS demonstrates that floral change across the Palaeocene/Eocene boundary is complex and composed of several phases of floral change.
C1 Univ Coll Cork, Dept Geol, Cork, Ireland.
Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
RP Harrington, GJ (reprint author), Univ Coll Cork, Dept Geol, Cork, Ireland.
NR 60
TC 21
Z9 21
U1 0
U2 3
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0031-0239
J9 PALAEONTOLOGY
JI Paleontology
PD JUL
PY 2003
VL 46
BP 725
EP 738
DI 10.1111/1475-4983.00318
PN 4
PG 14
WC Paleontology
SC Paleontology
GA 705NK
UT WOS:000184401000006
ER
PT J
AU Krems, RV
Dalgarno, A
AF Krems, RV
Dalgarno, A
TI Disalignment transitions in cold collisions of P-3 atoms with
structureless targets in a magnetic field
SO PHYSICAL REVIEW A
LA English
DT Article
ID FINE-STRUCTURE TRANSITIONS; LOWEST EXCITED-STATES; LOG-DERIVATIVE
METHOD; EXCITATION TRANSFER; CROSS-SECTIONS; NE-ASTERISK(2P(5)3P)+HE
COLLISIONS; INTRAMULTIPLET TRANSITIONS; SCATTERING; HE; RELAXATION
AB A method for quantum-mechanical calculations of cross sections for the Zeeman transitions in collisions of P-3 atoms with structureless targets in a magnetic field is presented and applied to the study of magnetic and electronic relaxation in oxygen-helium and carbon-helium collisions at cold and ultracold temperatures. The rate constants for collisionally induced transitions between Zeeman levels in ground-state oxygen have large magnitudes in a 1 T field. It is shown that magnetic fields induce the forbidden P-3(1) --> P-3(0) transition in ultracold collisions of carbon with helium. The cross section vanishes at zero energy for field-free collisions, but becomes infinitely large in a finite magnetic field, varying with velocity v and magnetic field B as B-2/v.
C1 Harvard Smithsonian Ctr Astrophys, ITAMP, Inst Theoret Atom & Mol & Opt Phys, Cambridge, MA 02138 USA.
Harvard Univ, Dept Phys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
RP Harvard Smithsonian Ctr Astrophys, ITAMP, Inst Theoret Atom & Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA.
EM rkrems@cfa.harvard.edu
NR 50
TC 35
Z9 35
U1 1
U2 3
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD JUL
PY 2003
VL 68
IS 1
AR 013406
DI 10.1103/PhysRevA.68.013406
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 708MP
UT WOS:000184571600092
ER
PT J
AU Geller, MJ
AF Geller, MJ
TI Cloaks and kudos for PHYSICS TODAY'S portrayal of women
SO PHYSICS TODAY
LA English
DT Letter
C1 Smithsonian Astrophys Observ, Cambridge, MA USA.
RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0031-9228
J9 PHYS TODAY
JI Phys. Today
PD JUL
PY 2003
VL 56
IS 7
BP 16
EP 17
DI 10.1063/1.1603062
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 696WN
UT WOS:000183910700012
ER
PT J
AU Tyree, MT
Engelbrecht, BMJ
Vargas, G
Kursar, TA
AF Tyree, MT
Engelbrecht, BMJ
Vargas, G
Kursar, TA
TI Desiccation tolerance of five tropical seedlings in Panama. Relationship
to a field assessment of drought performance
SO PLANT PHYSIOLOGY
LA English
DT Article
ID 2 DESERT SUCCULENTS; HYDRAULIC CONDUCTANCE; MOIST FOREST; NEOTROPICAL
TREE; WATER RELATIONS; RAIN-FOREST; ROOT; VULNERABILITY; ADAPTATION;
SARAWAK
AB Studies of the desiccation tolerance of the seedlings of five tropical trees were made on potted plants growing in a greenhouse. Pots were watered to field capacity and then dehydrated for 3 to 9 weeks to reach various visual wilting stages, from slightly wilted to dead. Saturated root hydraulic conductance was measured with a high-pressure flowmeter, and whole-stem hydraulic conductance was measured by a vacuum chamber method. Leaf punches (5.6-mm diameter) were harvested for measurement of leaf water potential by a thermocouple psychrometer method and for measurement of fresh and dry weight. In a parallel study, the same five species were studied in a field experiment in the understory of a tropical forest, where these species frequently germinate. Control seedlings were maintained in irrigated plots during a dry season, and experimental plants were grown in similar plots with rain exclusion shelters. Every 2 to 4 weeks, the seedlings were scored for wilt state and survivorship. After a 22-week drought, the dry plots were irrigated for several weeks to verify visual symptoms of death. The field trials were used to rank drought performance of species, and the greenhouse desiccation studies were used to determine the conditions of moribund plants. Our conclusion is that the desiccation tolerance of moribund plants correlated with field assessment of drought-performance for the five species (r(2) > 0.94).
C1 ARS, USDA, Burlington, VT 05402 USA.
Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
Smithsonian Trop Res Inst, Balboa, Panama.
RP Tyree, MT (reprint author), ARS, USDA, POB 968, Burlington, VT 05402 USA.
RI Engelbrecht, Bettina/E-9914-2012
NR 33
TC 65
Z9 76
U1 2
U2 38
PU AMER SOC PLANT BIOLOGISTS
PI ROCKVILLE
PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 USA
SN 0032-0889
J9 PLANT PHYSIOL
JI Plant Physiol.
PD JUL
PY 2003
VL 132
IS 3
BP 1439
EP 1447
DI 10.1104/pp.102.018937
PG 9
WC Plant Sciences
SC Plant Sciences
GA 717FU
UT WOS:000185076800035
PM 12857825
ER
PT J
AU Montenegro, H
Guterrez, M
Romero, LI
Ortega-Barria, E
Capson, TL
Rios, LC
AF Montenegro, H
Guterrez, M
Romero, LI
Ortega-Barria, E
Capson, TL
Rios, LC
TI Aporphine alkaloids from Guatteria spp. with leischmanicidal activity
SO PLANTA MEDICA
LA English
DT Article
ID IN-VITRO; ANNONACEAE
AB Fractionation of Guatteria amplifolia yielded the alkaloids xylopine (1), nornuciferine (4), lysicamine (6), and laudanosine (5). Fractionation of Guatteria dumetorum yielded the alkaloids cryptodorine (2) and nornantenine (3). Compounds 1-4 demonstrated significant activity against Leishmania mexicana and L. panamensis. Xylopine (1) was among the most active compounds (LD50 = 3muM) and showed a 37-fold higher toxicity towards L. mexicana than macrophages, the regular host cells of Leishmania spp.
C1 Univ Panama, Dept Quim Organ, Panama City, Panama.
Florida State Univ, Inst Trop Med & Hlth Sci, Panama City, Panama.
Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Rios, LC (reprint author), Univ Panama, Dept Quim Organ, Apdo 0824-10835, Panama City, Panama.
FU FIC NIH HHS [1U10 TW01021-01]
NR 15
TC 45
Z9 51
U1 3
U2 15
PU GEORG THIEME VERLAG KG
PI STUTTGART
PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY
SN 0032-0943
J9 PLANTA MED
JI Planta Med.
PD JUL
PY 2003
VL 69
IS 7
BP 677
EP 679
PG 3
WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary
Medicine; Pharmacology & Pharmacy
SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary
Medicine
GA 714AK
UT WOS:000184890000018
PM 12898429
ER
PT J
AU Smith, DR
Saini, MS
AF Smith, DR
Saini, MS
TI A new species of Conaspidia Konow (Hymenoptera : Tenthredinidae) from
India and review of the Indian species
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE India; Conaspidia; sawfly; Tenthredininae
AB Conaspidia maculosa, new species, is described from Sikkim, India. It is the fourth species of this Asian genus known from India, the other species being C. dubiosa Forsius, C. fasciatipennis Turner, and C. sikkimensis Konow. The new species belongs in the scutellaris group of Conaspidia and is separated from related species in that group and the other Indian species.
C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA.
Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India.
RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA.
NR 5
TC 1
Z9 3
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 555
EP 558
PG 4
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100005
ER
PT J
AU Brown, JW
AF Brown, JW
TI Three new genera, two new species, and some rectifications in
neotropical Euliini (Lepidoptera : Tortricidae)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE genitalia; biodiversity; synonymy; new combinations; classification;
Euryeulia; Pseudapina; Circapina; Pycnospina; Lobogenesis; Osmaria;
Anopina; Chirotes; Prochirotes; Strophotina
AB Three new genera in the tortricid tribe Euliini are described and illustrated: Euryeulia, with type species E. biocellata (Walsingham 1914), new combination, from Mexico; Pseudapina, with type species P. lanceovalva, new species, from Venezuela; and Circapina, with type species C flexalana, new species, from Costa Rica. Three new generic synonymies are proposed: Pycnospina Razowski 1997 is a junior synonym of Lobogenesis Razowski 1990, with the new combination L. centrota (Razowski 1997); Osmaria Razowski 1991 is a junior synonym of Anopina Obraztsov 1962, with the new combination A. psaeroptera (Razowski and Becker 1991); and Chirotes Razowski and Becker 1999, along with its replacement name, Prochirotes Razowski 2001, are junior synonyms of Strophotina Brown 1998, with the new combinations S. chorestis (Razowski and Becker 1999) and S. niphochondra (Razowski and Becker 1999).
C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA.
RP Brown, JW (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA.
EM jbrown@sel.barc.usda.gov
NR 19
TC 1
Z9 2
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 630
EP 640
PG 11
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100012
ER
PT J
AU Saini, MS
Smith, DR
Saini, TP
AF Saini, MS
Smith, DR
Saini, TP
TI Review of the southeastern Asian sawfly genus Anapeptamena Konow
(Hymenoptera : Tenthredinidae)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE India; Myanmar; Selandriinae
AB Anapeptamena Konow (Tenthredinidae: Selandriinae) has been known only by its type species, A. albipes Konow, from India and Myanmar. Two new species have been discovered from India and are described: Anapeptamena darjeelingensis, n. sp., and A. dhanoultiensis, n. sp. A male of the genus, that of A. dhanoultiensis, is described for the first time. Descriptions, illustrations, and a key are provided for identification of the species.
C1 Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India.
ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA.
RP Smith, DR (reprint author), Punjabi Univ, Dept Zool, Patiala 147002, Punjab, India.
NR 5
TC 2
Z9 3
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 641
EP 646
PG 6
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100013
ER
PT J
AU Gordon, RD
McCleve, S
AF Gordon, RD
McCleve, S
TI Five new species of Euparixia brown (Coleoptera : Aphodiidae :
Eupariinae), with a revised key to species
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE taxonomy; new species; ant nests
AB Five previously undescribed species of Euparixia Brown, E. boliviana from Bolivia, E. campbelli from Costa Rica, E. isthmia and E. panamaensis from Panama, and E. mexicana from Mexico are described and integrated into the existing classification. A revised key to all known species is presented.
C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entom Lab, Washington, DC 20560 USA.
RP Gordon, RD (reprint author), No Plains Entomol, POB 65, Willow City, ND 58384 USA.
NR 2
TC 4
Z9 5
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 685
EP 697
PG 13
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100018
ER
PT J
AU Marsh, PM
Shaw, SR
AF Marsh, PM
Shaw, SR
TI Revision of North American Aleiodes Wesmael (Part 7): The compressor
Herrich-Schaeffer, ufei (Walley), gressitti (Muesebeck), and procerus
Wesmael species-groups (Hymenoptera : Braconidae : Rogadinae)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Hymenoptera; Braconidae; parasitoids
AB Six North American species in four species-groups of the genus Aleiodes are treated. The compressor (Herrich-Schaeffer) species-group includes A. palmatus (Walley), new combination and A. palmatoides, new species; the ufei (Walley) species-group includes only A. ufei (Walley), new combination; the gressitti (Muesebeck) species-group includes A. lissos, new species; and the procerus species-group includes A. granulatus (DeGant), new combination, and A. angustipennis, new species. Other new combinations proposed are: A. aligharensis (Quadri), new combination; A. compressor (Herrich-Schaeffer), new combination; A. gressitti (Muesebeck), new combination; and A. narangae (Rohwer), new combination.
C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
Univ Wyoming, Dept Renewable Resources, Insect Museum, Laramie, WY 82071 USA.
RP Marsh, PM (reprint author), POB 384, N Newton, KS 67117 USA.
NR 20
TC 7
Z9 7
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 698
EP 707
PG 10
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100019
ER
PT J
AU Braud, R
Smith, DR
Strazanac, JS
Butler, L
AF Braud, R
Smith, DR
Strazanac, JS
Butler, L
TI Diversity, abundance, and seasonality of adult and larval Symphyta
(Hymenoptera) in the George Washington National Forest, Virginia, and
the Monongahela National Forest, West Virginia
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
DE Symphyta; richness; abundance; diversity; Acordulecera dorsalis
ID FOOD; TRAP
AB Adult Symphyta richness and abundance were studied using data collected from 36 Malaise traps in the Monongahela National Forest, Pocahontas County, West Virginia, and in the George Washington National Forest, Augusta County, Virginia. A total of 8,884 adults representing 155 species in 49 genera and 8 families were collected. Diversity estimators suggest that approximately 81% of the actual species present on the two forests were sampled over five years (1995-1999). Fifty percent of all adults (4,48 1) were Acordulecera dorsalis Say ((Pergidae). The next most :abundant species were Pristphora banksi Marlatt (Tenthredinidae) (12.8%), Pachynematus corniger,(Norton) (Tenthredinidae) (4%), Pracharactus rudis (Norton) (Tenthredinidae) (3%), and Taxonus palipes (Say) (Tenthredinidae) (2%). Larval symphytan richness and abundance were determined by foliage collections from Quercus spp., Carya spp., and Acer spp. Symphytan larvae from foliage numbered 11,621 specimens representing eight genera. Sixty-three percent of all larvae (7,373) were Acordulecera spp. The next most abundant genus was Periclista (2,328) which accounted for 20% of the total larvae. Differences in species,richness and abundance of both adults and larvae occurred between forests and between years.
C1 W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA.
Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
RP Braud, R (reprint author), W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA.
NR 15
TC 6
Z9 8
U1 0
U2 1
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 756
EP 768
PG 13
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100023
ER
PT J
AU Poinar, G
Smith, DR
AF Poinar, G
Smith, DR
TI Food plant, life history notes, and distribution of Nematus atriceps
(Marlatt) - (Hymenoptera : Tenthredinidae)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
ID ZIGADENUS LILIACEAE
C1 Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA.
Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
RP Poinar, G (reprint author), Oregon State Univ, Dept Zool, Corvallis, OR 97331 USA.
NR 6
TC 1
Z9 2
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 778
EP 780
PG 3
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100026
ER
PT J
AU Smith, DR
Marshall, SA
AF Smith, DR
Marshall, SA
TI First report of nuptial feeding in sawflies, Aneugmenus flavipes
(Norton) (Hymenoptera : Tenthredinidae)
SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
C1 Smithsonian Inst, Natl Museum Nat Hist, Agr Res Serv, PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
Univ Guelph, Dept Environm Biol, Guelph, ON N1G 2W1, Canada.
RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Agr Res Serv, PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
NR 8
TC 2
Z9 4
U1 0
U2 0
PU ENTOMOL SOC WASHINGTON
PI WASHINGTON
PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA
SN 0013-8797
J9 P ENTOMOL SOC WASH
JI Proc. Entomol. Soc. Wash.
PD JUL
PY 2003
VL 105
IS 3
BP 789
EP 791
PG 3
WC Entomology
SC Entomology
GA 694CK
UT WOS:000183756100030
ER
PT J
AU Roalson, EH
Skog, LE
Zimmer, EA
AF Roalson, EH
Skog, LE
Zimmer, EA
TI Phylogenetic relationships and the diversification of floral form in
Achimenes (Gesneriaceae)
SO SYSTEMATIC BOTANY
LA English
DT Article
ID MAXIMUM-LIKELIHOOD ANALYSES; NDHF SEQUENCES; CLADISTIC-ANALYSIS;
SAINTPAULIA GESNERIACEAE; EPISCIEAE GESNERIACEAE; TRIBAL RELATIONSHIPS;
POLLINATION SYSTEMS; CHLOROPLAST DNA; EVOLUTION; ORCHIDACEAE
AB Achimenes is a genus in the Gesneriaceae, subfamily Gesnerioideae, tribe Gloxinieae that shows remarkable variation in floral form and possibly floral pollination syndrome. This includes flowers that are salverform, tubular, or infundibuliform, white, yellow, pink, purple, and red, and with or without corolla spurs. Previous classifications of Achimenes have relied heavily on floral form as a measure of relationship. This study explores phylogenetic relationships in Achimenes and addresses questions of proper supraspecific classification, evolution of floral forms and pollination syndromes, the origins of floral spurs, chromosome evolution, and biogeographic patterns using nrDNA ITS and cpDNA trnL-F spacer sequences analyzed using maximum parsimony and maximum likelihood methodologies. Phylogenetic hypotheses support the non-monophyly of most of the supraspecific classification units currently recognized in Achimenes, multiple origins of each of the pollination syndromes and the major morphological characteristics used to define these syndromes, multiple origins of floral spurs, multiple tetraploid events, and sympatric distributions of many closely related species.
C1 Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA.
Natl Museum Nat Hist, Labs Analyt Biol, Smithsonian Inst, Suitland, MD 20746 USA.
Smithsonian Inst, Dept Systemat Biol Bot, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Roalson, EH (reprint author), Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA.
EM roalson@mail.wsu.edu
RI Zimmer, Elizabeth/G-3890-2011
NR 77
TC 18
Z9 19
U1 0
U2 7
PU AMER SOC PLANT TAXONOMISTS
PI LARAMIE
PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071
USA
SN 0363-6445
EI 1548-2324
J9 SYST BOT
JI Syst. Bot.
PD JUL-SEP
PY 2003
VL 28
IS 3
BP 593
EP 608
PG 16
WC Plant Sciences; Evolutionary Biology
SC Plant Sciences; Evolutionary Biology
GA 713FF
UT WOS:000184845900013
ER
PT J
AU Warner, DJ
AF Warner, DJ
TI The art of teaching physics: Instrumentation of Jean-Antoine Nollet
1700-1770
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
RP Warner, DJ (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4319 USA
SN 0040-165X
J9 TECHNOL CULT
JI Technol. Cult.
PD JUL
PY 2003
VL 44
IS 3
BP 603
EP 604
DI 10.1353/tech.2003.0141
PG 2
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 715TG
UT WOS:000184987900014
ER
PT J
AU Langley, HD
AF Langley, HD
TI Medicine under sail.
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
RP Langley, HD (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4319 USA
SN 0040-165X
J9 TECHNOL CULT
JI Technol. Cult.
PD JUL
PY 2003
VL 44
IS 3
BP 609
EP 610
DI 10.1353/tech.2003.0118
PG 2
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 715TG
UT WOS:000184987900018
ER
PT J
AU Molella, A
AF Molella, A
TI Technomanifestos: Visions from the information revolutionaries.
SO TECHNOLOGY AND CULTURE
LA English
DT Book Review
C1 Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
RP Molella, A (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4319 USA
SN 0040-165X
J9 TECHNOL CULT
JI Technol. Cult.
PD JUL
PY 2003
VL 44
IS 3
BP 639
EP 640
DI 10.1353/tech.2003.0123
PG 2
WC History & Philosophy Of Science
SC History & Philosophy of Science
GA 715TG
UT WOS:000184987900038
ER
PT J
AU McNair, DB
Dean, JP
AF McNair, DB
Dean, JP
TI Distributional information on birds from egg sets collected by Henry
Rogers Durkee in 1870 in Southwestern Wyoming
SO WESTERN NORTH AMERICAN NATURALIST
LA English
DT Article
DE eggs; museum collections; Wyoming; distribution; history; Ammodramus
savannarum; Grasshopper Sparrow; Calamospiza melanocorys; Lark Bunting;
Passerella iliaca schistacea; Fox Sparrow; Grus canadensis; Sandhill
Crane
ID SPARROW
AB Henry Rogers Durkee collected 74 egg sets of 27 avian species in 1870 at Gilmer, Uinta County, in southwestern Wyoming. Despite the paucity of documented breeding evidence from this region during the late 19th and early 20th centuries, his material at the Smithsonian Institution was generally overlooked and has never been critically examined. Durkee's egg sets included 5 species (Sandhill Crane, Grus canadensis; Northern Rough-winged Swallow, Stelgidopteryx serripennis; Grasshopper Sparrow, Ammodramus savannarum; Fox Sparrow, Passerella iliaca; Cassin's Finch, Carpodacus cassinii) whose breeding distribution was then poorly known, 25 to more than 70 years before nests and eggs were otherwise documented in Wyoming. Durkee also collected complete egg sets of Lark Bunting (Calamospiza melanocorys) over 70 years before breeding was confirmed at other peripheral locations in Wyoming. In addition, Durkee's incomplete egg sets of Grasshopper Sparrow were the 1st for the western subspecies (A. s. perpallidus); his incomplete egg set and nest of the Fox Sparrow collected at Gilmer constituted the 2nd locality for the species or species group (P. i. schistacea). Although the number of egg sets Durkee collected is modest, he made a meaningful contribution to the early history of avifaunal exploration in Wyoming.
C1 Tall Timbers Res Stn, Tallahassee, FL 32312 USA.
Smithsonian Inst, Dept Systemat Biol, Div Birds, Washington, DC 20013 USA.
RP McNair, DB (reprint author), Dept Planning & Nat Resources, Div Game & Fish, 45 Mars Hill, Frederiksted, VI 00840 USA.
NR 93
TC 1
Z9 1
U1 0
U2 3
PU BRIGHAM YOUNG UNIV
PI PROVO
PA 290 LIFE SCIENCE MUSEUM, PROVO, UT 84602 USA
SN 1527-0904
J9 WEST N AM NATURALIST
JI West. North Am. Naturalist
PD JUL
PY 2003
VL 63
IS 3
BP 320
EP 332
PG 13
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 712HG
UT WOS:000184791800005
ER
PT J
AU Hershler, R
Liu, HP
Thompson, FG
AF Hershler, R
Liu, HP
Thompson, FG
TI Phylogenetic relationships of North American nymphophiline gastropods
based on mitochondrial DNA sequences
SO ZOOLOGICA SCRIPTA
LA English
DT Article
ID HYDROBIIDAE MOLLUSCA; GENUS PYRGULOPSIS; RISSOOIDEA; SYSTEMATICS; SNAIL;
PROSOBRANCHIA; SUBSTITUTION; SUBUNIT; GENERA; MODEL
AB Phylogenetic relationships of 36 nymphophiline species representing 10 genera were inferred from mtCOI sequence data and compared to recent morphology-based classifications of this group. Parsimony and maximum likelihood analyses of the molecular data set suggested monophyly of the North American nymphophilines and a sister or otherwise close relationship between this fauna and a European species assigned to the subfamily. Results also supported a previously hypothesized close relationship between the predominantly freshwater nymphophilines and the brackish-water genus Hydrobia . Our analyses resolved a North American nymphophiline subclade composed of Floridobia , Nymphophilus , and Pyrgulopsis , and depicted the remaining North American genera (Cincinnatia , Marstonia , Notogillia , Rhapinema , Spilochlamys , Stiobia ) as either a monophyletic or paraphyletic group. Two of the large North American genera (Floridobia , Marstonia ) were supported as monophyletic groups while monophyly of Pyrgulopsis , a western North American group containing > 100 species, was equivocal. North American nymphophiline phylogeny implies that vicariance of eastern and western North American groups was followed by a secondary invasion of eastern coastal areas from the west. We attribute this to dispersal of salt-tolerant progenitors along the Gulf of Mexico coast.
C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA.
Univ Denver, Dept Biol Sci, Denver, CO 80208 USA.
Univ Florida, Florida Museum Nat Hist, Div Malacol, Gainesville, FL 32611 USA.
RP Hershler, R (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB W-305,MRC 118, Washington, DC 20013 USA.
NR 50
TC 36
Z9 36
U1 0
U2 3
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0300-3256
J9 ZOOL SCR
JI Zool. Scr.
PD JUL
PY 2003
VL 32
IS 4
BP 357
EP 366
DI 10.1046/j.1463-6409.2003.00115.x
PG 10
WC Evolutionary Biology; Zoology
SC Evolutionary Biology; Zoology
GA 688NZ
UT WOS:000183443300004
ER
PT J
AU Randall, JE
Allen, GR
Robertson, DR
AF Randall, JE
Allen, GR
Robertson, DR
TI Myripristis earlei, a new soldierfish (Beryciformes : Holocentridae)
from the Marquesas and Phoenix Islands
SO ZOOLOGICAL STUDIES
LA English
DT Article
DE fish taxonomy; Holocentridae; new soldierfish; oceania
AB The common holocentrid fish in the Marquesas Islands, previously regarded as an insular variant of the wide-ranging Myripristis berndti, is described as a new species, M. earlei, after discovering a typical M. berndti in the islands and also finding the species in the Phoenix Islands with M. berndti. No meristic or proportional measurement differences were found to separate the 2 species, and no mtDNA differences were detected. Myripristis earlei differs from M. berndti by lacking or having only a few small scales on the lower 1/2 of the pectoral-fin axil; the lower jaw of adults not as strongly projecting; the leading edges of the soft dorsal, anal, and caudal fins not white; and the spinous portion of the dorsal fin red instead of being orange-yellow on the outer part as in M. berndti.
C1 Bernice P Bishop Museum, Honolulu, HI 96817 USA.
Conservat Int, Roleystone, Australia.
Western Australian Museum, Perth, WA, Australia.
Smithsonian Trop Res Inst, APO, AA 34002 USA.
RP Randall, JE (reprint author), Bernice P Bishop Museum, 1525 Bernice St, Honolulu, HI 96817 USA.
NR 5
TC 3
Z9 5
U1 2
U2 3
PU ACAD SINICA INST ZOOLOGY
PI TAIPEI
PA EDITORIAL OFFICE, TAIPEI 115, TAIWAN
SN 1021-5506
J9 ZOOL STUD
JI Zool. Stud.
PD JUL
PY 2003
VL 42
IS 3
BP 405
EP 410
PG 6
WC Zoology
SC Zoology
GA 705PD
UT WOS:000184402700002
ER
PT J
AU Pawson, DL
Gage, JD
Belyaev, GM
Mironov, AN
Smirnov, AV
AF Pawson, DL
Gage, JD
Belyaev, GM
Mironov, AN
Smirnov, AV
TI The deep sea synaptid Protankyra brychia (Echinodermata : Holothuroidea)
and its near-surface dwelling planktotrophic larva, Auricularia
nudibranchiata
SO SARSIA
LA English
DT Article
DE Holothurians; synaptids; auricularia; bathyal; abyssal
ID NORTHEAST ATLANTIC-OCEAN; ROCKALL TROUGH; ABYSSAL-PLAIN; REPRODUCTION
AB Pacific and Atlantic Ocean material of the bathyal to abyssal synaptid holothurian genus Protankyra confirm that P. abyssicola (Theel) and P. pacifica (Ludwig) are subjective synonyms of P. brychia (Verrill 1885). This species is probably cosmopolitan in distribution at 869-4990 m. Post-larval juveniles from several localities in the Atlantic and Pacific Oceans retain wheel ossicles from pelagic planktotrophic larvae; the wheels are identical to those of the giant pelagic larva Auricularia nudibranchiata Chun 1896. We believe that Auricularia nudibranchiata is the larva of P. brychia.
C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
Scottish Marine Biol Assoc, Oban PA34 4AD, Argyll, Scotland.
USSR Acad Sci, Inst Oceanol, Moscow, Russia.
Russian Acad Sci, Inst Oceanol, Moscow 117218, Russia.
Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia.
RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC163, Washington, DC 20560 USA.
NR 54
TC 5
Z9 6
U1 4
U2 4
PU TAYLOR & FRANCIS AS
PI OSLO
PA CORT ADELERSGT 17, PO BOX 2562, SOLLI, 0202 OSLO, NORWAY
SN 0036-4827
J9 SARSIA
JI Sarsia
PD JUN 30
PY 2003
VL 88
IS 3
BP 159
EP 174
DI 10.1080/00364820310001165
PG 16
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 700AM
UT WOS:000184090500001
ER
PT J
AU Clarke, RD
Tyler, JC
AF Clarke, RD
Tyler, JC
TI Differential space utilization by male and female spinyhead blennies,
Acanthemblemaria spinosa (Teleostei : Chaenopsidae)
SO COPEIA
LA English
DT Article
ID MALE REPRODUCTIVE SUCCESS; CORAL-REEF; GENUS ACANTHEMBLEMARIA; TUBE
BLENNIES; HABITAT USE; FISHES; MICROHABITAT; COMPETITION; CHOICE
AB To assess the ways in which different selection pressures on male and female spinyhead blennies (Acanthemblemaria spinosa) influence their use of space, we measured a number of features of their shelter sites. Both sexes occurred primarily on dead surfaces of elkhorn coral (Acropora palmata), but significantly more males than females were found on live coral surfaces. Males occurred twice. as frequently as females in the vacated constructed tubes of serpulid worms or vermetid molluscs, which provide greater surface for egg deposition than the shorter cavities excavated by other organisms. There was no difference between the sexes in shelter height above the reef surface. Fish size was positively correlated with shelter height above the reef surface for both sexes. Number of eggs being guarded by males was positively correlated with both fish size and shelter height above the reef surface; in concert they account for 44% of the variance in egg number. To assess the effects of competition, we removed spinybeads from corals and documented recolonization along with shelter site parameters. Corals originally harboring larger fish were recolonized at a higher rate, and in all cases the mean size of recolonists was smaller than originals; the original correlation of fish size with height above the reef surface collapsed for recolonists. These observations are consistent with others that indicate that spinyhead blennies compete for quality shelters.
C1 Sarah Lawrence Coll, Dept Biol, Bronxville, NY 10708 USA.
Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Clarke, RD (reprint author), Sarah Lawrence Coll, Dept Biol, Bronxville, NY 10708 USA.
EM rclarke@mail.slc.edu
NR 28
TC 7
Z9 7
U1 0
U2 3
PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS
PI MIAMI
PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200
SW 8TH STREET, MIAMI, FL 33199 USA
SN 0045-8511
EI 1938-5110
J9 COPEIA
JI Copeia
PD JUN 23
PY 2003
IS 2
BP 241
EP 247
PG 7
WC Zoology
SC Zoology
GA 695EG
UT WOS:000183817700002
ER
PT J
AU Sumner, S
Nash, DR
Boomsma, JJ
AF Sumner, S
Nash, DR
Boomsma, JJ
TI The adaptive significance of inquiline parasite workers
SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES
LA English
DT Article
DE reproductive suppression; social parasitism; Acromyrmex insinuator;
adaptation
ID SOCIAL PARASITISM; ACROMYRMEX INSINUATOR; CUCULUS-CANORUS; ANTS;
HYMENOPTERA; FORMICIDAE; BEHAVIOR; CASTE; EVOLUTION; CUCKOOS
AB Social parasites exploit the socially managed resources of their host's society. Inquiline social parasites are dependent on their host throughout their life cycle, and so many of the traits inherited from their free-living ancestor are removed by natural selection. One trait that is commonly lost is the worker caste, the functions of which are adequately fulfilled by host workers. The few inquiline parasites that have retained a worker caste are thought to be at a transitional stage in the evolution of social parasitism, and their worker castes are considered vestigial and non-adaptive. However, this idea has not been tested. Furthermore, whether inquiline workers have an adaptive role outside the usual worker repertoire of foraging, brood care and colony maintenance has not been examined. In this paper, we present data that suggest that workers of the inquiline ant Acromyrmex insinuator play a vital role in ensuring the parasite's fitness. We show that the presence of these parasite workers has a positive effect on the production of parasite sexuals and a negative effect on the production of host sexuals. This suggests that inquiline workers play a vital role in suppressing host queen reproduction, thus promoting the rearing of parasite sexuals. To our knowledge, these are the first experiments on inquiline workers and the first to provide evidence that inquiline workers have an adaptive role.
C1 Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen, Denmark.
RP Sumner, S (reprint author), Smithsonian Trop Res Inst, Balboa, Panama.
EM sumners@naos.si.edu
RI Nash, David/B-2916-2009; Sumner, Seirian/E-6611-2011; Nash,
David/H-4433-2012; Boomsma, Jacobus/M-2785-2014
OI Nash, David/0000-0002-0462-6794; Nash, David/0000-0002-0462-6794;
Boomsma, Jacobus/0000-0002-3598-1609
NR 27
TC 16
Z9 16
U1 0
U2 9
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 JUN 22
PY 2003
VL 270
IS 1521
BP 1315
EP 1322
DI 10.1098/rspb.2003.2362
PG 8
WC Biology; Ecology; Evolutionary Biology
SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences &
Ecology; Evolutionary Biology
GA 693BV
UT WOS:000183695500013
PM 12816646
ER
PT J
AU Neufeld, DA
Bergin, EA
Melnick, GJ
Goldsmith, PF
AF Neufeld, DA
Bergin, EA
Melnick, GJ
Goldsmith, PF
TI Submillimeter Wave Astronomy Satellite mapping observations of water
vapor around Sagittarius B2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : abundances; ISM : clouds; ISM : individual (Sagittarius B2); ISM :
molecules; molecular processes; submillimeter
ID MOLECULAR LINE SURVEY; GALACTIC-CENTER; ORION-KL; 263 GHZ; SGR B2;
CLOUDS; ABSORPTION; EMISSION; AMMONIA; CO
AB Observations of the 1(10)-1(01) 556.936 GHz transition of ortho-water with the Submillimeter Wave Astronomy Satellite have revealed the presence of widespread emission and absorption by water vapor around the strong submillimeter continuum source Sagittarius B2. An incompletely sampled spectral line map of a region of size 26' x 19' around Sgr B2 reveals three noteworthy features. First, absorption by foreground water vapor is detectable at local standard of rest (LSR) velocities in the range -100 to 0 km s(-1) at almost every observed position. Second, spatially extended emission by water is detectable at LSR velocities in the range 80-120 km s(-1) at almost every observed position. This emission is attributable to the 180 pc molecular ring identified from previous observations of CO. The typical peak antenna temperature of 0.075 K for this component implies a typical water abundance of (1.2-8) x 10(-6) relative to H-2. Third, strong absorption by water is observed within 50 of Sgr B2 at LSR velocities in the range 60-82 km s(-1). An analysis of this absorption yields a (H2O)-O-16 abundance similar to(2-4) x 10(-7) relative to H-2 if the absorbing water vapor is located within the core of Sgr B2 itself, or, alternatively, a water column density of similar to(2.5-4) x 10(16) cm(-2) if the water absorption originates in the warm, foreground layer of gas proposed previously as the origin of ammonia absorption observed toward Sgr B2.
C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Cornell Univ, Dept Astron, NAIC, Ithaca, NY 14853 USA.
RP Neufeld, DA (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RI Goldsmith, Paul/H-3159-2016
NR 30
TC 23
Z9 23
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2003
VL 590
IS 2
BP 882
EP 894
DI 10.1086/375024
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 688WA
UT WOS:000183459200024
ER
PT J
AU Takakuwa, S
Ohashi, N
Hirano, N
AF Takakuwa, S
Ohashi, N
Hirano, N
TI Interaction between the outflow and the core in IRAM 04191+1522
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : abundances; ISM : individual (IRAM 04191+1522); ISM : jets and
outflows; ISM : molecules; stars : formation; stars : mass loss
ID MASS STAR-FORMATION; MAGNETOHYDRODYNAMIC SHOCK-WAVES; YOUNG STELLAR
OBJECTS; L1157 DARK CLOUD; DENSE CORES; MOLECULAR CLOUD; SIO EMISSION;
PROTOSTELLAR OUTFLOWS; METHANOL ENHANCEMENT; CH3OH
AB We have carried out mapping observations of the molecular core associated with the young Class 0 protostar, IRAM 04191+ 1522, in the CH3OH (J(K) = 2(K)-1(K)) and (CS)-S-34 (J = 2-1) lines, using the 45 m telescope at Nobeyama Radio Observatory. Our observations have revealed that there is a condensation associated with the protostar, elongated in the east-west direction mostly perpendicular to the axis of the associated CO out. flow. Its size and mass are estimated to be 0.07 x 0.04 pc and 2.3M(.), respectively, from the CH3OH data. In addition to the elongated envelope, two compact (similar to0.03 pc) condensations were found in the CH3OH line at the southern edge of the elongated envelope, where the blueshifted CO outflow emerging from the protostar is located. In contrast to the elongated envelope, those compact CH3OH condensations show much larger line width (up to 2.0 km s(-1)), with centroid velocities blueshifted by similar to0.8 km s(-1). The compact condensations have momenta (similar to0.06 M-. km s(-1)) comparable to that of the blueshifted molecular outflow. In addition, they are gravitationally unbound, and most probably will dissipate eventually. These results suggest that the compact condensations are probably formed in the course of interaction between the outflow and the ambient gas surrounding the protostar and that such interaction may cause dissipation of a part of the ambient gas. No drastic, localized enhancement of the CH3OH abundance is, however, observed toward the compact condensations, implying that there seems to be no significant shock heating at the compact condensations, in spite of the interaction with the outflow. This may be because the CO outflow velocity (< 10 km s(-1)) is too low to cause effective heating to release CH3OH on dust grains into the gas phase.
C1 Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan.
RP Takakuwa, S (reprint author), Harvard Smithsonian Ctr Astrophys, 82 Puuhonu Pl,Suite 210, Hilo, HI 96720 USA.
NR 68
TC 16
Z9 16
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2003
VL 590
IS 2
BP 932
EP 943
DI 10.1086/375190
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 688WA
UT WOS:000183459200028
ER
PT J
AU Casares, J
Steeghs, D
Hynes, RI
Charles, PA
O'Brien, K
AF Casares, J
Steeghs, D
Hynes, RI
Charles, PA
O'Brien, K
TI Bowen fluorescence from the companion star in X1822-371
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries : close; stars : individual
(X1822-371); X-rays : binaries; X-rays : stars
ID X-1822-371; SPECTROSCOPY
AB We present clear evidence for the motion of the companion star in the low-mass X-ray binary (LMXB) X1822 - 371. We detect NIII lambda4640 emission moving in antiphase with the radial velocity curve of the neutron star and produced on the X-ray - heated hemisphere of the donor star. From the motion of this feature we derive a lower limit to the radial velocity semiamplitude of the companion star, K-2 greater than or equal to 300 +/- 8 km s(-1), which, combined with a previous determination of the inclination angle and the pulsar's radial velocity curve, yields M-2 greater than or equal to 0.36(2) M-. and M-1 greater than or equal to 1.14(6)M-.. The He I lambda4471 absorption line moves at lower velocities (similar or equal to225 km s(-1)) and with a -0.05 phase shift, suggesting a likely origin on the gas stream near the L1 point. In addition, we detect an S-wave emission of O vi lambda3811 produced by illumination of the hot spot bulge by the central source. The Balmer lines are dominated by broad absorptions probably due to obscuration of the accretion disk by vertically extended cool material from the splash region and over. owing stream. We also derive a more accurate, and significantly different ( compared to earlier work), systemic velocity of gamma = -44 +/- 5 km s(-1), based on the motion of the He II lambda4686 wings and Doppler tomography. This work confirms the power of imaging the companion stars in LMXBs and outbursting transients using the Bowen fluorescence transitions.
C1 Inst Astrofis Canarias, Tenerife 38200, Spain.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Texas, Dept Astron, Austin, TX 78712 USA.
Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England.
European So Observ, Santiago 19, Chile.
RP Casares, J (reprint author), Inst Astrofis Canarias, Tenerife 38200, Spain.
RI Steeghs, Danny/C-5468-2009
OI Steeghs, Danny/0000-0003-0771-4746
NR 25
TC 40
Z9 40
U1 1
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2003
VL 590
IS 2
BP 1041
EP 1048
DI 10.1086/375055
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 688WA
UT WOS:000183459200037
ER
PT J
AU Wang, J
Yaqoob, T
Szokoly, G
Gilli, R
Kewley, L
Mainieri, V
Nonino, M
Rosati, P
Tozzi, P
Zheng, W
Zirm, A
Norman, C
AF Wang, J
Yaqoob, T
Szokoly, G
Gilli, R
Kewley, L
Mainieri, V
Nonino, M
Rosati, P
Tozzi, P
Zheng, W
Zirm, A
Norman, C
TI A puzzling X-ray source found in the Chandra Deep Field-South
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; galaxies : individual (CXOCDFS J033225.3-274219)
galaxies : peculiar; X-rays : galaxies
ID ACTIVE GALACTIC NUCLEI; EMISSION-LINE; AFTERGLOW; NGC-6240; GALAXY;
BURST
AB In this Letter, we report the detection of an extremely strong X-ray emission line in the 940 ks Chandra ACIS-I spectrum of CXOCDFS J033225.3-274219. The source was identified as a type 1 active galactic nucleus at a redshift of z = 1.617, with a 2.0-10.0 keV rest-frame X-ray luminosity of similar to10(44) ergs s(-1). The emission line was detected at 6.2(-0.1)(+0.2) keV, with an equivalent width ( EW) of 4.4(-1.4)(+3.2) keV; both quantities refer to the observed frame. In the rest frame, the line is at 16.2(-0.3)(+0.4) keV with an EW of 11.5(-3.7)(+8.3) keV. An X-ray emission line at a similar energy(similar to17 keV, in the rest frame) in PKS 2149-306 was discovered before using ASCA data. We reject the possibility that the line is due to a statistical or instrumental artifact. The line is most likely due to blueshifted Fe K emission from an relativistic outflow, probably an inner X-ray jet, with velocities of the order of similar to0.6c-0.7c. Other possible explanations are also discussed.
C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
European So Observ, D-85748 Garching, Germany.
Ist Nazl Astrofis, Osservatorio Astron, I-34131 Trieste, Italy.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
RP Wang, J (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RI Gilli, Roberto/P-1110-2015
OI Gilli, Roberto/0000-0001-8121-6177
NR 20
TC 12
Z9 12
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 20
PY 2003
VL 590
IS 2
BP L87
EP L90
DI 10.1086/376821
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 688WE
UT WOS:000183459600006
ER
PT J
AU Kirshner, RP
AF Kirshner, RP
TI Throwing light on dark energy
SO SCIENCE
LA English
DT Review
ID HIGH-REDSHIFT SUPERNOVAE; HUBBLE DEEP FIELD; IA SUPERNOVAE; COSMOLOGICAL
CONSTANT; ACCELERATING UNIVERSE; ELEMENTARY PARTICLES; LAMBDA;
CONSEQUENCES; DECELERATION; PARAMETERS
AB Supernova observations show that the expansion of the universe has been speeding up. This unexpected acceleration is ascribed to a dark energy that pervades space. Supernova data, combined with other observations, indicate that the universe is about 14 billion years old and is composed of about 30% matter and 70% dark energy. New observational programs can trace the history of cosmic expansion more precisely and over a larger span of time than has been done to date to learn whether the dark energy is a modern version of Einstein's cosmological constant or another form of dark energy that changes with time. Either conclusion is an enigma that points to gaps in our fundamental understanding of gravity.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA.
RP Kirshner, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA.
EM kirshner@cfa.harvard.edu
NR 54
TC 29
Z9 29
U1 0
U2 4
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD JUN 20
PY 2003
VL 300
IS 5627
BP 1914
EP 1918
DI 10.1126/science.1086879
PG 5
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 691RN
UT WOS:000183619400036
PM 12817141
ER
PT J
AU Riley, S
AF Riley, S
TI The difference between you and me.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Lib, Washington, DC USA.
RP Riley, S (reprint author), Smithsonian Inst Lib, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 15
PY 2003
VL 128
IS 11
BP 99
EP 99
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 688XZ
UT WOS:000183463700200
ER
PT J
AU Watters, TR
AF Watters, TR
TI Thrust faults along the dichotomy boundary in the eastern hemisphere of
Mars
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE thrust faults; dichotomy boundary; lobate scarps; Mars; lithospheric
flexure
ID ORBITER LASER ALTIMETER; CRUSTAL DICHOTOMY; LOBATE SCARPS; TERRESTRIAL
PLANETS; GIANT IMPACT; DISPLACEMENT; TOPOGRAPHY; MERCURY; EVOLUTION;
LINKAGE
AB Mars Orbiter Laser Altimetry (MOLA) data have been used to characterize lobate scarps along the dichotomy boundary in the eastern hemisphere of Mars. These structures are the surface expression of thrust faulting of the southern highlands. Displacement on the thrust faults is generally less than 1 km except in the case of the Amenthes Rupes thrust fault, where the maximum displacement is on the order of 3 km. The ratio of maximum displacement to fault length g of the population of thrust faults is similar to6.2 x 10(-3) (n = 26), consistent with previous estimates for Martian thrust faults based on photoclinometrically derived topography, and other planetary thrust fault populations. Thrust faulting is roughly coincident with Late Noachian to Early Hesperian fracturing and normal faulting along the dichotomy boundary. This suggests that the formation of the present-day dichotomy boundary involved compressional and extensional deformation. The long-wavelength topography suggests that the dichotomy boundary in the eastern hemisphere may have been formed by flexure of the southern highlands lithosphere. Lithospheric flexure alone cannot account for the thrust faulting of the highlands along the dichotomy boundary. A combination of stresses due to bending, erosion, and global contraction may have formed the lobate scarp thrust faults.
C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
NR 67
TC 34
Z9 34
U1 0
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD JUN 14
PY 2003
VL 108
IS E6
AR 5054
DI 10.1029/2002JE001934
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 691XJ
UT WOS:000183631000002
ER
PT J
AU Vikhlinin, A
Voevodkin, A
Mullis, CR
VanSpeybroeck, L
Quintana, H
McNamara, BR
Gioia, I
Hornstrup, A
Henry, JP
Forman, WR
Jones, C
AF Vikhlinin, A
Voevodkin, A
Mullis, CR
VanSpeybroeck, L
Quintana, H
McNamara, BR
Gioia, I
Hornstrup, A
Henry, JP
Forman, WR
Jones, C
TI Cosmological constraints from the evolution of the cluster baryon mass
function at z similar to 0.5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmological parameters; galaxies : clusters : general; surveys; X-rays
: galaxies : clusters
ID MEDIUM-SENSITIVITY SURVEY; NEARBY GALAXY CLUSTERS; RAY SCALING
RELATIONS; TEMPERATURE RELATION; INTRACLUSTER MEDIUM; HIGH-REDSHIFT;
DARK-MATTER; FRACTION; OMEGA(M); CONSTANT
AB We present a new method for deriving cosmological constraints based on the evolution of the baryon mass function of galaxy clusters and implement it using 17 distant clusters from our 160 deg(2) ROSAT survey. The method uses the cluster baryon mass as a proxy for the total mass, thereby avoiding the large uncertainties of the M-tot-T or M-tot-L-X relations used in all previous studies. Instead, we rely on a well-founded assumption that the M-b/M-tot ratio is a universal quantity, which should result in a much smaller systematic uncertainty. Taking advantage of direct and accurate Chandra measurements of the gas masses for distant clusters, we find strong evolution of the baryon mass function between z > 0.4 and the present. The observed evolution defines a narrow band in the Omega(m)-Lambda plane, Omega(m) + 0.23Lambda = 0.41 +/- 0.10 at 68% confidence, which intersects with constraints from the cosmic microwave background and Type Ia supernovae near Omega(m) = 0.3 and Lambda = 0.7.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Russian Acad Sci, Space Res Inst, Moscow 117997, Russia.
European So Observ, D-85748 Garching, Germany.
Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile.
Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
CNR, Ist Radioastron, I-40129 Bologna, Italy.
Danish Space Res Inst, DK-2100 Copenhagen O, Denmark.
Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Gioia, Isabella/B-6982-2012
OI Gioia, Isabella/0000-0003-3127-498X
NR 57
TC 65
Z9 65
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 15
EP 25
DI 10.1086/374863
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700003
ER
PT J
AU Winn, JN
Kochanek, CS
Keeton, CR
Lovell, JEJ
AF Winn, JN
Kochanek, CS
Keeton, CR
Lovell, JEJ
TI The quintuple quasar: Radio and optical observations
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing; quasars : individual (PMN J0134-0931)
ID GALACTIC-CENTER; A-ASTERISK; LENS; PKS-1830-211; GALAXY; GHZ
AB We present results from high-resolution radio and optical observations of PMN J0134-0931, a gravitational lens with a unique radio morphology and an extremely red optical counterpart. Our data support the theory of Keeton & Winn: five of the six observed radio components are multiple images of a single quasar, produced by a pair of lens galaxies. Multifrequency Very Long Baseline Array maps show that the sixth and faintest component has a different radio spectrum than the others, confirming that it represents a second component of the background source rather than a sixth image. The lens models predict that there should be additional faint images of this second source component, and we find evidence for one of the predicted images. The previously observed large angular sizes of two of the five bright components are not intrinsic (which would have excluded the possibility that they are lensed images) but are instead due to scatter broadening. Both the extended radio emission observed at low frequencies and the intrinsic image shapes observed at high frequencies can be explained by the lens models. The pair of lens galaxies is marginally detected in Hubble Space Telescope images. The differential extinction of the quasar images suggests that the extreme red color of the quasar is at least partly due to dust in the lens galaxies.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia.
RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 20
TC 16
Z9 16
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 26
EP 38
DI 10.1086/374832
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700004
ER
PT J
AU Keeton, CR
Winn, JN
AF Keeton, CR
Winn, JN
TI The quintuple quasar: Mass models and interpretation
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing; quasars : individual (PMN J0134-0931)
ID GRAVITATIONALLY LENSED QUASAR; EARLY-TYPE GALAXIES; SUBSTRUCTURE;
POTENTIALS; STATISTICS; B1359+154; SYSTEMS; HALOS
AB The strange morphology of the six-component gravitational lens PMN J0134-0931 has resisted explanation. We present the first successful quantitative models for the system, based on the idea that there are two lens galaxies and two components of the background source. One source is quintuply imaged and corresponds to the five brightest observed radio components. The other source is triply imaged and corresponds to the sixth component, along with two others too faint to have been detected. The models reproduce the observed image positions and fluxes and make falsi. able predictions about other properties of the system. Some of these predictions have been confirmed by high-resolution radio and optical observations, as described in the companion paper by Winn and coworkers. Although we cannot determine the lens model uniquely with current data, we predict that the lens galaxies are spiral galaxies with roughly equal velocity dispersions sigma similar to 120 km s(-1) and a projected separation of only 0."4 (2 h(-1) kpc at z(l) = 0.76). This system is the first known lens with five images of a single quasar and the second with more than four images.
C1 Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Keeton, CR (reprint author), Univ Chicago, Ctr Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA.
NR 40
TC 22
Z9 22
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 39
EP 51
DI 10.1086/374833
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700005
ER
PT J
AU Kuraszkiewicz, JK
Wilkes, BJ
Hooper, EJ
McLeod, KK
Wood, K
Bjorkman, J
Delain, KM
Hughes, DH
Elvis, MS
Impey, CD
Lonsdale, CJ
Malkan, MA
McDowell, JC
Whitney, B
AF Kuraszkiewicz, JK
Wilkes, BJ
Hooper, EJ
McLeod, KK
Wood, K
Bjorkman, J
Delain, KM
Hughes, DH
Elvis, MS
Impey, CD
Lonsdale, CJ
Malkan, MA
McDowell, JC
Whitney, B
TI The far-infrared spectral energy distributions of X-ray - Selected
active galaxies
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies : active; galaxies : nuclei; infrared : galaxies; X-rays :
galaxies
ID RADIO-QUIET QUASARS; GALACTIC NUCLEI; SEYFERT-GALAXIES; HOST GALAXIES;
DUST EMISSION; STATISTICAL-METHODS; IONIZING CONTINUUM; ASTRONOMICAL
DATA; STEEP-SPECTRUM; OBSCURING TORI
AB Hard X-ray selection is, arguably, the optimal method for de. ning a representative sample of active galactic nuclei (AGNs). Hard X-rays are unbiased by the effects of obscuration and reprocessing along the line of sight intrinsic/external to the AGN, which result in unknown fractions of the population being missed from traditional optical/soft X-ray samples. We present the far-infrared (far-IR) observations of 21 hard X-ray-selected AGNs from the HEAO 1 A2 sample observed with Infrared Space Observatory (ISO). We characterize the far-IR continua of these X-ray-selected AGNs and compare them with those of various radio and optically selected AGN samples and with models for an AGN-heated, dusty disk. The X-ray selected AGNs show broad, warm IR continua covering a wide temperature range (similar to20-1000 K in a thermal emission scenario). Where a far-IR turnover is clearly observed, the slopes are less than 2.5 in all but three cases so that nonthermal emission remains a possibility, although the presence of cooler dust resulting in a turnover at wavelengths longward of the ISO range is considered more likely. The sample also shows a wider range of optical/UV shapes than the optical/radio-selected samples, extending to redder near-IR colors. The bluer objects are type 1 Seyfert galaxies, while the redder AGNs are mostly intermediate or type 2 Seyfert galaxies. This is consistent with a modified unification model in which obscuration increases as we move from a face-on toward a more edge-on line of sight. However, this relation does not extend to the mid-infrared as the 25/60 mum ratios are similar in Seyfert galaxies with differing type and optical/UV reddening. The resulting limits on the column density of obscuring material through which we are viewing the redder AGNs (N-H similar to 10(22) cm(-2)) are inconsistent with standard optically thick torus models (NH similar to 1024 cm(-2)) and simple unification models. Instead our results support more complex models in which the amount of obscuring material increases with viewing angle and may be clumpy. Such a scenario, already suggested by differing optical/near-IR spectroscopic and X-ray AGN classifications, allows for different amounts of obscuration of the continuum emission in different wave bands and of the broad emission line region, which, in turn, results in a mixture of behaviors for AGNs with similar optical emission-line classifications. The resulting decrease in the optical depth of the obscuring material also allows the AGN to heat more dust at larger radial distances. We show that an AGN-heated, flared, dusty disk with mass of similar to10(9) M. and size of approximately a few hundred parsecs is able to generate optical-far-IR spectral energy distributions (SEDs) that reproduce the wide range of SEDs present in our sample with no need for an additional starburst component to generate the long-wavelength, cooler part of the IR continuum.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Texas, Dept Astron, Austin, TX 78712 USA.
Wellesley Coll, Dept Astron, Wellesley, MA 02481 USA.
Univ St Andrews, Dept Phys & Astron, St Andrews, Fife, Scotland.
Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA.
Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
Inst Natl Astrofis Opt & Elect, Mexico City, DF, Mexico.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
CALTECH, IPAC, Pasadena, CA 91125 USA.
Univ Calif Los Angeles, Dept Astron, Los Angeles, CA 90095 USA.
Space Sci Inst, Boulder, CO 80303 USA.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jkuraszkiewicz@cfa.harvard.edu; bwilkes@cfa.harvard.edu;
ehooper@astro.as.utexas.edu; kmcleod@wellesley.edu;
kw25@st-andrews.ac.uk; jon@astro.utoledo.edu; kdelain@astro.umn.edu;
dhughes@inaoep.mx; melvis@cfa.harvard.edu; impey@as.arizona.edu;
cjl@ipac.caltech.edu; malkan@bonnie.astro.ucla.edu;
jmcdowell@cfa.harvard.edu; bwhitney@colorado.edu
OI Wilkes, Belinda/0000-0003-1809-2364
NR 114
TC 50
Z9 50
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 128
EP 148
DI 10.1086/374919
PN 1
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700014
ER
PT J
AU Peck, AB
Henkel, C
Ulvestad, JS
Brunthaler, A
Falcke, H
Elitzur, M
Menten, KM
Gallimore, JF
AF Peck, AB
Henkel, C
Ulvestad, JS
Brunthaler, A
Falcke, H
Elitzur, M
Menten, KM
Gallimore, JF
TI The flaring H2O megamaser and compact radio source in Markarian 348
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; galaxies : individual (Markarian 348, NGC 262);
galaxies : jets; galaxies : Seyfert; masers; radio lines : galaxies
ID STAR-FORMING REGIONS; ACTIVE GALACTIC NUCLEI; FREE-FREE ABSORPTION;
NARROW-LINE REGION; X-RAY-EMISSION; III ZW 2; SEYFERT-GALAXIES;
WATER-VAPOR; NEUTRAL HYDROGEN; OBSCURING TORUS
AB We report on single-dish monitoring and extremely high angular resolution observations of the flaring H2O megamaser in the Seyfert 2 galaxy Mrk 348. The H2O line is redshifted by similar to130 km s(-1) with respect to the systemic velocity, is very broad, with an FWHM of 130 km s(-1), and has no detectable high-velocity components within 1500 km s(-1) on either side of the strong line. Monitoring observations made with the Effelsberg 100 m telescope show that the maser varies significantly on timescales as short as 1 day and that the integrated line flux is loosely correlated with the continuum flux. Very Long Baseline Array (VLBA) observations indicate that the maser emission arises entirely from a region less than 0.25 pc in extent, located toward a continuum component thought to be associated with the receding jet. We also report on integrated flux monitoring with the VLA between 1.4 and 43 GHz, and VLBA continuum observations of the milliarcsecond scale jets at 1.7, 8, 15, and 22 GHz. These observations have allowed us to tentatively pinpoint the location of the core, and also show the ejection of a new jet component during the current radio "flare''.
C1 Max Planck Inst Radioastron, D-53121 Bonn, Germany.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA.
Bucknell Univ, Dept Phys, Lewisburg, PA 17837 USA.
RP Peck, AB (reprint author), Harvard Smithsonian Ctr Astrophys, SAO SMA Project, POB 824, Hilo, HI 96721 USA.
EM apeck@cfa.harvard.edu
RI Falcke, Heino/H-5262-2012
OI Falcke, Heino/0000-0002-2526-6724
NR 71
TC 52
Z9 53
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 149
EP 161
DI 10.1086/374924
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700015
ER
PT J
AU Greenhill, LJ
Booth, RS
Ellingsen, SP
Herrnstein, JR
Jauncey, DL
McCulloch, PM
Moran, JM
Norris, RP
Reynolds, JE
Tzioumis, AK
AF Greenhill, LJ
Booth, RS
Ellingsen, SP
Herrnstein, JR
Jauncey, DL
McCulloch, PM
Moran, JM
Norris, RP
Reynolds, JE
Tzioumis, AK
TI A warped accretion disk and wide-angle outflow in the inner parsec of
the Circinus galaxy
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; galaxies : individual (Circinus); galaxies : Seyfert;
ISM : jets and outflows; ISM : molecules; masers
ID ACTIVE GALACTIC NUCLEI; WATER MASER EMISSION; STAR-FORMING REGIONS;
SEYFERT-GALAXIES; MOLECULAR DISK; LINE REGION; H2O MASERS; NGC-4258;
NGC-5548; SPECTROPOLARIMETRY
AB We present the first VLBI maps of H2O maser emission (lambda1.3 cm) in the nucleus of the Circinus galaxy, constructed from data obtained with the Australia Telescope Long Baseline Array. The maser emission traces a warped, edge-on accretion disk between radii of 0.11 +/- 0.02 and similar to0.40 pc, as well as a wide-angle outflow that extends up to similar to1 pc from the estimated disk center. The disk rotation is close to Keplerian ( v proportional to r(-0).5), the maximum detected rotation speed is 260 km s(-1), and the inferred central mass is (1.7 +/- 0.3) x 106 M.. The out. owing masers are irregularly distributed above and below the disk, with relative outflow velocities up to similar to+/-160 km s(-1), projected along the line of sight. The flow probably originates closer than 0.1 pc to the central engine, possibly in an inward extension of the accretion disk, although there is only weak evidence of rotation in the outward-moving material. We observe that the warp of the disk appears to collimate the outflow and to. x the extent of the ionization cone observed on larger angular scales. This study provides the first direct evidence (i.e., through imaging) of dusty, high-density, molecular material in a nuclear outflow less than 1 pc from the central engine of a Seyfert galaxy, as well as the first graphic evidence that warped accretion disks can channel outflows and illumination patterns in active galactic nuclei. We speculate that the same arrangement, which in some ways obviates the need for a geometrically thick, dusty torus, may apply to other type 2 active galactic nuclei.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Chalmers Inst Technol, Onsala Space Observ, S-43992 Onsala, Sweden.
Univ Tasmania, Sch Phys, Hobart, Tas 7001, Australia.
Australia Telescope Natl Facil, Epping, NSW 2121, Australia.
RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Ellingsen, Simon/J-7754-2014; Norris, Ray/A-1316-2008;
OI Ellingsen, Simon/0000-0002-1363-5457; Norris, Ray/0000-0002-4597-1906;
Moran, James/0000-0002-3882-4414
NR 50
TC 178
Z9 180
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 162
EP 173
DI 10.1086/374862
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700016
ER
PT J
AU Churazov, E
Forman, W
Jones, C
Bohringer, H
AF Churazov, E
Forman, W
Jones, C
Bohringer, H
TI XMM-Newton observations of the Perseus Cluster. I. The temperature and
surface brightness structure
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cooling flows; galaxies : active; galaxies : clusters : individual
(Perseus); galaxies : individual (NGC 1275); X-rays : galaxies; X-rays :
galaxies : clusters
ID RAY-EMITTING GAS; GALAXY CLUSTERS; NGC-1275; ROSAT; RADIO; CORE; IMAGES;
FLOWS; ASCA
AB We present preliminary results of a XMM-Newton 50 ks observation of the Perseus Cluster that provides an unprecedented view of the central 0.5 Mpc region. The projected gas temperature declines smoothly by a factor of 2 from a maximum value of similar to 7 keV in the outer regions to just above 3 keV at the cluster center. Over this same range, the heavy-element abundance rises slowly from 0.4 to 0.5 solar as the radius decreases from 140 to 50, and then it rises to a peak of almost 0.7 solar at 1.'25 before declining to 0.4 at the center. The global east-west asymmetry of the gas temperature and surface brightness distributions, approximately aligned with the chain of bright galaxies, suggests an ongoing merger, although the modest degree of the observed asymmetry certainly excludes a major merger interpretation. The chain of galaxies probably traces the. lament along which accretion started some time ago and is continuing at the present time. A cold and dense (low-entropy) cluster core like Perseus is probably well "protected'' against the penetration of the gas of infalling groups and poor clusters, whereas in noncooling core clusters such as Coma and A1367, infalling subclusters can penetrate deeply into the core region. In Perseus, gas associated with infalling groups may be stripped completely at the outskirts of the main cluster and only compression waves (shocks) may reach the central regions. We argue, and show supporting simulations, that the passage of such a wave(s) can qualitatively explain the overall horseshoe shaped appearance of the gas temperature map (the hot horseshoe surrounds the colder, low-entropy core) as well as other features of the Perseus Cluster core. These simulations also show that as compression waves traverse the cluster core, they can induce oscillatory motion of the cluster gas that can generate multiple sharp "edges'' on opposite sides of the central galaxy. Gas motions induced by mergers may be a natural way to explain the high frequency of "edges'' seen in clusters with cooling cores.
C1 Max Planck Inst Astrophys, D-85740 Garching, Germany.
Space Res Inst IKI, Moscow 117810, Russia.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany.
RI Churazov, Eugene/A-7783-2013
NR 50
TC 186
Z9 187
U1 1
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 225
EP 237
DI 10.1086/374923
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700022
ER
PT J
AU Luhman, KL
Briceno, C
Stauffer, JR
Hartmann, L
Navascues, DBY
Caldwell, N
AF Luhman, KL
Briceno, C
Stauffer, JR
Hartmann, L
Navascues, DBY
Caldwell, N
TI New low-mass members of the Taurus star-forming region
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared : stars; stars : evolution; stars : formation; stars :
low-mass, brown dwarfs; stars : luminosity function, mass function;
stars : pre-main-sequence
ID BROWN DWARFS; MAIN-SEQUENCE; EMISSION; SPECTROSCOPY; ACCRETION; OBJECT;
IC-348; L1495E; LIMIT
AB Briceno et al. recently used optical imaging, data from the Two-Micron All-Sky Survey (2MASS), and follow-up spectroscopy to search for young low-mass stars and brown dwarfs in 8 deg(2) of the Taurus star-forming region. By the end of that study, there remained candidate members of Taurus that lacked the spectroscopic observations needed to measure spectral types and determine membership. In this work, we have obtained spectroscopy of the 22 candidates that have A(V) less than or equal to 8, from which we find six new Taurus members with spectral types of M2.75 through M9. The new M9 source has the second latest spectral type of the known members of Taurus (similar to0.02 M-.). Its spectrum contains extremely strong emission in Halpha (W-lambda similar to 950 Angstrom), as well as emission in He I 6678 Angstrom and the Ca II IR triplet. This is the least massive object known to exhibit emission in He I and Ca II, which together with the strong Halpha are suggestive of intense accretion.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Ctr Invest Astron, Merida 5101 A, Venezuela.
CALTECH, SIRTF Sci Ctr, MS 314 6, Pasadena, CA 91125 USA.
RP Luhman, KL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Barrado Navascues, David/C-1439-2017
OI Barrado Navascues, David/0000-0002-5971-9242
NR 30
TC 127
Z9 127
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 348
EP 356
DI 10.1086/374983
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700033
ER
PT J
AU Antiochos, SK
Karpen, JT
DeLuca, EE
Golub, L
Hamilton, P
AF Antiochos, SK
Karpen, JT
DeLuca, EE
Golub, L
Hamilton, P
TI Constraints on active region coronal heating
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun : corona; Sun : transition region; Sun : UV radiation
ID TRANSITION REGION; SOLAR CORONA; LOOPS; EXPLORER; TRACE; TEMPERATURE;
DIAGNOSTICS; NANOFLARES; PLASMA; MODELS
AB We derive constraints on the time variability of coronal heating from observations of the so-called active region moss by the Transition Region and Coronal Explorer ( TRACE). The moss is believed to be due to million-degree emission from the transition regions at the footpoints of coronal loops whose maximum temperatures are several million degrees. The two key results from the TRACE observations discussed in this paper are that in the moss regions one generally sees only moss, not million-degree loops, and that the moss emission exhibits only weak intensity variations, similar to10% over periods of hours. TRACE movies showing these results are presented. We demonstrate, using both analytic and numerical calculations, that the lack of observable million-degree loops in the moss regions places severe constraints on the possible time variability of coronal heating in the loops overlying the moss. In particular, the heating in the hot moss loops cannot be truly flarelike with a sharp cutoff, but instead must be quasi-steady to an excellent approximation. Furthermore, the lack of significant variations in the moss intensity implies that the heating magnitude is only weakly varying. The implications of these conclusions for coronal heating models will be discussed.
C1 USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA.
EM antiochos@nrl.navy.mil
RI Karpen, Judith/E-1484-2012; Antiochos, Spiro/D-4668-2012; Hamilton,
Paul/E-7891-2015; DeLuca, Edward/L-7534-2013
OI Antiochos, Spiro/0000-0003-0176-4312; Hamilton,
Paul/0000-0001-6080-632X; DeLuca, Edward/0000-0001-7416-2895
NR 30
TC 58
Z9 58
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP 547
EP 553
DI 10.1086/375003
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TE
UT WOS:000183278700049
ER
PT J
AU Kong, AKH
Sjouwerman, LO
Williams, BF
Garcia, MR
Dickel, JR
AF Kong, AKH
Sjouwerman, LO
Williams, BF
Garcia, MR
Dickel, JR
TI Discovery of radio/X-ray/optical-resolved supernova remnants in the
center of the Andromeda galaxy
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (M31); supernova remnants; X-rays : ISM
ID LARGE-MAGELLANIC-CLOUD; RAY POINT SOURCES; X-RAY; NOVA REMNANTS;
CASSIOPEIA-A; M31; CHANDRA; EMISSION; CANDIDATES; RCW-103
AB We have detected a spatially resolved supernova remnant (SNR) in the center of the Andromeda galaxy, in radio, X-ray, and optical wavelengths. These observations provide the highest spatial resolution imaging of a radio/X-ray/optical SNR in that galaxy to date. The multiwavelength morphology, radio spectral index, X-ray colors, and narrowband optical imaging are consistent with a shell-type SNR. A second SNR is also seen resolved in both radio and X-ray. By comparing the morphological structure of the SNRs in different wavelengths and with that in our own Galaxy, we can study the shock morphologies of SNRs in the Andromeda galaxy. The proximity of the SNRs to the core suggests a high interstellar medium density in the vicinity of the SNRs in the center of the Andromeda galaxy.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 39
TC 21
Z9 21
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP L21
EP L24
DI 10.1086/376687
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TF
UT WOS:000183278800006
ER
PT J
AU Kong, AKH
Di Stefano, R
AF Kong, AKH
Di Stefano, R
TI A luminous recurrent supersoft X-ray source in NGC 300
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 300); X-rays : binaries; X-rays : galaxies
ID GALAXY NGC-300; SPACED DATA; CHANDRA; CATALOG
AB We report the results of XMM-Newton observations for an especially luminous supersoft X-ray source (SSS) with a bolometric luminosity of 10(39) ergs s(-1) in the spiral galaxy NGC 300. The source was detected as an SSS in 1992 and disappeared in subsequent X-ray observations. The source was active again during recent XMM-Newton observations. It appeared to be very soft (kT similar to 60 eV) and very luminous (similar to10(38)-10(39) ergs s(-1)). The two XMM-Newton observations also reveal that the source went from a "high" state to a "low" state in 6 days. We also found a 5.4 hr periodicity during the low state. We consider white dwarf, black hole, and neutron star models in order to explain the nature of the source.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 25
TC 28
Z9 28
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP L13
EP L16
DI 10.1086/376552
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TF
UT WOS:000183278800004
ER
PT J
AU McMahon, RJ
McCarthy, MC
Gottlieb, CA
Dudek, JB
Stanton, JF
Thaddeus, P
AF McMahon, RJ
McCarthy, MC
Gottlieb, CA
Dudek, JB
Stanton, JF
Thaddeus, P
TI The radio spectrum of the phenyl radical
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : molecules; line : identification; molecular data; molecular
processes; radio lines : ISM
ID MOLECULAR LINE SURVEY; BENZENE; CRL-618; ORION; BEAM; GHZ
AB The phenyl radical, C6H5, derived from benzene by removal of one hydrogen atom, was detected at centimeter wavelengths in a pulsed supersonic molecular beam and subsequently at millimeter wavelengths in a low-pressure direct current glow discharge. Fourteen rotational transitions between 9 and 40 GHz and over 50 transitions between 150 and 330 GHz, each split by spin doubling, have been measured for the normal isotopic species, and a comparable number have been measured for the fully deuterated species. The spectrum of both isotopic species at millimeter wavelengths is reproduced to an uncertainty of 0.5 km s(-1) or better with seven spectroscopic constants. Rotational constants predicted from high-level molecular structure calculations are in excellent agreement with the measurements. Phenyl is a prime candidate for astronomical detection, because it is the prototypical aromatic hydrocarbon radical and a possible progenitor of other aromatic species.
C1 Univ Wisconsin, Dept Chem, Madison, WI 53706 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
Univ Texas, Dept Chem & Biochem, Inst Theoret Chem, Austin, TX 78712 USA.
RP McMahon, RJ (reprint author), Univ Wisconsin, Dept Chem, 1101 Univ Ave, Madison, WI 53706 USA.
NR 24
TC 28
Z9 28
U1 1
U2 10
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 10
PY 2003
VL 590
IS 1
BP L61
EP L64
DI 10.1086/376587
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 685TF
UT WOS:000183278800016
ER
PT J
AU Soon, W
Baliunas, S
Idso, SB
Kondratyev, KY
Posmentier, ES
AF Soon, W
Baliunas, S
Idso, SB
Kondratyev, KY
Posmentier, ES
TI Modeling climatic effects of anthropogenic carbon dioxide emissions:
unknowns and uncertainties. Reply to Karoly et al. (2003)
SO CLIMATE RESEARCH
LA English
DT Editorial Material
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Mt Wilson Observ, Mt Wilson, CA 91023 USA.
US Water Conservat Lab, Phoenix, AZ 85040 USA.
Russian Acad Sci, Res Ctr Ecol Safety, St Petersburg 197110, Russia.
Long Isl Univ, Brooklyn, NY 11201 USA.
RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 5
TC 0
Z9 0
U1 1
U2 4
PU INTER-RESEARCH
PI OLDENDORF LUHE
PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY
SN 0936-577X
J9 CLIMATE RES
JI Clim. Res.
PD JUN 10
PY 2003
VL 24
IS 1
BP 93
EP 94
DI 10.3354/cr024093
PG 2
WC Environmental Sciences; Meteorology & Atmospheric Sciences
SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences
GA 741FQ
UT WOS:000186448400010
ER
PT J
AU Weck, PF
Stancil, PC
Kirby, K
AF Weck, PF
Stancil, PC
Kirby, K
TI Theoretical study of the rovibrationally resolved transitions of CaH
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID ELECTRONIC STATES; SPECTRA; COEFFICIENTS; MOLECULES
AB Comprehensive absorption line lists for (CaH)-Ca-40 have been calculated for electronic transitions from the X(2)Sigma(+) ground state to the A (2)Pi, B/B' (2)Sigma(+), and E (2)Pi low-lying excited states. The lists include transition energies and oscillator strengths for all possible allowed transitions and were computed using the most recent set of theoretical potential energy curves and dipole transition moment functions, with adjustments to account for experimental dissociation energies and asymptotic limits. Good agreement with previous calculations and available experimental data has been obtained. Oscillator strengths for the transition from the X (2)Sigma(+) state to the D (2)Sigma(+) state are also given, but due to the large uncertainty of the available dipole transition moment function the line list is highly uncertain. For the C (2)Sigma(+) <-- X (2)&USigma;(+) transition, a Franck-Condon approximation has been used. (C) 2003 American Institute of Physics.
C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA.
RP Weck, PF (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
OI , Philippe/0000-0002-7610-2893
NR 26
TC 26
Z9 26
U1 0
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD JUN 8
PY 2003
VL 118
IS 22
BP 9997
EP 10005
DI 10.1063/1.1573181
PG 9
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 680TC
UT WOS:000182993800012
ER
PT J
AU Kreamer, CM
AF Kreamer, CM
TI A tribute to Roy Sieber Part 2 (His contributions as the consummate
connoisseur of tradition-based African arts)
SO AFRICAN ARTS
LA English
DT Article
C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
NR 30
TC 0
Z9 0
U1 0
U2 0
PU UNIV CALIF
PI LOS ANGELES
PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA
SN 0001-9933
J9 AFR ARTS
JI Afr. Arts
PD SUM
PY 2003
VL 36
IS 2
BP 10
EP +
PG 0
WC Art
SC Art
GA 751XQ
UT WOS:000187115900004
ER
PT J
AU Moffett, D
Mellor, S
AF Moffett, D
Mellor, S
TI The curator-conservator collaboration - Remembering Roy Sieber (African
art connoisseurship and the contribution of science)
SO AFRICAN ARTS
LA English
DT Article
C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
RP Moffett, D (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
NR 11
TC 0
Z9 0
U1 0
U2 0
PU UNIV CALIF
PI LOS ANGELES
PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA
SN 0001-9933
J9 AFR ARTS
JI Afr. Arts
PD SUM
PY 2003
VL 36
IS 2
BP 44
EP +
PG 0
WC Art
SC Art
GA 751XQ
UT WOS:000187115900006
ER
PT J
AU Arnoldi, MJ
AF Arnoldi, MJ
TI Symbolically inscribing the city - Public monuments in Mali, 1995-2002
SO AFRICAN ARTS
LA English
DT Article
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 5
TC 5
Z9 5
U1 0
U2 0
PU UNIV CALIF
PI LOS ANGELES
PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA
SN 0001-9933
J9 AFR ARTS
JI Afr. Arts
PD SUM
PY 2003
VL 36
IS 2
BP 56
EP +
PG 0
WC Art
SC Art
GA 751XQ
UT WOS:000187115900007
ER
PT J
AU Hacker, BC
AF Hacker, BC
TI Amchitka and the bomb: Nuclear testing in Alaska.
SO AMERICAN HISTORICAL REVIEW
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Hacker, BC (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER HISTORICAL REVIEW
PI WASHINGTON
PA 400 A ST SE, WASHINGTON, DC 20003 USA
SN 0002-8762
J9 AM HIST REV
JI Am. Hist. Rev.
PD JUN
PY 2003
VL 108
IS 3
BP 873
EP 874
DI 10.1086/529686
PG 2
WC History
SC History
GA 692CU
UT WOS:000183643400095
ER
PT J
AU Jantz, RL
Owsley, DW
AF Jantz, RL
Owsley, DW
TI Reply to Van Vark et al.: Is European Upper Paleolithic cranial
morphology a useful analogy for early Americans?
SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY
LA English
DT Editorial Material
DE cranial morphology; Paleoamericans; population history
ID CRANIOMETRIC VARIATION; PLEISTOCENE; ORIGINS; SHAPE
C1 Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA.
Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA.
RP Jantz, RL (reprint author), Univ Tennessee, Dept Anthropol, Knoxville, TN 37996 USA.
NR 33
TC 18
Z9 18
U1 0
U2 1
PU WILEY-LISS
PI NEW YORK
PA DIV JOHN WILEY & SONS INC, 605 THIRD AVE, NEW YORK, NY 10158-0012 USA
SN 0002-9483
J9 AM J PHYS ANTHROPOL
JI Am. J. Phys. Anthropol.
PD JUN
PY 2003
VL 121
IS 2
BP 185
EP 188
DI 10.1002/ajpa.10188
PG 4
WC Anthropology; Evolutionary Biology
SC Anthropology; Evolutionary Biology
GA 682HB
UT WOS:000183084700011
ER
PT J
AU Power, ML
Tardif, SD
Power, RA
Layne, DG
AF Power, ML
Tardif, SD
Power, RA
Layne, DG
TI Resting energy metabolism of Goeldi's monkey (Callimico goeldii) is
similar to that of other callitrichids
SO AMERICAN JOURNAL OF PRIMATOLOGY
LA English
DT Article
DE metabolic rate; Callitrichidae; circadian phase; primates
ID THERMOREGULATION; PRIMATES
AB The resting metabolic rates (RMRs) of six adult Goeldi's monkeys (Callimico, goeldii) were measured using standard methods of open circuit respirometry during both the active (daytime) and inactive (nighttime) circadian phases for this species. One subject was measured both while she was pregnant and after she delivered a full-term, stillborn infant. Inactive-phase RMR within thermal neutrality (above 27.5degreesC) averaged 288.5 +/- 30.8 ml O-2/hr; active-phase RMR within thermal neutrality averaged 416.3 +/- 60.9 ml O-2/hr. These values are 74.6% and 107.6%, respectively, of the mammalian expected for animals of this body mass. During the inactive phase, metabolic rate increased an estimated 4.3% for every degree decline in temperature below 27.5degreesC. The RMR in Goeldi's monkey is similar quantitatively and qualitatively to those of other captive callitrichids that have been studied, with active-phase RMR being at or slightly above the mammalian expected, and inactive-phase RMR being significantly reduced. We propose that this circadian pattern of RMR is a consequence of small body size, and is not a specific metabolic adaptation within the Callitrichidae. Thus we predict that metabolic studies measuring both circadian phases in other small primates will also find this pattern of reduced RMR during the inactive phase. The inactive-phase RMR within thermal neutrality of the pregnant female was not different from that measured after the stillbirth, despite an almost 15% difference in body mass. During pregnancy, however, the female was more metabolically responsive to temperature below thermal neutrality, and had a lower upper critical temperature (i.e., was less tolerant of heat). (C) 2003 Wiley-Liss, Inc.
C1 Smithsonian Natl Zool Pk, Dept Conservat Biol, Nutr Lab, Washington, DC 20008 USA.
SW Reg Primate Res Ctr, San Antonio, TX USA.
Univ Florida, Coll Vet Med, Dept Physiol Sci, Gainesville, FL 32610 USA.
RP Power, ML (reprint author), Smithsonian Natl Zool Pk, Dept Conservat Biol, Nutr Lab, Washington, DC 20008 USA.
EM powerm@nzp.si.edu
OI Power, Michael/0000-0002-6120-3528
FU NCRR NIH HHS [RR2022]
NR 31
TC 4
Z9 4
U1 0
U2 6
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0275-2565
EI 1098-2345
J9 AM J PRIMATOL
JI Am. J. Primatol.
PD JUN
PY 2003
VL 60
IS 2
BP 57
EP 67
DI 10.1002/ajp.10078
PG 11
WC Zoology
SC Zoology
GA 697TN
UT WOS:000183959500003
PM 12784286
ER
PT J
AU Bloom, JS
AF Bloom, JS
TI Is the redshift clustering of long-duration gamma-ray bursts
significant?
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology : miscellaneous; cosmology : observations; gamma rays
ID HOST GALAXY; OPTICAL AFTERGLOW; SPACE DENSITIES; MS 1054-03; DISCOVERY;
LUMINOSITIES; SPECTROSCOPY; SUPERNOVA; FAINT; IDENTIFICATION
AB The 26 long-duration gamma-ray bursts (GRBs) with known redshifts form a distinct cosmological set, selected differently than other cosmological probes such as quasars and galaxies. Since the progenitors are now believed to be connected with active star formation and since burst emission penetrates dust, one hope is that with a uniformly selected sample, the large-scale redshift distribution of GRBs can help constrain the star formation history of the universe. However, we show that strong observational biases in ground-based redshift discovery hamper a clean determination of the large-scale GRB rate and hence the connection of GRBs to the star formation history. We then focus on the properties of the small-scale (clustering) distribution of GRB redshifts. When corrected for heliocentric motion relative to the local Hubble flow, the observed redshifts appear to show a propensity for clustering: eight of 26 GRBs occurred within a recession velocity difference of 1000 km s(-1) of another GRB. That is, four pairs of GRBs occurred within 30 h(65)(-1) Myr in cosmic time, despite being causally separated on the sky. We investigate the significance of this clustering using a simulation that accounts for at least some of the strong observational and intrinsic biases in redshift discovery. Comparison of the numbers of close redshift pairs expected from the simulation with that observed shows no significant small-scale clustering excess in the present sample; however, the four close pairs occur in only about 20% of the simulated data sets (the precise significance of the clustering is dependent on the modeled biases). We conclude with some impetuses and suggestions for future precise GRB redshift measurements.
C1 Harvard Soc Fellows, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Harvard Soc Fellows, 78 Mt Auburn St, Cambridge, MA 02138 USA.
NR 68
TC 36
Z9 36
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
EI 1538-3881
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2003
VL 125
IS 6
BP 2865
EP 2875
DI 10.1086/374945
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 684YM
UT WOS:000183234100008
ER
PT J
AU Caldwell, N
Rose, JA
Concannon, KD
AF Caldwell, N
Rose, JA
Concannon, KD
TI Star formation histories of early-type galaxies. I. Higher order Balmer
lines as age indicators
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies : abundances; galaxies : stellar content
ID OLD STELLAR POPULATIONS; COLOR-MAGNITUDE RELATION; DWARF ELLIPTIC
GALAXIES; M31 GLOBULAR-CLUSTERS; VIRGO CLUSTER; 47 TUCANAE;
SPECTRAL-RESOLUTION; EVOLUTIONARY TRACKS; INTEGRATED SPECTRA;
SPECTROSCOPIC AGE
AB We have obtained blue integrated spectra of 175 nearby early-type galaxies, covering a wide range in galaxy velocity dispersion and emphasizing those with sigma<100 km s(-1). Galaxies have been observed both in the Virgo Cluster and in lower density environments. The main goals are the evaluation of higher order Balmer lines as age indicators and differences in stellar populations as a function of mass, environment, and morphology. In this first paper, our emphasis is on presenting the methods used to characterize the behavior of the Balmer lines through evolutionary population synthesis models. Lower σ galaxies exhibit a substantially greater intrinsic scatter, in a variety of line-strength indicators, than do higher σ galaxies, with the large intrinsic scatter setting in below a σ of 100 km s(-1). Moreover, a greater contrast in scatter is present in the Balmer lines than in the lines of metal features. Evolutionary synthesis modeling of the observed spectral indexes indicates that the strong Balmer lines found primarily among the low-σ galaxies are caused by young age, rather than by low metallicity. Thus we find a trend between the population age and the central velocity dispersion, such that low-σ galaxies have younger luminosity-weighted mean ages. We have repeated this analysis using several different Balmer lines and find consistent results from one spectral indicator to another.
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
RP Caldwell, N (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
NR 79
TC 145
Z9 146
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2003
VL 125
IS 6
BP 2891
EP 2926
DI 10.1086/375308
PG 36
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 684YM
UT WOS:000183234100010
ER
PT J
AU Schlegel, EM
Pannuti, TG
AF Schlegel, EM
Pannuti, TG
TI Chandra-detected X-ray sources in the nearby spiral Scd galaxy NGC 2403
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 2403); galaxies : spiral; X-rays
ID SUPERNOVA-REMNANTS; STAR-FORMATION; RADIO SEARCH; ETA-CARINAE; NGC-2403;
ROSAT; NGC-6946; EMISSION; LUMINOSITY; STARBURST
AB We present an analysis of a 35.6 ks observation made with the Chandra X-Ray Observatory of the nearby spiral Scd galaxy NGC 2403. Forty-one discrete sources are detected at a significance of 3 sigma or greater within the portion of the galaxy sampled by the Chandra detectors. The luminosities of the discrete sources range from similar to10(36) through similar to10(39) ergs s(-1) over the energy range of 0.5-10 keV. We have also analyzed Einstein, ROSAT, and ASCA observations of this galaxy to search for time variability from the detected sources. One luminous X-ray source seen in an Einstein observation of this galaxy is not detected by Chandra or in a separate observation made with ASCA, while a luminous source observed by Chandra was not detected by Einstein or ASCA. For the four most luminous X-ray sources detected by the Chandra observation including one previously identified as an ultraluminous X-ray source-spectral fits to these sources provide the best broadband CCD spectra to date. We have searched for counterparts at optical and radio wavelengths. Only one of the 35 optically identified supernova remnants (SNRs) in this galaxy, MFBL 31, is clearly associated with an X-ray source in our sample. Three other optically identified SNRs-MFBL 15, MFBL 17, and MFBL 29-may also have X-ray counterparts, but the associations are far less robust. A similar search for X-ray counterparts to known discrete radio sources seen toward NGC 2403 yields a single coincidence between an X-ray source and a candidate radio SNR, TH-2. None of the detected X-ray sources are coincident with either candidate globular clusters or massive star clusters associated with NGC 2403. The only historical supernova in NGC 2403, SN 1954J, is not detected; neither is an X-ray counterpart to the galaxy's optical nucleus detected. Finally, we confirm the diffuse emission results of Fraternali et al.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 56
TC 21
Z9 21
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2003
VL 125
IS 6
BP 3025
EP 3036
DI 10.1086/374990
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 684YM
UT WOS:000183234100018
ER
PT J
AU Mochejska, BJ
Stanek, KZ
Kaluzny, J
AF Mochejska, BJ
Stanek, KZ
Kaluzny, J
TI Long-term variability survey of the old open cluster NGC 6791
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries : eclipsing; color-magnitude diagrams; novae, cataclysmic
variables; open clusters and associations : individual (NGC 6791); stars
: variables : other
ID IMAGE SUBTRACTION; CCD PHOTOMETRY; VARIABLE-STARS; BINARY STARS;
NGC-6791; SEARCH; FIELD; DISCOVERY; SYSTEMS
AB We present the results of a long-term variability survey of the old open cluster NGC 6791. The BVI observations, collected over a time span of 6 years, were analyzed using the ISIS image subtraction package. The main target of our observations were two cataclysmic variables, B7 and B8. We have identified possible cycle lengths of about 25 and 18 days for B7 and B8, respectively. We tentatively classify B7 as a VY Sculptoris type nova-like variable or a Z Camelopardalis type dwarf nova. B8 is most likely an SS Cygni type dwarf nova. We have also extracted the light curves of 42 other previously reported variable stars and discovered seven new ones. The new variables show long-period or nonperiodic variability. The long baseline of our observations has also allowed us to derive more precise periods for the variables, especially for the short-period eclipsing binaries.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
RP Mochejska, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 26
TC 16
Z9 16
U1 1
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2003
VL 125
IS 6
BP 3175
EP 3184
DI 10.1086/374993
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 684YM
UT WOS:000183234100028
ER
PT J
AU Torres, G
Mader, JA
Marschall, LA
Neuhauser, R
Duffy, AS
AF Torres, G
Mader, JA
Marschall, LA
Neuhauser, R
Duffy, AS
TI Optical photometry and X-ray monitoring of the "cool Algol" BD +05
degrees 706: Determination of the physical properties
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries : eclipsing; binaries : spectroscopic; stars : activity; stars
: fundamental parameters; stars : individual (BD+05 degrees 706)
ID BINARY STAR LIGHT; ECLIPSING BINARIES; SPECTROSCOPIC BINARIES;
DIFFERENTIAL ROTATION; ABSOLUTE DIMENSIONS; MAIN-SEQUENCE; SPOT;
MONOCEROTIS; STARSPOTS; SYSTEMS
AB We present new photometric observations in the BVRI bands of the double-lined eclipsing binary BD + 05degrees706 conducted over three observing seasons, as well as new X-ray observations obtained with ROSAT covering a full orbital cycle ( P = 18.9 days). A detailed light-curve analysis of the optical data shows the system to be semidetached, confirming indications from an earlier analysis by Torres et al. (published in 1998), with the less massive and cooler star filling its Roche lobe. The system is a member of the rare class of cool Algol systems, which are different from the "classical'' Algol systems in that the mass-gaining component is also a late-type star rather than a B- or A-type star. By combining the new photometry with a reanalysis of the spectroscopic observations reported by Torres et al., we derive accurate absolute masses for the components of M-1 = 2.633 +/- 0.028 M-. and M-2 = 0.5412 +/- 0.0093 M-., radii of R-1 = 7.55 +/- 0.20 R-. and R-2 = 11.02 +/- 0.21 R-., as well as effective temperatures of 5000 +/- 100 and 4640 +/- 150 K, for the primary and secondary, respectively. There are obvious signs of activity (spottedness) in the optical light curve of the binary. Our X-ray light curve clearly shows the primary eclipse but not the secondary eclipse, suggesting that the primary star is the dominant source of the activity in the system. The depth and duration of the eclipse allow us to infer some of the properties of the X-ray-emitting region around that star.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Texas, McDonald Observ, Hobby Eberly Telescope, Ft Davis, TX 79734 USA.
Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA.
Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
Univ Jena, Inst Astrophys, D-07445 Jena, Germany.
Univ Jena, Univ Sternwarte, D-07445 Jena, Germany.
RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 51
TC 4
Z9 4
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD JUN
PY 2003
VL 125
IS 6
BP 3237
EP 3251
DI 10.1086/375203
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 684YM
UT WOS:000183234100034
ER
PT J
AU Haverkorn, M
Katgert, P
de Bruyn, AG
AF Haverkorn, M
Katgert, P
de Bruyn, AG
TI Multi-frequency polarimetry of the Galactic radio background around 350
MHz - II. A region in Horologium around l=137 degrees, b=7 degrees
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic
fields; ISM : structure; radio continuum : ISM
ID GALAXY; POLARIZATION; SCALE
AB We study a conspicuous ring-like structure with a radius of about 1.4degrees which was observed with the Westerbork Synthesis Radio Telescope (WSRT) at 5 frequencies around 350 MHz. This ring is very prominent in Stokes Q and U, and less so in polarized intensity P. No corresponding structure is visible in total intensity Stokes I, which indicates that the ring is created by Faraday rotation and depolarization processes. The polarization angle changes from the center of the ring outwards to a radius greater than or similar to1.7degrees. Thus, the structure in polarization angle is not ring-like but resembles a disk, and it is larger than the ring in P. The rotation measure RM decreases almost continuously over the disk, from RM approximate to 0 rad m(-2) at the edge, to -8 rad m(-2) in the center, while outside the ring the RM is slightly positive. This radial variation of RM yields stringent constraints on the nature of the ring-like structure, because it rules out any spherically symmetrical magnetic field configuration, such as might be expected from supernova remnants or wind-blown bubbles. We discuss several possible connections between the ring and known objects in the ISM, and conclude that the ring is a predominantly magnetic funnel-like structure. This description can explain both the field reversal from outside to inside the ring, and the increase in magnetic field, probably combined with an electron density increase, towards the center of the ring. The ring-structure in P is most likely caused by a lack of depolarization due to a very uniform RM distribution at that radius. Beyond the ring, the RM gradient increases, depolarizing the polarized emission, so that the polarized intensity decreases. In the southwestern corner of the field a pattern of narrow filaments of low polarization, aligned with Galactic longitude, is observed, indicative of beam depolarization due to abrupt changes in RM. This explanation is supported by the observed RM.
C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands.
Kapteyn Inst, NL-9700 AV Groningen, Netherlands.
Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA.
EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl
NR 40
TC 37
Z9 37
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 404
IS 1
BP 233
EP 247
DI 10.1051/0004-6361:20030530
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FP
UT WOS:000183081300025
ER
PT J
AU Menard, B
Hamana, T
Bartelmann, M
Yoshida, N
AF Menard, B
Hamana, T
Bartelmann, M
Yoshida, N
TI Improving the accuracy of cosmic magnification statistics
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE cosmology : gravitational lensing; cosmology : large-scale structure of
Universe
ID LARGE-SCALE STRUCTURE; QUASAR-GALAXY CORRELATIONS; ANGULAR-CORRELATIONS;
DARK-MATTER; SHEAR; SIMULATIONS; FIELDS; HYDRA; BIAS; QSO
AB The systematic magnification of background sources by the weak gravitational-lensing effects of foreground matter, also called cosmic magnification, is becoming an efficient tool both for measuring cosmological parameters and for exploring the distribution of galaxies relative to the dark matter. We extend here the formalism of magnification statistics by estimating the contribution of second-order terms in the Taylor expansion of the magnification and show that the effect of these terms was previously underestimated. We test our analytical predictions against numerical simulations and demonstrate that including second-order terms allows the accuracy of magnification-related statistics to be substantially improved. We also show, however, that both numerical and analytical estimates can provide only lower bounds to real correlation functions, even in the weak lensing regime. We propose to use count-in-cells estimators rather than correlation functions for measuring cosmic magnification since they can more easily be related to correlations measured in numerical simulations.
C1 Max Planck Inst Astrophys, D-85741 Garching, Germany.
Inst Astrophys Paris, F-75014 Paris, France.
Natl Astron Observ Japan, Tokyo 1818588, Japan.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Menard, B (reprint author), Max Planck Inst Astrophys, POB 1317, D-85741 Garching, Germany.
RI Yoshida, Naoki/A-4305-2011; Bartelmann, Matthias/A-5336-2014
NR 39
TC 34
Z9 34
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 403
IS 3
BP 817
EP 828
DI 10.1051/0004-6361:20030406
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FE
UT WOS:000183080400008
ER
PT J
AU Sasaki, M
Pietsch, W
Haberl, F
AF Sasaki, M
Pietsch, W
Haberl, F
TI XMM-Newton observations of high Mass X-ray binaries in the SMC
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE X-rays : galaxies; X-rays : binaries; stars : neutron; Magellanic Clouds
ID SMALL MAGELLANIC CLOUD; ROSAT OBSERVATIONS; SPECTRUM; CATALOG; PULSAR;
SPECTROSCOPY; HERCULES-X-1; EMISSION; SMC-X-1; LMC-X-4
AB Based on XMM-Newton EPIC data of four pointings towards the Small Magellanic Cloud (SMC), results on timing and spectral analyses of 16 known high mass X-ray binaries (HMXBs) and HMXB candidates in the SMC are presented. We confirm the pulse periods of four sources which were known to show pulsations. In addition, two new X-ray pulsars are discovered: XMMU J005605.2-722200 with P-pulse = 140.1 +/- 0.3 s and RX J0057.8-7207 with P-pulse = 152.34 +/- 0.05 s. Due to the low Galactic foreground absorption, X-ray binary systems in the Magellanic Clouds are well suited for studies of the soft component in their X-ray spectrum. Spectral analysis reveals soft emission besides a power law component in the spectra of three sources. The existence of emission lines in at least one of them corroborates the thermal nature of this emission with temperatures of 0.2-0.3 keV and heavy element abundances lower than solar. For the HMXB SMCX-2 which was in a low luminosity state, we determine a flux upper limit of 1.5 x 10(-14) erg cm(-2) s(-1) (0.3-10.0 keV). Furthermore, two new sources (XMMU J005735.7-721932 and XMMU J010030.2-722035) with hard spectrum and emission line objects as likely optical counterparts are proposed as new X-ray binary candidates.
C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM msasaki@cfa.harvard.edu
RI Sasaki, Manami/P-3045-2016
OI Sasaki, Manami/0000-0001-5302-1866
NR 53
TC 38
Z9 38
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 403
IS 3
BP 901
EP 916
DI 10.1051/0004-6361:20030420
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FE
UT WOS:000183080400015
ER
PT J
AU Haverkorn, M
Katgert, P
de Bruyn, AG
AF Haverkorn, M
Katgert, P
de Bruyn, AG
TI Multi-frequency polarimetry of the Galactic radio background around 350
MHz - I. A region in Auriga around l=161 degrees, b=16 degrees
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic
fields; ISM : structure; radio continuum : ISM
ID MAGNETIC-FIELD; ROTATION MEASURES; FARADAY-ROTATION;
LINEAR-POLARIZATION; INTERSTELLAR-MEDIUM; INNER GALAXY; SPIRAL ARMS;
SCALE; EMISSION; DENSITY
AB With the Westerbork Synthesis Radio Telescope (WSRT), multi-frequency polarimetric images were taken of the diffuse radio synchrotron background in a similar to5degrees x 7degrees region centered on (l,b) = (161degrees,16degrees) in the constellation of Auriga. The observations were done simultaneously in 5 frequency bands, from 341 MHz to 375 MHz, and have a resolution of similar to5.0' x 5.0' cosec delta. The polarized intensity P and polarization angle phi show ubiquitous structure on arcminute and degree scales, with polarized brightness temperatures up to about 13 K. On the other hand, no structure at all is observed in total intensity I to an rms limit of 1.3 K, indicating that the structure in the polarized radiation must be due to Faraday rotation and depolarization mostly in the warm component of the nearby Galactic interstellar medium ( ISM). Different depolarization processes create structure in polarized intensity P. Beam depolarization creates "depolarization canals" of one beam wide, while depth depolarization is thought to be responsible for creating most of the structure on scales larger than a beam width. Rotation measures (RM) can be reliably determined, and are in the range -17 less than or similar to RM less than or similar to 10 rad m(-2) with a non-zero average RM0 approximate to -3/4 rad m(-2). The distribution of RMs on the sky shows both abrupt changes on the scales of the beam and a gradient in the direction of positive Galactic longitude of similar to1 rad m(-2) per degree. The gradient and average RM are consistent with a regular magnetic field of similar to1 muG which has a pitch angle of p = -14degrees. There are 13 extragalactic sources in the field for which RMs could be derived, and those have \RM\ less than or similar to 13 rad m(-2), with an estimated intrinsic source contribution of similar to3.6 rad m(-2). The RMs of the extragalactic sources show a gradient that is about 3 times larger than the gradient in the RMs of the diffuse emission and that is approximately in Galactic latitude. This difference is ascribed to a vastly different effective length of the line of sight. The RMs of the extragalactic sources also show a sign reversal which implies a reversal of the magnetic field across the region on scales larger than about ten degrees. The observations are interpreted in terms of a simple single-cell-size model of the warm ISM which contains gas and magnetic fields, with a polarized background. The observations are best fitted with a cell size of 10 to 20 pc and a ratio of random to regular magnetic fields B-ran/B-reg approximate to 0.7 +/- 0.5. The polarization horizon, beyond which most diffuse polarized emission is depolarized, is estimated to be at a distance of about 600 pc.
C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands.
Univ Groningen, Kapteyn Inst, NL-9700 AV Groningen, Netherlands.
Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA.
EM mhaverkorn@cfa.harvard.edu; katgert@strw.leidenuniv.nl; ger@astron.nl
NR 60
TC 48
Z9 48
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 403
IS 3
BP 1031
EP 1044
DI 10.1051/0004-6361:20030432
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FE
UT WOS:000183080400026
ER
PT J
AU Haverkorn, M
Katgert, P
de Bruyn, AG
AF Haverkorn, M
Katgert, P
de Bruyn, AG
TI Characteristics of the structure in the Galactic polarized radio
background at 350 MHz
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE magnetic fields; polarization; techniques : polarimetric; ISM : magnetic
fields; ISM : structure; radio continuum : ISM
ID MAGNETIC-FIELD; ROTATION MEASURES; LINEAR-POLARIZATION;
INTERSTELLAR-MEDIUM; POWER SPECTRUM; INNER GALAXY; EMISSION;
SYNCHROTRON; DENSITY; SCALE
AB Angular power spectra and structure functions of the Stokes parameters Q and U and polarized intensity P are derived from three sets of radio polarimetric observations. Two of the observed fields have been studied at multiple frequencies, allowing determination of power spectra and structure functions of rotation measure RM as well. The third field extends over a large part of the northern sky, so that the variation of the power spectra over Galactic latitude and longitude can be studied. The power spectra of Q and U are steeper than those of P, probably because a foreground Faraday screen creates extra structure in Q and U, but not in P. The extra structure in Q and U occurs on large scales, and therefore causes a steeper spectrum. The derived slope of the power spectrum of P is the multipole spectral index alpha(P), and is consistent with earlier estimates. The multipole spectral index alpha(P) decreases with Galactic latitude (i.e. the spectrum becomes flatter), but is consistent with a constant value over Galactic longitude. Power spectra of the rotation measure RM show a spectral index alpha(RM) approximate to 1, while the structure function of RM is approximately flat. The structure function is flatter than earlier estimates from polarized extragalactic sources, which could be due to the fact that extragalactic source RM probes the complete line of sight through the Galaxy, whereas as a result of depolarization diffuse radio polarization only probes the nearby ISM.
C1 ASTRON, NL-7990 AA Dwingeloo, Netherlands.
Univ Groningen, Kapteyn Inst, NL-9700 AV Groningen, Netherlands.
Leiden Observ, NL-2300 RA Leiden, Netherlands.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-67, Cambridge, MA 02138 USA.
EM mhaverkorn@cfa.harvard.edu; ger@astron.nl
NR 40
TC 38
Z9 38
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 403
IS 3
BP 1045
EP 1057
DI 10.1051/0004-6361:20030464
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FE
UT WOS:000183080400027
ER
PT J
AU Kurster, M
Endl, M
Rouesnel, F
Els, S
Kaufer, A
Brillant, S
Hatzes, AP
Saar, SH
Cochran, WD
AF Kurster, M
Endl, M
Rouesnel, F
Els, S
Kaufer, A
Brillant, S
Hatzes, AP
Saar, SH
Cochran, WD
TI The low-level radial velocity variability in Barnard's star (= GJ 699) -
Secular acceleration, indications for convective redshift, and planet
mass limits
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE techniques : radial velocities; stars : kinematics; stars : planetary
systems; stars : activity
ID SURFACE CONVECTION; MAGNETIC ACTIVITY; PROXIMA CENTAURI; LINE
ASYMMETRIES; SEARCH; GRANULATION; SHIFTS; SYSTEM; ROSAT
AB We report results from 2 1/2 yr of high precision radial velocity ( RV) monitoring of Barnard's star. The high RV measurement precision of the VLT-UT2+UVES of 2.65 m s(-1) made the following findings possible. ( 1) The first detection of the change in the RV of a star caused by its space motion ( RV secular acceleration). ( 2) An anti-correlation of the measured RV with the strength of the filling-in of the H-alpha line by emission. ( 3) Very stringent mass upper limits to planetary companions. Using only data from the first 2 years, we obtain a best-fit value for the RV secular acceleration of 5.15 +/- 0.89 m s(-1) yr(-1). This agrees within 0.95sigma with the predicted value of 4.50 m s(-1) yr(-1) based on the Hipparcos proper motion and parallax combined with the known absolute radial velocity of the star. When the RV data of the last half-year are added the best-fit slope is strongly reduced to 2.97 +/- 0.51 m s(-1) yr(-1) (3.0sigma away from the predicted value), clearly suggesting the presence of additional RV variability in the star. Part of it can be attributed to stellar activity as we demonstrate by correlating the residual RVs with an index that describes the filling-in of the H-alpha line by emission. A correlation coefficient of -0.50 indicates that the appearance of active regions causes a blueshift of photospheric absorption lines. Assuming that active regions basically inhibit convection we discuss the possibility that the fundamental ( inactive) convection pattern in this M4V star produces a convective redshift which would indicate that the majority of the absorption lines relevant for our RV measurements is formed in a region of convective overshoot. This interpretation could possibly extend a trend indicated in the behaviour of earlier spectral types that exhibit convective blueshift, but with decreasing line asymmetries and blueshifts as one goes from G to K dwarfs. Based on this assumption, we estimate that the variation of the visible plage coverage is about 20%. We also determine upper limits to the projected mass m sin i and to the true mass m of hypothetical planetary companions in circular orbits. For the separation range 0.017-0.98 AU we exclude any planet with m sin i > 0.12 M-Jupiter and m > 0.86 M-Jupiter. Throughout the habitable zone around Barnard's star, i.e. 0.034-0.082 AU, we exclude planets with m sin i > 7.5 M-Earth and m > 3.1 M-Neptune.
C1 Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany.
Univ Texas, McDonald Observ, Austin, TX 78712 USA.
Univ Paris 11, F-91405 Orsay, France.
Isaac Newton Grp Telescopes, Santa Cruz De La Palma 38700, Canary Islands, Spain.
European So Observ, Santiago 19, Chile.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kurster, M (reprint author), Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany.
NR 47
TC 76
Z9 77
U1 0
U2 1
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD JUN
PY 2003
VL 403
IS 3
BP 1077
EP 1087
DI 10.1051/0004-6361:20030396
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FE
UT WOS:000183080400030
ER
PT J
AU Soker, N
David, LP
AF Soker, N
David, LP
TI Observed non-steady state cooling and the moderate cluster cooling flow
model
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cooling flows; galaxies : clusters : general; intergalactic medium;
X-rays : galaxies : clusters
ID HYDRA-A CLUSTER; CHANDRA X-RAY; FEEDBACK; GALAXIES; CORES; GAS
AB We examine recent developments in the cluster cooling flow scenario following recent observations by Chandra and XMM-Newton. We show that the distribution of gas emissivity versus temperature determined by XMM-Newton gratings observations demonstrates that the central gas, when the cooling time is less than the age of the cluster, in cooling flow clusters cannot be in simple steady state; i.e., (M)over dot is not a constant at all temperatures. On the basis of the measured gas emissivity, the gas can be in steady state only if there exists a steady heating mechanism that scales as H(T) proportional to T-alpha, where alpha = 1-2. A heating mechanism that preferentially targets the hottest and highest entropy gas seems very unlikely. Combining this result with the lack of spectroscopic evidence for gas below one-third of the ambient cluster temperature is strong evidence that the gas is heated intermittently. While the old steady state isobaric cooling flow model is incompatible with recent observations, a moderate cooling flow model in which the gas undergoes intermittent heating that effectively reduces the age of a cooling flow is consistent with observations. Most of the gas within cooling flows resides in the hottest gas, which is prevented from cooling continuously and attaining a steady state configuration. This results in a mass cooling rate that decreases with decreasing temperature, with a much lower mass cooling rate at the lowest temperatures. Such a temperature-dependent (M)over dot is required by the XMM-Newton RGS data and will produce an increasing amount of intermediate-temperature gas that will then be reheated during the next heating cycle. We show the compatibility of this model with the cooling flow cluster A2052. This paper strengthens the moderate cooling flow model, which can accommodate the unique activities observed in cooling flow clusters.
C1 Oranim, Dept Phys, IL-36006 Tivon, Israel.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Soker, N (reprint author), Oranim, Dept Phys, IL-36006 Tivon, Israel.
NR 25
TC 9
Z9 9
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2003
VL 589
IS 2
BP 770
EP 773
DI 10.1086/374815
PN 1
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 681NX
UT WOS:000183043200009
ER
PT J
AU Marengo, M
Karovska, M
Sasselov, DD
Papaliolios, C
Armstrong, JT
Nordgren, TE
AF Marengo, M
Karovska, M
Sasselov, DD
Papaliolios, C
Armstrong, JT
Nordgren, TE
TI Theoretical limb darkening for classical Cepheids. II. Corrections for
the geometric Baade-Wesselink method
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Cepheids; stars : atmospheres; stars : individual (zeta Geminorum) stars
: oscillations; techniques : interferometric
ID FUNDAMENTAL PARAMETERS; LINE; STAR
AB The geometric Baade-Wesselink method is one of the most promising techniques for obtaining a better calibration of the Cepheid period-luminosity relation by means of interferometric measurements of accurate diameters. In this paper we present new wavelength- and phase-dependent limb-darkening (LD) corrections based on our time-dependent hydrodynamic models of the classical Cepheid zeta Gem. We show that a model simulation of a Cepheid atmosphere, taking into account the hydrodynamic effects associated with the pulsation, shows strong departures from the LD otherwise predicted by a static model. For most of its pulsational cycle the hydrodynamic model predicts a larger LD than the equivalent static model. The hydrodynamics affects the LD mainly at UV and optical wavelengths. Most of these effects evolve slowly as the star pulsates, but there are phases, associated with shocks propagating into the photosphere, in which significant changes in the LD take place on timescales of the order of less than a day. We assess the implication of our model LD corrections fitting the geometric Baade-Wesselink distance of zeta Gem for the available near-IR PTI data. We discuss the effects of our model LD on the best-fit result and analyze the requirements needed to test the time dependence of the LD with future interferometric measurements.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA.
Univ Redlands, Dept Phys, Redlands, CA 92373 USA.
RP Marengo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 20
TC 28
Z9 28
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2003
VL 589
IS 2
BP 968
EP 975
DI 10.1086/374736
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 681NX
UT WOS:000183043200028
ER
PT J
AU Israel, GL
Covino, S
Perna, R
Mignani, R
Stella, L
Campana, S
Marconi, G
Bono, G
Mereghetti, S
Motch, C
Negueruela, I
Oosterbroek, T
Angelini, L
AF Israel, GL
Covino, S
Perna, R
Mignani, R
Stella, L
Campana, S
Marconi, G
Bono, G
Mereghetti, S
Motch, C
Negueruela, I
Oosterbroek, T
Angelini, L
TI The infrared counterpart to the anomalous X-ray pulsar 1RXS
J170849-400910
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared : stars; pulsars : general; pulsars : individual (1RXS
J170849-400910); stars : neutron; X-rays : stars
ID MAGNETIZED NEUTRON-STARS; FALLBACK DISKS; EXTINCTION; REPEATERS;
EMISSION; BURSTS; MODEL; MASS
AB We report the discovery of the likely IR counterpart to the anomalous X-ray pulsar (AXP) 1RXS J170849-400910 based on the Chandra High Resolution Camera (imaging detector) X-ray position and the deep optical/IR observations carried out from ESO telescopes and the Canada-France-Hawaii Telescope during 1999-2002. Within the narrow uncertainty region, we found two relatively faint (K' = 20.0 and K' = 17.53) IR objects. Based on their color and position in the J-K' versus J-H diagram, only the brighter object is consistent with the known IR properties of the counterparts to other AXPs. No variability was detected for this source, which is similar to what is observed in the case of 4U 0142+614. Like in other AXPs, we found that the IR flux of 1RXS J170849-400910 is higher than expected for a simple blackbody component extrapolated from the X-ray data. If confirmed, this object would be the fourth IR counterpart to a source of the AXP class and would make the IR excess a likely new characteristic of AXPs.
C1 Osserv Astron Roma, INAF, I-00040 Rome, Italy.
Osserv Astron Brera, INAF, I-23807 Merate, Lc, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
European So Observ, D-85748 Garching, Germany.
European So Observ, Santiago 19, Chile.
CNR, IASF, Sez Milano G Occhialini, I-20133 Milan, Italy.
Observ Strasbourg, F-67000 Strasbourg, France.
Univ Alicante, Dept Fis Ingn Sistemas & Teor Senales, E-03080 Alicante, Spain.
European Space Agcy, European Space Res & Technol Ctr, Dept Astrophys, NL-2200 AG Noordwijk, Netherlands.
NASA, High Energy Astrophys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Israel, GL (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Rome, Italy.
RI Negueruela, Ignacio/L-5483-2014;
OI Negueruela, Ignacio/0000-0003-1952-3680; MEREGHETTI,
SANDRO/0000-0003-3259-7801; Israel, GianLuca/0000-0001-5480-6438;
Covino, Stefano/0000-0001-9078-5507
NR 36
TC 44
Z9 44
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD JUN 1
PY 2003
VL 589
IS 2
BP L93
EP L96
DI 10.1086/375832
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 681NZ
UT WOS:000183043400009
ER
PT J
AU Aguilar, A
Covington, AM
Hinojosa, G
Phaneuf, RA
Alvarez, I
Cisneros, C
Bozek, JD
Dominguez, I
Sant'Anna, MM
Schlachter, AS
Nahar, SN
McLaughlin, BM
AF Aguilar, A
Covington, AM
Hinojosa, G
Phaneuf, RA
Alvarez, I
Cisneros, C
Bozek, JD
Dominguez, I
Sant'Anna, MM
Schlachter, AS
Nahar, SN
McLaughlin, BM
TI Absolute photoionization cross section measurements of O II ions from
29.7 to 46.2 eV
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE atomic data; atomic processes; methods : laboratory
ID OSCILLATOR-STRENGTHS; ATOMIC DATA; K+ IONS; ULTRAVIOLET; THRESHOLD;
OXYGEN; STATE; RECOMBINATION; NITROGEN
AB Absolute photoionization cross sections have been measured for a mixture of ground-state and metastable O II (O+) ions at photon energies ranging from 29.9 to 46.0 eV (414.7 to 269.5 Angstrom). All measurements were performed by merging an O+ beam with synchrotron radiation from an undulator beam line at the Advanced Light Source (ALS). At a resolution of 17 meV, more than 70 spectral features have been resolved, most of them identified and characterized. These measurements are compared with two independent R-matrix calculations and the data in TOPbase. All three calculations agree within 25% on the direct photoionization cross section, and with the absolute measurements within 40%. Some differences are noted in the predicted resonance positions among the three close-coupling R-matrix calculations, the TOPbase data being the least accurate. The estimated total experimental uncertainty varies from 15% to 20%. Such measurements benchmark theoretical photoionization cross section calculations performed within the framework of the Opacity Project and the Iron Project.
C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA.
Univ Nacl Autonoma Mexico, Ctr Ciencias Fis, Cuernavaca 62131, Morelos, Mexico.
Univ Calif Berkeley, Lawrence Berkeley Lab, Adv Light Source, Berkeley, CA 94720 USA.
Ohio State Univ, Dept Astron, Columbus, OH 43210 USA.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Aguilar, A (reprint author), Univ Nevada, Dept Phys, Reno, NV 89557 USA.
RI Bozek, John/E-4689-2010; Sant'Anna, Marcelo/B-9355-2013; Bozek,
John/E-9260-2010; Dominguez-Lopez, Ivan/B-6072-2016
OI Sant'Anna, Marcelo/0000-0001-5342-5799; Bozek, John/0000-0001-7486-7238;
Dominguez-Lopez, Ivan/0000-0001-8084-8711
NR 34
TC 26
Z9 26
U1 0
U2 2
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 JUN
PY 2003
VL 146
IS 2
BP 467
EP 477
DI 10.1086/368077
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680ZP
UT WOS:000183010200010
ER
PT J
AU Smith, AR
Weislo, WT
O'Donnell, S
AF Smith, AR
Weislo, WT
O'Donnell, S
TI Assured fitness returns favor sociality in a mass-provisioning sweat
bee, Megalopta genalis (Hymenoptera : Halictidae)
SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY
LA English
DT Article
DE assured fitness returns; social evolution; ant predation; brood defense
ID RUBICUNDUS HYMENOPTERA; LATITUDINAL GRADIENT; ALLODAPINE BEE; EVOLUTION;
EUSOCIALITY; SOLITARY; ABUNDANCE; INSURANCE; PREDATION; ADVANTAGE
AB Assured fitness returns models for the evolution of sociality emphasize the selective value of ensuring that offspring receive adequate parental care to reach maturity. If a member of a social group dies, it can accrue returns on investment in offspring through the efforts of surviving social partners. We provide evidence that in the mass-provisioning, facultatively social sweat bee Megalopta genalis, adult presence in the nest throughout brood development provides protection from ant predation. Nests with adults present were well protected, and brood in nests with adults removed suffered higher predation. Females in observation nests showed effective defensive behavior against experimentally introduced ants, and bees in natural nests repulsed naturally occurring ant raids. Megalopta nest architecture and behavior are such that the brood of several cooperating females can be defended with little additional cost relative to solitary nesting. The benefits of cooperative defense may favor group living in mass provisioning bees. Our observations and experiments suggest that parental care throughout brood development can be adaptive in mass provisioning species, supporting the predictions of assured fitness returns models.
C1 Smithsonian Trop Res Inst, Unit 0948, APO AA, Panama City, FL 34002 USA.
RP Smith, AR (reprint author), Univ Washington, Dept Psychol, Anim Behav Area, Seattle, WA 98195 USA.
NR 52
TC 41
Z9 41
U1 0
U2 12
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0340-5443
J9 BEHAV ECOL SOCIOBIOL
JI Behav. Ecol. Sociobiol.
PD JUN
PY 2003
VL 54
IS 1
BP 14
EP 21
DI 10.1007/s00265-003-0589-0
PG 8
WC Behavioral Sciences; Ecology; Zoology
SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology
GA 698BU
UT WOS:000183978400003
ER
PT J
AU Weiss, JV
Emerson, D
Backer, SM
Megonigal, JP
AF Weiss, JV
Emerson, D
Backer, SM
Megonigal, JP
TI Enumeration of Fe(II)-oxidizing and Fe(III)-reducing bacteria in the
root zone of wetland plants: Implications for a rhizosphere iron cycle
SO BIOGEOCHEMISTRY
LA English
DT Article
DE Fe(II)-oxidizing bacteria; Fe(III)-reducing bacteria; rhizosphere;
wetland
ID FE(III) OXIDE REDUCTION; FERRIC HYDROXIDE PLAQUE; TYPHA-LATIFOLIA L;
RICE ROOTS; OXIDIZING BACTERIA; METHANE OXIDATION; DENITRIFYING
BACTERIA; PHRAGMITES-AUSTRALIS; AQUATIC SEDIMENTS; REDUCING BACTERIA
AB Iron plaque occurs on the roots of most wetland and submersed aquatic plant species and is a large pool of oxidized Fe(III) in some environments. Because plaque formation in wetlands with circumneutral pH has been largely assumed to be an abiotic process, no systematic effort has been made to describe plaque-associated microbial communities or their role in plaque deposition. We hypothesized that Fe(II)-oxidizing bacteria (FeOB) and Fe(III)-reducing bacteria (FeRB) are abundant in the rhizosphere of wetland plants across a wide range of biogeochemical environments. In a survey of 13 wetland and aquatic habitats in the Mid-Atlantic region, FeOB were present in the rhizosphere of 92% of the plant specimens collected (n = 37), representing 25 plant species. In a subsequent study at six of these sites, bacterial abundances were determined in the rhizosphere and bulk soil using the most probable number technique. The soil had significantly more total bacteria than the roots on a dry mass basis (1.4 x 10(9) cells/g soil vs. 8.6 x 10(7) cells/g root; p < 0.05). The absolute abundance of aerobic, lithotrophic FeOB was higher in the soil than in the rhizosphere (3.7 x 10(6)/g soil vs. 5.9 x 10(5)/g root; p < 0.05), but there was no statistical difference between these habitats in terms of relative abundance (similar to1% of the total cell number). In the rhizosphere, FeRB accounted for an average of 12% of all bacterial cells while in the soil they accounted for <1% of the total bacteria. We concluded that FeOB are ubiquitous and abundant in wetland ecosystems, and that FeRB are dominant members of the rhizosphere microbial community. These observations provide a strong rationale for quantifying the contribution of FeOB to rhizosphere Fe(II) oxidation rates, and investigating the combined role of FeOB and FeRB in a rhizosphere iron cycle.
C1 George Mason Univ, Environm Sci & Policy Dept, Fairfax, VA 22030 USA.
Amer Type Culture Collect, Manassas, VA 22010 USA.
RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA.
NR 63
TC 95
Z9 109
U1 9
U2 66
PU KLUWER ACADEMIC PUBL
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD JUN
PY 2003
VL 64
IS 1
BP 77
EP 96
DI 10.1023/A:1024953027726
PG 20
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 705UJ
UT WOS:000184413200004
ER
PT J
AU Heyer, WR
AF Heyer, WR
TI Ultraviolet-B and amphibia
SO BIOSCIENCE
LA English
DT Editorial Material
C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20012 USA.
RP Heyer, WR (reprint author), Natl Museum Nat Hist, Smithsonian Inst, MRC 162,POB 37012, Washington, DC 20012 USA.
NR 4
TC 6
Z9 6
U1 0
U2 1
PU AMER INST BIOLOGICAL SCI
PI WASHINGTON
PA 1444 EYE ST, NW, STE 200, WASHINGTON, DC 20005 USA
SN 0006-3568
J9 BIOSCIENCE
JI Bioscience
PD JUN
PY 2003
VL 53
IS 6
BP 540
EP 541
DI 10.1641/0006-3568(2003)053[0540:UAA]2.0.CO;2
PG 2
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 687BA
UT WOS:000183354900002
ER
PT J
AU Elias, M
Potvin, C
AF Elias, M
Potvin, C
TI Assessing inter- and intra-specific variation in trunk carbon
concentration for 32 neotropical tree species
SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE
FORESTIERE
LA English
DT Article
ID WOOD SPECIFIC-GRAVITY; TROPICAL FORESTS; BIOMASS; STORAGE; GROWTH;
PLANTATIONS; CYCLE; SINKS
AB Trunk carbon (C) concentrations were assessed for 32 species of tropical trees to understand sources of variation. The main effect of species accounted for 38% of the total variance in C concentration (p < 0.0001). Tectona grandis demonstrated the greatest C concentration (49.4%), while Ormosia macrocalyx displayed the lowest C concentration (44.4%). We also observed significant differences among the sampling sites (F = 2.2, p < 0.02). For three of the species sampled in both plantations and natural forests, the natural forest individuals had significantly higher C concentrations (Dipteryx panamensis: F = 6.10, p = 0.06; Hura crepitans: F = 5.53, p = 0.06; and Miconia argentea: F = 8.92, p = 0.02). C concentration was highly correlated with wood specific gravity (r(2) = 0.86). A canonical correspondence analysis was performed to identify the environmental and (or) growth factors explaining variation in trunk C concentration. The two factors with the highest loading values on the first canonical axis are site and diameter at breast height (DBH), while DBH and density load on axis 2. The biplot shows that species respond differently to environmental factors. Our results suggest that a better consideration of interspecific variation in C concentration could reduce the error associated with estimates of C sequestration by up to 10%.
C1 McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada.
Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Potvin, C (reprint author), McGill Univ, Dept Biol, 1205 Ave Dr Penfield, Montreal, PQ H3A 1B1, Canada.
NR 35
TC 54
Z9 65
U1 0
U2 16
PU NATL RESEARCH COUNCIL CANADA
PI OTTAWA
PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA
SN 0045-5067
J9 CAN J FOREST RES
JI Can. J. For. Res.-Rev. Can. Rech. For.
PD JUN
PY 2003
VL 33
IS 6
BP 1039
EP 1045
DI 10.1139/X03-018
PG 7
WC Forestry
SC Forestry
GA 685JQ
UT WOS:000183259800008
ER
PT J
AU Pontailler, JY
Hymus, GJ
Drake, BG
AF Pontailler, JY
Hymus, GJ
Drake, BG
TI Estimation of leaf area index using ground-based remote sensed NDVI
measurements: validation and comparison with two indirect techniques
SO CANADIAN JOURNAL OF REMOTE SENSING
LA English
DT Article
ID VEGETATION; RED; FOREST; REFLECTANCE; INSTRUMENT
AB This study took place in an evergreen scrub oak ecosystem in Florida. Vegetation reflectance was measured in situ with a laboratory-made sensor in the red (640-665 nm) and near-infrared (750-950 nm) bands to calculate the normalized difference vegetation index (NDVI) and derive the leaf area index (LAI). LAI estimates from this technique were compared with two other nondestructive techniques, intercepted photosynthetically active radiation (PAR) and hemispherical photographs, in four contrasting 4 m(2) plots in February 2000 and two 4 m(2) plots in June 2000. We used Beer's law to derive LAI from PAR interception and gap fraction distribution to derive LAI from photographs. The plots were harvested manually after the measurements to determine a "true" LAI value and to calculate a light extinction coefficient (k). The technique based on Beer's law was affected by a large variation of the extinction coefficient, owing to the larger impact of branches in winter when LAI was low. Hemispherical photographs provided satisfactory estimates, slightly overestimated in winter because of the impact of branches or underestimated in summer because of foliage clumping. NDVI provided the best fit, showing only saturation in the densest plot (LAI = 3.5). We conclude that in situ measurement of NDVI is an accurate and simple technique to nondestructively assess LAI in experimental plots or in crops if saturation remains acceptable.
C1 Univ Paris Sud 11, CNRS, UMR 8079, Syst & Evolut ESE,Lab Ecol,Dept Ecophysiol Vegeta, F-91405 Orsay, France.
Smithsonian Environm Res Ctr, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA.
RP Pontailler, JY (reprint author), Univ Paris Sud 11, CNRS, UMR 8079, Syst & Evolut ESE,Lab Ecol,Dept Ecophysiol Vegeta, Bat 362, F-91405 Orsay, France.
NR 24
TC 22
Z9 22
U1 0
U2 9
PU CANADIAN AERONAUTICS SPACE INST
PI OTTAWA
PA 1685 RUSSELL RD, UNIT 1-R, OTTAWA, ON K1G 0N1, CANADA
SN 0703-8992
J9 CAN J REMOTE SENS
JI Can. J. Remote Sens.
PD JUN
PY 2003
VL 29
IS 3
BP 381
EP 387
PG 7
WC Remote Sensing
SC Remote Sensing
GA 686YZ
UT WOS:000183349700009
ER
PT J
AU Lidgard, DC
Boness, DJ
Bowen, WD
McMillan, JI
AF Lidgard, DC
Boness, DJ
Bowen, WD
McMillan, JI
TI Diving behaviour during the breeding season in the terrestrially
breeding male grey seal: implications for alternative mating tactics
SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE
LA English
DT Article
ID LAND-FAST ICE; HALICHOERUS-GRYPUS; GRAY SEALS; REPRODUCTIVE-BEHAVIOR;
HARBOR SEAL; FORAGING BEHAVIOR; PHOCA-VITULINA; SABLE ISLAND; NORTH
RONA; SUCCESS
AB We examined the diving behaviour of breeding male grey seals (Halichoerus grypus) at Sable Island, Nova Scotia, from 1997 to 2001. The proportion of time spent at sea varied between 0 and 78% (N=30). Males engaged in deep (43.4+/-3.3 m (mean+/-SE), N=27) diving, and these dives were clustered into bouts, which mostly occurred during long trips (62.2+/-14.7 h). We suggest that males spent time foraging during deep dives. Shallow diving (5.9+/-0.1 m, N=27) accounted for 40.8% of dives, which were also clustered into bouts that mostly occurred during short trips (2.1+/-0.37 h). We suggest that shallow diving comprised a suite of behaviours, but included little foraging behaviour. Phenotypic traits had little influence on diving behaviour. Further work is required to understand the extent to which foraging behaviour enhances reproductive success, and whether shallow diving is a component of the mating tactics of male grey seals at Sable Island.
C1 Univ La Rochelle, Lab Biol & Environm Marins, F-17000 La Rochelle, France.
Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Washington, DC 20008 USA.
Fisheries & Oceans Canada, Bedford Inst Oceanog, Marine Fish Div, Dartmouth, NS B2Y 4A2, Canada.
RP Lidgard, DC (reprint author), Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA.
RI Bowen, William/D-2758-2012
NR 45
TC 5
Z9 5
U1 3
U2 10
PU NATL RESEARCH COUNCIL CANADA
PI OTTAWA
PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA
SN 0008-4301
J9 CAN J ZOOL
JI Can. J. Zool.-Rev. Can. Zool.
PD JUN
PY 2003
VL 81
IS 6
BP 1025
EP 1033
DI 10.1139/Z03-085
PG 9
WC Zoology
SC Zoology
GA 711AG
UT WOS:000184714500010
ER
PT J
AU Mawdsley, JR
AF Mawdsley, JR
TI The importance of species of Dasytinae (Coleoptera : Melyridae) as
pollinators in western North America
SO COLEOPTERISTS BULLETIN
LA English
DT Article
ID BEETLE POLLINATION; FRENCH-GUIANA; SCARABAEIDAE; MALAYSIA; SARAWAK;
FLOWERS; ARACEAE; AFRICA
AB Species of 11 families of Coleoptera are known to pollinate flowering plants. In western North America, the 300+ species of the beetle subfamily Dasytinae (Coleoptera: Melyridae) are commonly found on flowers, where adults feed on both nectar and pollen. The dense setae and pubescence of adult dasytines often trap pollen grains, which are transported to other flowers during the course of normal adult feeding. Adults of many dasytine species are abundant, and may form large feeding aggregations. A preliminary list is presented of plant species on whose flowers or pollen cones adult dasytines have been collected, based on literature records and museum specimen labels. These plant species represent 68 genera in 26 families, and include species grown as food crops and species that are important browse or forage plants for livestock and wildlife. At least two plant species, both in the family Polemoniaceae, rely predominantly on species of Dasytinae for pollination.
C1 Smithsonian Inst, Sect Entomol, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Mawdsley, JR (reprint author), Smithsonian Inst, Sect Entomol, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
NR 31
TC 7
Z9 10
U1 1
U2 9
PU COLEOPTERISTS SOC
PI NATCHEZ
PA PO BOX 767, NATCHEZ, MS 39121 USA
SN 0010-065X
J9 COLEOPTS BULL
JI Coleopt. Bull.
PD JUN
PY 2003
VL 57
IS 2
BP 154
EP 160
DI 10.1649/541
PG 7
WC Entomology
SC Entomology
GA 693UL
UT WOS:000183736700010
ER
PT J
AU Petit, LJ
Petit, DR
AF Petit, LJ
Petit, DR
TI Evaluating the importance of human-modified lands for neotropical bird
conservation
SO CONSERVATION BIOLOGY
LA English
DT Article
ID SHADE COFFEE; BIODIVERSITY; COMMUNITIES; CHIAPAS; FOREST; PANAMA; MEXICO
AB Development of effective conservation plans for terrestrial animals will require some assessment of which human-modified and natural habitats can support populations of priority species. We examined bird communities associated with 11 natural and human-modified habitats in Panama and assessed the importance of those habitats for species of different vulnerability to disturbance. We calculated habitat importance scores using both relative habitat preferences and vulnerability scores for all species present. Species of moderate and high vulnerability were primarily those categorized as forest specialists or forest generalists. As expected, even species-rich nonforest habitats provided little conservation value for the most vulnerable species. However, shaded coffee plantations and gallery forest corridors were modified habitats with relatively high conservation value. Sugar cane fields and Caribbean pine plantations offered virtually no conservation value for birds. Our method of assessing the conservation importance of different habitats is useful because it considers the types of species present and the potential role of the habitat in the conservation of those species (i.e., habitat preference). This method of habitat evaluation could be tailored to other conservation contexts with any measure of species vulnerability desired.
C1 Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA.
US Geol Survey, Biol Resources Div, Reston, VA 20192 USA.
RP Petit, LJ (reprint author), Cuyahoga Valley Natl Pk, Natl Pk Serv, 15610 Vaughn Rd, Brecksville, OH 44141 USA.
NR 35
TC 74
Z9 79
U1 2
U2 34
PU BLACKWELL PUBLISHING INC
PI MALDEN
PA 350 MAIN ST, MALDEN, MA 02148 USA
SN 0888-8892
J9 CONSERV BIOL
JI Conserv. Biol.
PD JUN
PY 2003
VL 17
IS 3
BP 687
EP 694
DI 10.1046/j.1523-1739.2003.00124.x
PG 8
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 682EF
UT WOS:000183077800012
ER
PT J
AU Kuchner, MJ
AF Kuchner, MJ
TI Planetary perturbers in debris disks
SO EARTH MOON AND PLANETS
LA English
DT Article
ID EDGEWORTH-KUIPER BELT; CIRCUMSTELLAR DUST DISK; SOLAR-SYSTEM DUST;
BETA-PICTORIS; GIANT PLANETS; RING; SIGNATURES; RESONANCE; JUPITER;
PERTURBATIONS
AB Neptune dominates the dynamics of the Kuiper Belt. By examining images of debris disks around other stars, we may be able to infer what kinds of planets shape the outer edges of other planetary systems. The last few years have seen a burst of progress in the modeling of azimuthal structures in debris disks created by planetary perturbers; new models incorporate planets on substantially eccentric orbits. I review this recent progress in debris disk dynamics and discuss the Kuiper Belt as a key example.
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Kuchner, MJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RI Kuchner, Marc/E-2288-2012
NR 47
TC 1
Z9 1
U1 1
U2 3
PU KLUWER ACADEMIC PUBL
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0167-9295
J9 EARTH MOON PLANETS
JI Earth Moon Planets
PD JUN
PY 2003
VL 92
IS 1-4
BP 435
EP 445
DI 10.1023/B:MOON.0000031957.71828.d3
PG 11
WC Astronomy & Astrophysics; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Geology
GA 829OD
UT WOS:000222057600037
ER
PT J
AU Zhu, RX
An, ZS
Potts, R
Hoffman, KA
AF Zhu, RX
An, ZS
Potts, R
Hoffman, KA
TI Magnetostratigraphic dating of early humans in China
SO EARTH-SCIENCE REVIEWS
LA English
DT Article
DE magnetic stratigraphy; China; human fossil remains; stone artifacts;
early Pleistocene; paleolithic
ID PALEOMAGNETIC DATES; EARLY HOMO; HOMINID; AGE; DMANISI; GEORGIA; BASIN;
SITES; ASIA; INDONESIA
AB China is a key area for research into human occupation in the Old World after the initial expansion of early humans out of Africa. Reliable age determinations are pivotal for assessing the patterns of human evolution and dispersal in this region. This paper reviews magnetostratigraphic studies of some early Pleistocene strata bearing hominin remains and/or artifact stone tools from northern to southern China. The quality and reliability of the paleomagnetic dates are also evaluated. New magnetostratigraphic results for the Xihoudu Paleolithic site in north-central China are also presented.
Among the few hominin or Paleolithic sites in China from the early Pleistocene, five have been well investigated. Three of these are in northern China at Xiaochangliang, Donggutuo and Gongwangling; the remaining two in southern China at Longgupo and Yuanmou. Considerable progress has been made during the past three decades towards paleomagnetically dating these sites. Indeed, the age estimates at Xiaochangliang and Gongwangling have been widely accepted. Magnetostratigraphic consensus about the age of the Donggutuo site has also been reached. However, the age determination for the two sites in southern China is still contested.
The integration of rock-magnetic stratigraphy with magnetic polarity stratigraphy has resulted in a determined age of 1.36 Ma for a stone tool-containing layer of lacustrine sediments at the Xiaochangliang site in the Nihewan Basin. Lithostratigraphic constraints have significantly contributed to determining the age of Lantian Homo erectus at Gongwangling, which occurred in a loess-paleosol sequence of the southern Loess Plateau. Its age, paleomagnetically derived, is about 1.15 Ma. These two paleomagnetic ages suggest an expansion and flourishing of human groups from northern to north-central China during the early Pleistocene. This suggestion has been reinforced by our new magnetostratigraphic age estimate of about 1.27 Ma for the Xihoudu site as will be presented in this paper. However, more work is needed for the age determinations of the hominin-bearing strata at the Longgupo and Yuanmou sites in southern China. Finally, we stress that it is necessary to combine biostratigraphy, lithostratigraphy and rock-magnetic stratigraphy with the traditional magnetic polarity stratigraphy in order to obtain reliable age determinations for strata bearing hominin remains or stone artifacts. (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Chinese Acad Sci, Inst Geol & Geophys, Paleomagnetism Lab, Beijing 100029, Peoples R China.
Chinese Acad Sci, Inst Earth Environm, Xian 710054, Peoples R China.
Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA.
California Polytech STate Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93410 USA.
RP Zhu, RX (reprint author), Chinese Acad Sci, Inst Geol & Geophys, Paleomagnetism Lab, POB 9825, Beijing 100029, Peoples R China.
RI AN, Zhisheng/F-8834-2012
NR 80
TC 91
Z9 125
U1 5
U2 25
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0012-8252
J9 EARTH-SCI REV
JI Earth-Sci. Rev.
PD JUN
PY 2003
VL 61
IS 3-4
BP 341
EP 359
DI 10.1016/S0012-8252(02)00132-0
PG 19
WC Geosciences, Multidisciplinary
SC Geology
GA 687UB
UT WOS:000183394400004
ER
PT J
AU Rappole, JH
King, DI
Diez, J
AF Rappole, JH
King, DI
Diez, J
TI Winter- vs. breeding-habitat limitation for an endangered avian migrant
SO ECOLOGICAL APPLICATIONS
LA English
DT Article
DE avian migrant; breeding habitat; Dendroica chrysoparia; endangered
species; Golden-cheeked Warbler; habitat limitation; population
limitation; remote sensing; winter habitat
ID WARBLERS; BIRDS
AB Migratory species have critical habitat needs during both breeding and wintering portions of the life cycle. Recent advances have made it possible to use satellite imagery and computer-assisted spatial analysis technology along with fieldwork to determine estimates for these critical habitat needs for the endangered Golden-cheeked Warbler, Dendroica chrysoparia. Using these procedures, we estimate that the Ashe juniper-oak breeding habitat for this species covers 6430 km(2) of central Texas, USA, whereas appropriate habitat in the known winter range covers 6750 km(2) of the Middle American cordillera. When combined with information on warbler breeding and wintering ecology, these figures indicate that the amount of available winter habitat (pine-oak above 1219 m [4000'] in elevation) supports only a fraction (15%) of the population that could be supported by the amount of estimated available breeding habitat, suggesting that Golden-cheeked Warbler populations could be limited by winter habitat availability.
C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA.
Univ Massachusetts, Holdsworth Nat Resources Ctr 203, US Forest Serv, NE Expt Stn, Amherst, MA 01003 USA.
Univ Georgia, Inst Ecol, Athens, GA 30602 USA.
RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA.
NR 26
TC 30
Z9 33
U1 0
U2 17
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA
SN 1051-0761
J9 ECOL APPL
JI Ecol. Appl.
PD JUN
PY 2003
VL 13
IS 3
BP 735
EP 742
DI 10.1890/1051-0761(2003)013[0735:WVBLFA]2.0.CO;2
PG 8
WC Ecology; Environmental Sciences
SC Environmental Sciences & Ecology
GA 707TA
UT WOS:000184524900013
ER
PT J
AU Liu, AZ
Kress, WJ
Long, CL
AF Liu, AZ
Kress, WJ
Long, CL
TI The ethnobotany of Musella lasiocarpa (Musaceae), an endemic plant of
southwest China.
SO ECONOMIC BOTANY
LA English
DT Article
C1 Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Peoples R China.
Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, MRC 166, Washington, DC 20013 USA.
RP Liu, AZ (reprint author), Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Peoples R China.
RI Liu, aizhong/F-1770-2010;
OI Long, Chunlin/0000-0002-6573-6049
NR 10
TC 8
Z9 11
U1 0
U2 3
PU NEW YORK BOTANICAL GARDEN
PI BRONX
PA PUBLICATIONS DEPT, BRONX, NY 10458 USA
SN 0013-0001
J9 ECON BOT
JI Econ. Bot.
PD SUM
PY 2003
VL 57
IS 2
BP 279
EP 281
DI 10.1663/0013-0001(2003)057[0279:TEOMLM]2.0.CO;2
PG 3
WC Plant Sciences
SC Plant Sciences
GA 710EA
UT WOS:000184666800010
ER
PT J
AU King, RS
Richardson, CJ
AF King, RS
Richardson, CJ
TI Integrating bioassessment and ecological risk assessment: An approach to
developing numerical water-quality criteria
SO ENVIRONMENTAL MANAGEMENT
LA English
DT Article
DE biological assessment; ecological thresholds; everglades; Index of
Biological integrity; macroinvertebrates; nutrients; phosphorus; risk
assessment; wetlands
ID BIOTIC INTEGRITY; STREAMS; EVERGLADES; LIMITATION; ENRICHMENT;
PERIPHYTON; COMMUNITY; NUTRIENTS; GRADIENT; WETLANDS
AB ioassessment is used worldwide to monitor aquatic health but is infrequently used with risk-assessment objectives, such as supporting the development of defensible, numerical water-quality criteria, To this end, we present a generalized approach for detecting potential ecological thresholds using assemblage-level attributes and a multimetric index (Index of Biological Integrity-IBI) as endpoints in response to numerical changes in water quality. To illustrate the approach, we used existing macroinvertebrate and surface-water total phosphorus (TP) datasets from an observed P gradient and a P-dosing experiment in wetlands of the south Florida coastal plain nutrient ecoregion. Ten assemblage attributes were identified as potential metrics using the observational data, and five were validated in the experiment. These five core metrics were subjected individually and as an aggregated Nutrient-IBI to nonparametric changepoint analysis (nCPA) to estimate cumulative probabilities of a threshold response to TP. Threshold responses were evident for all metrics and the IBI, and were repeatable through time. Results from the observed gradient indicated that a threshold was greater than or equal to50% probable between 12.6 and 19.4 mug/L TP for individual metrics and 14.8 mug/L TP for the IBI. Results from the P-dosing experiment revealed greater than or equal to50% probability of a response between 11.2 and 13.0 mug/L TP for the metrics and 12.3 mug/L TIP for the IBI. Uncertainty analysis indicated a low (typically greater than or equal to5%) probability that an IBI threshold occurred at less than or equal to 10 mug/L TP, while there was greater than or equal to95% certainty that the threshold was less than or equal to 17 mug/L TP. The weight-of-evidence produced from these analyses implies that a TP concentration > 12-15 mug/L is likely to cause degradation of macroinvertebrate assemblage structure and function, a reflection of biological integrity, in the study area. This finding may assist in the development of a numerical water-quality criterion for TP in this ecoregion, and illustrates the utility of bioassessment to environmental decision-making.
C1 Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA.
RP King, RS (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,Box 28, Edgewater, MD 21037 USA.
NR 62
TC 74
Z9 80
U1 6
U2 42
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0364-152X
J9 ENVIRON MANAGE
JI Environ. Manage.
PD JUN
PY 2003
VL 31
IS 6
BP 795
EP 809
DI 10.1007/s00267-002-0036-4
PG 15
WC Environmental Sciences
SC Environmental Sciences & Ecology
GA 711AK
UT WOS:000184714800010
PM 14565699
ER
PT J
AU Castro, MS
Driscoll, CT
Jordan, TE
Reay, WG
Boynton, WR
AF Castro, MS
Driscoll, CT
Jordan, TE
Reay, WG
Boynton, WR
TI Sources of nitrogen to estuaries in the United States
SO ESTUARIES
LA English
DT Article
ID COASTAL EUTROPHICATION; CHESAPEAKE BAY; ATMOSPHERIC DEPOSITION;
NUTRIENTS; DENITRIFICATION; GROUNDWATER; TEMPERATURE; TRANSPORT;
BUDGETS; BLOOMS
AB The purpose of this study was to quantify the nitrogen (N) inputs to 34 estuaries on the Atlantic and Gulf Coasts of the United States. Total nitrogen (TN) inputs ranged from 1 kg N ha(-1) yr(-1) for Upper Laguna Madre, Texas, to 49 kg N ha(-1) yr(-1) for Massachusetts Bay, Massachusetts. TN inputs to 11 of the 34 estuaries were dominated by urban N sources (point sources and septic systems) and nonpoint source N runoff (5% of total); point sources accounted for 36-86% of the TN inputs to these 11 urban-dominated estuaries. TN inputs to 20 of the 34 estuaries were dominated by agricultural N sources; N fertilization was the dominant source (46% of the total), followed by manure (32% of the total) and N fixation by crops (16% of the total). Atmospheric deposition (runoff from watershed plus direct deposition to the surface of the estuary) was the dominant N source for three estuaries (Barnegat Bay, New Jersey: 64%; St. Catherines-Sapelo, Georgia: 72%; and Barataria Bay, Louisiana: 53%). Six estuaries had atmospheric contributions 30% of the TN inputs (Casco Bay, Maine: 43%; Buzzards Bay, Massachusetts: 30%; Great Bay, New Jersey: 40%; Chesapeake Bay: 30%; Terrebonne-Timbalier Bay, Louisiana: 59%; and Upper Laguna Madre: 41%). Results from our study suggest that reductions in N loadings to estuaries should be accomplished by implementing watershed specific programs that target the dominant N sources.
C1 Appalachian Lab, Frostburg, MD 21532 USA.
Syracuse Univ, Dept Civil & Environm Engn, Syracuse, NY 13244 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA.
RP Castro, MS (reprint author), Appalachian Lab, 301 Braddock Rd, Frostburg, MD 21532 USA.
RI Boynton, Walter/C-3035-2012; Driscoll, Charles/F-9832-2014; Castro,
Mark/J-6529-2015;
OI Castro, Mark/0000-0002-4279-8204; Driscoll, Charles/0000-0003-2692-2890
NR 24
TC 54
Z9 55
U1 5
U2 39
PU ESTUARINE RES FEDERATION
PI LAWRENCE
PA PO BOX 368, LAWRENCE, KS 66044 USA
SN 0160-8347
J9 ESTUARIES
JI Estuaries
PD JUN
PY 2003
VL 26
IS 3
BP 803
EP 814
DI 10.1007/BF02711991
PG 12
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 712NN
UT WOS:000184803900017
ER
PT J
AU Weems, HV
Thompson, FC
Rotheray, G
Deyrup, MA
AF Weems, HV
Thompson, FC
Rotheray, G
Deyrup, MA
TI The genus Rhopalosyrphus (Diptera : Syrphidae)
SO FLORIDA ENTOMOLOGIST
LA English
DT Article
DE taxonomy; identification key; neotropics; nearctic
AB The flower fly genus Rhopalosyrphus Giglio-Tos (Diptera: Syrphidae) is revised. The genus is redescribed; a key to species is presented; the phylogenetic relationships of the genus and species are hypothesized; the included species are described; with new species, R. ramulorum Weems & Deyrup, described from Florida (type) and Mexico; R. australis Thompson from Brazil and Paraguay (type); and the critical characters are illustrated.
C1 USDA, Systemat Entomol Lab, Smithsonian Inst NHB168, Washington, DC 20560 USA.
Royal Museum Scotland, Dept Nat Hist, Edinburgh EH1 1JF, Midlothian, Scotland.
Archbold Biol Stn, Lake Placid, FL 33862 USA.
RP Weems, HV (reprint author), USDA, Systemat Entomol Lab, Smithsonian Inst NHB168, Washington, DC 20560 USA.
NR 27
TC 4
Z9 4
U1 0
U2 0
PU FLORIDA ENTOMOLOGICAL SOC
PI LUTZ
PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA
SN 0015-4040
J9 FLA ENTOMOL
JI Fla. Entomol.
PD JUN
PY 2003
VL 86
IS 2
BP 186
EP 193
DI 10.1653/0015-4040(2003)086[0186:TGRDS]2.0.CO;2
PG 8
WC Entomology
SC Entomology
GA 697ZJ
UT WOS:000183972900013
ER
PT J
AU Pearson, TRH
Burslem, DFRP
Mullins, CE
Dalling, JW
AF Pearson, TRH
Burslem, DFRP
Mullins, CE
Dalling, JW
TI Functional significance of photoblastic germination in neotropical
pioneer trees: a seed's eye view
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE Gap size; litter; r : fr; seed size; tropical forest
ID TROPICAL RAIN-FOREST; ECOLOGICAL SIGNIFICANCE; PIPER-AURITUM; LIGHT;
SOIL; PENETRATION; PHYTOCHROME; LITTER; PERCEPTION; DYNAMICS
AB 1. We investigated the relationship between seed mass and the suitability of microsites for germination for five small-seeded (<2.4 mg fresh mass) photoblastic neotropical pioneer trees. We determined the germination response of these species to the ratio of red to far-red irradiance (r:fr) and compared it to r:fr measured under varying conditions of canopy openness, litter and soil thickness.
2. At a constant temperature the germination percentage of each of the species increased sharply with increasing r:fr above a species-specific threshold r:fr. The smallest-seeded species, Miconia argentea , had the lowest r:fr threshold for germination (0.12) while the larger-seeded Cecropia species and Solanum hayesii possessed higher values (0.21-0.27). The largest seeded species, Solanum hayesii , also showed a positive germination response to a 10degreesC temperature fluctuation, which was independent of the response to r:fr.
3. The mean r:fr at ground level declined with decreasing gap size but not sufficiently to suppress the germination of these five species. However, a covering of one litter leaf in direct sunlight reduced the r:fr to between 0.18 and 0.83 depending on the species and leaf wetness. The top-soil at our study site was aggregated and irradiance was transmitted or reflected between soil aggregates with little change in r:fr. Light did not penetrate the aggregates.
4. We suggest that photoblastic germination in neotropical pioneers has evolved to inhibit germination in response to conditions most likely to alter within the life of an individual seed (i.e. superficial burial by leaf litter or incorporation into the surface soil), rather than to fine scale variation in canopy openness. Among photoblastic species, the pattern of response to r:fr suggests that smaller-seeded species would germinate in a broader range of microsites than larger-seeded species. This lower degree of discrimination may be associated with their higher risk of mortality and therefore more limited persistence in the soil seed bank.
C1 Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland.
Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.
Smithsonian Trop Res Inst, UNIT 0948, APO, AA 34002 USA.
RP Pearson, TRH (reprint author), Univ Aberdeen, Sch Biol Sci, Cruickshank Bldg,St Machar Dr, Aberdeen AB24 3UU, Scotland.
OI Burslem, David/0000-0001-6033-0990
NR 33
TC 49
Z9 63
U1 1
U2 22
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0269-8463
J9 FUNCT ECOL
JI Funct. Ecol.
PD JUN
PY 2003
VL 17
IS 3
BP 394
EP 402
DI 10.1046/j.1365-2435.2003.00747.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 687FA
UT WOS:000183364400013
ER
PT J
AU Ferrari, FD
Fornshell, JA
Ong, L
Ambler, JW
AF Ferrari, FD
Fornshell, JA
Ong, L
Ambler, JW
TI Diel distribution of copepods across a channel of an overwash mangrove
island
SO HYDROBIOLOGIA
LA English
DT Article
DE planktonic copepods; swarms; age structure; diel changes
ID DIOITHONA-OCULATA; ZOOPLANKTON
AB The distribution of copepod species and their nauplii was studied in a narrow, blind channel on an overwash mangrove island offshore of Belize. Copepodids were sampled with a pump at five stations across the channel during a diel cycle. Diel changes of copepodid stages II - VI were marked by horizontal dispersal of Dioithona oculata, the dominant species, from swarms in the prop roots along the shore during the day to the edge of the prop root habitat at night. Migration of copepodids back to the prop roots appeared to be controlled endogenously because change from a night to a daytime age structure began before first light. Mean copepodid stage at subsurface depths in the channel and prop root edge decreased from 4.2 ( with 6.0 = all adults) to 2.9 at predawn to 1.1 during day. The oceanic Oithona nana and O. simplex, and the coastal zone O. fonsecae were evenly distributed with depth and distance from shore during day and night, with avoidance of prop root shoreline during day. These species were much less abundant than Dioithona oculata in the prop roots, but of comparable or greater abundance in the channel. Coastal zone Acartia spinata exhibited evidence of swarming. Nauplii, sampled with a 25 mum plankton net, were dominated by harpacticoid (50%) and cyclopoid (34%) nauplii, which generally were more abundant at 1m than at the surface and more abundant at night than the day. Lagrangian current measurements indicated velocities at ebb tide twice those of flood tide (1.9 vs. 0.8 cm s(-1)) and a minimal residence time of 5 days, which could result in advection of D. oculata nauplii out of the Lair Channel before their recruitment into swarms as copepodid stage II. Previously reported maximum swimming speeds of swarming D. oculata copepodid stages (2.0 cm s(-1)) and greater densities in prop roots and near the benthos may help copepodids avoid advection. The swarming behavior and diel horizontal migration ( or dispersal) reported for D. oculata appears analogous to that of limnetic zooplankton, which may swarm among macrophytes along shorelines during the day to avoid visual predators and disperse or migrate away from the shoreline at night.
C1 Smithsonian Inst, Dept Invertebrate Zool, MSC, Washington, DC 20013 USA.
Millersville Univ Pennsylvania, Dept Biol, Millersville, PA 17551 USA.
RP Ferrari, FD (reprint author), Smithsonian Inst, Dept Invertebrate Zool, MSC, POB 37012,MRC 534, Washington, DC 20013 USA.
NR 24
TC 2
Z9 3
U1 1
U2 1
PU SPRINGER
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0018-8158
EI 1573-5117
J9 HYDROBIOLOGIA
JI Hydrobiologia
PD JUN
PY 2003
VL 499
IS 1-3
BP 147
EP 159
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 737LY
UT WOS:000186235100011
ER
PT J
AU Tong, CYE
Meledin, DV
Marrone, DP
Paine, SN
Gibson, H
Blundell, R
AF Tong, CYE
Meledin, DV
Marrone, DP
Paine, SN
Gibson, H
Blundell, R
TI Near field vector beam measurements at 1 THz
SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS
LA English
DT Article
DE antenna pattern; Gaussian beam; submillimeter wave; vector measurements
AB We have performed near-field vector beam measurements at 1.03 THz to characterize and align the receiver optics of a superconducting receiver. The signal source is a harmonic generator mounted on an X-Y translation stage. We model the measured two-dimensional complex beam pattern by a fundamental. Gaussian mode, from which we derive the position of the beam center, the beam radius and the direction of propagation. By performing scans in the planes separated by 400 mm, we have confirmed that our beam pattern measurements are highly reliable.
RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Tong, Edward/0000-0002-7736-4203
NR 6
TC 11
Z9 11
U1 0
U2 2
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1531-1309
J9 IEEE MICROW WIREL CO
JI IEEE Microw. Wirel. Compon. Lett.
PD JUN
PY 2003
VL 13
IS 6
BP 235
EP 237
DI 10.1109/LMWC.2003.814602
PG 3
WC Engineering, Electrical & Electronic
SC Engineering
GA 697KH
UT WOS:000183941400015
ER
PT J
AU Meledin, D
Tong, CYE
Blundell, R
Kaurova, N
Smirnov, K
Voronov, B
Goltsman, G
AF Meledin, D
Tong, CYE
Blundell, R
Kaurova, N
Smirnov, K
Voronov, B
Goltsman, G
TI Study of the IF bandwidth of NbNHEB mixers based on crystalline quartz
substrate with an MgO buffer layer
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article; Proceedings Paper
CT Applied Superconductivity Conference
CY AUG 04-09, 2002
CL HOUSTON, TEXAS
SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang
DE electron temperature; hot-electron bolometer; self-heating parameter
ID ELECTRON BOLOMETER MIXER
AB In this paper, we present the results of IF bandwidth measurements on 3-4 mn thick NbN hot electron bolometer waveguide mixers, which have been fabricated on a 200-nm thick MgO buffer layer deposited on a crystalline quartz substrate. The 3-dB IF bandwidth, measured at an LO frequency of 0.81 THz, is 3.7 GHz at the optimal bias point for low noise receiver operation. We have-also made measurements of the IF dynamic impedance, which allow us to evaluate the intrinsic electron temperature relaxation time and self-heating parameters at different bias conditions.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Moscow State Pedag Univ, Moscow 119435, Russia.
RP Meledin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Tong, Edward/0000-0002-7736-4203
NR 15
TC 20
Z9 20
U1 0
U2 4
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1051-8223
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2003
VL 13
IS 2
BP 164
EP 167
DI 10.1109/TASC.2003.813671
PN 1
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 702UB
UT WOS:000184241700022
ER
PT J
AU Maezawa, H
Tong, CYE
Noguchi, T
Matsunaga, T
Blundell, R
Pan, SK
AF Maezawa, H
Tong, CYE
Noguchi, T
Matsunaga, T
Blundell, R
Pan, SK
TI An Nb-based waveguide SIS distributed mixer employing coplanar inductor
loaded microstrip transformer for the 800 GHz frequency band
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article; Proceedings Paper
CT Applied Superconductivity Conference
CY AUG 04-09, 2002
CL HOUSTON, TEXAS
SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang
ID RECEIVER; LINE
AB We present a novel superconducting waveguide mixer for 800 GHz. In this mixer, a half-wave Nb/Al-AlOx/Nb superconducting-insulator-superconductor (SIS) resonator is integrated with a microstrip superconducting transmission line loaded with coplanar inductors. This hybrid coplanar/microstrip transmission line acts as an impedance matching section between the distributed junction and the waveguide feed point of the mixer mount. We have designed mixers with a simple model which predicts that the insertion loss of the matching network is less than 10 percent up to 840 GHz. Preliminary experimental results show that the resonator can work up to 800 GHz but the parameters of the coplanar inductor loaded microstrip line need to be refined to improve power coupling to the resonator.
C1 Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
RP Maezawa, H (reprint author), Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan.
OI Tong, Edward/0000-0002-7736-4203
NR 11
TC 0
Z9 0
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1051-8223
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2003
VL 13
IS 2
BP 668
EP 671
DI 10.1109/TASC.2003.813991
PN 1
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 702UB
UT WOS:000184241700146
ER
PT J
AU Tong, CYE
Blundell, R
Megerian, KG
Stern, JA
LeDuc, HG
AF Tong, CYE
Blundell, R
Megerian, KG
Stern, JA
LeDuc, HG
TI A 650 GHz fixed-tuned waveguide SIS distributed mixer with no integrated
tuning circuit
SO IEEE TRANSACTIONS ON APPLIED SUPERCONDUCTIVITY
LA English
DT Article; Proceedings Paper
CT Applied Superconductivity Conference
CY AUG 04-09, 2002
CL HOUSTON, TEXAS
SP Apple, Argonne Natl Lab, Florida State Univ, Ctr Adv Power Syst, Cingular Wireless, Council SuperCond Amer Competit, Hewlett Packard Co, Houston Adv Res Ctr, IEEE CSC Council Supercond, IISSC, Marimon, Naval Res Lab, Oak Ridge Natl Lab, Univ Houston, Texas Ctr Supercond & Adv Mat, US DOE, Div High Energy Phys, Univ Houston, Cullen Coll Engn, Univ Houston, Coll Nat Sci & Math, Univ Houston, Div Res, Wah Chang
DE distributed mixing; integrated tuning network; resonant mixer; SIS
devices
ID LINE
AB A Superconductor-Insulator-Superconductor (SIS) distributed mixer with no integrated tuning circuit has been designed for use in a fixed-tuned waveguide mixer block. This mixer employs two half-wave SIS resonators connected in series across the feed point of the waveguide circuit. By selecting appropriate dimensions for the resonators, we can obtain proper impedance matching over a reasonable input bandwidth. Since there is no lossy thin film microstrip line in front of the SIS junction, efficient power transfer from the waveguide feed to the mixer element can be achieved. A receiver noise temperature of 185 K at 650 GHz has been measured with a dual 0.33 x 16.8 mum SIS resonator. The noise temperature remains below 300 K over an input bandwidth of about 10%. This design can be used at much higher frequency where the loss of tuning circuit becomes significant.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA.
RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Tong, Edward/0000-0002-7736-4203
NR 6
TC 5
Z9 5
U1 0
U2 1
PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC
PI PISCATAWAY
PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA
SN 1051-8223
J9 IEEE T APPL SUPERCON
JI IEEE Trans. Appl. Supercond.
PD JUN
PY 2003
VL 13
IS 2
BP 680
EP 683
DI 10.1109/TASC.2003.813996
PN 1
PG 4
WC Engineering, Electrical & Electronic; Physics, Applied
SC Engineering; Physics
GA 702UB
UT WOS:000184241700149
ER
PT J
AU McGovern, CF
AF McGovern, CF
TI The politics of consumption: Material culture and citizenship in Europe
and America.
SO JOURNAL OF INTERDISCIPLINARY HISTORY
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP McGovern, CF (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 3
TC 0
Z9 0
U1 0
U2 1
PU M I T PRESS
PI CAMBRIDGE
PA FIVE CAMBRIDGE CENTER, CAMBRIDGE, MA 02142 USA
SN 0022-1953
J9 J INTERDISCIPL HIST
JI J. Interdiscip. Hist.
PD SUM
PY 2003
VL 34
IS 1
BP 69
EP 71
DI 10.1162/002219503322645510
PG 4
WC History
SC History
GA 756FU
UT WOS:000187455800009
ER
PT J
AU Hussein, AA
Bozzi, B
Correa, M
Capson, TL
Kursar, TA
Coley, PD
Solis, PN
Gupta, MP
AF Hussein, AA
Bozzi, B
Correa, M
Capson, TL
Kursar, TA
Coley, PD
Solis, PN
Gupta, MP
TI Bioactive constituents from three Vismia species
SO JOURNAL OF NATURAL PRODUCTS
LA English
DT Article
ID PRENYLATED ANTHRANOIDS; GENUS VISMIA; CHEMISTRY; XANTHONES; GUINEENSIS
AB Bioassay-guided fractionation of the methanolic extracts of Vismia baccifera, V. jefensis, and V. macrophylla against human breast, CNS, and lung cancer cell lines resulted in the isolation of a new compound, ferruginin C (1), and seven known compounds, ferruginins A (2) and B (3), vismin (4), harunganin (5), vismione B (6), deacetylvismione H (7), and deacetylvismione A (8), as active constituents. In addition, bivismiaquinone (9) and vismiaquinone (10) were obtained as inactive constituents. The structure of ferruginin C was elucidated by spectroscopic means. Compounds 6-8 were the most active, and the cytotoxic activity of compounds 2-5 and 7 is reported for the first time.
C1 Univ Panama, CIFLORPAN, Fac Farm, Panama City, Panama.
Smithsonian Trop Res Inst, Panama City, Panama.
Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.
RP Gupta, MP (reprint author), Univ Panama, CIFLORPAN, Fac Farm, Apartado 10767,Estafeta Univ, Panama City, Panama.
EM cytedqff@ancon.up.ac.pa
OI Gupta, Mahabir/0000-0002-9302-7864; Hussein, Ahmed/0000-0002-3877-9959
FU FIC NIH HHS [1U01 TW 01021-01]
NR 25
TC 41
Z9 43
U1 0
U2 3
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0163-3864
J9 J NAT PROD
JI J. Nat. Prod.
PD JUN
PY 2003
VL 66
IS 6
BP 858
EP 860
DI 10.1021/np020566w
PG 3
WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy
SC Plant Sciences; Pharmacology & Pharmacy
GA 695CY
UT WOS:000183814600023
PM 12828475
ER
PT J
AU Rubio-Palis, Y
Wilkerson, R
Guzman, H
AF Rubio-Palis, Y
Wilkerson, R
Guzman, H
TI Morphological characters of adult Anopheles (Nyssorhynchus) marajoara in
Venezuela
SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION
LA English
DT Article
DE Anopheles marajoara; malaria vectors; morphology; random amplified
polymorphic DNA-polymerase; chain reaction
ID AMPLIFIED POLYMORPHIC DNA; POLYMERASE CHAIN-REACTION; ALBITARSIS
COMPLEX; WESTERN VENEZUELA; MALARIA VECTOR; CULICIDAE; DIPTERA; BRAZIL;
ARGENTINA
AB A morphometric study was carried out to find diagnostic characters with which to update taxonomic keys for field identification of Anopheles (Nyssorhynchus) marajoara and the 3 other sympatric Anopheles (Nyssorhynchus) species (An. darlingi, An. argyritarsis, and An. braziliensis) that occur in Venezuela. Diagnostic random amplified polymorphic DNA-polymerase chain reaction markers from wild-caught specimens showed that An. marajoara was the only species in the Anopheles albitarsis complex collected in Venezuela.
C1 Inst Altos Estudios Dr Arnoldo Gabaldon, Maracay 2101A, Venezuela.
Univ Carabobo, BIOMED, Bioanalisis, Maracay, Venezuela.
Smithsonian Inst, Walter Reed Biosystemat Unit, Washington, DC 20560 USA.
RP Rubio-Palis, Y (reprint author), Inst Altos Estudios Dr Arnoldo Gabaldon, Apartado 2073, Maracay 2101A, Venezuela.
NR 30
TC 12
Z9 15
U1 0
U2 0
PU AMER MOSQUITO CONTROL ASSOC
PI EATONTOWN
PA P O BOX 234, EATONTOWN, NJ 07724-0234 USA
SN 8756-971X
J9 J AM MOSQUITO CONTR
JI J. Am. Mosq. Control Assoc.
PD JUN
PY 2003
VL 19
IS 2
BP 107
EP 114
PG 8
WC Entomology
SC Entomology
GA 693LZ
UT WOS:000183720200001
PM 12825659
ER
PT J
AU Verling, E
Crook, AC
Barnes, DKA
Harrison, SSC
AF Verling, E
Crook, AC
Barnes, DKA
Harrison, SSC
TI Structural dynamics of a sea-star (Marthasterias glacialis) population
SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM
LA English
DT Article
ID PARACENTROTUS-LIVIDUS LAMARCK; ASTERIAS-VULGARIS; FEEDING ECOLOGY; LOUGH
INE; PREY; BEHAVIOR; RECRUITMENT; SELECTION; SEASTARS; PREDATOR
AB The dynamics and feeding biology of a population of Marthasterias glacialis (Echinodermata: Asteroidea) was examined over a two-year period from 2000-2002 at Lough Hyne Marine Nature Reserve, Co. Cork, Ireland. A multivariate approach was used and both multiple factors and multiple interactions between factors were found to influence population structure. These included time of year, site, individual sea-star size, depth, and predator density. Individuals belonging to the smallest size-classes (0-50 mm and 51-100 mm) were most abundant amongst boulders in shallow water (0-1 m), while larger individuals were primarily found in water below 1 m in depth on finer grade substratum and shell debris. Dietary composition was also found to differ with depth; sea-stars in the immediate subtidal had an opportunistic diet, and fed on a variety of taxa, whilst those M. glacialis from 1-6 m were more selective and restrictive, feeding chiefly on bivalve prey. We propose that spatial partitioning of different size-classes and a generalist feeding strategy may account for the success of M. glacialis at Lough Hyne.
C1 Natl Univ Ireland Univ Coll Cork, Dept Zool & Anim Ecol, Cork, Ireland.
British Antarctic Survey, Div Biol Sci, Cambridge CB3 0ET, England.
RP Verling, E (reprint author), Smithsonian Environm Res Ctr, Marine Invas Res Lab, POB 28, Edgewater, MD 21037 USA.
NR 31
TC 23
Z9 25
U1 1
U2 5
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 0025-3154
J9 J MAR BIOL ASSOC UK
JI J. Mar. Biol. Assoc. U.K.
PD JUN
PY 2003
VL 83
IS 3
BP 583
EP 592
DI 10.1017/S0025315403007513h
PG 10
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 679HR
UT WOS:000182915100023
ER
PT J
AU Stevens, MA
Boness, DJ
AF Stevens, MA
Boness, DJ
TI Influences of habitat features and human disturbance on use of breeding
sites by a declining population of southern fur seals (Arctocephalus
australis)
SO JOURNAL OF ZOOLOGY
LA English
DT Article
DE fur seals; Arctocephalus australis; breeding habitat; El Nino;
population decline; Allee effect
ID MONK SEAL; DISCRIMINANT-ANALYSIS; GREY SEALS; BEHAVIOR; SELECTION;
VARIABLES; POLYGYNY; PERU
AB Southern fur seals Arctocephalus australis in Peru have declined gradually over the past decade, and declined dramatically (72%) as a result of low food availability during the severe El Nino in 1997-98. In 1999, seals abandoned some historically important breeding sites. This is particularly alarming because new sites were not colonized. Our objective was to examine how habitat features and human disturbance influenced whether sites were currently used, abandoned or apparently not used in the past by fur seals for breeding. Data were collected on 14 variables at 70 potential breeding sites at three guano reserves in Peru. Discriminant analysis revealed significant multivariate differences among sites currently used for breeding, abandoned sites and unused sites (F = 5.97, P < 0.00001), and the model classified 74% of sites correctly. Currently used sites were less likely to have human disturbance and more likely to have offshore islands, stacked rocks, tide pools and abundant shade. Separate discriminant analyses for each reserve produced similar results. Habitat associated with thermoregulation (e.g. shade or pools) may be more important to fur seals in Peru, which breed at lower latitudes and are at greater risk of overheating on land than other populations. Habitat with minimized human access may be especially important to seals in small populations in which individuals may perceive themselves as more vulnerable because of decreased vigilance and dilution effects. Seals in our study selected breeding habitat with stacked rocks, which create shade and tide pools for thermoregulation and make human access difficult; but pups might suffer higher mortality in this habitat. We hypothesize that fur seals in Peru may exhibit an Allee effect, whereby suitability of habitat varies with population abundance.
C1 Univ New Hampshire, Dept Zool, Durham, NH 03824 USA.
Smithsonian Inst, Natl Zool Pk, Dept Conservat Biol, Washington, DC 20008 USA.
RP Stevens, MA (reprint author), Univ New Hampshire, Dept Zool, 46 Coll Rd, Durham, NH 03824 USA.
NR 51
TC 34
Z9 37
U1 3
U2 21
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 0952-8369
J9 J ZOOL
JI J. Zool.
PD JUN
PY 2003
VL 260
BP 145
EP 152
DI 10.1017/S0952836903003583
PN 2
PG 8
WC Zoology
SC Zoology
GA 695CK
UT WOS:000183813400007
ER
PT J
AU Smith, HA
AF Smith, HA
TI Designer filters rely on metal mesh
SO LASER FOCUS WORLD
LA English
DT Article
AB Infrared filters fabricated from metal grids allow easy tailoring of the filters' optical properties.
C1 Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, Cambridge, MA 02138 USA.
RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, Opt & Infrared Div, 60 Garden St, Cambridge, MA 02138 USA.
NR 9
TC 0
Z9 0
U1 2
U2 2
PU PENNWELL PUBL CO
PI NASHUA
PA 98 SPIT BROOK RD, NASHUA, NH 03062-2801 USA
SN 0740-2511
J9 LASER FOCUS WORLD
JI Laser Focus World
PD JUN
PY 2003
VL 39
IS 6
BP 123
EP 125
PG 3
WC Optics
SC Optics
GA 696GF
UT WOS:000183878700038
ER
PT J
AU Schroll, S
AF Schroll, S
TI American expressionism: Art and social change 1920-1950.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst, Lib, Washington, DC 20560 USA.
RP Schroll, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 1
PY 2003
VL 128
IS 10
BP 112
EP +
PG 2
WC Information Science & Library Science
SC Information Science & Library Science
GA 685WX
UT WOS:000183288100044
ER
PT J
AU Aiello, A
AF Aiello, A
TI An obsession with butterflies: Our long love affair with a singular
insect.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Trop Res Inst, Ancon, Panama.
RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD JUN 1
PY 2003
VL 128
IS 10
BP 160
EP 160
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 685WX
UT WOS:000183288100178
ER
PT J
AU Dick, MH
Herrera-Cubilla, A
Jackson, JBC
AF Dick, MH
Herrera-Cubilla, A
Jackson, JBC
TI Molecular phylogeny and phylogeography of free-living Bryozoa
(Cupuladriidae) from both sides of the Isthmus of Panama
SO MOLECULAR PHYLOGENETICS AND EVOLUTION
LA English
DT Article
ID TROPICAL AMERICAN MOLLUSKS; MITOCHONDRIAL-DNA; EVOLUTIONARY
RELATIONSHIPS; MORPHOLOGICAL DIVERGENCE; EASTERN PACIFIC; 16S RDNA;
CRABS; SEA; SUBSTITUTION; SPECIATION
AB Genetic data were used to identify Recent species of free-living bryozoans (Cupuladriidae) from both sides of the Isthmus of Panama, and to examine their phylogenetic relationships, species richness, and population structures. An approximately 480 bp fragment of the 16S mitochondrial rRNA gene was sequenced from 182 individuals from Panama, the Gulf of Mexico, and El Salvador. Ten haplotype groups (Cupuladria 4, 5, and 6; Discoporella 1, 2, 3A, 3B, 3C, 7, and 8) were identified. Genetic distances between haplotype groups (3.2-26.5%; K2P + Gamma) were 1-2 orders of magnitude greater than within groups (0.1-1.4%). Seven of the haplotype groups represent morphologically distinct species; Discoporellas 3A-C appear to be cryptic species. Phylogenetic analyses identified two pairs of transisthmian sister clades. An average divergence rate derived from other taxa suggests that Cupuladrias 4 and 5 diverged approximate to7 Ma, a Discoporella 7 clade diverged from a 3A-C clade approximate to11 Ma, and the 3A-C clade radiated approximate to6-4 Ma; these events all predated final closure of the isthmus? 3 Ma. The Caribbean side of the isthmus, with 5 species, is only marginally richer in cupuladriids than the Pacific side, with 4, but has greater phylogenetic depth. The Caribbean retains lineages stemming from a New World Miocene radiation that are not represented in the eastern Pacific; extant eastern Pacific cupuladriids share most recent common ancestry with only two of the Caribbean lineages. Species in the eastern Pacific tend to show shallow population structures, with high levels of gene flow between geographically separate populations, whereas Caribbean species tend to show deeper populations structures, with indications of restricted gene flow between Bocas del Toro/Gulf of Mosquitos and Costa Arriba/San Blas. The population structures derive from Pleistocene histories and may be of limited value in interpreting the macroevolutionary pattern, as our results provide no evidence of speciation on either side of the isthmus following closure in the late Pliocene. (C) 2003 Elsevier Science (USA). All rights reserved.
C1 Middlebury Coll, Dept Biol, Middlebury, VT 05753 USA.
Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Balboa, Panama.
Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Dick, MH (reprint author), Middlebury Coll, Dept Biol, Middlebury, VT 05753 USA.
EM dick@middlebury.edu
RI Dick, Matthew/E-1327-2012
NR 79
TC 32
Z9 35
U1 1
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 JUN
PY 2003
VL 27
IS 3
BP 355
EP 371
DI 10.1016/S1055-7903(03)00025-3
PG 17
WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics &
Heredity
GA 680VG
UT WOS:000182999200001
PM 12742742
ER
PT J
AU Burke, DJ
Collins, CA
Sharples, RM
Romer, AK
Nichol, RC
AF Burke, DJ
Collins, CA
Sharples, RM
Romer, AK
Nichol, RC
TI The Southern SHARC catalogue: a ROSAT survey for distant galaxy clusters
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE catalogues; surveys; galaxies : clusters : general; X-rays : galaxies :
clusters
ID SPATIAL CORRELATION-FUNCTION; X-RAY-CLUSTERS; N-LOG-S;
MEDIUM-SENSITIVITY SURVEY; FLUX-LIMITED SAMPLE; ALL-SKY SURVEY;
LUMINOSITY FUNCTION; RICH CLUSTERS; WARPS SURVEY; PSPC OBSERVATIONS
AB X-ray selection provides a way of creating well-defined samples of distant clusters free from projection effects and with a well-understood selection function. This paper describes the creation of one such catalogue - the Southern Serendipitous High-redshift Archival ROSAT Cluster (SHARC) survey - which covers an area of 17.7 deg(2) and consists of 32 clusters with redshifts between 0.05 and 0.7 and X-ray luminosities between 7 x 10(42) and 4 x 10(44) erg s(-1): the high-redshift subsample contains 16 clusters with z greater than or equal to 0.3 and X-ray luminosities greater than 2 x 10(43) erg s(-1) (luminosities are quoted for the 0.5-2.0 keV energy band). The catalogue is in good agreement with those of other ROSAT cluster surveys for those fields in common. The high-redshift sample is consistent with there being no evolution in the cluster X-ray luminosity function at luminosities similar to10(44) erg s(-1): the implications of this work have been described elsewhere.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England.
Univ Durham, Dept Phys, Durham DH1 3LE, England.
Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dburke@cfa.harvard.edu
RI Sharples, Ray/N-7309-2013;
OI Sharples, Ray/0000-0003-3449-8583; Burke, Douglas/0000-0003-4428-7835
NR 92
TC 24
Z9 24
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2003
VL 341
IS 4
BP 1093
EP 1108
DI 10.1046/j.1365-8711.2003.06378.x
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FD
UT WOS:000183080200012
ER
PT J
AU Torres, MAP
Callanan, PJ
Garcia, MR
AF Torres, MAP
Callanan, PJ
Garcia, MR
TI Time-resolved spectroscopy of the M15 X-ray binary AC211/X2127+119
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; binaries : close; stars : individual :
AC211; stars : individual : X2127+119; X-rays : binaries
ID ACCRETION DISK CORONAE; GLOBULAR-CLUSTERS; OPTICAL COUNTERPART;
X2127+119; PERIOD; EVOLUTION; EMISSION; BURST; DISCOVERY; OUTFLOW
AB We present time-resolved spectroscopy acquired during two epochs (spaced apart by similar to15 d) of the eclipsing low-mass X-ray binary AC211/X2127+119 in the globular cluster M15. The spectra show variations in the He iilambda4686 emission line not only modulated on the orbital period, but also on time-scales of a few days. During the first epoch of observation, the emission line shows a strong S -wave superimposed on the average double-peaked profile. The line exhibits no evidence of rotational disturbance at the orbital phases when the eclipse is observed in the optical continuum. During the second epoch, no double-peak or S -wave component is present. The He i absorption lines detected by other authors are not present in our spectra. A Doppler image of He iilambda4686 for the first epoch supports the presence of the accretion disc. No hotspot is detected, although enhanced emission at V-X = 30 km s(-1) , V-Y = 160 km s(-1) is observed. We discuss the implications of this emission in the context of an X-ray heated donor star, in which case a high mass ratio and neutron star primary are implied. Finally, we speculate on the possibility of a misaligned secondary star in AC211.
C1 Univ Coll, Dept Phys, Cork, Ireland.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Torres, MAP (reprint author), Univ Coll, Dept Phys, Cork, Ireland.
NR 46
TC 3
Z9 3
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2003
VL 341
IS 4
BP 1231
EP 1238
DI 10.1046/j.1365-8711.2003.06486.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FD
UT WOS:000183080200024
ER
PT J
AU Saija, R
Iati, MA
Giusto, A
Borghese, F
Denti, P
Aiello, S
Cecchi-Pestellini, C
AF Saija, R
Iati, MA
Giusto, A
Borghese, F
Denti, P
Aiello, S
Cecchi-Pestellini, C
TI Radiation pressure cross-sections of fluffy interstellar grains
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE radiation mechanisms : general; dust, extinction
ID OPTICAL-PROPERTIES; ELECTROMAGNETIC SCATTERING; DUST GRAINS; GALAXIES;
PARTICLES; EMISSION; SPHERES; EFFLUX
AB We computed, through the transition matrix method, the radiation pressure cross-sections of cosmic dust grains modelled as aggregates (clusters) of spheres of appropriate geometry. The calculation is performed without resorting to any approximation and with a computational effort that is noticeably lighter than the one required by other methods. Our results show that radiation pressure cross-sections decrease with increasing particle fluffiness in the near-ultraviolet and visible range of the spectrum. This is due to the decrease of the corresponding strength of the multiple scattering processes that couple the aggregated spheres to each other. As a result, the inertial response to radiation forces of highly porous aggregates tends to become similar to that of the constituent particles.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Messina, Dipartimento Fis Mat & Tecnol Fis Avanzate, I-98166 Messina, Italy.
Ist Nazl Fis Mat, Unita Messina, Messina, Italy.
Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy.
RP Saija, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Cecchi Pestellini, Cesare/0000-0001-7480-0324; IATI', MARIA
ANTONIA/0000-0002-3576-8656; IATI', MARIA ANTONIA/0000-0003-0467-8049
NR 34
TC 24
Z9 24
U1 0
U2 3
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2003
VL 341
IS 4
BP 1239
EP 1245
DI 10.1046/j.1365-8711.2003.06490.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FD
UT WOS:000183080200025
ER
PT J
AU Hernquist, L
Springel, V
AF Hernquist, L
Springel, V
TI An analytical model for the history of cosmic star formation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE methods : analytical; galaxies : formation; cosmology : theory
ID ULTRAVIOLET LUMINOSITY DENSITY; GALAXY REDSHIFT SURVEY; HUBBLE DEEP
FIELD; SIMULATIONS; POPULATION; EVOLUTION; UNIVERSE; LAW
AB We use simple analytic reasoning to identify physical processes that drive the evolution of the cosmic star formation rate, (rho) over dot(*), in cold dark matter universes. Based on our analysis, we formulate a model to characterize the redshift dependence of (rho) over dot(*) and compare it with results obtained from a set of hydrodynamic simulations that include star formation and feedback.
We find that the cosmic star formation rate is described by two regimes. At early times, densities are sufficiently high and cooling times sufficiently short that abundant quantities of star-forming gas are present in all dark matter haloes that can cool by atomic processes. Consequently, (rho) over dot(*) generically rises exponentially as z decreases, independent of the details of the physical model for star formation, but dependent on the normalization and shape of the cosmological power spectrum. This part of the evolution is dominated by gravitationally driven growth of the halo mass function. At low redshifts, densities decline as the universe expands to the point that cooling is inhibited, limiting the amount of star-forming gas available. We find that in this regime the star formation rate scales approximately as (rho) over dot(*) proportional to H(z)(4/3), in proportion to the cooling rate within haloes.
We demonstrate that the existence of these two regimes leads to a peak in the star formation rate at an intermediate redshift z =z (peak). We discuss how the location of this peak depends on our model parameters, and show that the peak cannot occur above a limiting redshift of z approximate to 8.7. For the star formation efficiency adopted in our numerical simulations, z (peak) approximate to 5-6, with half of all stars forming at redshifts larger than z similar or equal to 2.2.
We derive analytic expressions for the full star formation history and show that they match our simulation results to better than similar or equal to10 per cent. Using various approximations, we reduce the expressions to a simple analytic fitting function for (rho) over dot(*) that can be used to compute global cosmological quantities that are directly related to the star formation history. As examples, we consider the integrated stellar density, the supernova and gamma-ray burst rates observable on Earth, the metal enrichment history of the Universe, and the density of compact objects. We also briefly discuss the expected dependence of the star formation history on cosmological parameters and the physics of the gas.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP Hernquist, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 55
TC 164
Z9 164
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD JUN 1
PY 2003
VL 341
IS 4
BP 1253
EP 1267
DI 10.1046/j.1365-8711.2003.06499.x
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 682FD
UT WOS:000183080200027
ER
PT J
AU Elander, N
Levin, S
Yarevsky, E
AF Elander, N
Levin, S
Yarevsky, E
TI Smooth exterior complex-scaling, full-angular-momentum, and
three-dimensional finite-element method applied to doubly excited states
of helium
SO PHYSICAL REVIEW A
LA English
DT Article
ID RESONANCE; HE; TRANSITIONS; THRESHOLDS; ENERGIES; SYSTEMS; ATOM
AB A technique based on the total-angular-momentum representation the smooth exterior complex-scaling procedure, and the three-dimensional finite-element method, is applied to calculations of S, P, and D resonant, so-called doubly excited, states of the helium atom. The resonances are calculated with an accuracy better than 10(-5) a.u. The applicability of an extrapolation procedure to complex energies is analyzed.
C1 Stockholm Univ, Alba Nova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
St Petersburg State Univ, Inst Phys, St Petersburg 198904, Russia.
Harvard Univ, Cambridge, MA 02138 USA.
Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
Int Solvay Inst Phys & Chem, B-1050 Brussels, Belgium.
RP Elander, N (reprint author), Stockholm Univ, Alba Nova Univ Ctr, Dept Phys, SE-10691 Stockholm, Sweden.
RI Yarevsky, Evgeny/J-4447-2013
OI Yarevsky, Evgeny/0000-0002-0921-6196
NR 34
TC 13
Z9 13
U1 0
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
EI 1094-1622
J9 PHYS REV A
JI Phys. Rev. A
PD JUN
PY 2003
VL 67
IS 6
AR 062508
DI 10.1103/PhysRevA.67.062508
PG 6
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 696YM
UT WOS:000183915200058
ER
PT J
AU Krems, RV
Dalgarno, A
Balakrishnan, N
Groenenboom, GC
AF Krems, RV
Dalgarno, A
Balakrishnan, N
Groenenboom, GC
TI Spin-flipping transitions in (2)Sigma molecules induced by collisions
with structureless atoms
SO PHYSICAL REVIEW A
LA English
DT Article
ID ULTRACOLD MOLECULES; COLD; TEMPERATURES; SCATTERING
AB It is shown that spin-flipping transitions in low energy collisions of (2)Sigma diatomic molecules in the lowest rotational N=0 level with structureless atoms proceed through coupling to the rotationally excited N>0 levels, and are determined by the spin-rotation interaction in the rotationally excited molecule. We carry out calculations for collisions of CaH and He-3. For the spin-flip rate coefficient corresponding to an interaction potential that does not generate a shape resonance, we obtain 1.20x10(-17) cm(3) s(-1) at a temperature of 0.4 K consistent with the measured value of 10(-17+/-1) cm(3) s(-1). We make predictions as to which molecules should have the least probability of spin-flipping in collisions with atoms.
C1 Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
Univ Nijmegen, Inst Theoret Chem, NSRIM, NL-6525 ED Nijmegen, Netherlands.
RP Krems, RV (reprint author), Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
RI Groenenboom, Gerrit/F-9692-2015
NR 16
TC 50
Z9 50
U1 1
U2 3
PU AMERICAN PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD JUN
PY 2003
VL 67
IS 6
AR 060703
DI 10.1103/PhysRevA.67.060703
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 696YM
UT WOS:000183915200007
ER
PT J
AU Wright, HE
AF Wright, HE
TI A quiz for our readers (Johannes de Mare, 1806-89)
SO PRINT QUARTERLY
LA English
DT Article
C1 Smithsonian Inst, Amer Museum Nat Hist, Washington, DC 20013 USA.
RP Wright, HE (reprint author), Smithsonian Inst, Amer Museum Nat Hist, PO Box 37012, Washington, DC 20013 USA.
EM wrighth@si.edu
NR 1
TC 0
Z9 0
U1 0
U2 0
PU PRINT QUART LTD
PI LONDON
PA 80 CARLTON HILL, LONDON NW8 0ER, ENGLAND
SN 0265-8305
J9 PRINT Q
JI Print Q.
PD JUN
PY 2003
VL 20
IS 2
BP 162
EP 163
PG 2
WC Art
SC Art
GA 712EL
UT WOS:000184784200005
ER
PT J
AU Katz, CA
Hewitt, JN
Corey, BE
Moore, CB
AF Katz, CA
Hewitt, JN
Corey, BE
Moore, CB
TI A survey for transient astronomical radio emission at 611 MHz
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID GAMMA-RAY BURST; BLACK-HOLE EXPLOSIONS; PULSES; SEARCH; AFTERGLOWS;
SUPERNOVAE; RADIATION; PULSARS; EVENTS; STARS
AB We have constructed and operated the Survey for Transient Astronomical Radio Emission ( STARE) to detect transient astronomical radio emission at 611 MHz originating from the sky over the northeastern United States. The system is sensitive to transient events on timescales of 0.125 s to a few minutes, with a typical zenith flux density detection threshold of approximately 27 kJy. During 18 months of around-the-clock observing with three geographically separated instruments, we detected a total of 4,318,486 radio bursts. Of these events, 99.9% were rejected as locally generated interference, determined by requiring the simultaneous observation of an event at all three sites for it to be identified as having an astronomical origin. The remaining 3898 events have been found to be associated with 99 solar radio bursts. These results demonstrate the remarkably effective radio frequency interference rejection achieved by a coincidence technique using precision timing (such as GPS clocks) at geographically separated sites. The nondetection of extrasolar bursting or flaring radio sources has improved the flux density sensitivity and timescale sensitivity limits set by several similar experiments in the 1970s. We discuss the consequences of these limits for the immediate solar neighborhood and the discovery of previously unknown classes of sources. We also discuss other possible uses for the large collection of 611 MHz monitoring data assembled by STARE.
C1 MIT, Elect Res Lab, Cambridge, MA 02139 USA.
MIT, Dept Phys, Cambridge, MA 02139 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
MIT, Haystack Observ, Westford, MA 01886 USA.
TransForm Pharmaceut, Lexington, MA 02421 USA.
RP Katz, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
EM ckatz@cfa.harvard.edu; jhewitt@mit.edu; bcorey@haystack.mit.edu;
cmoore@alum.mit.edu
NR 51
TC 16
Z9 16
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
EI 1538-3873
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD JUN
PY 2003
VL 115
IS 808
BP 675
EP 687
DI 10.1086/375568
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679WF
UT WOS:000182944400005
ER
PT J
AU Gonsalves, R
Nisenson, P
AF Gonsalves, R
Nisenson, P
TI Calculation of optimized apodizers for a Terrestrial Planet Finder
coronagraphic telescope
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC
LA English
DT Article
ID RECTANGULAR APERTURES
AB One of two approaches to implementing NASA's Terrestrial Planet Finder is to build a space telescope that utilizes the techniques of coronagraphy and apodization to suppress diffraction and image exoplanets. We present a method for calculation of a telescope's apodizer that suppresses the sidelobes of the image of a star so as to optimally detect an Earth-like planet. Given the shape of a telescope's aperture and given a search region for a detector, we solve an integral equation to determine an amplitude modulation ( an apodizer) that suppresses the star's energy in the focal plane search region. The method is quite general and yields as special cases the product apodizer reported by Nisenson & Papaliolios and the prolate spheroidal apodizer of Kasdin et al. and Aime et al. We show computer simulations of the apodizers and the corresponding point-spread functions for various aperture-detector configurations.
C1 Tufts Univ, Dept Elect Engn & Comp Sci, Medford, MA 02155 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01803 USA.
RP Gonsalves, R (reprint author), Tufts Univ, Dept Elect Engn & Comp Sci, Medford, MA 02155 USA.
NR 12
TC 23
Z9 23
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6280
J9 PUBL ASTRON SOC PAC
JI Publ. Astron. Soc. Pac.
PD JUN
PY 2003
VL 115
IS 808
BP 706
EP 711
DI 10.1086/374914
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679WF
UT WOS:000182944400008
ER
PT J
AU Christy, JH
AF Christy, JH
TI Reproductive timing and larval dispersal of intertidal crabs: the
predator avoidance hypothesis
SO REVISTA CHILENA DE HISTORIA NATURAL
LA English
DT Article; Proceedings Paper
CT Symposium on Behavioral Ecology of Crustaceans
CY MAY, 2002
CL VALDIVIA, CHILE
DE larval release; larval dispersal; crabs; reproductive timing; plankton;
predation
ID MALE FIDDLER-CRABS; ADAPTIVE SIGNIFICANCE; UCA-PUGILATOR; PLANKTIVOROUS
FISHES; HATCHING RHYTHMS; GENUS UCA; RELEASE; MECHANISMS; SYNCHRONY;
CYCLES
AB Many intertidal and shallow water crabs have strong reproductive cycles and migratory larvae. Females release larvae near the time of high water of the larger amplitude nocturnal tides during the semilunar or lunar cycles. Newly hatched larvae move quickly at night toward and into the sea where, weeks later, they develop to megalopae that then ride nocturnal flood tides inshore and up estuaries to settle in adult habitats. It was first thought that crabs might time larval release so that larvae will become megalopae when they can ride the larger amplitude spring flood tides to adult habitats. This idea was rejected when it was found that were was no change in the timing of hatching during the breeding season by several estuarine species that would compensate for the decrease in the larval development period as the water temperature increased. In addition, megalopae moved up-stream at night but not on the largest spring flood tides. Attention shifted to the possible value to larvae of leaving the estuary quickly to avoid high temperatures, low salinities or stranding. This idea was not supported when it was found that species on open coasts exhibit the same reproductive patterns as do estuarine species. Alternatively, by moving quickly to the ocean at night larvae may best escape visual planktivorous fishes that are especially abundant in shallow areas. This predator avoidance hypothesis has been broadly supported: species with larvae that are cryptic, spiny and better protected from predation lack both strong reproductive cycles and larval migration. The mechanisms that promote precise reproductive timing have been little studied. evidence is presented that female fiddler crabs may adjust the timing of fertilization to compensate for variation in incubation temperatures that would otherwise induce timing errors. However, crabs on colder coasts, as in Chile, apparently do not exhibit biweekly or monthly cycles of larval release. The consequences of this for adults and larvae have vet to be explored.
C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Christy, JH (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Ancon, Panama.
NR 50
TC 35
Z9 35
U1 0
U2 4
PU SOCIEDAD BIOLGIA CHILE
PI SANTIAGO
PA CASILLA 16164, SANTIAGO 9, CHILE
SN 0716-078X
J9 REV CHIL HIST NAT
JI Rev. Chil. Hist. Nat.
PD JUN
PY 2003
VL 76
IS 2
BP 177
EP 185
PG 9
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 689TN
UT WOS:000183509200005
ER
PT J
AU Corrales, JF
Epstein, ME
AF Corrales, JF
Epstein, ME
TI Revision of the Natada fusca complex and description of six new
Neotropical species (Lepidoptera : Limacodidae)
SO REVISTA DE BIOLOGIA TROPICAL
LA English
DT Article
DE Limacodidae; Natada fusca complex; Natada; Costa Rica; larval host
plants; defoliation
AB Six new species in the genus Natada, which have been hidden under Natada fusca Druce, are described and defined primarily by genitalia. New species include N. burnsi, N. truncata, N. singulara, N. chaconi, N. covelli, and N. confusa. Five of eight species in the Natada fusca complex, which also includes N.fuscodivisa Dognin, occur in Costa Rica. Distribution of the complex ranges from Mexico to the upper Amazon Basin and Guianas. Detailed geographic information and multiple genitalic drawings of males of one species, N. confusa, are provided to help define and separate species. The lectotype and paralectotype of N. fusca are designated.
C1 Inst Nacl Biodiversidad, INBio, Heredia, Costa Rica.
Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.
RP Corrales, JF (reprint author), Inst Nacl Biodiversidad, INBio, 22-3100 Sto Domingo, Heredia, Costa Rica.
EM epstein.marc@nmnh.si.edu
NR 9
TC 1
Z9 1
U1 0
U2 2
PU REVISTA DE BIOLOGIA TROPICAL
PI SAN JOSE
PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, COSTA RICA
SN 0034-7744
J9 REV BIOL TROP
JI Rev. Biol. Trop.
PD JUN
PY 2003
VL 51
IS 2
BP 445
EP 462
PG 18
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 764TY
UT WOS:000188223200017
PM 15162738
ER
PT J
AU De Queiroz, K
Poe, S
AF De Queiroz, K
Poe, S
TI Failed refutations: Further comments on parsimony and likelihood methods
and their relationship to Popper's degree of corroboration
SO SYSTEMATIC BIOLOGY
LA English
DT Article
DE assumptions; corroboration; Karl Popper; likelihood; parsimony;
philosophy; phylogenetics; probability
ID MAXIMUM-LIKELIHOOD; PHYLOGENETIC INFERENCE; EVOLUTIONARY TREES;
SUBSTITUTION; MODELS; SYSTEMATICS; CONSEQUENCES; CONJECTURES;
HYPOTHESES; PHILOSOPHY
AB Kluge's (2001, Syst. Biol. 50: 322 - 330) continued arguments that phylogenetic methods based on the statistical principle of likelihood are incompatible with the philosophy of science described by Karl Popper are based on false premises related to Kluge's misrepresentations of Popper's philosophy. Contrary to Kluge's conjectures, likelihood methods are not inherently verificationist; they do not treat every instance of a hypothesis as confirmation of that hypothesis. The historical nature of phylogeny does not preclude phylogenetic hypotheses from being evaluated using the probability of evidence. The low absolute probabilities of hypotheses are irrelevant to the correct interpretation of Popper's concept termed degree of corroboration, which is defined entirely in terms of relative probabilities. Popper did not advocate minimizing background knowledge; in any case, the background knowledge of both parsimony and likelihood methods consists of the general assumption of descent with modification and additional assumptions that are deterministic, concerning which tree is considered most highly corroborated. Although parsimony methods do not assume ( in the sense of entailing) that homoplasy is rare, they do assume ( in the sense of requiring to obtain a correct phylogenetic inference) certain things about patterns of homoplasy. Both parsimony and likelihood methods assume ( in the sense of implying by the manner in which they operate) various things about evolutionary processes, although violation of those assumptions does not always cause the methods to yield incorrect phylogenetic inferences. Test severity is increased by sampling additional relevant characters rather than by character reanalysis, although either interpretation is compatible with the use of phylogenetic likelihood methods. Neither parsimony nor likelihood methods assess test severity ( critical evidence) when used to identify a most highly corroborated tree(s) based on a single method or model and a single body of data; however, both classes of methods can be used to perform severe tests. The assumption of descent with modification is insufficient background knowledge to justify cladistic parsimony as a method for assessing degree of corroboration. Invoking equivalency between parsimony methods and likelihood models that assume no common mechanism emphasizes the necessity of additional assumptions, at least some of which are probabilistic in nature. Incongruent characters do not qualify as falsifiers of phylogenetic hypotheses except under extremely unrealistic evolutionary models; therefore, justifications of parsimony methods as falsificationist based on the idea that they minimize the ad hoc dismissal of falsifiers are questionable. Probabilistic concepts such as degree of corroboration and likelihood provide a more appropriate framework for understanding how phylogenetics conforms with Popper's philosophy of science. Likelihood ratio tests do not assume what is at issue but instead are methods for testing hypotheses according to an accepted standard of statistical significance and for incorporating considerations about test severity. These tests are fundamentally similar to Popper's degree of corroboration in being based on the relationship between the probability of the evidence e in the presence versus absence of the hypothesis h, i.e., between p(e\hb) and p(e\b), where b is the background knowledge.
Both parsimony and likelihood methods are inductive in that their inferences ( particular trees) contain more information than ( and therefore do not follow necessarily from) the observations upon which they are based; however, both are deductive in that their conclusions ( tree lengths and likelihoods) follow necessarily from their premises ( particular trees, observed character state distributions, and evolutionary models). For these and other reasons, phylogenetic likelihood methods are highly compatible with Karl Popper's philosophy of science and offer several advantages over parsimony methods in this context.
C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA.
RP De Queiroz, K (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
EM dequeiroz.kevin@nmnh.si.edu
NR 41
TC 20
Z9 20
U1 1
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1063-5157
J9 SYST BIOL
JI Syst. Biol.
PD JUN
PY 2003
VL 52
IS 3
BP 352
EP 367
DI 10.1080/10635150390196984
PG 16
WC Evolutionary Biology
SC Evolutionary Biology
GA 680VL
UT WOS:000182999600005
PM 12775524
ER
PT J
AU Harshman, J
Huddleston, CJ
Bollback, JP
Parsons, TJ
Braun, MJ
AF Harshman, J
Huddleston, CJ
Bollback, JP
Parsons, TJ
Braun, MJ
TI True and false gharials: A nuclear gene phylogeny of Crocodylia
SO SYSTEMATIC BIOLOGY
LA English
DT Article
DE c-myc; crocodylia; data conflict; data partitions; partitioned
likelihood analysis; phylogeny; rooting
ID DATA SET INCONGRUENCE; DNA-SEQUENCE DATA; C-MYC; NUCLEOTIDE-SEQUENCE;
EVOLUTIONARY TREES; BAYESIAN-INFERENCE; MITOCHONDRIAL-DNA; SYSTEMATICS;
FAMILY; BIOGEOGRAPHY
AB The phylogeny of Crocodylia offers an unusual twist on the usual molecules versus morphology story. The true gharial (Gavialis gangeticus) and the false gharial (Tomistoma schlegelii), as their common names imply, have appeared in all cladistic morphological analyses as distantly related species, convergent upon a similar morphology. In contrast, all previous molecular studies have shown them to be sister taxa. We present the first phylogenetic study of Crocodylia using a nuclear gene. We cloned and sequenced the c-myc proto-oncogene from Alligator mississippiensis to facilitate primer design and then sequenced an 1,100-base pair fragment that includes both coding and noncoding regions and informative indels for one species in each extant crocodylian genus and six avian outgroups. Phylogenetic analyses using parsimony, maximum likelihood, and Bayesian inference all strongly agreed on the same tree, which is identical to the tree found in previous molecular analyses: Gavialis and Tomistoma are sister taxa and together are the sister group of Crocodylidae. Kishino-Hasegawa tests rejected the morphological tree in favor of the molecular tree. We excluded long-branch attraction and variation in base composition among taxa as explanations for this topology. To explore the causes of discrepancy between molecular and morphological estimates of crocodylian phylogeny, we examined puzzling features of the morphological data using a priori partitions of the data based on anatomical regions and investigated the effects of different coding schemes for two obvious morphological similarities of the two gharials.
C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Suitland, MD 20746 USA.
Univ Rochester, Dept Biol, Rochester, NY 14627 USA.
Univ Calif San Diego, Sect Ecol Behav & Evolut, Div Biol Sci, La Jolla, CA 92093 USA.
Armed Forces Inst Pathol, US Armed Forces DNA Identificat Lab, Rockville, MD 20850 USA.
RP Harshman, J (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Suitland, MD 20746 USA.
EM jharshman@pacbell.net; braun@lab.si.edu
NR 64
TC 61
Z9 64
U1 0
U2 14
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 1063-5157
EI 1076-836X
J9 SYST BIOL
JI Syst. Biol.
PD JUN
PY 2003
VL 52
IS 3
BP 386
EP 402
DI 10.1080/10635150390197028
PG 17
WC Evolutionary Biology
SC Evolutionary Biology
GA 680VL
UT WOS:000182999600008
PM 12775527
ER
PT J
AU Langley, HD
AF Langley, HD
TI From the collection: Warren Opie's sailor's uniform at Winterthur
SO WINTERTHUR PORTFOLIO-A JOURNAL OF AMERICAN MATERIAL CULTURE
LA English
DT Article
AB A visitor's curiosity about the garb of a sailor in a Winterthur exhibit led him to investigate the uniform and the person who wore it. The result is a brief sketch of the life of Warren Opie of Burlington, New Jersey, and his participation in the expedition of Commo. Matthew C. Perry to open Japan to American commerce. Also discussed are the decorations on Opie's uniform and sea bag and thier significance to his life and service.
C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA.
NR 4
TC 0
Z9 0
U1 0
U2 0
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0084-0416
J9 WINTERTHUR PORTFOLIO
JI Winterthur Portfol.-J. Amer. Mater. Cult.
PD SUM-FAL
PY 2003
VL 38
IS 2-3
BP 131
EP 141
DI 10.1086/421424
PG 11
WC Art
SC Art
GA 812TI
UT WOS:000220861400003
ER
PT J
AU McCarthy, MC
Thaddeus, P
AF McCarthy, MC
Thaddeus, P
TI Rotational spectrum and structure of Si-3
SO PHYSICAL REVIEW LETTERS
LA English
DT Article
ID SMALL SILICON CLUSTERS; LABORATORY MEASUREMENT; GROUND-STATE; LINE
SURVEY; SIC2; IRC+10216; IONS
AB The rotational spectrum of a pure silicon cluster, the Si-3 trimer, has been observed for the first time. From the rotational constants of the normal and the Si-29 and Si-30 isotopic species, a precise geometrical structure has been derived: the trimer is an isosceles triangle with a bond to the apex Si of length 2.177(1) Angstrom and an apex angle of 78.10(3)degrees. The substantial inertial defect and fairly large centrifugal distortion suggest that the molecule possesses a shallow bending potential. Si-3 is a good candidate for astronomical detection because radio lines of comparably massive silicon molecules (e.g., SiC2, SiC4, and SiS) are readily observed in at least one astronomical source. The rotational spectra of Si-6, Si-9, and even larger polar silicon clusters may be detectable with the present technique, as well as similar germanium clusters.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 36
TC 34
Z9 34
U1 0
U2 2
PU AMERICAN PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0031-9007
J9 PHYS REV LETT
JI Phys. Rev. Lett.
PD MAY 30
PY 2003
VL 90
IS 21
AR 213003
DI 10.1103/PhysRevLett.90.213003
PG 4
WC Physics, Multidisciplinary
SC Physics
GA 684TV
UT WOS:000183223400015
PM 12786553
ER
PT J
AU Towe, KM
AF Towe, KM
TI Evolution of protein amino acids
SO SCIENCE
LA English
DT Letter
C1 Smithsonian Inst, Tennille, GA 31089 USA.
RP Towe, KM (reprint author), Smithsonian Inst, 230 W Adams St, Tennille, GA 31089 USA.
NR 3
TC 4
Z9 4
U1 0
U2 2
PU AMER ASSOC ADVANCEMENT SCIENCE
PI WASHINGTON
PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA
SN 0036-8075
J9 SCIENCE
JI Science
PD MAY 30
PY 2003
VL 300
IS 5624
BP 1370
EP 1371
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 683ZW
UT WOS:000183181800019
PM 12775820
ER
PT J
AU Smith, HA
Rebbert, M
Sternberg, O
AF Smith, HA
Rebbert, M
Sternberg, O
TI Designer infrared filters using stacked metal lattices
SO APPLIED PHYSICS LETTERS
LA English
DT Article
ID BAND-GAP STRUCTURES
AB We have designed and fabricated infrared filters for use at wavelengths greater than or similar to 15 microns. Unlike conventional dielectric filters used at the short wavelengths, ours are made from stacked metal grids, spaced at a very small fraction of the performance wavelengths. The individual lattice layers are gold, the spacers are polyimide, and they are assembled using integrated circuit processing techniques; they resemble some metallic photonic band-gap structures. We simulate the filter performance accurately, including the coupling of the propagating, near-field electromagnetic modes, using computer aided design codes. We find no anomalous absorption. The geometrical parameters of the grids are easily altered in practice, allowing for the production of tuned filters with predictable useful transmission characteristics. Although developed for astronomical instrumentation, the filters are broadly applicable in systems across infrared and terahertz bands. (C) 2003 American Institute of Physics.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
USN, Res Lab, Washington, DC 20375 USA.
RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 15
TC 18
Z9 18
U1 0
U2 7
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0003-6951
J9 APPL PHYS LETT
JI Appl. Phys. Lett.
PD MAY 26
PY 2003
VL 82
IS 21
BP 3605
EP 3607
DI 10.1063/1.1579115
PG 3
WC Physics, Applied
SC Physics
GA 680TB
UT WOS:000182993700007
ER
PT J
AU Mege, D
Cook, AC
Garel, E
Lagabrielle, Y
Cormier, MH
AF Mege, D
Cook, AC
Garel, E
Lagabrielle, Y
Cormier, MH
TI Volcanic rifting at Martian grabens
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Review
DE rifting; graben; pit crater; magma chamber; dyke
ID EAST PACIFIC RISE; ORBITER LASER ALTIMETER; FAST SPREADING RIDGES; GIANT
DIKE SWARMS; VALLES-MARINERIS; SURFACE DEFORMATION; INTERNAL STRUCTURE;
MIDOCEAN RIDGE; MAGMA CHAMBERS; PLATE BOUNDARY
AB [1] A large fraction of surface extension on Mars occurred at segmented grabens having width/length ratios akin to oceanic rifts on Earth. Association with volcanic landforms such as pit craters clearly suggests interconnection between tectonic and magmatic processes. A Martian rift evolution model is proposed on the basis of new geomorphological and structural interpretations of imagery, high-resolution digital elevation models (DEMs), scaled experimental modeling and three-dimensional boundary element modeling of magmatic and tectonic processes, and a comparison with terrestrial rifts. The DEMs were obtained from Mars Observer Laser Altimeter, Viking Orbiter stereo images, or a combination of both. Comparison of terrestrial rifts included Afar, Iceland, and the East Pacific Rise. The ambient extensional stress field induced by regional body forces is combined at depth with decompression melting and mantle plume thermal anomaly, resulting in emplacement of elongated magma reservoirs along the grabens. Injection of dikes above the reservoirs and flood basalt eruption result in a reservoir underpressurization of up to hundreds of MPa and induces surface collapse. Each collapse event is associated with an eruption of volcanic volumes akin to those of individual flow eruptions in large terrestrial igneous provinces. The geometry and mechanisms of graben formation and surface collapse are described and used to infer reservoir depth and width. We conclude from this study that giant dike swarms akin to typical giant terrestrial dike swarms are unlikely to underlie the volcanic Martian grabens on the basis one graben-one dike. Rather, every volcanic graben segment appears to own a local dike swarm perhaps analogous to the dike swarms in the Icelandic fissure zones.
C1 Univ Paris 06, Lab Tecton, CNRS, UMR 7072, F-75252 Paris 05, France.
Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
Univ Maine, Lab Geodynam Rifts & Marges Pass, F-72085 Le Mans 9, France.
Univ Bretagne Occidentale, Inst Rech Dev, CNRS, UMR 6538, F-29280 Plouzane, France.
Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA.
RP Mege, D (reprint author), Univ Paris 06, Lab Tecton, CNRS, UMR 7072, Boite 129,4 Pl Jussieu, F-75252 Paris 05, France.
EM dmege@lgs.jussieu.fr; acc@cs.nott.ac.uk; Erwan.Garel@univ-lemans.fr;
yvesla@univ-brest.fr; cormier@ldeo.columbia.edu
RI Mege, Daniel/A-2331-2009;
OI Mege, Daniel/0000-0003-4304-9878
NR 149
TC 44
Z9 44
U1 1
U2 4
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY 22
PY 2003
VL 108
IS E5
AR 5044
DI 10.1029/2002JE001852
PG 33
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 683YY
UT WOS:000183179700001
ER
PT J
AU Zimbelman, JR
AF Zimbelman, JR
TI Flow field stratigraphy surrounding Sekmet Mons Volcano, Kawelu
Planitia, Venus
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE fracture zones; pahoehoe; Strenia Fluctus; effusion rate; Carrizozo;
northern lowlands
ID GLOBAL DISTRIBUTION; IMPACT CRATERS; LAVA FLOWS; RADAR DATA;
EMPLACEMENT; MAGELLAN; BASALT; ASSOCIATIONS; EVOLUTION; FEATURES
AB [1] Detailed mapping has revealed several stratigraphic components among lobate plains in the vicinity of Sekmet Mons volcano (44.5degreesN. lat., 240.5degrees long.), located on the northern lowland plains of Kawelu Planitia on Venus. Volcanic effusion events produced discrete lobate plains throughout the area. Superposition of flow margins between adjacent lobate plains components indicate that the effusive activity generally progressed from southwest to northeast across the Sekmet Mons area, leading to a cumulative total of 1.5 million km(2) covered by adjacent lobate plains components. Source areas for the effusion responsible for the lobate plains components occur primarily along fracture zones or from concentrations of low volcanic domes ("shield fields'') instead of from single constructs. Magellan radar backscatter values from a mixture of both radar bright and radar dark flow components within the flow fields are well below values typical of clinkery a a lava flows on Earth, but they are consistent with values from terrestrial pahoehoe flows. Detailed mapping of Strenia Fluctus (centered on 41.5degrees N. lat., 251.0degrees long.), one of the latest lobate plains units in the area, does not show a systematic trend among effusive centers that contributed to the generation of this flow field. Instead, the Strenia Fluctus flow field is a complex mixture of flows that emanated from a shield field along Mist Chasma and that flowed down a very gentle (>0.1degrees) regional slope to the east. A 4-km-diameter cone north of Strenia Fluctus was the source of a flow complex traceable for more than 200 km over a slope of only 0.03degrees. Individual flows within Strenia Fluctus are composed of intermixed lobes, similar to relationships observed on the distal portion of the 75-km-long Carrizozo basalt flow in New Mexico, which also displays abundant inflation features and a predominant pahoehoe surface texture. If the Venusian lobate plains consist of pahoehoe flows comparable to the Carrizozo flow, they were most likely emplaced at modest effusion rates (similar to50 to 500 m(3)/s), and even with inflation the flows are likely less than or equal to15 m in thickness. Under these conditions all of the lobate plains surrounding Sekmet Mons could have been emplaced in similar to14,000 to 1400 Earth years, assuming continuous effusion with only one source vent active at a time. At similar rates all of the lowland plains in the northern hemisphere of Venus could have been resurfaced by 15-m-thick flows through continuous single-vent effusion in similar to1.4 million to similar to140 thousand Earth years.
C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
RP Zimbelman, JR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
NR 59
TC 1
Z9 1
U1 1
U2 2
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD MAY 21
PY 2003
VL 108
IS E5
AR 5043
DI 10.1029/2002JE001965
PG 12
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 683YX
UT WOS:000183179600001
ER
PT J
AU Sankrit, R
Blair, WP
Raymond, JC
AF Sankrit, R
Blair, WP
Raymond, JC
TI Optical and far-ultraviolet spectroscopy of knot D in the Vela supernova
remnant
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : individual (Vela Supernova Remnant); shock waves; supernova
remnants; ultraviolet : ISM
ID X-RAY; CYGNUS-LOOP; RADIATIVE SHOCKS; ABSORPTION LINES; RX J0852.0-4622;
HIGH-VELOCITY; EMITTING GAS; TELESCOPE; PERFORMANCE; CALIBRATION
AB We present spectra of optical. laments associated with the X-ray knot D in the Vela supernova remnant. It has been suggested that knot D is formed by a bullet of supernova ejecta, that it is a breakout of the shock front of the Vela supernova remnant, and also that it is an outflow from the recently discovered remnant RX J0852.0-4622. We find that knot D is a bow shock propagating into an interstellar cloud with normal abundances and typical cloud densities (n(H) similar to 4-11 cm(-3)). Optical long-slit spectra show that the [S II] lambdalambda6716, 6731 to Halpha line ratio is greater than unity, proving that the optical. laments are shock excited. The analysis of far-ultraviolet spectra obtained with the Hopkins Ultraviolet Telescope and with the Far Ultraviolet Spectroscopic Explorer ( FUSE) LWRS aperture show that slower shocks (similar to100 km s(-1)) produce most of the low-ionization lines such as O III] lambda1662, while faster shocks (similar to180 km s(-1)) produce the O VI lambdalambda1032, 1038 and other high-ionization lines. C III and O vi lines are also detected in the FUSE MDRS aperture, which was located on an X-ray-bright region away from the optical. laments. The lines have two velocity components consistent with similar to 150 km s(-1) shocks on the near and far sides of the knot. The driving pressure in the X-ray knot, P/k(B) similar to 1.8 x 10(7) cm(-3) K, is derived from the shock properties. This is over an order of magnitude larger than the characteristic X-ray pressure in the Vela supernova remnant. The velocity distribution of the emission and the overpressure support the idea that knot D is a bow shock around a bullet or cloud that originated near the center of the Vela remnant.
C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Sankrit, R (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
EM ravi@pha.jhu.edu; wpb@pha.jhu.edu; jraymond@cfa.harvard.edu
NR 42
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP 242
EP 252
DI 10.1086/374591
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679VW
UT WOS:000182943500019
ER
PT J
AU Trinidad, MA
Curiel, S
Canto, J
D'Alessio, P
Rodriguez, LF
Torrelles, JM
Gomez, JF
Patel, N
Ho, PTP
AF Trinidad, MA
Curiel, S
Canto, J
D'Alessio, P
Rodriguez, LF
Torrelles, JM
Gomez, JF
Patel, N
Ho, PTP
TI Observations of water masers and radio continuum emission in AFGL 2591
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE HII regions; ISM : individual (AFGL 2591); ISM : jets and outflows;
masers; stars : formation
ID YOUNG STELLAR OBJECTS; ACCRETION DISKS; MOLECULAR OUTFLOWS; VLA
OBSERVATIONS; H2O MASERS; CEPHEUS-A; STAR; SYSTEM; GL-2591; JET
AB We report results of continuum (1.3 and 3.6 cm) and H2O maser line high angular resolution observations, made with the Very Large Array (VLA) in the A configuration, toward the star-forming region AFGL 2591. Three radio continuum sources (VLA 1, VLA 2, and VLA 3) were detected in the region at 3.6 cm, and one source (VLA 3) at 1.3 cm. VLA 1 and VLA 2 appear resolved and their spectral indices suggest free-free emission from optically thin H II regions. VLA 3 is elongated in the east-west direction, along the axis of the bipolar molecular outflow observed in the region. Its spectral energy distribution is consistent with it being a similar to200 AU optically thick disk plus a photoionized wind. In addition, we detected 85 water maser spots toward the AFGL 2591 region, which are distributed in three main clusters. Two of these clusters are spatially associated with VLA 2 and VLA 3, respectively. The third cluster of masers, including the strongest water maser of the region, does not coincide with any known continuum source. We suggest that this third cluster of masers is excited by an undetected protostar that we predict to be located similar or equal to0."5 (500 AU) north from VLA 3. The maser spots associated with VLA 3 are distributed along a shell-like structure of 0."01 size, showing a peculiar velocity-position helical distribution. We propose that VLA 3 is the powering source of the observed molecular outflow in this region. Finally, we support the notion that the AFGL 2591 region is a cluster of B0-B3 type stars.
C1 Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico.
Univ Nacl Autonoma Mexico, Astron Inst, Morelia 58089, Michoacan, Mexico.
CSIC, Inst Estudis Espacials Catalunya, E-08034 Barcelona, Spain.
INTA, Lab Astrofis Espacial & Fis Fundamental, E-28080 Madrid, Spain.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Trinidad, MA (reprint author), Univ Nacl Autonoma Mexico, Astron Inst, Apartado Postal 70-264, Mexico City 04510, DF, Mexico.
RI Gomez, Jose Francisco/D-8392-2016;
OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose
Maria/0000-0002-6896-6085
NR 50
TC 39
Z9 39
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP 386
EP 396
DI 10.1086/374618
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679VW
UT WOS:000182943500030
ER
PT J
AU Ford, KES
Neufeld, DA
Goldsmith, PF
Melnick, GJ
AF Ford, KES
Neufeld, DA
Goldsmith, PF
Melnick, GJ
TI Detection of OH toward the extreme carbon star IRC+10216
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE comets : general; Kuiper Belt; planetary systems; radio lines : stars;
stars : AGB and post-AGB; stars : individual (IRC+10216)
ID CIRCUMSTELLAR DUST SHELLS; GIANT BRANCH STARS; MULTIPLE SHELLS;
WATER-VAPOR; ENVELOPE; MASER; GAS; IRC; EVOLUTION; DISCOVERY
AB We report the detection of the 1665 and 1667 MHz main lines of OH ( hydroxyl) and upper limits on the 1612 MHz satellite line of OH toward the carbon-rich AGB star IRC + 10216. We find a beam-averaged fractional abundance x(OH) similar to4 x 10(-8). This detection supports the identification by Melnick et al. of the 1(10)-1(01) transition of water vapor with a 556.936 GHz rest-frequency emission feature detected toward IRC + 10216, since OH is the expected photodissociation product of water vapor. The shape of the OH lines, however, differs significantly from the shape expected on the basis of the observations of Melnick et al. Possible explanations for the anomalous shapes of the 1665 and 1667 MHz lines are discussed. The most likely explanations for the unexpected OH line shapes are either masing or an asymmetric distribution of OH molecules around IRC + 10216.
C1 Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA.
Cornell Univ, Natl Astron & Ionosphere Ctr, Dept Astron, Ithaca, NY 14853 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ford, KES (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA.
RI Goldsmith, Paul/H-3159-2016
NR 29
TC 22
Z9 22
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP 430
EP 438
DI 10.1086/374552
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679VW
UT WOS:000182943500034
ER
PT J
AU Maness, HL
Vrtilek, SD
Kastner, JH
Soker, N
AF Maness, HL
Vrtilek, SD
Kastner, JH
Soker, N
TI Abundance anomalies in the X-ray spectra of planetary nebulae NGC 7027
and BD +30 degrees 3639
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE planetary nebulae : general; planetary nebulae : individual; (BD+30
degrees 3639, NGC 7027); stars : winds, outflows; X-rays : ISM
ID NGC-7027; EMISSION; BD+30-DEGREES-3639; MODEL; DUST; STARS; PLASMAS;
NOVA
AB We revisit Chandra observations of planetary nebulae NGC 7027 and BD + 30degrees3639 in order to address the question of abundance anomalies in the X-ray-emitting gas. Enhanced abundances relative to solar of magnesium (Mg) for NGC 7027 and neon (Ne) for BD + 30degrees3639 are required to fit their X-ray spectra, whereas observations at optical and infrared wavelengths show depleted Mg and Ne in these systems. We attribute the enhancement of Mg in NGC 7027 in the X-ray, relative to the optical, to the depletion of Mg onto dust grains within the optical nebula. For BD + 30degrees3639, we speculate that the highly enhanced Ne comes from a white dwarf companion, which accreted a fraction of the wind blown by the asymptotic giant branch progenitor and went through a novalike outburst that enriched the X-ray-emitting gas with Ne.
C1 Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA.
Dept Phys, IL-36006 Oranim, Tivon, Israel.
RP Maness, HL (reprint author), Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA.
NR 34
TC 16
Z9 16
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP 439
EP 443
DI 10.1086/374414
PN 1
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679VW
UT WOS:000182943500035
ER
PT J
AU Evans, NR
Seward, FD
Krauss, MI
Isobe, T
Nichols, J
Schlegel, EM
Wolk, SJ
AF Evans, NR
Seward, FD
Krauss, MI
Isobe, T
Nichols, J
Schlegel, EM
Wolk, SJ
TI Chandra observations of associates of eta Carinae. I. Luminosities
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations : individual (Trumpler 14, Trumpler 16);
X-rays : stars
ID WOLF-RAYET STARS; X-MEGA TARGETS; O-TYPE STARS; OPEN CLUSTER
TRUMPLER-14; OPTICAL SPECTROSCOPY; ORION-NEBULA; FUNDAMENTAL PARAMETERS;
PROGENITOR MASSES; MULTIPLE SYSTEM; STELLAR CONTENT
AB The region around the eta Carinae Nebula has three OB associations, which contain a Wolf-Rayet star and several massive O3 stars. An early Chandra ACIS-I image was centered on eta Car and includes Trumpler 16 and part of Trumpler 14. The Chandra image confirms the well-known result that O and very early B stars are X-ray sources with L-X similar or equal to 10(-7) L-bol over an X-ray luminosity range of about 100. Two new, anomalously strong X-ray sources have been found among the hot star population: Tr 16-244, a heavily reddened O3 I star, and Tr 16-22, a heavily reddened O8.5 V star. Two stars have an unusually large L-X/L-bol: HD 93162, a Wolf-Rayet star ( and possible binary), and Tr 16-22, a possible colliding-wind binary. In addition, a population of sources associated with cool stars is detected. In the color-magnitude diagram, these X-ray sources sit above the sequence of field stars in the Carina arm. The OB stars are on average more X-ray-luminous than the cool star X-ray sources. X-ray sources among A stars have X-ray luminosities similar to those of cooler stars and may be due to cooler companions. Upper limits are presented for B stars that are not detected in X-rays. These upper limits are also the upper limits for any cool companions that the hot stars may have. Hardness ratios are presented for the most luminous sources in bands 0.5-0.9, 0.9-1.5, and 1.5-2.04 keV. The available information on the binary nature of the hot stars is discussed, but binarity does not correlate with X-ray strength in a simple way.
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA.
NR 45
TC 33
Z9 33
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP 509
EP 525
DI 10.1086/374355
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679VW
UT WOS:000182943500042
ER
PT J
AU Nicastro, F
Martocchia, A
Matt, G
AF Nicastro, F
Martocchia, A
Matt, G
TI The lack of broad-line regions in low accretion rate active galactic
nuclei as evidence of their origin in the accretion disk
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; galaxies : active; quasars : emission lines
ID SEYFERT-2 GALAXIES; EMISSION
AB In this Letter, we present evidence suggesting that the absence or presence of hidden broad-line regions (HBLRs) in Seyfert 2 galaxies is regulated by the rate at which matter accretes onto a central supermassive black hole, in units of the Eddington rate. Evidence is based on data from a subsample of type 2 active galactic nuclei extracted from the Tran spectropolarimetric sample and made up of all those sources that also have good-quality X-ray spectra available and for which a bulge luminosity can be estimated. We use the intrinsic (i.e., unabsorbed) Xray luminosities of these sources and their black hole masses ( estimated by using the well-known relationship between nuclear mass and bulge luminosity in galaxies) to derive the nuclear accretion rate in Eddington units. We find that virtually all HBLR sources have accretion rates larger than a threshold value of (m) over dot(thres) similar or equal to 10(-3) (in Eddington units), while non-HBLR sources lie at (m) over dot less than or similar to (m) over dot(thres). These data nicely fit predictions from a model proposed by Nicastro in which the broad- line regions ( BLRs) are formed by accretion disk instabilities occurring in proximity of the critical radius at which the disk changes from gas pressure dominated to radiation pressure dominated. This radius diminishes with decreasing (m) over dot; for low enough accretion rates ( and therefore luminosities),. the critical radius becomes smaller than the innermost stable orbit and BLRs cannot form.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy.
Astron Observ, F-67000 Strasbourg, France.
RP Nicastro, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
OI Nicastro, Fabrizio/0000-0002-6896-1364
NR 21
TC 78
Z9 78
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 20
PY 2003
VL 589
IS 1
BP L13
EP L16
DI 10.1086/375715
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 679WA
UT WOS:000182943900004
ER
PT J
AU Handler, MR
Wysoczanski, RJ
Gamble, JA
AF Handler, MR
Wysoczanski, RJ
Gamble, JA
TI Proterozoic lithosphere in Marie Byrd Land, West Antarctica: Re-Os
systematics of spinel peridotite xenoliths
SO CHEMICAL GEOLOGY
LA English
DT Article
DE Re-Os isotopes; continental lithospheric mantle; xenoliths; Marie Byrd
Land; West Antarctica
ID IONIZATION MASS-SPECTROMETRY; OSMIUM ISOTOPIC COMPOSITION; OCEANIC
ISLAND BASALTS; MANTLE-PLUME ACTIVITY; NEW-ZEALAND; SOUTHEASTERN
AUSTRALIA; SUBCONTINENTAL MANTLE; SUBDUCTION ZONES; PACIFIC MARGIN;
UNITED-STATES
AB Marie Byrd Land, which forms part of the composite West Antarctica microplate, experienced a long history of subduction during Paleozoic and Mesozoic times, and has been argued to have been affected by at least one mantle plume. The age of the Marie Byrd Land lithosphere is not known, as the only lower crustal samples (granulite and pyroxenite xenoliths) have proven resistant to conventional radiogenic dating methods. The oldest exposed magmatic rocks are Cambrian, and any Precambrian history for Marie Byrd Land, while speculated upon, is unknown.
Here we present the first geochemical data for a peridotite xenolith suite from Marie Byrd Land, including Re-Os isotope measurements for 17 samples. The 17 spinel peridotites are from three volcanic centers: Mt Hampton and Mt Cumming, in the Executive Committee Range, and Mt Aldaz, in the USAS Escarpment. The xenoliths are residual lherzolites and harzburgites, ranging from fertile to depleted (e.g. 0.39-3.38 wt.% CaO) compositions. Re-Os isotopic systematics indicate a complex evolution for the Marie Byrd Land lithosphere. One sample records Re + Cu +/- Os enrichment and two samples document localized Os enrichment, which is most likely related to supra-subduction zone processing, although enrichment due to plume interaction cannot be ruled out.
Proterozoic lithosphere stabilization model ages of ca. 1.1 and > 1.3 Ga are recorded in xenoliths from the Executive Committee Range. The Proterozoic ages are significantly older than outcropping mid-crustal rocks, marking Marie Byrd Land as a third circum-Pacific Phanerozoic mobile belt with preserved Proterozoic lithospheric mantle. The Mesoproterozoic Os model ages are consistent with Proterozoic Nd model ages in Marie Byrd Land granites and orthogneisses, and with a significant detrital zircon age component (ca. 1.0-1.2 Ga) in the thick Swanson Formation sediments that are exposed along the coast. The simplest interpretation of the available mantle and crustal age data is that the lower crust beneath Marie Byrd Land is also Proterozoic in age. Alternatively, if the mantle and lower crust in Marie Byrd Land are not temporally coupled, possible origins for the Proterozoic mantle include older lithosphere impinging from the adjacent East Antarctic craton, or lithospheric mantle that was incorporated into younger oceanic lithosphere during "messy" continental breakup (e.g. within an oceanic plateau) and subsequently accreted to the Antarctic margin. (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Carnegie Inst Washington, DTM, Washington, DC 20015 USA.
Smithsonian Inst, NMNH, Dept Mineral Sci, Washington, DC 20560 USA.
Victoria Univ Wellington, Dept Geol, Wellington, New Zealand.
RP Handler, MR (reprint author), JAMSTEC, IFREE, 2-15 Natsushima Cho, Kanagawa 2370061, Japan.
EM monica@jamstec.go.jp
RI Wysoczanski, Richard/C-2930-2009; Handler`, Monica/E-9460-2011;
Wysoczanski, Richard/I-7730-2012
OI Handler`, Monica/0000-0001-7095-0835;
NR 80
TC 31
Z9 33
U1 2
U2 11
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
J9 CHEM GEOL
JI Chem. Geol.
PD MAY 15
PY 2003
VL 196
IS 1-4
BP 131
EP 145
DI 10.1016/S0009-2541(02)00410-2
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 671HA
UT WOS:000182458200008
ER
PT J
AU Parkinson, WH
Rufus, J
Yoshino, K
AF Parkinson, WH
Rufus, J
Yoshino, K
TI Absolute absorption cross section measurements of CO2 in the wavelength
region 163-200 nm and the temperature dependence
SO CHEMICAL PHYSICS
LA English
DT Article
DE carbon dioxide; cross sections
ID CARBON-DIOXIDE; HIGH-RESOLUTION; SPECTRUM; PHOTODISSOCIATION;
ATMOSPHERE; TRANSITION; MARS
AB Laboratory measurements of the absorption cross section Of CO2 at the temperatures 195 and 295 K have been made throughout the wavelength region 163-200 nm by using a high resolution grating spectrometer. Cross sections at 195 K are smaller than those at 295 K, and the band structures are more emphasized as expected. In combining with our previous measurements [J. Quant. Spectrosc. Radiat. Transfer, 55 (1996) 53], the absorption cross sections Of CO2 are available in the wavelength region 117.8-200.0 nm at 295 K and 117.8-192.5 nm at 195 K. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Yoshino, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-50, Cambridge, MA 02138 USA.
NR 18
TC 38
Z9 38
U1 1
U2 12
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0301-0104
J9 CHEM PHYS
JI Chem. Phys.
PD MAY 15
PY 2003
VL 290
IS 2-3
BP 251
EP 256
DI 10.1016/S0301-0104(03)00146-0
PG 6
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 679ZA
UT WOS:000182950800012
ER
PT J
AU Kalfatovic, MR
AF Kalfatovic, MR
TI Ceanne and Provence: The painter in his culture.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Lib, Washington, DC USA.
RP Kalfatovic, MR (reprint author), Smithsonian Inst Lib, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD MAY 15
PY 2003
VL 128
IS 9
BP 84
EP 84
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 678RN
UT WOS:000182880400042
ER
PT J
AU Riley, S
AF Riley, S
TI Brilliant.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Lib, Washington, DC 20560 USA.
RP Riley, S (reprint author), Smithsonian Inst Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD MAY 15
PY 2003
VL 128
IS 9
BP 125
EP 125
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 678RN
UT WOS:000182880400230
ER
PT J
AU Chandra, S
Ziemke, JR
Martin, RV
AF Chandra, S
Ziemke, JR
Martin, RV
TI Tropospheric ozone at tropical and middle latitudes derived from
TOMS/MLS residual: Comparison with a global model
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE biomass burning; tropospheric ozone; stratospheric ozone; El Nino;
global circulation model; tropopause
ID SOUTH-ATLANTIC-OCEAN; 1997-1998 EL-NINO; STRATOSPHERIC OZONE;
UNITED-STATES; COLUMN OZONE; WATER-VAPOR; 3-D MODELS; PACIFIC;
CHEMISTRY; POLLUTION
AB The tropospheric ozone residual method is used to derive zonal maps of tropospheric column ozone using concurrent measurements of total column ozone from Nimbus 7 and Earth Probe (EP) Total Ozone Mapping Spectrometer (TOMS) and stratospheric column ozone from the Microwave Limb Sounder (MLS) instrument on the Upper Atmosphere Research Satellite (UARS). Our study shows that the zonal variability in TOMS total column ozone at tropical and subtropical latitudes is mostly of tropospheric origin. The seasonal and zonal variability in tropospheric column ozone (TCO), derived from the TOMS/MLS residual, is consistent with that derived from the convective cloud differential method and ozonesonde measurements in regions where these data overlap. A comparison of TCO derived from the TOMS/MLS residual and a global three-dimensional model of tropospheric chemistry (GEOS-CHEM) for 1996-1997 shows good agreement in the tropics south of the equator. Both the model and observations show similar zonal and seasonal characteristics including an enhancement of TCO in the Indonesian region associated with the 1997 El Nino. Both show the decline of the wave-1 pattern from the tropics to the extratropics as lightning activity and the Walker circulation decline. Both show enhanced ozone in the downwelling branches of the Hadley Circulation near +/-30degrees. Model and observational differences increase with latitude during winter and spring.
C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA.
Harvard Univ, Harvard Smithsonian Ctr Astrophys, Div Engn & Appl Sci, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA.
RP NASA, Goddard Space Flight Ctr, Code 916, Greenbelt, MD 20771 USA.
EM chandra@chapman.gsfc.nasa.gov; ziemke@jwocky.gsfc.nasa.gov;
rvmartin@fas.harvard.edu
RI Martin, Randall/A-2051-2008; Martin, Randall/C-1205-2014; Chem,
GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
NR 57
TC 34
Z9 34
U1 0
U2 5
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-897X
EI 2169-8996
J9 J GEOPHYS RES-ATMOS
JI J. Geophys. Res.-Atmos.
PD MAY 13
PY 2003
VL 108
IS D9
AR 4291
DI 10.1029/2002JD002912
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 682QN
UT WOS:000183103300009
ER
PT J
AU Molbo, D
Machado, CA
Sevenster, JG
Keller, L
Herre, EA
AF Molbo, D
Machado, CA
Sevenster, JG
Keller, L
Herre, EA
TI Cryptic species of fig-pollinating wasps: Implications for the evolution
of the fig-wasp mutualism, sex allocation, and precision of adaptation
SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF
AMERICA
LA English
DT Article
DE coevolution; symbiosis; fig wasp; ficus; local mate competition
ID MITOCHONDRIAL-DNA SEQUENCES; PHYLOGENETIC-RELATIONSHIPS; RATIOS; FICUS;
COOPERATION; AGAONIDAE; CONFLICT; BIOGEOGRAPHY; SPECIFICITY; COEVOLUTION
AB Fig-pollinating wasps have provided model systems for developing and testing theories of the evolution of mutualism, sex allocation, and precision of adaptation. With few exceptions, previous studies have assumed one species of pollinator wasp per host fig species. Here we report genetic data demonstrating the coexistence of previously undetected cryptic fig wasp species in at least half of the host fig species surveyed. The substantial mitochondrial sequence differences (4.2-6.1%) imply old divergences ( approximate to 1.5-5.1 million years ago) among these species. Furthermore, some cryptic species pairs seem to be sister taxa, whereas others clearly are not, indicating both long-term coexistence on shared hosts and the colonization of novel fig species. These findings undermine the prevalent notion of strict one-to-one specificity between cospeciating figs and their pollinators, thereby challenging existing theory concerning the evolution and stability of mutualisms. Moreover, the incorporation of the genetic information significantly improves the fit of the observed sex ratios to predictions of local mate-competition theory, further strengthening support for sex allocation theory and the precision of adaptation.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Univ Lausanne, Inst Ecol, CH-1015 Lausanne, Switzerland.
Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
Leiden Univ, Sect Anim Ecol, Inst Biol, NL-2300 RA Leiden, Netherlands.
RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Apartado 22072, Balboa, Panama.
EM herrea@gamboa.si.edu
RI Machado, Carlos/B-8855-2009;
OI Machado, Carlos/0000-0003-1546-7415; keller,
laurent/0000-0002-5046-9953; Molbo, Drude/0000-0003-3372-8711
NR 56
TC 187
Z9 205
U1 7
U2 64
PU NATL ACAD SCIENCES
PI WASHINGTON
PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA
SN 0027-8424
J9 P NATL ACAD SCI USA
JI Proc. Natl. Acad. Sci. U. S. A.
PD MAY 13
PY 2003
VL 100
IS 10
BP 5867
EP 5872
DI 10.1073/pnas.0930903100
PG 6
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 679UB
UT WOS:000182939400056
PM 12714682
ER
PT J
AU Lee, S
Pak, S
Davis, CJ
Herrnstein, RM
Geballe, TR
Ho, PTP
Wheeler, JC
AF Lee, S
Pak, S
Davis, CJ
Herrnstein, RM
Geballe, TR
Ho, PTP
Wheeler, JC
TI Interaction between the north-eastern boundary of Sgr A East and giant
molecular clouds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM : individual : Sgr A East; ISM : individual : M-0.02-0.07; ISM :
lines and bands; ISM : molecules; Galaxy : centre; infrared : ISM
ID SAGITTARIUS-A EAST; GALACTIC-CENTER; ORION NEBULA; PHOTODISSOCIATION
REGIONS; RESOLUTION OBSERVATIONS; INTERSTELLAR SHOCKS; HYDROGEN
EMISSION; GALAXY; MASERS; H-2
AB We have detected the v = 1 --> 0 S(1) (lambda= 2.1218 mum) and v = 2 --> 1 S(1) (lambda= 2.2477 mum) lines of H-2 in the Galactic Centre, in a 90 x 27 arcsec(2) region between the north-eastern boundary of the non-thermal source Sgr A East, and the giant molecular cloud (GMC) M-0.02 - 0.07. The detected H-2 v = 1 --> 0 S(1) emission has an intensity of 1.6-21 x 10(-18) W m(-2) arcsec(-2) and is present over most of the region. Along with the high intensity, the large linewidths (FWHM = 40-70 km s(-1) ) and the H-2 v = 2 --> 1 S(1) to v = 1 --> 0 S(1) line ratios (0.3-0.5) can be best explained by a combination of C-type shocks and fluorescence. The detection of shocked H-2 is clear evidence that Sgr A East is driving material into the surrounding adjacent cool molecular gas. The H-2 emission lines have two velocity components at similar to+50 and similar to0 km s(-1) , which are also present in the NH3 (3, 3) emission mapped by McGary, Coil & Ho. This two-velocity structure can be explained if Sgr A East is driving C-type shocks into both the GMC M-0.02 - 0.07 and the northern ridge of McGary et al.
C1 Seoul Natl Univ, Astron Programme SEES, Seoul 151742, South Korea.
Korea Astron Observ, Taejon 305348, South Korea.
Joint Astron Ctr, Hilo, HI 96720 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Gemini Observ, Hilo, HI 96720 USA.
Univ Texas, Dept Astron, Austin, TX 78712 USA.
RP Lee, S (reprint author), Seoul Natl Univ, Astron Programme SEES, Seoul 151742, South Korea.
RI Pak, Soojong/E-2360-2013;
OI Pak, Soojong/0000-0002-2548-238X
NR 44
TC 11
Z9 11
U1 0
U2 1
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 11
PY 2003
VL 341
IS 2
BP 509
EP 516
DI 10.1046/j.1365-8711.2003.06425.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 674TE
UT WOS:000182651400011
ER
PT J
AU Scappini, F
Cecchi-Pestellini, C
Smith, H
Klemperer, W
Dalgarno, A
AF Scappini, F
Cecchi-Pestellini, C
Smith, H
Klemperer, W
Dalgarno, A
TI Hydrated sulphuric acid in dense molecular clouds
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE ISM : clouds; dust, extinction; ISM : lines and bands; ISM : molecules;
infrared : ISM
ID HOT CORES; CHEMISTRY; WATER; SULFIDE; MODELS; ABUNDANCES; INVENTORY;
EMISSIONS; DEPLETION; FEATURES
AB We consider sulphur depletion in dense molecular clouds, and suggest hydrated sulphuric acid, H(2) SO(4) . n H(2) O, as a component of interstellar dust in icy mantles. We discuss the formation of hydrated sulphuric acid in collapsing clouds and its instability in heated regions in terms of the existing hot core models and observations. We also show that some features of the infrared spectrum of hydrated sulphuric acid have correspondence in the observed spectra of young stellar objects.
C1 CNR, Ist Studio Mat Nanostrutturati, I-40129 Bologna, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Dept Chem, Cambridge, MA 02138 USA.
RP Scappini, F (reprint author), CNR, Ist Studio Mat Nanostrutturati, Via P Gobetti 101, I-40129 Bologna, Italy.
EM ccecchi-pestellini@cfa.harvard.edu
OI Cecchi Pestellini, Cesare/0000-0001-7480-0324
NR 37
TC 15
Z9 15
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 MAY 11
PY 2003
VL 341
IS 2
BP 657
EP 661
DI 10.1046/j.1365-8711.2003.06443.x
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 674TE
UT WOS:000182651400024
ER
PT J
AU Colley, WN
Shapiro, II
Pegg, J
Turner, EL
Kundic, T
Loomis, K
Hastings, NC
McMillan, R
AF Colley, WN
Shapiro, II
Pegg, J
Turner, EL
Kundic, T
Loomis, K
Hastings, NC
McMillan, R
TI Rapid brightness fluctuations in Q0957+561A,B: Microlensing or seeing?
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies : halos; gravitational lensing; methods : data
analysis; quasars : individual (0957+561); techniques : photometric
ID TIME-DELAY; PHOTOMETRY; 0957+561A
AB We address the following question: How does one reliably distinguish rapid microlensing events from atmospheric or instrumental effects on observed brightness fluctuations of distant objects? Our approach was to do a controlled, albeit limited, experiment, the first of its kind: observe Q0957+561A,B simultaneously through filters of the same characteristics with two telescopes with comparable fields of view but separated sufficiently for atmospheric fluctuations to be independent. Over the 1998-1999 viewing season, we succeeded in obtaining simultaneous data on 14 of the 55 nights scheduled. Analysis of these data led to the following: (1) after correction for "blending'' of the A and B images, most rapid microlensing candidate outliers disappeared, and the agreement of the photometry from the two telescopes improved to an rms difference of about 15 mmag; (2) no microlensing events of amplitude greater than 0.1 mag were observed in either data set over the entire run, nearly ruling out similar to10(-5) M-circle dot MACHOs as composing more than about half the dark matter in the lens galaxy, if the source size is less than or similar to3x10(14) cm.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Princeton Univ Observ, Princeton, NJ 08544 USA.
Renaissance Technol, E Setauket, NY 11733 USA.
Apache Point Observ, Sunspot, NM 88349 USA.
RP Colley, WN (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA.
RI Turner, Edwin/A-4295-2011
NR 9
TC 3
Z9 3
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 711
EP 715
DI 10.1086/374308
PN 1
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900006
ER
PT J
AU Stepanian, JA
Benitez, E
Krongold, Y
Cruz-Gonzalez, I
de Diego, JA
Chavushyan, V
Mujica, R
Dultzin-Hacyan, D
Verdugo, T
AF Stepanian, JA
Benitez, E
Krongold, Y
Cruz-Gonzalez, I
de Diego, JA
Chavushyan, V
Mujica, R
Dultzin-Hacyan, D
Verdugo, T
TI A multiwavelength study of narrow-line Seyfert 1 galaxies from the
Second Byurakan Survey
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; galaxies : Seyfert; quasars : general
ID X-RAY PROPERTIES; ALL-SKY SURVEY; ACTIVE GALACTIC NUCLEI; SPECTRAL
ENERGY-DISTRIBUTIONS; OPTICALLY SELECTED QUASARS; POINT-SOURCE CATALOG;
WARM IRAS SOURCES; FE-II-EMISSION; COMPLETE SAMPLE; MARKARIAN GALAXIES
AB In this work we present a multiwavelength study of narrow-line Seyfert 1 galaxies (NLS1s) discovered in the Second Byurakan Survey (SBS). The sample consists of 26 objects, which have M-B greater than or equal to -23.0, or -19.9>M-B>-23.0, 0.02431). The traditional linear correlation L-X and L-op, which seems to hold for active galactic nuclei in general, is found for SBS NLS1s. An anticorrelation between the FWHM of Hbeta and the ratio of Fe II lambda4570/Hbeta is also observed. A weak correlation is found between alpha(ox) slope and L-op. One of our main findings is that almost all SBS NLS1s may not have an FIR bump. Their spectral energy distribution suggests that they may also possess a big blue bump. The absence of an IR bump in most SBS NLS1s and the weakness of X-ray radiation in some of them may argue against the presence of a broad-line region. The surface density of SBS NLS1s is less than 0.015 deg(-2) (B<17.5; z<0.16).
C1 Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Nacl Astrofis Opt & Elect, Puebla 7200, Mexico.
RP Stepanian, JA (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico.
OI Verdugo, Tomas/0000-0003-4062-6123; Jose A., de
Diego/0000-0001-7040-069X
NR 75
TC 15
Z9 16
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 746
EP 762
DI 10.1086/374215
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900010
ER
PT J
AU Done, C
Madejski, GM
Zycki, PT
Greenhill, LJ
AF Done, C
Madejski, GM
Zycki, PT
Greenhill, LJ
TI Simultaneous Chandra and Rossi X-Ray Timing Explorer observations of the
nearby bright Seyfert 2 galaxy NGC 4945
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 4945); galaxies : Seyfert; X-rays : galaxies
ID ACTIVE GALACTIC NUCLEI; MASER EMISSION; COLD MATTER; XMM-NEWTON;
NGC-4945; SPECTROSCOPY; NGC-3079; DISK; GAS; REFLECTION
AB We analyze recent simultaneous Chandra/RXTE observations of the Seyfert 2 galaxy NGC 4945. The unprecedented spatial resolution of Chandra means we are able to separate the spectra of the nucleus, starburst, and superwind regions, while the RXTE data extend the spectrum to higher energies. The extreme absorbing column of NHsimilar to4x10(24) cm(-2) means that the nucleus is only directly seen above 8-10 keV, while the lower energy spectrum from the nuclear region in Chandra is dominated by reflection. By contrast, the superwind is dominated by emission from hot plasma, but the starburst region contains both hot plasma and reflection signatures. Forming a reflected spectrum requires that the starburst region contain clumps of cool, optically thick material, perhaps star-forming cores, which are irradiated by 7-10 keV photons from the nucleus. Since photons of this energy are obscured along the line of sight, this confirms the result of Madejski et al. that the extreme absorption material is disklike rather than toroidal. However, the IR/optical limits on the lack of high-excitation emission lines show that, by contrast, the lower energy photons from the nucleus are obscured in all directions. We discuss the complex absorption structure revealed by these observations and propose an overall source geometry in which the nucleus is completely embedded in material with NHsimilar to10(23) cm(-2).
C1 Univ Durham, Dept Phys, Durham DH1 3LE, England.
Stanford Linear Accelerator Ctr, Menlo Pk, CA 94025 USA.
Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Done, C (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England.
RI done, chris/D-4605-2016
OI done, chris/0000-0002-1065-7239
NR 39
TC 35
Z9 35
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 763
EP 770
DI 10.1086/374332
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900011
ER
PT J
AU Holt, SS
Schlegel, EM
Hwang, U
Petre, R
AF Holt, SS
Schlegel, EM
Hwang, U
Petre, R
TI Chandra observation of the X-ray source population of NGC 6946
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 6946); X-rays : binaries; X-rays : galaxies;
X-rays : general
ID SPIRAL GALAXY NGC-6946; ULTRALUMINOUS SUPERNOVA REMNANT; POINT SOURCES;
LUMINOSITY; COMPLEX; STARBURST; M101; BAR; M31
AB We present the results of a study of discrete X-ray sources in NGC 6946 using a deep Chandra ACIS observation. Based on the slope of the log N-log S distribution and the general correlation of sources with the spiral arms, we infer that the overall discrete source sample in NGC 6946 is dominated by high-mass X-ray binaries, in contrast to the source distributions in M31 and the Milky Way. This is consistent with the higher star formation rate in NGC 6946 than in those galaxies. We find that the strong X-ray sources in the region of the galactic center do not correlate in detail with images of the region in the near-IR, although one of them may be coincident with the galactic center. The noncentral ultraluminous X-ray source in NGC 6946, previously identified with a supernova remnant, has an X-ray spectrum and luminosity that is inconsistent with either a traditional pulsar wind nebula or a blast wave remnant.
C1 Franklin W Olin Coll Engn, Needham, MA 02492 USA.
Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Harvard Coll Observ, Cambridge, MA 02138 USA.
NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA.
RP Holt, SS (reprint author), Franklin W Olin Coll Engn, 1735 Great Plain Ave, Needham, MA 02492 USA.
NR 33
TC 29
Z9 29
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 792
EP 800
DI 10.1086/374311
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900013
ER
PT J
AU Kraemer, KE
Jackson, JM
Kassis, M
Deutsch, LK
Hora, JL
Simon, R
Hoffmann, WF
Fazio, GG
Dayal, A
Bania, TM
Clemens, DP
Heyer, MH
AF Kraemer, KE
Jackson, JM
Kassis, M
Deutsch, LK
Hora, JL
Simon, R
Hoffmann, WF
Fazio, GG
Dayal, A
Bania, TM
Clemens, DP
Heyer, MH
TI Five star-forming cores in the Galactic Ring Survey: A mid-infrared
study
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE infrared : ISM; stars : formation
ID H-II REGIONS; YOUNG MASSIVE STARS; VLA OBSERVATIONS; ISOGAL SURVEY;
ARRAY CAMERA; NGC 6334; DUST; ABSORPTION; EMISSION; CLUSTER
AB We have imaged five dense molecular cores, selected from the Galactic Ring Survey (GRS), in the mid-infrared with the MIRAC3 instrument. We obtained high spatial resolution (similar to1") images through narrow-band filters at 12.5 and 20.6 mum. Four of the five cores show multiple compact sources, extended structure, or both. Lower resolution observations by the Infrared Space Observatory (ISO) and the Midcourse Space Experiment (MSX) suggest that the fifth core is also surrounded by extended emission on large scales (greater than or similar to2'). The extended mid-infrared structure is well-correlated with the radio continuum morphology in each of the five cores. This similarity suggests that the hot dust traced by the mid-infrared is located within the H II region, traced by the radio continuum, and not merely in a surrounding photodissociation region or molecular cloud. If a single exciting source is assumed for each core, estimates of the zero-age main-sequence spectral types based on the infrared luminosities are typically 1-2 spectral types earlier than those based on the radio free-free emission. However, allowing for multiple exciting sources and apportioning the far-infrared and radio fluxes to the component sources according to the mid-infrared flux distribution produces better agreement between the derived spectral types, with an average difference of less than half a spectral type.
C1 USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA.
Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
IPAC JPL, Pasadena, CA 91125 USA.
Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA.
RP USAF, Res Lab, Space Vehicles Directorate, 29 Randolph Rd, Hanscom AFB, MA 01731 USA.
EM kathleen.kraemer@hanscom.af.mil; jackson@bu.edu; mkassis@bu.edu;
deutschl@bu.edu; jhora@cfa.harvard.edu; simonr@chub.bu.edu;
whoffmann@as.arizona.edu; gfazio@cfa.harvard.edu;
adayal@ipac.caltech.edu; bania@bu.edu; clemens@bu.edu;
heyer@astro.umass.edu
RI Bania, Thomas/H-2318-2014;
OI Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155
NR 48
TC 13
Z9 13
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 918
EP 930
DI 10.1086/374264
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900024
ER
PT J
AU Damiani, F
Flaccomio, E
Micela, G
Sciortino, S
Harnden, FR
Murray, SS
Wolk, SJ
Jeffries, RD
AF Damiani, F
Flaccomio, E
Micela, G
Sciortino, S
Harnden, FR
Murray, SS
Wolk, SJ
Jeffries, RD
TI Chandra X-ray observations of the young open cluster NGC 2516
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE open clusters and associations : individual (NGC 2516); stars : coronae;
X-rays : stars
ID COUNTING DETECTOR IMAGES; ROSAT HRI OBSERVATIONS; DEEP FIELD-SOUTH;
WAVELET TRANSFORMS; OPTICAL SURVEY; NGC-2516; STARS; LUMINOSITY;
EMISSION; PLEIADES
AB We present a comprehensive study of the Chandra X-ray observations of the young open cluster NGC 2516. We have analyzed eight individual Chandra observations. We have combined the data to achieve the greatest sensitivity, reaching down to logf(X) = -14.56 (ergs s(-1) cm(-2)), or log L-X = 28.69 (ergs s(-1)) at the distance of NGC 2516. Out of 284 X-ray sources detected, 155 are identified with photometric cluster members, with very little ambiguity. We have studied the X-ray luminosity functions for the various spectral types, correcting for nonmember contamination those for later type stars. We find strong X-ray emission from a couple of B stars that cannot be due to companions. Among A stars, chemically peculiar stars show a detection fraction much larger than normal A stars. The luminosity functions decrease monotonically from F to M stars, and those for K stars are significantly lower than similar stars in the Pleiades, a cluster only slightly younger than NGC 2516. We discuss possible causes of this discrepancy, including differences in age and stellar rotation.
C1 Osservatorio Astron Palermo GS Vaiana, INAF, I-90134 Palermo, Italy.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
Univ Keele, Dept Phys, Keele ST5 5BG, Staffs, England.
RP Damiani, F (reprint author), Osservatorio Astron Palermo GS Vaiana, INAF, Piazza Parlamento 1, I-90134 Palermo, Italy.
OI Flaccomio, Ettore/0000-0002-3638-5788; Wolk, Scott/0000-0002-0826-9261;
Damiani, Francesco/0000-0002-7065-3061
NR 27
TC 21
Z9 21
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 1009
EP 1024
DI 10.1086/374214
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900032
ER
PT J
AU Kuchner, MJ
Holman, MJ
AF Kuchner, MJ
Holman, MJ
TI The geometry of resonant signatures in debris disks with planets
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE celestial mechanics; circumstellar matter; interplanetary medium;
planetary systems; stars : individual (alpha Lyrae, epsilon Eridani,
Fomalhaut)
ID CIRCUMSTELLAR DUST DISK; MEAN-MOTION RESONANCES; POYNTING-ROBERTSON
DRAG; BETA-PICTORIS; SOLAR-SYSTEM; ZODIACAL EMISSION; EVOLUTION; RING;
PERTURBATIONS; ASYMMETRIES
AB Using simple geometrical arguments, we paint an overview of the variety of resonant structures a single planet with moderate eccentricity (e less than or similar to 0.6) can create in a dynamically cold, optically thin dust disk. This overview may serve as a key for interpreting images of perturbed debris disks and inferring the dynamical properties of the planets responsible for the perturbations. We compare the resonant geometries found in the solar system dust cloud with observations of dust clouds around Vega, epsilon Eridani, and Fomalhaut.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kuchner, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Kuchner, Marc/E-2288-2012
NR 43
TC 105
Z9 106
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 10
PY 2003
VL 588
IS 2
BP 1110
EP 1120
DI 10.1086/374213
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 680RV
UT WOS:000182991900039
ER
PT J
AU Kazmi, QB
Manning, RB
AF Kazmi, QB
Manning, RB
TI A new genus and species of pinnotherid crab from Karachi, northern
Arabian Sea (Crustacea, Decapoda, Brachyura)
SO JOURNAL OF NATURAL HISTORY
LA English
DT Article
DE Decapoda; Pinnotheridae; commensal; Gastrochaena; Sindheres; Pakistan;
new genus; new species
AB A new monotypic genus, Sindheres, is established to accommodate a new species, S. karachiensis, of pinnotherid crab from the northern Arabian Sea. The new genus resembles Nepinnotheres Manning, 1993 in having the dactylus of the third maxilliped inserted near the mid-length of the ventral margin of the propodus but it differs in having a sub-hexagonal carapace.
C1 Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA.
Univ Karachi, Marine Reference Collect & Resource Ctr, Karachi 75270, Pakistan.
RP Manning, RB (reprint author), Smithsonian Inst, Museum Natl Hist Nat, Dept Invertebrate Zool, Washington, DC 20560 USA.
NR 8
TC 3
Z9 4
U1 0
U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0022-2933
J9 J NAT HIST
JI J. Nat. Hist.
PD MAY 10
PY 2003
VL 37
IS 9
BP 1085
EP 1089
DI 10.1080/00222930110108353
PG 5
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 676MV
UT WOS:000182756600003
ER
PT J
AU Ashworth, AC
Thompson, FC
AF Ashworth, AC
Thompson, FC
TI A fly in the biogeographic ointment
SO NATURE
LA English
DT Article
ID TRANSANTARCTIC MOUNTAINS; SIRIUS GROUP; ANTARCTICA
C1 N Dakota State Univ, Dept Geosci, Fargo, ND 58105 USA.
Smithsonian Inst, USDA, Systemat Entomol Lab, Washington, DC 20560 USA.
RP Ashworth, AC (reprint author), N Dakota State Univ, Dept Geosci, Fargo, ND 58105 USA.
NR 11
TC 19
Z9 19
U1 0
U2 7
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 8
PY 2003
VL 423
IS 6936
BP 135
EP 136
DI 10.1038/423135a
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 675MR
UT WOS:000182699600033
PM 12736672
ER
PT J
AU Bice, KL
Huber, BT
Norris, RD
AF Bice, KL
Huber, BT
Norris, RD
TI Extreme polar warmth during the Cretaceous greenhouse? Paradox of the
late Turonian delta O-18 record at Deep Sea Drilling Project Site 511
SO PALEOCEANOGRAPHY
LA English
DT Article
DE carbon dioxide; Cretaceous; Turonian; oxygen isotopes; modeling;
salinity
ID STRONTIUM-ISOTOPE STRATIGRAPHY; SOUTHWEST ATLANTIC; OXYGEN-ISOTOPE;
PLANKTONIC-FORAMINIFERA; FALKLAND PLATEAU; OCEAN; ANTARCTICA; LEG-71;
PRECIPITATION; EVOLUTION
AB [1] Oxygen isotope data for upper Turonian planktonic foraminifera at Deep Sea Drilling Project Site 511 (Falkland Plateau, 60degreesS paleolatitude) exhibit an similar to2parts per thousand excursion to values as low as -4.66parts per thousand (Vienna Peedee belemnite standard; PDB) coincident with the warmest tropical temperature estimates yet obtained for the open ocean. The lowest planktonic foraminifer delta(18)O values suggest that the upper ocean was as warm as 30-32degreesC. This is an extraordinary temperature for 60degreesS latitude but is consistent with temperatures estimated from apparently coeval mollusc delta(18)O from nearby James Ross Island (65 p S paleolatitude). Glassy textural preservation, a well-defined depth distribution in Site 511 planktonics, low sediment burial temperature (similar to32degreesC), and lack of evidence of highly depleted pore waters argue against diagenesis (even solid state diffusion) as the cause of the very depleted planktonic values. The lack of change in benthic foraminifer delta(18)O suggests brackish water capping as the mechanism for the low planktonic delta(18)O values. However, mixing ratio calculations show that the amount of freshwater required to produce a 2% shift in ambient water would drive a 7 psu decrease in salinity. The abundance and diversity of planktonic foraminifera and nannofossils, high planktonic: benthic ratios, and the appearance of keeled foraminifera argue against lower-than-normal marine salinities. Isotope calculations and climate models indicate that we cannot call upon more depleted freshwater delta(18)O to explain this record. Without more late Turonian data, especially from outside the South Atlantic basin, we can currently only speculate on possible causes of this paradoxical record from the core of the Cretaceous greenhouse.
C1 Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA.
Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA.
RP Bice, KL (reprint author), Woods Hole Oceanog Inst, Dept Geol & Geophys, Mail Stop 23, Woods Hole, MA 02543 USA.
NR 45
TC 44
Z9 46
U1 0
U2 6
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0883-8305
J9 PALEOCEANOGRAPHY
JI Paleoceanography
PD MAY 7
PY 2003
VL 18
IS 2
AR 1031
DI 10.1029/2002PA000848
PG 13
WC Geosciences, Multidisciplinary; Oceanography; Paleontology
SC Geology; Oceanography; Paleontology
GA 678QN
UT WOS:000182878100001
ER
PT J
AU Drake, JJ
Marshall, HL
AF Drake, JJ
Marshall, HL
TI Is RXJ1856.5-3754 a strange quark star?
SO NUCLEAR PHYSICS A
LA English
DT Article; Proceedings Paper
CT 7th International Symposium on Nuclei in the Cosmos (NIC7)
CY JUL 08-12, 2002
CL FUJI, JAPAN
SP Todai Int Symp, Univ Tokyo, Int Symp Minist Educ, Culture, Spoets, Sci & Technol, Commemorat Assoc Japan World Exposit 1970, Japan Soc Promot Sci, Inoue Fdn Sci, Kajima Fdn, Natl Astronom Observ Japan
ID ISOLATED NEUTRON-STAR; X-RAY-SPECTRUM; RX J1856.5-3754; RADIO PULSARS;
RX-J1856.5-3754; J185635-3754; EQUATION
AB Deep Chandra LETGS observations Of the isolated neutron star candidate RXJ1856.5-3754 have demonstrated that, to within the accuracy of the observations, the X-ray spectrum is consistent with a blackbody with a temperature of 7 x 10(5) K and a radiation radius R-infinity similar to 5 km-much too small for current neutron star equations of state. The small apparent radius, lack of X-ray pulsations down to a level of 3%, and failure to explain the observations in terms of current neutron star models, lead to the suggestion that R-XJ1856.5-3754 might be a strange quark star. We discuss some issues associated with this interpretation and look briefly at RX J1856.5-3754 in the context of other strange star candidates and recent Chandra observations of neutron stars that appear to have smooth featureless spectra. Both X-ray and optical spectra of some of these objects might be explained by "naked" crusted neutron stars or strange quark stars with thin coronae. RX J1856.5-3754 remains an interesting strange quark star candidate.
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
RP Drake, JJ (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA.
NR 39
TC 2
Z9 2
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0375-9474
J9 NUCL PHYS A
JI Nucl. Phys. A
PD MAY 5
PY 2003
VL 718
BP 351C
EP 358C
DI 10.1016/S0375-9474(03)00738-3
PG 8
WC Physics, Nuclear
SC Physics
GA 668VR
UT WOS:000182314300053
ER
PT J
AU Post, JE
Heaney, PJ
Von Dreele, RB
Hanson, JC
AF Post, JE
Heaney, PJ
Von Dreele, RB
Hanson, JC
TI Neutron and temperature-resolved synchrotron X-ray powder diffraction
study of akaganeite
SO AMERICAN MINERALOGIST
LA English
DT Article
ID BETA-FEOOH; RIETVELD REFINEMENT; THERMAL-DECOMPOSITION
AB Rietveld refinements using neutron powder diffraction data were used to locate H atom positions and obtain a more precise crystal structure refinement for akaganeite [Fe7.63+Ni0.42+O6.35 (OH)(9.65)Cl(1.25)(.)nH(2)O]. Difference Fourier maps clearly showed H atoms positions near those O atoms at the midpoints of the tunnel edges. The O-H vectors point toward the Cl sites at the center of the tunnel, and weak hydrogen bonds likely form between the framework 0 atoms and Cl. The Cl position is near the center of a prism defined by the eight hydroxyl H atoms. The Cl atoms fill similar to2/3 of the tunnel sites, suggesting an ordering scheme in a given tunnel with every third tunnel site vacant. Such an arrangement allows the Cl anions to increase their separation distance along a tunnel by displacing away from one another toward their respective adjacent vacancies. The Fe-O octahedra in akaganeite are distorted with Fe-(O, OH) distances ranging from 1.94 to 2.13 Angstrom and show three longer and three shorter Fe-O distances; as expected the longer distances are associated with the OH- anions.
Temperature-resolved synchrotron X-ray powder diffraction data and Rietveld refinements were used to investigate changes in the akagandite structure and its transformation into hematite as it was heated from 26 to 800 degreesC. Rietveld refinements revealed surprising consistency in all unit-cell parameters between room temperature and similar to225 degreesC, resulting in nearly zero thermal expansion of the akaganeite structure over a 200 degreesC interval. Above similar to225 degreesC, the unit-cell volume gradually decreased, primarily in response to decreases in c and b, and an increase in the P angle. The a parameter remained nearly constant until similar to225 degreesC and increased thereafter. Akaganeite started to transform to hematite in the temperature range 290 to 310 degreesC with no evidence for maghemite as an intermediate phase.
C1 Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
Los Alamos Natl Lab, LANSCE 12, Los Alamos, NM 87545 USA.
Brookhaven Natl Lab, Dept Chem, Upton, NY 11793 USA.
RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
RI Hanson, jonathan/E-3517-2010
NR 26
TC 66
Z9 66
U1 3
U2 13
PU MINERALOGICAL SOC AMER
PI WASHINGTON
PA 1015 EIGHTEENTH ST, NW SUITE 601, WASHINGTON, DC 20036 USA
SN 0003-004X
J9 AM MINERAL
JI Am. Miner.
PD MAY-JUN
PY 2003
VL 88
IS 5-6
BP 782
EP 788
PG 7
WC Geochemistry & Geophysics; Mineralogy
SC Geochemistry & Geophysics; Mineralogy
GA 677XY
UT WOS:000182835600007
ER
PT J
AU Reed, DH
O'Grady, JJ
Ballou, JD
Frankham, R
AF Reed, DH
O'Grady, JJ
Ballou, JD
Frankham, R
TI The frequency and severity of catastrophic die-offs in vertebrates
SO ANIMAL CONSERVATION
LA English
DT Article
ID DYNAMICS; STOCHASTICITY; CONSERVATION; VARIABILITY; HURRICANE; ECOLOGY;
MAMMALS; TERM
AB Rare bouts of extreme environmental perturbations (catastrophes) have been predicted to have a major influence on the probability of extinction. Yet very little information is available on the frequency and severity of catastrophes. Improving the available information concerning catastrophe parameters would allow for an evaluation of their effect and a start towards understanding their causes. We used the Global Population Dynamics Database to determine the frequency and severity of die-offs in 88 species of vertebrates. We define a catastrophe as any 1-year decrease in population size of 50% or greater. The data yielded three findings. (1) The frequency of severe die-offs in vertebrate populations is strongly related to the generation length of the organism. (2) The probability of a severe die-off for a particular population is approximately 14% per generation. (3) The frequency of die-off severity can be modelled as a modified power function with the frequency of die-offs decreasing with increasing magnitude of effect. The distribution is not consistent with catastrophes stemming from environmental sources different than those responsible for smaller fluctuations, but seems to represent the tail of a continuous distribution of environmental perturbations.
C1 Smithsonian Inst, Natl Zool Pk, Conservat & Res Ctr, Dept Conservat Biol, Washington, DC 20008 USA.
RP Reed, DH (reprint author), Univ Mississippi, Dept Biol, POB 1848, University, MS 38677 USA.
NR 23
TC 63
Z9 64
U1 4
U2 28
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 1367-9430
J9 ANIM CONSERV
JI Anim. Conserv.
PD MAY
PY 2003
VL 6
BP 109
EP 114
DI 10.1017/S1367943003003147
PN 2
PG 6
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 688XB
UT WOS:000183461600003
ER
PT J
AU Karanth, KU
Nichols, JD
Seidensticker, J
Dinerstein, E
Smith, JLD
McDougal, C
Johnsingh, AJT
Chundawat, RS
Thapar, V
AF Karanth, KU
Nichols, JD
Seidensticker, J
Dinerstein, E
Smith, JLD
McDougal, C
Johnsingh, AJT
Chundawat, RS
Thapar, V
TI Science deficiency in conservation practice: the monitoring of tiger
populations in India
SO ANIMAL CONSERVATION
LA English
DT Article
ID LEOPARD; DHOLE
AB Conservation practices are supposed to get refined by advancing scientific knowledge. We study this phenomenon in the context of monitoring tiger populations in India, by evaluating the 'pugmark census method' employed by wildlife managers for three decades. We use an analytical framework of modern animal population sampling to test the efficacy of the pugmark censuses using scientific data on tigers and our field observations. We identify three critical goals for monitoring tiger populations, in order of increasing sophistication: (1) distribution mapping, (2) tracking relative abundance, (3) estimation of absolute abundance. We demonstrate that the present census-based paradigm does not work because it ignores the first two simpler goals, and targets, but fails to achieve, the most difficult third goal. We point out the utility and ready availability of alternative monitoring paradigms that deal with the central problems of spatial sampling and observability. We propose an alternative sampling-based approach that can be tailored to meet practical needs of tiger monitoring at different levels of refinement.
C1 Wildlife Conservat Soc, Int Program, Bronx, NY 10460 USA.
US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA.
Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA.
World Wildlife Fund, Washington, DC 20037 USA.
Univ Minnesota, Dept Fisheries & Wildlife, St Paul, MN 55108 USA.
Tiger Tops, Kathmandu, Nepal.
Wildlife Inst India, Dehra Dun 248001, Uttar Pradesh, India.
RP Karanth, KU (reprint author), 26-2,Aga Abbas Ali Rd,Apt 403, Bangalore 560042, Karnataka, India.
NR 40
TC 66
Z9 72
U1 3
U2 26
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 1367-9430
J9 ANIM CONSERV
JI Anim. Conserv.
PD MAY
PY 2003
VL 6
BP 141
EP 146
DI 10.1017/S1367943003003184
PN 2
PG 6
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 688XB
UT WOS:000183461600007
ER
PT J
AU Uson, JM
Matthews, LD
AF Uson, JM
Matthews, LD
TI HI imaging observations of superthin galaxies. I. UGC 7321
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies : individual (UGC 7321); galaxies : ISM; galaxies : kinematics
and dynamics; galaxies : spiral; ISM : HI
ID SURFACE BRIGHTNESS GALAXIES; DARK-MATTER HALOS; EDGE-ON GALAXIES;
NEUTRAL HYDROGEN OBSERVATIONS; TIDAL DWARF GALAXY; SPIRAL GALAXIES;
ROTATION CURVES; GALACTIC DISKS; STAR-FORMATION; INTERSTELLAR-MEDIUM
AB We have used the Very Large Array to image the isolated "superthin'' galaxy UGC 7321 in the H I line with a spatial resolution of 16" and a spectral resolution of 24 kHz (5.2 km s(-1)). We have reached a sensitivity of (0.36-0.40) mJy beam(-1) channel(-1), which correspond to a column density of (8-9) x 10(18) atoms cm(-2) (1 sigma). UGC 7321 has a gas-rich disk, with M-HI = (1.06 +/- 0.01) x 10(9) d(10)(2) M-. and M-H I/ L-B = 1.0 (d(10) is the distance to UGC 7321 in units of 10 Mpc, the value adopted in this paper), and no detectable radio continuum emission (F-CONT = 0.41 +/- 0.25 mJy). The global H I distribution of UGC 7321 is rather symmetric and extends to similar to1.5 times the optical radius (D-H I = 8.'65 +/- 0.'15 at n(HI) = 3 x 10(19) atoms cm(-2)). An "integral sign'' warp is observed in the H I disk, commencing near the edge of the stellar distribution and twisting back toward the equatorial plane in the outermost regions. In addition, the position-velocity diagram suggests the presence of a bar or inner arm within similar to40" from the center. The rotation curve of UGC 7321 is slowly rising; it reaches its asymptotic velocity of similar to110 km s(-1) at similar to2.'5 from the center ( about 0.9 optical radii) and declines near the edge of the H I disk. The ratio of the inferred dynamical mass to the mass in gas and stars is similar to12d(10)(-1) implying that UGC 7321 is a highly dark-matter-dominated galaxy.
C1 Natl Radio Astron Observ, Charlottesville, VA 22903 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Uson, JM (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA.
NR 78
TC 38
Z9 40
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2003
VL 125
IS 5
BP 2455
EP 2472
DI 10.1086/374627
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 669VU
UT WOS:000182371800013
ER
PT J
AU Cohen, M
Megeath, ST
Hammersley, PL
Martin-Luis, F
Stauffer, J
AF Cohen, M
Megeath, ST
Hammersley, PL
Martin-Luis, F
Stauffer, J
TI Spectral irradiance calibration in the infrared. XIII. "Supertemplates''
and on-orbit calibrators for the SIRTF Infrared Array Camera
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared radiation; methods : analytical; stars : late-type; techniques
: spectroscopic
ID MIDCOURSE SPACE EXPERIMENT; PHOTOMETRIC STANDARD STARS; MU-M SPECTRA;
INTERSTELLAR EXTINCTION; ULTRAVIOLET EXTINCTION; MODEL ATMOSPHERES;
CELESTIAL EQUATOR; STELLAR SPECTRA; TEMPERATURE; PASSBANDS
AB We describe the technique that will be used to develop a set of on-orbit calibrators for the Infrared Array Camera (IRAC) and demonstrate the validity of the method for stars with spectral types either K0-M0 III or A0-A5 V. For application to SIRTF, the approach is intended to operate with all available optical, near-infrared (NIR), and mid-infrared (MIR) photometry and to yield complete absolute spectra from UV to MIR. One set of stars is picked from Landolt's extensive network of optical (UBVRI) calibrators, the other from the Carter-Meadows set of faint IR standards. Traceability to the "Cohen-Walker-Witteborn'' framework of absolute photometry and stellar spectra is assured. The method is based on the use of either "supertemplates,'' which represent the intrinsic shapes of the spectra of K0-M0 III stars from far-UV (1150 Angstrom) to MIR (35 mum) wavelengths, or Kurucz synthetic spectra for A0-A5 V stars. Each supertemplate or Kurucz model is reddened according to the individual star's extinction and is normalized using available characterized optical photometry. This paper tests our capability to predict NIR (JHK) magnitudes using supertemplates or models constrained by Hipparcos/Tycho or precision ground-based optical data. We provide absolutely calibrated 0.275-35.00 mum spectra of 33 Landolt and Carter-Meadows optical standard stars to demonstrate the viability of this technique, and to offer a set of IR calibrators 100-1000 times fainter than those we have previously published. As an indication of what we can expect for actual IRAC calibration stars, we have calculated the absolute uncertainties associated with predicting the IRAC magnitudes for the faintest cool giant and hot dwarf in this new set of calibration stars.
C1 Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Astrofis Canarias, E-38200 Tenerife, Spain.
CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA.
RP Cohen, M (reprint author), Univ Calif Berkeley, Radio Astron Lab, 601 Campbell Hall, Berkeley, CA 94720 USA.
NR 54
TC 152
Z9 152
U1 0
U2 4
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2003
VL 125
IS 5
BP 2645
EP 2663
DI 10.1086/374362
PG 19
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 669VU
UT WOS:000182371800028
ER
PT J
AU Franklin, FA
Soper, PR
AF Franklin, FA
Soper, PR
TI Some effects of mean motion resonance passage on the relative migration
of Jupiter and Saturn
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE minor planets, asteroids; planets and satellites : general; planets and
satellites : individual (Jupiter, Saturn); solar system : formation;
solar system : general
ID PLANETS; SYSTEM
AB We look for clues to the amount and direction of Saturn's migration relative to Jupiter in their current orbits, specifically, from the fact that the former lies barely sunward of their 5 : 2 mean motion resonance. Numerical simulations suggest that Saturn has moved in the same direction (presumably inward) as has Jupiter but that the pair has never passed through their more distant 3 : 1 resonance. Thus, their relative migration has been less than about 1.5 AU. Passage through 5 : 2 is consistent with their current orbits and could have contributed to their present eccentricities, e (and especially to their large periodic variations), but it probably cannot generate their e's if both, and particularly Jupiter's, were initially less than about 0.03. In fact, it is most likely that their initial e's were both close to the current values. Very long term capture into 5 : 2 for the Sun-Jupiter-Saturn case occurs with a remarkably high frequency.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Massachusetts Lowell, Lowell, MA 01854 USA.
RP Franklin, FA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 11
TC 5
Z9 5
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAY
PY 2003
VL 125
IS 5
BP 2678
EP 2691
DI 10.1086/374228
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 669VU
UT WOS:000182371800030
ER
PT J
AU Testi, L
Natta, A
Shepherd, DS
Wilner, DJ
AF Testi, L
Natta, A
Shepherd, DS
Wilner, DJ
TI Large grains in the disk of CQ Tau
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars : planetary systems : protoplanetary disks; stars : planetary
systems : formation; stars : formation; stars : individual : CQ Tauri
ID SPECTRAL ENERGY-DISTRIBUTIONS; INTERMEDIATE-MASS STARS; HERBIG AE
SYSTEMS; T-TAURI; CIRCUMSTELLAR DISKS; PROTOPLANETARY DISKS; ACCRETION
DISKS; HIGH-RESOLUTION; DUST; MODEL
AB We present 7 mm observations of the dusty disk surrounding the 10 Myr old 1.5 M(.) pre-main-sequence star CQ Tauri obtained at the Very Large Array with 0.8 arcsec resolution and 0.1 mJy rms sensitivity. These observations resolve the 7 mm emission in approximately the north-south direction, confirming previous results obtained with lower resolution. We use a two-layer flared disk model to interpret the observed fluxes from 7 mm to 1.3 mm together with the resolved 7 mm structure. We find that the disk radius is constrained to the range 100 to 300 AU, depending on the steepness of the disk surface density distribution. The power law index of the dust opacity coefficient, beta, is constrained to be 0.5 to 0.7. Since the models indicate that the disk is optically thin at millimeter wavelengths for radii greater than 8 AU, the contribution of an optically thick region to the emission is less than 10%. This implies that high optical depth or complex disk geometry cannot be the cause of the observed shallow millimeter spectral index. Instead, the new analysis supports the earlier suggestion that dust particles in the disk have grown to sizes as large as a few centimeters. The dust in the CQ Tauri system appears to be evolved much like that in the TW Hydra system, a well-studied pre-main-sequence star of similar age and lower mass. The survival of gas-rich disks with incomplete grain evolution at such old ages deserves further investigations.
C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Testi, L (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM lt@arcetri.astro.it
NR 31
TC 122
Z9 123
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2003
VL 403
IS 1
BP 323
EP 328
DI 10.1051/0004-6361:20030362
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 673CC
UT WOS:000182561100034
ER
PT J
AU Moy, E
Barmby, P
Rigopoulou, D
Huang, JS
Willner, SP
Fazio, GG
AF Moy, E
Barmby, P
Rigopoulou, D
Huang, JS
Willner, SP
Fazio, GG
TI H-band observations of the Chandra Deep Field South
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE catalogs; surveys; infrared : general; galaxies : general; stars :
general; cosmology : observations
ID CAMPANAS INFRARED SURVEY; HIGH-REDSHIFT GALAXIES; ESO IMAGING SURVEY;
PHOTOMETRIC REDSHIFTS; NUMBER COUNTS; SELECTION; EVOLUTION; CATALOG
AB We report results of our H-band survey of the Chandra Deep Field South (CDFS). The observations, made with SofI on the NTT, cover 0.027 square degrees to H < 20.5 and 0.17 square degrees to H < 19.8 ( 50% completeness limits). In total, 4819 objects were detected, of which 80% are galaxies based on the SExtractor parameter "stellarity index" having a value less than 0.5. Our astrometric solutions are in good agreement with those of the Las Campanas Infrared Survey (LCIRS), the COMBO-17, and the ESO-EIS surveys. Our photometry compares satisfactorily with the LCIRS results as well as with GOODS data. Galaxy number counts are similar to50 000 galaxies per square degree at H < 20.75, in good agreement with those of LCIRS. The object catalog is published electronically at the CDS**.
C1 Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Moy, E (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312, D-85741 Garching, Germany.
EM moy@discovery.saclay.cea.fr
RI Barmby, Pauline/I-7194-2016
OI Barmby, Pauline/0000-0003-2767-0090
NR 30
TC 22
Z9 22
U1 0
U2 1
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2003
VL 403
IS 2
BP 493
EP 499
DI 10.1051/0004-6361:20030245
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 675DY
UT WOS:000182678800015
ER
PT J
AU Durret, F
Neto, GBL
Forman, W
Churazov, E
AF Durret, F
Neto, GBL
Forman, W
Churazov, E
TI An XMM-Newton view of the extended "filament" near the cluster of
galaxies Abell 85
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies : clusters : individual : Abell 85; X-rays : galaxies :
clusters
ID RAY; EVOLUTION
AB We have observed with XMM-Newton the extended 4 Mpc filament detected by the ROSAT PSPC in the neighbourhood of the cluster of galaxies Abell 85. We confirm that there is an extended feature, aligned at the same position angle as the major axis of the central cD, the bright cluster galaxies, and nearby groups and clusters. We find that the X-ray emission from the filament is best described by thermal emission with a temperature of similar to2 keV, which is significantly lower than the ambient cluster medium, but is significantly higher than anticipated for a gas in a weakly bound extended filament. It is not clear whether this is a filament of diffuse emission, a chain of several groups of galaxies, or stripped gas from the infalling south blob.
C1 CNRS, Inst Astrophys Paris, F-75014 Paris, France.
Univ Sao Paulo, Inst Astron Geofis & C Atmosf, BR-05508090 Sao Paulo, Brazil.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP CNRS, Inst Astrophys Paris, 98 Bis Bd Arago, F-75014 Paris, France.
EM durret@iap.fr
RI Churazov, Eugene/A-7783-2013; Lima Neto, Gastao/J-6117-2014;
OI Forman, William/0000-0002-9478-1682
NR 20
TC 32
Z9 32
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 1432-0746
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2003
VL 403
IS 2
BP L29
EP L32
DI 10.1051/0004-6361:20030424
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 675DY
UT WOS:000182678800002
ER
PT J
AU Ovaldsen, JE
Teuber, J
Schild, RE
Stabell, R
AF Ovaldsen, JE
Teuber, J
Schild, RE
Stabell, R
TI New aperture photometry of QSO 0957+561; application to time delay and
microlensing
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE gravitational lensing; quasars : individual : QSO 0957+561; techniques :
photometric; methods : data analysis
ID QUASAR Q0957+561; LIGHT CURVES; OPTICAL-DATA; QSO-0957+561; VARIABILITY;
LIGHTCURVES; PARAMETERS; FEATURES; IMAGES; LENS
AB We present a re-reduction of archival CCD frames of the doubly imaged quasar 0957 + 561 using a new photometry code. Aperture photometry with corrections for both cross contamination between the quasar images and galaxy contamination is performed on about 2650 R-band images from a five year period (1992-1997). From the brightness data a time delay of 424.9 +/- 1.2 days is derived using two different statistical techniques. The amount of gravitational microlensing in the quasar light curves is briefly investigated, and we find unambiguous evidence of both long term and short term microlensing. We also note the unusual circumstance regarding time delay estimates for this gravitational lens. Estimates by different observers from different data sets or even with the same data sets give lag estimates differing by typically 8 days, and error bars of only a day or two. This probably indicates several complexities where the result of each estimate depends upon the details of the calculation.
C1 Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
Ctr Adv Signal Proc, Copenhagen, Denmark.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Ovaldsen, JE (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
NR 35
TC 20
Z9 20
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAY
PY 2003
VL 402
IS 3
BP 891
EP 904
DI 10.1051/0004-6361:20030145
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EH
UT WOS:000182452000019
ER
PT J
AU Furlanetto, SR
Loeb, A
AF Furlanetto, SR
Loeb, A
TI Metal absorption lines as probes of the intergalactic medium prior to
the reionization epoch
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology : theory; galaxies : high-redshift; intergalactic medium;
quasars : absorption lines
ID LY-ALPHA FOREST; GAMMA-RAY BURSTS; GALACTIC WINDS; HIGH-REDSHIFT;
INTERSTELLAR-MEDIUM; DWARF GALAXIES; STAR-FORMATION; DRIVEN SUPERWINDS;
ENRICHMENT; UNIVERSE
AB Winds from star-forming galaxies provide the most promising explanation for the enrichment of the inter-galactic medium with heavy elements. Theoretical and observational arguments indicate that the pollution may have occurred at z greater than or similar to 6; however, direct observational tests of such a scenario are needed. We model star-burst winds in the high-redshift universe and find that the fraction of space filled by enriched material varies strongly with the assumed star formation efficiency f(*) and the fraction of supernova energy powering each wind f(esc). We show that metals carried by these winds can be seen in absorption against bright background sources, such as quasars or gamma-ray bursts, in narrow lines with characteristic equivalent widths similar to0.5 Angstrom less than or similar to W less than or similar to 5 Angstrom. We argue that a substantial fraction of the metals in high-redshift winds are likely to reside in low-ionization states (C II, O I, Si II, and Fe II), but higher ionization states (C IV and Si IV) could also provide useful probes of the winds. The number of such lines can constrain both f(*) and f(esc). Statistics of metal absorption lines can also be used to identify whether H-2 is an efficient coolant in the early universe and to study the initial mass function of stars at high redshifts.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Adv Study, Princeton, NJ 08540 USA.
RP Furlanetto, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 91
TC 89
Z9 89
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 18
EP 34
DI 10.1086/374045
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800003
ER
PT J
AU Shapley, AE
Steidel, CC
Pettini, M
Adelberger, KL
AF Shapley, AE
Steidel, CC
Pettini, M
Adelberger, KL
TI Rest-frame ultraviolet spectra of z similar to 3 Lyman break galaxies
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
ID STAR-FORMING GALAXIES; HUBBLE DEEP FIELD; RESOLUTION IMAGING
SPECTROMETER; SPACE-TELESCOPE SPECTROSCOPY; LY-ALPHA; REDSHIFT
Z-SIMILAR-TO-3; STARBURST GALAXIES; CONTINUUM EMISSION; LUMINOSITY
DENSITY; STELLAR YIELDS
AB We present the results of a systematic study of the rest-frame UV spectroscopic properties of Lyman break galaxies (LBGs). The database of almost 1000 LBG spectra proves useful for constructing high signal-to-noise composite spectra. The composite spectrum of the entire sample reveals a wealth of features attributable to hot stars, H II regions, dust, and out. owing neutral and ionized gas. By grouping the database according to galaxy parameters such as Lyalpha equivalent width, UV spectral slope, and interstellar kinematics, we isolate some of the major trends in LBG spectra that are least compromised by selection effects. We find that LBGs with stronger Lyalpha emission have bluer UV continua, weaker low-ionization interstellar absorption lines, smaller kinematic offsets between Lyalpha and the interstellar absorption lines, and lower star formation rates. There is a decoupling between the dependence of low- and high-ionization outflow features on other spectral properties. Additionally, galaxies with rest-frame W-Lyalpha greater than or equal to 20 Angstrom in emission have weaker than average high-ionization lines and nebular emission lines that are significantly stronger than in the sample as a whole. Most of the above trends can be explained in terms of the properties of the large-scale outflows seen in LBGs. According to this scenario, the appearance of LBG spectra is determined by a combination of the covering fraction of out. owing neutral gas, which contains dust and the range of velocities over which this gas is absorbing. In contrast, the strengths of collisionally excited nebular emission lines should not be affected by the nature of the outflow, and variations in these lines may indicate differences in the temperatures and metallicities in H II regions of galaxies with very strong Lyalpha emission. Higher sensitivity and spectral resolution observations are still required for a full understanding of the covering fraction and velocity dispersion of the out. owing neutral gas in LBGs and its relationship to the escape fraction of Lyman continuum radiation in galaxies at z similar to 3.
C1 CALTECH, Pasadena, CA 91125 USA.
Inst Astron, Cambridge CB3 0HE, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA.
RP Shapley, AE (reprint author), CALTECH, MS 105-24, Pasadena, CA 91125 USA.
NR 81
TC 843
Z9 843
U1 2
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 65
EP 89
DI 10.1086/373922
PN 1
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800006
ER
PT J
AU Bechtold, J
Siemiginowska, A
Shields, J
Czerny, B
Janiuk, A
Hamann, F
Aldcroft, TL
Elvis, M
Dobrzycki, A
AF Bechtold, J
Siemiginowska, A
Shields, J
Czerny, B
Janiuk, A
Hamann, F
Aldcroft, TL
Elvis, M
Dobrzycki, A
TI Chandra survey of radio-quiet, high-redshift quasars
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE accretion, accretion disks; intergalactic medium; quasars : general;
X-rays : galaxies
ID ACTIVE GALACTIC NUCLEI; X-RAY-PROPERTIES; DOMINATED ACCRETION FLOWS;
BAND ENERGY-DISTRIBUTION; OPTICALLY SELECTED QSOS; ROSAT DETECTED
QUASARS; PALOMAR SKY SURVEY; BLACK-HOLES; Z-GREATER-THAN-4 QUASARS;
ABSORPTION SYSTEMS
AB We observed 17 optically selected, radio-quiet, high-redshift quasars with the Chandra ACIS and detected 16 of them. The quasars have redshifts between 3.70 and 6.28 and include the highest-redshift quasars known. When compared with low-redshift quasars observed with ROSAT, these high-redshift quasars are significantly more X-ray-quiet. We also find that the X-ray spectral index of the high-redshift objects is flatter than the average at lower redshift. These trends confirm the predictions of models in which the accretion flow is described by a cold, optically thick accretion disk surrounded by a hot, optically thin corona, provided the viscosity parameter alpha greater than or equal to 0.02. The high-redshift quasars have supermassive black holes, with masses of similar to10(10) M-circle dot, and are accreting material at similar to0.1 times the Eddington limit. We detect 10 X-ray photons from the z = 6.28 quasar SDSS 1030+0524, which might have a Gunn-Peterson trough and be near the redshift of reionization of the intergalactic medium. The X-ray data place an upper limit on the optical depth of the intergalactic medium, tau(IGM) < 10(6), compared to the lower limit from the spectrum of Lyα and Lyβ, which implies τ(IGM) > 20.
C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA.
Nicholaus Copernicus Astron Ctr, Warsaw, Poland.
Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA.
RP Bechtold, J (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA.
RI Czerny, Bozena/A-2363-2015
OI Czerny, Bozena/0000-0001-5848-4333
NR 101
TC 69
Z9 70
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 119
EP 127
DI 10.1086/378724
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800010
ER
PT J
AU Fabbiano, G
Elvis, M
Markoff, S
Siemiginowska, A
Pellegrini, S
Zezas, A
Nicastro, F
Trinchieri, G
McDowell, J
AF Fabbiano, G
Elvis, M
Markoff, S
Siemiginowska, A
Pellegrini, S
Zezas, A
Nicastro, F
Trinchieri, G
McDowell, J
TI The X-ray-faint emission of the supermassive nuclear black hole of IC
1459
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; black hole physics; galaxies : individual
(IC 1459); galaxies : nuclei
ID EARLY-TYPE GALAXIES; ACTIVE GALACTIC NUCLEI; ADVECTION-DOMINATED
ACCRETION; IONIZED-GAS; RADIO GALAXIES; COUNTERROTATING CORE;
SEYFERT-GALAXIES; SPECTRAL MODELS; FLOWS; DISK
AB Chandra observations of the supermassive black hole in the nucleus of IC 1459 show a weak (L-X = 8 x 10(40) ergs s(-1), 0.3-8 keV), unabsorbed nuclear X-ray source, with a slope Gamma = 1.88 +/- 0.09, and no strong Fe K line at 6.4 keV (EW < 382 eV). This describes a normal active galactic nucleus (AGN) X-ray spectrum but lies at 3 x 10(-7) below the Eddington limit. The spectral energy distribution of the IC 1459 nucleus is extremely radio-loud compared to normal radio-loud quasars. The nucleus is surrounded by a hot interstellar medium (kT &SIM; 0.5-0.6 keV) with an average density of 0.3 cm(-3), within the central &SIM;180 pc radius, which is comparable to the gravitational capture radius, r(A) &SIM; 140 pc. We estimate that for a standard AGN efficiency of 10%, the Bondi accretion would correspond to a luminosity of &SIM;6 x 10(44) ergs s(-1), nearly 4 orders of magnitude higher than L-X. ADAF solutions can explain the X-ray spectrum, but not the high radio/X-ray ratio. A jet model fits the radio-100 μm and X-ray spectra well. The total power in this jet is &SIM;10% of L-Bondi, implying that accretion close to the Bondi rate is needed.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
Univ Bologna, Dipartimento Astron, I-40126 Bologna, Italy.
Osserv Astron Brera, I-20121 Milan, Italy.
RP Fabbiano, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Zezas, Andreas/C-7543-2011;
OI Zezas, Andreas/0000-0001-8952-676X; Nicastro,
Fabrizio/0000-0002-6896-1364
NR 87
TC 49
Z9 49
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 175
EP 185
DI 10.1086/374040
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800015
ER
PT J
AU Gaensler, BM
Schulz, NS
Kaspi, VM
Pivovaroff, MJ
Becker, WE
AF Gaensler, BM
Schulz, NS
Kaspi, VM
Pivovaroff, MJ
Becker, WE
TI XMM-Newton observations of PSR B1823-13: An asymmetric synchrotron
nebula around a Vela-like pulsar
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : individual (G18.0-0.7); pulsars : individual (PSR B1823-13) stars
: neutron; supernova remnants; X-rays : ISM
ID X-RAY OBSERVATIONS; WIND-DRIVEN BUBBLES; SUPERNOVA REMNANT;
NEUTRON-STARS; YOUNG PULSARS; BOW-SHOCK; EMISSION; SHELL; EVOLUTION;
CRAB
AB We present a deep observation with the X-Ray Multimirror Mission of PSR B1823-13, a young pulsar with similar properties to the Vela pulsar. We detect two components to the X-ray emission associated with PSR B1823-13: an elongated core of extent 3000 immediately surrounding the pulsar embedded in a fainter, diffuse component of emission 50 in extent, seen only on the southern side of the pulsar. The pulsar itself is not detected, either as a point source or through its pulsations. Both components of the X-ray emission are well fitted by a power-law spectrum, with photon index Gamma approximate to 1.6 and X-ray luminosity (0.5-10 keV) L-X approximate to 9 x 10(32) ergs s(-1) for the core and Gamma approximate to 2.3 and L-X approximate to 3 x 10(33) ergs s(-1) for the diffuse emission, for a distance of 4 kpc. We interpret both components of emission as corresponding to a pulsar wind nebula, which we designate G18.0-0.7. We argue that the core region represents the wind termination shock of this nebula, while the diffuse component indicates the shocked downstream wind. We propose that the asymmetric morphology of the diffuse emission with respect to the pulsar is the result of a reverse shock from an associated supernova remnant, which has compressed and distorted the pulsar-powered nebula. Such an interaction might be typical for pulsars at this stage in their evolution. The associated supernova remnant is not detected directly, most likely being too faint to be seen in existing X-ray and radio observations.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA.
Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
RP Gaensler, BM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-6, Cambridge, MA 02138 USA.
RI Gaensler, Bryan/F-8655-2010; Pivovaroff, Michael/M-7998-2014;
OI Pivovaroff, Michael/0000-0001-6780-6816; Gaensler,
Bryan/0000-0002-3382-9558
NR 54
TC 71
Z9 72
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 441
EP 451
DI 10.1086/368356
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800037
ER
PT J
AU Heinke, CO
Grindlay, JE
Lloyd, DA
Edmonds, PD
AF Heinke, CO
Grindlay, JE
Lloyd, DA
Edmonds, PD
TI X-ray studies of two neutron stars in 47 tucanae: Toward constraints on
the equation of state
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE accretion, accretion disks; binaries : close; binaries : eclipsing;
globular clusters : individual (NGC 104); stars : neutron; X-rays :
binaries
ID GLOBULAR-CLUSTER 47-TUCANAE; THERMAL EMISSION; CENTAURUS X-4;
BLACK-HOLE; AQUILA X-1; ROSAT OBSERVATIONS; MODEL ATMOSPHERES;
XMM-NEWTON; QUIESCENCE; MASS
AB We report spectral and variability analysis of two quiescent low-mass X-ray binaries (X5 and X7, previously detected with the ROSAT HRI) in a Chandra ACIS-I observation of the globular cluster 47 Tuc. X5 demonstrates sharp eclipses with an 8.666 +/- 0.01 hr period, as well as dips showing an increased N-H column. The thermal spectra of X5 and X7 are well modeled by unmagnetized hydrogen atmospheres of hot neutron stars. No hard power-law component is required. A possible edge or absorption feature is identified near 0.64 keV, perhaps an O V edge from a hot wind. Spectral fits imply that X7 is significantly more massive than the canonical 1.4 M-circle dot neutron star mass, with M > 1: 8 M-circle dot for a radius range of 9-14 km, while X5's spectrum is consistent with a neutron star of mass 1.4 M-circle dot for the same radius range. Alternatively, if much of the X-ray luminosity is due to continuing accretion onto the neutron star surface, the feature may be the 0.87 keV rest-frame absorption complex (O VIII and other metal lines) intrinsic to the neutron star atmosphere, and a mass of 1.4 M-circle dot for X7 may be allowed.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM cheinke@cfa.harvard.edu
OI Heinke, Craig/0000-0003-3944-6109
NR 71
TC 51
Z9 51
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 452
EP 463
DI 10.1086/374039
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800038
ER
PT J
AU Dobrzycka, D
Raymond, JC
Biesecker, DA
Li, J
Ciaravella, A
AF Dobrzycka, D
Raymond, JC
Biesecker, DA
Li, J
Ciaravella, A
TI Ultraviolet spectroscopy of narrow coronal mass ejections
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun : coronal mass ejections (CMEs); Sun : UV radiation
ID ANGLE SPECTROMETRIC CORONAGRAPH; X-RAY TELESCOPE; WHITE-LIGHT; SOLAR
MINIMUM; JETS; MODEL; SOHO; TRANSIENTS; DENSITY; HOLES
AB We present Ultraviolet Coronagraph Spectrometer (UVCS) observations of five narrow coronal mass ejections (CMEs) that were among 15 narrow CMEs originally selected by Gilbert and coworkers. Two events (1999 March 27, April 15) were "structured," i.e., in white-light data they exhibited well-defined interior features, and three (1999 May 9, May 21, June 3) were "unstructured," i.e., appeared featureless. In UVCS data the events were seen as 4degrees-13degrees wide enhancements of the strongest coronal lines H I Lyalpha and O VI lambdalambda1032, 1037. We derived electron densities for several of the events from the Large Angle and Spectrometric Coronagraph Experiment (LASCO) C2 white-light observations. They are comparable to or smaller than densities inferred for other CMEs. We modeled the observable properties of examples of the structured (1999 April 15) and unstructured (1999 May 9) narrow CMEs at different heights in the corona between 1.5 and 2 R-circle dot. The derived electron temperatures, densities, and outflow speeds are similar for those two types of ejections. They were compared with properties of polar coronal jets and other CMEs. We discuss different scenarios of narrow CME formation as either a jet formed by reconnection onto open field lines or a CME ejected by expansion of closed field structures. Overall, we conclude that the existing observations do not definitively place the narrow CMEs into the jet or the CME picture, but the acceleration of the 1999 April 15 event resembles acceleration seen in many CMEs, rather than constant speeds or deceleration observed in jets.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Ocean & Atmospher Adm, Space Environm Ctr, Boulder, CO 80305 USA.
Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA.
Osservatorio Astron Palermo Giuseppe S Vaina, I-90134 Palermo, Italy.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ddobrzycka@cfa.harvard.edu; jraymond@cfa.harvard.edu;
doug.biesecker@noaa.gov; jing@ifa.hawaii.edu; ciarave@astropa.unipa.it
NR 40
TC 20
Z9 20
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 586
EP 595
DI 10.1086/374047
PN 1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800049
ER
PT J
AU Gottlieb, CA
Myers, PC
Thaddeus, P
AF Gottlieb, CA
Myers, PC
Thaddeus, P
TI Precise millimeter-wave laboratory frequencies for CS and (CS)-S-34
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : molecules; methods : laboratory; molecular data; molecular
processes; radio lines : ISM; stars : formation
ID SUB-DOPPLER MEASUREMENTS; ROTATIONAL TRANSITIONS; HYPERFINE-STRUCTURE;
CARBON-MONOXIDE; INFALL MOTIONS; STARLESS CORES; N2H+; SPECTRUM; CLOUDS
AB Nine successive rotational lines in the ground vibrational state of CS and (CS)-S-34 between 96 GHz ( J = 2-1) and 500 GHz (10-9) were measured in the laboratory to an accuracy of a few kHz. When our measurements are combined with the submillimeter-wave measurements of Ahrens & Winnewisser, the entire rotational spectrum of both isotopic species is predicted to an accuracy of about 1 part in 10(8) up to 500 GHz and 5 parts in 10(8) near 1000 GHz. These frequencies should be useful for quantitative studies of cloud core collapse and star formation in the millimeter- and submillimeter-wave bands.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
RP Gottlieb, CA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 20
TC 36
Z9 36
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAY 1
PY 2003
VL 588
IS 1
BP 655
EP 661
DI 10.1086/368378
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 671EF
UT WOS:000182451800055
ER
PT J
AU Jennions, MD
Moller, AP
AF Jennions, MD
Moller, AP
TI A survey of the statistical power of research in behavioral ecology and
animal behavior
SO BEHAVIORAL ECOLOGY
LA English
DT Article
DE effect size; meta-analysis; publication bias; sample sizes; statistical
power
ID RANDOMIZED CONTROLLED TRIALS; FILE DRAWER PROBLEM; PUBLICATION BIAS;
FLUCTUATING ASYMMETRY; BIOLOGICAL-RESEARCH; METAANALYSIS; EVOLUTION;
SIZE
AB We estimated the statistical power of the first and last statistical test presented in 697 papers from 10 behavioral journals. First tests had significantly greater statistical power and reported more significant results (smaller p values) than did last tests. This trend was consistent across journals, taxa, and the type of statistical test used. On average, statistical power was 13-16% to detect a small effect and 40-47% to detect a medium effect. This is far lower than the general recommendation of a power of 80%. By this criterion, only 2-3%, 13-21%, and 37-50% of the tests examined had the requisite power to detect a small, medium, or large effect, respectively. Neither p values nor statistical power varied significantly across the 10 journals or 11 taxa. However, mean p values of first and last tests were significantly correlated across journals (r =.67, n = 10, p =.034), with a similar trend for mean power (r =.63, n = 10, p =.051). There is therefore some evidence that power and p values are repeatable among journals. Mean p values or power of first and last tests were, however, uncorrelated across taxa. Finally, there was a significant correlation between power and reported p value for both first (r =.13, n = 684, p =.001) and last tests (r =.16, n = 654, p <.0001). If true effect sizes are unrelated to study sample sizes, the average true effect size must be nonzero for this pattern to emerge. This suggests that failure to observe significant relationships is partly owing to small sample sizes, as power increases with sample size. Key words: effect size, meta-analysis, publication bias, sample sizes, statistical power.
C1 Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia.
Smithsonian Trop Res Inst, Balboa, Panama.
Univ Paris 06, CNRS, Lab Ecol Evolut Parasitaire, FRE 2365, F-75252 Paris 5, France.
RP Jennions, MD (reprint author), Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia.
RI Rohlf, F/A-8710-2008; Jennions, Michael/C-7560-2009
OI Jennions, Michael/0000-0001-9221-2788
NR 40
TC 87
Z9 92
U1 0
U2 26
PU OXFORD UNIV PRESS INC
PI CARY
PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA
SN 1045-2249
J9 BEHAV ECOL
JI Behav. Ecol.
PD MAY
PY 2003
VL 14
IS 3
BP 438
EP 445
DI 10.1093/beheco/14.3.438
PG 8
WC Behavioral Sciences; Biology; Ecology; Zoology
SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics;
Environmental Sciences & Ecology; Zoology
GA 680CC
UT WOS:000182957900020
ER
PT J
AU Baldwin, CC
Smith, DG
AF Baldwin, CC
Smith, DG
TI Larval gobiidae (teleostei : perciformes) of Carrie Bow Cay, Belize,
central America
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article
ID EARLY-LIFE-HISTORY; WESTERN ATLANTIC; STAGE LARVAE; GOBIOIDEI;
MICRODESMIDAE; SYSTEMATICS; GOBIES; FISHES; PISCES; GOBY
AB Little descriptive and specific taxonomic information is available regarding the early life history stages of Caribbean coral-reef fishes. Ongoing studies at the Smithsonian Institution's research station at Carrie Bow Cay, Belize, involving the rearing of net-collected larval fishes is allowing specific identifications of numerous larval types. Field protocol includes preserving larval types in ethanol plus butylated hydroxytoluene to enhance the retention of orange and yellow pigments. Studies of fish larvae at Carrie Bow during the summer months of several years between 1993-1997 have yielded generic or specific identifications of 21 goby larvae belonging to ten genera. Separating closely related larval types in the field was facilitated by microscopic observations of combined patterns of melanophores and chromatophores. Identification of morphological types was aided by comparing countable features of larvae and reared juveniles with those of adult Caribbean gobies from USNM collections. Continued implementation of the methods outlined herein should prove valuable in identifying much more of the ichthyoplankton fauna of the Caribbean. Species-level identifications of larvae of coral reef fishes will render these life history stages useful in a variety of studies including those of phylogenetic relationships, ecology, as well as reproductive and fisheries biology. Including information from larval morphology in systematic studies of the Gobioidei may help clarify poorly understood relationships within the Suborder. Supraspecific patterns of chromatophores warrant further investigation as a novel suite of phylogenetically informative ontogenetic features.
C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA.
RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA.
NR 29
TC 11
Z9 14
U1 0
U2 3
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD MAY
PY 2003
VL 72
IS 3
BP 639
EP 674
PG 36
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 750YR
UT WOS:000187026500004
ER
PT J
AU Saavedra-Diaz, LM
Munroe, TA
Acero, A
AF Saavedra-Diaz, LM
Munroe, TA
Acero, A
TI Symphurus hernandezi (Pleuronectiformes : Cynoglossidae), a new
deep-water tonguefish from the southern Caribbean sea off Colombia
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article
ID REDESCRIPTION; BRACHYURA; DECAPODA; COAST
AB A new cynoglossid species, Symphurus hernandezi, is described from 83 specimens (50.9-126.9 min SL) taken on the outer continental shelf (82 specimens collected between 148 and 301 in) off Caribbean Colombia. This species is distinguished from all congeners by its unique purplish pigmentation and pepperdot pattern of melanophores on the blind side of the body. Symphurus hernandezi has a 1-3-2 pattern of interdigitation of dorsal-fin pterygiophores and neural spines, 12 caudal-fin rays and a black peritoneum. Among congeners, S. hernandezi is most similar to the sympatrically occurring S. marginatus, but is easily distinguished from that species by differences in ocular- and blind-side pigmentation patterns, fewer longitudinal and head scales (77-86 and 13-16 in S. hernandezi vs 86-99 and 16-20 in S. marginatus, respectively), and by several morphometric features including shorter dorsal- and anal-fin rays, deeper body depth in the caudal region, longer head and postorbital lengths, and a smaller pupil diameter. Symphurus hernandezi has a restricted distribution on the outer continental shelf off Caribbean Colombia.
C1 INVEMAR, Inst Invest Marinas & Costeras, AA-1016 Santa Marta, Colombia.
Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA.
Univ Nacl Colombia, Inst Ciencias Nat, Santa Marta, Colombia.
RP Saavedra-Diaz, LM (reprint author), INVEMAR, Inst Invest Marinas & Costeras, AA-1016 Santa Marta, Colombia.
NR 29
TC 2
Z9 4
U1 0
U2 2
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD MAY
PY 2003
VL 72
IS 3
BP 955
EP 970
PG 16
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 750YR
UT WOS:000187026500021
ER
PT J
AU Haug, JD
AF Haug, JD
TI The fate of knowledge.
SO COLLEGE & RESEARCH LIBRARIES
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Haug, JD (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU ASSOC COLL RESEARCH LIBRARIES
PI CHICAGO
PA 50 E HURON ST, CHICAGO, IL 60611 USA
SN 0010-0870
J9 COLL RES LIBR
JI Coll. Res. Libr.
PD MAY
PY 2003
VL 64
IS 3
BP 243
EP 246
PG 4
WC Information Science & Library Science
SC Information Science & Library Science
GA 681AX
UT WOS:000183015200007
ER
PT J
AU Gonzalez, MA
Eberhard, JR
Lovette, IJ
Olson, SL
Bermingham, E
AF Gonzalez, MA
Eberhard, JR
Lovette, IJ
Olson, SL
Bermingham, E
TI Mitochondrial DNA phylogeography of the Bay Wren (Troglodytidae :
Thryothorus nigricapillus) complex
SO CONDOR
LA English
DT Article
DE Bay Wren; Panama isthmus; phylogeny; phylogeography; plumage;
speciation; Thryothorus nigricapillus
ID REPRODUCTIVE STRATEGIES; GENETIC-DIVERGENCE; CENTRAL-AMERICA; SONG
BEHAVIOR; DUETTING WREN; HYBRID ZONE; EVOLUTIONARY; DIFFERENTIATION;
BIOGEOGRAPHY; POPULATIONS
AB The Bay Wren (Thryothorus nigricapillus) is distributed from Costa Rica to Ecuador and includes seven described subspecies, five of which occur in the Caribbean lowlands of Panama. The subspecies vary in plumage characters, with particularly striking differences between Bay Wrens from western Panama (to the north), and eastern Panama (to the south). We surveyed mitochondrial DNA (mtDNA) sequence variation from a geographically broad sample of Bay Wrens and compared the phylogeographic structure of mtDNA diversity with previously described patterns of morphological variation. The mtDNA-based phylogeographic reconstructions revealed a basal split separating populations in far eastern Panama and South America from those in central Panama through Costa Rica. These two clades are concordant with previous morphology-based groupings of T. nigricapillus subspecies into the "castaneus group" (costaricensis, odicus, castaneus, and reditus) and the "nigricapillus group" (schottii, connectens, and nigricapillus). Morphological intergradation between the two groups takes place in central Panama, but all intergrades possess the mtDNA haplotype of the castaneus group, suggesting that mitochondrial gene flow is introgressing from west to east. In spite of the marked body size and plumage variation present among subspecies of the castaneus group, mtDNA variation within this group was low. At a deeper phylogenetic level, the mtDNA data support recognition of the Riverside Wren, T. semibadius, as a full species. This taxon has sometimes been considered conspecific with T nigricapillus, but the high mtDNA divergence between these species is consistent with previous suggestions that the morphological similarity results from convergence in plumage traits.
C1 Smithsonian Trop Res Inst, Naos Labs, Balboa, Panama.
Louisiana State Univ, Dept Sci Biol, Baton Rouge, LA 70803 USA.
Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA.
Cornell Lab Ornithol, Ithaca, NY 14850 USA.
Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA.
RP Bermingham, E (reprint author), Smithsonian Trop Res Inst, Naos Labs, Apartado 2072, Balboa, Panama.
RI Lovette, Irby/P-3477-2014
NR 39
TC 16
Z9 17
U1 0
U2 5
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 MAY
PY 2003
VL 105
IS 2
BP 228
EP 238
DI 10.1650/0010-5422(2003)105[0228:MDPOTB]2.0.CO;2
PG 11
WC Ornithology
SC Zoology
GA 674YF
UT WOS:000182664700005
ER
PT J
AU Darke, AK
Megonigal, JP
AF Darke, AK
Megonigal, JP
TI Control of sediment deposition rates in two mid-Atlantic Coast tidal
freshwater wetlands
SO ESTUARINE COASTAL AND SHELF SCIENCE
LA English
DT Article
DE sediment deposition; tidal freshwater wetland; sea level rise; flood
depth; plant density; turbidity maximum; Mattapom River; VA;
mid-Atlantic Coast
ID SUSPENDED PARTICULATE MATTER; CHESAPEAKE BAY; CLIMATE-CHANGE; SALT
MARSHES; TURBIDITY MAXIMUM; POTENTIAL IMPACTS; UNITED-STATES; ESTUARY;
RIVER; TRANSPORT
AB Eustatic sea level rise and rapidly increasing coastal development threaten tidal freshwater wetlands. Sediment deposition is one process that affects their ability to maintain surface elevations relative to adjacent rivers. Sediment dynamics in salt marshes have been studied extensively, but little is known about the factors that control sediment deposition rates in tidal freshwater wetlands. We examined geomorphic, hydrological, and biotic factors that may influence sedimentation in two tidal freshwater wetlands that fell at opposite ends of the riverine-estuarine continuum. Our data demonstrate that sediment dynamics are highly variable among tidal freshwater wetlands, and are influenced by the location of the wetland on the continuum. Sediment deposition was up to 10 times higher during the growing season at the downstream site than the upstream site. Plant density and height were highly correlated with sediment deposition rates at the downstream site (r greater than or equal to 0.92, p less than or equal to 0.009) but not at the upstream site. Elevation, flood depth, and flood duration were correlated with deposition rates only when each site/season combination was considered separately. River suspended sediment and surficial floodwater suspended sediment concentrations were significantly higher at the downstream site (p = 0.02 and p = 0.04, respectively). These data suggest that vegetation is important in determining sediment deposition rates when river suspended sediment is not limiting. which is not always the case. Longer flood duration increased sediment deposition, but was of secondary importance. Land use and proximity to the turbidity maximum (near the forward extent of the salt water intrusion) appear to be critically important in determining river suspended sediment availability in the tidal freshwater zone of the Mattaponi River, VA. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
George Mason Univ, Environm Sci & Publ Program, Fairfax, VA 22030 USA.
RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
NR 59
TC 30
Z9 30
U1 3
U2 21
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0272-7714
J9 ESTUAR COAST SHELF S
JI Estuar. Coast. Shelf Sci.
PD MAY
PY 2003
VL 57
IS 1-2
BP 255
EP 268
DI 10.1016/S0272-7714(02)00353-0
PG 14
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 707FR
UT WOS:000184500300022
ER
PT J
AU Naisbit, RE
Jiggins, CD
Mallet, J
AF Naisbit, RE
Jiggins, CD
Mallet, J
TI Mimicry: developmental genes that contribute to speciation
SO EVOLUTION & DEVELOPMENT
LA English
DT Article
ID WARNING-COLOR; HELICONIUS BUTTERFLIES; REPRODUCTIVE ISOLATION;
NATURAL-SELECTION; EVOLUTIONARY GENETICS; POSTZYGOTIC ISOLATION;
ADAPTIVE RADIATION; MULLERIAN MIMICRY; PATTERN-FORMATION; HYBRID ZONES
AB Despite renewed interest in the role of natural selection as a catalyst for the origin of species, the developmental and genetic basis of speciation remains poorly understood. Here we describe the genetics of Mullerian mimicry in Heliconius cydno and H. melpomene (Lepidoptera: Nymphalidae), sister species that recently diverged to mimic other Heliconius. This mimetic shift was a key step in their speciation, leading to pre- and postmating isolation. We identify 10 autosomal loci, half of which have major effects. At least eight appear to be homologous with genes known to control pattern differences within each species. Dominance has evolved under the influence of identifiable "modifier" loci rather than being a fixed characteristic of each locus. Epistasis is found at many levels: phenotypic interaction between specific pairs of genes, developmental canalization due to polygenic modifiers so that patterns are less sharply defined in hybrids, and overall fitness through ecological selection against nonmimetic hybrid genotypes. Most of the loci are clustered into two genomic regions or "supergenes," suggesting color pattern evolution is constrained by preexisting linked elements that may have arisen via tandem duplication rather than having been assembled by natural selection. Linkage, modifiers, and epistasis affect the strength of mimicry as a barrier to gene flow between these naturally hybridizing species and may permit introgression in genomic regions unlinked to those under disruptive selection. Mullerian mimics in Heliconius use different genetic architectures to achieve the same mimetic patterns, implying few developmental constraints. Therefore, although developmental and genomic constraints undoubtedly influence the evolutionary process, their effects are probably not strong in comparison with natural selection.
C1 UCL, Galton Lab, Dept Biol, London NW1 2HE, England.
Smithsonian Trop Res Inst, Balboa, Panama.
RP Naisbit, RE (reprint author), Univ Neuchatel, Inst Zool, Lab Ecol Anim & Entomol, CH-2007 Neuchatel, Switzerland.
EM russell.naisbit@unine.ch
RI Jiggins, Chris/B-9960-2008; Naisbit, Russell/B-9658-2011; mallet,
james/B-5114-2008;
OI Jiggins, Chris/0000-0002-7809-062X; Naisbit,
Russell/0000-0003-0190-9323; Mallet, James/0000-0002-3370-0367
NR 82
TC 78
Z9 81
U1 1
U2 25
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 1520-541X
J9 EVOL DEV
JI Evol. Dev.
PD MAY-JUN
PY 2003
VL 5
IS 3
BP 269
EP 280
DI 10.1046/j.1525-142X.2003.03034.x
PG 12
WC Evolutionary Biology; Developmental Biology; Genetics & Heredity
SC Evolutionary Biology; Developmental Biology; Genetics & Heredity
GA 672TT
UT WOS:000182539500006
PM 12752766
ER
PT J
AU Vila, R
Mundina, M
Tomi, F
Ciccio, JF
Gupta, MP
Iglesias, J
Casanova, J
Canigueral, S
AF Vila, R
Mundina, M
Tomi, F
Ciccio, JF
Gupta, MP
Iglesias, J
Casanova, J
Canigueral, S
TI Constituents of the essential oils from Piper friedrichsthalii C.DC. and
P-pseudolindenii C.DC. from Central America
SO FLAVOUR AND FRAGRANCE JOURNAL
LA English
DT Article
DE Piper friedrichsthalii; Piper pseudolindenii; Piperaceae; essential oil;
GC-MS; C-13-NMR; alpha-apinene; alpha-selinene; 11-selinen-4 alpha-ol;
beta-elemene; beta-caryophyllene
ID C-13 NMR; COMPLEX
AB Essential oils obtained by hydrodistillation from the leaves and flower spikes of Piper friedrichsthalii from Costa Rica and Panama, and leaves of P. pseudolindenii from Costa Rica were analysed by GC-FID, GC-MS and C-13-NMR. Monoterpenoids constituted the main fraction of the oils of P. friedrichsthalii from Costa Rica, particularly a-pinene, camphene, beta-phellandrene, limonene and menthane derivatives, whereas the oils from leaves of P. friedrichsthalii from Panama and of P. pseudolindenii from Costa Rica were characterized by a high sesquiterpene content, especially 11-selinen-4alpha-ol, alpha-selinene, germacrene D and beta-selinene in the former, and beta-elemene, beta-caryophyllene, germacrene D and alpha-humulene in the latter. Copyright (C) 2003 John Wiley Sons, Ltd.
C1 Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognisa, E-08028 Barcelona, Spain.
Univ Corse, CNRS, UMR 6134, F-75700 Paris, France.
Univ Costa Rica, Escuela Quim, CIPRONA, San Jose 2060, Costa Rica.
Univ Panama, Estafeta Univ, Fac Farm, CIFLORPAN, Panama City, Panama.
Smithsonian Trop Res Inst, Panama City, Panama.
RP Canigueral, S (reprint author), Univ Barcelona, Fac Farm, Unitat Farmacol & Farmacognisa, Avda Diagonal 643, E-08028 Barcelona, Spain.
RI Canigueral, Salvador/O-2767-2013
OI Canigueral, Salvador/0000-0001-5056-489X
NR 9
TC 7
Z9 8
U1 0
U2 2
PU JOHN WILEY & SONS LTD
PI W SUSSEX
PA BAFFINS LANE CHICHESTER, W SUSSEX PO19 1UD, ENGLAND
SN 0882-5734
J9 FLAVOUR FRAG J
JI Flavour Frag. J.
PD MAY-JUN
PY 2003
VL 18
IS 3
BP 198
EP 201
DI 10.1002/ffj.1181
PG 4
WC Chemistry, Applied; Food Science & Technology
SC Chemistry; Food Science & Technology
GA 675UD
UT WOS:000182713600004
ER
PT J
AU Zito, M
Evans, S
Weldon, PJ
AF Zito, M
Evans, S
Weldon, PJ
TI Owl monkeys (Aotus spp.) self-anoint with plants and millipedes
SO FOLIA PRIMATOLOGICA
LA English
DT Article
DE owl monkeys; Aotus; self-anointing; millipedes
C1 Primate Conservancy, Land OLakes, FL 34639 USA.
DuMond Conservancy, Miami, FL USA.
Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA USA.
RP Zito, M (reprint author), Primate Conservancy, POB 1551, Land OLakes, FL 34639 USA.
NR 12
TC 22
Z9 26
U1 1
U2 8
PU KARGER
PI BASEL
PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND
SN 0015-5713
J9 FOLIA PRIMATOL
JI Folia Primatol.
PD MAY-JUN
PY 2003
VL 74
IS 3
BP 159
EP 161
DI 10.1159/000070649
PG 3
WC Zoology
SC Zoology
GA 698DV
UT WOS:000183983100005
PM 12826735
ER
PT J
AU Petaev, MI
Wood, JA
Meibom, A
Krot, AN
Keil, K
AF Petaev, MI
Wood, JA
Meibom, A
Krot, AN
Keil, K
TI The ZONMET thermodynamic and kinetic model of metal condensation
SO GEOCHIMICA ET COSMOCHIMICA ACTA
LA English
DT Article
ID CH CARBONACEOUS CHONDRITES; SOLAR NEBULA; OXIDIZING CONDITIONS;
NUCLEATION PROCESS; MIXING PROPERTIES; HIGH-TEMPERATURE; GRAIN
FORMATION; SYSTEM; ELEMENTS; ORIGIN
AB The ZONMET model of metal condensation is a FORTRAN computer code that calculates condensation with partial isolation-type equilibrium partitioning of the 19 most abundant elements among 203 gaseous and 488 condensed phases and growth in the nebula of a zoned metal grain by condensation from the nebular gas accompanied by diffusional redistribution of Ni, Co, and Cr. Of five input parameters of the ZONMET model (chemical composition of the system expressed as the dust/gas [D/G] ratio, nebular pressure [P-tot], isolation degree [xi], cooling rate (CR), and seed size), only two-the D/G ratio and the CR of the nebular source region of a zoned Fe,Ni grain-are important in determining the grain radius and Ni, Co, and Cr zoning profiles. We found no evidence for the supercooling during condensation of Fe,Ni metal that is predicted by the homogeneous nucleation theory. The model allows estimates to be made of physicochemical parameters in the CH chondrite nebular source regions.
Modeling growth and simultaneous diffusional redistribution of Ni, Co, and Cr in the zoned metal grains of CH chondrites reveals that the condensation zoning profiles were substantially modified by diffusion while the grains were growing in the nebula. This means that previous estimates of the physicochemical conditions in the nebular source regions of CH and CB chondrites, based on measured zoning profiles of Ni, Co, Cr, and platinum group elements in Fe,Ni metal grains, need to be corrected.
The two zoned metal grains in the PAT 91456 and NWA 470 CH chondrites studied so far require nebular source regions with different chemical compositions (D/G = 1 and D/G = 4, respectively) and thermal histories characterized by variable cooling rates (CR = 0.011 + 0.0022 X DeltaT K/h and CR = 0.05 + 0.0035 X DeltaT K/h, respectively). It appears that the metal grains of the CH chondrites were formed in multiple nebular source regions or in different events within the same source region as the CB chondrite metal grains were formed. Copyright (C) 2003 Elsevier Science Ltd.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02128 USA.
Stanford Univ, Stanford, CA 94305 USA.
Univ Hawaii Manoa, Sch Ocean & Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA.
RP Petaev, MI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 67
TC 21
Z9 21
U1 0
U2 5
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0016-7037
J9 GEOCHIM COSMOCHIM AC
JI Geochim. Cosmochim. Acta
PD MAY
PY 2003
VL 67
IS 9
BP 1737
EP 1751
AR PII S0016-7037(02)00956-0
DI 10.1016/S0016-7037(02)00956-0
PG 15
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 673PT
UT WOS:000182589900012
ER
PT J
AU Golombek, MP
Grant, JA
Parker, TJ
Crisp, JA
Squyres, SW
AF Golombek, MP
Grant, JA
Parker, TJ
Crisp, JA
Squyres, SW
TI Landing the Mars Exploration Rovers
SO GEOTIMES
LA English
DT Article
C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
Natl Air Space Museum Washington, Ctr Earth & Planetary Studies, Smithsonian Inst, Washington, DC USA.
Cornell Univ, Dept Astron, Ithaca, NY 14853 USA.
RP Golombek, MP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA.
RI Crisp, Joy/H-8287-2016
OI Crisp, Joy/0000-0002-3202-4416
NR 0
TC 0
Z9 0
U1 0
U2 1
PU AMER GEOLOGICAL INST
PI ALEXANDRIA
PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 USA
SN 0016-8556
J9 GEOTIMES
JI Geotimes
PD MAY
PY 2003
VL 48
IS 5
BP 18
EP 23
PG 6
WC Geosciences, Multidisciplinary
SC Geology
GA 779WY
UT WOS:000189326000015
ER
PT J
AU Baliunas, S
Donahue, R
Rampino, MR
Gaffey, MJ
Shelton, JC
Mohanty, S
AF Baliunas, S
Donahue, R
Rampino, MR
Gaffey, MJ
Shelton, JC
Mohanty, S
TI Multispectral analysis of Asteroid 3 Juno taken with the 100-inch
telescope at Mount Wilson Observatory
SO ICARUS
LA English
DT Article
AB High-resolution multispectral images of main-belt asteroid 3 Juno were taken at visible and near-IR wavelengths with the 100-inch telescope at Mount Wilson Observatory equipped with an adaptive optics system. The images show spectral features that may represent a large relatively recent impact that deeply excavated the coarse-grained olivine-pyroxene-rich crust of the asteroid. (C) 2003 Elsevier Science (USA). All rights reserved.
C1 NYU, Earth & Environm Sci Program, New York, NY 10003 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
NASA, Goddard Inst Space Studies, New York, NY 10025 USA.
Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA.
Mt Wilson Inst, Pasadena, CA 91106 USA.
Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Rampino, MR (reprint author), NYU, Earth & Environm Sci Program, 100 Washington Sq E Room 1009, New York, NY 10003 USA.
NR 18
TC 8
Z9 8
U1 3
U2 4
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0019-1035
J9 ICARUS
JI Icarus
PD MAY
PY 2003
VL 163
IS 1
BP 135
EP 141
DI 10.1016/S0019-1035(03)00049-6
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 681VN
UT WOS:000183056400009
ER
PT J
AU Ortner, DJ
AF Ortner, DJ
TI Human remains: Conservation, retrieval and analysis
SO INTERNATIONAL JOURNAL OF OSTEOARCHAEOLOGY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
Univ Bradford, Bradford BD7 1DP, W Yorkshire, England.
RP Ortner, DJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 1
U2 2
PU JOHN WILEY & SONS LTD
PI CHICHESTER
PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND
SN 1047-482X
J9 INT J OSTEOARCHAEOL
JI Int. J. Osteoarchaeol.
PD MAY-JUN
PY 2003
VL 13
IS 3
BP 173
EP 174
DI 10.1002/oa.632
PG 2
WC Anthropology; Archaeology
SC Anthropology; Archaeology
GA 691RE
UT WOS:000183618600009
ER
PT J
AU Reich, PB
Wright, IJ
Cavender-Bares, J
Craine, JM
Oleksyn, J
Westoby, M
Walters, MB
AF Reich, PB
Wright, IJ
Cavender-Bares, J
Craine, JM
Oleksyn, J
Westoby, M
Walters, MB
TI The evolution of plant functional variation: Traits, spectra, and
strategies
SO INTERNATIONAL JOURNAL OF PLANT SCIENCES
LA English
DT Review
DE plant traits; adaptation; fitness; functional groups; selection
ID CARBON-ISOTOPE DISCRIMINATION; LEAF LIFE-SPAN; PINUS-SYLVESTRIS
POPULATIONS; RELATIVE GROWTH-RATE; SHADE TOLERANCE; RAIN-FOREST; SCOTS
PINE; LOW-LIGHT; PHOTOSYNTHETIC CAPACITY; COMMON-GARDEN
AB Variation in plant functional traits results from evolutionary and environmental drivers that operate at a variety of different scales, which makes it a challenge to differentiate among them. In this article we describe patterns of functional trait variation and trait correlations within and among habitats in relation to several environmental and trade-off axes. We then ask whether such patterns reflect natural selection and can be considered plant strategies. In so doing we highlight evidence that demonstrates that (1) patterns of trait variation across resource and environmental gradients (light, water, nutrients, and temperature) probably reflect adaptation, (2) plant trait variation typically involves multiple-correlated traits that arise because of inevitable trade-offs among traits and across levels of whole-plant integration and that must be understood from a whole-plant perspective, and (3) such adaptation may be globally generalizable for like conditions; i. e., the set of traits (collections of traits in syndromes) of taxa can be considered as "plant strategies."
C1 Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Landcare Res, Dunedin, New Zealand.
Polish Acad Sci, Inst Dendrol, PL-62035 Kornik, Poland.
Michigan State Univ, Dept Forestry, E Lansing, MI 48824 USA.
RP Reich, PB (reprint author), Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA.
RI Craine, Joseph/D-4569-2009; Wright, Ian/G-4979-2012; Oleksyn,
Jacek/I-4539-2012; Cavender-Bares, Jeannine/K-5716-2013
OI Craine, Joseph/0000-0001-6561-3244; Wright, Ian/0000-0001-8338-9143;
NR 166
TC 430
Z9 458
U1 41
U2 337
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 1058-5893
J9 INT J PLANT SCI
JI Int. J. Plant Sci.
PD MAY
PY 2003
VL 164
IS 3
SU S
BP S143
EP S164
DI 10.1086/374368
PG 22
WC Plant Sciences
SC Plant Sciences
GA 698UW
UT WOS:000184018500011
ER
PT J
AU Fogel, ML
Tuross, N
AF Fogel, ML
Tuross, N
TI Extending the limits of paleodietary studies of humans with compound
specific carbon isotope analysis of amino acids
SO JOURNAL OF ARCHAEOLOGICAL SCIENCE
LA English
DT Article
DE paleodiet; humans; stable carbon isotopes; plants
ID DIETARY-PROTEIN INTAKE; STABLE CARBON; PLASMA-CONCENTRATIONS;
DIURNAL-VARIATIONS; NITROGEN; COLLAGEN; ECOLOGY; RATIOS; C-13
AB Stable carbon isotopes in the bone collagen of prehistoric humans are valuable tools for determining human diet. We studied carbon isotopes in individual amino acids (IAA) in plants and collagen from herbivores and humans from North American prehistoric sites in order to determine whether more specific dietary information about Indians could be predicted. The VC of plant amino acids ranged extensively, whereas delta(13)C values of each amino acid from the C-3 (n = 3) and C-4 (n = 3) plant species were linearly related with a slope of 0.8. Essential amino acids from herbivores had delta(13)C values that were completely different from those measured in either C-3 or C-4 plants, suggesting metabolic resynthesis in the gut by microflora. The delta(13)C of essential amino acids from prehistoric North Americans, who had diets ranging from primarily maize-based (C-4) to hunter-gathers (C-3) subsistence, were highly correlated with delta(13)C values of herbivore essential amino acids. There was no significant correlation of delta(13)C in IAA from humans with those of plants. The delta(13)C of nonessential amino acids in human bone collagen can distinguish the presence of maize in the diet, whereas the delta(13)C of essential amino acids were transparent to a maize-derived carbon signal. Compound specific isotopic data on IAA distinguish between total carbon intake versus total protein intake and are useful for discerning the extent and nature of omnivory. (C) 2003 Elsevier Science Ltd. All rights reserved.
C1 Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA.
Natl Museum Nat Hist, Smithsonian Inst, Ctr Mat Res & Educ, Suitland, MD 20746 USA.
Natl Museum Nat Hist, Labs Analyt Biol, Suitland, MD 20746 USA.
RP Fogel, ML (reprint author), Carnegie Inst Washington, Geophys Lab, 5251 Broad Branch Rd NW, Washington, DC 20015 USA.
RI Fogel, Marilyn/M-2395-2015
OI Fogel, Marilyn/0000-0002-1176-3818
NR 30
TC 64
Z9 65
U1 2
U2 22
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0305-4403
J9 J ARCHAEOL SCI
JI J. Archaeol. Sci.
PD MAY
PY 2003
VL 30
IS 5
BP 535
EP 545
DI 10.1016/S0305-4403(02)00199-1
PG 11
WC Anthropology; Archaeology; Geosciences, Multidisciplinary
SC Anthropology; Archaeology; Geology
GA 663HZ
UT WOS:000182001300003
ER
PT J
AU Andersson, M
Wallander, J
Oring, L
Akst, E
Reed, JM
Fleischer, RC
AF Andersson, M
Wallander, J
Oring, L
Akst, E
Reed, JM
Fleischer, RC
TI Adaptive seasonal trend in brood sex ratio: test in two sister species
with contrasting breeding systems
SO JOURNAL OF EVOLUTIONARY BIOLOGY
LA English
DT Article
DE brood sex ratio trend; molecular sexing; monogamy; Monte Carlo test;
polyandry; sex role reversal
ID REPRODUCTIVE SUCCESS; SPOTTED SANDPIPERS; ACTITIS-MACULARIA; KESTREL
BROODS; LEK PARADOX; BIRDS; ALLOCATION; HYPOTHESIS; ADJUSTMENT;
EVOLUTION
AB Evolutionary theory predicts adaptive adjustment in offspring sex ratio by females. Seasonal change in sex ratio is one possibility, tested here in two sister species, the Common sandpiper and the Spotted sandpiper Actitis hypoleucos and A. macularia. In the monogamous Common sandpiper, males are the most competitive sex. In each of 3 years, there was a change from mainly sons in early clutches to mainly daughters in late clutches. This seasonal adjustment of clutch sex ratio took place within the female before the eggs were laid, not by differential egg or chick survival. The sex of all eggs laid in the clutches used here was determined molecularly from chick blood taken at the time of hatching. The Spotted sandpiper in contrast is polyandrous, with partly reversed sex roles. There was no seasonal trend from sons to daughters in this species. When tested together, the two species differed significantly as predicted by the hypothesis of adaptive sex ratio adjustment by females.
C1 Univ Gothenburg, Dept Zool, SE-40530 Gothenburg, Sweden.
Univ Nevada, Dept Environm & Resource Sci, Reno, NV 89557 USA.
Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Genet Program, Washington, DC 20560 USA.
RP Andersson, M (reprint author), Univ Gothenburg, Dept Zool, Box 463, SE-40530 Gothenburg, Sweden.
NR 46
TC 40
Z9 40
U1 1
U2 8
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 1010-061X
J9 J EVOLUTION BIOL
JI J. Evol. Biol.
PD MAY
PY 2003
VL 16
IS 3
BP 510
EP 515
DI 10.1046/j.1420-9101.2003.00533.x
PG 6
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 668XV
UT WOS:000182322200015
PM 14635851
ER
PT J
AU Scherneck, HG
Johansson, JM
Koivula, H
van Dam, T
Davis, JL
AF Scherneck, HG
Johansson, JM
Koivula, H
van Dam, T
Davis, JL
TI Vertical crustal motion observed in the BIFROST project
SO JOURNAL OF GEODYNAMICS
LA English
DT Article; Proceedings Paper
CT 10th International Symposium on Recent Crustal Movement
CY AUG 27-31, 2001
CL HELSINKI, FINLAND
ID PERMANENT GPS NETWORK; SIGNAL SCATTERING; ENERGY BALANCES; SITE
POSITIONS; SURFACE LOADS; LAND WATER; FENNOSCANDIA; DISPLACEMENTS;
DEFORMATION; RATES
AB This paper reports from investigations on the robustness of estimated rates of intraplate motion from the continuous GPS project BIFROST (Baseline Inferences from Fennoscandian Rebound Observations, Sealevel and Tectonics). We study loading effects due to ocean, atmosphere and hydrology and their impact on estimated rate parameters. We regularly find the admittance of a modelled perturbation at less than fifty percent of the full effect. We think that the finding relates to a difficult noise situation at all periods, and that a satisfying model for the dominating noise source has not been found yet. An additional reason for low admittance is found in the mapping process of the no-fiducial network solution into a conventional reference frame. (C) 2003 Elsevier Science Ltd. All rights reserved.
C1 Chalmers Univ Technol, Onsala Space Observ, SE-43992 Onsala, Sweden.
Finnish Geodet Inst, FI-02431 Masala, Finland.
European Ctr Geodynam & Seismol, L-7256 Walferdange, Luxembourg.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Scherneck, HG (reprint author), Chalmers Univ Technol, Onsala Space Observ, SE-43992 Onsala, Sweden.
RI Davis, James/D-8766-2013
OI Davis, James/0000-0003-3057-477X
NR 21
TC 32
Z9 33
U1 1
U2 1
PU PERGAMON-ELSEVIER SCIENCE LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND
SN 0264-3707
J9 J GEODYN
JI J. Geodyn.
PD MAY-JUL
PY 2003
VL 35
IS 4-5
BP 425
EP 441
DI 10.1016/S0264-3707(03)00005-X
PG 17
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 678ZQ
UT WOS:000182896900004
ER
PT J
AU Franz, NM
Wcislo, WT
AF Franz, NM
Wcislo, WT
TI Foraging behavior in two species of Ectatomma (Formicidae : Ponerinae):
Individual learning of orientation and timing
SO JOURNAL OF INSECT BEHAVIOR
LA English
DT Article
DE cognitive ecology; Ectatomma; foraging behavior; individual learning;
Ponerinae
ID RUIDUM ROGER HYMENOPTERA; GIANT TROPICAL ANT; NESTMATE RECOGNITION;
PARAPONERA-CLAVATA; COGNITIVE ECOLOGY; TUBERCULATUM; ENVIRONMENTS;
POLYETHISM; EFFICIENCY; PREDATION
AB The foraging behavior of marked individuals of Ectatomma ruidum and E. tuberculatum (Formicidae: Ponerinae) was observed on Barro Colorado Island, Panama, in order to determine whether learning of orientation and timing is involved when foraging on patchy resources on the forest floor. Foraging experiments under seminatural conditions were designed to control for the spatiotemporal distribution of resources at one or two preying sites. Using both single- and multi-event past experience, individual foragers of E. ruidum and (although less significantly) E. tuberculatum made directional and temporal adjustments to their behavior in response to previous differential foraging success. In spite of considerable individual variation in foraging efficiency, it is hypothesized that the observed differences in cognitive abilities can be invoked to explain ecological differences among both species.
C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Ancon, Panama.
NR 45
TC 9
Z9 10
U1 1
U2 15
PU KLUWER ACADEMIC/PLENUM PUBL
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0892-7553
J9 J INSECT BEHAV
JI J. Insect Behav.
PD MAY
PY 2003
VL 16
IS 3
BP 381
EP 410
DI 10.1023/A:1024880110189
PG 30
WC Entomology
SC Entomology
GA 702ZA
UT WOS:000184253900006
ER
PT J
AU McShea, WJ
Pagels, J
Orrock, J
Harper, E
Koy, K
AF McShea, WJ
Pagels, J
Orrock, J
Harper, E
Koy, K
TI Mesic deciduous forest as patches of small-mammal richness within an
Appalachian Mountain Forest
SO JOURNAL OF MAMMALOGY
LA English
DT Article
DE biodiversity; Clethrionomys; forest ecology; landscape ecology;
metapopulation theory; Napaeozapus; Peromyscus; Sorex
ID MICE PEROMYSCUS-LEUCOPUS; SOUTHERN APPALACHIANS; MANAGED FOREST;
NORTH-AMERICA; LANDSCAPE; ABUNDANCE; POPULATION; MANICULATUS; DYNAMICS;
SCALE
AB Forests of Southern Appalachia are critical habitats with respect to biodiversity, with a large portion of these forests residing on public multiuse lands. With pressure to extract timber from maturing forests, there is a need to identify the relative importance of forest types within the larger forest matrix. We examined small-mammal populations at 350 sample points across 157 km(2) of forested habitat in the George Washington and Jefferson National Forests, Virginia, to determine landscape and habitat correlates of species abundance and richness. A total of 3,955 individuals representing 20 species were captured using live trap and pitfall sampling at each point during 1996 and 1997. Nine species were sufficiently common to examine their abundance relative to landscape and habitat features. We found species abundance and richness to be highest in mesic deciduous forest types, with the exception of Peromyscus leucopus. Soil moisture capacity and the proportion of mesic habitat within 100 m of the sample point were also important for several species. If mesic deciduous forest can be considered patches within a matrix of xeric forest, then the abundance of 4 species and species richness could be predicted based on the distance of the sample point to the nearest mesic patch and the abundance of 3 species inside mesic patches was related to patch size. At least 73% of mesic patches within this forest were <25 ha and separated from other patches by >100 m. Our results indicate that mesic forest patches contain the bulk of the species richness for small mammals in the Southern Appalachian ecotype. Designing timber harvests that minimize use of mesic deciduous forest type and that does not decrease patch numbers would achieve the largest benefits to small mammals within the region.
C1 Smithsonian Inst, Conservat & Res Ctr, Front Royal, VA 22630 USA.
Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA.
Iowa State Univ Sci & Technol, Ecol & Evolutionary Biol Program, Ames, IA 50011 USA.
Univ Minnesota, Dept Fisheries & Wildlife, St Paul, MN 55108 USA.
RP McShea, WJ (reprint author), Smithsonian Inst, Conservat & Res Ctr, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA.
EM wmcshea@crc.si.edu
NR 66
TC 17
Z9 18
U1 3
U2 17
PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS
PI LAWRENCE
PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA
SN 0022-2372
EI 1545-1542
J9 J MAMMAL
JI J. Mammal.
PD MAY
PY 2003
VL 84
IS 2
BP 627
EP 643
DI 10.1644/1545-1542(2003)084<0627:MDFAPO>2.0.CO;2
PG 17
WC Zoology
SC Zoology
GA 685VN
UT WOS:000183284500027
ER
PT J
AU Matsui, T
Cheung, ASC
Leung, KWS
Yoshino, K
Parkinson, WH
Thorne, AP
Murray, JE
Ito, K
Imajo, T
AF Matsui, T
Cheung, ASC
Leung, KWS
Yoshino, K
Parkinson, WH
Thorne, AP
Murray, JE
Ito, K
Imajo, T
TI High resolution absorption cross-section measurements of the
Schumann-Runge bands of O-2 by VUV Fourier transform spectroscopy
SO JOURNAL OF MOLECULAR SPECTROSCOPY
LA English
DT Article
ID HERZBERG-I BANDS; OSCILLATOR-STRENGTHS; PREDISSOCIATION LINEWIDTHS;
REGION; STATE; SPECTROMETER; OXYGEN
AB The photoabsorption spectrum of the O-2 Schumann-Runge bands was measured with resolution comparable to the Doppler widths by using the VUV Fourier transform spectrometer from Imperial College, London, combined with synchrotron radiation as a continuum light source at the Photon Factory, KEK, Japan. The analysis of the (12,0)-(17,0) bands of the Schumann-Runge system provides accurate rotational line positions as well as the line intensities from 185 to 175nm. Molecular constants of the v' = 12 to 17 levels of the B(3)Sigma(u)(-) state have been determined. The (v', 0) band oscillator strengths were determined as 2.38, 2.62, 2.70, 2.66, 2.40, and 2.12 x 10(-5) for the bands from v' = 12 to 17, respectively. (C) 2003 Elsevier Science (USA). All rights reserved.
C1 Univ Tsukuba, Tsukuba, Ibaraki 3058573, Japan.
Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England.
KEK, Photon Factory, Tsukuba, Ibaraki 3050801, Japan.
Japan Womens Univ, Tokyo 1128681, Japan.
RP Yoshino, K (reprint author), Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058565, Japan.
RI Cheung, Allan/D-3059-2009
NR 36
TC 10
Z9 10
U1 1
U2 11
PU ACADEMIC PRESS INC ELSEVIER SCIENCE
PI SAN DIEGO
PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA
SN 0022-2852
J9 J MOL SPECTROSC
JI J. Mol. Spectrosc.
PD MAY
PY 2003
VL 219
IS 1
BP 45
EP 57
DI 10.1016/S0022-2852(03)00009-2
PG 13
WC Physics, Atomic, Molecular & Chemical; Spectroscopy
SC Physics; Spectroscopy
GA 684RW
UT WOS:000183221200005
ER
PT J
AU Laurance, WF
Merona, JMRD
Andrade, A
Laurance, SG
D'Angelo, S
Lovejoy, TE
Vasconcelos, HL
AF Laurance, WF
Merona, JMRD
Andrade, A
Laurance, SG
D'Angelo, S
Lovejoy, TE
Vasconcelos, HL
TI Rain-forest fragmentation and the phenology of Amazonian tree
communities
SO JOURNAL OF TROPICAL ECOLOGY
LA English
DT Article
DE Amazon; edge effects; flowering; fruiting; habitat fragmentation; leaf
production; plant reproduction; rain forest; trees
ID REPRODUCTIVE PHENOLOGY; POPULATION; RESPONSES; DYNAMICS; BEES
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Natl Inst Amazonian Res, INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama.
RI Laurance, William/B-2709-2012; Vasconcelos, Heraldo/C-3353-2013;
Laurance, Susan/G-6021-2011
OI Vasconcelos, Heraldo/0000-0001-6969-7131; Laurance,
Susan/0000-0002-2831-2933
NR 29
TC 21
Z9 22
U1 4
U2 16
PU CAMBRIDGE UNIV PRESS
PI NEW YORK
PA 40 WEST 20TH ST, NEW YORK, NY 10011-4221 USA
SN 0266-4674
J9 J TROP ECOL
JI J. Trop. Ecol.
PD MAY
PY 2003
VL 19
BP 343
EP 347
DI 10.1017/S0266467403003389
PN 3
PG 5
WC Ecology
SC Environmental Sciences & Ecology
GA 692JU
UT WOS:000183658600014
ER
PT J
AU Schroll, S
AF Schroll, S
TI Critical terms for art history, 2nd edition.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Libs, Washington, DC USA.
RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD MAY 1
PY 2003
VL 128
IS 8
BP 109
EP 109
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 672TA
UT WOS:000182536600053
ER
PT J
AU Thresher, R
Proctor, C
Ruiz, G
Gurney, R
MacKinnon, C
Walton, W
Rodriguez, L
Bax, N
AF Thresher, R
Proctor, C
Ruiz, G
Gurney, R
MacKinnon, C
Walton, W
Rodriguez, L
Bax, N
TI Invasion dynamics of the European shore crab, Carcinus maenas, in
Australia
SO MARINE BIOLOGY
LA English
DT Article
ID GREEN CRAB; DECAPODA; RECRUITMENT; DISPERSAL; LARVAE; CALIFORNIA;
IMPACT; SPREAD; SHELF; COAST
AB In Australia and most other invaded locations, rates of range expansion by the European shore crab, Carcinus maenas, are-typically only a few kilometres per year, despite a planktonic duration upwards of 50 days and off-shore larval development. This relatively static A distribution is punctuated by rare episodes of long-distance and large-scale spread, some of which appear to be related to unusual oceanographic conditions and some of which are likely to be human assisted. These observations suggest, first, that long planktonic duration and off-shore development in a marine invertebrate does not preclude very localised recruitment, and, second, that this recruitment norm may be punctuated by brief episodes of wide scale mixing of propagules. Punctuated dispersal has previously been suggested to account for large-scale biogeographic patterns of distribution and speciation, but may also have implications for the processes that stabilise structured spatial metapopulations.
C1 CSIRO, Ctr Res Introduced Marine Pests, Hobart, Tas 7001, Australia.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Univ Tasmania, Dept Zool, Taroona, Tas, Australia.
RP Thresher, R (reprint author), CSIRO, Ctr Res Introduced Marine Pests, GPO Box 1538, Hobart, Tas 7001, Australia.
EM Ron.Thresher@csiro.au
RI Thresher, Ronald/C-7442-2009; Bax, Nicholas/A-2321-2012; Proctor,
Craig/I-3710-2016;
OI Bax, Nicholas/0000-0002-9697-4963; Ruiz, Gregory/0000-0003-2499-441X
NR 46
TC 58
Z9 61
U1 2
U2 30
PU SPRINGER HEIDELBERG
PI HEIDELBERG
PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY
SN 0025-3162
EI 1432-1793
J9 MAR BIOL
JI Mar. Biol.
PD MAY
PY 2003
VL 142
IS 5
BP 867
EP 876
DI 10.1007/s00227-003-1011-1
PG 10
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 693NQ
UT WOS:000183724000005
ER
PT J
AU Sanchez, JA
McFadden, CS
France, SC
Lasker, HR
AF Sanchez, JA
McFadden, CS
France, SC
Lasker, HR
TI Molecular phylogenetic analyses of shallow-water Caribbean octocorals
SO MARINE BIOLOGY
LA English
DT Article
ID GORGONACEAN OCTOCORALS; SARCOPHYTON GLAUCUM; MITOCHONDRIAL-DNA; MISMATCH
REPAIR; COELENTERATA; CORAL; ANTHOZOA; CNIDARIA; GENE; SUBSTITUTION
AB Octocorals, especially gorgonians, are conspicuous on Caribbean coral reefs, but there is no consensus regarding species relationships. Mitochondrial protein-coding genes [NADH-dehydrogenase subunits 2 (ND2) and 6 (ND6), and mutS homolog (msh1), 1633 bp] from 28 shallow-water species were sequenced to develop the first molecular phylogeny for Caribbean octocorals. The specimens were collected primarily in the Caribbean or off Brazil in 1999-2001. Morphological characters (sclerites and axial ultrastructure) were also examined in order to map them onto the molecular phylogeny. Analyses of both nucleotide and amino acid substitutions using maximum parsimony and likelihood (including maximum-likelihood and Bayesian analysis) generated very similar results, with most nodes having high levels of support. These molecular results were significantly different from the generally accepted classification. Neither Plexauridae nor Gorgoniidae were monophyletic. Plexaurella spp., nominal plexaurids, were basal to the gorgoniids, sharing many morphological characters with them. This corroborates previous findings using secondary metabolites and biosynthetic pathways. The sea fans, Gorgonia spp. and Pacifigorgia spp., as well as the pinnate gorgonians, Muriceopsis flavida and Pseudopterogorgia spp., did not have sea fan or pinnate relatives, suggesting there has been convergent evolution of colony form. Caribbean plexaurids appeared more derived and/or recently evolved according to both morphological and molecular data (e.g. Eunicea spp. and Plexaura spp.). Molecular phylogenetics is a promising approach for reconstructing phylogenetic relationships among octocorals as well as to understand their complex morphology.
C1 SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA.
Harvey Mudd Coll, Dept Biol, Claremont, CA 91711 USA.
Coll Charleston, Dept Biol, Grice Marine Lab, Charleston, SC 29412 USA.
RP Sanchez, JA (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NMNH W 329,MRC-0163, Washington, DC 20013 USA.
RI Johnson, Selena/K-3541-2013
NR 60
TC 75
Z9 81
U1 1
U2 13
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD MAY
PY 2003
VL 142
IS 5
BP 975
EP 987
DI 10.1007/s00227-003-1018-7
PG 13
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 693NQ
UT WOS:000183724000015
ER
PT J
AU Myers, ST
Jackson, NJ
Browne, IWA
de Bruyn, AG
Pearson, TJ
Readhead, ACS
Wilkinson, PN
Biggs, AD
Blandford, RD
Fassnacht, CD
Koopmans, LVE
Marlow, DR
McKean, JP
Norbury, MA
Phillips, PM
Rusin, D
Shepherd, MC
Sykes, CM
AF Myers, ST
Jackson, NJ
Browne, IWA
de Bruyn, AG
Pearson, TJ
Readhead, ACS
Wilkinson, PN
Biggs, AD
Blandford, RD
Fassnacht, CD
Koopmans, LVE
Marlow, DR
McKean, JP
Norbury, MA
Phillips, PM
Rusin, D
Shepherd, MC
Sykes, CM
TI The Cosmic Lens All-Sky Survey - I. Source selection and observations
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE gravitational lensing; cosmology : observations
ID 4-IMAGE GRAVITATIONAL LENS; PHASE CALIBRATION SOURCES; RADIO-SOURCES;
SYSTEM; GALAXY; SPECTRUM; B2114+022; B1608+656; REDSHIFTS; B1152+199
AB The Cosmic Lens All-Sky Survey (CLASS) is an international collaborative programme which has obtained high-resolution radio images of over 10 000 flat-spectrum radio sources in order to create the largest and best-studied statistical sample of radio-loud gravitationally lensed systems. With this survey, combined with detailed studies of the lenses found therein, constraints can be placed on the expansion rate, matter density and dark energy (e.g. cosmological constant, quintessence) content of the Universe that are complementary to and independent of those obtained through other methods. CLASS is aimed at identifying lenses where multiple images are formed from compact flat-spectrum radio sources, which should be easily identifiable in the radio maps. Because CLASS is radio-based, dust obscuration in lensing galaxies is not a factor, and the relative insensitivity of the instrument to environmental conditions (e.g. weather, 'seeing') leads to nearly uniform sensitivity and resolution over the entire survey. In four observing 'seasons' from 1994 to 1999, CLASS has observed 13 783 radio sources with the Very Large Array (VLA) at 8.4 GHz in its largest 'A'-configuration (0.2-arcsec resolution). When combined with the Jodrell Bank VLA Astrometric Survey (JVAS), the CLASS sample contains over 16 000 images. A complete sample of 11 685 sources was observed, selected to have a flux density of at least 30 mJy in the Green Bank Survey (GB6) catalogue at 4.85 GHz (spanning the declination range 0degrees less than or equal to delta less than or equal to 75degrees and \b\ greater than or equal to 10degrees, excluding the Galactic plane) and a spectral index alpha greater than or equal to -0.5 between the NRAO-VLA Sky Survey (NVSS) at 1.4 GHz and the GB6. A typical 30-s CLASS snapshot reached an rms noise level of 0.4 mJy. So far, CLASS has found 16 new gravitational lens systems, and the JVAS/CLASS survey contains a total of 22 lenses. The follow-up of a small number of candidates using the VLA, MERLIN, the Very Long Baseline Array (VLBA) and optical telescopes is still underway. In this paper, we present a summary of the CLASS observations, the JVAS/CLASS sample, and statistics on sub-samples of the survey. An accompanying paper presents the lens candidate selection, and in a third paper the implications for cosmology are discussed.
C1 Natl Radio Astron Observ, Socorro, NM 87801 USA.
Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands.
Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands.
CALTECH, Pasadena, CA 91125 USA.
Space Telescope Sci Inst, Baltimore, MD 21218 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Myers, ST (reprint author), Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA.
EM smyers@nrao.edu
RI Pearson, Timothy/N-2376-2015
OI Pearson, Timothy/0000-0001-5213-6231
NR 63
TC 212
Z9 213
U1 1
U2 3
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2003
VL 341
IS 1
BP 1
EP 12
DI 10.1046/j.1365-8711.2003.06256.x
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 673JN
UT WOS:000182577300002
ER
PT J
AU Browne, IWA
Wilkinson, PN
Jackson, NJF
Myers, ST
Fassnacht, CD
Koopmans, LVE
Marlow, DR
Norbury, M
Rusin, D
Sykes, CM
Biggs, AD
Blandford, RD
de Bruyn, AG
Chae, KH
Helbig, P
King, LJ
McKean, JP
Pearson, TJ
Phillips, PM
Readhead, ACS
Xanthopoulos, E
York, T
AF Browne, IWA
Wilkinson, PN
Jackson, NJF
Myers, ST
Fassnacht, CD
Koopmans, LVE
Marlow, DR
Norbury, M
Rusin, D
Sykes, CM
Biggs, AD
Blandford, RD
de Bruyn, AG
Chae, KH
Helbig, P
King, LJ
McKean, JP
Pearson, TJ
Phillips, PM
Readhead, ACS
Xanthopoulos, E
York, T
TI The Cosmic Lens All-Sky Survey - II. Gravitational lens candidate
selection and follow-up
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE gravitation; gravitational lensing; radio continuum : galaxies
ID PHASE CALIBRATION SOURCES; TIME-DELAY MEASUREMENTS; HUBBLE SPACE
TELESCOPE; VLA ASTROMETRIC SURVEY; COMPACT RADIO-SOURCES; COSMOLOGICAL
CONSTANT; EXTRAGALACTIC SURVEYS; VLBI OBSERVATIONS; SYSTEM B1933+503;
CLASS B2319+051
AB We report the final results of the search for gravitationally lensed flat-spectrum radio sources found in the combination of CLASS (Cosmic Lens All-Sky Survey) and JVAS (Jodrell Bank VLA Astrometric Survey). VLA (Very Large Array) observations of 16 503 sources have been made, resulting in the largest sample of arcsec-scale lens systems available. Contained within the 16 503 sources is a complete sample of 11 685 sources which have two-point spectral indices between 1.4 and 5 GHz flatter than -0.5, and 5-GHz flux densities greater than or equal to30 mJy. A subset of 8958 sources form a well-defined statistical sample suitable for analysis of the lens statistics. We describe the systematic process by which 149 candidate lensed sources were picked from the statistical sample on the basis of possessing multiple compact components in the 0.2-arcsec resolution VLA maps. Candidates were followed up with 0.05-arcsec resolution MERLIN and 0.003-arcsec VLBA observations at 5 GHz and rejected as lens systems if they failed well-defined surface brightness and/or morphological tests. To illustrate the candidate elimination process, we show examples of sources representative of particular morphologies that have been ruled out by the follow-up observations. 194 additional candidates, not in the well-defined sample, were also followed up. Maps for all the candidates can be found on the World Wide Web at http://www.jb.man.ac.uk/research/gravlens/index.html. We summarize the properties of each of the 22 gravitational lens systems in JVAS/CLASS. 12 are double-image systems, nine are four-image systems and one is a six-image system. 13 constitute a statistically well-defined sample giving a point-source lensing rate of 1:690 +/- 190. The interpretation of the results in terms of the properties of the lensing galaxy population and cosmological parameters will be published elsewhere.
C1 Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
Netherlands Fdn Res Astron, NL-7990 AA Dwingeloo, Netherlands.
CALTECH, Pasadena, CA 91125 USA.
Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA.
Univ Groningen, Kapteyn Astron Inst, NL-9700 AA Groningen, Netherlands.
Univ Bonn, D-53121 Bonn, Germany.
STScI, Baltimore, MD 21218 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Browne, IWA (reprint author), Univ Manchester, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England.
EM iwb@jb.man.ac.uk
RI Pearson, Timothy/N-2376-2015
OI Pearson, Timothy/0000-0001-5213-6231
NR 115
TC 203
Z9 204
U1 1
U2 7
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAY 1
PY 2003
VL 341
IS 1
BP 13
EP 32
DI 10.1046/j.1365-8711.2003.06257.x
PG 20
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 673JN
UT WOS:000182577300003
ER
PT J
AU Arnold, AE
Herre, EA
AF Arnold, AE
Herre, EA
TI Canopy cover and leaf age affect colonization by tropical fungal
endophytes: Ecological pattern and process in Theobroma cacao
(Malvaceae)
SO MYCOLOGIA
LA English
DT Article
DE Barro Colorado Island; ecology; endophytic fungi; leaf chemistry; leaf
toughness; Panama; sporefall; tropical forest
ID PAECILOMYCES-FUMOSOROSEUS DEUTEROMYCOTINA; ENTOMOPATHOGENIC FUNGUS;
WATER-STRESS; MONILINIA-FRUCTICOLA; MYCELIAL GROWTH; PECAN SCAB;
DIVERSITY; LEAVES; GERMINATION; INFECTION
AB Fungal endophytes inhabit healthy tissues of all terrestrial plant taxa studied to date and arc diverse and abundant in leaves of tropical woody angiosperms. Studies have demonstrated that plant location and leaf age influence density of endophyte infection in leaves of tropical forest trees. However, ecological factors underlying these observations have not been explored in detail. Here, we establish that foliar endophytes of a tropical tree (Theobroma cacao, Malvaceae) are transmitted horizontally and that endophyte-free seedlings can be produced for experimental manipulation by protecting aerial tissues from surface wetting. At Barro Colorado Island, Panama, we used transects of endophyte-free seedlings to determine the importance of several factors (canopy cover, abundance of aerial and epiphytic propagules, leaf age, leaf chemistry, leaf toughness and duration of exposure to viable air spora) in shaping colonization by endophytic fungi. Endophytes colonized leaves of T cacao more rapidly beneath the forest canopy than in cleared sites, reflecting local abundance of aerial and epiphytic propagules. The duration of exposure, rather than absolute leaf age, influenced endophyte infection, whereas leaf toughness and chemistry had no observed effect. Endophytes isolated from mature T cacao grew more rapidly on media containing leaf extracts of T cacao than on media containing extracts from other co-occurring tree species, suggesting that interspecific differences in leaf chemistry influence endophyte assemblages. Together, these data allow us to identify factors underlying patterns of endophyte colonization within healthy leaves of this tropical tree.
C1 Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
Smithsonian Trop Res Inst, Balboa 2072, Panama.
RP Arnold, AE (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA.
NR 76
TC 125
Z9 139
U1 4
U2 54
PU NEW YORK BOTANICAL GARDEN
PI BRONX
PA PUBLICATIONS DEPT, BRONX, NY 10458 USA
SN 0027-5514
J9 MYCOLOGIA
JI Mycologia
PD MAY-JUN
PY 2003
VL 95
IS 3
BP 388
EP 398
DI 10.2307/3761880
PG 11
WC Mycology
SC Mycology
GA 705KG
UT WOS:000184393800002
PM 21156627
ER
PT J
AU Sweeney, A
Jiggins, C
Johnsen, S
AF Sweeney, A
Jiggins, C
Johnsen, S
TI Insect communication: Polarized light as a butterfly mating signal
SO NATURE
LA English
DT Article
ID COLOR
C1 Duke Univ, Dept Biol, Durham, NC 27708 USA.
Smithsonian Trop Res Inst, Balboa, Panama.
Univ Edinburgh, Inst Cell Anim & Populat Biol, Edinburgh EH9 3JT, Midlothian, Scotland.
RP Sweeney, A (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA.
RI Jiggins, Chris/B-9960-2008
OI Jiggins, Chris/0000-0002-7809-062X
NR 12
TC 125
Z9 131
U1 2
U2 42
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD MAY 1
PY 2003
VL 423
IS 6935
BP 31
EP 32
DI 10.1038/423031a
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 673CG
UT WOS:000182561600030
PM 12721616
ER
PT J
AU Takacs, E
Silver, E
Laming, JM
Gillaspy, JD
Schnopper, H
Brickhouse, N
Barbera, M
Mantraga, M
Ratliff, LP
Tawara, H
Makonyi, K
Madden, N
Landis, D
Beeman, J
Haller, EE
AF Takacs, E
Silver, E
Laming, JM
Gillaspy, JD
Schnopper, H
Brickhouse, N
Barbera, M
Mantraga, M
Ratliff, LP
Tawara, H
Makonyi, K
Madden, N
Landis, D
Beeman, J
Haller, EE
TI Astrophysics and spectroscopy with microcalorimeters on an electron beam
ion trap
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 11th International Conference on the Physics of Highly Charged Ions (HCI
2002)
CY SEP 01-06, 2002
CL CAEN, FRANCE
DE electron beam ion trap; X-ray; microcalorimeter; highly charged ion;
laboratory astrophysics
ID X-RAY SPECTROSCOPY; TRANSMISSION GRATING SPECTROMETER; FE-XVII;
LABORATORY ASTROPHYSICS; EMISSION; SPECTRA; CAPELLA; TEMPERATURE;
INTENSITY; PROGRESS
AB Electron beam ion traps combined with X-ray microcalorimeters provide an indispensable tool for laboratory astrophysics supporting recent and future X-ray missions. The program at the National Institute of Standards and Technology uses spectroscopic methods to study highly ionized plasmas and atomic physics related to astrophysics problems (C) 2003 Elsevier Science B.V. All rights reserved.
C1 Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
MIT, Cambridge, MA USA.
Debrecen Univ, H-4026 Debrecen, Hungary.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
USN, Res Lab, EO Hulburt Ctr Space Res, Washington, DC 20375 USA.
INAF, Osserv Astron Palermo GS Vaiana, Palermo, Italy.
Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
RP Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
EM endre.takacs@nist.gov
OI Brickhouse, Nancy/0000-0002-8704-4473; Barbera,
Marco/0000-0002-3188-7420
NR 36
TC 6
Z9 6
U1 0
U2 3
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
EI 1872-9584
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD MAY
PY 2003
VL 205
BP 144
EP 155
DI 10.1016/S0168-583X(03)00937-6
PG 12
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 684MM
UT WOS:000183211200028
ER
PT J
AU Beiersdorfer, P
Behar, E
Boyce, KR
Brown, GV
Chen, H
Gendreau, KC
Graf, A
Gu, MF
Harris, CL
Kahn, SM
Kelley, RL
Lepson, JK
May, MJ
Neill, PA
Pinnington, EH
Porter, FS
Smith, AJ
Stahle, CK
Szymkowiak, AE
Tillotson, A
Thorn, DB
Trabert, E
Wargelin, BJ
AF Beiersdorfer, P
Behar, E
Boyce, KR
Brown, GV
Chen, H
Gendreau, KC
Graf, A
Gu, MF
Harris, CL
Kahn, SM
Kelley, RL
Lepson, JK
May, MJ
Neill, PA
Pinnington, EH
Porter, FS
Smith, AJ
Stahle, CK
Szymkowiak, AE
Tillotson, A
Thorn, DB
Trabert, E
Wargelin, BJ
TI Overview of the Livermore electron beam ion trap project
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 11th International Conference on the Physics of Highly Charged Ions (HCI
2002)
CY SEP 01-06, 2002
CL CAEN, FRANCE
DE electron beam ion trap; SuperEBIT; microcalorimeter; spectroscopy (X-ray
and optical)
ID M1 TRANSITION RATES; HIGH-RESOLUTION; FE-XVII; LINES; MICROCALORIMETER;
SPECTROMETER; INTENSITY
AB The Livermore electron beam ion trap facility has recently been moved to a new location within LLNL, and new instrumentation was added, including a 32-pixel microcalorimeter. The move was accompanied by a shift of focus toward in situ measurements of highly charged ions, which continue with increased vigor. Overviews of the facility, which includes EBIT-I and SuperEBIT, and the research projects are given, including results from optical spectroscopy, QED, and X-ray line excitation measurements. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 Lawrence Livermore Natl Lab, Livermore, CA 94550 USA.
Columbia Univ, New York, NY 10027 USA.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
Univ Calif Davis, Davis, CA 95616 USA.
MIT, Cambridge, MA 02139 USA.
Univ Nevada, Reno, NV 89557 USA.
Univ Calif Berkeley, Berkeley, CA 94720 USA.
Univ Alberta, Edmonton, AB T6G 2J1, Canada.
Morehouse Coll, Atlanta, GA 30314 USA.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Beiersdorfer, P (reprint author), Lawrence Livermore Natl Lab, L-260, Livermore, CA 94550 USA.
RI Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012
OI Porter, Frederick/0000-0002-6374-1119;
NR 31
TC 11
Z9 11
U1 0
U2 1
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD MAY
PY 2003
VL 205
BP 173
EP 177
DI 10.1016/S0168-583X(03)00941-8
PG 5
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 684MM
UT WOS:000183211200032
ER
PT J
AU Matranga, M
Barbera, M
Maggio, A
Peres, G
Serio, S
Takacs, E
Silver, E
Gillaspy, J
Schnopper, H
Laming, M
Beeman, J
Haller, E
Madden, N
AF Matranga, M
Barbera, M
Maggio, A
Peres, G
Serio, S
Takacs, E
Silver, E
Gillaspy, J
Schnopper, H
Laming, M
Beeman, J
Haller, E
Madden, N
TI EBIT diagnostics using X-ray spectra of highly ionized Ne
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 11th International Conference on the Physics of Highly Charged Ions (HCI
2002)
CY SEP 01-06, 2002
CL CAEN, FRANCE
DE X-ray spectra; EBIT; excitation; ionization of atoms
ID BEAM ION-TRAP; LABORATORY ASTROPHYSICS
AB We have carried out a detailed analysis of highly ionized neon spectra collected at the NIST EBIT using an NTD germanium X-ray microcalorimeter developed at the Harvard-Smithsonian Center for Astrophysics [Nucl. Instr. and Meth. A 444 (2000) 156]. Our attention was focused especially on the Ne IX He-like triplet to check electron density diagnostics through the intercombination/forbidden line ratio. We have investigated possible effects of the ion dynamics on the plasma emission line intensities, looking at the dependence of the count-rate and the charge state distribution on the electron beam energy and current. The temperature and spatial distribution of the neon ions, and hence the overlap between the electron beam and the ion cloud, depend on the electron beam operating parameters. The overlap affects the average electron density seen by the ions, and in turn the measured line ratio. These results underscore the value of future improved studies of the trapped ion dynamics, both for understanding the EBIT performance and for allowing experimenters to take full advantage of its potential for astrophysical plasma diagnostics. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 INAF, Osserv Astron Palermo, I-90134 Palermo, Italy.
Univ Palermo, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy.
MIT, Cambridge, MA 02139 USA.
Univ Debrecen, H-4026 Debrecen, Hungary.
Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
Natl Inst Stand & Technol, Gaithersburg, MD 20899 USA.
USN, Res Lab, Washington, DC 20375 USA.
Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA.
RP INAF, Osserv Astron Palermo, I-90134 Palermo, Italy.
EM barbera@astropa.unipa.it
RI Maggio, Antonio/P-5700-2015;
OI Maggio, Antonio/0000-0001-5154-6108; Barbera, Marco/0000-0002-3188-7420;
PERES, Giovanni/0000-0002-6033-8180
NR 11
TC 6
Z9 6
U1 0
U2 4
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
EI 1872-9584
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD MAY
PY 2003
VL 205
BP 244
EP 249
DI 10.1016/S0168-583X(03)00943-1
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 684MM
UT WOS:000183211200047
ER
PT J
AU Merabet, H
Bruch, R
Fulling, S
Bailey, M
Godunov, AL
McGuire, JH
Grum-Grzhimailo, AN
Bartschat, K
AF Merabet, H
Bruch, R
Fulling, S
Bailey, M
Godunov, AL
McGuire, JH
Grum-Grzhimailo, AN
Bartschat, K
TI Ionization-excitation magnetic sublevel cross sections for He+
(2p)P-2(0) states following fast electron and proton impact
SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM
INTERACTIONS WITH MATERIALS AND ATOMS
LA English
DT Article; Proceedings Paper
CT 11th International Conference on the Physics of Highly Charged Ions (HCI
2002)
CY SEP 01-06, 2002
CL CAEN, FRANCE
DE ionization-excitation; sublevel cross sections; electron impact; proton
impact; helium
ID HELIUM; EMISSION; SYSTEMS; ATOMS
AB The first experimental magnetic substate scattering-angle-integrated cross sections following ionization-excitation of He(1s(2))S-1 to He-(2p) P-2(0) in the e(-) + He collision system have been determined using a combination of total cross sections and polarization fraction measurements in the extreme ultraviolet range. The derived magnetic sublevel cross sections, sigma(0) and sigma(1), for M-L = 0, +/-1 have been studied over a wide range of electron velocities (2-8.5 a.u.). These results are compared with previous cross sections for equi-velocity proton impact. In addition, our experimental data are compared with earlier theoretical predictions, our recent second-Born calculations fully including off-energy shell terms, and new R-matrix results. We have extended our polarization measurements for H+ + He collisions and found excellent agreement between theory and experiment at nearly all impact energies. However, the present second-Born and R-matrix results deviate slightly from the experimental electron data. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 Univ Nevada, Dept Phys, Reno, NV 89557 USA.
Tulane Univ, Dept Phys, New Orleans, LA 70118 USA.
Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA.
Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.
Moscow MV Lomonosov State Univ, Inst Nucl Phys, Moscow 119992, Russia.
Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA.
RP Univ Nevada, Dept Phys, Reno, NV 89557 USA.
EM hocine@physics.unr.edu
RI Godunov, Alexander/G-4266-2011; Grum-Grzhimailo, Alexei/D-6274-2012;
Bartschat, Klaus/I-2527-2012
NR 21
TC 0
Z9 0
U1 0
U2 0
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0168-583X
EI 1872-9584
J9 NUCL INSTRUM METH B
JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms
PD MAY
PY 2003
VL 205
BP 399
EP 404
DI 10.1016/S0168-583X(02)02047-5
PG 6
WC Instruments & Instrumentation; Nuclear Science & Technology; Physics,
Atomic, Molecular & Chemical; Physics, Nuclear
SC Instruments & Instrumentation; Nuclear Science & Technology; Physics
GA 684MM
UT WOS:000183211200078
ER
PT J
AU Janzen, PH
Gardner, LD
Reisenfeld, DB
Kohl, JL
AF Janzen, PH
Gardner, LD
Reisenfeld, DB
Kohl, JL
TI Absolute cross section for Si2+(3s3p P-3(o)-> 3s3p P-1(o))
electron-impact excitation
SO PHYSICAL REVIEW A
LA English
DT Article
ID SOLAR TRANSITION REGION; 3S(2) S-1->3S3P P-3; RESONANCE STRUCTURE; LINE
RATIOS; IONS; INTERFERENCE
AB We have measured the absolute energy-averaged cross section for electron-impact excitation of Si2+(3s3p P-3(o)-->3s3p P-1(o)) from energies below threshold to the turn-on of the 3s3p P-3(o)-->3p(2) P-3 transition. A beams modulation technique with inclined electron and ion beams was used. Radiation at 120.65 nm from the decay of the excited ions to the 3s(2) S-1 ground state was detected using an absolutely calibrated optical system. The fractional population of metastable Si2+(3s3p P-3(o)) in the incident ion beam was determined to be 0.256+/-0.035(1.65sigma). The experimental energy spread ranged from 0.85 eV (full width at half maximum) at the lowest energies to 0.56 eV at the highest. Resonance features consistent with 12-state close-coupling R-matrix calculations are seen.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Janzen, PH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Reisenfeld, Daniel/F-7614-2015
NR 28
TC 4
Z9 4
U1 0
U2 0
PU AMERICAN PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 1050-2947
J9 PHYS REV A
JI Phys. Rev. A
PD MAY
PY 2003
VL 67
IS 5
AR 052702
DI 10.1103/PhysRevA.67.052702
PG 7
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 686AU
UT WOS:000183298800054
ER
PT J
AU Krems, RV
Dalgarno, A
AF Krems, RV
Dalgarno, A
TI Threshold laws for collisional reorientation of electronic angular
momentum
SO PHYSICAL REVIEW A
LA English
DT Article
ID ULTRACOLD MOLECULES; COLD; TEMPERATURES
AB It is shown that the velocity dependence of cross sections for projection-changing transitions in collisions of paramagnetic atoms or molecules with structureless targets near threshold has the form v(2Deltam) when Deltam is even and v(2(Deltam+1)) when Deltam is odd, where Deltam is the change in the projection quantum number and v is the relative velocity.
C1 Harvard Smithsonian Ctr Astrophys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Harvard Smithsonian Ctr Astrophys, Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA.
EM rkrems@cfa.harvard.edu
NR 15
TC 26
Z9 26
U1 1
U2 2
PU AMER PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 2469-9926
EI 2469-9934
J9 PHYS REV A
JI Phys. Rev. A
PD MAY
PY 2003
VL 67
IS 5
AR 050704
DI 10.1103/PhysRevA.67.050704
PG 3
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 686AU
UT WOS:000183298800008
ER
PT J
AU Laurance, WF
AF Laurance, WF
TI Slow burn: the insidious effects of surface fires on tropical forests
SO TRENDS IN ECOLOGY & EVOLUTION
LA English
DT Article
ID EL-NINO; AMAZONIAN FORESTS; EASTERN AMAZON; CLIMATE-CHANGE; GROUND
FIRES; RAIN-FOREST; RESPONSES; ECOLOGY; IMPACT; EVENT
AB Accidental surface fires are emerging as one of the most pervasive threats to tropical forests. Although unimpressive in appearance, these fires can have surprisingly potent impacts on rainforest plant and animal communities, as demonstrated by recent studies led by Jos Barlow and Carlos Peres in central Amazonia. Even worse, surface fires greatly increase the likelihood of far larger conflagrations that can lead to complete forest destruction.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
RP Laurance, WF (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama.
RI Laurance, William/B-2709-2012
NR 25
TC 37
Z9 39
U1 2
U2 14
PU ELSEVIER SCIENCE LONDON
PI LONDON
PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND
SN 0169-5347
J9 TRENDS ECOL EVOL
JI Trends Ecol. Evol.
PD MAY
PY 2003
VL 18
IS 5
BP 209
EP 212
DI 10.1016/S0169-5347(03)00064-8
PG 4
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 682XF
UT WOS:000183117100002
ER
PT J
AU Temeles, EJ
Kress, WJ
AF Temeles, EJ
Kress, WJ
TI Adaptation in a plant-hummingbird association
SO SCIENCE
LA English
DT Article
ID AGE-SEX CLASSES; RUFOUS HUMMINGBIRDS; DIMORPHISM; BEHAVIOR
AB Sexual dimorphism in bill morphology and body size of the Caribbean purple-throated carib hummingbird is associated with a reversal in. oral dimorphism of its Heliconia food plants. This hummingbird is the sole pollinator of H. caribaea and H. bihai, with flowers of the former corresponding to the short, straight bills of males, the larger sex, and flowers of the latter corresponding to the long, curved bills of females. On St. Lucia, H. bihai compensates for the rarity of H. caribaea by evolving a second color morph with flowers that match the bills of males, whereas on Dominica, H. caribaea evolves a second color morph with flowers that match the bills of females. The nectar rewards of all Heliconia morphs are consistent with each sex's choice of the morph that corresponds to its bill morphology and energy requirements, supporting the hypothesis that feeding preferences have driven their coadaptation.
C1 Amherst Coll, Dept Biol, Amherst, MA 01002 USA.
Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, MRC166, Washington, DC 20013 USA.
RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA.
NR 16
TC 96
Z9 97
U1 3
U2 63
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 APR 25
PY 2003
VL 300
IS 5619
BP 630
EP 633
DI 10.1126/science.1080003
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 671FB
UT WOS:000182453700039
PM 12714743
ER
PT J
AU Schneider, R
Ferrara, A
Salvaterra, R
Omukai, K
Bromm, V
AF Schneider, R
Ferrara, A
Salvaterra, R
Omukai, K
Bromm, V
TI Low-mass relics of early star formation
SO NATURE
LA English
DT Article
ID NUCLEOSYNTHESIS
AB The earliest stars to form in the Universe were the first sources of light, heat and metals after the Big Bang. The products of their evolution will have had a profound impact on subsequent generations of stars. Recent studies(1-7) of primordial star formation have shown that, in the absence of metals (elements heavier than helium), the formation of stars with masses 100 times that of the Sun would have been strongly favoured, and that low-mass stars could not have formed before a minimum level of metal enrichment had been reached. The value of this minimum level is very uncertain, but is likely to be between 10(-6) and 10(-4) that of the Sun(6,8). Here we show that the recent discovery(9) of the most iron-poor star known indicates the presence of dust in extremely low-metallicity gas, and that this dust is crucial for the formation of lower-mass second-generation stars that could survive until today. The dust provides a pathway for cooling the gas that leads to fragmentation of the precursor molecular cloud into smaller clumps, which become the lower-mass stars.
C1 Osserv Astrofis Arcetri, I-50125 Florence, Italy.
Enrico Fermi Ctr, I-00184 Rome, Italy.
Scuola Int Super Studi Avanzati, SSISA, I-34100 Trieste, Italy.
Natl Astron Observ, Div Theoret Astrophys, Tokyo 1818588, Japan.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schneider, R (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy.
RI Ferrara, Andrea/A-4357-2011; Schneider, Raffaella/E-4216-2017;
OI Schneider, Raffaella/0000-0001-9317-2888; Salvaterra,
Ruben/0000-0002-9393-8078
NR 14
TC 155
Z9 155
U1 2
U2 4
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 24
PY 2003
VL 422
IS 6934
BP 869
EP 871
DI 10.1038/nature01579
PG 3
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 670WR
UT WOS:000182432600047
PM 12712198
ER
PT J
AU Dickerson, PW
AF Dickerson, PW
TI Intraplate mountain building in response to continent-continent
collision - the Ancestral Rocky Mountains (North America) and inferences
drawn from the Tien Shan (Central Asia)
SO TECTONOPHYSICS
LA English
DT Article; Proceedings Paper
CT Annual Conference on Collisional Orogenesis in the Geological Record and
Modern Analogues
CY 2001
CL SION, SWITZERLAND
DE Tien Shan; Ancestral Rocky Mountains; tectonics; neotectonics;
intraplate deformation; late Paleozoic; India; Eurasia; Laurentia;
Gondwana; lithosphere
ID LATE PALEOZOIC DEFORMATION; UNITED-STATES; MEXICO; EVOLUTION; TEXAS;
LITHOSPHERE; CHIHUAHUA; EXAMPLES; MARGIN; BASIN
AB The intraplate Ancestral Rocky Mountains of western North America extend from British Columbia, Canada, to Chihuahua, Mexico, and formed during Early Carboniferous through Early Permian time in response to continent-continent collision of Laurentia with Gondwana-the conjoined masses of Africa and South America, including Yucatan and Florida. Uplifts and flanking basins also formed within the Laurentian Midcontinent. On the Gondwanan continent, well inboard from the marginal fold belts, a counterpart structural array developed during the same period. Intraplate deformation began when full collisional plate coupling had been achieved along the continental margin; the intervening ocean had been closed and subduction had ceased-that is, the distinction between upper versus lower plates became moot. Ancestral Rockies deformation was not accompanied by volcanism. Basement shear zones that formed during Mesoproterozoic rifting of Laurentia were reactivated and exerted significant control on the locations, orientations, and modes of displacement on late Paleozoic faults.
Ancestral Rocky Mountain uplifts extend as far south as Chihuahua and west Texas (28degrees to 33degreesN, 102degrees to 109degreesW) and include the Florida-Moyotes, Placer de Guadalupe-Carrizalillo, Ojinaga-Tascotal and Hueco Mountain blocks, as well as the Diablo and Central Basin Platforms. All are cored with Laurentian Proterozoic crystalline basement rocks and host correlative Paleozoic stratigraphic successions. Pre-late Paleozoic deformational, thermal, and metamorphic histories are similar as well. Southern Ancestral Rocky Mountain structures terminate along a line that trends approximately N 40degreesE (present coordinates), a common orientation for Mesoproterozoic extensional structures throughout southern to central North America.
Continuing Tien Shan intraplate deformation (Central Asia) has created an analogous array of uplifts and basins in response to the collision of India with Eurasia, beginning in late Miocene time when full coupling of the colliding plates had occurred. As in the Laurentia-Gondwana case, structures of similar magnitude and spacing to those in Eurasia have developed in the Indian plate. Within the present orogen two ancient suture zones have been reactivated-the early Paleozoic Terskey zone and the late Paleozoic Turkestan suture between the Siberian and East Gondwanan cratons. Inverted Proterozoic to early Paleozoic rift structures and passive-margin deposits are exposed north of the Terskey zone. In the Alay and Tarim complexes, Vendian to mid-Carboniferous passive-margin strata and the subjacent Proterozoic crystalline basement have been uplifted. Data on Tien Shan uplifts, basins, structural arrays, and deformation rates guide paleotectonic interpretations of ancient intraplate mountain belts. Similarly,. exhumed deep crustal shear zones in the Ancestral Rockies offer insight into partitioning and reorientation of strain, during contemporary intraplate deformation. (C) 2003 Elsevier Science B.V. All rights reserved.
C1 NASA, Lyndon B Johnson Space Ctr, Lockheed Martin, Houston, TX 77058 USA.
RP Dickerson, PW (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 66
TC 9
Z9 10
U1 0
U2 8
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0040-1951
J9 TECTONOPHYSICS
JI Tectonophysics
PD APR 24
PY 2003
VL 365
IS 1-4
SI SI
BP 129
EP 142
DI 10.1016/S0040-1951(03)00019-2
PG 14
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 674ND
UT WOS:000182642100007
ER
PT J
AU Nizinski, MS
AF Nizinski, MS
TI Annotated checklist of decapod crustaceans of Atlantic coastal and
continental shelf waters of the United States
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Review
ID LOBSTER PANULIRUS-ARGUS; GULF-OF-MEXICO; CRAB CARCINUS-MAENAS; WESTERN
ATLANTIC; HEMIGRAPSUS-SANGUINEUS; NORTHWESTERN ATLANTIC; MOLECULAR
PHYLOGENY; HERMIT-CRABS; CALLIANASSIDAE CRUSTACEA; TOMOPAGURUS CRUSTACEA
AB The decapod crustacean assemblage inhabiting estuarine, neritic and continental shelf waters (to 190 m) of the temperate eastern United States is diverse, with 391 species reported from Maine to Cape Canaveral, Florida. Three recognized biogeographic provinces (Boreal in part, Virginian and Carolinian) are included in this region. The assemblage contains 122 shrimp species (28 penaeids, 2 stenopodids, and 92 carideans), 10 thalassinideans, 8 lobsters, 61 anomurans and 190 brachyurans. Since previous compilation of this fauna, 12 additional species have been described, including four carideans, one callianassid, four anomurans, and three brachyurans. Range extensions into the region have been reported for another five species (Parapenaeus americanus, Scyllarides aequinoctialis, Petrolisthes armatus, Dromia erythropus, Clythrocerus nitidus). One species, Hemigrapsus sanguineus, has been introduced and become established throughout intertidal environments from southern Maine to northern North Carolina. Six species previously recorded from this region are no longer considered to occur there. Two of these species occur south of the Carolinian biogeographic province, three others are now known to occur only in the Pacific Ocean, and one species previously considered as likely to occur in the region has never actually been recorded there. Scientific nomenclature for all species recorded from the region is updated and referenced. Geographic distributions are summarized for each species incorporating recent published information where available.
C1 Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA.
RP Nizinski, MS (reprint author), Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, POB 37012,NHB,MRC-0153, Washington, DC 20013 USA.
NR 176
TC 35
Z9 40
U1 1
U2 7
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 APR 23
PY 2003
VL 116
IS 1
BP 96
EP 157
PG 62
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 672PH
UT WOS:000182529200010
ER
PT J
AU Blow, WC
AF Blow, WC
TI New brachyuran crabs (Crustacea : Decapoda) from the Upper Pliocene
Yorktown Formation of southeastern Virginia
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB Six new species of crabs, representing three families and one new genus, are described and illustrated from the Upper Pliocene Yorktown Formation of southeastern Virginia. They are remarkable for their state of preservation and represent the first fossil record for three of these living genera in Virginia's rich Neogene marine deposits. The presence of Stenocionops along with the common occurrence of Persephona in these deposits suggests that warm temperate waters covered southeastern Virginia during the deposition of late Yorktown sediments.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
RP Blow, WC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
NR 42
TC 4
Z9 7
U1 0
U2 0
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 APR 23
PY 2003
VL 116
IS 1
BP 168
EP 189
PG 22
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 672PH
UT WOS:000182529200012
ER
PT J
AU Bayer, FM
Cairns, SD
AF Bayer, FM
Cairns, SD
TI A new genus of the scleraxonian family Coralliidae (Octocorallia :
Gorgonacea)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB A new genus of the family Coralliidae is established for seven species having longitudinally grooved axes and autozooids seated in distinctive axial pits with beaded margins.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20013 USA.
RP Bayer, FM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, POB 37012, Washington, DC 20013 USA.
NR 28
TC 23
Z9 25
U1 0
U2 0
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 APR 23
PY 2003
VL 116
IS 1
BP 222
EP 228
PG 7
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 672PH
UT WOS:000182529200017
ER
PT J
AU Robinson, H
AF Robinson, H
TI New taxa and combinations of Ageratina from Ecuador, Colombia, and
Venezuela (Eupatorieae : Oxylobinae)
SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON
LA English
DT Article
AB Thirteen new species, one new combination, and one new forma of Ageratina are validated, mostly from from Ecuador, some from Colombia and Venezuela. The new taxa in subg. Ageratina are Ageratina adenophoroides, A. campii, A. cumbensis, A. cumbensis f. glandulifera, A. ewanii, A. parviceps, A. pseudogracilis, A. rosei, A. serrulata, A. villonacoensis, and A. websteri, with a new combination for A. rhodopappa f. glandularis. New species in subg. Andinia are A. harlingii, A. maranonii, and A. regalis.
C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA.
RP Robinson, H (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA.
NR 4
TC 0
Z9 0
U1 0
U2 0
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 APR 23
PY 2003
VL 116
IS 1
BP 229
EP 255
PG 27
WC Biology
SC Life Sciences & Biomedicine - Other Topics
GA 672PH
UT WOS:000182529200018
ER
PT J
AU Balakrishnan, N
Groenenboom, GC
Krems, RV
Dalgarno, A
AF Balakrishnan, N
Groenenboom, GC
Krems, RV
Dalgarno, A
TI The He-CaH((2)Sigma(+)) interaction. II. Collisions at cold and
ultracold temperatures
SO JOURNAL OF CHEMICAL PHYSICS
LA English
DT Article
ID VIBRATIONAL-RELAXATION; INELASTIC-COLLISIONS; DIATOMIC MOLECULE; NEUTRAL
MOLECULES; CHEMICAL PHYSICS; ENERGY-TRANSFER; SCATTERING; AR;
SUPERCHEMISTRY; RESONANCE
AB We present cross sections for rotational, vibrational, and fine-structure transitions in He-CaH((2)Sigma) collisions at cold and ultracold temperatures calculated using the ab initio potential energy surface reported in the preceding paper. Rotational quenching is fast, vibrational quenching is slow. The spin-rotational interaction, although small and having no influence at temperatures above 10 K, changes significantly the rate coefficients for rotational quenching at lower temperatures. The theoretical rotational, vibrational, and elastic cross sections are compared with the results of a buffer gas cooling experiment carried out at a temperature of about 0.4 K. The theoretical predictions for the vibrational and elastic cross sections are larger than the measured values. The sensitivity to the potential energy surface is explored. A modified surface diminishes but does not remove the differences between theory and experiment. (C) 2003 American Institute of Physics.
C1 Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
Univ Nijmegen, Inst Theoret Chem, NSRIM, NL-6525 ED Nijmegen, Netherlands.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Balakrishnan, N (reprint author), Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA.
EM naduvala@unlv.edu; gerritg@theochem.kun.nl; rkrems@cfa.harvard.edu;
adalgarno@cfa.harvard.edu
RI Groenenboom, Gerrit/F-9692-2015
NR 55
TC 63
Z9 64
U1 0
U2 3
PU AMER INST PHYSICS
PI MELVILLE
PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1,
MELVILLE, NY 11747-4501 USA
SN 0021-9606
J9 J CHEM PHYS
JI J. Chem. Phys.
PD APR 22
PY 2003
VL 118
IS 16
BP 7386
EP 7393
DI 10.1063/1.1562947
PG 8
WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical
SC Chemistry; Physics
GA 666CH
UT WOS:000182157700027
ER
PT J
AU O'Sullivan, E
Ponman, TJ
Collins, RS
AF O'Sullivan, E
Ponman, TJ
Collins, RS
TI X-ray scaling properties of early-type galaxies
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies : elliptical and lenticular, cD; galaxies : haloes; X-rays :
galaxies
ID ELLIPTIC GALAXIES; DARK-MATTER; PSPC OBSERVATIONS; POOR CLUSTERS; HOT
PLASMA; ROSAT; GAS; EMISSION; LUMINOSITIES; CATALOG
AB We present an analysis of 39 X-ray luminous early-type galaxies observed with the ROSAT PSPC. Using multicomponent spectral and spatial fits to these data, we have measured halo abundance, temperature, luminosity and surface brightness profile. We compare these measurements to similar results from galaxy groups and clusters, fitting a number of relations commonly used in the study of these larger objects. In particular, we find that the sigma-T-X relation for our sample is similar to that reported for clusters, consistent with beta(spec)=1, and that the L-X-T-X relation has a steep slope (gradient 4.8+/-0.7) comparable with that found for galaxy groups. Assuming isothermality, we construct three-dimensional models of our galaxies, allowing us to measure gas entropy. We find no correlation between gas entropy and system mass, but do find a trend for low-temperature systems to have reduced gas fractions. We conclude that the galaxies in our sample are likely to have developed their haloes through galaxy winds, influenced by their surrounding environment.
C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Collins, Ross/G-1450-2010
NR 79
TC 91
Z9 91
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 21
PY 2003
VL 340
IS 4
BP 1375
EP 1399
DI 10.1046/j.1365-8711.2003.06396.x
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665KC
UT WOS:000182118200030
ER
PT J
AU Sun, M
Jones, C
Murray, SS
Allen, SW
Fabian, AC
Edge, AC
AF Sun, M
Jones, C
Murray, SS
Allen, SW
Fabian, AC
Edge, AC
TI Chandra observations of the galaxy cluster A478: The interaction of hot
gas and radio plasma in the core, and an improved determination of the
compton y-parameter
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE distance scale; galaxies : clusters : individual (A478); radio continuum
: galaxies; X-rays : galaxies : clusters
ID HYDRA-A CLUSTER; COOLING FLOW; HUBBLE CONSTANT; RAY; ABELL-2052;
ABELL-478; REDSHIFT; BUBBLES
AB We present the results from a 42 ks Chandra ACIS observation of the galaxy cluster A478. This cluster is generally considered to be highly relaxed. The Chandra image reveals, for the first time, X-ray cavities in the hot gas within the central 15 kpc radius of A478. Two weak and small (similar to4 kpc) radio lobes that extend from the central nucleus are detected in a 1.4 GHz VLA observation. The radio lobes are roughly along the direction of the X-ray cavities, but are much smaller than the X-ray cavities. We propose a "doughnut" configuration for the hot gas within the central 15 kpc, created by the interaction of the gas with the radio plasma that originated from the nucleus. The current radio activity of the central radio source is weak (similar to0.2% of Hydra A) and the total radio power is at least 10 times smaller than the minimum power needed to create the cavities. We compare A478 with other galaxy clusters in which similar X-ray cavities were found. A478 and A4059 host much weaker central radio sources than do others with similarly sized X-ray cavities. On larger scales, deprojected temperature and density profiles are obtained for A478. We used these to derive the Compton y-parameter, for the first time, through direct integration. The result has a much smaller statistical uncertainty than previous ones. This serves as an example of how high-quality X-ray data can help constrain H-0. The corresponding H-0 also was derived combining the available Sunyaev-Zeldovich effect measurement.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Univ Durham, Dept Phys, Durham DH1 3LE, England.
RP Sun, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 31
TC 47
Z9 47
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2003
VL 587
IS 2
BP 619
EP 624
DI 10.1086/368300
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 666CR
UT WOS:000182159400014
ER
PT J
AU Fish, VL
Reid, MJ
Wilner, DJ
Churchwell, E
AF Fish, VL
Reid, MJ
Wilner, DJ
Churchwell, E
TI HI absorption toward ultracompact HII regions: Distances and Galactic
structure
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Galaxy : disk; Galaxy : structure; HII regions; radio lines : ISM
ID II-REGIONS; KINEMATIC DISTANCES; SPIRAL STRUCTURE; STAR-FORMATION;
GALAXY; PLANE; RECOMBINATION; LINES; MILKY; DUST
AB The Very Large Array was used to observe H I absorption against 20 compact and ultracompact H II (UC H II) regions, thereby resolving the kinematic distance ambiguity to these sources. Combining these results with other sources whose distances were resolved through H I absorption, the half-width at half-maximum of the distribution of source height above and below the Galactic plane is found to be 35 +/- 2 pc within the solar circle. The vertical height distribution is used to investigate the predictive accuracy of the Galactic latitude in resolving the kinematic distance ambiguity to UC H II regions without the need for H I observations. For a large difference between far and near kinematic distances, high accuracy can be achieved by choosing the kinematic distance closer to 1.84\b\(-1) kpc, where b is the Galactic latitude in degrees.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Fish, VL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 30
TC 95
Z9 96
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2003
VL 587
IS 2
BP 701
EP 713
DI 10.1086/368284
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 666CR
UT WOS:000182159400022
ER
PT J
AU Butt, YM
Maccarone, TJ
Prantzos, N
AF Butt, YM
Maccarone, TJ
Prantzos, N
TI Jet-induced nucleosynthesis in misaligned microquasars
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; ISM : jets and outflows; novae, cataclysmic
variables; nuclear reactions, nucleosynthesis, abundances; X-rays :
binaries
ID X-RAY BINARIES; BLACK-HOLE; RELATIVISTIC JETS; EMISSION-LINE;
NEUTRON-CAPTURE; LITHIUM; ANNIHILATION; SPECTRUM; SYSTEMS; NOVA
AB The jet axes and the orbital planes of microquasar systems are usually assumed to be approximately perpendicular, even though this is not currently an observational requirement. On the contrary, in one of the few systems where the relative orientations are well constrained, V4641 Sgr, the jet axis is known to lie not more than similar to36degrees from the binary plane. Such a jet, lying close to the binary plane, and traveling at a significant fraction of the speed of light, may periodically impact the secondary star, initiating nuclear reactions on its surface. The integrated yield of such nuclear reactions over the age of the binary system (less the radiative mass loss) will detectably alter the elemental abundances of the companion star. This scenario may explain the anomalously high Li enhancements (roughly similar to20-200 times the Sun's photospheric value) seen in the companions of some black hole/X-ray binary systems. (Such enhancements are puzzling, since Li nuclei are exceedingly fragile, being easily destroyed in the interiors of stars, and Li would be expected to be depleted rather than enhanced there.) Gamma-ray line signatures of the proposed process could include the 2.22 MeV neutron-capture line as well as the 0.478 MeV Li-7* deexcitation line, both of which may be discernible with the INTEGRAL satellite if produced in an optically thin region during a large outburst. For very energetic jets, a relatively narrow neutral pion gamma-decay signature at 67.5 MeV could also be measurable with the GLAST satellite. We argue that about 10%-20% of all microquasar systems ought to be sufficiently misaligned to be undergoing the proposed jet-secondary impacts.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Scuola Int Super Studi Avanzati, Trieste, Italy.
Inst Astrophys, F-75014 Paris, France.
RP Butt, YM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 44
TC 16
Z9 16
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 20
PY 2003
VL 587
IS 2
BP 748
EP 753
DI 10.1086/368301
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 666CR
UT WOS:000182159400025
ER
PT J
AU Friedrich, AM
Wernicke, BP
Niemi, NA
Bennett, RA
Davis, JL
AF Friedrich, AM
Wernicke, BP
Niemi, NA
Bennett, RA
Davis, JL
TI Comparison of geodetic and geologic data from the Wasatch region, Utah,
and implications for the spectral character of Earth deformation at
periods of 10 to 10 million years
SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH
LA English
DT Review
DE geodetic; geologic; fault slip rate; normal fault; timescale; earthquake
cycle
ID WESTERN UNITED-STATES; SAN-ANDREAS FAULT; SEISMIC-REFLECTION DATA;
GREAT-BASIN PROVINCE; RANGE PROVINCE; SLIP RATES; EXTENSIONAL TECTONICS;
STRAIN ACCUMULATION; GPS MEASUREMENTS; ROCKY-MOUNTAINS
AB [1] The Wasatch fault and adjacent fault zones provide an opportunity to compare present-day deformation rate estimates obtained from space geodesy with geologic displacement rates over at least four temporal windows, ranging from the last millennium up to 10 Myr. The three easternmost GPS sites of the Basin and Range Geodetic Network (BARGEN) at this latitude define a similar to130-km-wide region spanning three major normal faults extending east-west at a total rate of 2.7 +/- 0.4 mm/yr, with an average regional strain rate estimated to be 21 +/- 4 nstrain/yr, about twice the Basin and Range average. On the Wasatch fault, the vertical component of the geologic displacement rate is 1.7 +/- 0.5 mm/yr since 6 ka, < 0.6 mm/yr since 130 ka, and 0.5 - 0.7 mm/yr since 10 Ma. However, it appears likely that at the longest timescale, rates slowed over time, from 1.0 to 1.4 mm/yr between 10 and 6 Ma to 0.2 to 0.3 mm/yr since 6 Ma. The cumulative vertical displacement record across all three faults also shows time-variable strain release ranging from 2 to 4 mm/yr since 10 ka to < 1 mm/yr averaged over the past 130 kyr. Conventional earthquake recurrence models ("Reid-type'' behavior) would require an accordingly large variation in strain accumulation or loading rate on a 10-kyr timescale, for which there appears to be no obvious geophysical explanation. Alternatively, seismic strain release, given a wide range of plausible constitutive behaviors for frictional sliding, may be clustered on the 10-kyr timescale, resulting in the high Holocene rates, with comparatively low, uniform strain accumulation rates on the 100-kyr timescale ("Wallace-type'' behavior). The latter alternative, combined with observations at the million-year timescale and the likelihood of a significant contribution of postseismic transients, implies maxima of spectral amplitude in the velocity field at periods of similar to10 Myr ( variations in tectonic loading), similar to10 kyr ( clustered strain release), and of 100 years ( postseismic transients). If so, measurements of strain accumulation and strain release may be strongly timescale-dependent for any given fault system.
C1 CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA.
Harvard Univ, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Friedrich, AM (reprint author), Univ Potsdam, Inst Geosci, Karl Liebknechtstr 24,Haus 25, D-14476 Golm, Germany.
EM anke@alum.mit.edu; brian@gps.caltech.edu; niemi@crustal.ucsb.edu;
rbennett@cfa.harvard.edu; jdavis@cfa.harvard.edu
RI Niemi, Nathan/A-9996-2011; Friedrich, Anke/G-2921-2011; Davis,
James/D-8766-2013
OI Friedrich, Anke/0000-0002-6938-8563; Davis, James/0000-0003-3057-477X
NR 106
TC 127
Z9 128
U1 3
U2 29
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 2169-9313
EI 2169-9356
J9 J GEOPHYS RES-SOL EA
JI J. Geophys. Res.-Solid Earth
PD APR 15
PY 2003
VL 108
IS B4
AR 2199
DI 10.1029/2001JB000682
PG 23
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 673RW
UT WOS:000182594800001
ER
PT J
AU Schroll, S
AF Schroll, S
TI Transgressions: The offenses of art.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Libs, Washington, DC USA.
RP Schroll, S (reprint author), Smithsonian Inst Libs, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 15
PY 2003
VL 128
IS 7
BP 81
EP 81
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 672MA
UT WOS:000182523400034
ER
PT J
AU Flambaum, VV
Shuryak, EV
AF Flambaum, VV
Shuryak, EV
TI Dependence of hadronic properties on quark masses and constraints on
their cosmological variation
SO PHYSICAL REVIEW D
LA English
DT Article
ID FINE-STRUCTURE CONSTANT; QSO ABSORPTION-LINES; TIME-VARIATION
AB We follow our previous paper on the possible cosmological variation of the weak scale (quark masses) and the strong scale, inspired by data on the cosmological variation of the electromagnetic fine structure constant from distant quasar absorption spectra. In this work we identify the strange quark mass m(s) as the most important quantity, and the sigma meson mass as the ingredient of the nuclear forces most sensitive to it. As a result, we claim significantly stronger limits on the ratio of weak/strong scale (W=m(s)/Lambda(QCD)) variation following from our previous discussion on primordial big-bang nucleosynthesis (\deltaW/W\<0.006) and the Oklo natural nuclear reactor [\deltaW/W\<1.2x10(-10); there is also a nonzero solution deltaW/W=(-0.56+/-0.05)x10(-9)].
C1 Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
Harvard Smithsonian Ctr Astrophys, Inst Atom & Mol Theory, Cambridge, MA 02138 USA.
SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
RP Flambaum, VV (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia.
NR 20
TC 54
Z9 54
U1 0
U2 0
PU AMERICAN PHYSICAL SOC
PI COLLEGE PK
PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA
SN 0556-2821
J9 PHYS REV D
JI Phys. Rev. D
PD APR 15
PY 2003
VL 67
IS 8
AR 083507
DI 10.1103/PhysRevD.67.083507
PG 7
WC Astronomy & Astrophysics; Physics, Particles & Fields
SC Astronomy & Astrophysics; Physics
GA 675ZV
UT WOS:000182728200021
ER
PT J
AU Davis, JL
Bennett, RA
Wernicke, BP
AF Davis, JL
Bennett, RA
Wernicke, BP
TI Assessment of GPS velocity accuracy for the Basin and Range Geodetic
Network (BARGEN)
SO GEOPHYSICAL RESEARCH LETTERS
LA English
DT Article
ID STRAIN ACCUMULATION; YUCCA MOUNTAIN; DEFORMATION; NEVADA
AB [1] We assess the accuracy of horizontal velocity estimates from the Basin and Range Geodetic Network (BARGEN), a continuous GPS network that has been in operation since 1996. To make this quantitative assessment, we use a procedure that we term the "whole-error'' method. In this method, the measure of the velocity errors is the root-mean-square (RMS) residual velocity relative to a simple geophysical model. This method produces a conservative estimate of the uncertainties, since errors in the geophysical models also contribute to the RMS residual. Using estimates from two different BARGEN subnetworks, the Northern Basin and Range and the Yucca Mountain Cluster, we determine velocity uncertainties of 0.1-0.2 mm yr(-1). Since BARGEN covers a significant fraction of area of the proposed Plate Boundary Observatory component of EarthScope, our results indicate a good ability of this project to determine highly accurate long-term horizontal crustal velocities and deformation rates in this region.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 42, Cambridge, MA 02138 USA.
EM jdavis@cfa.harvard.edu; rbennett@cfa.harvard.edu; brian@gps.caltech.edu
RI Davis, James/D-8766-2013
OI Davis, James/0000-0003-3057-477X
NR 16
TC 26
Z9 27
U1 0
U2 1
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0094-8276
EI 1944-8007
J9 GEOPHYS RES LETT
JI Geophys. Res. Lett.
PD APR 11
PY 2003
VL 30
IS 7
AR 1411
DI 10.1029/2003GL016961
PG 4
WC Geosciences, Multidisciplinary
SC Geology
GA 669JP
UT WOS:000182348400008
ER
PT J
AU Lucas, SG
Holbrook, LT
Emry, RJ
AF Lucas, SG
Holbrook, LT
Emry, RJ
TI Isectolophus (Mammalia, Perissodactyla) from the Eocene of the Zaysan
Basin, Kazakstan and its biochronological significance
SO JOURNAL OF VERTEBRATE PALEONTOLOGY
LA English
DT Article
AB We describe a skull and fragments of lower jaws of a ceratomorph perissodactyl from the Arshantan (Eocene) strata of the Zaysan Basin, eastern Kazakstan, and refer these specimens to Isectolophus latidens (Osborn, Scott, and Speir, 1878). The material from the Zaysan Basin is indistinguishable from the holotypes of Isectolophus bogdulensis Reshetov from Mongolia and Homogalax reliquius Qi from China. These two species are junior subjective synonyms of L latidens. The presence of L latidens, known also from Bridgerian strata of North America, in Asian deposits of Arshantan age provides further support for a correlation between the Arshantan and the Bridgerian land-mammal "ages.".
C1 New Mexico Museum Nat Hist, Albuquerque, NM 87104 USA.
Rowan Univ, Dept Biol Sci, Glassboro, NJ 08028 USA.
Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA.
RP Lucas, SG (reprint author), New Mexico Museum Nat Hist, 1801 Mt Rd NW, Albuquerque, NM 87104 USA.
NR 26
TC 4
Z9 5
U1 2
U2 2
PU SOC VERTEBRATE PALEONTOLOGY
PI NORTHBROOK
PA 60 REVERE DR, STE 500, NORTHBROOK, IL 60062 USA
SN 0272-4634
J9 J VERTEBR PALEONTOL
JI J. Vertebr. Paleontol.
PD APR 11
PY 2003
VL 23
IS 1
BP 238
EP 243
DI 10.1671/0272-4634(2003)23[238:IMPFTE]2.0.CO;2
PG 6
WC Paleontology
SC Paleontology
GA 666MG
UT WOS:000182180600019
ER
PT J
AU Sanderson, AJR
Ponman, TJ
Finoguenov, A
Lloyd-Davies, EJ
Markevitch, M
AF Sanderson, AJR
Ponman, TJ
Finoguenov, A
Lloyd-Davies, EJ
Markevitch, M
TI The Birmingham-CfA cluster scaling project - I. Gas fraction and the
M-T-X relation
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE galaxies : clusters : general; galaxies : haloes; intergalactic medium;
X-rays : galaxies; X-rays : galaxies : clusters
ID MASS-TEMPERATURE RELATION; HYDRA-A CLUSTER; GALAXY CLUSTERS; ELLIPTIC
GALAXIES; RAY-CLUSTERS; INTRACLUSTER MEDIUM; HOT GAS; INTERGALACTIC
MEDIUM; COOLING FLOWS; DARK MATTER
AB We have assembled a large sample of virialized systems, comprising 66 galaxy clusters, groups and elliptical galaxies with high-quality X-ray data. To each system we have fitted analytical profiles describing the gas density and temperature variation with radius, corrected for the effects of central gas cooling. We present an analysis of the scaling properties of these systems and focus in this paper on the gas distribution and M-T-X relation. In addition to clusters and groups, our sample includes two early-type galaxies, carefully selected to avoid contamination from group or cluster X-ray emission. We compare the properties of these objects with those of more massive systems and find evidence for a systematic difference between galaxy-sized haloes and groups of a similar temperature.
We derive a mean logarithmic slope of the M-T-X relation within R-200 of 1.84 +/- 0.06, although there is some evidence of a gradual steepening in the M-T-X relation, with decreasing mass. We recover a similar slope using two additional methods of calculating the mean temperature. Repeating the analysis with the assumption of isothermality, we find the slope changes only slightly, to 1.89 +/- 0.04, but the normalization is increased by 30 per cent. Correspondingly, the mean gas fraction within R-200 changes from (0.13 +/- 0.01) h(70)(-3/2) to (0.11 +/- 0.01) h(70)(-3/2), for the isothermal case, with the smaller fractional change reflecting different behaviour between hot and cool systems. There is a strong correlation between the gas fraction within 0.3R(200) and temperature. This reflects the strong (5.8sigma) trend between the gas density slope parameter, beta, and temperature, which has been found in previous work.
These findings are interpreted as evidence for self-similarity breaking from galaxy feedback processes, active galactic nuclei heating or possibly gas cooling. We discuss the implications of our results in the context of a hierarchical structure formation scenario.
C1 Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
Max Planck Inst Extraterr Phys, D-85748 Garching, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA.
Univ Illinois, Dept Astron, Urbana, IL 61801 USA.
RP Sanderson, AJR (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.
NR 91
TC 156
Z9 157
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2003
VL 340
IS 3
BP 989
EP 1010
DI 10.1046/j.1365-8711.2003.06401.x
PG 22
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 664AN
UT WOS:000182039700033
ER
PT J
AU Handler, G
O'Donoghue, D
Muller, M
Solheim, JE
Gonzalez-Perez, JM
Johannessen, F
Paparo, M
Szeidl, B
Viraghalmy, G
Silvotti, R
Vauclair, G
Dolez, N
Pallier, E
Chevreton, M
Kurtz, DW
Bromage, GE
Cunha, MS
Ostensen, R
Fraga, L
Kanaan, A
Amorim, A
Giovannini, O
Kepler, SO
da Costa, AFM
Anderson, RF
Wood, MA
Silvestri, N
Klumpe, EW
Carlton, RF
Miller, RH
McFarland, JP
Grauer, AD
Kawaler, SD
Riddle, RL
Reed, MD
Nather, RE
Winget, DE
Hill, JA
Metcalfe, TS
Mukadam, AS
Kilic, M
Watson, TK
Kleinman, SJ
Nitta, A
Guzik, JA
Bradley, PA
Sekiguchi, K
Sullivan, DJ
Sullivan, T
Shobbrook, RR
Jiang, X
Birch, PV
Ashoka, BN
Seetha, S
Girish, V
Joshi, S
Dorokhova, TN
Dorokhov, NI
Akan, MC
Meistas, EG
Janulis, R
Kalytis, R
Alisauskas, D
Anguma, SK
Kalebwe, PC
Moskalik, P
Ogloza, W
Stachowski, G
Pajdosz, G
Zola, S
AF Handler, G
O'Donoghue, D
Muller, M
Solheim, JE
Gonzalez-Perez, JM
Johannessen, F
Paparo, M
Szeidl, B
Viraghalmy, G
Silvotti, R
Vauclair, G
Dolez, N
Pallier, E
Chevreton, M
Kurtz, DW
Bromage, GE
Cunha, MS
Ostensen, R
Fraga, L
Kanaan, A
Amorim, A
Giovannini, O
Kepler, SO
da Costa, AFM
Anderson, RF
Wood, MA
Silvestri, N
Klumpe, EW
Carlton, RF
Miller, RH
McFarland, JP
Grauer, AD
Kawaler, SD
Riddle, RL
Reed, MD
Nather, RE
Winget, DE
Hill, JA
Metcalfe, TS
Mukadam, AS
Kilic, M
Watson, TK
Kleinman, SJ
Nitta, A
Guzik, JA
Bradley, PA
Sekiguchi, K
Sullivan, DJ
Sullivan, T
Shobbrook, RR
Jiang, X
Birch, PV
Ashoka, BN
Seetha, S
Girish, V
Joshi, S
Dorokhova, TN
Dorokhov, NI
Akan, MC
Meistas, EG
Janulis, R
Kalytis, R
Alisauskas, D
Anguma, SK
Kalebwe, PC
Moskalik, P
Ogloza, W
Stachowski, G
Pajdosz, G
Zola, S
TI Amplitude and frequency variability of the pulsating DB white dwarf
stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth
Telescope
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE stars : individual : KUV 05134+2605; stars : individual : PG 1654+160;
stars : oscillations; stars : variables : other
ID XX-PYX; MODES; ASTEROSEISMOLOGY; DISCOVERY
AB We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time.
We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (approximate to40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree l = 1. If so, PG 1654+160 has a mass around 0.6 M..
The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data.
C1 S African Astron Observ, ZA-7935 Cape Town, South Africa.
Univ Cape Town, Dept Astron, ZA-7700 Rondebosch, South Africa.
Univ Tromso, Inst Matemat Realfag, N-9000 Tromso, Norway.
Konkoly Observ Budapest, H-1525 Budapest, Hungary.
Osserv Astron Capodimonte, I-80131 Naples, Italy.
Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France.
Observ Paris, LESIA, F-92195 Meudon, France.
Univ Cent Lancashire, Ctr Astrophys, Preston PR1 2HE, Lancs, England.
Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal.
Inst Super Maia, P-4470 Castelo Da Maia, Portugal.
Isaac Newton Grp Telescopes, Santa Cruz De La Palma 37800, Canary Isl, Spain.
Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil.
Univ Caixas do Sul, Dept Quim & Fis, BR-95001970 Caxias Do Sul, RS, Brazil.
Univ Fed Rio Grande do Sul, Inst Fis, BR-15051 Porto Alegre, RS, Brazil.
Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA.
Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA.
Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA.
Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA.
Univ Arkansas, Dept Phys & Astron, Little Rock, AR 72204 USA.
Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
SW Missouri State Univ, Dept Phys Astron & Mat Sci, Springfield, MO 65804 USA.
Univ Texas, Dept Astron, Austin, TX 78712 USA.
Univ Texas, McDonald Observ, Austin, TX 78712 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Southwestern Univ, Informat Technol Serv Dept, Georgetown, TX 78626 USA.
Apache Pt Observ, Sloan Digital Sky Survey, Sunspot, NM 88349 USA.
Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA.
Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand.
Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia.
Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China.
Chinese Acad Sci, Joint Inst Opt Astron, Beijing 100012, Peoples R China.
Perth Observ, Bickley, WA 6076, Australia.
Indian Space Res Org, Bangalore 560017, Karnataka, India.
Uttar Pradesh State Observ, Naini Tal 263129, India.
Odessa II Mechnikov State Univ, Astron Observ, UA-270014 Odessa, Ukraine.
Ege Univ, Fac Sci, Dept Astron & Space Sci, TR-35100 Izmir, Turkey.
Inst Theoret Phys & Astrophys, LT-2600 Vilnius, Lithuania.
Vilnius State Univ, Astron Observ, LT-2009 Vilnius, Lithuania.
Mbarara Univ Sci & Technol, Dept Phys, Mbarara, Uganda.
Univ Zambia, Dept Phys, Lusaka, Zambia.
Copernicus Astron Ctr, PL-00716 Warsaw, Poland.
Krakow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland.
Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland.
RP Univ Vienna, Inst Astron, Turkenschanzstr 17, A-1180 Vienna, Austria.
EM handler@astro.univie.ac.at
RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Fraga,
Luciano/K-9075-2013; de Amorim, Andre/H-5143-2016;
OI Metcalfe, Travis/0000-0003-4034-0416; Silvotti,
Roberto/0000-0002-1295-8174; Kepler, S. O. /0000-0002-7470-5703; Cunha,
Margarida/0000-0001-8237-7343; Stachowski, Greg/0000-0003-1560-1039;
Kawaler, Steven/0000-0002-6536-6367
NR 26
TC 9
Z9 9
U1 0
U2 5
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 11
PY 2003
VL 340
IS 3
BP 1031
EP 1038
DI 10.1046/j.1365-8711.2003.06373.x
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 664AN
UT WOS:000182039700036
ER
PT J
AU Colley, WN
Schild, RE
Abajas, C
Alcalde, D
Aslan, Z
Bikmaev, I
Chavushyan, V
Chinarro, L
Cournoyer, JP
Crowe, R
Dudinov, V
Evans, AKD
Jeon, YB
Goicoechea, LJ
Golbasi, O
Khamitov, I
Kjernsmo, K
Lee, HJ
Lee, J
Lee, KW
Lee, MG
Lopez-Cruz, O
Mediavilla, E
Moffat, AFJ
Mujica, R
Ullan, A
Munoz, J
Oscoz, A
Park, MG
Purves, N
Saanum, O
Sakhibullin, N
Serra-Ricart, M
Sinelnikov, I
Stabell, R
Stockton, A
Teuber, J
Thompson, R
Woo, HS
Zheleznyak, A
AF Colley, WN
Schild, RE
Abajas, C
Alcalde, D
Aslan, Z
Bikmaev, I
Chavushyan, V
Chinarro, L
Cournoyer, JP
Crowe, R
Dudinov, V
Evans, AKD
Jeon, YB
Goicoechea, LJ
Golbasi, O
Khamitov, I
Kjernsmo, K
Lee, HJ
Lee, J
Lee, KW
Lee, MG
Lopez-Cruz, O
Mediavilla, E
Moffat, AFJ
Mujica, R
Ullan, A
Munoz, J
Oscoz, A
Park, MG
Purves, N
Saanum, O
Sakhibullin, N
Serra-Ricart, M
Sinelnikov, I
Stabell, R
Stockton, A
Teuber, J
Thompson, R
Woo, HS
Zheleznyak, A
TI Around-the-clock observations of the Q0957+561A,B gravitationally lensed
quasar. II. Results for the second observing season
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE gravitational lensing; quasars : individual (Q0957+561A,B)
ID QSO 0957+561 A,B; TIME-DELAY; MICROLENSING VARIABILITY; LIGHT-CURVE;
PARAMETERS
AB We report on an observing campaign in 2001 March to monitor the brightness of the later arriving Q0957+ 561B image in order to compare with the previously published brightness observations of the (first-arriving) A image. The 12 participating observatories provided 3543 image frames, which we have analyzed for brightness fluctuations. From our classical methods for time-delay determination, we find a 417.09 +/- 0.07 day time delay, which should be free of effects due to incomplete sampling. During the campaign period, the quasar brightness was relatively constant and only small fluctuations were found; we compare the structure function for the new data with structure function estimates for the 1995-1996 epoch and show that the structure function during our observing interval is unusually depressed. We also examine the data for any evidence of correlated fluctuations at zero lag. We discuss the limits of our ability to measure the cosmological time delay if the quasar's emitting surface is time resolved, as seems likely.
C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Astrofis Canarias, E-38200 Tenerife, Canary Isl, Spain.
Akdeniz Univ, Dept Phys, TR-07058 Antalya, Turkey.
Tubitak Natl Observ, TR-07058 Antalya, Turkey.
Kazan VI Lenin State Univ, Kazan 420008, Russia.
Inst Nacl Astrofis Opt & Electr, Puebla 72840, Mexico.
Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada.
Observ Mont Megant, Montreal, PQ, Canada.
Univ Hawaii, Hilo, HI 96720 USA.
Kharkov Natl Univ, Astron Observ, UA-61022 Kharkov, Ukraine.
Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway.
Seoul Natl Univ, Astron Program, SEES, Seoul 151742, South Korea.
Univ Cantabria, Dept Fis Moderna, E-39005 Santander, Spain.
DACOM Corp, Internet Technol Div, Seoul 135610, South Korea.
UCL, London WC1E 6BT, England.
Univ Guanajuato, Dept Astron, Guanajuato 36000, Mexico.
Observ Carnegie Inst Washington, Washington, DC 20005 USA.
Kyungpook Natl Univ, Taegu 702701, South Korea.
Danish Lib Nat & Med Sci, DK-2200 Copenhagen, Denmark.
RP Colley, WN (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA.
NR 24
TC 22
Z9 22
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 APR 10
PY 2003
VL 587
IS 1
BP 71
EP 79
DI 10.1086/368076
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600006
ER
PT J
AU Winn, JN
Rusin, D
Kochanek, CS
AF Winn, JN
Rusin, D
Kochanek, CS
TI Investigation of the possible third image and mass models of the
gravitational lens PMN J1632-0033
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : nuclei; galaxies : structure; gravitational lensing
ID FREE-FREE ABSORPTION; DARK-MATTER HALOES; SCALING RELATIONS; GALAXY;
CONSTRAINTS; RESOLUTION; PARSEC; MG-1131+0456; PROFILES; CURVES
AB We present multifrequency VLBA(2) observations of PMN J1632-0033, one of the few gravitationally lensed quasars suspected of having a central "odd'' image. The central component has a different spectral index than the two bright quasar images. Therefore, either the central component is not a third image, and is instead the active nucleus of the lens galaxy, or else it is a third image whose spectrum is inverted by free-free absorption in the lens galaxy. In either case, we have more constraints on mass models than are usually available for a two-image lens, especially when combined with the observed orientations of the radio jets of the two bright quasars. If there is no third quasar image, the simplest permitted model is a singular isothermal sphere in an external shear field: beta = 2.05(-0.10)(+0.23) (2 sigma), where rho(r) proportional to r(-beta). If the central component is a third image, a hypothesis that can be tested with future high-frequency observations, then the density distribution is only slightly shallower than isothermal: beta = 1.91 +/- 0.02 (2 sigma). We also derive limits on the size of a constant-density core, and the break radius and exponent of an inner density cusp.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 57
TC 31
Z9 31
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 80
EP 89
DI 10.1086/368150
PN 1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600007
ER
PT J
AU Rusin, D
Kochanek, CS
Falco, EE
Keeton, CR
McLeod, BA
Impey, CD
Lehar, J
Munoz, JA
Peng, CY
Rix, HW
AF Rusin, D
Kochanek, CS
Falco, EE
Keeton, CR
McLeod, BA
Impey, CD
Lehar, J
Munoz, JA
Peng, CY
Rix, HW
TI The evolution of a mass-selected sample of early-type field galaxies
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE galaxies : elliptical and lenticular, cD; galaxies : evolution;
gravitational lensing
ID HUBBLE-SPACE-TELESCOPE; COLOR-MAGNITUDE RELATION; GRAVITATIONAL LENS
GALAXIES; DIGITAL SKY SURVEY; CLUSTER CL 1358+62; FUNDAMENTAL PLANE;
ELLIPTIC GALAXIES; LUMINOSITY FUNCTION; DISTANT CLUSTERS; DARK-MATTER
AB We investigate the evolution of mass-selected early-type field galaxies using a sample of 28 gravitational lenses spanning the redshift range 0 less than or similar to z less than or similar to 1. Based on the redshift-dependent intercept of the fundamental plane in the rest-frame B band, we measure an evolution rate of d log (M/L)(B)/dz = -0.56 +/- 0.04 (all errors are 1 sigma unless noted) if we directly compare to the local intercept measured from the Coma Cluster. Refitting the local intercept helps minimize potential systematic errors and yields an evolution rate of d log (M/L)(B)/dz = -0.54 +/- 0.09. An evolution analysis of properly corrected aperture mass-to-light ratios (defined by the lensed image separations) is closely related to the Faber-Jackson relation. In the rest-frame B band, we find an evolution rate of d log(M/L)(B)/dz = -0.41 +/- 0.21, a present-day characteristic magnitude of M*0 = -19.70 + 5 log h +/- 0.29 (assuming a characteristic velocity dispersion of sigma(DM*) = 225 km s(-1)), and a Faber-Jackson slope of gamma(FJ) = 3.29 +/- 0.58. The measured evolution rates favor old stellar populations ( mean formation redshift [z(f)] > 1.8 at 2 sigma confidence for a Salpeter initial mass function and a. at Omega(m) = 0.3 cosmology) among early-type field galaxies and argue against significant episodes of star formation at z < 1.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Smithsonian Inst, FL Whipple Observ, Amado, AZ 85645 USA.
Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
Inst Astrofis Canarias, E-38200 Tenerife, Spain.
Max Planck Inst Astron, D-69117 Heidelberg, Germany.
RP Rusin, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 110
TC 115
Z9 115
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 143
EP 159
DI 10.1086/346206
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600013
ER
PT J
AU Reid, MJ
Menten, KM
Genzel, R
Ott, T
Schodel, R
Eckart, A
AF Reid, MJ
Menten, KM
Genzel, R
Ott, T
Schodel, R
Eckart, A
TI The position of Sagittarius A*. II. Accurate positions and proper
motions of stellar SiO masers near the Galactic center
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE astrometry; Galaxy : center; masers; stars : AGB and post-AGB; stars :
variables : other
ID SUPERMASSIVE BLACK-HOLE; MILKY-WAY; GALAXY; SYSTEM; RADIO; STARS; VLT
AB In 1979, Menten and coworkers accurately determined the position of Sgr A* on an infrared image by aligning the infrared image with positions measured for SiO masers, associated with infrared-bright evolved stars, at radio wavelengths. We now report greatly improved radio positions and, for the first time, proper motions of many stellar SiO masers at the Galactic center. These positions and motions, coupled with better infrared imaging, allow a much improved location of Sgr A* on infrared images. With current data, infrared stars can be placed in a reference frame tied to Sgr A*, to an accuracy of approximate to10 mas in position and approximate to1 mas yr(-1) in motion. The position of Sgr A* is, within uncertainties, consistent with stellar accelerations and the measured orbital focus of the star S2. The star S2 was observed within 16 mas (approximate to130 AU in projection) of Sgr A* on 2002 May 2. Finally, we find that the central stellar cluster moves with Sgr A* to within approximate to70 km s(-1).
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
Max Planck Inst Extraterr Phys, D-85741 Garching, Germany.
Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Schoedel, Rainer/D-4751-2014
OI Schoedel, Rainer/0000-0001-5404-797X
NR 21
TC 52
Z9 52
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 208
EP 220
DI 10.1086/368074
PN 1
PG 13
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600017
ER
PT J
AU Li, D
Goldsmith, PF
Menten, K
AF Li, D
Goldsmith, PF
Menten, K
TI Massive quiescent cores in Orion. I. Temperature structure
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : clouds; ISM : individual (Orion); radio lines : ISM
ID GIANT MOLECULAR CLOUDS; STAR-FORMATION; DENSE CORES; INTERSTELLAR
AMMONIA; DARK CLOUDS; AMBIPOLAR DIFFUSION; CARBON-MONOXIDE; PROPER
MOTIONS; MULTITRANSITION; THERMOMETER
AB We have mapped four massive cores in Orion using the NH3 (J, K) = (1, 1) and (J, K) = (2, 2) inversion transitions as part of our effort to study the pre-protostellar phase of massive star formation. These cores were selected to be quiescent; i.e., they contain no apparent IR sources and are not associated with any molecular outflows. These cores are 1 order of magnitude more massive than dark cloud cores and have about twice the line width. This paper focuses on their temperature structure. We find a statistically significant correlation between the gas kinetic temperature and the gas column density. The general trend is for the gas to be colder where the column density is higher, which we interpret to mean that the interiors of these cores are colder than the regions surrounding them. This is in contrast with dark cloud cores, which exhibit relatively. at temperature profiles. The temperature gradient within the massive quiescent Orion cores is consistent with an external radiation source heating the dust and dust-gas collisions providing relatively close coupling between dust and gas temperatures. Thus, we suggest that the initial stage of massive pre-protostellar cloud cores is relatively quiescent condensations that are cooler than their surroundings.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
RP Li, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Goldsmith, Paul/H-3159-2016
NR 51
TC 34
Z9 35
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 262
EP 277
DI 10.1086/368078
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600022
ER
PT J
AU Ransom, RR
Bartel, N
Bietenholz, MF
Ratner, MI
Lebach, DE
Shapiro, II
Lestrade, JF
AF Ransom, RR
Bartel, N
Bietenholz, MF
Ratner, MI
Lebach, DE
Shapiro, II
Lestrade, JF
TI Very long baseline interferometry imaging of the RS Canum Venaticorum
binary star system HR 5110
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : close; radio continuum : stars; stars : activity; stars :
imaging; stars : individual (BH Canum Venaticorum); techniques :
interferometric
ID RADIO-EMISSION; MICROWAVE OBSERVATIONS; CLOSE BINARY; HR-5110; ALGOL;
POLARIZATION; ASTROMETRY; HR-1099; REGION; GHZ
AB We present VLBI images of the RS CVn binary star HR 5110 (= BH CVn; HD 118216), obtained from observations made at 8.4 GHz on 1994 May 29/30 in support of the NASA/Stanford Gravity Probe B project. Our images show an emission region with a core-halo morphology. The core was 0.39 +/- 0.09 mas (FWHM) in size, or 66% +/- 20% of the 0.6 +/- 0.1 mas diameter of the chromospherically active K subgiant star in the binary system. The halo was 1.95 +/- 0.22 mas (FWHM) in size, or 1.8 +/- 0.2 times the 1.1 +/- 0.1 mas separation of the centers of the K and F stars. (The uncertainties given for the diameter of the K star and its separation from the F star each reflect the level of agreement of the two most recent published determinations.) The core increased significantly in brightness over the course of the observations and seems to have been the site of. are activity that generated an increase in the total flux density of similar to200% in 12 hr. The fractional circular polarization simultaneously decreased from similar to10% to 2.5%.
C1 York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Observ Paris, Dept Millimetr Radio Astron, F-75014 Paris, France.
RP Ransom, RR (reprint author), York Univ, Dept Phys & Astron, 4700 Keele St, Toronto, ON M3J 1P3, Canada.
NR 28
TC 6
Z9 6
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 390
EP 397
DI 10.1086/368070
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600032
ER
PT J
AU Nisenson, P
van Ballegooijen, AA
de Wijn, AG
Sutterlin, P
AF Nisenson, P
van Ballegooijen, AA
de Wijn, AG
Sutterlin, P
TI Motions of isolated G-band bright points in the solar photosphere
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE Sun : atmospheric motions; Sun : faculae, plages; Sun : magnetic fields;
techniques : high angular resolution
ID MAGNETIC-FLUX TUBES; QUIET PHOTOSPHERE; FACULAR POINTS; NETWORK; SUN;
GRANULATION; RESOLUTION; FIELDS; SIMULATIONS; DYNAMICS
AB Magnetic elements on the quiet Sun are buffeted by convective flows that cause lateral motions on time-scales of minutes. The magnetic elements can be observed as bright points (BPs) in the G band at 4305 Angstrom. We present observations of BPs based on a long sequence of G-band images recorded with the Dutch Open Telescope and postprocessed using speckle-masking techniques. From these images we measured the proper motions of isolated BPs and derived the autocorrelation function of their velocity relative to the solar granulation pattern. The accuracy of BP position measurements is estimated to be less than 23 km on the Sun. The rms velocity of BPs (corrected for measurement errors) is about 0.89 km s(-1), and the correlation time of BP motions is about 60 s. This rms velocity is about 3 times the velocity measured using cork tracking, almost certainly due to the fact that isolated BPs move more rapidly than clusters of BPs. We also searched for evidence of vorticity in the motions of G-band BPs.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Sterrekundig Inst, NL-3508 TA Utrecht, Netherlands.
RP Nisenson, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 15, Cambridge, MA 02138 USA.
EM pnisenson@cfa.harvard.edu; vanballe@cfa.harvard.edu;
a.g.dewijn@astro.uu.nl; p.suetterlin@astro.uu.nl
OI van Ballegooijen, Adriaan/0000-0002-5622-3540
NR 36
TC 48
Z9 51
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP 458
EP 463
DI 10.1086/368067
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EA
UT WOS:000182105600039
ER
PT J
AU Metcalfe, TS
AF Metcalfe, TS
TI White dwarf asteroseismology and the C-12(alpha, gamma) O-16 rate
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE methods : numerical; nuclear reactions, nucleosynthesis, abundances
stars : individual (CBS 114, GD 358); stars : interiors; stars :
oscillations; white dwarfs
ID WHOLE EARTH TELESCOPE; GD-358; STARS; C-12(ALPHA,GAMMA)O-16
AB Due to a new global analysis method, it is now possible to measure the internal composition of pulsating white dwarf stars, even with relatively simple theoretical models. The precise internal mixture of carbon and oxygen is the largest single source of uncertainty in ages derived from white dwarf cosmochronometry, and it contains information about the rate of the astrophysically important, but experimentally uncertain, C-12(alpha, gamma)O-16 nuclear reaction. Recent determinations of the internal composition and structure of two helium-atmosphere variable (DBV) white dwarf stars, GD 358 and CBS 114, initially led to conflicting implied rates for the C-12(alpha, gamma)O-16 reaction. If both stars were formed through single-star evolution, then the initial analyses of their pulsation frequencies must have differed in some systematic way. I present improved fits to the two sets of pulsation data, resolving the tension between the initial results and leading to a value for the C-12(alpha, gamma)O-16 reaction rate that is consistent with recent laboratory measurements.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Metcalfe, TS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Metcalfe, Travis/A-9388-2008
OI Metcalfe, Travis/0000-0003-4034-0416
NR 19
TC 40
Z9 41
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP L43
EP L46
DI 10.1086/375044
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EB
UT WOS:000182105700011
ER
PT J
AU Risaliti, G
Elvis, M
Gilli, R
Salvati, M
AF Risaliti, G
Elvis, M
Gilli, R
Salvati, M
TI A Chandra minisurvey of X-ray-weak quasars
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : active; X-rays : diffuse background
ID BLACK-HOLES; PERFORMANCE; POPULATION; OBJECTS; SAMPLE; 2MASS
AB We present Chandra observations of 18 spectroscopically selected quasars, which are already known to be X-ray weak from previous ROSAT observations. All the sources but one are detected by Chandra, and spectral analysis suggests that most of them are intrinsically underluminous in the X-rays (by a factor from 3 to >100). These objects could represent a large population of quasars with a spectral energy distribution different from that of standard blue quasars. We discuss the possibility that a significant fraction of the obscured active galactic nuclei needed in synthesis models of the X-ray background could instead be optical, broad-line, X-ray-weak quasars.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
RP Risaliti, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM grisaliti@cfa.harvard.edu
RI Gilli, Roberto/P-1110-2015;
OI Gilli, Roberto/0000-0001-8121-6177; Risaliti, Guido/0000-0002-3556-977X
NR 24
TC 17
Z9 17
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 10
PY 2003
VL 587
IS 1
BP L9
EP L13
DI 10.1086/375048
PN 2
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665EB
UT WOS:000182105700003
ER
PT J
AU Hall, JPW
Callaghan, CJ
AF Hall, JPW
Callaghan, CJ
TI A revision of the new riodinid butterfly genus Pseudotinea (Lepidoptera
: Riodinidae)
SO JOURNAL OF NATURAL HISTORY
LA English
DT Article
DE biogeography; Calydna; conservation; morphology
AB A revision of the new South American riodinid genus Pseudotinea is presented that includes taxonomic and ecological notes, distributional data and illustrations of adults and genital structures for all species. The systematic position of Pseudotinea within the Riodinidae, its ecology and biogeography are discussed. Five species are recognized: volcanicus Callaghan and Salazar, hemis Schaus and caprina Hewitson are transferred from Calydna (comb. n.) and two new species, P. eiselei and P. gagarini, are described here. The genus is confined to the Andes and south-east Brazil where all species are very rare and many endangered.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA.
RP Hall, JPW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Entomol, Washington, DC 20560 USA.
EM jpwhall@hotmail.com
NR 48
TC 6
Z9 8
U1 0
U2 0
PU TAYLOR & FRANCIS LTD
PI ABINGDON
PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND
SN 0022-2933
J9 J NAT HIST
JI J. Nat. Hist.
PD APR 10
PY 2003
VL 37
IS 7
BP 821
EP 837
DI 10.1080/00222930110096771
PG 17
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 674WH
UT WOS:000182659800003
ER
PT J
AU Sioris, CE
Haley, CS
McLinden, CA
von Savigny, C
McDade, IC
McConnell, JC
Evans, WFJ
Lloyd, ND
Llewellyn, EJ
Chance, KV
Kurosu, TP
Murtagh, D
Frisk, U
Pfeilsticker, K
Bosch, H
Weidner, F
Strong, K
Stegman, J
Megie, G
AF Sioris, CE
Haley, CS
McLinden, CA
von Savigny, C
McDade, IC
McConnell, JC
Evans, WFJ
Lloyd, ND
Llewellyn, EJ
Chance, KV
Kurosu, TP
Murtagh, D
Frisk, U
Pfeilsticker, K
Bosch, H
Weidner, F
Strong, K
Stegman, J
Megie, G
TI Stratospheric profiles of nitrogen dioxide observed by Optical
Spectrograph and Infrared Imager System on the Odin satellite
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE optical; Sun-synchronous; polar-orbiting; Fraunhofer; Ring effect;
iterative onion peel
ID OZONE MONITORING EXPERIMENT; LIMB SCATTER MEASUREMENTS; ABSORPTION
SPECTROSCOPY; RADIATIVE-TRANSFER; MIDDLE ATMOSPHERE; O-3 PROFILES;
TRACE-GAS; MODEL; RETRIEVAL; MISSION
AB [1] Vertical profiles of nitrogen dioxide in the 19-40 km altitude range are successfully retrieved over the globe from Optical Spectrograph and Infrared Imager System (OSIRIS) limb scatter observations in late 2001 and early 2002. The inclusion of multiple scattering in the radiative transfer model used in the inversion algorithm allows for the retrieval of NO2 down to 19 km. The slant column densities, which represent the observations in the inversion, are obtained by fitting the fine structure in normalized radiance spectra over the 435-449 nm range, where NO2 electronic absorption is readily observable because of long light paths through stratospheric layers rich in this constituent. Details of the spectral fitting and inversion algorithm are discussed, including the discovery of a pseudo-absorber associated with pixelated detectors and a new method to verify altitude registration. Comparisons are made with spatially and temporally coincident profile measurements of this photochemically active trace gas. Better than 20% agreement is obtained with all correlative measurements over the common retrieval altitude range, confirming the validity of OSIRIS NO2 profiles. Systematic biases in the number densities are not observed at any altitude. A "snapshot'' meridional cross section between 40degreesN and 70degreesS is shown from observations during a fraction of an orbit.
C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA.
Univ Heidelberg, Inst Environm Phys, D-69120 Heidelberg, Germany.
Trent Univ, Dept Phys, Peterborough, ON K9J 7B8, Canada.
Swedish Space Corp, SE-17104 Solna, Sweden.
York Univ, Ctr Earth & Space Sci, Toronto, ON M3J 2R7, Canada.
Univ Saskatchewan, Dept Phys & Engn Phys, Saskatoon, SK S7N 5E2, Canada.
Environm Canada, Meteorol Serv Canada, Toronto, ON, Canada.
Univ Paris 06, IPSL, CNRS, Serv Aeron, F-75252 Paris 05, France.
Chalmers Univ, Dept Radio & Space Sci, SE-41296 Gothenburg, Sweden.
Stockholm Univ, Dept Meteorol, SE-10691 Stockholm, Sweden.
Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada.
Univ Bremen, Inst Environm Phys, D-28359 Bremen, Germany.
RP Sioris, CE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA.
EM csioris@cfa.harvard.edu; chris.mclinden@ec.gc.ca;
csavigny@iup.physik.uni-bremen.de; mcdade@yorku.ca;
jack@nimbus.yorku.ca; wevans@trentu.ca; llewellyn@skisas.usask.ca;
kchance@cfa.harvard.edu; tkurosu@cfa.harvard.edu; donal@rss.chalmers.se;
pf@iup.uni-heidelberg.de; strong@atmosp.physics.utoronto.ca;
jacek@misu.su.se
RI McLinden, Chris/A-7710-2010; The Odin satellite, aeronomy
mission/F-1671-2011; Strong, Kimberly/D-2563-2012; von Savigny,
Christian/B-3910-2014; Boesch, Hartmut/G-6021-2012; Murtagh,
Donal/F-8694-2011
OI McLinden, Chris/0000-0001-5054-1380; Murtagh, Donal/0000-0003-1539-3559
NR 52
TC 43
Z9 44
U1 1
U2 2
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 APR 9
PY 2003
VL 108
IS D7
AR 4215
DI 10.1029/2002JD002672
PG 19
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 669KB
UT WOS:000182349500002
ER
PT J
AU Puyravaud, JP
AF Puyravaud, JP
TI Standardizing the calculation of the annual rate of deforestation
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE annual rate of deforestation; compound interest law; exponential decay
model
ID WESTERN GHATS; CONSERVATION
AB Different authors utilize different formulae to calculate the annual rate of change of forest cover (or its opposite, the annual rate of deforestation) and use different terms to describe it. This generates confusion. I suggest that the annual rate of change of forest cover should be calculated as: r = (1/(t(2) - t(1))) x ln(A(2)/A(1)). This formula is derived from the Compound Interest Law. It is also derived from the mean annual rate of change and for this reason, is more intuitive than the formula used by FAO [q = ((A(2)/A(1))(1/(t2-t1))) - 1]. The rate r is always higher than q, but in most cases, the difference between the two quantities is lower than the sampling error. The rate r is significantly higher than q only when deforestation is extremely high. To ease comparisons between sites of annual rates of forest change, the forest area, time of measurements and formulae used should be clearly indicated. (C) 2002 Elsevier Science B.V All rights reserved.
C1 ECOS 50, Pondicherry 605001, India.
RP Puyravaud, JP (reprint author), Smithsonian Trop Res Inst, Box 2072, Balboa, Panama.
NR 14
TC 164
Z9 175
U1 4
U2 27
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD APR 7
PY 2003
VL 177
IS 1-3
BP 593
EP 596
AR PII S0378-1127(02)00335-3
DI 10.1016/S0378-1127(02)00335-3
PG 4
WC Forestry
SC Forestry
GA 664BL
UT WOS:000182041800044
ER
PT J
AU Schultz, TR
AF Schultz, TR
TI Pheidole in the New World - A dominant, hyperdiverse ant genus
SO SCIENCE
LA English
DT Book Review
C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20013 USA.
RP Schultz, TR (reprint author), Smithsonian Inst, Dept Systemat Biol, POB 37012,NHB,CE516,MRC 188, Washington, DC 20013 USA.
EM schultz@lab.si.edu
NR 1
TC 0
Z9 0
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 APR 4
PY 2003
VL 300
IS 5616
BP 57
EP 58
DI 10.1126/science.1084090
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 663CP
UT WOS:000181988900022
ER
PT J
AU Wilf, P
Cuneo, NR
Johnson, KR
Hicks, JF
Wing, SL
Obradovich, JD
AF Wilf, P
Cuneo, NR
Johnson, KR
Hicks, JF
Wing, SL
Obradovich, JD
TI High plant diversity in Eocene South America: Evidence from Patagonia
SO SCIENCE
LA English
DT Article
ID AMAZONIAN SPECIATION; CLIMATE-CHANGE; RAIN-FOREST; VEGETATION; HISTORY;
HYPOTHESIS; TAPHONOMY; EVOLUTION; TERTIARY; COLORADO
AB Tropical South America has the highest plant diversity of any region today, but this richness is usually characterized as a geologically recent development (Neogene or Pleistocene). From caldera-lake beds exposed at Laguna del Hunco in Patagonia, Argentina, paleolatitude similar to47degreesS, we report 102 leaf species. Radioisotopic and paleomagnetic analyses indicate that the. ora was deposited 52 million years ago, the time of the early Eocene climatic optimum, when tropical plant taxa and warm, equable climates reached middle latitudes of both hemispheres. Adjusted for sample size, observed richness exceeds that of any other Eocene leaf. ora, supporting an ancient history of high plant diversity in warm areas of South America.
C1 Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA.
Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA.
Museo Paleontol Egidio Feruglio, RA-9100 Trelew, Chubut, Argentina.
Denver Museum Nat & Sci, Dept Earth Sci, Denver, CO 80205 USA.
Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
US Geol Survey, Lakewood, CO 80225 USA.
RP Wilf, P (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA.
EM pwilf@geosc.psu.edu
OI Wing, Scott/0000-0002-2954-8905
NR 68
TC 148
Z9 157
U1 2
U2 16
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 APR 4
PY 2003
VL 300
IS 5616
BP 122
EP 125
DI 10.1126/science.1080475
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 663CP
UT WOS:000181988900046
PM 12677065
ER
PT J
AU Wood, JA
AF Wood, JA
TI Planetary science - Of asteroids and onions
SO NATURE
LA English
DT Editorial Material
ID PARENT BODIES
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Wood, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jwood@cfa.harvard.edu
NR 10
TC 8
Z9 8
U1 0
U2 3
PU NATURE PUBLISHING GROUP
PI LONDON
PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND
SN 0028-0836
J9 NATURE
JI Nature
PD APR 3
PY 2003
VL 422
IS 6931
BP 479
EP 481
DI 10.1038/422479a
PG 2
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 662TW
UT WOS:000181965400023
PM 12673234
ER
PT J
AU Muench, AA
Lada, EA
Lada, CJ
Elston, RJ
Alves, JF
Horrobin, M
Huard, TH
Levine, JL
Raines, SN
Roman-Zuniga, C
AF Muench, AA
Lada, EA
Lada, CJ
Elston, RJ
Alves, JF
Horrobin, M
Huard, TH
Levine, JL
Raines, SN
Roman-Zuniga, C
TI A study of the luminosity and mass functions of the young IC 348 cluster
using FLAMINGOS wide-field near-infrared images
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE infrared radiation; open clusters and associations : individual (IC
348); stars : formation; stars : luminosity function, mass function;
stars : low-mass, brown dwarfs
ID ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; T-TAURI STARS; BROWN DWARFS;
MOLECULAR CLOUD; EVOLUTIONARY MODELS; DUST EXTINCTION; IC-348;
ASSOCIATIONS; VARIABILITY
AB We present wide-field near-infrared (JHK) images of the young, tau = 2 Myr IC 348 cluster taken with FLAMINGOS. We use these new data to construct an infrared census of sources, which is sensitive enough to detect a 10 M-Jup brown dwarf seen through an extinction of A(V)similar to7. We examine the cluster's structure and relationship to the molecular cloud and to construct the cluster's K-band luminosity function. Using our model luminosity function algorithm, we derive the cluster's initial mass function ( IMF) throughout the stellar and substellar regimes and find that the IC 348 IMF is very similar to that found for the Trapezium cluster, with both cluster IMFs having a mode between 0.2-0.08 M-.. In particular, we find that, similar to our results for the Trapezium, brown dwarfs constitute only one in four of the sources in the IC 348 cluster. We show that a modest secondary peak forms in the substellar IC 348 K-band luminosity function (KLF), corresponding to the same mass range responsible for a similar KLF peak found in the Trapezium. We interpret this KLF peak as either evidence for a corresponding secondary IMF peak at the deuterium burning limit or as arising from a feature in the substellar mass-luminosity relation that is not predicted by current theoretical models. Finally, we find that IC 348 displays radial variations of its subsolar (0.5-0.08 M-.) IMF on a parsec scale. Whatever mechanism that is breaking the universality of the IMF on small spatial scales in IC 348 does not appear to be acting on the brown dwarf population, whose relative size does not vary with distance from the cluster center.
C1 Univ Florida, Dept Astron, Gainesville, FL 32611 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
European So Observ, D-8574 Garching, Germany.
RP Muench, AA (reprint author), CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA.
RI Roman-Zuniga, Carlos/F-6602-2016;
OI Roman-Zuniga, Carlos/0000-0001-8600-4798; Muench,
August/0000-0003-0666-6367; Alves, Joao/0000-0002-4355-0921
NR 59
TC 103
Z9 103
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2003
VL 125
IS 4
BP 2029
EP 2049
DI 10.1086/373925
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GK
UT WOS:000181713100027
ER
PT J
AU Walter, FM
Beck, TL
Morse, JA
Wolk, SJ
AF Walter, FM
Beck, TL
Morse, JA
Wolk, SJ
TI Deconstructing HD 28867
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE open clusters and associations : individual (Taurus-Auriga); stars :
individual (HD 28867)
ID X-RAY-EMISSION; T-TAURI STARS; LATE B-TYPE; OPEN CLUSTER; EINSTEIN
OBSERVATIONS; ORION NEBULA; ROSAT SURVEY; AURIGA; PLEIADES; CATALOG
AB The 3" pair of B9 stars HD 28867 is one of the brightest X-ray sources in the Taurus-Auriga star-forming region. In this multiwavelength study, we attempt to deduce the source of the X-ray emission. We show that the east component is the X-ray source. The east component has a near-IR excess and displays narrow absorption lines in the optical, both of which are consistent with a cool stellar companion. This companion is one of the brightest low-mass pre-main-sequence stars in Tau-Aur; at 2 mum, it and the B9 star are equally bright. We see evidence of radial velocity variability in the cool component of over 34 km s(-1). It is not visible in K-band speckle imaging, which constrains the companion to lie within 14 AU of the B star. We also report on a possible fourth member of the group, an M1 star 18" south of HD 28867.
C1 SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
Gemini Observ, Hilo, HI 96720 USA.
Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Walter, FM (reprint author), SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA.
EM fwalter@astro.sunysb.edu; tbeck@gemini.edu; morsey@casa.colorado.edu;
swolk@cfa.harvard.edu
OI Wolk, Scott/0000-0002-0826-9261
NR 53
TC 6
Z9 6
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD APR
PY 2003
VL 125
IS 4
BP 2123
EP 2133
DI 10.1086/368245
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GK
UT WOS:000181713100033
ER
PT J
AU Haas, M
Klaas, U
Muller, SAH
Bertoldi, F
Camenzind, M
Chini, R
Krause, O
Lemke, D
Meisenheimer, K
Richards, PJ
Wilkes, BJ
AF Haas, M
Klaas, U
Muller, SAH
Bertoldi, F
Camenzind, M
Chini, R
Krause, O
Lemke, D
Meisenheimer, K
Richards, PJ
Wilkes, BJ
TI The ISO view of Palomar-Green quasars
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies : fundamental parameters; galaxies : photometry; galaxies :
quasars : general; infrared : galaxies
ID ACTIVE GALACTIC NUCLEI; HYPERLUMINOUS INFRARED GALAXIES; CONTINUUM
ENERGY-DISTRIBUTIONS; HIGH-REDSHIFT QUASARS; RADIO-QUIET QUASARS;
OBSCURING DUST TORI; SKY SURVEY; EMISSION; ULTRAVIOLET; PHOTOMETRY
AB Mining the ISO data archive we provide the complete ISO view of PG quasars containing 64 infrared spectral energy distributions between 5 and 200 mum. About half of the sample was supplemented by MAMBO and SCUBA (sub-) millimetre data. Since the PG quasars were selected optically, the high infrared detection rate of more than 80% suggests that every quasar possesses luminous to hyperluminous dust emission with dust masses comparable to Seyferts and ultraluminous IR galaxies (ULIRGs). The gas-to-dust mass ratio (of those sources where CO measurements are available in the literature) is consistent with the galactic value providing further evidence for the thermal nature of the IR emission of radio quiet quasars. The SEDs represent templates of unprecedented detail and sensitivity. The power-law like near- to mid-IR SEDs (F-v proportional to v(alpha)) are smooth up to far-infrared wavelengths, favouring dust heating by the central AGN, and we conclude that, in particular for our hyperluminous quasars at z=1, starbursts play only a minor role for powering the dust emission, even in the FIR. The IR spectral slopes alpha(1-10) mum range from -0.9 to -2.2 with a mean of -1.3+/-0.3. They neither correlate with the optical spectral slope alpha(0.3-1) mum, nor with the IR luminosity, nor with the FIR/MIR luminosity ratio, nor with inclination-dependent extinction effects in the picture of a dusty torus. We suggest that the diversity of the SEDs reflects largely the evolution of the dust distribution, and we propose a classification of the SED shapes as well as an evolutionary scheme in which this variety can be understood. During the evolution the surrounding dust redistributes, settling more and more into a torus/disk like configuration, while the SEDs show an initial FIR bump, then an increasing MIR emission and a steeper near- to mid-infrared slope, both of which finally also decrease. Strikingly, based on the sensitive ISO data now we do not only see the coarse IR differences between ULIRGs and quasars, but also the details and a possible evolution of the dust distribution and emission even among the optically selected PG sample. Regarding cosmic evolution, our hyperluminous quasars in the "local" universe at z=1 do not show the hyperluminous (L(FIR)greater than or similar to10(13) L-circle dot) starburst activity inferred for z=4 quasars detected in several (sub-) millimetre surveys. In view of several caveats this difference should be established further, but it already suggests that in the early dense universe stronger merger events led to more powerful starbursts accompanying the quasar phenomenon, while at later cosmic epochs any coeval starbursts obviously do not reach that high power and are outshone by the AGN.
C1 Max Planck Inst Astron, D-69117 Heidelberg, Germany.
Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
Landessternwarte Heidelberg, D-69117 Heidelberg, Germany.
Rutherford Appleton Lab, CLRC, Didcot OX11 0QX, Oxon, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Haas, M (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
OI Wilkes, Belinda/0000-0003-1809-2364
NR 86
TC 144
Z9 144
U1 0
U2 4
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2003
VL 402
IS 1
BP 87
EP 111
DI 10.1051/0004-6361:20030110
PG 25
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 665NU
UT WOS:000182128200012
ER
PT J
AU Kepler, SO
Nather, RE
Winget, DE
Nitta, A
Kleinman, SJ
Metcalfe, T
Sekiguchi, K
Jiang, XJ
Sullivan, D
Sullivan, T
Janulis, R
Meistas, E
Kalytis, R
Krzesinski, J
Ogloza, W
Zola, S
O'Donoghue, D
Romero-Colmenero, E
Martinez, P
Dreizler, S
Deetjen, J
Nagel, T
Schuh, SL
Vauclair, G
Ning, FJ
Chevreton, M
Solheim, JE
Perez, JMG
Johannessen, F
Kanaan, A
Costa, JE
Costa, AFM
Wood, MA
Silvestri, N
Ahrens, TJ
Jones, AK
Collins, AE
Boyer, M
Shaw, JS
Mukadam, A
Klumpe, EW
Larrison, J
Kawaler, S
Riddle, R
Ulla, A
Bradley, P
AF Kepler, SO
Nather, RE
Winget, DE
Nitta, A
Kleinman, SJ
Metcalfe, T
Sekiguchi, K
Jiang, XJ
Sullivan, D
Sullivan, T
Janulis, R
Meistas, E
Kalytis, R
Krzesinski, J
Ogloza, W
Zola, S
O'Donoghue, D
Romero-Colmenero, E
Martinez, P
Dreizler, S
Deetjen, J
Nagel, T
Schuh, SL
Vauclair, G
Ning, FJ
Chevreton, M
Solheim, JE
Perez, JMG
Johannessen, F
Kanaan, A
Costa, JE
Costa, AFM
Wood, MA
Silvestri, N
Ahrens, TJ
Jones, AK
Collins, AE
Boyer, M
Shaw, JS
Mukadam, A
Klumpe, EW
Larrison, J
Kawaler, S
Riddle, R
Ulla, A
Bradley, P
TI The everchanging pulsating white dwarf GD358
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE stars : white dwarfs; stars : variables : general; stars : oscillations;
stars : individual : GD 358; stars : evolution
ID ZZ-CETI STARS; WHOLE EARTH TELESCOPE; GRAVITY MODES; TURBULENT
CONVECTION; GD-358; SPECTRA; PERIOD; G29-38; ASTEROSEISMOLOGY;
INSTABILITY
AB We report 323 hours of nearly uninterrupted time series photometric observations of the DBV star GD 358 acquired with the Whole Earth Telescope ( WET) during May 23rd to June 8th, 2000. We acquired more than 232 000 independent measurements. We also report on 48 hours of time-series photometric observations in Aug 1996. We detected the non-radial g-modes consistent with degree l = 1 and radial order 8 to 20 and their linear combinations up to 6th order. We also detect, for the first time, a high amplitude l = 2 mode, with a period of 796 s. In the 2000 WET data, the largest amplitude modes are similar to those detected with the WET observations of 1990 and 1994, but the highest combination order previously detected was 4th order. At one point during the 1996 observations, most of the pulsation energy was transferred into the radial order k = 8 mode, which displayed a sinusoidal pulse shape in spite of the large amplitude. The multiplet structure of the individual modes changes from year to year, and during the 2000 observations only the k = 9 mode displays clear normal triplet structure. Even though the pulsation amplitudes change on timescales of days and years, the eigenfrequencies remain essentially the same, showing the stellar structure is not changing on any dynamical timescale.
C1 UFRGS, Inst Fis, Porto Alegre, RS, Brazil.
Univ Texas, Dept Astron, Austin, TX 78712 USA.
Univ Texas, McDonald Observ, Austin, TX 78712 USA.
Apache Pt Observ, Sloan Digital Sky Survey, Sunspot, NM 88349 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Acad Sinica, Beijing Astron Observ, Beijing 100080, Peoples R China.
Victoria Univ Wellington, Wellington, New Zealand.
Inst Theoret Phys & Astron, LT-2600 Vilnius, Lithuania.
Cracow Pedag Univ, Mt Suhora Observ, PL-30084 Krakow, Poland.
Jagiellonian Univ, Krakow, Poland.
S African Astron Observ, ZA-7935 Cape Town, South Africa.
Univ Tubingen, D-72074 Tubingen, Germany.
Univ Toulouse 3, Observ Midi Pyrenees, CNRS, UMR5572, F-31400 Toulouse, France.
Observ Paris, DAEC, F-92195 Meudon, France.
Inst Fys, N-9037 Tromso, Norway.
Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil.
Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA.
Florida Inst Technol, SARA Observ, Melbourne, FL 32901 USA.
Univ Florida, Nucl Sci Ctr 202, Gainesville, FL 32611 USA.
NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA.
Univ Minnesota, Dept Phys & Astron, Minneapolis, MN 55455 USA.
Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
Middle Tennessee State Univ, Dept Phys & Astron, Murfreesboro, TN 37132 USA.
Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA.
Univ Vigo, Dept Fis Aplicada, Fac Ciencias, Vigo 36200, Pontevedra, Spain.
Los Alamos Natl Lab, Los Alamos, NM 87545 USA.
RP Kepler, SO (reprint author), UFRGS, Inst Fis, Porto Alegre, RS, Brazil.
EM kepler@if.ufrgs.br; travis@whitedwarf.org; kaz@subaru.naoj.org;
jiang@astro.as.utexas.edu; zola@ao.uj.edu.pl; chevreton@obspm.fr;
kanaan@fsc.ufsc.br; ulla@uvigo.es
RI Metcalfe, Travis/A-9388-2008; Kepler, S. O. /H-5901-2012; Ulla Miguel,
Ana Maria/M-2860-2014;
OI Metcalfe, Travis/0000-0003-4034-0416; Kepler, S. O.
/0000-0002-7470-5703; Kawaler, Steven/0000-0002-6536-6367
NR 45
TC 48
Z9 48
U1 0
U2 1
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2003
VL 401
IS 2
BP 639
EP 654
DI 10.1051/0004-6361:20030105
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658EN
UT WOS:000181708800026
ER
PT J
AU Risaliti, G
Woltjer, L
Salvati, M
AF Risaliti, G
Woltjer, L
Salvati, M
TI The nature of the absorbing torus in compact radio galaxies
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE galaxies : active; X-rays : galaxies
ID PARSEC-SCALE JETS; OBSCURING TORUS; SPECTRUM; OBSCURATION; ABSORPTION;
NUCLEUS; HYDRA; ASCA; GAS
AB We present BeppoSAX observations of the two radio galaxies PKS 1934-63 and S5 1946 + 708. Strong Iron Kalpha lines are detected in both objects indicating that the two sources are absorbed by column densities higher than 1024 cm(-2). Combining radio continuum, HI absorption and X-ray data we can constrain the physical state and the dimensions of the absorber. We find that the putative obscuring torus is molecular and located at a distance higher than 20 pc from the center in S5 1946 + 70. In PKS 1934-63 no radio nucleus has been observed. If this is due to free-free absorption a radius of only a few pc is inferred. Since the Kalpha lines have been detected only at 90% confidence, we also discuss the implications if they would be not as strong as found from our data. From our results it appears that the combination of hard X-ray data and spatially resolved HI absorption measurements provides a powerful diagnostic for conditions in the absorbing "torus".
C1 Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Observ Haute Provence, CNRS, F-04870 St Michel, France.
RP Risaliti, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy.
EM risaliti@arcetri.astro.it
OI Risaliti, Guido/0000-0002-3556-977X
NR 20
TC 7
Z9 7
U1 0
U2 0
PU EDP SCIENCES S A
PI LES ULIS CEDEX A
PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A,
FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD APR
PY 2003
VL 401
IS 3
BP 895
EP 901
DI 10.1051/0004-6361:20030124
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 662DA
UT WOS:000181929900009
ER
PT J
AU Wyithe, JSB
Loeb, A
AF Wyithe, JSB
Loeb, A
TI Reionization of hydrogen and helium by early stars and quasars
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmology : theory; early universe; intergalactic medium; stars :
formation
ID MICROWAVE BACKGROUND ANISOTROPIES; DIGITAL SKY SURVEY; INTERGALACTIC
MEDIUM; LUMINOSITY FUNCTION; IONIZING-RADIATION; GALAXY FORMATION; HE
2347-4342; UNIVERSE; Z-SIMILAR-TO-6; FRAGMENTATION
AB We compute the reionization histories of hydrogen and helium caused by the ionizing radiation fields produced by stars and quasars. For the quasars we use a model based on halo-merger rates that reproduces all known properties of the quasar luminosity function at high redshifts. The less constrained properties of the ionizing radiation produced by stars are modeled with two free parameters: ( i) a transition redshift, z(tran), above which the stellar population is dominated by massive, zero-metallicity stars and below which it is dominated by a Scalo mass function; and (ii) the product of the escape fraction of stellar ionizing photons from their host galaxies and the star formation efficiency, f(esc) f*. We constrain the allowed range of these free parameters at high redshifts on the basis of the lack of the H I Gunn-Peterson trough at z less than or similar to 6 and the upper limit on the total intergalactic optical depth for electron scattering, tau(es) < 0.18, from recent cosmic microwave background (CMB) experiments. We find that quasars ionize helium by a redshift z similar to 4, but cannot reionize hydrogen by themselves before z similar to 6. A major fraction of the allowed combinations of f(esc) f* and z(tran) leads to an early peak in the ionized fraction because of the presence of metal-free stars at high redshifts. This sometimes results in two reionization epochs, namely, an early H ii or He III overlap phase followed by recombination and a second overlap phase. Even if early overlap is not achieved, the peak in the visibility function for scattering of the CMB often coincides with the early ionization phase rather than with the actual reionization epoch. Consequently, tau(es) does not correspond directly to the reionization redshift. We generically find values of tau(es) greater than or similar to 7%, which should be detectable by the MAP satellite.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Adv Study, Princeton, NJ 08540 USA.
RP Wyithe, JSB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM swyithe@cfa.harvard.edu; loeb@sns.ias.edu
OI Wyithe, Stuart/0000-0001-7956-9758
NR 53
TC 182
Z9 183
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 693
EP 708
DI 10.1086/367721
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500001
ER
PT J
AU Kim, DW
Fabbiano, G
AF Kim, DW
Fabbiano, G
TI Chandra X-ray observations of NGC 1316 (Fornax A)
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : abundances; galaxies : individual (NGC 1316, NGC 1317)
galaxies : ISM; X-rays : galaxies
ID EARLY-TYPE GALAXIES; HUBBLE-SPACE-TELESCOPE; ROSAT PSPC OBSERVATIONS;
ELLIPTIC GALAXIES; MULTIPARAMETRIC ANALYSIS; EMISSION MECHANISMS;
INTERSTELLAR-MEDIUM; SPECTRAL PROPERTIES; METAL ABUNDANCES; EINSTEIN
SAMPLE
AB We report the results of the Chandra ACIS subarcsecond resolution X-ray observation of the archetypal merger radio galaxy NGC 1316 (Fornax A). We confirm the presence of. ne substructures in the hot interstellar medium (ISM). Some of these are likely to result from interaction with the radio jets, while others may be related to a complex intermingling of different phases of the ISM. We detect a low-luminosity X-ray active galactic nucleus (AGN) with L-X = 5 x 10(39) ergs s(-1) (in 0.3-8 keV) and a Gamma = 1.7 power-law energy spectrum. We also detect 81 point sources within the 25th magnitude isophotal ellipse of NGC 1316 (LX in the range of 2 x 10(37) to 2 x 10(39) ergs s(-1)), with hard (kT similar to 5 keV) X-ray spectra, typical of X-ray binaries, and a spatial radial distribution consistent with that of the optical (i.e., stellar) surface brightness. We derive the X-ray luminosity function (XLF) of these sources, correcting for the incompleteness at the faint end caused by the presence of the diffuse emission from the hot ISM in the central regions of NGC 1316 and by the widening of the Chandra point-spread functions at increasing distance from the aim point. With these corrections, the XLF is well reproduced by a single-unbroken-power law with a slope of -1.3 down to our threshold luminosity of similar to3 x 10(37) ergs s(-1). The hot ISM has temperatures in the 0.5-0.6 keV range, its surface brightness distribution is more centrally concentrated than that of the point sources, and its temperature appears to decrease at larger radii. These properties suggest that the ISM may be subject to partial winds. Taking into account the spectral complexity of the ISM, and the presence of unresolved low luminosity X-ray sources ( which can be inferred from the spectra), we constrain the metal abundance of the hot ISM to be Z = 0.25-1.3 Z. (90% confidence).
C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA.
RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA.
NR 87
TC 110
Z9 110
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 826
EP 849
DI 10.1086/367930
PN 1
PG 24
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500012
ER
PT J
AU Paolillo, M
Fabbiano, G
Peres, G
Kim, DW
AF Paolillo, M
Fabbiano, G
Peres, G
Kim, DW
TI ROSAT HRI investigation of the NGC 507 X-ray halo
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dark matter; galaxies : clusters : individual (Perseus-Pisces); galaxies
: halos; galaxies : jets; radio continuum : galaxies; X-rays :
individual (NGC 507)
ID EARLY-TYPE GALAXIES; LUMINOSITY RADIO GALAXIES; COUNTING DETECTOR
IMAGES; COOLING FLOW GALAXIES; ELLIPTIC GALAXIES; XMM-NEWTON;
INTRACLUSTER MEDIUM; WAVELET TRANSFORMS; PSPC OBSERVATIONS; VLA
OBSERVATIONS
AB We present an X-ray investigation of the elliptical galaxy NGC 507 in the Pisces cluster. We make use of archival ROSAT HRI and Chandra data, and of previously published PSPC data, to connect the large-scale structure of the halo to the core morphology. Our analysis, based on a bidimensional double beta model of the halo surface brightness, shows that the halo core (r < 2-3r(e)) and the external halo (r > 3r(e)) are characterized by different dynamical properties and suggests a different origin of the two components. The halo core has a complex morphology with a main X-ray emission peak, coincident with the center of the optical galaxy, and several secondary peaks. The spatial and spectral analysis of the central peak shows that this feature is produced by denser hot gas in the galaxy core. While both homogeneous and inhomogeneous cooling flow models predict a deposited mass exceeding the observed amount, our data support the scenario in which the gas is kinetically heated by stellar mass losses. Comparison with previously published studies suggests that the core of an X-ray extended galaxy is associated with the stellar distribution and has properties similar to the X-ray halos of compact galaxies. The secondary peaks are due instead to interactions between the radio-emitting plasma and the surrounding ISM, producing density fluctuations in the hot gas. We find that the energy input by the central radio source in the ISM is large enough to prevent gas cooling and may explain the failure of the cooling flow models. The total mass pro. le derived from the bidimensional model shows that a significant amount of dark matter is present at large radii. The dark halo extends on cluster scales and is likely associated with the whole cluster rather than with NGC 507. This structure is typical of many X-ray bright early-type galaxies and may explain the spatial and spectral differences with X-ray compact galaxies largely debated in the literature. The large-scale surface brightness distribution is irregular and more extended in the northeast direction. The displacement of the cluster halo from the optical galaxy and the filamentary structures observed in the halo core further suggest that the galaxy may be slowly moving within the group potential. Finally, we found that similar to20% of the sources detected by Kim & Fabbiano in the NGC 507 halo are due to point sources, while the nature of the remaining population is not clear. If associated with NGC 507, they could be either accreting binaries hosting a massive black hole or density clumps of the X-ray halo.
C1 Univ Palermo, Sez Astron, DSFA, I-90134 Palermo, Italy.
Osserv Astron Capodimonte, I-80131 Naples, Italy.
Harvard Smithsonian Ctr Astrophys, High Energy Div, Cambridge, MA 02138 USA.
RP Paolillo, M (reprint author), Univ Palermo, Sez Astron, DSFA, Piazza Parlamento 1, I-90134 Palermo, Italy.
EM paolillo@astropa.unipa.it; pepi@head-cfa.harvard.edu;
peres@astropa.unipa.it; kim@head-cfa.harvard.edu
RI Paolillo, Maurizio/J-1733-2012
OI Paolillo, Maurizio/0000-0003-4210-7693
NR 66
TC 19
Z9 19
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 850
EP 867
DI 10.1086/367718
PN 1
PG 18
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500013
ER
PT J
AU Eskridge, PB
Frogel, JA
Taylor, VA
Windhorst, RA
Odewahn, SC
Chiarenza, CATC
Conselice, CJ
de Grijs, R
Matthews, LD
O'Connell, RW
Gallagher, JS
AF Eskridge, PB
Frogel, JA
Taylor, VA
Windhorst, RA
Odewahn, SC
Chiarenza, CATC
Conselice, CJ
de Grijs, R
Matthews, LD
O'Connell, RW
Gallagher, JS
TI Ultraviolet-optical pixel maps of face-on spiral galaxies: Clues for
dynamics and star formation histories
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (NGC 6753, NGC 6782); galaxies : photometry;
galaxies : spiral; galaxies : structure; ultraviolet : galaxies
ID H-II REGIONS; SURFACE PHOTOMETRY; RINGED GALAXIES; DISK GALAXIES;
STELLAR; MORPHOLOGY; DECOMPOSITION; PROFILES; TELESCOPE; ABUNDANCE
AB Ultraviolet and optical images of the face-on spiral galaxies NGC 6753 and NGC 6782 reveal regions of strong ongoing star formation that are associated with structures traced by the old stellar populations. We use these images to construct NUV-(NUV-I(814)) pixel color-magnitude diagrams (pCMDs) that reveal plumes of pixels with strongly varying near-ultraviolet (NUV) surface brightness and nearly constant I(814) surface brightness. The plumes correspond to sharply bounded radial ranges, with (NUV- I(814)) at a given NUV surface brightness being bluer at larger radii. The plumes are parallel to both the reddening vector and simple model mixtures of young and old populations, thus neither reddening nor the fraction of the young population can produce the observed separation between the plumes. The images and radial surface brightness and color plots indicate that the separate plumes are caused by sharp declines in the surface densities of the old populations at radii corresponding to disk resonances. The maximum surface brightness of the NUV light remains essentially constant with radius, while the maximum I(814) surface brightness declines sharply with radius. A mid-ultraviolet (MUV) image of NGC 6782 shows emission from the nuclear ring. The distribution of points in an (MUV-NUV)-(NUV-I(814)) pixel color-color diagram is broadly consistent with the simple mixture model but shows a residual trend that the bluest pixels in (MUV-NUV) are the reddest pixels in (NUV-I(814)). This may be due to a combination of red continuum from late-type supergiants and [S III] emission lines associated with H II regions in active star-forming regions. We have shown that pixel mapping is a powerful tool for studying the distribution and strength of ongoing star formation in galaxies. Deep, multicolor imaging can extend this to studies of extinction and the ages and metallicities of composite stellar populations in nearby galaxies.
C1 Minnesota State Univ, Dept Phys & Astron, Trafton Sci Ctr N 141, Mankato, MN 56001 USA.
Ohio State Univ, Dept Astron, McPherson Lab, Columbus, OH 43210 USA.
NASA Headquarters, Washington, DC 20546 USA.
Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA.
CALTECH, Dept Astron, Pasadena, CA 91125 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA.
Univ Wisconsin, Dept Astron, Madison, WI 53706 USA.
RP Eskridge, PB (reprint author), Minnesota State Univ, Dept Phys & Astron, Trafton Sci Ctr N 141, Mankato, MN 56001 USA.
RI Conselice, Christopher/B-4348-2013;
OI Conselice, Christopher/0000-0003-1949-7638; de Grijs,
Richard/0000-0002-7203-5996
NR 45
TC 16
Z9 16
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 923
EP 938
DI 10.1086/367820
PN 1
PG 16
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500017
ER
PT J
AU Magnani, L
Chastain, RJ
Kim, CH
Hartmann, D
Truong, AT
Thaddeus, P
AF Magnani, L
Chastain, RJ
Kim, CH
Hartmann, D
Truong, AT
Thaddeus, P
TI CH, CO, and E(B-V) as molecular gas tracers in a translucent cloud
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : abundances; ISM : clouds; ISM : molecules; molecular processes
ID H-2 CONVERSION FACTOR; INTERSTELLAR-MEDIUM; H-I; INFRARED-EMISSION;
MILKY-WAY; DIFFUSE; GALAXY; CIRRUS; TURBULENCE; DENSITY
AB The effectiveness of three molecular hydrogen gas tracers-the CH(2)Pi(1/2), J = 1/2, F = 1-1 transition, the CO(1-0) transition, and the color excess, E(B-V)-is evaluated for the translucent molecular cloud MBM 16. The CH emission line and E(B-V) are well correlated with each other but not with the CO(1-0) emission line. It is likely that in translucent molecular clouds CO is not a linear tracer of the molecular hydrogen column density because, in these objects, the CO/H-2 ratio is undergoing rapid fluctuations as a function of the molecular hydrogen column density. For translucent and diffuse molecular clouds, and possibly for the translucent envelopes of giant molecular clouds, CH observations should be used to calibrate the CO to H-2 conversion factor.
C1 Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
Columbia Univ, New York, NY 10027 USA.
Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands.
Univ Calif Berkeley, Berkeley, CA 94720 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Magnani, L (reprint author), Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA.
NR 41
TC 18
Z9 18
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 1111
EP 1119
DI 10.1086/367883
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500026
ER
PT J
AU Osorio, M
D'Alessio, P
Muzerolle, J
Calvet, N
Hartmann, L
AF Osorio, M
D'Alessio, P
Muzerolle, J
Calvet, N
Hartmann, L
TI A comprehensive study of the L1551 IRS 5 binary system
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE binaries : general; circumstellar matter; stars : formation; stars :
individual (L1551 IRS 5); stars : pre-main-sequence
ID MILLIMETER-CONTINUUM OBSERVATIONS; AURIGA MOLECULAR CLOUD; YOUNG STELLAR
OBJECTS; T-TAURI STARS; ACCRETION DISKS; INFRARED OBSERVATIONS;
PROTOPLANETARY DISKS; CO; SPECTRUM; MODELS
AB We model the Class I source L1551 IRS 5, adopting a flattened infalling envelope surrounding a binary disk system and a circumbinary disk. With our composite model, we calculate self-consistently the spectral energy distribution of each component of the L1551 IRS 5 system, using additional constraints from recent observations by ISO, the water ice feature from observations with SpeX, the SCUBA extended spatial brightness distribution at submillimeter wavelengths, and the VLA spatial intensity distributions at 7 mm of the binary disks. We analyze the sensitivity of our results to the various parameters involved. Our results show that a flattened-envelope collapse model is required to explain simultaneously the large-scale fluxes and the water ice and silicate features. On the other hand, we find that the circumstellar disks are optically thick in the millimeter range and are inclined so that their outer parts hide the emission along the line of sight from their inner parts. We also find that these disks have lower mass accretion rates than the infall rate of the envelope.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
RP Osorio, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM mosorio@cfa.harvard.edu; p.dalessio@astrosmo.unam.mx;
jamesm@as.arizona.edu; ncalvet@cfa.harvard.edu; hartmann@cfa.harvard.edu
NR 62
TC 39
Z9 39
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 1148
EP 1161
DI 10.1086/367695
PN 1
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500030
ER
PT J
AU Long, KS
Reynolds, SP
Raymond, JC
Winkler, PF
Dyer, KK
Petre, R
AF Long, KS
Reynolds, SP
Raymond, JC
Winkler, PF
Dyer, KK
Petre, R
TI Chandra CCD imagery of the northeast and northwest limbs of SN 1006
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : individual (SN 1006); supernova remnants; X-rays : ISM
ID SUPERNOVA REMNANT SN-1006; ULTRAVIOLET-ABSORPTION-LINES; X-RAY-EMISSION;
NONLINEAR AMPLIFICATION; NONRADIATIVE SHOCKS; MAGNETIC-FIELD;
COSMIC-RAYS; HIGH-ENERGY; ACCELERATION; INSTABILITIES
AB We present deep images of the SN 1006 remnant (G327.6+14.6) with the ACIS instrument on the Chandra X-Ray Observatory. Two regions have been observed, the synchrotron-dominated northeast limb and the thermally dominated northwest limb, as well as a substantial portion of the interior of the remnant shell. The brightest features in the X-ray images correspond closely to radio features in the northeast and to Balmer-dominated. laments in the northwest. The spectra of the brighter. laments in the northeast are harder, with less prominent line emission than those in the northwest. In addition to highly elongated. laments, both images show enhanced clumps of emission well inside of the shock front that appear to be dominated by emission from oxygen. These probably arise from shock-heated ejecta, based on analysis of their X-ray spectra. We find no firm evidence for a halo of X-ray emission outside the shock to the northeast, as predicted by the Fermi shock-acceleration picture, in which relativistic electrons should be diffusing ahead of the shock. Our limits on upstream emission are less than 1.5% of the postshock levels in regions where the supernova remnant is brightest. This strongly suggests that the bright rims are flattened sheets nearly perpendicular to the plane of the sky and that the magnetic field strength jumps at the shock by a factor significantly larger than 4, as has been proposed if the shock puts significant energy into accelerating nonthermal ions. The spectra obtained of the northwest rim are all dominated by the helium-like ions of O, Ne, Mg, and Si expected from shocks with ionization (n(e)t) parameters of order 100 cm(-3) yr and electron temperatures of 0.5-1 keV, far lower than the postshock ion temperature implied by estimates of the shock speed obtained from the shape of the Halpha line.
C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA.
N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Long, KS (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA.
NR 39
TC 117
Z9 119
U1 0
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 1162
EP 1178
DI 10.1086/367832
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500031
ER
PT J
AU Akerlof, CW
Biller, S
Boyle, P
Buckley, J
Carter-Lewis, DA
Catanese, M
Cawley, MF
Connaughton, V
Fegan, DJ
Finley, J
Gaidos, J
Hillas, AM
Krennrich, F
Lamb, RC
Lessard, R
McEnery, J
Mohanty, G
Porter, NA
Quinn, J
Rodgers, A
Rose, HJ
Samuelson, F
Schubnell, MS
Sembroski, G
Srinivasan, R
Weekes, TC
Zweerink, J
AF Akerlof, CW
Biller, S
Boyle, P
Buckley, J
Carter-Lewis, DA
Catanese, M
Cawley, MF
Connaughton, V
Fegan, DJ
Finley, J
Gaidos, J
Hillas, AM
Krennrich, F
Lamb, RC
Lessard, R
McEnery, J
Mohanty, G
Porter, NA
Quinn, J
Rodgers, A
Rose, HJ
Samuelson, F
Schubnell, MS
Sembroski, G
Srinivasan, R
Weekes, TC
Zweerink, J
TI A search for correlations of TeV gamma rays with ultra-high-energy
cosmic rays
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE cosmic rays; galaxies : active; galaxies : individual (3C 147); gamma
rays : observations
ID BURSTS; SYSTEM; RADIATION; ASTRONOMY; PHOTONS; ARRAY
AB A search was conducted for TeV gamma-rays emitted from the direction of the ultra-high-energy cosmic ray detected by the Fly's Eye experiment with energy E similar to 3 x 10(20) eV. No enhancement was found at a level of 10(-10)gamma cm(-2) s(-1) for E > 350 GeV. A steady source of ultra-high-energy cosmic ray protons or photons would be expected to produce a gamma-ray flux above this level. An upper limit was also set for the flux of TeV gamma-rays from 3C 147, the most prominent active galactic nucleus in the error box.
C1 Univ Michigan, Dept Phys, Randall Lab 2477, Ann Arbor, MI 48109 USA.
Univ Oxford, Dept Phys, Oxford OX1 3RH, England.
Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA.
Univ Coll Dublin, Dept Phys, Dublin 4, Ireland.
Iowa State Univ Sci & Technol, Dept Phys & Astron, Ames, IA 50011 USA.
St Patricks Coll, Dept Expt Phys, Maynooth, Kildare, Ireland.
Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA.
RP Akerlof, CW (reprint author), Univ Michigan, Dept Phys, Randall Lab 2477, 500 E Univ Ave, Ann Arbor, MI 48109 USA.
EM tweekes@cfa.harvard.edu
RI McEnery, Julie/D-6612-2012
NR 34
TC 3
Z9 3
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 1232
EP 1237
DI 10.1086/367825
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500036
ER
PT J
AU Homan, J
Klein-Wolt, M
Rossi, S
Miller, JM
Wijnands, R
Belloni, T
van der Klis, M
Lewin, WHG
AF Homan, J
Klein-Wolt, M
Rossi, S
Miller, JM
Wijnands, R
Belloni, T
van der Klis, M
Lewin, WHG
TI High-frequency quasi-periodic oscillations in the black hole X-ray
transient XTE J1650-500
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; stars : individual (XTE J1650-500); stars :
oscillations; X-rays : binaries; X-rays : stars
ID MICROQUASAR GRO J1655-40; RXTE OBSERVATIONS; POWER SPECTRA; CANDIDATE;
BINARIES; GRS-1915+105; DISCOVERY; J1550-564; SPIN; PCA
AB We report the detection of high-frequency variability in the black hole X-ray transient XTE J1650-500. A quasi-periodic oscillation (QPO) was found at 250 Hz during a transition from the hard to the soft state. We also detected less coherent variability around 50 Hz that disappeared when the 250 Hz QPO showed up. There are indications that when the energy spectrum hardened the QPO frequency increased from similar to110 to similar to270 Hz, although the observed frequencies are also consistent with being 1 : 2 : 3 harmonics of each other. Interpreting the 250 Hz as the orbital frequency at the innermost stable orbit around a Schwarzschild black hole leads to a mass estimate of 8.2 M-circle dot. The spectral results by Miller et al., which suggest considerable black hole spin, would imply a higher mass.
C1 Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy.
Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
MIT, Ctr Space Res, Cambridge, MA 02139 USA.
MIT, Dept Phys, Cambridge, MA 02139 USA.
RP Homan, J (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy.
EM homan@merate.mi.astro.it; klein@astro.uva.nl; srossi@merate.mi.astro.it;
jmmiller@head-cfa.harvard.edu; radw@st-andrews.ac.uk;
belloni@merate.mi.astro.it; michiel@astro.uva.nl; lewin@space.mit.edu
NR 48
TC 55
Z9 57
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP 1262
EP 1267
DI 10.1086/367699
PN 1
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GP
UT WOS:000181713500040
ER
PT J
AU Rodriguez, LF
Porras, A
Claussen, MJ
Curiel, S
Wilner, DJ
Ho, PTP
AF Rodriguez, LF
Porras, A
Claussen, MJ
Curiel, S
Wilner, DJ
Ho, PTP
TI The binary jet in L1551 IRS 5
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : jets and outflows; stars : individual (L1551 IRS 5)
ID IRS 5; L1551; SPECTROSCOPY; COLLIMATION; SYSTEM; STARS; DISKS
AB We have used the Very Large Array with the Pie Town antenna of the Very Long Baseline Array to image for the first time L1551 IRS 5 at 3.5 cm with an angular resolution of similar to0."1. These observations clearly reveal the presence of a binary jet, with each component approximately centered on the 7 mm compact protoplanetary disks previously reported. As anticipated from results at various wavelengths, L1551 IRS 5 is a binary system where each star is surrounded by a disk and drives a collimated jet. The curved morphology of the northern jet, showing reflection symmetry, is suggestive of that expected for a source in a binary orbit. A region of radio emission located between the two jets could be a zone of shock interaction between the two outflows.
C1 Univ Nacl Autonoma Mexico, Inst Astron, Morelia 58190, Michoacan, Mexico.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Rodriguez, LF (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, Antigua Carretera Patzcuaro 8701, Morelia 58190, Michoacan, Mexico.
EM l.rodriguez@astrosmo.unam.mx; a.porras@astrosmo.unam.mx;
mclausse@nrao.edu; scuriel@astroscu.unam.mx; dwilner@cfa.harvard.edu;
pho@cfa.harvard.edu
NR 11
TC 35
Z9 35
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD APR 1
PY 2003
VL 586
IS 2
BP L137
EP L139
DI 10.1086/374882
PN 2
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658GQ
UT WOS:000181713600007
ER
PT J
AU Robbins, MB
Braun, MJ
Finch, DW
AF Robbins, MB
Braun, MJ
Finch, DW
TI Discovery of a population of the endangered Red Siskin (Carduelis
cucullata) in Guyana
SO AUK
LA English
DT Article
AB A heretofore unknown population of the endangered Red Siskin (Carduelis cucullata) was discovered in southwestern Guyana, similar to950 km from populations along the Venezuela coastal cordilleras. Most Venezuelan populations have been greatly reduced by the pet trade during the past 150 years, thus the newly discovered Guyana population represents an opportunity to insure the survival of this highly endangered species in the wild. Breeding of Guyanese siskins coincides with both breeding periods (May to early July and November-December) that have been documented in Venezuela. Breeding behavior, vocalizations, feeding habits, and immature plumages are described.
C1 Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA.
Natl Museum Nat Hist, Smithsonian Inst, Dept Systemat Biol, Suitland, MD 20746 USA.
Natl Museum Nat Hist, Smithsonian Inst, Lab Analyt Biol, Suitland, MD 20746 USA.
WINGS, Tucson, AZ 85712 USA.
RP Robbins, MB (reprint author), Univ Kansas, Museum Nat Hist, Div Birds, Lawrence, KS 66045 USA.
NR 11
TC 4
Z9 5
U1 0
U2 2
PU AMER ORNITHOLOGISTS UNION
PI LAWRENCE
PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA
SN 0004-8038
J9 AUK
JI AUK
PD APR
PY 2003
VL 120
IS 2
BP 291
EP 298
DI 10.1642/0004-8038(2003)120[0291:DOAPOT]2.0.CO;2
PG 8
WC Ornithology
SC Zoology
GA 695KG
UT WOS:000183829200004
ER
PT J
AU Vann, CD
Megonigal, JP
AF Vann, CD
Megonigal, JP
TI Elevated CO2 and water depth regulation of methane emissions: Comparison
of woody and non-woody wetland plant species
SO BIOGEOCHEMISTRY
LA English
DT Article
DE elevated CO2; global change; methane emissions; methane oxidation;
productivity; Taxodium distichum; wetlands
ID CARBON-DIOXIDE; CH4 EMISSIONS; BOREAL MIRE; SOIL; RHIZOSPHERE; RICE;
ROOT; OXIDATION; ENRICHMENT; ATMOSPHERE
AB Elevated CO2 has been shown to increase methane emissions in herbaceous wetlands, but it is not clear that this will occur in wetlands dominated by woody plants or in wetlands that are not inundated. We determined the effects of elevated CO2 and water table position on methane emission and oxidation rates from plant-soil microcosms planted with a woody tree, Taxodium distichum, or an emergent aquatic macrophyte, Orontium aquaticum. Experiments were conducted in replicate glasshouses (n = 2) at CO2 concentrations of either 350 or 700 ppmv. Plants were grown from seed and subjected to two water level depths, flooded (+5 cm above the soil surface) and non-flooded (-10 cm for T. distichum and -6 cm for O. aquaticum). Elevated CO2 increased whole-plant photosynthetic rates in both water table treatments. Methane emission rates increased by 62 to 69% in the T. distichum treatment and 27 to 29% in the O. aquaticum treatment. Whole-plant photosynthesis and biomass were strongly correlated with methane emissions (r(2) greater than or equal to 0.75, P less than or equal to 0.01). This relationship provides evidence of a tight coupling between plant and microbial activity and suggests that similar relationships from other wetland studies measured at ambient CO2 can be extrapolated into the future. In the O. aquaticum, non-flooded treatment, methanotrophy consumed 14 and 22% ( replicate glasshouses) of the methane produced in the ambient treatment compared to 29 and 36% in the elevated CO2 treatment. However, there was no significant methane oxidation detected in the flooded treatment. We concluded that woody and non-woody wetland ecosystems growing in a future CO2-enriched atmosphere will emit more methane regardless of water table position, but the degree of stimulation will be sensitive to changes in water table position, particularly in forested wetlands.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
George Mason Univ, Fairfax, VA 22030 USA.
RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
NR 45
TC 56
Z9 66
U1 3
U2 64
PU KLUWER ACADEMIC PUBL
PI DORDRECHT
PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS
SN 0168-2563
J9 BIOGEOCHEMISTRY
JI Biogeochemistry
PD APR-MAY
PY 2003
VL 63
IS 2
BP 117
EP 134
DI 10.1023/A:1023397032331
PG 18
WC Environmental Sciences; Geosciences, Multidisciplinary
SC Environmental Sciences & Ecology; Geology
GA 668MN
UT WOS:000182297900001
ER
PT J
AU Caldas, A
Robbins, RK
AF Caldas, A
Robbins, RK
TI Modified Pollard transects for assessing tropical butterfly abundance
and diversity
SO BIOLOGICAL CONSERVATION
LA English
DT Article
DE butterfly abundance; butterfly diversity; transects; Pollard; tropics
ID TEMPORAL DIMENSIONS; SPECIES-DIVERSITY; ASSEMBLAGES
AB This paper introduces and discusses the consistency and effectiveness of an inexpensive modification of Pollard transects for assessing the diversity and abundance of tropical butterfly communities in two national parks in Rio de Janeiro, Brazil. To measure butterfly abundance, students walked simultaneous timed transects at the interface of forest and cleared areas. They either counted the number of individuals observed or tabulated the number of specimens collected with nets. After a short training period, the number of butterflies observed or collected on simultaneous transects was statistically indistinguishable among student groups, and there was a significant positive correlation between observation counts and collected number of individuals. As a measure of species richness, the number of butterfly species sampled on each simultaneous transect was tabulated and did not differ statistically. To measure diversity, alpha of the logseries model was calculated for each collected sample, and statistical fit to a logseries model was determined. Although virtually all daily samples and the year's accumulated sample at one park fit the logseries model, about 35% of the daily samples and the entire year's sample did not fit at the other park. Despite these differences between the two parks, values for alpha from daily samples at both parks varied similarly (from 15 to 50 in almost all cases), and values from the entire year's samples were statistically indistinguishable. The repeatability of results among novices, such as students, suggests that timed transects have great promise for furthering our understanding of butterfly community demographics. Published by Elsevier Science Ltd.
C1 Smithsonian Inst, Natl Museum Nat Hist, Sect Entomol, Dept Systemat Biol, Washington, DC 20560 USA.
UERJ, Dept Biol Anim & Vegetal, BR-20550900 Rio De Janeiro, Brazil.
RP Caldas, A (reprint author), Univ Maryland, Dept Entomol, College Pk, MD 20742 USA.
NR 40
TC 30
Z9 38
U1 1
U2 15
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 0006-3207
J9 BIOL CONSERV
JI Biol. Conserv.
PD APR
PY 2003
VL 110
IS 2
BP 211
EP 219
AR PII S0006-3207(02)00190-8
DI 10.1016/S0006-3207(02)00190-8
PG 9
WC Biodiversity Conservation; Ecology; Environmental Sciences
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 642RR
UT WOS:000180818400005
ER
PT J
AU Harrison, RD
Hamid, AA
Kenta, T
Lafrankie, J
Lee, HS
Nagamasu, H
Nakashizuka, T
Palmiotto, P
AF Harrison, RD
Hamid, AA
Kenta, T
Lafrankie, J
Lee, HS
Nagamasu, H
Nakashizuka, T
Palmiotto, P
TI The diversity of hemi-epiphytic figs (Ficus; Moraceae) in a Bornean
lowland rain forest
SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE canopy; niche specialization; rare species; species diversity; strangler
fig; Urostigma
ID VENEZUELAN PALM SAVANNA; STRANGLER FIG; WATER RELATIONS; TREE; CANOPY;
GROWTH; ANTS; HEMIEPIPHYTES; ESTABLISHMENT; CONSEQUENCES
AB The diversity and niche specificity of hemi-epiphytic figs in a lowland dipterocarp forest in Sarawak were investigated in 1998. Twenty-seven fig species (264 individuals, c. 120 ha) colonized a diversity of host taxa (35 families), but densities were very low and only 1.77% of trees >30 cm d.b.h. were occupied. There were no significant associations with host taxa or host-bark roughness but among 11 common species (greater than or equal to9 individuals) the distributions of all other parameters (host-d.b.h., height and position of colonization, crown illumination, soil-texture and slope-angle) were significantly different, and we identified five fig guilds. The guilds corresponded to canopy strata, and appeared to reflect the establishment microsite requirements of different species. A fundamental trade-off within the hemiepiphytic habit was revealed: Species colonizing larger hosts were rarer, because of lower host densities and more specific microsite requirements, but had better light environments and attained a larger maximum size. The single strangler species appeared to escape many of these constraints, and an important source of mortality caused by host-toppling, indicating the advantages of this strategy. Thus, the hemi-epiphytic figs in this community have come to fill a remarkable diversity of niches, despite low levels of competition, through the exigencies of a complex environment. (C) 2003 The Linnean Society of London.
C1 Kyoto Univ, Ctr Ecol Res, Otsu, Shiga 5202113, Japan.
Forest Res Ctr, Forest Dept Sarawak, Kuching Sarawak 93762, Malaysia.
Nanyang Technol Univ, CTFS Asia Program, Singapore 1025, Singapore.
Kyoto Univ, Kyoto Univ Museum, Yoshida Honmachi, Sakyo 6068501, Japan.
Antioch New England Grad Sch, Dept Environm Studies, Keene, NH USA.
RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, APDO 2072, Balboa, Panama.
RI Kenta, Tanaka/B-2652-2014
NR 61
TC 20
Z9 21
U1 2
U2 12
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0024-4066
J9 BIOL J LINN SOC
JI Biol. J. Linnean Soc.
PD APR
PY 2003
VL 78
IS 4
BP 439
EP 455
DI 10.1046/j.0024-4066.2002.00205.x
PG 17
WC Evolutionary Biology
SC Evolutionary Biology
GA 672VW
UT WOS:000182544500002
ER
PT J
AU Collin, R
AF Collin, R
TI The utility of morphological characters in gastropod phylogenetics: an
example from the Calyptraeidae
SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY
LA English
DT Article
DE Calyptraea; Cheilea; Crepidula; Crucibulum; gastropod taxonomy
ID SEX-CHANGE; CREPIDULA-FORNICATA; LARVAL; GROWTH; PLANA; MESOGASTROPODA;
PROSOBRANCHIA; RAPANINAE; MOLLUSCA; PATTERNS
AB Organismal taxonomy is often based on a single or a small number of morphological characters. When they are morphologically simple or known to be plastic, we may not have great confidence in the taxonomic conclusions of analyses based on these characters. For example, calyptraeid gastropod shells are well known for their simplicity and plasticity, and appear to be subject to frequent evolutionary convergences, but are nevertheless the basis for calyptraeid taxonomy. In a case like this, knowing how the pattern of relationships inferred from morphological features used in traditional taxonomy compares to the patterns of relationships inferred from other morphological characters or DNA sequence data would be useful. In this paper, I examine the relative utility of traditional taxonomic characters (shell characters), anatomical characters and molecular characters for reconstructing the phylogeny of calyptraeid gastropods. The results of an ILD test and comparisons of the recovered tree topologies suggest that there is conflict between the DNA sequence data and the morphological data. Very few of the nodes recovered by the morphological data were recovered by any other dataset. Despite this conflict, the inclusion of morphological data increased the resolution and support of nodes in the topology recovered from a combined dataset. The RIs and CIs of the morphological data on the best estimate topology were not any worse than these indices for the other datasets. This analysis demonstrates that although analyses can be misled by these convergences if morphological characters are used alone, these characters contribute significantly to the combined dataset. (C) 2003 The Linnean Society of London.
C1 Univ Chicago, Comm Evolutionary Biol, Chicago, IL 60637 USA.
Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA.
Smithsonian Trop Res Inst, APO, AA 34002 USA.
RP Collin, R (reprint author), Univ Chicago, Comm Evolutionary Biol, Culver Hull,Rm 402,1025 E 57th St, Chicago, IL 60637 USA.
RI Collin, Rachel/G-2001-2010;
OI Collin, Rachel/0000-0001-5103-4460
NR 68
TC 26
Z9 30
U1 0
U2 5
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0024-4066
J9 BIOL J LINN SOC
JI Biol. J. Linnean Soc.
PD APR
PY 2003
VL 78
IS 4
BP 541
EP 593
DI 10.1046/j.0024-4066.2002.00166.x
PG 53
WC Evolutionary Biology
SC Evolutionary Biology
GA 672VW
UT WOS:000182544500010
ER
PT J
AU Breitburg, DL
Jordan, TE
Lipton, D
AF Breitburg, DL
Jordan, TE
Lipton, D
TI Preface-from ecology to economics: Tracing human influence in the
Patuxent River estuary and its watershed
SO ESTUARIES
LA English
DT Editorial Material
C1 Acad Nat Sci, Estuarine Res Ctr, St Leonard, MD 20678 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Univ Maryland, Dept Agr & Resource Econ, College Pk, MD 20742 USA.
RP Breitburg, DL (reprint author), Acad Nat Sci, Estuarine Res Ctr, 10545 Mackall Rd, St Leonard, MD 20678 USA.
NR 22
TC 1
Z9 2
U1 0
U2 3
PU ESTUARINE RES FEDERATION
PI LAWRENCE
PA PO BOX 368, LAWRENCE, KS 66044 USA
SN 0160-8347
J9 ESTUARIES
JI Estuaries
PD APR
PY 2003
VL 26
IS 2A
BP 167
EP 170
DI 10.1007/BF02695959
PG 4
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 699JE
UT WOS:000184052600001
ER
PT J
AU Jordan, TE
Weller, DE
Correll, DL
AF Jordan, TE
Weller, DE
Correll, DL
TI Sources of nutrient inputs to the Patuxent River estuary
SO ESTUARIES
LA English
DT Article
ID PARTIALLY STRATIFIED ESTUARY; ATLANTIC COASTAL-PLAIN; LONG-TERM TRENDS;
CHESAPEAKE BAY; LAND-USE; ATMOSPHERIC NITROGEN; AGRICULTURAL WATERSHEDS;
PARTICULATE MATTER; NITRATE-NITROGEN; AIR-TEMPERATURE
AB We quantified annual nutrient inputs to the Patuxent River estuary from point and nonpoint sources and from direct atmospheric deposition. We also compared nonpoint source (NPS) discharges from Piedmont and Coastal Plain regions and from agricultural and developed lands. Using continuous automated-sampling, we measured discharges of water, nitrogen, phosphorus, organic carbon (C), and suspended solids from a total of 23 watersheds selected to represent various proportions of developed land and cropland in the Patuxent River basin and the neighboring Rhode River basin. The sampling period spanned two years that differed in annual precipitation by a factor of 1.7. Water discharge from the watershed to the Patuxent River estuary was 3.4 times higher in the wet year than in the dry year. Annual water discharges from the study watersheds increased as the proportion of developed land increased. As the proportion of cropland increased, there were increases in the annual flow-weighted mean concentrations of nitrate (NO3-), total nitrogen (TN), dissolved silicate (Si), total phosphate (TPO43-), total organic phosphorus (TOP), total P (TP), and total suspended solids (TSS) in NPS discharges. The effect of cropland on the concentrations of NO3- and TN was stronger for Piedmont watersheds than for Coastal Plain watersheds. As the proportion of developed land increased, there were increases in annual mean concentrations of NO3-, total ammonium (TNH4+), total organic N (TON), TN, total organic C (TOC), TPO43-, TOP, TP, and TSS and decreases in concentrations of Si. Annual mean concentrations of TON, TOC, forms of P, and TSS were highest in the wet year. Annual mean concentrations of NO3-, TNH4+, TN, and Si did not differ significantly between years. We directly measured NPS discharges from about half of the Patuxent River basin and estimated discharges from the other half of the basin using statistical models that related annual water flow and material concentrations to land cover and physiographic province. We compared NPS discharges to public data on point source (PS) discharges. We estimated direct atmospheric deposition of forms of N, P, and organic C to the Patuxent River estuary based on analysis of bulk deposition near the Rhode River. During the wet year, most of the total terrestrial and atmospheric inputs of forms of N and P came from NPS discharges. During the dry year, 53% of the TNH4+ input was from atmospheric deposition and 58% of the NO3- input was from PS discharges; NPS and PS discharges were about equally important in the total inputs of TN and TPO43-. During the entire 2-yr period, the Coastal Plain portion of the Patuxent basin delivered about 80% of the NPS water discharges to the estuary and delivered similar proportions of the NPS TNH4+, TN, TOP, and TSS. The Coastal Plain delivered greater proportions of the NPS TON, TOC, Si, and TP (89%, 90%, 93%, and 95%, respecfively) than of water, and supplied nearly all of the NPS TPO43- (99%). The Piedmont delivered 33% of the NPS NO3- while delivering only 20% of the NPS water to the estuary. We used statistical models to infer the percentages of NPS discharges supplied by croplands, developed lands, and other lands.
Although cropland covers only 10% of the Patuxent River basin, it was the most important source of most materials in NPS discharge, supplying about 84% of the total NPS discharge of NO3-; about three quarters of the TPO43-, TOP, TP, and TSS; and about half of the TNH4+ and TN. Compared to developed land, cropland supplied a significantly higher percentage of the NPS discharges of NO3-, TN, TPO43-, TOP, TP, and TSS, despite the fact developed land covered 12% of the basin.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Jordan, TE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
OI Weller, Donald/0000-0002-7629-5437
NR 92
TC 55
Z9 59
U1 0
U2 8
PU ESTUARINE RES FEDERATION
PI LAWRENCE
PA PO BOX 368, LAWRENCE, KS 66044 USA
SN 0160-8347
J9 ESTUARIES
JI Estuaries
PD APR
PY 2003
VL 26
IS 2A
BP 226
EP 243
DI 10.1007/BF02695964
PG 18
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 699JE
UT WOS:000184052600006
ER
PT J
AU Weller, DE
Jordan, TE
Correll, DL
Liu, ZJ
AF Weller, DE
Jordan, TE
Correll, DL
Liu, ZJ
TI Effects of land-use change on nutrient discharges from the Patuxent
River watershed
SO ESTUARIES
LA English
DT Article
ID GULF-OF-MEXICO; CHESAPEAKE BAY; UNITED-STATES; NITROGEN FLUX; ESTUARY;
PHOSPHORUS; LANDSCAPE; PRECIPITATION; TRANSPORT; QUALITY
AB We developed an empirical model integrating nonpoint source (NPS) runoff, point sources (PS), and reservoir management to predict watershed discharges of water, sediment, organic carbon, silicate, nitrogen, and phosphorus to the Patuxent River in Maryland. We estimated NPS discharges with linear models fit to measurements of weekly flow and 10 material concentrations from 22 study watersheds. The independent variables were the proportions of cropland and developed land, physiographic province (Coastal Plain or Piedmont), and time (week). An but one of the NPS models explained between 62% and 83% of the variability among concentration or flow measurements. Geographic factors (land cover and physiographic province) accounted for the explained variability in largely dissolved material concentrations (nitrate [NO(3)], Silicate [Si], and total nitrogen [TN]), but the explained variability in flow and particulates (sediment and forms of phosphorus) was more strongly related to temporal variability or its interactions with land cover and province. Average concentrations of all materials increased with cropland proportion and also with developed land (except Si), but changes in cropland produced larger concentration shifts than equivalent changes in developed land proportion. Among land cover transitions, conversions between cropland and forest-grassland cause the greatest changes in material discharges, cropland and developed land conversions are intermediate, and developed land and forest-grassland conversions have the weakest effects. Changing land cover has stronger effects on NO(3) and TN in the Piedmont than in the Coastal Plain, but for all other materials, the effects of land-use change are greater in the Coastal Plain. We predicted the changes in nutrient load to the estuary under several alternate land cover configurations, including a state planning scenario that extrapolates current patterns of population growth and land development to the year 2020. In that scenario, declines in NPS discharges from reducing cropland are balanced by NPS discharge increases from developing an area almost six times larger than the lost cropland. When PS discharges are included, there are net increases in total water, total phosphorus, and TN discharges.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 20137 USA.
RP Weller, DE (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 20137 USA.
EM wellerd@si.edu
OI Weller, Donald/0000-0002-7629-5437
NR 76
TC 53
Z9 55
U1 1
U2 16
PU ESTUARINE RESEARCH FEDERATION
PI PORT REPUBLIC
PA 2018 DAFFODIL, PO BOX 510, PORT REPUBLIC, MD 20676 USA
SN 0160-8347
J9 ESTUARIES
JI Estuaries
PD APR
PY 2003
VL 26
IS 2A
BP 244
EP 266
DI 10.1007/BF02695965
PG 23
WC Environmental Sciences; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 699JE
UT WOS:000184052600007
ER
PT J
AU White, GG
Munroe, TA
Austin, HM
AF White, GG
Munroe, TA
Austin, HM
TI Reproductive seasonality, fecundity, and spawning frequency of tautog
(Tautoga onitis) in the lower Chesapeake Bay and coastal waters of
Virginia
SO FISHERY BULLETIN
LA English
DT Article
ID MIDDLE ATLANTIC BIGHT; ADULT TAUTOG; FISHES; PATTERNS; LABRIDAE; GROWTH;
AGE
AB The tautog, Thutoga onitis (Linnaeus), ranges from Nova Scotia to South Carolina and has become a popular target for recreational and commercial fisheries. Although tautog are a multiple spawning species, reproductive potential, measured as annual fecundity, has not been estimated previously with methods (batch fecundity, spawning frequency) necessary for a species with indeterminate annual fecundity. A total of 960 tautog were collected from the mouth of the Rappahannock River in the lower Chesapeake Bay to 45 kin offshore of Virginia's coastline to investigate tautog reproductive biology in the southern portion of the species range. Tautog did not exhibit a 1:1 sex ratio; 56% were females. Male tautog reached 50% maturity at 218 mm TL, females at 224 mm TL. Tautog spawned from 7 April 1995 to 15 June 1995, at locations from the York River to 45 kin offshore. Batch fecundity estimates ranged from 2800 to 181,200 eggs per spawning for female tautog age 3-9, total length 259516 mm. Mean batch fecundity +/-SEM for female tautog ages 4-6 was 54,243 2472 eggs and 106,256 3837 eggs for females ages 7-9. Spawning frequency was estimated at 1.2 days, resulting in 58 spawning days per female in 1995. Estimates of potential annual fecundity for tautog ages 3-9 ranged from 160,000 to 10,510,000 eggs.
C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, NOAA, Washington, DC 20013 USA.
RP White, GG (reprint author), Atlantic States Marine Fisheries Commiss, 1444 Eye St NW,6th Floor, Washington, DC 20005 USA.
NR 44
TC 12
Z9 12
U1 0
U2 1
PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE
PI SEATTLE
PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA
SN 0090-0656
J9 FISH B-NOAA
JI Fish. Bull.
PD APR
PY 2003
VL 101
IS 2
BP 424
EP 442
PG 19
WC Fisheries
SC Fisheries
GA 670CJ
UT WOS:000182389600019
ER
PT J
AU Rasse, DP
Li, JH
Drake, BG
AF Rasse, DP
Li, JH
Drake, BG
TI Carbon dioxide assimilation by a wetland sedge canopy exposed to ambient
and elevated CO2: measurements and model analysis
SO FUNCTIONAL ECOLOGY
LA English
DT Article
DE canopy structure; global change; leaf nitrogen; open-top chamber;
Scirpus
ID PLANT-COMMUNITIES; ATMOSPHERIC CO2; TEMPERATE FORESTS; ESTUARINE MARSH;
SCIRPUS-OLNEYI; GAS-EXCHANGE; PHOTOSYNTHESIS; GROWTH; NITROGEN; FLUXES
AB 1. The wetland sedge Scirpus olneyi Gray displays fast rates of CO2 assimilation and responds positively to increased atmospheric CO2 concentration. The present study was aimed at identifying the ecophysiological traits specific to S. olneyi that drive these CO2 -assimilation patterns under ambient and elevated CO2 conditions.
2. The net ecosystem exchange (NEE) of CO2 between S. olneyi communities and the atmosphere was measured in open-top chambers.
3. We developed a new mechanistic model for S. olneyi communities based on published ecophysiological data and additional measurements of photosynthetic parameters.
4. Our NEE measurements confirmed that S. olneyi communities have a high rate of summertime CO2 assimilation, with noontime peaks reaching 40 mumol CO2 m(-2) ground s(-1) on productive summer days, and that elevated CO2 increased S. olneyi CO2 assimilation by c . 35-40%.
5. Using S. olneyi -specific ecophysiological parameters, comparison with measured NEE showed that the model accurately simulated these high rates of CO2 uptake under ambient or elevated CO2 .
6. The model pointed to the Rubisco capacity of Scirpus leaves associated with their high total nitrogen content as the primary explanation for the high rates of CO2 assimilation, and indicated that the vertical-leaf canopy structure of S. olneyi had comparatively little influence on CO2 assimilation.
C1 Univ Liege, B-4000 Liege, Belgium.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Drake, BG (reprint author), Univ Liege, 17 Allee 6 Aout, B-4000 Liege, Belgium.
OI Daniel, Rasse/0000-0002-5977-3863
NR 36
TC 9
Z9 11
U1 2
U2 13
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0269-8463
J9 FUNCT ECOL
JI Funct. Ecol.
PD APR
PY 2003
VL 17
IS 2
BP 222
EP 230
DI 10.1046/j.1365-2435.2003.00730.x
PG 9
WC Ecology
SC Environmental Sciences & Ecology
GA 671GV
UT WOS:000182457700009
ER
PT J
AU MacLeod, KG
Fullagar, PD
Huber, BT
AF MacLeod, KG
Fullagar, PD
Huber, BT
TI Sr-87/Sr-86 test of the degree of impact-induced slope failure in the
Maastrichtian of the western North Atlantic
SO GEOLOGY
LA English
DT Article
DE Cretaceous-Tertiary boundary; strontium isotopes; slump; Maastrichtian;
Ocean Drilling Program
ID CRETACEOUS-TERTIARY BOUNDARY; STRONTIUM ISOTOPE STRATIGRAPHY;
EXTINCTION; MARGIN; EVOLUTION; RECORD
AB Analyses of Sr-87/Sr-86 in foraminifera and sedimentollogical observations suggest that the Chicxulub impact was not the trigger for slumps or a hiatus within the Maastrichtian section recovered at Ocean Drilling Program Sites 1049, 1050, and 1052 (subtropical western North Atlantic). The slumps and hiatus occur within a sequence dominated by pelagic chalk. The Sr-87/Sr-86 measurements show a general increase through the Maastrichtian at each site, but suggest chronostratigraphic gaps on the order of 10(6) yr across the slumps. Some of the slumps have burrowed upper surfaces and are composed of material that is older and coarser grained than the bounding chalks. Pelagic deposition punctuated by gravity flows easily explains the Maastrichtian record on Blake Nose, whereas an impact-based explanation for slumping is difficult to reconcile with sedimentological and geochemical observations.
C1 Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
Univ N Carolina, Dept Geol Sci, Chapel Hill, NC 27599 USA.
Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
RP MacLeod, KG (reprint author), Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA.
RI MacLeod, Kenneth/C-4042-2017
OI MacLeod, Kenneth/0000-0002-6016-0837
NR 29
TC 9
Z9 9
U1 0
U2 1
PU GEOLOGICAL SOC AMERICA, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD APR
PY 2003
VL 31
IS 4
BP 311
EP 314
DI 10.1130/0091-7613(2003)031<0311:SSTOTD>2.0.CO;2
PG 4
WC Geology
SC Geology
GA 662CN
UT WOS:000181928700006
ER
PT J
AU Stix, J
Kennedy, B
Hannington, M
Gibson, H
Fiske, R
Mueller, W
Franklin, J
AF Stix, J
Kennedy, B
Hannington, M
Gibson, H
Fiske, R
Mueller, W
Franklin, J
TI Caldera-forming processes and the origin of submarine volcanogenic
massive sulfide deposits
SO GEOLOGY
LA English
DT Article
DE calderas; volcanogenic massive sulfide deposits; fluids; subsidence
ID IZU-BONIN ARC; SEA-FLOOR; HYDROTHERMAL SYSTEM; YELLOWSTONE; SUBSIDENCE;
MOUNTAINS; COLLAPSE; MAGMA; LAKE
AB (C)ertain volcanogenic massive sulfide (VMS) ore deposits form in submarine calderas. This association is well known, but the link between caldera formation and the origins of the deposits remains poorly understood. Here we show that the size and location of a VMS deposit within a submarine caldera may be determined by how and when the caldera formed. These spatial-temporal conditions control development of the hydrothermal system associated with the VMS deposit. We propose that caldera opening along outward-dipping faults promotes magma degassing, seawater influx, and high-temperature leaching, resulting in a metal-rich hydrothermal fluid. These outward-dipping faults are considered to provide critical pathways for ore-forming fluids responsible for some caldera-hosted VMS deposits and may also be fundamentally important for the formation of many other caldera-hosted ore deposit types.
C1 McGill Univ, Dept Earth & Planetary Sci, Montreal, PQ H3A 2A7, Canada.
Geol Survey Canada, Ottawa, ON K1A 0E8, Canada.
Laurentian Univ, Dept Earth Sci, Mineral Explorat Res Ctr, Sudbury, ON P3E 2C6, Canada.
Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
Univ Quebec, Chicoutimi, PQ G7H 2B1, Canada.
RP Stix, J (reprint author), McGill Univ, Dept Earth & Planetary Sci, 3450 Univ St, Montreal, PQ H3A 2A7, Canada.
NR 36
TC 44
Z9 45
U1 1
U2 10
PU GEOLOGICAL SOC AMERICA, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD APR
PY 2003
VL 31
IS 4
BP 375
EP 378
DI 10.1130/0091-7613(2003)031<0375:CFPATO>2.0.CO;2
PG 4
WC Geology
SC Geology
GA 662CN
UT WOS:000181928700022
ER
PT J
AU James, HF
Ericson, PGP
Slikas, B
Lei, FM
Gill, FB
Olson, SL
AF James, HF
Ericson, PGP
Slikas, B
Lei, FM
Gill, FB
Olson, SL
TI Pseudopodoces humilis, a misclassified terrestrial tit (Paridae) of the
Tibetan Plateau: evolutionary consequences of shifting adaptive zones
SO IBIS
LA English
DT Article
ID DNA-DNA HYBRIDIZATION; MAJOR LINEAGES; SEQUENCE DATA; C-MYC; PHYLOGENY;
PARUS; GENE; TITMICE; CHICKADEES; PATTERNS
AB Pseudopodoces humilis (Hume's Ground-Jay) is a small passerine bird that inhabits the high rocky steppes of the Tibetan (Qinghai-Xizang) Plateau. Although it was long classified as a small species of ground jay (Podoces ), two previous anatomical studies cast doubt on its assignment to the Corvidae (crows and jays). We studied the evolutionary relationships of Pseudopodoces using three independent datasets drawn from comparative osteology, the nuclear c-myc gene, and the mitochondrial cytochrome b gene. All three datasets agree on the placement of Pseudopodoces in the family Paridae (tits and chickadees). The cytochrome b data further suggest that Pseudopodoces may be closest to the Great Tit Parus major species group. Pseudopodoces is the only species of parid whose distribution is limited to treeless terrain. Its evolutionary relationships were long obscured by adaptations to open habitat, including pale, cryptic plumage; a long, decurved bill for probing in crevices among rocks or in the ground; and long legs for terrestrial locomotion. Despite these accommodations to a novel adaptive zone, its evolutionary affinity with the Paridae is clearly expressed in comparative osteology and genetics, and is supported by its habit of nesting in cavities.
C1 Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
Swedish Museum Nat Hist, Dept Vertebrate Zool, SE-10405 Stockholm, Sweden.
Smithsonian Inst, Natl Zool Pk, Dept Res, Washington, DC 20008 USA.
Chinese Acad Sci, Inst Zool, Beijing 100080, Peoples R China.
Natl Audubon Soc, New York, NY 10003 USA.
RP James, HF (reprint author), Smithsonian Inst, Dept Systemat Biol, Natl Museum Nat Hist, Washington, DC 20560 USA.
RI Slikas, Beth/E-7275-2013
NR 51
TC 48
Z9 62
U1 3
U2 22
PU BRITISH ORNITHOLOGISTS UNION
PI TRING
PA C/O NATURAL HISTORY MUSEUM, SUB-DEPT ORNITHOLOGY, TRING HP23 6AP, HERTS,
ENGLAND
SN 0019-1019
J9 IBIS
JI Ibis
PD APR
PY 2003
VL 145
IS 2
BP 185
EP 202
DI 10.1046/j.1474-919X.2003.00170.x
PG 18
WC Ornithology
SC Zoology
GA 660JY
UT WOS:000181831100007
ER
PT J
AU Chave, J
Condit, R
Lao, S
Caspersen, JP
Foster, RB
Hubbell, SP
AF Chave, J
Condit, R
Lao, S
Caspersen, JP
Foster, RB
Hubbell, SP
TI Spatial and temporal variation of biomass in a tropical forest: results
from a large census plot in Panama
SO JOURNAL OF ECOLOGY
LA English
DT Article
DE above-ground biomass change; carbon cycle; dry living above-ground
biomass; tropical rain forest
ID NET PRIMARY PRODUCTION; BARRO-COLORADO ISLAND; RAIN-FOREST;
CARBON-DIOXIDE; NEOTROPICAL FOREST; ATMOSPHERIC CO2; LOWLAND FOREST;
AMAZON FOREST; TREE; GROWTH
AB 1 We estimated the dry, living, above-ground biomass (AGB) standing stock and its turnover in a 50-hectare forest plot located in moist tropical forest on Barro Colorado Island, Panama. The estimates were obtained using inventory data collected every 5 years from 1985 to 2000, including measurements of all trees greater than or equal to 1 cm diameter.
2 Four different allometric regressions relating trunk diameter and height with AGB were compared. Based on the most consistent method, we estimated that the Barro Colorado forest holds 281 +/- 20 Mg ha(-1) (1 Mg = 10(3) kg) of AGB, lianas included. A third of the AGB is stored in trees larger than 70 cm in diameter.
3 Stand-level AGB increment (growth plus recruitment) was highest in the period 1985-90 (7.05 +/- 0.32 Mg ha(-1) year(-1) , mean +/- 95% confidence limits based on samples of multiple hectares) and smallest in the period 1990-95 (5.25 +/- 0.26 Mg ha(-1) year(-1)), while AGB losses were similar during the three intervals (mean 5.43 +/- 0.72 Mg ha(-1) year(-1)). This resulted in significant differences in AGB change (defined as increment minus loss) among census intervals; including branchfalls, the AGB of Barro Colorado Island increased in 1985-90 (+0.82 +/- 0.84 Mg ha(-1) year(-1)), decreased in 1990-95 (-0.69 +/- 0.82 Mg ha(-1) year(-1)), and increased again in 1995-2000 (+0.45 +/- 0.70 Mg ha(-1) year(-1)). The 15-year average was +0.20 Mg ha(-1) year(-1), but with a confidence interval that spanned zero (-0.68 to 0.63 Mg ha(-1) year(-1)).
4 Branchfalls and partial breakage of stems had a significant influence on the AGB changes. They contributed an average of 0.46 Mg ha(-1) year(-1) to the AGB loss. About 5% of AGB increment was due to trees less than 10 cm in diameter.
5 To test whether the AGB of tropical forests is increasing due to climate change, we propose that in each forest type, at least 10 hectares of forest be inventoried, and that measurements of the small classes (< 10 cm diameter) as well as large size classes be included. Biomass loss due to crown damage should also be estimated.
C1 UPS, CNRS, Lab Evolut & Divers Biol, F-31062 Toulouse, France.
Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA.
Smithsonian Inst, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20560 USA.
Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada.
Field Museum Nat Hist, Dept Bot, Chicago, IL 60605 USA.
Univ Georgia, Dept Bot, Athens, GA 30602 USA.
RP Chave, J (reprint author), UPS, CNRS, Lab Evolut & Divers Biol, 118 Route Narbonne Batiment IVR3, F-31062 Toulouse, France.
NR 70
TC 187
Z9 219
U1 12
U2 65
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0022-0477
J9 J ECOL
JI J. Ecol.
PD APR
PY 2003
VL 91
IS 2
BP 240
EP 252
DI 10.1046/j.1365-2745.2003.00757.x
PG 13
WC Plant Sciences; Ecology
SC Plant Sciences; Environmental Sciences & Ecology
GA 662UT
UT WOS:000181967800007
ER
PT J
AU Leckie, RM
Huber, B
AF Leckie, RM
Huber, B
TI 2002 Joseph A. Cushman Award - Isabella Premoli Silva
SO JOURNAL OF FORAMINIFERAL RESEARCH
LA English
DT Biographical-Item
C1 Univ Massachusetts, Amherst, MA 01003 USA.
Smithsonian Inst, Washington, DC 20560 USA.
RP Leckie, RM (reprint author), Univ Massachusetts, Amherst, MA 01003 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU CUSHMAN FOUNDATION FORAMINIFERAL RES
PI CAMBRIDGE
PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST,
HARVARD UNIV, CAMBRIDGE, MA 02138 USA
SN 0096-1191
J9 J FORAMIN RES
JI J. Foraminifer. Res.
PD APR
PY 2003
VL 33
IS 2
BP 171
EP 172
DI 10.2113/0330171
PG 2
WC Paleontology
SC Paleontology
GA 694AR
UT WOS:000183751000006
ER
PT J
AU von Sternberg, R
Cumberlidge, N
AF von Sternberg, R
Cumberlidge, N
TI Autapomorphies of the endophragmal system in trichodactylid freshwater
crabs (Crustacea : Decapoda : Eubrachyura)
SO JOURNAL OF MORPHOLOGY
LA English
DT Article
DE freshwater crabs; Trichodactylidae; Eubrachyura; endophragmal system;
sella turcica; interosternites; junction plate
ID BRACHYURA
AB An examination of the thoracic endophragmal system in trichodactylid freshwater crabs revealed several derived features that appear restricted to this family. Trichodactylids have a highly reduced sella turcica with a rim-like overall configuration; as a consequence of sella turcica reduction the median septum is dorsoventrally diminished and exposed along its length. In addition, interosternite 7/8 is medially erased with the remnants restricted to the lateral regions of the sternum. The configurations of the sella turcica and interosternite 7/8 in trichodactylids underscore the monophyly of this family. The Dilocarcininae is characterized by having interosternites 5/6 through 7/8 restricted to the lateral sectors of the sternum, the lateral remnants of interosternite 4/5 forming prominent, rib-like ridges oriented diagonally to the longitudinal axis of the crab, and the median septum forming with interosternite 4/5 a Y-shaped pattern. These autapomorphies of the endophragmal system separate the trichodactylids from all other eubrachyurans and emphasize the morphological distinctness of the group. A description of the trichodactylid endophragmal junction plate is also provided. (C) 2003 Wiley-Liss, Inc.
C1 Smithsonian Inst, Dept Syst Biol, NHB 163, Washington, DC 20013 USA.
No Michigan Univ, Dept Biol, Marquette, MI 49855 USA.
RP von Sternberg, R (reprint author), NIH, NLM, Natl Ctr Biotechnol Informat, GenBank, Bethesda, MD 20894 USA.
EM Sternber@ncbi.nlm.nih.gov; Sternberg.Richard@nmnh.si.edu
NR 29
TC 6
Z9 7
U1 0
U2 0
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0362-2525
EI 1097-4687
J9 J MORPHOL
JI J. Morphol.
PD APR
PY 2003
VL 256
IS 1
BP 23
EP 28
DI 10.1002/jmor.10072
PG 6
WC Anatomy & Morphology
SC Anatomy & Morphology
GA 655NU
UT WOS:000181559600003
PM 12616572
ER
PT J
AU Faust, MA
AF Faust, MA
TI Protoperidinium belizeanum sp nov (Dinophyceae) from Manatee Cay,
Belize, Central America
SO JOURNAL OF PHYCOLOGY
LA English
DT Article
DE biodiversity; dinoflagellates; distribution; Dinophyceae; ecology; coral
reef-mangrove pond; morphology; Protoperidinium belizeanum sp nov.;
scanning electron microscopy; taxonomy
AB A new marine heterotrophic dinoflagellate species, Protoperidinium belizeanum sp. nov., from a coral reef-mangrove pond was identified from scanning electron micrographs. Recognition of this new species was based on unique features of the thecal morphology, which included cell size and shape, presence of short and wide postcingular plates, sulcal architecture, antapical spines, and intricate thecal plate patterns of ridged hexagonal depressions. The thecal plate formula is as follows: Po, X, 4', 3a, 7', 4C (3+t), 6S, 5''', 2''''. Species association of P. belizeanum sp. nov. within the genus Protoperidinium , its habitat, and associated dinoflagellates species are discussed.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Bot, Suitland, MD 20746 USA.
RP Faust, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol Bot, 4210 Silver Hill Rd, Suitland, MD 20746 USA.
NR 32
TC 0
Z9 0
U1 0
U2 2
PU BLACKWELL PUBLISHING INC
PI MALDEN
PA 350 MAIN ST, MALDEN, MA 02148 USA
SN 0022-3646
J9 J PHYCOL
JI J. Phycol.
PD APR
PY 2003
VL 39
IS 2
BP 390
EP 394
PG 5
WC Plant Sciences; Marine & Freshwater Biology
SC Plant Sciences; Marine & Freshwater Biology
GA 660YB
UT WOS:000181861800016
ER
PT J
AU Arneson, L
Wcislo, WT
AF Arneson, L
Wcislo, WT
TI Dominant-subordinate relationships in a facultatively social, nocturnal
bee, Megalopta genalis (Hymenoptera : Halictidae)
SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Halictidae; bees; dominance; agonism social behavior
ID LASIOGLOSSUM-ZEPHYRUM; SOLITARY; EXPERIENCE; CONFLICT; COLONIES;
FAMILIARITY; ENCOUNTERS; HIERARCHY; BEHAVIOR; SIZE
AB The potential for the formation of social relationships was explored for the facultatively social halictine bee, Megalopta genalis, using experimental circular arenas, Observing pairs of females from different nests, we examined the initiation of agonistic behavior, and the expression and relative frequency of dominance behavior in terms of phenotypic differences betA been interacting bees. Within pairs, older females with relatively larger ovaries tended to be dominant over younger females with smaller ovaries, and females with fewer nest-mates tended to initiate agonistic interactions. Bees also modified their behavior over a 24-hour time frame and were more pacific when paired with the same bee in repeated trials. Our observations suggest that these predominantly solitary bees have the capabilities to express cooperative and social dominance behavior typical of the halictines A with obligate social behavior.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
RP Wcislo, WT (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
NR 52
TC 29
Z9 29
U1 1
U2 4
PU KANSAS ENTOMOLOGICAL SOC
PI LAWRENCE
PA PO BOX 368, LAWRENCE, KS 66044 USA
SN 0022-8567
J9 J KANSAS ENTOMOL SOC
JI J. Kans. Entomol. Soc.
PD APR
PY 2003
VL 76
IS 2
BP 183
EP 193
PG 11
WC Entomology
SC Entomology
GA 664XR
UT WOS:000182090400013
ER
PT J
AU Norden, BB
Krombein, KV
Deyrup, MA
Edirisinghe, JP
AF Norden, BB
Krombein, KV
Deyrup, MA
Edirisinghe, JP
TI Biology and behavior of a seasonally aquatic bee, Perdita (Alloperdita)
floridensis Timberlake (Hymenoptera : Andrenidae : Panurginae)
SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Andrenidae; bees; Florida; Ilex; Perdita; submerged nests
ID NESTING BIOLOGY
AB The small panurgine bee. Perdita Timberlake, nests in sand during mid-April to mid-May in south-central Florida. This species is solitary. but often nests gregariously in dense aggregations. It is univoltine, with some larvae delaying emergence by a year, and is oligolectic, primarily foraging on gallberry. Ilex glabra (L) Gray. Details of nest construction, foraging, pollen transport and provisions, activity periods. and male behaviors are described. Mating is presumed to occur within nests and was never observed on host plants. Bees over-wintered as post-defecated larvae (prepupae) in a semi-diapause. The biology and behaviors associated with a prolonged period ffi e to six months) underwater for some prepupae are detailed. and the possible oxygenating role of algae in their survival is discussed. Predators and parasites associated with P. floridensis include: the cleptoparasitic bee, Sphecodes brachycephalus Mitchell; two multillids, Pseudomethoca torrida Krombein and Dasymutilla archboldi Schmidt and Mickek an undetermined species of mite: the asilid fly. Mallophorina clausicella (Macquart) and the harvester ant, Pogonomyrmex badius (Latreille). In addition. an undetermined nematode species, and mosquitofish, Gambusia holbrooki Girard A ere associated with P. floridensis nest sites.
C1 Smithsonian Inst, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA.
Univ Peradeniya, Dept Zool, Peradeniya, Sri Lanka.
RP Norden, BB (reprint author), Smithsonian Inst, Entomol Sect, Dept Systemat Biol, Washington, DC 20560 USA.
NR 24
TC 7
Z9 7
U1 0
U2 2
PU KANSAS ENTOMOLOGICAL SOC
PI LAWRENCE
PA PO BOX 368, LAWRENCE, KS 66044 USA
SN 0022-8567
J9 J KANSAS ENTOMOL SOC
JI J. Kans. Entomol. Soc.
PD APR
PY 2003
VL 76
IS 2
BP 236
EP 249
PG 14
WC Entomology
SC Entomology
GA 664XR
UT WOS:000182090400019
ER
PT J
AU Kalfatovic, MR
AF Kalfatovic, MR
TI Renaissance rivals: Michelangelo, Leonardo, Raphael, Titian.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Libs, Washington, DC USA.
RP Kalfatovic, MR (reprint author), Smithsonian Inst Libs, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 1
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 1
PY 2003
VL 128
IS 6
BP 94
EP 94
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 673WP
UT WOS:000182603500043
ER
PT J
AU Riley, S
AF Riley, S
TI Brown eyes blue.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 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 BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD APR 1
PY 2003
VL 128
IS 6
BP 130
EP 130
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 673WP
UT WOS:000182603500197
ER
PT J
AU Mair, RW
Wang, R
Rosen, MS
Candela, D
Cory, DG
Walsworth, RL
AF Mair, RW
Wang, R
Rosen, MS
Candela, D
Cory, DG
Walsworth, RL
TI Applications of controlled-flow laser-polarized xenon gas to porous and
granular media study
SO MAGNETIC RESONANCE IMAGING
LA English
DT Article; Proceedings Paper
CT 6th International Conference on the Recent Advances in Magnetic
Resonance Applications to Porous Media
CY SEP 08-12, 2002
CL UNIV ULM, ULM, GERMANY
HO UNIV ULM
DE Xe-129; He-3; diffusion; gases; laser-polarization; porous media; gas
flow; diffusive diffraction
ID HYPERPOLARIZED NOBLE-GASES; TO-VOLUME RATIO; FIELD-GRADIENT; DIFFUSION
NMR; FLUIDS; CONVECTION; TORTUOSITY; TRANSPORT; MOTION; ROCKS
AB We report initial NMR studies of continuous flow laser-polarized xenon gas, both in unrestricted tubing, and in a model porous media. The study uses Pulsed Gradient Spin Echo-based techniques in the gas-phase, with the aim of obtaining more sophisticated information than just translational self-diffusion coefficients. Pulsed Gradient Echo studies of continuous flow laser-polarized xenon gas in unrestricted tubing indicate clear diffraction minima resulting from a wide distribution of velocities in the flow field. The maximum velocity experienced in the flow can be calculated from this minimum, and is seen to agree with the information from the complete velocity spectrum, or motion propagator, as well as previously published images. The susceptibility of gas flows to parameters such as gas mixture content, and hence viscosity, are observed in experiments aimed at identifying clear structural features from echo attenuation plots of gas flow in porous media. Gas-phase NMR scattering, or position correlation flow-diffraction, previously clearly seen in the echo attenuation data from laser-polarized xenon flowing through a 2 mm glass bead pack is not so clear in experiments using a different gas mixture. A propagator analysis shows most gas in the sample remains close to static, while a small portion moves through a presumably near-unimpeded path at high velocities. (C) 2003 Elsevier Science Inc. All rights reserved.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
MIT, Cambridge, MA 02139 USA.
Univ Massachusetts, Amherst, MA 01003 USA.
RP Mair, RW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 29
TC 11
Z9 11
U1 0
U2 5
PU ELSEVIER SCIENCE INC
PI NEW YORK
PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA
SN 0730-725X
J9 MAGN RESON IMAGING
JI Magn. Reson. Imaging
PD APR-MAY
PY 2003
VL 21
IS 3-4
BP 287
EP 292
DI 10.1016/S0730-725X(03)00156-5
PG 6
WC Radiology, Nuclear Medicine & Medical Imaging
SC Radiology, Nuclear Medicine & Medical Imaging
GA 702DD
UT WOS:000184205700020
PM 12850720
ER
PT J
AU Fukami, H
Omori, M
Shimoike, K
Hayashibara, T
Hatta, M
AF Fukami, H
Omori, M
Shimoike, K
Hayashibara, T
Hatta, M
TI Ecological and genetic aspects of reproductive isolation by different
spawning times in Acropora corals
SO MARINE BIOLOGY
LA English
DT Article
ID MONTASTRAEA-ANNULARIS; EVOLUTIONARY HISTORY; GENUS ACROPORA; REEF;
MITOCHONDRIAL; SCLERACTINIA; PATTERNS; CNIDARIA; COMPLEX
AB In Okinawa, Japan, we found several species of the coral genus Acropora that spawn 1.5-3 h earlier than other mass-spawning acroporids. In six early-spawning species, gamete bundles appear on the surface of the colony ("setting") about 1 h before sunset, whereas setting occurs about 1 h after sunset in the more common late mass spawners. These early spawners are divided further into two sub-groups: three species that release their gametes within 1 h after setting and three that release their gametes 1.5-2 h after setting. DNA phylogenetic analyses show that each of these groups forms an independent genetic clade. These genetic relationships suggest that different spawning times form the basis of reproductive isolation among these broadcast-spawning corals. Late spawning appears to be the ancestral state, and the shift of spawning to earlier times may have played a role in the speciation process in these sympatric species.
C1 Ochanomizu Univ, Dept Biol, Tokyo 1128610, Japan.
Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
Akajima Marine Sci Lab, Okinawa, Zamami Son 9013311, Japan.
Seikai Natl Fisheries Res Inst, Okinawa, Ishigaki 9070451, Japan.
RP Hatta, M (reprint author), Ochanomizu Univ, Dept Biol, Tokyo 1128610, Japan.
NR 21
TC 39
Z9 40
U1 1
U2 9
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD APR
PY 2003
VL 142
IS 4
BP 679
EP 684
DI 10.1007/s00227-002-1001-8
PG 6
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 681JF
UT WOS:000183032500007
ER
PT J
AU Lazzati, D
Perna, R
AF Lazzati, D
Perna, R
TI Time-dependent photoionization in a dusty medium - III. The effect of
dust on the photoionization of metals
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE dust, extinction; gamma-rays : bursts; X-rays : general; X-rays : ISM
ID GAMMA-RAY BURST; CROSS-SECTIONS; ABSORPTION; GRB-990705; EVOLUTION;
SPECTRUM; NUCLEI
AB We use the time-dependent photoionization and dust destruction code recently developed by Perna and Lazzati to study the time evolution of the medium in a dusty gaseous cloud illuminated by a bright central source that sets on at time zero. We study the case of a bright source, which lasts for a time-scale much smaller than the recombination and dust creation time-scales. For this reason an equilibrium is never reached. We show that the presence of dust and its properties, such as its composition, can have a big effect on the time-scale for the evaporation of the soft X-ray absorption, in particular for ionizing sources with hard spectra. We discuss the profile of evaporation of the soft X-ray absorbing column, as well as how the apparent ionization state of the cloud evolves in time. We finally consider the apparent metallicity of the cloud that is left behind as a function of the cloud and ionizing source properties.
C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Harvard Soc Fellows, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lazzati, D (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM lazzati@ast.cam.ac.uk; rperna@cfa.harvard.edu
NR 29
TC 10
Z9 10
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD APR 1
PY 2003
VL 340
IS 2
BP 694
EP 704
DI 10.1046/j.1365-8711.2003.06334.x
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 658VG
UT WOS:000181740700031
ER
PT J
AU Labandeira, CC
AF Labandeira, CC
TI Reading the tree leaves
SO NATURAL HISTORY
LA English
DT Letter
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Labandeira, CC (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU AMER MUSEUM NAT HISTORY
PI NEW YORK
PA ATTN: LIBRARY SERIALS UNIT CENTRAL PK WEST AT 79TH ST, NEW YORK, NY
10024-5192 USA
SN 0028-0712
J9 NAT HIST
JI Nat. Hist.
PD APR
PY 2003
VL 112
IS 3
BP 13
EP 13
PG 1
WC Biodiversity Conservation; Ecology
SC Biodiversity & Conservation; Environmental Sciences & Ecology
GA 656ZN
UT WOS:000181641100011
ER
PT J
AU Lin, J
Soon, W
Baliunas, SL
AF Lin, J
Soon, W
Baliunas, SL
TI Theories of solar eruptions: a review
SO NEW ASTRONOMY REVIEWS
LA English
DT Review
DE the Sun; eruptions; theoretical mechanisms; MHD models; magnetic
reconnection
ID CORONAL MASS EJECTIONS; FREE MAGNETIC-FIELDS; POST-FLARE LOOPS;
FLUX-ROPE MODELS; 29 JULY 1973; SOFT-X-RAY; PHOTOSPHERIC MOTIONS;
MERIDIONAL PLANE; 2-RIBBON FLARES; EMERGING FLUX
AB This review highlights current theoretical research on eruptive phenomena in the solar atmosphere. We start by looking back upon the early theories and their development. Any theory and model of solar eruptions must explain two key aspects of eruption physics. The first aspect concerns the original cause of the eruption and the second pertains to the nature of the morphological features that form during its evolution. Those features include rapid ejection of large-scale magnetic flux and plasma into interplanetary space, and the separating of ribbons of Ha emission on the solar disk joined by a rising arcade of soft X-ray and Ha loops, with hard X-ray emission at their summits and feet. We intercompare relevant theories and models by discussing their advantages as well as by pointing out important aspects that need improvement, (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Lin, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM jlin@cfa.harvard.edu
RI LIN, JUN/B-9890-2017
NR 197
TC 119
Z9 125
U1 2
U2 4
PU ELSEVIER SCI LTD
PI OXFORD
PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND
SN 1387-6473
J9 NEW ASTRON REV
JI New Astron. Rev.
PD APR
PY 2003
VL 47
IS 2
BP 53
EP 84
DI 10.1016/S1387-6473(02)00271-3
PG 32
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 661WW
UT WOS:000181913700001
ER
PT J
AU Lovelock, CE
Andersen, K
Morton, JB
AF Lovelock, CE
Andersen, K
Morton, JB
TI Arbuscular mycorrhizal communities in tropical forests are affected by
host tree species and environment
SO OECOLOGIA
LA English
DT Article
DE Glomales; Acaulospora morrowiae; Acaulospora mellea; Acaulospora foveata
ID HYACINTHOIDES NON-SCRIPTA; RAIN-FOREST; ENDOMYCORRHIZAL FUNGI; ROOT
COLONIZATION; SPATIAL PATTERNS; PLANT DIVERSITY; ACER-SACCHARUM; SOIL
PATHOGENS; DYNAMICS; INOCULUM
AB Arbuscular mycorrhizal (AM) fungi are mutualists with plant roots that are proposed to enhance plant community diversity. Models indicate that AM fungal communities could maintain plant diversity in forests if functionally different communities are spatially separated. In this study we assess the spatial and temporal distribution of the AM fungal community in a wet tropical rainforest in Costa Rica. We test whether distinct fungal communities correlate with variation in tree life history characteristics, with host tree species, and the relative importance of soil type, seasonality and rainfall. Host tree species differ in their associated AM fungal communities, but differences in the AM community between hosts could not be generalized over life history groupings of hosts. Changes in the relative abundance of a few common AM fungal species were the cause of differences in AM fungal communities for different host tree species instead of differences in the presence and absence of AM fungal species. Thus, AM fungal communities are spatially distinguishable in the forest, even though all species are widespread. Soil fertility ranging between 5 and 9 Mg/ha phosphorus did not affect composition of AM fungal communities, although sporulation was more abundant in lower fertility soils. Sampling soils over seasons revealed that some AM fungal species sporulate profusely in the dry season compared to the rainy season. On one host tree species sampled at two sites with vastly different rainfall, relative abundance of spores from Acaulospora was lower and that of Glomus was relatively higher at the site with lower and more seasonal rainfall.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Univ Illinois, Program Ecol & Evolut, Urbana, IL 61801 USA.
W Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA.
RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
RI Lovelock, Catherine/G-7370-2012
OI Lovelock, Catherine/0000-0002-2219-6855
NR 88
TC 69
Z9 78
U1 2
U2 34
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD APR
PY 2003
VL 135
IS 2
BP 268
EP 279
DI 10.1007/s00442-002-1166-3
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 676LQ
UT WOS:000182753900013
PM 12698349
ER
PT J
AU Currie, CR
Bot, ANM
Boomsma, JJ
AF Currie, CR
Bot, ANM
Boomsma, JJ
TI Experimental evidence of a tripartite mutualism: bacteria protect ant
fungus gardens from specialized parasites
SO OIKOS
LA English
DT Article
ID LEAF-CUTTING ANTS; URINARY-TRACT INFECTIONS; GROWING ANTS; HYMENOPTERA;
FORMICIDAE; EVOLUTION; COOPERATION; AGRICULTURE; STIMULATION;
MAINTENANCE
AB Symbioses shape all levels of biological organization. Although symbiotic interactions are typically viewed as bipartite associations, with two organisms interacting largely in isolation from other organisms, the presence and importance of additional symbionts is becoming increasingly more apparent. This study examines the importance of a third mutualist within the ancient symbiosis between leaf-cutting ants and their fungal cultivars. Specifically, we experimentally examine the role of a filamentous bacterium (actinomycete), which is typically carried on the cuticle of fungus-growing ants, in suppressing the growth of a specialized microfungal parasite (Escovopsis) of the fungus garden. We conducted two-by-two factorial design experiments crossing the presence/absence of actinomycete with the presence/absence of Escovopsis within small sub-colonies of Acromyrmex octospinosus. In these experiments, infection by Escovopsis became much more extensive within fungus gardens and had a greater impact on the health of gat-dens in those sub-colonies with the bacterium removed from workers as compared to gardens with the bacterium still present on the ants. We establish that the actinomycete bacterium is most abundant on those major workers tending the garden, providing further support that the bacterium is involved in garden hygiene. We also found a significantly higher abundance of actinomycete on workers in colonies experimentally infected with Escovopsis as compared to uninfected control colonies. We suggest that mutualisms between antibiotic-producing microbes and higher organisms may be common associations that are mostly overlooked and that the role of symbionts in reducing the impact of parasites is likely an important aspect in the cost-benefit assessment of mutualisms.
C1 Univ Kansas, Dept Ecol & Evolut Biol, Lawrence, KS 66045 USA.
Aarhus Univ, Dept Ecol & Genet, Inst Biol Sci, DK-8000 Aarhus C, Denmark.
Univ Copenhagen, Inst Zool, Dept Populat Ecol, DK-2100 Copenhagen E, Denmark.
Univ Toronto, Dept Bot, Toronto, ON M5S 3B2, Canada.
Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Currie, CR (reprint author), Univ Kansas, Dept Ecol & Evolut Biol, 1200 Sunnyside Ave, Lawrence, KS 66045 USA.
EM ccurrie@ku.edu
RI Boomsma, Jacobus/M-2785-2014
OI Boomsma, Jacobus/0000-0002-3598-1609
NR 61
TC 95
Z9 102
U1 2
U2 41
PU WILEY-BLACKWELL
PI MALDEN
PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA
SN 0030-1299
J9 OIKOS
JI Oikos
PD APR
PY 2003
VL 101
IS 1
BP 91
EP 102
DI 10.1034/j.1600-0706.2003.12036.x
PG 12
WC Ecology
SC Environmental Sciences & Ecology
GA 665EL
UT WOS:000182106600010
ER
PT J
AU Forrey, RC
Jonsell, S
Saenz, A
Froelich, P
Dalgarno, A
AF Forrey, RC
Jonsell, S
Saenz, A
Froelich, P
Dalgarno, A
TI Cold collisions of spin-polarized metastable hydrogen atoms
SO PHYSICAL REVIEW A
LA English
DT Article
AB Cross sections and rate coefficients for collisions of two spin-polarized metastable hydrogen atoms are calculated at low energies and temperatures using complex scaling and Feshbach projection methods for the determination of the molecular potential-energy curves. The inclusion of the Lamb shift and fine-structure splitting of the excited n=2 atoms leads to an attractive van der Waals potential for two 2s(1/2) atoms with an exceptionally large coefficient. The quenching of the metastable atoms is dominated at temperatures below 20 mK by ionization. The calculated values for the total loss rate coefficient at 87 muK and 230 muK are within a factor of 2 or 3 of the error bars of recent measurements of metastable loss rate coefficients.
C1 Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA.
Umea Univ, Dept Phys, SE-90187 Umea, Sweden.
Univ Konstanz, Fachbereich Chem, D-78457 Constance, Germany.
Univ Uppsala, Dept Quantum Chem, S-75120 Uppsala, Sweden.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Forrey, RC (reprint author), Penn State Univ, Berks Lehigh Valley Coll, Reading, PA 19610 USA.
RI Jonsell, Svante/J-2251-2016
OI Jonsell, Svante/0000-0003-4969-1714
NR 10
TC 9
Z9 10
U1 0
U2 1
PU AMERICAN 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 APR
PY 2003
VL 67
IS 4
AR 040701
DI 10.1103/PhysRevA.67.040701
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 673WY
UT WOS:000182604300005
ER
PT J
AU Moore, MG
Sadeghpour, HR
AF Moore, MG
Sadeghpour, HR
TI Controlling two-species Mott-insulator phases in an optical lattice to
form an array of dipolar molecules
SO PHYSICAL REVIEW A
LA English
DT Article
ID BOSE-EINSTEIN CONDENSATION; BOSONIC ATOMS; FORCES
AB We consider the transfer of a two-species Bose-Einstein condensate (BEC) into an optical lattice with a density such that a Mott-insulator state with one atom per species per lattice site is obtained in a deep lattice regime. Depending on collisional and transition parameters, the result could be either a "mixed" or a "separated" Mott-insulator phase. Such a mixed two-species insulator would be well suited for the formation of dipolar molecules via photoassociation. The resulting array of dipolar molecules could then be used for the formation of a dipolar molecular condensate or for computation. For the case of a Rb-87-K-41 two-species BEC, however, the large interspecies scattering length makes it difficult to obtain the desired mixed Mott-insulator phase. To overcome this difficulty, we investigate the effect of varying the lattice frequency on the mean-field interaction and propose a favorable parameter regime, under which a lattice of dipolar molecules could be generated.
C1 Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
RP Moore, MG (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
NR 19
TC 21
Z9 22
U1 0
U2 2
PU AMERICAN 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 APR
PY 2003
VL 67
IS 4
AR 041603
DI 10.1103/PhysRevA.67.041603
PG 4
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 673WY
UT WOS:000182604300013
ER
PT J
AU Zygelman, B
Dalgarno, A
Jamieson, MJ
Stancil, PC
AF Zygelman, B
Dalgarno, A
Jamieson, MJ
Stancil, PC
TI Multichannel study of spin-exchange and hyperfine-induced frequency
shift and line broadening in cold collisions of hydrogen atoms
SO PHYSICAL REVIEW A
LA English
DT Article
ID CROSS-SECTIONS; GROUND-STATE; LOW-TEMPERATURES; SCATTERING; MASER;
ENERGIES; MOLECULE; RECOMBINATION; IONIZATION; OXYGEN
AB We calculate the cross sections that characterize the frequency shift and broadening of the resonance magnetic hyperfine transition in atomic hydrogen due to collisions with hydrogen atoms in a masing cavity. We consider collision energies that correspond to the temperature range, 10 mK delay 3 days, suggesting that submillimeter wavelengths tend to peak first. Only marginal day-to-day variations in flux density (2- 3 sigma) have been detected at 1.3 mm. No significant flares on a short timescale (similar to1 hr) have been observed at 1.3 mm. We also failed to detect significant periodic signals at a level of 5% (3 sigma) from Sgr A* in a periodic searching window ranging from 10 minutes to 2.5 hr. The flares observed at the wavelengths between short-centimeter and submillimeter might be a result of collective mass ejections associated with X-ray flares that originate from the inner region of the accretion disk near the supermassive black hole.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan.
Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA.
Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA.
RP Zhao, JH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA.
EM jzhao@cfa.harvard.edu; kyoung@cfa.harvard.edu; rmcgary@cfa.harvard.edu;
pho@cfa.harvard.edu; ttsutsumi@cfa.harvard.edu; flo@nrao.edu;
mgoss@aoc.nrao.edu; gbower@astron.berkeley.edu
NR 28
TC 79
Z9 80
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 20
PY 2003
VL 586
IS 1
BP L29
EP L32
DI 10.1086/374581
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 653RX
UT WOS:000181451800007
ER
PT J
AU Palmer, PI
Jacob, DJ
Fiore, AM
Martin, RV
Chance, K
Kurosu, TP
AF Palmer, PI
Jacob, DJ
Fiore, AM
Martin, RV
Chance, K
Kurosu, TP
TI Mapping isoprene emissions over North America using formaldehyde column
observations from space
SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES
LA English
DT Article
DE Isoprene; Formaldehyde; GOME; biogenic emissions; satellite instrument;
volatile organic compounds
ID VOLATILE ORGANIC-COMPOUNDS; OZONE MONITORING EXPERIMENT; SOUTHEASTERN
UNITED-STATES; CARBONYL-COMPOUNDS; ATMOSPHERIC CHEMISTRY; TRANSPORT;
OXIDATION; MECHANISM; MODEL; GOME
AB [1] We present a methodology for deriving emissions of volatile organic compounds (VOC) using space-based column observations of formaldehyde ( HCHO) and apply it to data from the Global Ozone Monitoring Experiment (GOME) satellite instrument over North America during July 1996. The HCHO column is related to local VOC emissions, with a spatial smearing that increases with the VOC lifetime. Isoprene is the dominant HCHO precursor over North America in summer, and its lifetime (similar or equal to1 hour) is sufficiently short that the smearing can be neglected. We use the Goddard Earth Observing System global 3-D model of tropospheric chemistry (GEOS-CHEM) to derive the relationship between isoprene emissions and HCHO columns over North America and use these relationships to convert the GOME HCHO columns to isoprene emissions. We also use the GEOS-CHEM model as an intermediary to validate the GOME HCHO column measurements by comparison with in situ observations. The GEOS-CHEM model including the Global Emissions Inventory Activity (GEIA) isoprene emission inventory provides a good simulation of both the GOME data (r(2) = 0.69, n = 756, bias = + 11%) and the in situ summertime HCHO measurements over North America (r(2) = 0.47, n = 10, bias = -3%). The GOME observations show high values over regions of known high isoprene emissions and a day-to-day variability that is consistent with the temperature dependence of isoprene emission. Isoprene emissions inferred from the GOME data are 20% less than GEIA on average over North America and twice those from the U. S. EPA Biogenic Emissions Inventory System (BEIS2) inventory. The GOME isoprene inventory when implemented in the GEOS-CHEM model provides a better simulation of the HCHO in situ measurements than either GEIA or BEIS2 (r(2) = 0.71, n = 10, bias = -10%).
C1 Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Atom Div, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Div Mol Phys, Cambridge, MA 02138 USA.
RP Palmer, PI (reprint author), Harvard Univ, Div Engn & Appl Sci, Cambridge, MA 02138 USA.
EM pip@io.harvard.edu
RI Martin, Randall/A-2051-2008; Palmer, Paul/F-7008-2010; Martin,
Randall/C-1205-2014; Chem, GEOS/C-5595-2014
OI Martin, Randall/0000-0003-2632-8402;
NR 48
TC 181
Z9 181
U1 6
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 MAR 20
PY 2003
VL 108
IS D6
AR 4180
DI 10.1029/2002JD002153
PG 16
WC Meteorology & Atmospheric Sciences
SC Meteorology & Atmospheric Sciences
GA 667GK
UT WOS:000182222800002
ER
PT J
AU Marshall, D
Groat, L
Giuliani, G
Murphy, D
Mattey, D
Ercit, TS
Wise, MA
Wengzynowski, W
Eaton, WD
AF Marshall, D
Groat, L
Giuliani, G
Murphy, D
Mattey, D
Ercit, TS
Wise, MA
Wengzynowski, W
Eaton, WD
TI Pressure, temperature and fluid conditions during emerald precipitation,
southeastern Yukon, Canada: fluid inclusion and stable isotope evidence
SO CHEMICAL GEOLOGY
LA English
DT Article; Proceedings Paper
CT 16th Biennial European Current Research on Fluid Inclusions (ECROFI)
CY MAY 02-06, 2001
CL OPORTO, PORTUGAL
SP Fluids & Metallog Team, GIMEF, Dept Geol, Univ Porto Ctr Geol
DE fluid inclusions; stable isotopes; emerald; thermobarometry; Yukon
ID OXYGEN-ISOTOPE; H2O-CO2-NACL FLUIDS; SOUTH-AFRICA; MINERALIZATION;
EVOLUTION; SYSTEM; FRACTIONATION; TRANSVAAL; EQUATION; COLOMBIA
AB The Crown emerald veins are somewhat enigmatic, displaying characteristics that are common to emerald deposits of tectonic-hydrothermal origin and of igneous origin. The veins cut the Fire Lake mafic meta-volcanic rocks, occurring within 600 m of an outcrop of Cretaceous S-type granite. Field work and vein petrography are consistent with a polythermal origin for the veins. The primary vein mineralogy is quartz and tourmaline with variable sized alteration haloes consisting of tourmaline, quartz, muscovite, chlorite and emerald. The veins weather a buff brown colour due to jarosite, scheelite and minor lepidocrocite, which were precipitated during the waning stages of vein formation. Microthermometic studies of primary fluid inclusions within emerald growth zones are consistent with emerald precipitation from H2O-CO2-CH4 ( +/- N-2 +/- H2S) bearing saline brines. The estimated fluid composition is approximately 0.9391 mol% H2O, 0.0473 mol% CO2, 0.0077 mol% CH4 and 0.0059 mol% NaCl ( similar to 2 wt.% NaCl eq.). Fluid inclusion and stable isotope studies are consistent with vein formation in the temperature range 365-498 T, with corresponding pressures along fluid inclusion isochore paths ranging from 700 to 2250 bars. These data correlate with a very slow uplift rate for the region of 0.02-0.07 mm/year.
Emerald deposits are generally formed when geological conditions bring together Cr (+/- V) and Be. Cr and V are presumed to have been derived locally from the mafic and ultramafic rocks during hydrothermal alteration. The Be is most likely derived from the nearby Cretaceous granite intrusion. (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada.
Univ British Columbia, Vancouver, BC V6T 1Z4, Canada.
Ctr Rech Petrog & Geochim, UPR A 6821, F-54501 Vandoeuvre Les Nancy, France.
Govt Yukon, Yukon Geol Program, Whitehorse, YT Y1A 2C6, Canada.
Univ London, Dept Geol, Egham TW20 OEX, Surrey, England.
Canadian Museum Nat, Div Res, Ottawa, ON K1P 6P4, Canada.
Smithsonian Inst, Mineral Sci NHB119, Washington, DC 20560 USA.
Expatriate Resources Ltd, Vancouver, BC V6B 1L8, Canada.
Archer Cathro & Associates 1981 Ltd, Vancouver, BC V6B 1L8, Canada.
RP Marshall, D (reprint author), Simon Fraser Univ, Dept Earth Sci, Burnaby, BC V5A 1S6, Canada.
NR 35
TC 8
Z9 9
U1 0
U2 9
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0009-2541
J9 CHEM GEOL
JI Chem. Geol.
PD MAR 15
PY 2003
VL 194
IS 1-3
BP 187
EP 199
AR PII S0009-2541(02)00277-2
DI 10.1016/S0009-2541(02)00277-2
PG 13
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 654RH
UT WOS:000181509500011
ER
PT J
AU Schroll, S
AF Schroll, S
TI Mondrian, 1892-1914: The path to abstraction.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst Libs, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD MAR 15
PY 2003
VL 128
IS 5
BP 80
EP 80
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 672LZ
UT WOS:000182523300025
ER
PT J
AU Doherty, M
Johnston, S
Green, AJ
Roberts, MSE
Romani, RW
Gaensler, BM
Crawford, F
AF Doherty, M
Johnston, S
Green, AJ
Roberts, MSE
Romani, RW
Gaensler, BM
Crawford, F
TI A search for the radio counterpart of the unidentified gamma-ray source
3EG J1410-6147
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE pulsars : individual : J1412-6145; pulsars : individual : J1413-6141
ID GALACTIC PLANE SURVEY; SUPERNOVA REMNANT; INNER GALAXY; YOUNG PULSAR;
MILKY-WAY; H-I; EMISSION; G312.4-0.4; DISCOVERY; SPECTRUM
AB We have made radio continuum, H I and X-ray observations in the direction of the unidentified EGRET source 3EG J1410-6147, using the Australia Telescope Compact Array and the Chandra X-ray Observatory. The observations encompass the supernova remnant (SNR) G312.4-0.4 and the two young pulsars PSRs J1412-6145 and J1413-6141.
We derive a lower distance limit of 6 kpc to the SNR, although interpretation of positive velocity features in the H I spectrum may imply that the SNR is more distant than 14 kpc. PSR J1412-6145, with an age of 50 kyr, is the pulsar most probably associated with SNR G312.4-0.4. X-rays are not detected from either pulsar and diffuse X-ray emission near the bright western edge of the SNR is weak. Although there is circumstantial evidence that this western region is a pulsar wind nebula (PWN), the embedded pulsar PSR J1412-6145 is apparently not sufficiently powerful to explain the radio enhancement. The origin of the electron acceleration in this region and of the gamma-rays remains unidentified, unless the distance to PSR J1413-6141 is at least a factor of 3 lower than its dispersion measure distance.
C1 Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia.
McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada.
Stanford Univ, Dept Phys, Stanford, CA 94025 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Haverford Coll, Dept Phys, Haverford, PA 19041 USA.
RP Doherty, M (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
EM md@ast.cam.ac.uk
RI Gaensler, Bryan/F-8655-2010
NR 37
TC 11
Z9 11
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 MAR 11
PY 2003
VL 339
IS 4
BP 1048
EP 1056
DI 10.1046/j.1365-8711.2003.06265.x
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650VD
UT WOS:000181283300016
ER
PT J
AU Perna, R
Lazzati, D
Fiore, F
AF Perna, R
Lazzati, D
Fiore, F
TI Time-dependent photoionization in a dusty medium. II. Evolution of dust
distributions and optical opacities
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE dust, extinction; galaxies : ISM
ID GAMMA-RAY BURST; ACTIVE GALACTIC NUCLEI; X-RAY; ABSORPTION; DESTRUCTION;
SPECTRUM; GRAINS; ENVIRONMENTS; CONSTRAINTS; AFTERGLOWS
AB The interaction of a radiation field with a dusty medium is a relevant issue in several astrophysical contexts. We use the time-dependent photoionization code in a dusty medium developed by Perna & Lazzati to study the modi cations in the dust distribution and the relative optical opacities when a strong X-ray/UV radiation flux propagates into a medium. We find that silicates are preferentially destroyed with respect to graphite, and the extinction curve becomes significantly flatter (hence implying less reddening), with the characteristic bump at 2175 Angstrom being highly suppressed because of the destruction of the small graphite grains. This could explain the observational lack of such a feature in gamma-ray burst afterglow and active galactic nuclei spectra. For a very intense and highly variable source irradiating a compact and dense region, time variability in the optical opacity resulting from dust destruction can be observed on a relatively short timescale. We show that, under these circumstances, monitoring the time variability of the opacity can yield powerful clues to the properties of dust in the environment of the source. In particular, it allows one to break the observational degeneracy as to whether a gray extinction is the result of a low dust-to-gas ratio or of a dust grain distribution that is skewed toward large grains.
C1 Harvard Soc Fellows, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Osserv Astron Roma, I-00040 Rome, Italy.
RP Perna, R (reprint author), Harvard Soc Fellows, 74 Mt Auburn St, Cambridge, MA 02138 USA.
OI Fiore, Fabrizio/0000-0002-4031-4157
NR 29
TC 68
Z9 68
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2003
VL 585
IS 2
BP 775
EP 784
DI 10.1086/346109
PN 1
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650WU
UT WOS:000181287200019
ER
PT J
AU Li, D
Goldsmith, PF
AF Li, D
Goldsmith, PF
TI HI narrow self-absorption in dark clouds
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE ISM : atoms; ISM : clouds; ISM : molecules; radio lines : ISM
ID WARM NEUTRAL HALOS; CARBON-MONOXIDE ABUNDANCE; MOLECULAR CLOUDS;
INTERSTELLAR GAS; ATOMIC-HYDROGEN; MAGNETIC-FIELD; I OBSERVATIONS;
MASSIVE CLOUD; LINE EMISSION; CORES
AB We have used the Arecibo telescope to carry out a survey of 31 dark clouds in the Taurus/Perseus region for narrow absorption features in H I (21 cm) and OH (1667 and 1665 MHz) emission. We detected H I narrow self-absorption (HINSA) in 77% of the clouds that we observed. HINSA and OH emission, observed simultaneously, are remarkably well correlated. Spectrally, they have the same nonthermal line width and the same line centroid velocity. Spatially, they both peak at the optically selected central position of each cloud, and both fall off toward the cloud edges. Sources with clear HINSA features have also been observed in transitions of CO, (CO)-C-13, (CO)-O-18, and C I. HINSA exhibits better correlation with molecular tracers than with C I. The line width of the absorption feature, together with analyses of the relevant radiative transfer, provides upper limits to the kinetic temperature of the gas producing the HINSA. Some sources must have a temperature close to or lower than 10 K. The correlation of column densities and line widths of HINSA with those characteristics of molecular tracers suggests that a significant fraction of the atomic hydrogen is located in the cold, well-shielded portions of molecular clouds and is mixed with the molecular gas. The average number density ratio [H I] / [H-2] is 1.5 x 10(-3). The inferred H I density appears consistent with, but slightly higher than, the value expected in steady state equilibrium between formation of H I via cosmic-ray destruction of H-2 and destruction via formation of H-2 on grain surfaces. The distribution and abundance of atomic hydrogen in molecular clouds are critical tests of dark cloud chemistry and structure, including the issues of grain surface reaction rates, PDRs, circulation, and turbulent diffusion.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
RP Li, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Goldsmith, Paul/H-3159-2016
NR 66
TC 66
Z9 67
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2003
VL 585
IS 2
BP 823
EP 839
DI 10.1086/346227
PN 1
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650WU
UT WOS:000181287200022
ER
PT J
AU Redfield, S
Ayres, TR
Linsky, JL
Ake, TB
Dupree, AK
Robinson, RD
Young, PR
AF Redfield, S
Ayres, TR
Linsky, JL
Ake, TB
Dupree, AK
Robinson, RD
Young, PR
TI A Far Ultraviolet Spectroscopic Explorer survey of coronal forbidden
lines in late-type stars
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE line : profiles; stars : coronae; stars : late-type; ultraviolet :
stars; X-rays : stars
ID HIGH-RESOLUTION SPECTROGRAPH; OBSERVING STELLAR CORONAE; X-RAY-EMISSION;
A-TYPE STARS; ROTATIONAL VELOCITIES; RADIAL-VELOCITIES; TRANSITION
REGION; HERTZSPRUNG GAP; BINARY-SYSTEM; CAPELLA
AB We present a survey of coronal forbidden lines detected in Far Ultraviolet Spectroscopic Explorer (FUSE) spectra of nearby stars. Two strong coronal features, Fe XVIII lambda974 and Fe XIX lambda1118, are observed in 10 of the 26 stars in our sample. Various other coronal forbidden lines, observed in solar ares, also were sought but not detected. The Fe XVIII feature, formed at log T = 6 : 8 K, appears to be free of blends, whereas the Fe XIX line can be corrupted by a C I multiplet. FUSE observations of these forbidden iron lines at spectral resolution = lambda/Deltalambda similar to 15,000 provides the opportunity to study dynamics of hot coronal plasmas. We find that the velocity centroid of the Fe XVIII feature deviates little from the stellar rest frame, confirming that the hot coronal plasma is confined. The observed line widths generally are consistent with thermal broadening at the high temperatures of formation and show little indication of additional turbulent broadening. The fastest rotating stars, 31 Com, alpha Aur Ab, and AB Dor, show evidence for excess broadening beyond the thermal component and the photospheric v sin i. The anomalously large widths in these fast-rotating targets may be evidence for enhanced rotational broadening, consistent with emission from coronal regions extending an additional DeltaR similar to 0.4-1.3 R-* above the stellar photosphere, or represent the turbulent broadening caused by flows along magnetic loop structures. For the stars in which Fe XVIII is detected, there is an excellent correlation between the observed Rontgensatellit (ROSAT) 0.2-2.0 keV soft X-ray flux and the coronal forbidden line flux. As a result, Fe XVIII is a powerful new diagnostic of coronal thermal conditions and dynamics that can be utilized to study high-temperature plasma processes in late-type stars. In particular, FUSE provides the opportunity to obtain observations of important transition region lines in the far-UV, as well as simultaneous measurements of soft X-ray coronal emission, using the Fe XVIII coronal forbidden line.
C1 Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA.
Natl Inst Stand & Technol, Boulder, CO 80309 USA.
Univ Colorado, CASA, Boulder, CO 80309 USA.
Johns Hopkins Univ, Baltimore, MD 21218 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Rutherford Appleton Lab, Space Sci & Technol Dept, Didcot OX11 0QX, Oxon, England.
RP Redfield, S (reprint author), Univ Colorado, Joint Inst Lab Astrophys, Boulder, CO 80309 USA.
OI Redfield, Seth/0000-0003-3786-3486
NR 54
TC 39
Z9 39
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2003
VL 585
IS 2
BP 993
EP 1006
DI 10.1086/346129
PN 1
PG 14
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650WU
UT WOS:000181287200037
ER
PT J
AU Uzzo, M
Ko, YK
Raymond, JC
Wurz, P
Ipavich, FM
AF Uzzo, M
Ko, YK
Raymond, JC
Wurz, P
Ipavich, FM
TI Elemental abundances for the 1996 streamer belt
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE solar wind; Sun : abundances; Sun : corona
ID SLOW SOLAR-WIND; ULTRAVIOLET CORONAGRAPH SPECTROMETER; SOURCE REGIONS;
SOHO; MINIMUM; ORIGIN; TEMPERATURE; TELESCOPE; UVCS/SOHO; LINES
AB The purpose of this paper is to explore the observed physical characteristics of the solar corona streamer belt from 1996 June 1 to August 5. The UV spectral data was collected by the Ultraviolet Coronagraph Spectrometer (UVCS) instrument on board the Solar and Heliospheric Observatory (SOHO) spacecraft. From this data the abundances of oxygen, silicon, and magnesium were determined on an almost daily basis during this time period at both the west and east limbs. The streamer belt was composed of both active and quiescent streamers, which allows for the comparison of these two categories of magnetic field structures. The depletion of these three elemental abundances in the core of quiescent streamers was found, as in previous observations. The variance in abundance with solar rotation was investigated as a consequence of the long time frame considered here. The first ionization potential (FIP) effect was present in the data, and the danger of exploring this phenomena by the traditional FIP bias was also covered. A comparison with in situ elemental abundance data from the Charge, Element, and Isotope Analysis System (CELIAS) instrument on SOHO provides evidence suggesting that active-region streamers and the outer leg structural component of quiescent streamers are definite contributors to the slow solar wind.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Bern, Inst Phys, CH-3012 Bern, Switzerland.
Univ Maryland, College Pk, MD 20742 USA.
RP Uzzo, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 32
TC 25
Z9 25
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2003
VL 585
IS 2
BP 1062
EP 1072
DI 10.1086/346132
PN 1
PG 11
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650WU
UT WOS:000181287200043
ER
PT J
AU Hasan, SS
Kalkofen, W
van Ballegooijen, AA
Ulmschneider, P
AF Hasan, SS
Kalkofen, W
van Ballegooijen, AA
Ulmschneider, P
TI Kink and longitudinal oscillations in the magnetic network on the Sun:
Nonlinear effects and mode transformation
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE MHD; Sun : magnetic fields; Sun : oscillations
ID SOLAR TRANSITION REGION; STELLAR CONVECTION ZONES; PHOTOSPHERIC FLUX
TUBES; ENERGY-BALANCE; INTERNETWORK OSCILLATIONS; SUMER OBSERVATIONS;
TRANSVERSE WAVES; ATMOSPHERE; CHROMOSPHERE; GENERATION
AB We examine the propagation of kink and longitudinal waves in the solar magnetic network. Previously, we investigated the excitation of network oscillations in vertical magnetic flux tubes through buffeting by granules and found that footpoint motions of the tubes can generate sufficient wave energy for chromospheric heating. We assumed that the kink and longitudinal waves are decoupled and linear. We overcome these limitations by treating the nonlinear MHD equations for coupled kink and longitudinal waves in a thin flux tube. For the parameters we have chosen, the thin tube approximation is valid up to the layers of formation of the emission features in the H and K lines of Ca II at a height of about 1 Mm. By solving the nonlinear, time-dependent MHD equations we are able to study the onset of wave coupling, which occurs when the Mach number of the kink waves is of the order of 0.3. We also investigate the transfer of energy from the kink to the longitudinal waves, which is important for the dissipation of the wave energy in shocks. We find that kink waves excited by footpoint motions of a flux tube generate longitudinal modes by mode coupling. For subsonic velocities, the amplitude of a longitudinal wave increases as the square of the amplitude of the transverse wave, and for amplitudes near Mach number unity, the coupling saturates and becomes linear when the energy is nearly evenly divided between the two modes.
C1 Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Inst Theoret Astrophys, D-69012 Heidelberg, Germany.
RP Indian Inst Astrophys, Bangalore 560034, Karnataka, India.
RI Hasan, Siraj/C-2927-2012;
OI van Ballegooijen, Adriaan/0000-0002-5622-3540
NR 52
TC 38
Z9 38
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
EI 1538-4357
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 10
PY 2003
VL 585
IS 2
BP 1138
EP 1146
DI 10.1086/346102
PN 1
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 650WU
UT WOS:000181287200049
ER
PT J
AU Bunyavejchewin, S
LaFrankie, JV
Baker, PJ
Kanzaki, M
Ashton, PS
Yamakura, T
AF Bunyavejchewin, S
LaFrankie, JV
Baker, PJ
Kanzaki, M
Ashton, PS
Yamakura, T
TI Spatial distribution patterns of the dominant canopy dipterocarp species
in a seasonal dry evergreen forest in western Thailand
SO FOREST ECOLOGY AND MANAGEMENT
LA English
DT Article
DE spatial patterns; dipterocarps; Thailand
ID TROPICAL TREE; NEOTROPICAL FOREST; RAIN-FOREST; DIVERSITY; SEEDLINGS;
DISPERSAL; DENSITY
AB Population structure and spatial patterns were examined for four species of canopy dipterocarps (Anisoptera costata, Dipterocarpus alatus, Hopea odorata, Vatica cinerea) in a 50 ha plot in seasonal dry evergreen forest at the Huai Kha Khaeng Wildlife Sanctuary in western Thailand. Spatial dispersion was assessed with Morisita's index for quadrat sizes ranging from 61 m(2) to 25 ha; spatial attraction and repulsion between species and size classes were measured with Iwao's index. Only Vatica had a negative exponential diameter distribution suggesting continuous recruitment. The other species had either normal (Hopea) or irregular diameter distributions with peaks in the large size classes (Anisoptera, Dipterocarpus). All four species were significantly clumped at most quadrat sizes. At the local scale, saplings and poles of Hopea and Anisoptera were negatively associated with adults at quadrat sizes <1000-5000 m(2), while the distributions of Dipterocarpus and Vatica saplings and poles were independent of adult trees. In general, saplings and poles were always positively associated with each other. Spatial segregation among species may imply habitat specialization. A torus-translation analysis of habitat association for each of the dipterocarp species revealed both positive and negative species- specific associations. At HKK,most of the dipterocarps' spatial distributions were independent of each other and there was no evidence of strong spatial segregation among species. The irregular diameter distributions, clumping at large spatial scales, and lack of positive association between juvenile and adult stems suggest that many of the dipterocarps at the 50 ha plot may have established after a large-scale catastrophic disturbance. In the absence of catastrophic disturbance, we hypothesize that the Hopea and Anisoptera populations will eventually disappear from the plot because of a lack of suitable recruitment conditions. (C) 2002 Elsevier Science B.V. All rights reserved.
C1 Royal Thai Forest Dept, Silvicultural Res Div, Forest Res Off, Bangkok 10900, Thailand.
Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Singapore 1025, Singapore.
Univ Washington, Coll Forest Resources, Seattle, WA 98195 USA.
Kyoto Univ, Grad Sch Agr, Kyoto 6068502, Japan.
Harvard Univ, Arnold Arboretum, Cambridge, MA 02138 USA.
Osaka City Univ, Fac Sci, Dept Biol, Sumiyoshi Ku, Osaka 5588585, Japan.
RP Baker, PJ (reprint author), US Forest Serv, USDA, Pacific SW Res Stn, Inst Pacific Isl Forestry, 23 E Kawili St, Hilo, HI 96720 USA.
OI Baker, Patrick/0000-0002-6560-7124
NR 38
TC 41
Z9 50
U1 4
U2 20
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0378-1127
J9 FOREST ECOL MANAG
JI For. Ecol. Manage.
PD MAR 3
PY 2003
VL 175
IS 1-3
BP 87
EP 101
AR PII S0378-1127(02)00126-3
DI 10.1016/S0378-1127(02)00126-3
PG 15
WC Forestry
SC Forestry
GA 654NY
UT WOS:000181504000006
ER
PT J
AU Oliver, JE
Weldon, PJ
Petersen, KS
Schmidt, WF
Debboun, M
AF Oliver, JE
Weldon, PJ
Petersen, KS
Schmidt, WF
Debboun, M
TI Mosquito-deterring acid from pelage of gaur, Bos gaurus.
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 225th National Meeting of the American-Chemical-Society
CY MAR 23-27, 2003
CL NEW ORLEANS, LA
SP Amer Chem Soc
C1 USDA ARS, BARC W, Chem Affecting Insect Behav Lab, Beltsville, MD 20705 USA.
Smithsonian Inst, Conservat & Res Ctr, Washington, DC 20560 USA.
USDA ARS, NRI, Environm Chem Lab, Washington, DC 20250 USA.
EM oliverj@ba.ars.usda.gov
NR 0
TC 0
Z9 0
U1 1
U2 1
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 MAR
PY 2003
VL 225
MA AGFD-030
BP U73
EP U73
PN 1
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 761PU
UT WOS:000187917800243
ER
PT J
AU Tuross, N
AF Tuross, N
TI Twilight zone of the fossilization process.
SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY
LA English
DT Meeting Abstract
CT 225th National Meeting of the American-Chemical-Society
CY MAR 23-27, 2003
CL NEW ORLEANS, LA
SP Amer Chem Soc
C1 Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20740 USA.
EM ntuross@lab.si.edu
NR 0
TC 0
Z9 0
U1 0
U2 0
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 MAR
PY 2003
VL 225
MA 131-GEOC
BP U932
EP U932
PN 1
PG 1
WC Chemistry, Multidisciplinary
SC Chemistry
GA 761PU
UT WOS:000187917804336
ER
PT J
AU Kreamer, CM
AF Kreamer, CM
TI A tribute to Roy Sieber (Shaping the discipline of African art history)
SO AFRICAN ARTS
LA English
DT Article
C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
RP Kreamer, CM (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA.
NR 10
TC 1
Z9 1
U1 0
U2 0
PU UNIV CALIF
PI LOS ANGELES
PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 USA
SN 0001-9933
J9 AFR ARTS
JI Afr. Arts
PD SPR
PY 2003
VL 36
IS 1
BP 12
EP +
PG 0
WC Art
SC Art
GA 721TH
UT WOS:000185333100003
ER
PT J
AU Paerl, HW
Steppe, TF
Buchan, KC
Potts, M
AF Paerl, HW
Steppe, TF
Buchan, KC
Potts, M
TI Hypersaline cyanobacterial mats as indicators of elevated tropical
hurricane activity and associated climate change
SO AMBIO
LA English
DT Article
ID BASIN
AB The Atlantic hurricanes of 1999 caused widespread environmental damage throughout the Caribbean and US mid-Atlantic coastal regions. However, these storms also proved beneficial to certain microbial habitats; specifically, cyanobacteria-dominated mats. Modern mats represent the oldest known biological communities on earth, stromatolites. Contemporary mats are dominant biological communities in the hypersaline Bahamian lakes along the Atlantic hurricane track. We examined the impacts of varying levels of hypersalinity on 2 processes controlling mat growth, photosynthesis and nitrogen fixation, in Salt Pond, San Salvador Island, Bahamas. Hypersalinity (> 5 times sea-water salinity) proved highly inhibitory to these processes. Freshwater input from Hurricane Floyd and other large storms alleviated this salt-inhibition. A predicted 10 to 40 year increase in Atlantic hurricane activity accompanied by more frequent "freshening" events will enhance mat productivity, CO2 sequestration and nutrient cycling. Cyanobacterial mats are sensitive short- and long-term indicators of climatic and ecological changes impacting these and other waterstressed environments.
C1 Univ N Carolina, Inst Marine Sci, Morehead City, NC 28557 USA.
Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
Virginia Tech, Ctr Genom, Blacksburg, VA USA.
RP Paerl, HW (reprint author), Univ N Carolina, Inst Marine Sci, 3431 Arendell St, Morehead City, NC 28557 USA.
NR 23
TC 20
Z9 20
U1 2
U2 10
PU ROYAL SWEDISH ACAD SCIENCES
PI STOCKHOLM
PA PUBL DEPT BOX 50005, S-104 05 STOCKHOLM, SWEDEN
SN 0044-7447
J9 AMBIO
JI Ambio
PD MAR
PY 2003
VL 32
IS 2
BP 87
EP 90
DI 10.1639/0044-7447(2003)032[0087:HCMAIO]2.0.CO;2
PG 4
WC Engineering, Environmental; Environmental Sciences
SC Engineering; Environmental Sciences & Ecology
GA 677GN
UT WOS:000182798700003
PM 12733791
ER
PT J
AU Ryan, MJ
Rand, W
Hurd, PL
Phelps, SM
Rand, AS
AF Ryan, MJ
Rand, W
Hurd, PL
Phelps, SM
Rand, AS
TI Generalization in response to mate recognition signals
SO AMERICAN NATURALIST
LA English
DT Article
DE generalization gradients; mate recognition; preference functions; sexual
selection; species recognition; tungara frogs
ID FEMALE MATING PREFERENCES; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION;
TUNGARA FROGS; ADVERTISEMENT CALLS; SPECIES RECOGNITION; NEOTROPICAL
FROG; NEURAL NETWORKS; HYLA-EBRACCATA; OLFACTORY CUES
AB Females usually exhibit strong and unequivocal recognition of conspecific mating signals and reject those of other sympatric heterospecifics. However, most species are allopatric with one another, and the degree to which females recognize mating signals of allopatric species is more varied. Such mating signals are often rejected but are sometimes falsely recognized as conspecific. We studied the dynamics of mate recognition in female tungara frogs (Physalaemus pustulosus) in response to a series of calls that were intermediate between the conspecific and each of five allopatric-heterospecific calls: two that elicited recognition from females in previous studies and three that did not. This study shows that females perceive variation in allopatric mating signals in a continuous manner with no evidence of perceptual category formation. The strength of recognition is predicted by how different the target stimulus is from the conspecific call within a series of calls. But the differences in recognition responses among call series are not predicted by the similarity of the call series to the conspecific call. The latter result suggests that the strength of recognition of allopatric signals might be influenced by processes of stimulus generalization and past evolutionary history.
C1 Univ Texas, Ctr Integrated Biol C0930, Austin, TX 78712 USA.
Smithsonian Trop Res Inst, Balboa, Panama.
Tufts Univ, Sch Med, Dept Community Hlth, Boston, MA 02111 USA.
Univ Alberta, Dept Psychol, Edmonton, AB T6G 2E9, Canada.
Emory Univ, Ctr Behav Neurosci, Atlanta, GA 30329 USA.
RP Ryan, MJ (reprint author), Univ Texas, Ctr Integrated Biol C0930, Austin, TX 78712 USA.
RI Hurd, Peter/A-4342-2009
OI Hurd, Peter/0000-0002-4389-0846
NR 68
TC 54
Z9 58
U1 0
U2 11
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0003-0147
J9 AM NAT
JI Am. Nat.
PD MAR
PY 2003
VL 161
IS 3
BP 380
EP 394
DI 10.1086/367588
PG 15
WC Ecology; Evolutionary Biology
SC Environmental Sciences & Ecology; Evolutionary Biology
GA 656MZ
UT WOS:000181612700003
PM 12699219
ER
PT J
AU Heyer, WR
Reid, YR
AF Heyer, WR
Reid, YR
TI Does advertisement call variation coincide with genetic variation in the
genetically diverse frog taxon currently known as Leptodactylus fuscus
(Amphibia : Leptodactylidae)?
SO ANAIS DA ACADEMIA BRASILEIRA DE CIENCIAS
LA English
DT Article
DE advertisement calls; Leptodactylus fuscus; speciation
ID HYLA ARENICOLOR COPE; NEOTROPICAL FROG; CANYON TREEFROG; ANURA;
DIVERGENCE; TOADS
AB The frog Leptodactylus fuscus is found throughout much of South America in open and disturbed habitats. Previous study of genetic differentiation in L fuscus demonstrated that there was lack of genetic exchange among population units consistent with multiple species, rather than a single species. We examine advertisement vocalizations of L. fuscus to determine whether call variation coincides with genetic differentiation. Calls were analyzed for 32 individual frogs from 25 localities throughout the distributional range of L. fuscus. Although there is variation in calls among geographic samples, call variation is not concordant with genetic variation or geographic distance and the call variation observed is less than that typically found among other closely related species of Leptodactylus. This study is an example of the rare pattern of strong genetic differentiation unaccompanied by salient differences in advertisement calls. The relative infrequency of this pattern as currently understood may only reflect the lack of detailed analyses of genetic and acoustic differentiation within population systems currently understood as single species with substantial geographic distributions.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA.
Haskell Indian Nations Univ, Lawrence, KS 66044 USA.
RP Heyer, WR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Systemat Biol, Washington, DC 20560 USA.
NR 32
TC 25
Z9 29
U1 0
U2 3
PU ACAD BRASILEIRA DE CIENCIAS
PI RIO JANEIRO
PA RUA ANFILOFIO DE CARVALHO, 29, 3 ANDAR, 20030-060 RIO JANEIRO, BRAZIL
SN 0001-3765
J9 AN ACAD BRAS CIENC
JI An. Acad. Bras. Cienc.
PD MAR
PY 2003
VL 75
IS 1
BP 39
EP 54
PG 16
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 656PC
UT WOS:000181615300006
PM 12715049
ER
PT J
AU Bronson, CL
Grubb, TC
Sattler, GD
Braun, MJ
AF Bronson, CL
Grubb, TC
Sattler, GD
Braun, MJ
TI Mate preference: a possible causal mechanism for a moving hybrid zone
SO ANIMAL BEHAVIOUR
LA English
DT Article
ID BLACK-CAPPED CHICKADEES; HIGH-RANKING MALES; WINTER FLOCKS;
PARUS-PALUSTRIS; WILLOW TITS; REPRODUCTIVE SUCCESS; TOWNSENDS WARBLERS;
SEXUAL SELECTION; MARSH TITS; FEMALE
AB The study of patterns and underlying mechanisms within hybrid zones may provide insight into speciation. Black-capped (Poecile atricapillus; BC) and Carolina (P. carolinensis; CA) chickadees hybridize in an east-west band in the U.S.A. from New Jersey to Kansas. Within the past century, the Ohio portion of this hybrid zone and the CA range to the south have been moving northward while the BC range has retracted. We examined mate preference in females of both species as one possible causal mechanism for this shift. To be conservative about the nomenclature and results, the samples are referred to as either 'BC-like' or 'CA-like' due to the observed genetic introgression in the study individuals. Given a choice within an aviary setting, in the aggregate, BC-like and CA-like females that had not observed the direct social interactions between a dyad of a BC-like male and a CA-like male preferred to associate with the BC-like male. In nature, both species form within-sex dominance hierarchies. In the aviary, CA-like males dominated BC-like males unless a CA-like male was substantially smaller. Once females of both types had observed the physical interaction of a particular heterospecific dyad, they associated preferentially with the dominant male, regardless of species type. Thus, the effect of CA male intrasexual dominance on female mate preference may be contributing to the northward movement of the hybrid zone. (C) 2003 Published by Elsevier Science Ltd on behalf of The Association for the Study of Animal Behaviour.
C1 Ohio State Univ, Behav Ecol Grp, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA.
Liberty Univ, Dept Biol & Chem, Lynchburg, VA 24502 USA.
Smithsonian Inst, Dept Systemat Biol, Suitland, MD 20746 USA.
RP Bronson, CL (reprint author), Ohio State Univ, Dept Internal Med, Div Immunol, Heart & Lung Res Inst 425, 473 W 12th Ave, Columbus, OH 43210 USA.
NR 61
TC 43
Z9 44
U1 0
U2 19
PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD
PI LONDON
PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND
SN 0003-3472
J9 ANIM BEHAV
JI Anim. Behav.
PD MAR
PY 2003
VL 65
BP 489
EP 500
DI 10.1006/anbe.2003.2103
PN 3
PG 12
WC Behavioral Sciences; Zoology
SC Behavioral Sciences; Zoology
GA 689HD
UT WOS:000183484800009
ER
PT J
AU Reents-Budet, D
Bishop, R
AF Reents-Budet, D
Bishop, R
TI What can we learn from a Maya vase? (Ceramics, archaeology, chemical
imagery)
SO ARCHAEOLOGY
LA English
DT Article
C1 Smithsonian Inst, Ctr Materials Res, Washington, DC 20560 USA.
RP Reents-Budet, D (reprint author), Smithsonian Inst, Ctr Materials Res, Washington, DC 20560 USA.
NR 0
TC 1
Z9 2
U1 0
U2 6
PU ARCHAEOLOGICAL INST
PI NEW YORK
PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 USA
SN 0003-8113
J9 ARCHAEOLOGY
JI Archaeology
PD MAR-APR
PY 2003
VL 56
IS 2
BP 26
EP 29
PG 4
WC Archaeology
SC Archaeology
GA 727ED
UT WOS:000185643200006
ER
PT J
AU Erwin, DH
AF Erwin, DH
TI Impact at the Permo-Triassic boundary: A critical evaluation
SO ASTROBIOLOGY
LA English
DT Article; Proceedings Paper
CT 10th Rubey Colloquium
CY FEB 08-09, 2002
CL LOS ANGELES, CA
DE Permo-Triassic mass extinction; extraterrestrial impact; flood basalt
volcanism
ID FLOOD-BASALT VOLCANISM; MORY,A.J. ET-AL.; MASS EXTINCTION;
WESTERN-AUSTRALIA; GIGANTIC RELEASE; CARNARVON BASIN; METHANE RELEASE;
BOLIDE IMPACT; SOUTH-CHINA; EVENT
AB The recognition in 1980 of a signature of an extraterrestrial impact at the Cretaceous-Tertiary boundary and its apparent involvement with the mass extinction generated considerable enthusiasm for impacts at other mass extinctions. Numerous claims of impact evidence for the Permo-Triassic mass extinction (251.6 Ma), the largest of the Phanerozoic mass extinctions, have generally been rejected, found wanting, or been difficult to reproduce. Despite this lack of repeatable support, considerable available evidence is consistent with an impact, including the rapidity of extinction, coincident carbon shift, and evident correlation between terrestrial and marine extinctions. However attractive the hypothesis, the coincidence with the Siberian flood basalts and the complex nature of the carbon shift are in conflict with an impact. The most intriguing possibility is that the greatest mass extinction of the Phanerozoic left signals very similar to the end-Cretaceous mass extinction but was produced by entirely Earth-bound processes. If true, this would tell us far more about the nature of ecosystems and how they fail than would identification of another impact.
C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
RP Erwin, DH (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA.
EM erwin.doug@nmnh.si.edu
RI Erwin, Douglas/A-9668-2009
NR 52
TC 12
Z9 15
U1 1
U2 5
PU MARY ANN LIEBERT INC
PI NEW ROCHELLE
PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA
SN 1531-1074
J9 ASTROBIOLOGY
JI Astrobiology
PD SPR
PY 2003
VL 3
IS 1
BP 67
EP 74
DI 10.1089/153110703321632426
PG 8
WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary
SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics;
Geology
GA 676LF
UT WOS:000182753000005
PM 12804365
ER
PT J
AU Bloom, JS
Berger, E
Kulkarni, SR
Djorgovski, SG
Frail, DA
AF Bloom, JS
Berger, E
Kulkarni, SR
Djorgovski, SG
Frail, DA
TI The redshift determination of GRB 990506 and GRB 000418 with the
Echellete Spectrograph Imager on Keck
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE cosmology : miscellaneous; cosmology : observations; gamma rays
ID GAMMA-RAY BURSTS; MICROWAVE BACKGROUND-RADIATION; STARBURST GALAXIES;
HOST GALAXY; EMISSION; AFTERGLOW; UNIVERSE; MAPS
AB Using the Echellete Spectrograph Imager (ESI) on the Keck II 10 m telescope we have measured the redshifts of the host galaxies of gamma-ray bursts GRB 990506 and GRB 000418, z = 1.30658 +/- 0.00004 and 1.1181 +/- 0.0001, respectively. Thanks to the excellent spectral resolution of ESI (lambda/Deltalambda = 13000), we resolved the [O II] lambda727 doublet in both cases. The measured redshift of GRB 990506 is the highest known for a dark-burst GRB, though entirely consistent with the notion that dark and non-dark bursts have a common progenitor origin. The relative strengths of the [O II], He I [Ne III], and Hgamma emission lines suggest that the host of GRB 000418 is a starburst galaxy, rather than a LINER or Seyfert 2. Since the host of GRB 000418 has been detected at submillimeter wavelengths, these spectroscopic observations suggest that the submillimeter emission is due to star formation ( as opposed to AGN) activity. The [O II]-derived unobscured star formation rates are 13 and 55 M(circle dot) yr(-1) for the hosts of GRB 990506 and GRB 000418, respectively. In contrast, the star formation rate of the host of GRB 000418 derived from submillimeter observations is 20 times larger.
C1 CALTECH, Palomar Observ, Pasadena, CA 91125 USA.
Harvard Soc Fellows, Cambridge, MA 02138 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Bloom, JS (reprint author), CALTECH, Palomar Observ, Mail Stop 105-24, Pasadena, CA 91125 USA.
EM jbloom@cfa.harvard.edu
NR 34
TC 42
Z9 43
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 999
EP 1005
DI 10.1086/367805
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700001
ER
PT J
AU Darling, J
Goldsmith, P
Li, D
Giovanelli, R
AF Darling, J
Goldsmith, P
Li, D
Giovanelli, R
TI A search for 6.7 GHz methanol masers in OH megamaser galaxies at 0.11 z
0.27
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies : ISM; galaxies : starburst; ISM : molecules; masers; radio
emission lines
ID MAGELLANIC CLOUDS; REGIONS
AB We report the results of a search for 6.7 GHz methanol (CH3OH) maser emission in OH megamaser galaxies at 0.11 < z < 0.27. No detections were made in the 25 objects observed down to rms noise levels of roughly 0.6 mJy in 150 kHz channels. The OH megamaser sample includes OH emission of all observed types: narrow and broad, physically compact and extended, variable and quiescent, and from simple single lines to multicomponent complexes to lines with high-velocity wings. Our null result indicates that, for the widest possible range of OH megamaser environments, methanol masing does not scale with OH from Galactic masers to megamasers. These observations, however, are not sensitive enough to rule out methanol masing that scales with star formation from Galactic compact H II regions to starbursts associated with major mergers. This and previous work suggest that OH megamasers do not represent large ensembles of individual masers associated with star-forming regions. Maser models combined with observational constraints on the physical settings of OH megamasers indicate that 6.7 GHz methanol megamasers will not be detected by this survey if T-dust < 100 K or if n(CH3OH) &LE; n(OH).
C1 Carnegie Inst Washington Observ, Pasadena, CA 91101 USA.
Cornell Univ, Ithaca, NY 14853 USA.
Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Darling, J (reprint author), Carnegie Inst Washington Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA.
RI Darling, Jeremy/A-7968-2009
OI Darling, Jeremy/0000-0003-2511-2060
NR 21
TC 14
Z9 14
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 1177
EP 1181
DI 10.1086/367804
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700016
ER
PT J
AU Strader, J
Brodie, JP
Forbes, DA
Beasley, MA
Huchra, JP
AF Strader, J
Brodie, JP
Forbes, DA
Beasley, MA
Huchra, JP
TI Spectroscopy of globular clusters in the Fornax dwarf galaxy
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE galaxies : dwarf; galaxies : individual (Fornax); galaxies : star
clusters; Local Group
ID OLD STELLAR POPULATIONS; COLOR-MAGNITUDE DIAGRAMS; SPHEROIDAL GALAXY;
STAR-CLUSTERS; KECK SPECTROSCOPY; AGE INDICATOR; PALOMAR 12;
METALLICITY; PHOTOMETRY; SPECTRA
AB We present low-resolution, integrated Keck spectra of the five globular clusters (GCs) of the Fornax dwarf spheroidal galaxy. We find a tentative age spread among the clusters, with the GC H5 younger by 2-3 Gyr than the others. The clusters generally appear to be very metal-poor ([Fe/H] similar to 1.8), with the cluster H4 slightly more metal-rich at [Fe/H] = 1.5. We speculate that cluster H4 is similar to the Galactic GC Ruprecht 106, which lacks the [alpha/Fe] enhancement typical among metal-poor GCs in the Milky Way. High-resolution spectroscopy of individual cluster and field stars will be needed to sort out the surprisingly complex history of GC formation and evolution in this galaxy.
C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Strader, J (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
EM strader@ucolick.org; brodie@ucolick.org; dforbes@astro.swin.edu.au;
mbeasley@astro.swin.edu.au; huchra@cfa.harvard.edu
NR 48
TC 43
Z9 43
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 1291
EP 1297
DI 10.1086/367599
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700024
ER
PT J
AU Dobrzycki, A
Macri, LM
Stanek, KZ
Groot, PJ
AF Dobrzycki, A
Macri, LM
Stanek, KZ
Groot, PJ
TI Variability-selected quasars behind the Small Magellanic Cloud
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE Magellanic Clouds; quasars : general
ID GRAVITATIONAL LENSING EXPERIMENT; PROPER MOTION; GALAXIES; SAMPLE;
FIELD; QSOS
AB We present follow-up spectroscopic observations of quasar candidates in the Small Magellanic Cloud selected by L. Eyer from the OGLE database. Of 12 observed objects identified as "QSO candidates, "five are confirmed as quasars, with emission redshifts ranging from 0.28 to 2.16. Two of these quasars were also recently identified independently in the MACHO database by Geha et al. We discuss the prospects of using the variability-based selection technique for quasar searches behind other dense stellar fields. An additional criterion utilizing a color-color diagram should reduce the number of stars in the candidate lists.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Kitt Peak Natl Observ, Natl Opt Astron Observ, Tucson, AZ 85726 USA.
Katholieke Univ Nijmegen, Afdeling Sterrenkunde, NL-6500 GL Nijmegen, Netherlands.
RP Dobrzycki, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Groot, Paul/K-4391-2016
OI Groot, Paul/0000-0002-4488-726X
NR 23
TC 22
Z9 22
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 1330
EP 1335
DI 10.1086/346144
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700027
ER
PT J
AU Schlegel, EM
AF Schlegel, EM
TI Upper limits on the X-ray emission of "uranium" stars
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE binaries : general; stars : abundances; stars : general; supernovae :
general; X-rays
ID R-PROCESS NUCLEOSYNTHESIS; METAL-POOR STARS; ALL-SKY SURVEY; SUPERNOVA
EXPLOSIONS; ABUNDANCES; GALAXY; SAMPLE
AB A paper by Qian & Wasserburg suggests the optical absorption lines of uranium observed in the spectra of ultra metal-poor stars (defined as [Fe/H] < -3) arise from contamination from a supernova in a binary star system. Assuming the binary survived the explosion, a collapsed compact object may be present and implies potential accretion processes with accompanying X-ray emission. Upper limits on X-ray emission from an accreting compact object are described here.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Schlegel, EM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 29
TC 2
Z9 2
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 1426
EP 1430
DI 10.1086/367597
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700036
ER
PT J
AU Smith, N
Gehrz, RD
Hinz, PM
Hoffmann, WF
Hora, JL
Mamajek, EE
Meyer, MR
AF Smith, N
Gehrz, RD
Hinz, PM
Hoffmann, WF
Hora, JL
Mamajek, EE
Meyer, MR
TI Mass and kinetic energy of the Homunculus Nebula around eta Carinae
SO ASTRONOMICAL JOURNAL
LA English
DT Article
DE circumstellar matter; ISM : individual (Homunculus Nebula); stars :
individual (eta Carinae)
ID HUBBLE-SPACE-TELESCOPE; TORUS
AB We examine thermal infrared images of eta Car at wavelengths from 4.8 to 25 mum obtained with the MIRAC3 camera system at the Magellan Observatory, and we conclude that eta Car's circumstellar Homunculus Nebula contains much more mass (greater than or similar to 12 M) and kinetic energy (10(49.6)-10(50) ergs) than had previously been recognized. Excess far-infrared emission from a large mass of cold dust had been discovered recently by Morris et al., which they attributed to 110 K dust in a compact equatorial torus. Our images suggest, however, that roughly 10 M or more resides instead in the rapidly expanding polar lobes of the Homunculus, known to be ejected during eta Car's Great Eruption in the 19th century. Combining this large mass with reliable expansion speeds for the polar lobes allows us to estimate the large kinetic energy and efficient momentum transfer associated with the eruption. Most mass resides in a cool outer layer of the lobes, with dust at similar to140 K. This material is only revealed at 18-25 mum with high spatial resolution images that can separate adjacent dust components. Warmer dust at similar to200 K that has been recognized for some time ( responsible for previous mass estimates of 2-3 M-.) blankets the inner surfaces of the mostly hollow polar lobes as they are irradiated more directly by the central engine.
C1 Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA.
Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Smith, N (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, 389 UCB, Boulder, CO 80309 USA.
NR 31
TC 167
Z9 167
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-6256
J9 ASTRON J
JI Astron. J.
PD MAR
PY 2003
VL 125
IS 3
BP 1458
EP 1466
DI 10.1086/346278
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647LR
UT WOS:000181094700041
ER
PT J
AU Mancuso, S
Raymond, JC
Kohl, J
Ko, YK
Uzzo, M
Wu, R
AF Mancuso, S
Raymond, JC
Kohl, J
Ko, YK
Uzzo, M
Wu, R
TI Plasma properties above coronal active regions inferred from SOHO/UVCS
and radio spectrograph observations
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE Sun : corona; Sun : UV radiation; Sun : magnetic fields; Sun : radio
radiation; shock waves
ID SOLAR CORONA; FARADAY-ROTATION; SOHO; SPECTROMETER; BURSTS; SHOCK;
VELOCITIES; UVCS/SOHO; STREAMERS; WAVES
AB Information on coronal plasma was inferred from the joint analysis of type II radio bursts and SOHO UltraViolet Coronagraph Spectrometer (UVCS) observations. The data sample comprises 37 metric type II radio bursts observed by ground-based radio spectrographs in 1999, during the rising phase of the solar cycle. The coronal electron densities n(e) were estimated with the diagnostic provided by UVCS observations of the O VI doublet line intensities. Upper limits to the coronal Alfven speed above active regions were inferred from the derived shock speeds by requiring that the disturbances propagate at least faster than the local characteristic speed. Information on the magnetic field strength B and plasma beta in the middle corona were finally extracted from the coronal Alfven speed upper limits. A major improvement with respect to previous studies that used type II radio bursts to derive plasma properties, is that density profiles of the pre-shock plasma obtained a few hours before the passage of the shock were used instead of general electron density models taken from literature. Our main result is expressed by the inequality B(r) less than or equal to (0.6 +/- 0.3)(r - 1)(-1.2) G, that is valid in the range 1.5 less than or equal to r less than or equal to 2.3 solar radii, and is consistent with previous estimates of the magnetic field above coronal active regions.
C1 Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Mancuso, S (reprint author), Osserv Astron Torino, INAF, Strada Osservatorio 20, I-10025 Pino Torinese, Italy.
NR 30
TC 30
Z9 30
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2003
VL 400
IS 1
BP 347
EP 353
DI 10.1051/0004-6361:20021844
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 648XT
UT WOS:000181177300036
ER
PT J
AU Kramer, C
Richer, J
Mookerjea, B
Alves, J
Lada, C
AF Kramer, C
Richer, J
Mookerjea, B
Alves, J
Lada, C
TI Dust properties of the dark cloud IC5146 - Submillimeter and NIR imaging
SO ASTRONOMY & ASTROPHYSICS
LA English
DT Article
DE ISM : clouds; ISM : dust, extinction; ISM : evolution; ISM : structure;
ISM : individual objects : IC5146
ID MOLECULAR CLOUDS; INTERSTELLAR DUST; STAR-FORMATION; CORES; EXTINCTION;
GAS; TEMPERATURES; OPACITIES; CONTINUUM; EMISSION
AB We present the results of a submillimeter dust continuum study of a molecular ridge in IC 5146 carried out at 850 mum and 450 mum with SCUBA on the James Clerk Maxwell Telescope (JCMT). The mapped region is similar to14'x2'.5 in size (similar to2 pc x 0.3 pc) and consists of at least four dense cores which are likely to be prestellar in nature. To study the dust properties of the ridge and its embedded cores, we combined the dust emission data with dust extinction data obtained by Lada et al. (1999) from the NIR colors of background giant stars. The ridge shows dust extinctions above similar to10 mag, rising up to 35 mag in the cores.
A map of dust temperatures, constructed from the continuum flux ratios, shows significant temperature gradients: we find temperatures of up to similar to20 K in the outskirts and between the cores, and down to similar to10 K in the cores themselves. The cores themselves are almost isothermal, although their average temperatures vary between 10 K and 18 K. We used the extinction data to derive in addition a map of the dust emissivity parametrized by kappa' = kappa(850)/kappa(V). The average value of kappa' agrees well with the canonical value of Mathis (1990). We find that kappa' increases by a factor of similar to4 from similar to1.3x10(-5) to similar to5x10(-5) when the dust temperature decreases from similar to20 K to similar to12 K. A Monte Carlo simulation shows that this change is significant with regard to the estimated calibration uncertainties. This is consistent with models of dust evolution in prestellar cores by Ossenkopf & Henning (1994) which predict that grain coagulation and the formation of ices on grain surfaces in the cold, dense cloud interiors lead to a significant increase of the 850 mum dust opacity. This interpretation is furthermore supported by the previous detection of gas-phase depletion of CO in one of the IC 5146 cores (Kramer et al. 1999). Observations of dust fluxes at short wavelengths are however needed to verify this result.
C1 Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany.
Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England.
European So Observ, D-85748 Garching, Germany.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Kramer, C (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany.
OI Alves, Joao/0000-0002-4355-0921
NR 46
TC 71
Z9 71
U1 0
U2 0
PU E D P SCIENCES
PI LES ULIS CEDEXA
PA 7, AVE DU HOGGAR, PARC D ACTIVITES COURTABOEUF, BP 112, F-91944 LES ULIS
CEDEXA, FRANCE
SN 0004-6361
J9 ASTRON ASTROPHYS
JI Astron. Astrophys.
PD MAR
PY 2003
VL 399
IS 3
BP 1073
EP 1082
DI 10.1051/0004-6361:20021823
PG 10
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QR
UT WOS:000181046200030
ER
PT J
AU Keshet, U
Waxman, E
Loeb, A
Springel, V
Hernquist, L
AF Keshet, U
Waxman, E
Loeb, A
Springel, V
Hernquist, L
TI Gamma rays from intergalactic shocks
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : clusters : general; gamma rays : theory; large-scale
structure of universe; methods : numerical; radiation mechanisms :
nonthermal; shock waves
ID SMOOTHED PARTICLE HYDRODYNAMICS; MAGNETIC-FIELDS; SUPERNOVA-REMNANTS;
COSMIC-RAYS; ORIGIN; GALAXIES; ACCELERATION; EMISSION; SIMULATIONS;
CLUSTERS
AB Structure formation in the intergalactic medium (IGM) produces large-scale, collisionless shock waves, in which electrons can be accelerated to highly relativistic energies. Such electrons can Compton-scatter cosmic microwave background photons up to gamma-ray energies. We study the radiation emitted in this process using a hydrodynamic cosmological simulation of a LambdaCDM universe. The resulting radiation, extending beyond TeV energies, has roughly constant energy flux per decade in photon energy, in agreement with the predictions of Loeb & Waxman. Assuming that a fraction xi(e)=0.05 of the shock thermal energy is transferred to the population of accelerated relativistic electrons, as inferred from collisionless nonrelativistic shocks in the interstellar medium, we find that the energy flux of this radiation, epsilon(2)(dJ/depsilon)similar or equal to50-160 eV cm(-2) s(-1) sr(-1), constitutes similar to10% of the extragalactic gamma-ray background flux. The associated gamma-ray point sources are too faint to account for the similar to60 unidentified EGRET gamma-ray sources, but GLAST should detect and resolve several gamma-ray sources associated with large-scale IGM structures for xi(e)similar or equal to0.03 and many more sources for larger xi(e). The intergalactic origin of the shock-induced radiation can be verified through a cross-correlation with, e. g., the galaxy distribution that traces the same structure. Its shock origin may be tested by cross-correlating its properties with radio synchrotron radiation, emitted as the same accelerated electrons gyrate in postshock magnetic fields. We predict that GLAST and Cerenkov telescopes such as MAGIC, VERITAS, and HESS should resolve gamma-rays from nearby (redshifts zless than or similar to0.01) rich galaxy clusters, perhaps in the form of a similar to5-10 Mpc diameter ringlike emission tracing the cluster accretion shock, with luminous peaks where the ring intersects galaxy laments detectable even at zsimilar or equal to0.025.
C1 Weizmann Inst Sci, Dept Condensed Matter Phys, IL-76100 Rehovot, Israel.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Astrophys, D-85740 Garching, Germany.
RP Keshet, U (reprint author), Weizmann Inst Sci, Dept Condensed Matter Phys, IL-76100 Rehovot, Israel.
RI WAXMAN, ELI/K-1557-2012
NR 70
TC 107
Z9 107
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP 128
EP 150
DI 10.1086/345946
PN 1
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QV
UT WOS:000181046500012
ER
PT J
AU Kochanek, CS
White, M
Huchra, J
Macri, L
Jarrett, TH
Schneider, SE
Mader, J
AF Kochanek, CS
White, M
Huchra, J
Macri, L
Jarrett, TH
Schneider, SE
Mader, J
TI Clusters of galaxies in the local universe
SO ASTROPHYSICAL JOURNAL
LA English
DT Review
DE cosmology : theory; galaxies : clusters : general; large-scale structure
of universe
ID ALL-SKY SURVEY; MASS-TEMPERATURE RELATION; X-RAY-PROPERTIES;
FLUX-LIMITED SAMPLE; MEDIUM-SENSITIVITY SURVEY; LUMINOSITY FUNCTION;
NEARBY CLUSTERS; REDSHIFT SURVEY; T RELATION; HIERARCHICAL UNIVERSE
AB We use a matched filter algorithm to find and study clusters in both N-body simulations artificially populated with galaxies and the Two Micron All Sky Survey (2MASS). In addition to numerous checks of the matched filter algorithm, we present results on the halo multiplicity function and the cluster number function. For a subset of our identified clusters we have information on X-ray temperatures and luminosities that we cross-correlate with optical richness and galaxy velocity dispersions. With all quantities normalized by the spherical radius corresponding to a mass overdensity of Delta(M)=200 or the equivalent galaxy number over-density of Delta(N)=200Omega(M)(-1) similar or equal to 666, we find that the number of L>L(*) galaxies in a cluster of mass M(200) is log N(*666)=(1.44+/-0.17)+(1.10+/-0.09)log(M(200)h/10(15) M(circle dot)), where the uncertainties are dominated by the scatter created by three choices for relating the observed quantities to the cluster mass. The region inside the virial radius has a K-band cluster mass-to-light ratio of (M/L)(K)=(116+/-46)h, which is essentially independent of cluster mass. Integrating over all clusters more massive than M(200)=10(14) h(-1) M(circle dot), the virialized regions of clusters contain similar or equal to7% of the local stellar luminosity, quite comparable to the mass fraction in such objects in currently popular LambdaCDM models.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA.
CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA.
Univ Massachusetts, Dept Phys & Astron, Lederle Grad Res Ctr 640, Amherst, MA 01003 USA.
Univ Texas, McDonald Observ, Austin, TX 78712 USA.
RP Kochanek, CS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM ckochanek@cfa.harvard.edu; mwhite@astron.berkeley.edu;
jhuchra@cfa.harvard.edu; lmacri@cfa.harvard.edu;
jarrett@ipac.caltech.edu; schneider@messier.astro.edu;
jmader@astro.as.utexas.edu
RI White, Martin/I-3880-2015;
OI White, Martin/0000-0001-9912-5070; Macri, Lucas/0000-0002-1775-4859
NR 120
TC 80
Z9 80
U1 0
U2 2
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP 161
EP 181
DI 10.1086/345896
PN 1
PG 21
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QV
UT WOS:000181046500014
ER
PT J
AU Kong, AKH
DiStefano, R
Garcia, MR
Greiner, J
AF Kong, AKH
DiStefano, R
Garcia, MR
Greiner, J
TI Chandra studies of the X-ray point source luminosity functions of M31
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE galaxies : individual (M31); X-rays : binaries; X-rays : galaxies
ID SUPERNOVA REMNANT CANDIDATES; HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTERS;
ANDROMEDA GALAXY; M-31
AB Three different M31 disk fields, spanning a range of stellar populations, were observed by Chandra. We report the X-ray point source luminosity function (LF) of each region, and the LF of M31's globular clusters, and compare these with each other and with the LF of the galaxy's bulge. To interpret the results we also consider tracers of the stellar population, such as OB associations and supernova remnants. We find differences in the LFs among the fields, but cannot definitively relate them to the stellar content of the fields. We find that stellar population information, average and maximum source luminosities, X-ray source densities, and slopes of the LF are useful in combination.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Tufts Univ, Dept Phys & Astron, Medford, MA 02155 USA.
Max Planck Inst Extraterr Phys, D-85740 Garching, Germany.
RP Kong, AKH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 37
TC 38
Z9 38
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP 298
EP 304
DI 10.1086/345947
PN 1
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QV
UT WOS:000181046500025
ER
PT J
AU Hartmann, L
AF Hartmann, L
TI Comments on inferences of star formation histories and birth lines
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE stars : formation; stars : pre-main sequence
ID T-TAURI STARS; MAIN-SEQUENCE STARS; ORION NEBULA CLUSTER; LOW-MASS
STARS; MOLECULAR CLOUDS; X-RAY; DISK ACCRETION; MAGNETOHYDRODYNAMIC
TURBULENCE; STELLAR BIRTHLINE; LITHIUM
AB Palla & Stahler have recently argued that star formation in Taurus and other nearby molecular clouds extends over a period of at least 10 Myr, implying quasi-static cloud evolution and star formation. Their conclusions contradict other recent results indicating that molecular clouds are transient objects and star formation proceeds rapidly. The Palla & Stahler picture implies that most molecular clouds should have extremely low rates of star formation and that in such inactive stages, the stellar initial mass function (IMF) should be strongly skewed toward producing stars with masses greater than or similar to 1 M.; neither prediction is supported by observations. I show that the Palla & Stahler conclusions for Taurus depend almost entirely on a small number of stars with masses greater than or similar to 1 M.; the lower mass stars show no evidence for such an extended period of star formation. I further show that most of the stars apparently older than 10 Myr in the direction of Taurus are probably foreground nonmembers. I also present birth line calculations that support the idea that the ages of the stars with masses greater than or similar to 1 M. have been systematically overestimated because birth line age corrections have been underestimated; such birth lines would eliminate the need to postulate skewed IMFs. The simplest and most robust explanation of current observations characterizing the vast majority of young stars in molecular clouds is that cloud and star formation is rapid and dynamic.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Hartmann, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 65
TC 124
Z9 124
U1 1
U2 2
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP 398
EP 405
DI 10.1086/345933
PN 1
PG 8
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QV
UT WOS:000181046500033
ER
PT J
AU Meakin, CA
Bieging, JH
Latter, WB
Hora, JL
Tielens, AGGM
AF Meakin, CA
Bieging, JH
Latter, WB
Hora, JL
Tielens, AGGM
TI Hubble Space Telescope/NICMOS near-infrared imaging of the proto
planetary nebula OH 231.8+4.2
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE circumstellar matter; infrared : stars; planetary nebulae : individual
(OH 231.8+4.2); stars : AGB and post-AGB
ID MODEL SCATTERING ENVELOPES; LONG-SLIT SPECTROSCOPY; YOUNG STELLAR
OBJECTS; OH 231.8+4.2; MOLECULAR OUTFLOW; BIPOLAR OUTFLOW; OH/IR STARS;
JETS; OH231.8+4.2; EMISSION
AB We present observations of the bipolar nebula OH 231.8+4.2, made with the Hubble Space Telescope (HST) NICMOS camera, in three wide filter bands (F205W, F160W, and F110W). The images have excellent dynamic range after removal of low-level instrumental artifacts. In the F205W filter (lambda approximate to 2.04 mum), we achieve a peak/rms of greater than 8000 with an angular resolution of 0."20 (FWHM). The combination of high dynamic range and angular resolution confirms previous observations but also reveals new features in the near-IR morphology of the nebula, which at these wavelengths is dominated by scattered light. The northern (approaching) lobe shows well-defined, limb-brightened edges. The central jet splits into two laments and exhibits some curvature between the center of the nebula and the end of the northern lobe. The southern (receding) lobe has a diffuse, occulent appearance without a sharply defined central jet, in contrast to the northern lobe. A sharpened version of the F205W image shows indications of turbulent structures both in the northern lobe and jet and in the southern lobe. A faint cylindrical halo of scattered light shows a sharp increase in surface brightness inside a radius of similar to4" from the center, possibly resulting from a transition from a spherical wind to a disk- or torus-like mass ejection, on the same timescale as the formation of the collimated fast wind seen in CO and HCO(+) images. We calculate the extinction through the nebula from the measured near-IR colors and a silicate grain model. For a simple geometric model of a dense central disk, we estimate a disk mass (gas and dust) in the range 0.03-0.06 M., relatively insensitive to grain size. The circumstance of an asymptotic giant branch (AGB) star with a massive, highly collimated, high-velocity bipolar flow may be understood in terms of the model of Soker & Rappaport if the central star underwent a change in mass-loss properties from a (roughly) spherical AGB wind to equatorially enhanced mass loss beginning similar to(1-3) X 10(3) yr ago. Supposing the presence of a dwarf companion in a suitable orbit, the bipolar nebula then is a consequence of a strong increase in mass loss as the central star evolves close to the tip of the AGB and will soon evolve to higher T(eff) and appear as a more typical proto planetary nebula.
C1 Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
CALTECH, SIRTF Sci Ctr, Pasadena, CA 91125 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Groningen, Kapteyn Astron Inst, NL-9700 Groningen, Netherlands.
RP Meakin, CA (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
EM cmeakin@as.arizona.edu; jbieging@as.arizona.edu
OI Hora, Joseph/0000-0002-5599-4650
NR 42
TC 14
Z9 14
U1 0
U2 1
PU IOP PUBLISHING LTD
PI BRISTOL
PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP 482
EP 493
DI 10.1086/345951
PN 1
PG 12
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QV
UT WOS:000181046500041
ER
PT J
AU Kharchenko, V
Rigazio, M
Dalgarno, A
Krasnopolsky, VA
AF Kharchenko, V
Rigazio, M
Dalgarno, A
Krasnopolsky, VA
TI Charge abundances of the solar wind ions inferred from cometary X-ray
spectra
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE atomic processes; comets : general; X-rays : general
ID EXTREME-ULTRAVIOLET EMISSION; HALE-BOPP; C/1995 O1; EXCHANGE; HYAKUTAKE;
NEUTRALS; SEARCH; EUVE
AB An emission spectrum of X-rays from comet McNaught-Hartley (C/1999 T1) detected with the Chandra X-ray telescope is analyzed on the assumption that it results from electron captures by heavy ions of the solar wind colliding with the atoms and molecules of the cometary atmosphere. An accurate value of the relative abundance of O+8 and O+7 ions is obtained by comparing the spectrum derived from the measurement data with the predicted spectrum. A close match is found for an abundance ratio of O+8 to O+7 of 0.34 +/- 0.07, the uncertainty reflecting the measurement statistics. A similar analysis of the contribution from captures by Ne+9 ions leads to an abundance ratio of Ne+9 to O+7 of 0.02 with an uncertainty of 40%. The spectrum consists of many unresolved lines. The brightest feature is composed mostly of the 2 S-3(1) --> 1 S-1(0) spin-forbidden line of O+6 at 561 eV with 74% of the intensity and the 2 P-3(1) --> 1 S-1(0) intercombination line at 568 eV with 12%. The strongest of the O+7 lines is the Lyalpha transition at 654 eV with an intensity of 29%, relative to the O+6 lines. The sensitivity of cometary X-ray spectra to variations in the abundances of highly charged oxygen ions in the solar wind is investigated.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA.
RP Kharchenko, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Krasnopolsky, Vladimir/L-5085-2013
NR 29
TC 75
Z9 75
U1 0
U2 5
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP L73
EP L75
DI 10.1086/374209
PN 2
PG 3
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QW
UT WOS:000181046600018
ER
PT J
AU Miller, JM
Fabbiano, G
Miller, MC
Fabian, AC
AF Miller, JM
Fabbiano, G
Miller, MC
Fabian, AC
TI X-ray spectroscopic evidence for intermediate-mass black holes: Cool
accretion disks in two ultraluminous X-ray sources
SO ASTROPHYSICAL JOURNAL
LA English
DT Article
DE black hole physics; X-rays : stars
ID SPIRAL GALAXIES; CANDIDATES; EMISSION
AB We have analyzed an XMM-Newton observation of the nearby spiral galaxy NGC 1313, which contains two "ultraluminous" X-ray (ULX) sources. We measure isotropic luminosities of L-x = 2.0 X 10(40) ergs s(-1) and 40 L-x = 6.6 X 10(39) ergs s(-1) for NGC 1313 X-1 and X-2 (0.2-10.0 keV, assuming a distance of 3.7 Mpc). The spectra statistically require soft and hard spectral components to describe the continuum emission; some prior studies of ULX sources have claimed cool soft components with lower statistics. The improvement over several single-component models exceeds the 8 sigma level of confidence for X-1; the improvement for X-2 is significant at the 3 sigma level. The soft components in these ULX spectra are well fitted by multicolor disk blackbody models with color temperatures of kT similar or equal to eV. This temperature differs markedly from those commonly measured in the spectra of stellar mass (10 M.) black holes in their brightest states (kT similar or equal to 1 keV). It is expected that the temperature of an accretion disk orbiting a black hole should decrease with increasing black hole mass. If the soft components we measure are due to emission from the inner region of an accretion disk, and disks extend close to the innermost stable circular orbit at the accretion rates being probed, the low color temperatures may be interpreted as spectroscopic evidence of black holes with intermediate masses: M-BH similar or equal to 10(3) M.. Simple Eddington scaling arguments suggest a minimum mass of M-BH similar to 10(2) M.. NGC 1313 X-1 and X-2 are found in optical nebulae, which may indicate that anisotropic emission geometries are unlikely to account for the fluxes observed.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Maryland, Dept Astron, College Pk, MD 20742 USA.
Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England.
RP Miller, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 26
TC 185
Z9 186
U1 0
U2 3
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0004-637X
J9 ASTROPHYS J
JI Astrophys. J.
PD MAR 1
PY 2003
VL 585
IS 1
BP L37
EP L40
DI 10.1086/368373
PN 2
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 646QW
UT WOS:000181046600010
ER
PT J
AU Winn, JN
Patnaik, AR
Wrobel, JM
AF Winn, JN
Patnaik, AR
Wrobel, JM
TI Interferometric phase calibration sources in the declination range 0
degrees to-30 degrees
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE astrometry; catalogs; radio continuum : general; techniques :
interferometric
ID NRAO PMN SURVEYS; SOURCE CATALOG; RADIO-SOURCES
AB We present a catalog of 321 compact radio sources in the declination range 0degrees > delta > -30degrees. The positions of these sources have been measured with a two-dimensional rms accuracy of 35 milliarcseconds using the NRAO(6) Very Large Array. Each source has a peak flux density > 50 mJy at 8.4 GHz. We intend for this catalog to be used mainly for selection of phase calibration sources for radio interferometers, although compact radio sources have other scientific uses.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Max Planck Inst Radioastron, D-53121 Bonn, Germany.
Natl Radio Astron Observ, Socorro, NM 87801 USA.
RP Winn, JN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
NR 26
TC 2
Z9 2
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2003
VL 145
IS 1
BP 83
EP 87
DI 10.1086/345541
PG 5
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 648KX
UT WOS:000181151500005
ER
PT J
AU Sanz-Forcada, J
Brickhouse, NS
Dupree, AK
AF Sanz-Forcada, J
Brickhouse, NS
Dupree, AK
TI The structure of stellar coronae in active binary systems
SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
LA English
DT Article
DE stars : coronae; stars : flare; ultraviolet : stars; X-rays : stars
ID EXTREME-ULTRAVIOLET-EXPLORER; CANUM-VENATICORUM BINARIES; LATE-TYPE
STARS; TRANSITION-REGION STRUCTURE; XI-URSAE-MAJORIS; ALPHA-CENTAURI;
AR-LACERTAE; RS CVN; INTERSTELLAR-MEDIUM; RADIAL-VELOCITIES
AB A survey of 28 stars (22 active binary systems, plus six single stars or wide binaries for comparison) using extreme ultraviolet spectra has been conducted to establish the structure of stellar coronae in active binary systems from the emission measure distribution (EMD), electron densities, and scale sizes. Observations obtained by the Extreme Ultraviolet Explorer satellite (EUVE) during 9 years of operation are included for the stars in the sample. EUVE data allow a continuous EMD to be constructed in the range log T-e(K) similar to 5.6-7.4, using iron emission lines. These data are complemented with IUE observations to model the lower temperature range [log T-e(K) similar to 4.0-5.6]. Inspection of the EMD shows an outstanding narrow enhancement, or "bump" peaking around log T-e(K) similar to 6.9 in 25 of the stars, de ning a fundamental coronal structure. The emission measure per unit stellar area decreases with increasing orbital (or photometric) periods of the target stars; stars in binaries generally have more material at coronal temperatures than slowly rotating single stars. High electron densities (N(e)greater than or similar to10(12) cm(-3)) are derived at similar to log T-e(K) similar to 7.0 for some targets, implying small emitting volumes.
The observations suggest the magnetic stellar coronae of these stars are consistent with two basic classes of magnetic loops: solar-like loops with maximum temperature around log T-e(K) similar to 6.3 and lower electron densities (N(e)greater than or similar to10(9)-10(10.5) cm(-3)), and hotter loops peaking around log T-e(K) similar to 6.9 with higher electron densities (N(e)greater than or similar to10(12) cm(-3)). For the most active stars, material exists at much higher temperatures [log T-e(K) greater than or equal to 6.9] as well. However, current ab initio stellar loop models cannot reproduce such a configuration. Analysis of the light curves of these systems reveals signatures of rotation of coronal material, as well as apparent seasonal (i.e., year-to-year) changes in the activity levels.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy.
RP Sanz-Forcada, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
RI Sanz-Forcada, Jorge/C-3176-2017;
OI Sanz-Forcada, Jorge/0000-0002-1600-7835; Brickhouse,
Nancy/0000-0002-8704-4473
NR 84
TC 71
Z9 71
U1 0
U2 1
PU UNIV CHICAGO PRESS
PI CHICAGO
PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA
SN 0067-0049
J9 ASTROPHYS J SUPPL S
JI Astrophys. J. Suppl. Ser.
PD MAR
PY 2003
VL 145
IS 1
BP 147
EP 179
PG 33
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 648KX
UT WOS:000181151500008
ER
PT J
AU Lasso, E
Naranjo, ME
AF Lasso, E
Naranjo, ME
TI Effect of pollinators and nectar robbers on nectar production and pollen
deposition in Hamelia patens (Rubiaceae)
SO BIOTROPICA
LA English
DT Article
DE Costa Rica; Hamelia patens; hummingbirds; La Selva; nectarivorous guild;
nectar robbery; pollen deposition; tropical rain forest
ID ROBBING BUMBLE BEES; SEED SET; ECOLOGICAL INTERACTIONS;
IPOMOPSIS-AGGREGATA; PLANT FITNESS; HUMMINGBIRDS; INTENSITY; VISITORS;
REPRODUCTION; AVAILABILITY
AB We conducted experimental manipulations and field observations to determine the role of members of a nectarivorous guild (pollinators and robbers) on nectar production and pollen deposition in Hamelia patens at the La Selva Biological Station (Costa Rica). Seven pollinators (hummingbirds) and four robbers (I hummingbird and 3 perching birds) comprised the avian nectarivorous guild visiting H. patens during March 1997. In addition, two florivorous birds were observed visiting H. patens during the study. Pollinators accounted for 85.6 percent of the visits, robbers for 12.4 percent, and florivores for 2 percent of the visits. Visitation by pollinators and robbers was greatest when floral nectar was highest. No aggressive interactions between pollinators and robbers were observed during the study. Pollinators differed in their ability to carry and deposit pollen on the stigma. Territorial hummingbirds were the least effective pollinators but the most frequent visitors. Flowers were frequently robbed (71%) during the study. Flowers experimentally robbed did not increase nectar production compared to control flowers; therefore, robbery may not involve an extra energy investment in terms of nectar production. The number of pollen grains deposited on artificially robbed flowers was significantly less than the number found in flowers with extra nectar (nectar added) but did not differ from the number found in non-manipulated flowers, indicating that nectar robbers may not affect the foraging behavior of hummingbirds, and therefore pollen deposition.
C1 Smithsonian Trop Res Inst, Ancon, Panama.
Univ Los Andes Hechicera, Fac Ciencias, Dept Biol, Merida, Venezuela.
RP Lasso, E (reprint author), Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 Goodwin Ave, Urbana, IL 61801 USA.
OI Lasso, Eloisa/0000-0003-4586-8674
NR 44
TC 21
Z9 23
U1 5
U2 29
PU ASSOC TROPICAL BIOLOGY INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0006-3606
J9 BIOTROPICA
JI Biotropica
PD MAR
PY 2003
VL 35
IS 1
BP 57
EP 66
PG 10
WC Ecology
SC Environmental Sciences & Ecology
GA 672PY
UT WOS:000182530700007
ER
PT J
AU Hines, AH
Jivoff, PR
Bushmann, PJ
van Montfrans, J
Reed, SA
Wolcott, DL
Wolcott, TG
AF Hines, AH
Jivoff, PR
Bushmann, PJ
van Montfrans, J
Reed, SA
Wolcott, DL
Wolcott, TG
TI Evidence for sperm limitation in the blue crab, Callinectes sapidus
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article; Proceedings Paper
CT Blue Crab Conference
CY MAR, 2000
CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NC
HO UNIV NORTH CAROLINA WILMINGTON
ID CHIONOECETES-OPILIO BRACHYURA; OF-SAINT-LAWRENCE; SNOW CRAB;
REPRODUCTIVE PRODUCTS; HOMARUS-AMERICANUS; SEXUAL COMPETITION;
CHESAPEAKE BAY; EGG-PRODUCTION; FEMALE CHOICE; SEMINAL FLUID
AB Reproductive success of female blue crabs may be limited by the amount of sperm received during the female's single, lifetime mating. Sperm must be stored in seminal receptacles until eggs are produced and fertilized months to years after mating. Further, intense fishing pressure impacts male abundance, male size and population sex ratio, which affect ejaculate quantity. We measured temporal variation in seminal receptacle contents in relation to brood production for two stocks differing in both fishing pressure on males and latitudinal effects on reproductive season: Chesapeake Bay, Maryland and Virginia, experienced intensive fishing and relatively short reproductive season; and the Indian River Lagoon, Florida, experienced lower exploitation and longer reproductive season. Nearly all (>98%) females were mated, and mating prevalence did not vary among sites during 1996. Seminal receptacle weight declined markedly for 2 mo following mating as seminal fluid disappeared to leave only spermatophores for long-term storage, which suggests that seminal fluid serves as a short-term sperm plug. Seminal receptacle weight in upper Chesapeake Bay declined by 31 % from 1992-1999, indicating that females received smaller ejaculates. In 1996, seminal receptacle contents were highest (3.75 g wet wt, 2.3 x 10(3) mug DNA, 1.2 x 10(9) sperm) in Florida, but were significantly lower by: 25% for weight and 50% for sperm number at the upper Chesapeake Bay site; and 30% for weight and 65% for sperm number at lower Chesapeake Bay sites. Generally, females receive 2-3 x 10(3) spermatophores and 10(8)-10(9) sperm cells for a full ejaculate, whereas females produce ca. 3 x 10(6) eggs per brood. Chesapeake Bay females appear to live about 3.5 yr, producing 1-3 broods (up to 9 x 10(6) eggs) per year and up to 6-7 broods (2.1 x 10(7) eggs) per lifetime. In contrast, Florida crabs produced up to 6-7 broods (2.1 X 101 eggs) per year. and up to 18 broods (5.4 x 10(7) eggs) per lifetime. In Florida, last broods produced by lab-held females were often infertile, indicating that females became sperm limited at the end of their lifetime. Experiments showed that male mating history affected female reproductive success, with females mated late in a sequence having only one third the brood hatching success of females mated early in the sequence. Sperm : egg ratios were estimated at 100: 1 to 400:1 for the first brood but only about 20:1 or 30:1 for maximum lifetime broods over 2 seasons, suggesting that about 67 x 10(6) sperm are used per brood of 3 x 10(6) eggs. A model of brood production and sperm depletion in blue crabs indicates that sperm limitation may be common in Florida as females age, and in Chesapeake Bay as a result of fishery-induced reductions in initial quantities of sperm transferred at mating.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
Smithsonian Marine Stn, Ft Pierce, FL 34949 USA.
N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA.
RP Hines, AH (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
EM hines@serc.si.edu
NR 83
TC 62
Z9 66
U1 0
U2 10
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
EI 1553-6955
J9 B MAR SCI
JI Bull. Mar. Sci.
PD MAR
PY 2003
VL 72
IS 2
BP 287
EP 310
PG 24
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 732CV
UT WOS:000185924000004
ER
PT J
AU Hines, AH
AF Hines, AH
TI Ecology of juvenile and adult blue crabs: Summary of discussion of
research themes and directions
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article; Proceedings Paper
CT Blue Crab Conference
CY MAR, 2000
CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NORTH CAROLINA
HO UNIV NORTH CAROLINA WILMINGTON
ID CALLINECTES-SAPIDUS RATHBUN; CENTRAL CHESAPEAKE BAY; HABITAT
FRAGMENTATION; POPULATION-DYNAMICS; DECAPOD CRUSTACEANS; TEMPORAL
VARIATION; SHALLOW-WATER; NURSERY ROLE; ABUNDANCE; RECRUITMENT
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Hines, AH (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA.
NR 60
TC 9
Z9 9
U1 1
U2 5
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD MAR
PY 2003
VL 72
IS 2
BP 423
EP 433
PG 11
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 732CV
UT WOS:000185924000013
ER
PT J
AU Lipcius, RN
Stockhausen, WT
Seitz, RD
Geer, PJ
AF Lipcius, RN
Stockhausen, WT
Seitz, RD
Geer, PJ
TI Spatial dynamics and value of a marine protected area and corridor for
the blue crab spawning stock in Chesapeake Bay
SO BULLETIN OF MARINE SCIENCE
LA English
DT Article; Proceedings Paper
CT Blue Crab Conference
CY MAR, 2000
CL UNIV NORTH CAROLINA WILMINGTON, WILMINGTON, NC
HO UNIV NORTH CAROLINA WILMINGTON
ID CALLINECTES-SAPIDUS; CONSERVATION; MODEL
AB In lower Chesapeake Bay, a 172,235 ha marine protected area and corridor (MPAC) was recently established to protect blue crab adult females either en route to or at the spawning grounds during the reproductive period. The MPAC was justified due to a recent substantial decline in spawning stock biomass. It was situated in waters deeper than 10 in throughout the lower bay due to the high abundances of adult females in this zone, and it was an expansion of a historical spawning sanctuary near the bay mouth to include northward extensions (upper and lower MPACs). We examined spatial dynamics of the blue crab spawning stock in relation to the MPAC through analyses of trawl Survey data (abundances of adult females and egg-bearing females from 1989-1997 and 1995-1997, respectively) partitioned by water depth, time (month and year), and spatial zone (upper MPAC, lower MPAC, MPAC Historical Sanctuary) during the reproductive period (June-September). Adult female abundance peaked at 6-14 m water depths. Consequently, nearly half of all adult females in the lower bay were deeper than 10 in, and therefore protected by the MPAC during the reproductive period, whereas the historical sanctuary protected about 1/3 that of the MPAC. All MPAC segments were utilized by adult females at different times of the spawning season, without consistent use of any particular segment. In contrast, abundance patterns of egg-bearing females were consistent and did not differ by developmental stage of the eggs. Peak abundances of egg-bearing females shifted from the northern to southern portions of the MPAC as the spawning season progressed. Differences in distribution of adult females and egg-bearing females demonstrated the importance of the expanded MPAC to the conservation of the spawning stock, which requires an extensive area to cover seasonal and yearly alterations in distribution. The expanded MPAC is much more effective than the historical sanctuary at protecting a consistent fraction of the blue crab spawning stock over the full spawning season and every year. Both the lower MPAC and historical sanctuary contained high abundances of adult females and egg-bearing females, and these segments therefore potentially function as corridors and spawning grounds. In contrast, whereas adult females were equally abundant in all MPAC segments, egg-bearing females were rarely common in the upper MPAC segment. Hence, the upper MPAC serves primarily as a corridor for females migrating to spawn or hatch their egg masses in the lower MPAC and historical sanctuary. The MPAC protects a major fraction of the spawning stock and spawning grounds both seasonally and yearly, and it encompasses a dispersal corridor for adult females in the deeper waters of Chesapeake Bay. The MPAC therefore serves as a foundation for long-term protection of the blue crab spawning stock, and should be utilized concurrently with complementary management measures to conserve the blue crab population in Chesapeake Bay. Furthermore, the MPAC for the blue crab in Chesapeake Bay may serve as a model system for investigating the value of marine protected areas for exploited marine populations with ontogenetically disjunct stages in the life cycle that encompass diverse habitats.
C1 Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA.
Smithsonian Environm Res Ctr, Smithsonian Inst, Edgewater, MD 21037 USA.
RP Lipcius, RN (reprint author), Coll William & Mary, Sch Marine Sci, Virginia Inst Marine Sci, POB 1346, Gloucester Point, VA 23062 USA.
EM rom@vims.edu
NR 26
TC 25
Z9 25
U1 0
U2 11
PU ROSENSTIEL SCH MAR ATMOS SCI
PI MIAMI
PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA
SN 0007-4977
J9 B MAR SCI
JI Bull. Mar. Sci.
PD MAR
PY 2003
VL 72
IS 2
BP 453
EP 469
PG 17
WC Marine & Freshwater Biology; Oceanography
SC Marine & Freshwater Biology; Oceanography
GA 732CV
UT WOS:000185924000015
ER
PT J
AU Touwaide, A
AF Touwaide, A
TI Hellenism and hippocratism in Mediterranean Europe: On D. Coray
SO BULLETIN OF THE HISTORY OF MEDICINE
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Touwaide, A (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4363 USA
SN 0007-5140
J9 B HIST MED
JI Bull. Hist. Med.
PD SPR
PY 2003
VL 77
IS 1
BP 195
EP 196
DI 10.1353/bhm.2003.0042
PG 2
WC Health Care Sciences & Services; History & Philosophy Of Science
SC Health Care Sciences & Services; History & Philosophy of Science
GA 655CB
UT WOS:000181532800024
ER
PT J
AU Lagarde, F
Bonnet, X
Henen, B
Legrand, A
Corbin, J
Nagy, K
Naulleau, G
AF Lagarde, F
Bonnet, X
Henen, B
Legrand, A
Corbin, J
Nagy, K
Naulleau, G
TI Sex divergence in space utilisation in the steppe tortoise (Testudo
horsfieldi)
SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE
LA English
DT Article
ID GMELIN REPTILIA-TESTUDINIDAE; HOME-RANGE; MULTIPLE PATERNITY; SPERM
STORAGE; POPULATION; MOVEMENT; TURTLES; ENVIRONMENT; DIMORPHISM;
SELECTION
AB In animal species without parental care, the fitness of males should increase with the number of females encountered, court, and fertilise, and the fitness of females depends strongly on the quantity and quality of resources acquired. This should translate into a marked sex differences in the patterns of space utilisation. We analysed the sex divergences in home range and movements pattern in the steppe tortoise (Testudo horsfieldi) in Uzbekistan. From the radio-tracking data of 36 individuals throughout the active season, the home range of the male steppe tortoise was estimated to be smaller than that of the female (24 vs. 57 ha), even when the analysis focused on the mating season only. During the mating season, males intensively patrolled a small area, going back and forth within their territory, thereby covering greater distances than females. The females movements were more unidirectional, resulting in large loops over a very extended home range. We proposed several nonexclusive hypothesis for such a pattern.
C1 CNRS, Ctr Etude Biol Chize, F-79360 Villiers En Bois, France.
Smithsonian Inst, Natl Zool Pk, Dept Zool Res, Washington, DC 20008 USA.
Univ Calif Los Angeles, Dept Biol, Los Angeles, CA 90095 USA.
RP Lagarde, F (reprint author), CNRS, Ctr Etude Biol Chize, F-79360 Villiers En Bois, France.
RI Henen, Brian/S-6552-2016
OI Henen, Brian/0000-0003-3412-4944
NR 59
TC 21
Z9 21
U1 0
U2 12
PU NATL RESEARCH COUNCIL CANADA
PI OTTAWA
PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA, ONTARIO K1A 0R6, CANADA
SN 0008-4301
J9 CAN J ZOOL
JI Can. J. Zool.-Rev. Can. Zool.
PD MAR
PY 2003
VL 81
IS 3
BP 380
EP 387
DI 10.1139/Z03-023
PG 8
WC Zoology
SC Zoology
GA 677BV
UT WOS:000182787800004
ER
PT J
AU Cavender-Bares, J
Wilczek, A
AF Cavender-Bares, J
Wilczek, A
TI Integrating micro- and macroevolutionary processes in community ecology
SO ECOLOGY
LA English
DT Editorial Material
ID PHENOTYPIC PLASTICITY; EVOLUTION; PHYLOGENY; DIVERSITY; PLANTS;
SPECIALIZATION; ADAPTATIONS; SPECIATION; BEETLES; FOREST
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
Harvard Univ, Dept Organism & Evolut Biol, Cambridge, MA 02138 USA.
RP Cavender-Bares, J (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA.
EM cavenderj@si.edu
RI Cavender-Bares, Jeannine/K-5716-2013
NR 39
TC 39
Z9 40
U1 0
U2 17
PU ECOLOGICAL SOC AMER
PI WASHINGTON
PA 1707 H ST NW, STE 400, WASHINGTON, DC 20006-3915 USA
SN 0012-9658
J9 ECOLOGY
JI Ecology
PD MAR
PY 2003
VL 84
IS 3
BP 592
EP 597
DI 10.1890/0012-9658(2003)084[0592:IMAMPI]2.0.CO;2
PG 6
WC Ecology
SC Environmental Sciences & Ecology
GA 656VF
UT WOS:000181629500010
ER
PT J
AU Sims, HJ
McConway, KJ
AF Sims, HJ
McConway, KJ
TI Nonstochastic variation of species-level diversification rates within
angiosperms
SO EVOLUTION
LA English
DT Review
DE angiosperms; diversity; evolutionary rates; likelihood; taxon pairs
ID FLOWERING PLANTS; STRATIGRAPHIC RANGES; CONFIDENCE-INTERVALS;
PHYLOGENETIC TREES; CENTRAL GEORGIA; FOSSIL FLOWERS; NUCLEOTIDE
SUBSTITUTION; MOLECULAR PHYLOGENIES; ORGANISMAL DIVERSITY; EVOLUTIONARY
PROCESS
AB Variations in the origination and extinction rates of species over geological time often are linked with a range of factors, including the evolution of key innovations, changes in ecosystem structure, and environmental factors such as shifts in climate and physical geography. Before hypothesizing causality of a single factor, it is critical to demonstrate that the observed variation in diversification is significantly greater than one would expect due to natural stochasticity in the evolutionary branching process. Here, we use a likelihood-ratio test to compare taxonomic rate heterogeneity to a neutral birth-death model, using data on well-supported sister pairs of taxa and their species richness. We test the likelihood that the distribution of extant species among angiosperm genera and families could be the result of constant diversification rates. Results strongly support the conclusion that there is significantly more heterogeneity in diversity at the species level within angiosperms than would be expected due to stochastic processes. This result is consistent in datasets of genus pairs and family pairs and is not affected significantly by degrading pairs to simulate inaccuracy in the assumption of simultaneous origin of sister taxa. When we parse taxon pairs among higher groups of angiosperms, results indicate that a constant rates model is not rejected by rosid and basal eudicot pairs but is rejected by asterid and eumagnoliid pairs. These results provide strong support for the hypothesis that species-level rates of origination and/or extinction have varied nonrandomly within angiosperms and that the magnitude of heterogeneity varies among major groups within angiosperms.
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
Open Univ, Dept Stat, Milton Keynes MK7 6AA, Bucks, England.
RP Sims, HJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
EM sims.hallie@nmnh.si.edu; k.j.mcconway@open.ac.uk
RI McConway, Kevin/G-3729-2012
OI McConway, Kevin/0000-0002-0236-7231
NR 169
TC 29
Z9 29
U1 0
U2 4
PU WILEY-BLACKWELL
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA
SN 0014-3820
EI 1558-5646
J9 EVOLUTION
JI Evolution
PD MAR
PY 2003
VL 57
IS 3
BP 460
EP 479
PG 20
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 666UA
UT WOS:000182193800002
PM 12703936
ER
PT J
AU Fallon, SM
Bermingham, E
Ricklefs, RE
AF Fallon, SM
Bermingham, E
Ricklefs, RE
TI Island and taxon effects in parasitism revisited: Avian malaria in the
Lesser Antilles
SO EVOLUTION
LA English
DT Article
DE avian malaria; coevolution; Haemoproteus; host-parasite interactions;
Lesser Antilles; passerines; Plasmodium
ID BLOOD PARASITES; HAEMATOZOAN INFECTIONS; MITOCHONDRIAL GENOME;
REPRODUCTIVE SUCCESS; PLASMODIUM-ELONGATUM; NATURAL-SELECTION; SEXUAL
SELECTION; PIED FLYCATCHER; GREAT TITS; HOST
AB We identify and describe the distribution of 12 genetically distinct malaria parasite lineages over islands and hosts in four common passerine birds in the Lesser Antilles. Combined parasite prevalence demonstrates strong host effects, little or no island effect, and a significant host-times-island interaction, indicating independent outcomes of host-parasite infections among island populations of the same host species. Host- and/or island-specific parasite lineages do not explain these host-parasite associations; rather, individual lineages themselves demonstrate the same type of independent interactions. Unlike overall prevalence, individual parasite lineages show considerable geographic structure (i.e., island effects) as well as species effects indicating that parasite lineages are constrained in their ability to move between hosts and locations. Together, our results suggest an upper limit to the number of host individuals that malaria parasites, as a community, can infect. Within this limit, however, the relative frequency of the different lineages varies reflecting fine scale interactions between host and parasite populations. Patterns of host-parasite associations within this system suggest both historical co-evolution and ecologically dynamic and independent host-parasite interactions.
C1 Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
Smithsonian Trop Res Inst, APO, AA 34002 USA.
RP Fallon, SM (reprint author), Univ Missouri, Dept Biol, 8001 Nat Bridge Rd, St Louis, MO 63121 USA.
NR 60
TC 96
Z9 97
U1 2
U2 33
PU SOC STUDY EVOLUTION
PI LAWRENCE
PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD MAR
PY 2003
VL 57
IS 3
BP 606
EP 615
PG 10
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 666UA
UT WOS:000182193800016
PM 12703950
ER
PT J
AU Bronson, CL
Grubb, TC
Braun, MJ
AF Bronson, CL
Grubb, TC
Braun, MJ
TI A test of the endogenous and exogenous selection hypotheses for the
maintenance of a narrow avian hybrid zone
SO EVOLUTION
LA English
DT Article
DE endogenous selection; exogenous selection; hybrid zone; Poecile
atricapilla; Poecile carolinensis; transplant experiment
ID GRASSHOPPER PODISMA-PEDESTRIS; TRANSPLANT EXPERIMENTS; TOWNSENDS
WARBLERS; NATURAL-SELECTION; MITOCHONDRIAL-DNA; CHICKADEES;
HYBRIDIZATION; INVIABILITY; ASYMMETRIES; DROSOPHILA
AB The contributions of genetic and environmental factors to differential reproductive success across hybrid zones have rarely been tested. Here, we report a manipulative experiment that simultaneously tested endogenous (genetic-based) and exogenous (environmental-based) selection within a hybrid zone. We transplanted mated pairs of two chickadee species (Poecile atricapilla and P. carolinensis) and their hybrids into isolated woodlots within their hybrid zone and monitored their reproductive success. Although clutch sizes were similar, based on an estimate of the genetic compatibility of a pair, hybrid pairs produced fewer nestlings and fledglings than did pairs of either parental species. According to a linear model generated from the data, a pure pair of either parental species would be expected to produce 1.91-2.48 times more fledglings per nesting attempt, respectively, than the average or least compatible pair in the experiment. Our result of decreased reproduction for hybrid pairs relative to parental species pairs within same environment (the hybrid zone in this experiment) support the endogenous selection hypothesis for maintenance of this hybrid zone. Because the experiment was conducted entirely within the hybrid zone (i.e., the same environment for parental and hybrid pairings), our data do not support the exogenous selection hypothesis as it predicts either all pairings doing poorly or the hybrid pairs more successful than the parental pairs.
C1 Smithsonian Inst, Museum Support Ctr, Natl Museum Nat Hist, Lab Analyt Biol, Suitland, MD 20746 USA.
Smithsonian Inst, Museum Support Ctr, Natl Museum Nat Hist, Dept Syst Biol, Suitland, MD 20746 USA.
Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA.
RP Bronson, CL (reprint author), Ohio State Univ, Dept Internal Med, Div Immunol, Heart & Lung Res Inst 435, 473 W 12th Ave, Columbus, OH 43210 USA.
NR 66
TC 41
Z9 41
U1 2
U2 14
PU SOC STUDY EVOLUTION
PI LAWRENCE
PA 810 E 10TH STREET, LAWRENCE, KS 66044 USA
SN 0014-3820
J9 EVOLUTION
JI Evolution
PD MAR
PY 2003
VL 57
IS 3
BP 630
EP 637
PG 8
WC Ecology; Evolutionary Biology; Genetics & Heredity
SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics &
Heredity
GA 666UA
UT WOS:000182193800018
PM 12703952
ER
PT J
AU Stanley, JD
Krom, MD
Cliff, RA
Woodward, JC
AF Stanley, JD
Krom, MD
Cliff, RA
Woodward, JC
TI Short contribution: Nile flow failure at the end of the old kingdom,
Egypt: Strontium isotopic and petrologic evidence
SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL
LA English
DT Article
ID HOLOCENE; FLUCTUATIONS; SEDIMENT; HISTORY; TROPICS; SAHARA; LAKES
AB Strontium isotopic and petrologic information, obtained from sediment cores collected in the Nile delta of Egypt, indicate that paleoclimatic and Nile baseflow conditions changed considerably from about 4200 to 4000 cal yr B.P. in the Nile basin. Our study records a higher proportion of White Nile sediment transported during the annual floods at ca. 6100 cal yr B.P. than towards 4200 cal yr B.P., at which time suspended sediment from the Blue Nile formed a significantly larger fraction of the total load. This resulted from a decrease in vegetative cover and an increase in erosion rate accompanying the marked decline in rainfall. These new geoscience data indicate major changes in annual flooding and baseflow of the river Nile, marked short-term paleoclimatic-related events that may in part have led to the collapse of the Old Kingdom. (C) 2003 Wiley Periodicals, Inc.
C1 Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Global Change Program, Washington, DC 20560 USA.
Univ Leeds, Sch Earth Sci, Leeds LS2 9JT, W Yorkshire, England.
Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England.
RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Global Change Program, E-206, Washington, DC 20560 USA.
NR 27
TC 50
Z9 55
U1 1
U2 33
PU JOHN WILEY & SONS INC
PI HOBOKEN
PA 111 RIVER ST, HOBOKEN, NJ 07030 USA
SN 0883-6353
J9 GEOARCHAEOLOGY
JI Geoarchaeology
PD MAR
PY 2003
VL 18
IS 3
BP 395
EP 402
DI 10.1002/gea.10065
PG 8
WC Archaeology; Geosciences, Multidisciplinary
SC Archaeology; Geology
GA 649GU
UT WOS:000181199600004
ER
PT J
AU Coates, AG
Aubry, MP
Berggren, WA
Collins, LS
Kunk, M
AF Coates, AG
Aubry, MP
Berggren, WA
Collins, LS
Kunk, M
TI Early neogene history of the Central American arc from Bocas del Toro,
western Panama
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
DE Neogene; Central America; Panama; Bocas del Toro; paleobathymetry;
stratigraphy
ID COSTA-RICA; LIMON-BASIN; PALEOENVIRONMENTS; STRATIGRAPHY; ISTHMUS
AB A newly discovered sequence of lower to middle Miocene rocks from the eastern Bocas del Toro archipelago, western Panama, reveals the timing and environment of the earliest stages in the rise of the Isthmus of Panama in this region. Two new formations, the Punta Alegre Formation (lower Miocene, Aquitanian to Burdigalian) and the Valiente Formation (middle Miocene, Langhian to Serravallian), are here named and formally described. The Punta Alegre Formation contains a diagnostic microfauna of benthic and planktic foraminifera and calcareous nannofossils that indicate deposition in a 2000-m-deep pre-isthmian neotropical ocean from as old as 21.5-18.3 Ma. Its lithology varies from silty mudstone to muddy foraminiferal ooze with rare thin microturbidite layers near the top. The Valiente Formation, which ranges in age from 16.4 to ca. 12.0 Ma, lies with slight angular unconformity on the Punta Alegre Formation and consists of five lithofacies: (1) columnar basalt and flow breccia, (2) pyroclastic deposits, (3) coarse-grained volcaniclastic deposits, (4) coral-reef limestone with diverse large coral colonies, and (5) marine debris-flow deposits and microturbidites. These lithofacies are interpreted to indicate that after ca. 16 Ma a volcanic arc developed in the region of Bocas del Toro and that by ca. 12 Ma an extensively emergent archipelago of volcanic islands had formed. Ar-39/Ar-40 dating of basalt flows associated with the fossiliferous sedimentary rocks in the upper part of the Valiente Formation strongly confirms the ages derived from planktic foraminifera and nannofossils. Paleobathymetric analysis of the two new formations in the Valiente Peninsula and Popa Island, in the Bocas del Toro archipelago, shows a general shallowing from lower- through upper-bathyal to upper-neritic and emergent laharic and fluviatile deposits from ca. 19 to 12 Ma. The overlying nonconformable Bocas del Toro Group contains a lower transgressive sequence ranging from basal nearshore sandstone to upper-bathyal mudstone (ca. 8.15.3 Ma) and an upper regressive sequence (5.3-3.5 Ma). A similar paleobathymetric pattern is observed from the Gatun to Chagres Formations (12-6 Ma) in the Panama Canal Basin area and in the Uscari, Rio Banana, Quebrada Chocolate, and Moin Formations (8-1.7 Ma) in the southern Limon Basin of Costa Rica.
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Univ Montpellier, Inst Sci Evolut, Montpellier 5, France.
Woods Hole Oceanog Inst, Dept Geol & Geophys, Woods Hole, MA 02543 USA.
Florida Int Univ, Dept Earth Sci, Miami, FL 33199 USA.
US Geol Survey, Denver Fed Ctr, Lakewood, CO 80225 USA.
RP Coates, AG (reprint author), Smithsonian Trop Res Inst, POB 2072, Balboa, Panama.
NR 40
TC 69
Z9 76
U1 2
U2 16
PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER
PI DENVER
PA 720 S COLORADO BLVD, STE 960-S, DENVER, CO 80246 USA
SN 0016-7606
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD MAR
PY 2003
VL 115
IS 3
BP 271
EP 287
DI 10.1130/0016-7606(2003)115<0271:ENHOTC>2.0.CO;2
PG 17
WC Geosciences, Multidisciplinary
SC Geology
GA 649EV
UT WOS:000181194700002
ER
PT J
AU Aranda-Gomez, JJ
Luhr, JF
Housh, TB
Connor, CB
Becker, T
Henry, CD
AF Aranda-Gomez, JJ
Luhr, JF
Housh, TB
Connor, CB
Becker, T
Henry, CD
TI Synextensional Pliocene-Pleistocene eruptive activity in the Camargo
volcanic field, Chihuahua, Mexico
SO GEOLOGICAL SOCIETY OF AMERICA BULLETIN
LA English
DT Article
DE basin and range province; Chihuahua; Mexico; extension faults;
intraplate; Pliocene; slip rates
ID WESTERN UNITED-STATES; NORTHERN MEXICO; SOUTHERN BASIN; LA-OLIVINA;
CENOZOIC EXTENSION; TERTIARY VOLCANISM; ALKALI BASALTS; DURANGO-CITY;
PETROLOGY; RANGE
AB The Camargo volcanic field is the largest mafic alkalic volcanic field in the Mexican Basin and Range province, and the relationship between volcanism and normal faulting is especially strong. The Camargo volcanic field lies in the northern part of the province, midway between the Sierra Madre Occidental and Trans-Pecos Texas. It is formed by Pliocene-Pleistocene (4.7-0.09 Ma) intraplate mafic alkalic volcanic rocks, some of which contain peridotite, pyroxenite, and granulite xenoliths. The volcanic field covers similar to3000 km(2) and has an estimated volume of similar to 120 km(3) erupted from >300 recognized vents. Twenty-six new Ar-40/Ar-39 age determinations for the Camargo volcanic field and its environs show that volcanic activity began in the southwest part of the field and shifted toward the northeast at similar to15 mm/yr. The average magmatic eruption rate during growth of the field was similar to0.026 km(3)/k.y. The Camargo volcanic field lies within an accommodation zone with west-dipping faults and east-tilted blocks to the north and east-dipping faults and west-tilted blocks to the south. These faults are expressed in the volcanic field by a N30degreesW-trending graben with scarps up to similar to100 m high through its central part. Volcanism and faulting were at least in part coeval, and younger volcanic products commonly drape fault scarps that cut earlier lavas. Normal faulting is bracketed between 4.7 and 2.1 Ma and may have also migrated northeastward. Estimated vertical slip rates on four Pliocene faults range from 0.03 mm/yr, a likely long-term rate, to 1.67 mm/ yr, interpreted as a short-term rate operative during periods of active faulting. Northwest-striking normal faults that cut alluvial-fan deposits and Pleistocene lavas in the northern Camargo volcanic field and geomorphic evidence for recent uplift to the south of the volcanic field suggest that the region is still extending.
C1 Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76001, Mexico.
Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA.
Univ Texas, Dept Geol Sci, Austin, TX 78712 USA.
Univ S Florida, Dept Geol, Tampa, FL 33620 USA.
Berkeley Geochronol Ctr, Berkeley, CA 94709 USA.
Univ Nevada, Nevada Bur Mines & Geol, Reno, NV 89557 USA.
RP Aranda-Gomez, JJ (reprint author), Univ Nacl Autonoma Mexico, Ctr Geociencias, Campus Juriquilla,POB 1-742, Queretaro 76001, Mexico.
NR 67
TC 31
Z9 32
U1 0
U2 1
PU ASSOC ENGINEERING GEOLOGISTS GEOLOGICAL SOCIETY AMER
PI DENVER
PA 720 S COLORADO BLVD, STE 960-S, DENVER, CO 80246 USA
SN 0016-7606
J9 GEOL SOC AM BULL
JI Geol. Soc. Am. Bull.
PD MAR
PY 2003
VL 115
IS 3
BP 298
EP 313
DI 10.1130/0016-7606(2003)115<0298:SPPEAI>2.0.CO;2
PG 16
WC Geosciences, Multidisciplinary
SC Geology
GA 649EV
UT WOS:000181194700004
ER
PT J
AU Watters, TR
AF Watters, TR
TI Lithospheric flexure and the origin of the dichotomy boundary on Mars
SO GEOLOGY
LA English
DT Article
DE Mars; tectonics; flexure; dichotomy boundary; elastic thickness
ID ORBITER LASER ALTIMETER; CRUSTAL DICHOTOMY; THERMAL EVOLUTION; GLOBAL
SURVEYOR; PLATE-TECTONICS; LOBATE SCARPS; GIANT IMPACT; TOPOGRAPHY;
STRESS; CONVECTION
AB The crustal dichotomy between the ancient highlands of the Southern Hemisphere and the young-appearing northern lowlands is a defining feature of Mars. In the Eastern Hemisphere the dichotomy boundary is marked by a prominent scarp and extensional and compressional tectonic features. Topographic data across the boundary returned from the Mars Global Surveyor indicate lithospheric flexure of the southern highlands. The topography of the boundary can be fit by a universal lithospheric deflection profile that corresponds to an elastic thickness of similar to31-36 km. Flexure of the southern highlands may be due to late Noachian-early Hesperian vertical loading of the northern lowlands. Fracturing and normal faulting along the boundary may be in response to bending stresses, while thrust faulting may result from a combination of stresses due to flexure, erosion, and global contraction.
C1 Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA.
NR 35
TC 30
Z9 30
U1 0
U2 1
PU GEOLOGICAL SOC AMERICA, INC
PI BOULDER
PA PO BOX 9140, BOULDER, CO 80301-9140 USA
SN 0091-7613
J9 GEOLOGY
JI Geology
PD MAR
PY 2003
VL 31
IS 3
BP 271
EP 274
DI 10.1130/0091-7613(2003)031<0271:LFATOO>2.0.CO;2
PG 4
WC Geology
SC Geology
GA 649GN
UT WOS:000181199100020
ER
PT J
AU Drake, JB
Knox, RG
Dubayah, RO
Clark, DB
Condit, R
Blair, JB
Hofton, M
AF Drake, JB
Knox, RG
Dubayah, RO
Clark, DB
Condit, R
Blair, JB
Hofton, M
TI Above-ground biomass estimation in closed canopy Neotropical forests
using lidar remote sensing: factors affecting the generality of
relationships
SO GLOBAL ECOLOGY AND BIOGEOGRAPHY
LA English
DT Article
DE above-ground biomass; allometry; carbon cycle; Central America;
environmental factors; forest structure; laser altimetry; lidar; remote
sensing; tropical forests
ID LARGE-FOOTPRINT LIDAR; TROPICAL RAIN-FOREST; LASER ALTIMETER; HEIGHT
PROFILES; LANDSCAPE-SCALE; BIOSPHERE MODEL; COSTA-RICA; VEGETATION;
SECONDARY; BRAZIL
AB Aim Previous studies have developed strong, site-specific relationships between canopy metrics from lidar (light detecting and ranging) remote sensing data and forest structural characteristics such as above-ground biomass (AGBM), but the generality of these relationships is unknown. In this study, we examine the generality of relationships between lidar metrics and forest structural characteristics, including AGBM, from two study areas in Central America with different precipitation patterns.
Location A series of tropical moist forest sites in Panama and a tropical wet forest in Costa Rica.
Methods Canopy metrics (e.g. canopy height) were calculated from airborne lidar data. Basal area, mean stem diameter and AGBM were calculated from measurements taken as a part of ongoing forest dynamics studies in both areas. We examined the generality of relationship between lidar metrics and forest structure, and possible environmental effects (e.g. leaf phenology).
Results We found that lidar metrics were strongly correlated (R-2:0.65-0.92) with mean stem diameter, basal area and AGBM in both regions. We also show that the relationships differed between these regions. Deciduousness of canopy trees in the tropical moist forest area accounted for the differences in predictive equations for stem diameter and basal area. The relationships between lidar metrics and AGBM, however, remained significantly different between the two study areas even after adjusting for leaf drop. We attribute this to significant differences in the underlying allometric relationships between stem diameter and AGBM in tropical wet and moist forests.
Conclusions Important forest structural characteristics can be estimated reliably across a variety of conditions sampled in these closed-canopy tropical forests. Environmental factors such as drought deciduousness have an important influence on these relationships. Future efforts should continue to examine climatic factors that may influence the generality of the relationships between lidar metrics and forest structural characteristics and assess more rigorously the generality of field-derived allometric relationships.
C1 Univ Maryland, Dept Geog, College Pk, MD 20742 USA.
NASA, Biospher Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
Univ Missouri, Dept Biol, St Louis, MO 63121 USA.
Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA.
NASA, Laser Remote Sensing Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA.
RP Drake, JB (reprint author), Univ Georgia, Warnell Sch Forest Resources, Athens, GA 30602 USA.
RI Knox, Robert/E-9657-2011; Blair, James/D-3881-2013; Beckley,
Matthew/D-4547-2013
NR 58
TC 146
Z9 149
U1 5
U2 63
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0960-7447
J9 GLOBAL ECOL BIOGEOGR
JI Glob. Ecol. Biogeogr.
PD MAR
PY 2003
VL 12
IS 2
BP 147
EP 159
DI 10.1046/j.1466-822X.2003.00010.x
PG 13
WC Ecology; Geography, Physical
SC Environmental Sciences & Ecology; Physical Geography
GA 652TU
UT WOS:000181396700006
ER
PT J
AU Rappole, JH
Helm, H
Ramos, MA
AF Rappole, JH
Helm, H
Ramos, MA
TI An integrative framework for understanding the origin and evolution of
avian migration
SO JOURNAL OF AVIAN BIOLOGY
LA English
DT Editorial Material
ID BIRD POPULATION; FLYCATCHERS; ECOLOGY
C1 Smithsonian Conservat & Res Ctr, Front Royal, VA 22630 USA.
Max Planck Res Ctr Ornithol, D-82346 Andechs, Germany.
World Bank, Global Environm Facil, Washington, DC 20433 USA.
RP Rappole, JH (reprint author), Smithsonian Conservat & Res Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA.
NR 64
TC 27
Z9 27
U1 0
U2 25
PU BLACKWELL MUNKSGAARD
PI COPENHAGEN
PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK
SN 0908-8857
J9 J AVIAN BIOL
JI J. Avian Biol.
PD MAR
PY 2003
VL 34
IS 1
BP 124
EP 128
PG 5
WC Ornithology
SC Zoology
GA 676GQ
UT WOS:000182743300017
ER
PT J
AU Wright, TF
Cortopassi, KA
Bradbury, JW
Dooling, RJ
AF Wright, TF
Cortopassi, KA
Bradbury, JW
Dooling, RJ
TI Hearing and vocalizations in the orange-fronted conure (Aratinga
canicularis)
SO JOURNAL OF COMPARATIVE PSYCHOLOGY
LA English
DT Article
ID PARAKEET MELOPSITTACUS-UNDULATUS; AUDITORY INTENSITY DISCRIMINATION;
ACOUSTIC COMMUNICATION; THRESHOLDS; EVOLUTION; NOISE; SENSITIVITY;
PERCEPTION; BIRDS; SONG
AB The auditory sensitivities of the orange-fronted conure (Aratinga canicularis) were examined in relation to the spectral characteristics of its vocalizations. Absolute thresholds, masked thresholds, frequency difference limens, and intensity difference limens for pure tones were obtained using psychoacoustic techniques. In general, hearing abilities are similar to those found in many avian auditory generalists. One exception is the unusually low critical ratio (masked threshold) between 2.0 and 4.0 kHz, similar to that previously found in the budgerigar (Melopsittacus undulatus). These auditory sensitivities were compared with average spectra for (a) contact calls and (b) a general sample of vocalizations recorded from wild birds. The spectral regions of both greatest vocal energy and best auditory sensitivity were between 2.0 and 5.0 kHz.
C1 Univ Maryland, Dept Psychol, College Pk, MD 20742 USA.
Cornell Lab Ornithol, Macaulay Lib Nat Sounds, Ithaca, NY USA.
RP Smithsonian Natl Zoo, Genet Mol Lab, 3001 Connecticut Ave, Washington, DC 20008 USA.
EM tw98@umail.umd.edu
FU NIDCD NIH HHS [DC00046, DC00198]; NIMH NIH HHS [F32 MH012111, MH12111]
NR 40
TC 17
Z9 18
U1 2
U2 7
PU AMER PSYCHOLOGICAL ASSOC
PI WASHINGTON
PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 USA
SN 0735-7036
EI 1939-2087
J9 J COMP PSYCHOL
JI J. Comp. Psychol.
PD MAR
PY 2003
VL 117
IS 1
BP 87
EP 95
DI 10.1037/0735-7036.117.1.87
PG 9
WC Behavioral Sciences; Psychology; Psychology, Multidisciplinary; Zoology
SC Behavioral Sciences; Psychology; Zoology
GA 667WD
UT WOS:000182256800011
PM 12735368
ER
PT J
AU Srygley, RB
AF Srygley, RB
TI Wind drift compensation in migrating dragonflies Pantala (Odonata :
Libellulidae)
SO JOURNAL OF INSECT BEHAVIOR
LA English
DT Article
DE insect; flight; energetics; optimal migration; behavioral ecology;
tropical
ID NATURAL FREE-FLIGHT; BUTTERFLIES; LEPIDOPTERA; PHYSIOLOGY; SEAS
AB Tailwind drift compensation serves to maximize a migrant's flight distance on a given amount of energy, and crosswind drift compensation serves to hold a course true and minimize the distance flown. With full or part compensation, airspeeds are predicted to increase with greater crosswind drift. To test whether migrating dragonflies compensated for wind drift, I measured the velocity and heading of Pantala hymenaea and P. flavescens in natural flight over a lake and the ambient wind speed and direction. P. hymenaea flew northeasterly (58degrees), whereas P. flavescens flew significantly more east-north easterly (74degrees) throughout the day. Pantala spp. demonstrated part compensation for changes in crosswind drift within individuals (mean compensation = 54%, P = 0.0000), evidence for use of a ground reference to correct for drift when flying over water. Among individuals, P. flavescens compensated for crosswind drift. P. hymenaea overcompensated and then drifted downwind on one morning and compensated for crosswind drift on the next. As predicted from optimal migration theory, airspeed (5.0 m/s for both species with no tailwind) decreased with tailwind velocity both among individuals ( data for both species pooled [n = 19]; P < 0.0001) and within each individual as it crossed the lake (P = 0.0016).
C1 Smithsonian Trop Res Inst, Balboa, Panama.
Univ Oxford, Dept Zool, Oxford OX1 3PS, England.
RP Srygley, RB (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama.
NR 22
TC 21
Z9 27
U1 0
U2 10
PU KLUWER ACADEMIC/PLENUM PUBL
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0892-7553
J9 J INSECT BEHAV
JI J. Insect Behav.
PD MAR
PY 2003
VL 16
IS 2
BP 217
EP 232
DI 10.1023/A:1023915802067
PG 16
WC Entomology
SC Entomology
GA 683BJ
UT WOS:000183126600004
ER
PT J
AU Ospina, CA
Rodriguez, AD
Ortega-Barria, E
Capson, TL
AF Ospina, CA
Rodriguez, AD
Ortega-Barria, E
Capson, TL
TI Briarellins J-P and polyanthellin A: New eunicellin-based diterpenes
from the gorgonian coral Briareum polyanthes and their antimalarial
activity
SO JOURNAL OF NATURAL PRODUCTS
LA English
DT Article
ID MARINE NATURAL-PRODUCTS; SCLEROPHYTIN-A; ASBESTINUM PALLAS;
(-)-SCLEROPHYTIN-A; CONSTITUENTS; ACETATE
AB A new chemical study of the hexane extract of the gorgonian Briareum polyanthes collected in Puerto Rico afforded 10 new diterpenes of the eunicellin class, briarellins 1-9 and polyanthellin A (10), along with the known diterpene briarellin D (11). The structures and relative stereochemistry of metabolites 1-10 were assigned on the basis of NMR studies, chemical methods, and comparisons to the spectral properties of 11. A reassessment of prior structural assignment for briarellin A and two known sclerophytin-type diterpenes, 13 and 14, is proposed. Antimalarial tests on 1-6 and 8-12 indicated that they were active against Plasmodium falciparum.
C1 Univ Puerto Rico, Dept Chem, Rio Piedras, PR 00931 USA.
Florida State Univ, Cell & Mol Biol Pathogens Unit, Inst Trop Med & Hlth Sci, Balboa, Panama.
Smithsonian Trop Res Inst, Balboa, Ancon, Panama.
RP Rodriguez, AD (reprint author), Univ Puerto Rico, Dept Chem, POB 23346, Rio Piedras, PR 00931 USA.
EM arodrig@goliath.cnnet.clu.edu
RI Johnson, Selena/K-3541-2013
FU FIC NIH HHS [1 UO1TW01021-01]; NINDS NIH HHS [U54-NS39408-04]
NR 30
TC 39
Z9 42
U1 0
U2 4
PU AMER CHEMICAL SOC
PI WASHINGTON
PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA
SN 0163-3864
J9 J NAT PROD
JI J. Nat. Prod.
PD MAR
PY 2003
VL 66
IS 3
BP 357
EP 363
DI 10.1021/np0204500
PG 7
WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy
SC Plant Sciences; Pharmacology & Pharmacy
GA 662AL
UT WOS:000181923100007
PM 12662092
ER
PT J
AU Suarez, W
Olson, SL
AF Suarez, W
Olson, SL
TI Red-shouldered Hawk and Aplomado Falcon from quaternary asphalt deposits
in Cuba
SO JOURNAL OF RAPTOR RESEARCH
LA English
DT Article
DE Aplomado Falcon; Falco femoralis; Red-Shouldered Hawk; Buteo lineatus;
Antilles; Cuba; extinctions; fossil birds; Quaternary; West Indies
ID AVES
C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
Museo Nacl Hist Nat, Havana 10100, Cuba.
RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
NR 18
TC 2
Z9 2
U1 0
U2 3
PU RAPTOR RESEARCH FOUNDATION INC
PI HASTINGS
PA 14377 117TH STREET SOUTH, HASTINGS, MN 55033 USA
SN 0892-1016
J9 J RAPTOR RES
JI J. Raptor Res.
PD MAR
PY 2003
VL 37
IS 1
BP 71
EP 75
PG 5
WC Ornithology
SC Zoology
GA 673CJ
UT WOS:000182561800011
ER
PT J
AU Andersen, NM
Polhemus, DA
AF Andersen, NM
Polhemus, DA
TI A new genus of terrestrial Mesoveliidae from the Seychelles (Hemiptera :
Gerromorpha)
SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Mesoveliidae; Seychelles; new genus; new species; zoogeography
ID WATER-STRIDER; HETEROPTERA
AB A new genus of Mesoveliidae, Seychellovelia, with a single included species, S. hygrobia n. sp., is described from the islands of Silhouette and Mahe in the granitic Seychelles. This new taxon is compared to other mesovehid genera, and its key morphological characters illustrated. Information is also provided on the habitat preferences of S. hygrobia, and an updated distributional map of mesoveliid genera on a world basis is provided, accompanied by a discussion of zoogeographical implications.
C1 Univ Copenhagen, Zool Museum, DK-2100 Copenhagen, Denmark.
Smithsonian Inst, Museum Natl Hist Nat, Dept Systemat Biol, Washington, DC 20560 USA.
RP Andersen, NM (reprint author), Univ Copenhagen, Zool Museum, Univ Pk 15, DK-2100 Copenhagen, Denmark.
NR 16
TC 11
Z9 13
U1 0
U2 0
PU NEW YORK ENTOMOLOGICAL SOC INC
PI NEW YORK
PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024
USA
SN 0028-7199
J9 J NEW YORK ENTOMOL S
JI J. N.Y. Entomol. Soc.
PD SPR
PY 2003
VL 111
IS 1
BP 12
EP 21
DI 10.1664/0028-7199(2003)111[0012:ANGOTM]2.0.CO;2
PG 10
WC Entomology
SC Entomology
GA 711KT
UT WOS:000184740300002
ER
PT J
AU Polhemus, DA
Polhemus, JT
AF Polhemus, DA
Polhemus, JT
TI A review of the Veliinae of Vietnam (Heteroptera : Veliidae) with
description of a new Velia species
SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Asia; Veliidae; Vietnam; new species; new records; distributions
AB The Veliinae of Vietnam are reviewed. and the new species Velia tonkina described from the Huong Lien Son mountains in the far north of the country. Three additional species of Veliinae, Chenevelia stridulans, Angilia bispinosa, and Angilia orientalis, are recorded from Vietnam for the first time. Distribution maps are provided for all these species, dorsal habitus illustrations are provided for Velia tonkina and Chenevelia stridulans, and illustrations of male genitalic structures are provided for Velia tonkina.
C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA.
Colorado Entomol Inst, Englewood, CO 80110 USA.
RP Polhemus, DA (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC 105, Washington, DC 20560 USA.
NR 7
TC 2
Z9 2
U1 0
U2 0
PU NEW YORK ENTOMOLOGICAL SOC INC
PI NEW YORK
PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024
USA
SN 0028-7199
J9 J NEW YORK ENTOMOL S
JI J. N.Y. Entomol. Soc.
PD SPR
PY 2003
VL 111
IS 1
BP 29
EP 40
DI 10.1664/0028-7199(2003)111[0029:AROTVO]2.0.CO;2
PG 12
WC Entomology
SC Entomology
GA 711KT
UT WOS:000184740300004
ER
PT J
AU Seago, A
Lingafelter, SW
AF Seago, A
Lingafelter, SW
TI Discovery of Crepidodera bella Parry (Coleoptera : Chrysomelidae :
Alticini) in Maryland and redescription
SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Crepidodera; Chrysomelidae; flea beetle; Maryland; Salix; willow;
redescription; range extension
AB Crepidodera bella Parry (Coleoptera: Chrysomelidae: Alticini), previously known only from Florida, South Carolina, Alabama, and Louisiana, is discovered in central Maryland. This species is sympatric with C. browni Parry on Salix nigra growing along swamps in the McKee-Besher Wildlife Management Area (39degrees04'30"N, 77degrees23'00"W). Morphological features of the integument and genitalia are described and compared to C. browni.
C1 Cornell Univ, Ithaca, NY 14853 USA.
Smithsonian Inst, Natl Museum Nat Hist, Res Training Program, Washington, DC 20560 USA.
USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA.
RP Seago, A (reprint author), Cornell Univ, Ithaca, NY 14853 USA.
RI Seago, Ainsley/B-4211-2009
NR 5
TC 2
Z9 2
U1 0
U2 0
PU NEW YORK ENTOMOLOGICAL SOC INC
PI NEW YORK
PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024
USA
SN 0028-7199
J9 J NEW YORK ENTOMOL S
JI J. N.Y. Entomol. Soc.
PD SPR
PY 2003
VL 111
IS 1
BP 51
EP 56
DI 10.1664/0028-7199(2003)111[0051:DOCBPC]2.0.CO;2
PG 6
WC Entomology
SC Entomology
GA 711KT
UT WOS:000184740300007
ER
PT J
AU Lingafelter, SW
AF Lingafelter, SW
TI New host and elevation records for Moneilema appressum LeConte
(Coleoptera : Cerambycidae : Lamiinae)
SO JOURNAL OF THE NEW YORK ENTOMOLOGICAL SOCIETY
LA English
DT Article
DE Moneilenia; Echinocereus; Opuntia; cactus; Lamiinae; Arizona;
hostplants; elevation record
AB An isolated population of Moneilema appressum LeConte was discovered above Long Park in the Chiricahua Mountains of southeastern Arizona (31degrees52'44"N, 109degrees17'12"W) during July 2001. Specimens of this flightless lamiine cerambycid were observed hiding and walking in the junctures of Echinocereus coccineus Engelmann (Cactaceae) at 2,760 m (9,055 feet). These data represent new host plant and elevation records for this species.
C1 USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA.
Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.
RP Lingafelter, SW (reprint author), USDA, ARS, PSI, Systemat Entomol Lab, Washington, DC 20250 USA.
NR 10
TC 4
Z9 4
U1 1
U2 2
PU NEW YORK ENTOMOLOGICAL SOC INC
PI NEW YORK
PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024
USA
SN 0028-7199
J9 J NEW YORK ENTOMOL S
JI J. N.Y. Entomol. Soc.
PD SPR
PY 2003
VL 111
IS 1
BP 57
EP 60
DI 10.1664/0028-7199(2003)111[0057:NHAERF]2.0.CO;2
PG 4
WC Entomology
SC Entomology
GA 711KT
UT WOS:000184740300008
ER
PT J
AU Riley, S
AF Riley, S
TI Man and wife.
SO LIBRARY JOURNAL
LA English
DT Book Review
C1 Smithsonian Inst, Lib, Washington, DC 20560 USA.
RP Riley, S (reprint author), Smithsonian Inst, Lib, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION
PI NEW YORK
PA 249 W 17TH ST, NEW YORK, NY 10011 USA
SN 0363-0277
J9 LIBR J
JI Libr. J.
PD MAR 1
PY 2003
VL 128
IS 4
BP 120
EP 120
PG 1
WC Information Science & Library Science
SC Information Science & Library Science
GA 673WN
UT WOS:000182603400179
ER
PT J
AU Mate, JL
AF Mate, JL
TI Ecological, genetic, and morphological differences among three Pavona
(Cnidaria : Anthozoa) species from the Pacific coast of Panama
SO MARINE BIOLOGY
LA English
DT Article
ID CORAL MONTASTRAEA-ANNULARIS; SCLERACTINIAN CORALS; EASTERN PACIFIC; REEF
CORALS; INTERSPECIFIC AGGRESSION; REPRODUCTIVE ISOLATION; COMMUNITY
STRUCTURE; COSTA-RICA; FERTILIZATION; POPULATIONS
AB Ecological, genetic, and morphological differences among three Panamanian Pacific Pavona species with strongly developed collines (Pavona varians, P. frondifera, and P. chiriquiensis) were examined. Ecological factors included geographical distributions of species, habitat preferences, interspecific interactions, reproductive ecology, and tolerance to bleaching. Genetic differences were based on the electrophoretic analysis of ten allozyme loci. Morphological analyses consisted of tissue coloration, colony morphology, and measurements and counts of ten macro- and micro-skeletal characters. P. varians, present on reefs or in coral communities, is the most widely distributed and shows considerable morphological variation. P. chiriquiensis, a recently described species, encrusts basalt rock and has little morphological variation. P. frondifera is a reef dweller with a compact foliose morphology. Tissue coloration varies from light to dark brown in P. varians, from pink to brown in P. frondifera, and from brick red to brown or silvery in Pavona chiriquiensis. Also, the white to silvery polyp mouths of the latter species are a diagnostic feature that allows an easy identification in the field. Aggressive dominance during short-term interspecific interactions were as follows: Pavona chiriquiensis > P. varians > P. frondifera. P. chiriquiensis and P. varians showed contrasting responses to sea warming during the 1997-1998 El Nino, Southern Oscillation. Whereas entire P. chiriquiensis bleached and died within 4 weeks of exposure to 30-31degreesC, colonies of P. varians did so only on their upper surfaces. The response of P. frondifera to elevated temperatures was not observed because it is mainly present in the Gulf of Panama where coral bleaching was absent in 1997-1998. The genetic data indicated that P. chiriquiensis differed strongly from both P. varians and P. frondifera, with Nei's unbiased genetic distances of 0.434 and 0.379, respectively. A fixed difference between P. varians and P. frondifera, and P. chiriquiensis exists at the triose phosphate isomerase (TPI-2) locus. A nearly fixed difference between P. chiriquiensis and P. frondifera and between P. chiriquiensis and P. varians was found at the hexokinase (HK) locus. P. varians differed slightly from P. frondifera with Nei's unbiased genetic distance of 0.068. No fixed difference was found between P. varians and P. frondifera. There were strong differences between P. chiriquiensis and P. varians in spawning times and gamete characteristics. Spawning in P. varians and P. chiriquiensis is 12 h out of phase. Also, eggs of the former species are white to beige and positively buoyant whereas those of the latter species are dark green and neutrally to negatively buoyant. No reproductive data are yet available for P. frondifera. Calicular diameters are significantly greater in P. chiriquiensis than in the other two species. In contrast, corallum thickness is greater in P. varians and P. frondifera than in P. chiriquiensis. Canonical discriminant function analysis readily separated the three species.
C1 Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA.
RP Mate, JL (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama.
NR 75
TC 8
Z9 9
U1 0
U2 7
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0025-3162
J9 MAR BIOL
JI Mar. Biol.
PD MAR
PY 2003
VL 142
IS 3
BP 427
EP 440
DI 10.1007/s00227-002-0956-9
PG 14
WC Marine & Freshwater Biology
SC Marine & Freshwater Biology
GA 670BR
UT WOS:000182387900003
ER
PT J
AU Dick, CW
Etchelecu, G
Austerlitz, F
AF Dick, CW
Etchelecu, G
Austerlitz, F
TI Pollen dispersal of tropical trees (Dinizia excelsa: Fabaceae) by native
insects and African honeybees in pristine and fragmented Amazonian
rainforest
SO MOLECULAR ECOLOGY
LA English
DT Article
DE Apis mellifera; microsatellites; pollen flow; pollination; tropical
rainforest; TwoGener analysis
ID N INDEPENDENT LOCI; RAIN-FOREST; 2-GENERATION ANALYSIS; HABITAT
FRAGMENTATION; GENETIC CONSEQUENCES; SPECIES RICHNESS; MATING SYSTEMS;
DRY FOREST; SEED SET; BEES
AB Tropical rainforest trees typically occur in low population densities and rely on animals for cross-pollination. It is of conservation interest therefore to understand how rainforest fragmentation may alter the pollination and breeding structure of remnant trees. Previous studies of the Amazonian tree Dinizia excelsa (Fabaceae) found African honeybees (Apis mellifera scutellata ) as the predominant pollinators of trees in highly disturbed habitats, transporting pollen up to 3.2 km between pasture trees. Here, using microsatellite genotypes of seed arrays, we compare outcrossing rates and pollen dispersal distances of (i) remnant D. excelsa in three large ranches, and (ii) a population in undisturbed forest in which African honeybees were absent. Self-fertilization was more frequent in the disturbed habitats (14%, n = 277 seeds from 12 mothers) than in undisturbed forest (10%, n = 295 seeds from 13 mothers). Pollen dispersal was extensive in all three ranches compared to undisturbed forest, however. Using a twogener analysis, we estimated a mean pollen dispersal distance of 1509 m in Colosso ranch, assuming an exponential dispersal function, and 212 m in undisturbed forest. The low effective density of D. excelsa in undisturbed forest (similar to0.1 trees/ha) indicates that large areas of rainforest must be preserved to maintain minimum viable populations. Our results also suggest, however, that in highly disturbed habitats Apis mellifera may expand genetic neighbourhood areas, thereby linking fragmented and continuous forest populations.
C1 Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil.
Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
INRA Domaine Hermitage, Lab Genet Ameliorat Arbres Forestiers, F-33612 Pierroton F Cestas, France.
RP Dick, CW (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
RI Dick, Christopher/A-8744-2008
NR 79
TC 206
Z9 220
U1 7
U2 52
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0962-1083
J9 MOL ECOL
JI Mol. Ecol.
PD MAR
PY 2003
VL 12
IS 3
BP 753
EP 764
DI 10.1046/j.1365-294X.2003.01760.x
PG 12
WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology
SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology;
Evolutionary Biology
GA 649WL
UT WOS:000181230900017
PM 12675830
ER
PT J
AU Bate, MR
Bonnell, IA
Bromm, V
AF Bate, MR
Bonnell, IA
Bromm, V
TI The formation of a star cluster: predicting the properties of stars and
brown dwarfs
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Review
DE accretion, accretion discs; hydrodynamics; binaries : general; stars :
formation; stars : low-mass, brown dwarfs; stars : luminosity function,
mass function
ID INITIAL MASS FUNCTION; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS;
SMOOTHED PARTICLE HYDRODYNAMICS; ROTATING INTERSTELLAR CLOUDS; ELONGATED
CYLINDRICAL CLOUDS; SOLAR-TYPE STARS; SELF-GRAVITATIONAL HYDRODYNAMICS;
WEAKLY MAGNETIZED DISKS; LOCAL SHEAR INSTABILITY
AB We present results from the largest numerical simulation of star formation to resolve the fragmentation process down to the opacity limit. The simulation follows the collapse and fragmentation of a large-scale turbulent molecular cloud to form a stellar cluster and, simultaneously, the formation of circumstellar discs and binary stars. This large range of scales enables us to predict a wide variety of stellar properties for comparison with observations.
The calculation clearly demonstrates that star formation is a highly-dynamic and chaotic process. Star formation occurs in localized bursts within the cloud via the fragmentation both of dense molecular cloud cores and of massive circumstellar discs. Star-disc encounters form binaries and truncate discs. Stellar encounters disrupt bound multiple systems. We find that the observed statistical properties of stars are a natural consequence of star formation in such a dynamical environment. The cloud produces roughly equal numbers of stars and brown dwarfs, with masses down to the opacity limit for fragmentation (approximate to5 Jupiter masses). The initial mass function is consistent with a Salpeter slope (Gamma=-1.35) above 0.5 M(circle dot) , a roughly flat distribution (Gamma= 0) in the range 0.006-0.5 M(circle dot) , and a sharp cut-off below approximate to0.005 M(circle dot). This is consistent with recent observational surveys. The brown dwarfs form by the dynamical ejection of low-mass fragments from dynamically unstable multiple systems before the fragments have been able to accrete to stellar masses. Close binary systems (with separations less than or similar to10 au) are not formed by fragmentation in situ . Rather, they are produced by hardening of initially wider multiple systems through a combination of dynamical encounters, gas accretion, and/or the interaction with circumbinary and circumtriple discs. Finally, we find that the majority of circumstellar discs have radii less than 20 au due to truncation in dynamical encounters. This is consistent with observations of the Orion Trapezium cluster and implies that most stars and brown dwarfs do not form large planetary systems.
C1 Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England.
Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Bate, MR (reprint author), Univ Exeter, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England.
EM mbate@astro.ex.ac.uk
NR 173
TC 474
Z9 475
U1 2
U2 10
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 MAR 1
PY 2003
VL 339
IS 3
BP 577
EP 599
DI 10.1046/j.1365-8711.2003.06210.x
PG 23
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647DN
UT WOS:000181077300001
ER
PT J
AU Jonker, PG
van der Klis, M
Groot, PJ
AF Jonker, PG
van der Klis, M
Groot, PJ
TI The mass of the neutron star in the low-mass X-ray binary 2A 1822-371
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE techniques : radial velocities; stars : individual : 2A 1822-371; stars
: neutron; X-rays : stars
ID CATACLYSMIC VARIABLES; SECONDARY STAR; RADIO PULSARS; DISCOVERY;
X-1822-371; IRRADIATION; MODULATION; VELOCITY
AB Using phase-resolved spectroscopic observations obtained with the Ultraviolet and Visual Echelle Spectrograph on the ESO Kueyen Very Large Telescope, supplemented by spectroscopic observations obtained with the Boller and Chivens spectrograph on the Walter Baade Magellan Telescope, we have found sinusoidal radial velocity variations with a semi-amplitude of 327 +/- 17 km s(-1) . From previous observations and from the fact that the epoch of minimum velocity arrived early with respect to the epoch calculated from pulse timing, we know that the companion star is suffering from irradiation. Since we most likely observed primarily the side of the companion star facing the observer at phase similar to0.75, the velocity quoted above is not the true radial velocity semi-amplitude of the companion star. Assuming a uniform contribution to the line profile from this hemisphere yields a radial velocity semi-amplitude of 280 +/- 26 km s(-1)for a systemic velocity of 54 +/- 24 km s(-1); if the contribution is instead weighted somewhat more towards the side of the companion facing the X-ray source then the true semi-amplitude is larger than this value. Together with the well-constrained inclination (81degrees < i < 84degrees) and the mass function determined from pulse-timing analysis(2.03 +/- 0.03 x 10(-2) M-circle dot ), we derive a lower limit to the mass of the neutron star and to that of the companion star of 0.97 +/- 0.24 and 0.33 +/- 0.05 M-circle dot , respectively (1sigma; including uncertainties in the inclination). We briefly discuss other aspects of the spectrum and the implications of our findings.
C1 Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England.
Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Nijmegen, Dept Astrophys, Nijmegen, Netherlands.
RP Jonker, PG (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.
RI Groot, Paul/K-4391-2016
OI Groot, Paul/0000-0002-4488-726X
NR 35
TC 28
Z9 29
U1 0
U2 3
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2003
VL 339
IS 3
BP 663
EP 668
DI 10.1046/j.1365-8711.2003.06193.x
PG 6
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647DN
UT WOS:000181077300009
ER
PT J
AU Strader, J
Brodie, JP
Huchra, JP
AF Strader, J
Brodie, JP
Huchra, JP
TI Spectroscopy of a globular cluster in the Local Group dwarf irregular
NGC 6822
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE globular clusters : general; galaxies : individual : NGC 6822; galaxies
: star clusters
ID SMALL-MAGELLANIC-CLOUD; HUBBLE-SPACE-TELESCOPE; STAR-CLUSTERS; AGES;
METALLICITY; NGC-6822; GALAXY
AB We present low-resolution Keck spectroscopy for the globular cluster (GC) H VIII in the Local Group dwarf irregular galaxy NGC 6822. We find the metallicity of the cluster to be [Fe/H]=-1.58 +/- 0.28 and the age of the cluster to be 3-4 Gyr, slightly older than but consistent with previous age estimates. H VIII seems to be more metal-poor than most intermediate-age GCs in the Local Group, and appears most similar to the anomalous Small Magellanic Cloud clusters Lindsay 113 and NGC 339.
C1 Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Strader, J (reprint author), Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA.
NR 22
TC 6
Z9 6
U1 0
U2 0
PU BLACKWELL PUBLISHING LTD
PI OXFORD
PA 9600 GARSINGTON RD, OXFORD OX4 2DG, OXON, ENGLAND
SN 0035-8711
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2003
VL 339
IS 3
BP 707
EP 710
DI 10.1046/j.1365-8711.2003.06212.x
PG 4
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647DN
UT WOS:000181077300015
ER
PT J
AU Steeghs, D
Perryman, MAC
Reynolds, A
de Bruijne, JHJ
Marsh, T
Dhillon, VS
Peacock, A
AF Steeghs, D
Perryman, MAC
Reynolds, A
de Bruijne, JHJ
Marsh, T
Dhillon, VS
Peacock, A
TI High-speed energy-resolved STJ photometry of the eclipsing dwarf nova
IYUMa
SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
LA English
DT Article
DE accretion, accretion discs; binaries : eclipsing; stars : dwarf novae;
stars : individual : IYUMa; novae, cataclysmic variables
ID IY-URSAE-MAJORIS; CATACLYSMIC VARIABLES; BINARIES; SUPERHUMPS
AB We present high-time-resolution photometry of the dwarf nova IY UMa using the S-Cam2 superconducting tunnel junction device attached to the 4.2-m William Herschel Telescope on La Palma. Exploiting the well-defined white dwarf and hotspot eclipse features, we derive an updated orbital ephemeris for IY UMa and an orbital period of 0.073 908 97(5) d. A white dwarf ingress/egress duration of 31 2 s along with the contact phases of the bright-spot gives M (1) = 0.79 0.04 M-circle dot and M (2) = 0.10 0.01 M-circle dot , corresponding to a mass ratio of q = 0.125 0.008. The white dwarf eclipse width of Deltaphi(WD) = 0.0637 then implies . A curious rise with a duration of 30 2 s is present in the orbital light curves during all three observed eclipses. It occurs between the end of white dwarf ingress and hotspot ingress, and is blue in colour. We suggest that the source of this light lies in the buried part of the gas stream, resulting in a compact, hot impact cavity.
C1 Univ Southampton, Dept Phys & Astron, Southampton S017 1BJ, Hants, England.
European Space Technol Ctr, Astrophys Missions Div, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands.
Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.
EM dsteeghs@cfa.harvard.edu
RI Steeghs, Danny/C-5468-2009;
OI Steeghs, Danny/0000-0003-0771-4746; Perryman,
Michael/0000-0002-3953-4750
NR 17
TC 26
Z9 26
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0035-8711
EI 1365-2966
J9 MON NOT R ASTRON SOC
JI Mon. Not. Roy. Astron. Soc.
PD MAR 1
PY 2003
VL 339
IS 3
BP 810
EP 816
DI 10.1046/j.1365-8711.2003.06226.x
PG 7
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 647DN
UT WOS:000181077300025
ER
PT J
AU Cooper, K
AF Cooper, K
TI Voices of a Thousand people: The Makah Cultural and Research Center
SO MUSEUM NEWS
LA English
DT Book Review
C1 Smithsonian Ctr Educ & Museum Studies, Washington, DC USA.
RP Cooper, K (reprint author), Smithsonian Ctr Educ & Museum Studies, Washington, DC USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU AMER ASSOC MUSEUMS
PI WASHINGTON
PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 USA
SN 0027-4089
J9 MUSEUM NEWS
JI Mus. News
PD MAR-APR
PY 2003
VL 82
IS 2
BP 24
EP +
PG 0
WC Art
SC Art
GA 651YX
UT WOS:000181352500022
ER
PT J
AU Seitel, P
AF Seitel, P
TI Theorizing genres, interpreting works
SO NEW LITERARY HISTORY
LA English
DT Article
ID TANZANIA; BARDS
C1 Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA.
RP Seitel, P (reprint author), Smithsonian Inst, Ctr Folklife & Cultural Heritage, Washington, DC 20560 USA.
NR 21
TC 12
Z9 12
U1 0
U2 0
PU JOHNS HOPKINS UNIV PRESS
PI BALTIMORE
PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD
21218-4319 USA
SN 0028-6087
J9 NEW LITERARY HIST
JI New Lit. Hist.
PD SPR
PY 2003
VL 34
IS 2
BP 275
EP 297
DI 10.1353/nlh.2003.0023
PG 23
WC Literature
SC Literature
GA 696WA
UT WOS:000183909500007
ER
PT J
AU Kress, WJ
Htun, T
AF Kress, WJ
Htun, T
TI A second species of Smithatris (Zingiberaceae) from Myanmar
SO NOVON
LA English
DT Article
DE Myanmar; Smithatris; Southeast Asia; Thailand; Zingiberaceae
ID GENUS
AB Smithatris myanmarensis, the second species of a previously monospecific genus, is described from Myanmar. This new species differs from its congener in Thailand by the overall smaller stature, elliptic leaf lamina with long petioles, dimorphic inflorescence bracts, corolla lobes of similar size and shape, the pouch formed by the labellum and lateral staminodes below the anther, and the shallowly lobed labellum.
C1 Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, Washington, DC 20013 USA.
Nat & Wildlife Conservat Div, Forest Dept, Insein, Yangon, Myanmar.
RP Kress, WJ (reprint author), Smithsonian Inst, US Natl Herbarium, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA.
NR 6
TC 2
Z9 2
U1 2
U2 2
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 SPR
PY 2003
VL 13
IS 1
BP 68
EP 71
DI 10.2307/3393567
PG 4
WC Plant Sciences
SC Plant Sciences
GA 661LD
UT WOS:000181891300011
ER
PT J
AU Strong, MT
AF Strong, MT
TI Cypringlea, a new genus of Cyperaceae from Mexico
SO NOVON
LA English
DT Article
DE Cyperaceae; Cyperoideae; Cypringlea; Mexico; Scirpeae; Scirpus;
Trichophorum
AB Studies of the floral morphology of the Mexican endemics Scirpus analecta Beetle and Scirpus coahuilensis Svenson, including embryo morphology and scanning electron microscopy (SEM) studies of the achenes, achene pericarp, and perianth bristles, indicate that like Scirpus L.,they are members of the tribe Scirpeae Knuth ex Dumortier. However, they were found to possess a Carex-type embryo that is characteristic of Trichophorum Persoon. Because of differences in habitat, leaf blade development and morphology, inflorescence morphology, and the possession of rudimentary perianth bristles, they are shown to be better circumscribed in a genus of their own, Cypringlea M. T Strong. Cypringlea is described, and the combinations C. analecta (Beetle) M. I Strong and C. coahuilensis (Svenson) M. I Strong are validated. Drawings of the embryos, SEM images of the achenes, achene pericarp, and perianth bristles, and photographic images of herbarium type specimens of the plants are provided, and the relationships of Cypringlea to Scirpus and Trichophorum are discussed.
C1 Smithsonian Inst, Dept Systemat Biol, Washington, DC 20560 USA.
RP Strong, MT (reprint author), Smithsonian Inst, Dept Systemat Biol, MRC-166,10th & Constitut Ave, Washington, DC 20560 USA.
NR 11
TC 9
Z9 12
U1 0
U2 0
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 SPR
PY 2003
VL 13
IS 1
BP 123
EP 132
DI 10.2307/3393577
PG 10
WC Plant Sciences
SC Plant Sciences
GA 661LD
UT WOS:000181891300021
ER
PT J
AU Galvez, D
Pearcy, RW
AF Galvez, D
Pearcy, RW
TI Petiole twisting in the crowns of Psychotria limonensis: implications
for light interception and daily carbon gain
SO OECOLOGIA
LA English
DT Article
DE crown architecture; petiole twisting; self-shading; light capture;
carbon dioxide assimilation
ID CORNUS-KOUSA CORNACEAE; TRIFOLIUM-REPENS; SOLAR TRACKING; LEAF DISPLAY;
WHITE CLOVER; CAPTURE; FOREST; PLANTS; ARCHITECTURE; PHYTOCHROME
AB We used Y-plant, a computer-based model of crown architecture, to examine the implications of leaf reorientation resulting from petiole bending in Psychotria limonensis (Rubiaceae) seedlings. During this reorientation process, bending of the petioles of lower leaves that are potentially self-shaded by the upper leaves rotates the lamina around the stem's orthotropic axis so that self-shading is reduced. Simulations of daily light capture and assimilation revealed a 66% increase in daily C gain due to reorientation of the leaves as compared to simulations where the leaves remained in their characteristic opposite decussate pattern set by the phyllotaxy. This was due to enhanced carbon (C) gain of the lower leaves because of the reduction of shading by upper developing leaves in the same vertical plane. The light signal for this movement was experimentally examined by placing leaf-shaped filters above already fully expanded leaves and following the resulting shade-avoiding movements. The filters were either neutral density shade cloth that reduced the photon flux density (PFD) but did not alter the red to far red ratio (R:FR) or a film that reduced the PFD equivalently but also reduced the R:FR. Leaf reorientation was much more rapid and complete under the low R:FR as compared to the high R:FR indicating involvement of a phytochrome photosensory system that detected the presence of a shading leaf. Plants in gaps were found to lack a reorientation response indicating that the reorientation is specific to the shaded understory environment.
C1 Univ Calif Davis, Sect Evol & Ecol, Div Biol Sci, Davis, CA 95616 USA.
Smithsonian Trop Res Inst, Balboa, Panama.
RP Pearcy, RW (reprint author), Univ Calif Davis, Sect Evol & Ecol, Div Biol Sci, 1 Shields Ave, Davis, CA 95616 USA.
NR 42
TC 24
Z9 28
U1 0
U2 9
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD MAR
PY 2003
VL 135
IS 1
BP 22
EP 29
DI 10.1007/s00442-002-1158-3
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 672AB
UT WOS:000182497200003
PM 12647100
ER
PT J
AU Becerro, MA
Thacker, RW
Turon, X
Uriz, MJ
Paul, VJ
AF Becerro, MA
Thacker, RW
Turon, X
Uriz, MJ
Paul, VJ
TI Biogeography of sponge chemical ecology: comparisons of tropical and
temperate defenses
SO OECOLOGIA
LA English
DT Article
DE anti-predatory defenses; defense effectiveness; Mediterranean vs
Indo-Pacific; latitudinal gradient; predator-prey relationships
ID PLANT-HERBIVORE INTERACTIONS; BROWN ALGAL PHLOROTANNINS; MARINE
NATURAL-PRODUCTS; PREDATORY REEF FISH; SECONDARY METABOLITES;
GEOGRAPHIC-VARIATION; INDUCIBLE DEFENSES; CARIBBEAN SPONGES;
CRAMBE-CRAMBE; TOXICITY
AB Examples from both marine and terrestrial systems have supported the hypothesis that predation is higher in tropical than in temperate habitats and that, as a consequence, tropical species have evolved more effective defenses to deter predators. Although this hypothesis was first proposed for marine sponges over 25 years ago, our study provides the first experimental test of latitudinal differences in the effectiveness of sponge chemical defenses. We collected 20 common sponge species belonging to 14 genera from tropical Guam and temperate Northeast Spanish coasts (Indo-Pacific and Mediterranean biogeographic areas) and conducted field-based feeding experiments with large and small fish predators in both geographic areas. We use the term global deterrence to describe the deterrent activity of a sponge extract against all of the predators used in our experiments and to test the hypothesis that sponges from Guam are chemically better defended than their Mediterranean counterparts. Sympatric and allopatric deterrence refer to the average deterrent activity of a sponge against sympatric or allopatric predators. All of the sponges investigated in this study showed deterrent properties against some predators. However, 35% of the sponge species were deterrent in at least one but not in all the experiments, supporting the idea that predators can respond to chemical defenses in a species-specific manner. Tropical and temperate sponges have comparable global, sympatric, and allopatric deterrence, suggesting not only that chemical defenses from tropical and temperate sponges are equally strong but also that they are equally effective against sympatric and allopatric predators. Rather than supporting geographic trends in the production of chemical defenses, our data suggest a recurrent selection for chemical defenses in sponges as a general life-history strategy.
C1 CSIC, Ctr Adv Studies, CEAB, Blanes 17300, GI, Spain.
Univ Guam, Marine Lab, Mangilao, GU 96923 USA.
Univ Barcelona, Dept Anim Biol Invertebrates, Barcelona 08028, Spain.
Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA.
Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA.
RP Becerro, MA (reprint author), CSIC, Ctr Adv Studies, CEAB, Blanes 17300, GI, Spain.
EM mikel@ceab.csic.es
RI Becerro, Mikel/A-5325-2008; Uriz, Maria /J-9001-2012; Turon,
Xavier/J-9211-2012;
OI Turon, Xavier/0000-0002-9229-5541; Becerro, Mikel/0000-0002-6047-350X;
Thacker, Robert/0000-0002-9654-0073
NR 91
TC 71
Z9 76
U1 4
U2 31
PU SPRINGER
PI NEW YORK
PA 233 SPRING ST, NEW YORK, NY 10013 USA
SN 0029-8549
EI 1432-1939
J9 OECOLOGIA
JI Oecologia
PD MAR
PY 2003
VL 135
IS 1
BP 91
EP 101
DI 10.1007/s00442-002-1138-7
PG 11
WC Ecology
SC Environmental Sciences & Ecology
GA 672AB
UT WOS:000182497200011
PM 12647108
ER
PT J
AU Lovelock, CE
Feller, IC
AF Lovelock, CE
Feller, IC
TI Photosynthetic performance and resource utilization of two mangrove
species coexisting in a hypersaline scrub forest
SO OECOLOGIA
LA English
DT Article
DE photosynthetic nitrogen use efficiency; photosynthetic water use
efficiency; Avicennia germinans; Laguncularia racemosa; Florida
ID NITROGEN-USE EFFICIENCY; WATER-USE EFFICIENCY; SPARTINA-ALTERNIFLORA;
SALINITY; GROWTH; SOIL; SEEDLINGS; PLANT; FERTILIZATION; AVAILABILITY
AB In a hypersaline mangrove scrub forest in northern Florida, coexisting trees of Laguncularia racemosa and Avicennia germinans were either fertilized with nitrogen or phosphorus, or not fertilized (controls). We aimed to test whether nutrient additions differentially altered photosynthetic performance and resource utilization in these two species. In control trees, photosynthetic rates were higher in L. racemosa than A. germinans. However, leaf nitrogen concentrations were higher in A. germinans than L. racemosa. Avicennia germinans responded to fertilization with nitrogen by increasing leaf nitrogen concentrations and rates of photosynthesis such that they were equivalent to photosynthesis in L. racemosa. Laguncularia racemosa did not show a response to nitrogen additions. Neither species showed strong responses to phosphorus fertilization. Avicennia germinans had high photosynthetic water-use efficiency (photosynthesis/transpiration), but low photosynthetic nitrogen-use efficiency (photosynthesis/leaf nitrogen). In contrast, L. racemosa had comparatively low photosynthetic water use efficiency and high photosynthetic nitrogen use efficiency. Leaf level characteristics lead us to hypothesize that coexistence of A. germinans and L. racemosa should occur where nitrogen levels are low and salinity is moderate, or at least moderate for some period of the year.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Lovelock, CE (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA.
RI Lovelock, Catherine/G-7370-2012;
OI Lovelock, Catherine/0000-0002-2219-6855; Feller,
Ilka/0000-0002-6391-1608
NR 40
TC 60
Z9 69
U1 3
U2 26
PU SPRINGER-VERLAG
PI NEW YORK
PA 175 FIFTH AVE, NEW YORK, NY 10010 USA
SN 0029-8549
J9 OECOLOGIA
JI Oecologia
PD MAR
PY 2003
VL 134
IS 4
BP 455
EP 462
DI 10.1007/s00442-002-1118-y
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 655ZD
UT WOS:000181582700001
PM 12647116
ER
PT J
AU Harrison, RD
Yamamura, N
AF Harrison, RD
Yamamura, N
TI A few more hypotheses for the evolution of dioecy in figs (Ficus,
Moraceae)
SO OIKOS
LA English
DT Article
ID WASP MUTUALISM; SEX-RATIOS; WORLD FIGS; PHENOLOGY; SEED; POLLINATORS;
POPULATIONS; COMMUNITY; DYNAMICS; ECOLOGY
AB In figs (Ficus, Moraceae) there are two breeding systems: monoecy is the ancestral condition but approximately half the 750 odd species are functionally dioecious. Three hypotheses have been proposed for the evolution of dioecy in figs, invoking seasonality (Kjellberg et al. 1987), the reduction of non-pollinating wasp species (Kerdelhue and Rasplus 1996), and the persistence of pollinator populations within small groups of trees (Kameyama et al. 1999). However, there are two major problems with these ideas. Firstly, dioecy has probably evolved only twice (Weiblen 2000), which severely limits our ability to test between alternative hypotheses. Secondly, it is very simple to suggest ways in which dioecy can evolve from monoecy (Charnov 1982). To illustrate this problem, and enlarge on some recent progress in our understanding of functionally dioecious figs, we are proposing a few more hypotheses.
C1 Kyoto Univ, Ctr Ecol Res, Otsu, Shiga 5202113, Japan.
RP Harrison, RD (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA.
NR 46
TC 39
Z9 44
U1 0
U2 10
PU BLACKWELL MUNKSGAARD
PI COPENHAGEN
PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK
SN 0030-1299
J9 OIKOS
JI Oikos
PD MAR
PY 2003
VL 100
IS 3
BP 628
EP 635
DI 10.1034/j.1600-0706.2003.11829.x
PG 8
WC Ecology
SC Environmental Sciences & Ecology
GA 662TD
UT WOS:000181963700026
ER
PT J
AU Behrensmeyer, AK
Stayton, CT
Chapman, RE
AF Behrensmeyer, AK
Stayton, CT
Chapman, RE
TI Taphonomy and ecology of modern avifaunal remains from Amboseli Park,
Kenya (vol 29, pg 52, 2002)
SO PALEOBIOLOGY
LA English
DT Correction
C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
Univ Chicago, Dept Geol & Geophys, Chicago, IL 60637 USA.
Idaho State Univ, ITRC, Pocatello, ID 83209 USA.
RP Behrensmeyer, AK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU PALEONTOLOGICAL SOC INC
PI LAWRENCE
PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA
SN 0094-8373
J9 PALEOBIOLOGY
JI Paleobiology
PD SPR
PY 2003
VL 29
IS 2
BP II
EP II
PG 1
WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology
SC Biodiversity & Conservation; Environmental Sciences & Ecology;
Evolutionary Biology; Paleontology
GA 682BM
UT WOS:000183070500001
ER
PT J
AU Nelson, R
Parker, G
Hom, M
AF Nelson, R
Parker, G
Hom, M
TI A portable airborne laser system for forest inventory
SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING
LA English
DT Article
ID STAND CHARACTERISTICS; CANOPY STRUCTURE; SCANNER DATA; BASAL AREA;
LIDAR; VOLUME; BIOMASS; ALTIMETER; HEIGHT
AB A simple, lightweight, inexpensive, portable airborne laser profiling system has been assembled from off-the-shelf, commercially available components. The system, which costs approximately $30,000, is designed to fly aboard small helicopters and single- or twin-engine high-wing aircraft without airframe modification, The system acquires first-return range and amplitude measurements at data rates up to 2000 hz (operator-con trolled) and has an operational envelope up to 300 m above terrain. The airborne laser profiling system includes the laser transmitter/receiver, differential GPS receiver, a CCD video camera and recorder, and a laptop computer which interleaves and records the GPS and laser range/amplitude data. The portable airborne laser system (PALS) was designed to acquire forest height measurements along linear flight transects in order to conduct regional or subcontinental forest inventories worldwide. This economical laser system now puts airborne laser mensuration within reach of operational foresters and researchers interested in making rapid forest structure and/or timber surveys in remote areas. PALS has been used to acquire over 5000 km of flight transect data over the state of Delaware.
C1 NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA.
Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Nelson, R (reprint author), NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Sci Syst & Applicat Inc, Code 923, Greenbelt, MD 20771 USA.
EM ross@ltpmail.gsfc.nasa.gov; parker@serc.si.edu;
mhom@pop900.gsfc.nasa.gov
RI Nelson, Ross/H-8266-2014;
OI Parker, Geoffrey/0000-0001-7055-6491
NR 28
TC 51
Z9 51
U1 1
U2 3
PU AMER SOC PHOTOGRAMMETRY
PI BETHESDA
PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA
SN 0099-1112
J9 PHOTOGRAMM ENG REM S
JI Photogramm. Eng. Remote Sens.
PD MAR
PY 2003
VL 69
IS 3
BP 267
EP 273
PG 7
WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing;
Imaging Science & Photographic Technology
SC Physical Geography; Geology; Remote Sensing; Imaging Science &
Photographic Technology
GA 817QU
UT WOS:000221192800004
ER
PT J
AU Yu, DH
Williams, JF
Chen, XJ
Hayes, PA
Bartschat, K
Zeman, V
AF Yu, DH
Williams, JF
Chen, XJ
Hayes, PA
Bartschat, K
Zeman, V
TI Cascade effects in the excitation of np(5)(n+1)p states of krypton and
xenon atoms by polarized electrons
SO PHYSICAL REVIEW A
LA English
DT Article
ID GASES; NEON
AB The integrated Stokes parameters of the decay photons from the excited np(5)(n+1)p[5/2](3), np(5)(n+1)p(')[3/2](2), and np(5)(n+1)p(')[3/2](1) (n=5 and 6) states of Kr and Xe, respectively, are measured from near threshold to 100 eV using incident polarized electrons. The effects of the cascade photons on the Stokes parameters have been investigated using a pulsed beam of polarized electrons. The cascade effects for the final excited states are more significant for the linear polarization P-1 parameter than for the circular polarization P-3 parameter and they do not always have depolarization effects. The integrated state multipoles, determined from the integrated Stokes parameters corrected for cascade effects, are closer to, but not in agreement with, the values from semirelativistic R matrix and relativistic distorted-wave approximation methods.
C1 Univ Western Australia, Ctr Atom Mol & Surface Phys, Dept Phys, Perth, WA 6009, Australia.
Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA.
Univ Toronto, Dept Chem, Toronto, ON M5S 3H6, Canada.
Univ Sci & Technol, Dept Modern Phys, Hefei, Peoples R China.
Drake Univ, Dept Phys & Astron, Des Moines, IA 50311 USA.
RP Yu, DH (reprint author), Univ Western Australia, Ctr Atom Mol & Surface Phys, Dept Phys, Perth, WA 6009, Australia.
RI Bartschat, Klaus/I-2527-2012
NR 11
TC 0
Z9 0
U1 0
U2 0
PU AMERICAN 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 MAR
PY 2003
VL 67
IS 3
AR 032707
DI 10.1103/PhysRevA.67.032707
PG 8
WC Optics; Physics, Atomic, Molecular & Chemical
SC Optics; Physics
GA 662TX
UT WOS:000181965900050
ER
PT J
AU Stoner, R
Walsworth, R
AF Stoner, R
Walsworth, R
TI Balancing atoms probe fundamental symmetries
SO PHYSICS WORLD
LA English
DT News Item
C1 Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Stoner, R (reprint author), Charles Stark Draper Lab Inc, Cambridge, MA 02139 USA.
NR 0
TC 0
Z9 0
U1 0
U2 0
PU IOP PUBLISHING LTD
PI BRISTOL
PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND
SN 0953-8585
J9 PHYS WORLD
JI Phys. World
PD MAR
PY 2003
VL 16
IS 3
BP 24
EP 25
PG 2
WC Physics, Multidisciplinary
SC Physics
GA 665LQ
UT WOS:000182122600034
ER
PT J
AU Field, CR
AF Field, CR
TI The Lincoln Memorial and American life
SO PUBLIC HISTORIAN
LA English
DT Book Review
C1 Smithsonian Inst, Washington, DC 20560 USA.
RP Field, CR (reprint author), Smithsonian Inst, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU UNIV CALIF PRESS
PI BERKELEY
PA C/O JOURNALS DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223
USA
SN 0272-3433
J9 PUBL HISTORIAN
JI Public Hist.
PD SPR
PY 2003
VL 25
IS 2
BP 139
EP 141
PG 3
WC History
SC History
GA 703NN
UT WOS:000184286500016
ER
PT J
AU Touwaide, A
AF Touwaide, A
TI Between imitation and plagiarism: Origins and influences in the
'Dioscorides' of Andres Laguna
SO RENAISSANCE QUARTERLY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU RENAISSANCE SOC AMER INC
PI NEW YORK
PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA
SN 0034-4338
J9 RENAISSANCE QUART
JI Renaiss. Q.
PD SPR
PY 2003
VL 56
IS 1
BP 197
EP 201
DI 10.2307/1262284
PG 5
WC Medieval & Renaissance Studies
SC Arts & Humanities - Other Topics
GA 652XW
UT WOS:000181407000039
ER
PT J
AU Touwaide, A
AF Touwaide, A
TI Andres Laguna and humanist medicine: Philological studies
SO RENAISSANCE QUARTERLY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU RENAISSANCE SOC AMER INC
PI NEW YORK
PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA
SN 0034-4338
J9 RENAISSANCE QUART
JI Renaiss. Q.
PD SPR
PY 2003
VL 56
IS 1
BP 197
EP 201
DI 10.2307/1262284
PG 5
WC Medieval & Renaissance Studies
SC Arts & Humanities - Other Topics
GA 652XW
UT WOS:000181407000038
ER
PT J
AU Touwaide, A
AF Touwaide, A
TI Medical humanists in Renaissance Valladolid
SO RENAISSANCE QUARTERLY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU RENAISSANCE SOC AMER INC
PI NEW YORK
PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA
SN 0034-4338
J9 RENAISSANCE QUART
JI Renaiss. Q.
PD SPR
PY 2003
VL 56
IS 1
BP 201
EP 205
DI 10.2307/1262285
PG 5
WC Medieval & Renaissance Studies
SC Arts & Humanities - Other Topics
GA 652XW
UT WOS:000181407000041
ER
PT J
AU Touwaide, A
AF Touwaide, A
TI Sixteenth-century medical humanism at the University of Salamanca
SO RENAISSANCE QUARTERLY
LA English
DT Book Review
C1 Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
RP Touwaide, A (reprint author), Smithsonian Inst, Natl Mus Nat Hist, Washington, DC 20560 USA.
NR 1
TC 0
Z9 0
U1 0
U2 0
PU RENAISSANCE SOC AMER INC
PI NEW YORK
PA 24 WEST 12TH STREET, NEW YORK, NY 10011 USA
SN 0034-4338
J9 RENAISSANCE QUART
JI Renaiss. Q.
PD SPR
PY 2003
VL 56
IS 1
BP 201
EP 205
DI 10.2307/1262285
PG 5
WC Medieval & Renaissance Studies
SC Arts & Humanities - Other Topics
GA 652XW
UT WOS:000181407000040
ER
PT J
AU Smith, DR
AF Smith, DR
TI A synopsis of the sawflies (Hymenoptera : Symphyta) of America south of
the United States: Tenthredinidae (Nematinae, Heterarthrinae,
Tenthredininae)
SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY
LA English
DT Article
ID OLIGOSPILUS FORSTER HYMENOPTERA; NEMATUS; ARGENTINA
AB The subfamilies Nematinae, Heterarthrinae, and Tenthredininae of the Tenthredinidae are reviewed for the Western Hemisphere south of the United States. A key is given for the seven subfamilies of Tenthredinidae for this region. Nematinae include six genera and 17 species, with the following new species: Pristiphora auricauda (Costa Rica), P. fernandezi (Colombia), P. fuscalae (Costa Rica), P. hansoni (Costa Rica), P. helveola (Mexico), and P. semialba (Venezuela). Heterarthrinae include three genera and eight species, with one new species, Brasinusa malaisei (Brazil). Tenthredininae include three genera and four species. All Tenthredininae and many of the Nematinae are southern extensions of northern groups into northern Mexico, and two species, Nematus oligospilus (Foerster) (Nematinae) and Caliroa cerasi (L.) (Heterarthrinae), are introductions into southern South America. All nine species of Pristiphora (Nematinae) and the genera Brasinusa and Notofenusa (Heterarthrinae) are endemic to the Neotropics.
C1 Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
RP Smith, DR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USDA, Agr Res Serv,PSI,Systemat Entomol Lab, Washington, DC 20560 USA.
NR 98
TC 14
Z9 17
U1 0
U2 1
PU AMER ENTOMOL SOC
PI PHILADELPHIA
PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA
SN 0002-8320
J9 T AM ENTOMOL SOC
JI Trans. Am. Entomol. Soc.
PD MAR
PY 2003
VL 129
IS 1
BP 1
EP 45
PG 45
WC Entomology
SC Entomology
GA 667ZN
UT WOS:000182265300001
ER
PT J
AU Stappers, BW
Gaensler, BM
Kaspi, VM
van der Klis, M
Lewin, WHG
AF Stappers, BW
Gaensler, BM
Kaspi, VM
van der Klis, M
Lewin, WHG
TI An x-ray nebula associated with the millisecond pulsar B1957+20
SO SCIENCE
LA English
DT Article
ID CRAB-NEBULA; PARTICLE-ACCELERATION; SYNCHROTRON NEBULA; RADIO PULSARS;
HIGH-ENERGY; BINARY; PSR1957+20; DISCOVERY; EMISSION; HST
AB We have detected an x-ray nebula around the binary millisecond pulsar B1957+20. A narrow tail, corresponding to the shocked pulsar wind, is seen interior to the known Halpha bow shock and proves the long-held assumption that the rotational energy of millisecond pulsars is dissipated through relativistic winds. Unresolved x-ray emission likely represents the shock where the winds of the pulsar and its companion collide. This emission indicates that the efficiency with which relativistic particles are accelerated in the postshock flow is similar to that for young pulsars, despite the shock proximity and much weaker surface magnetic field of this millisecond pulsar.
C1 Stichting ASTRON, NL-7990 Dwingeloo, Netherlands.
Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
McGill Univ, Dept Phys, Montreal, PQ H3A 278, Canada.
MIT, Dept Phys, Cambridge, MA 02139 USA.
MIT, Space Res Ctr, Cambridge, MA 02139 USA.
RP Stappers, BW (reprint author), Stichting ASTRON, NL-7990 Dwingeloo, Netherlands.
RI Gaensler, Bryan/F-8655-2010;
OI Gaensler, Bryan/0000-0002-3382-9558
NR 28
TC 93
Z9 93
U1 0
U2 0
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 FEB 28
PY 2003
VL 299
IS 5611
BP 1372
EP 1374
DI 10.1126/science.1079841
PG 4
WC Multidisciplinary Sciences
SC Science & Technology - Other Topics
GA 649DU
UT WOS:000181192300045
PM 12610299
ER
PT J
AU Clark, KL
Ruiz, GM
Hines, AH
AF Clark, KL
Ruiz, GM
Hines, AH
TI Diel variation in predator abundance, predation risk and prey
distribution in shallow-water estuarine habitats
SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY
LA English
DT Article
DE Chesapeake Bay; diel effects; Palaemonetes pugio; predation risk; prey
response
ID SUBMERGED AQUATIC VEGETATION; CALLINECTES-SAPIDUS RATHBUN; PERCH
MORONE-AMERICANA; TIDAL SALT-MARSH; GULF-OF-MEXICO; CHESAPEAKE-BAY; BLUE
CRABS; PALAEMONETES-PUGIO; FEEDING-HABITS; GRASS SHRIMP
AB Predation by visual predators is often affected by light conditions and may therefore exhibit strong diel variation. The dominant predators on grass shrimp, Palaemonetes pugio, are finfish predators that are thought to locate their prey by visual cues. We examined the response of grass shrimp to diel variation in predation risk in the nearshore shallow waters of the Chesapeake Bay. We used diel shoreline seines to assess the relative abundance of predators, We assessed the relative risk of predation with shrimp tethered at refuge (30 cm) and nourefuge (60 cm) depths. To measure grass shrimp response to predation risk, we used dipnets to monitor habitat use. Four predominantly visual predators dominated the shoreline seine catches, Fundulus heteroclitus, Micropogonias undulatus, Morone americana and Morone saxatilis. Total predator abundance had a diel component, with dramatic nighttime decreases in total abundance, whereas guild composition and relative abundance remained unchanged. Relative predation risk for tethered shrimp exhibited significant time by habitat interaction. During the day, depth negatively affected survivorship of tethered shrimp while at night overall survivorship increased and there was no effect of depth. Shrimp habitats use reflected diel predation risks. Abundances in the near shore were highest during the day with decreased abundances at night. Together, the seine and tethering data highlight the importance for a refuge (e.g., shallow water) from predation during the daytime and a relaxation of predation pressure at night. Published by Elsevier Science B.V.
C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA.
RP Clark, KL (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA.
OI Ruiz, Gregory/0000-0003-2499-441X
NR 63
TC 58
Z9 60
U1 3
U2 18
PU ELSEVIER SCIENCE BV
PI AMSTERDAM
PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS
SN 0022-0981
J9 J EXP MAR BIOL ECOL
JI J. Exp. Mar. Biol. Ecol.
PD FEB 26
PY 2003
VL 287
IS 1
BP 37
EP 55
AR PII S0022-0981(02)00439-2
DI 10.1016/S0022-0981(02)00439-2
PG 19
WC Ecology; Marine & Freshwater Biology
SC Environmental Sciences & Ecology; Marine & Freshwater Biology
GA 646GG
UT WOS:000181026800003
ER
PT J
AU Rufus, J
Stark, G
Smith, PL
Pickering, JC
Thorne, AP
AF Rufus, J
Stark, G
Smith, PL
Pickering, JC
Thorne, AP
TI High-resolution photoabsorption cross section measurements of SO2, 2:
220 to 325 nm at 295 K
SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS
LA English
DT Article
DE ultraviolet absorption spectra; planetary atmospheres; photoabsorption
cross sections
ID FOURIER-TRANSFORM SPECTROMETER; HUBBLE-SPACE-TELESCOPE; SULFUR-DIOXIDE;
ABSORPTION-SPECTRUM; UV; ULTRAVIOLET; SPECTROSCOPY; ATMOSPHERE; IO;
REGION
AB [1] High-resolution, ultraviolet SO2 photoabsorption cross section data are required for modeling density and temperature profiles of SO2 in solar system atmospheres. We report measurements of such cross sections on SO2 at 295 K for the (B) over tilde B-1(1) - (X) over tilde (1)A(1) and (C) over tilde B-1(2)-(X) over tilde (1)A(1) bands over the wavelength range 220 to 325 nm. Resolving powers of up to 550,000 were employed in order to study the congested spectrum of sharp SO2 features in parts of this region. Our data are compared to earlier values obtained with lower resolving power.
C1 Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2BZ, England.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Wellesley Coll, Dept Phys, Wellesley, MA USA.
RP Rufus, J (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Huxley Bldg, London SW7 2BZ, England.
NR 35
TC 40
Z9 40
U1 3
U2 12
PU AMER GEOPHYSICAL UNION
PI WASHINGTON
PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA
SN 0148-0227
J9 J GEOPHYS RES-PLANET
JI J. Geophys. Res.-Planets
PD FEB 25
PY 2003
VL 108
IS E2
AR 5011
DI 10.1029/2002JE001931
PG 5
WC Geochemistry & Geophysics
SC Geochemistry & Geophysics
GA 664RV
UT WOS:000182075500003
ER
PT J
AU Shibatsuka, T
Matsushita, S
Kohno, K
Kawabe, R
AF Shibatsuka, T
Matsushita, S
Kohno, K
Kawabe, R
TI Multi-line observations of molecular gas in the central region of the
low star-formation efficiency "starburst" galaxy NGC 4527
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE galaxies : individual (NGC 4527); galaxies : ISM; galaxies : starburst;
ISM : molecules
ID NEARBY SPIRAL GALAXIES; DENSE GAS; GALACTIC-CENTER; 1.49 GHZ; IC 342;
CO; KINEMATICS; EMISSION; NGC-253; M82
AB We performed high-resolution CO (J = 2-1), CO (J = 1-0), HCN (J = 1-0), HCO+ (J = 1-0), and 3 mm continuum observations of the low star formation efficiency (SFE) "starburst" galaxy NGC 4527 with the Nobeyama Millimeter Array. From CO (J = 1-0) observations, we found two offset ridges with non-circular motion and a central gas concentration. The distribution and kinematics of NGC 4527 are very similar to those of barred spiral galaxies. The distribution of CO (J = 2-1) emission resembles the features of the concentrated component of CO (J = 1-0). HCN (J = 1-0) and HCO+ (J = 1-0) emissions concentrated toward the center have also been detected. The total mass of molecular gas detected in the central r < 30" is 2.5 x 10(9) MD. The HCN (J = 1-0)/CO (J = 1-0) integrated intensity ratio of 0.075 +/- 0.008 in the central r; 3"-4" region of NGC 4527 could suggest that the fraction of dense molecular gas to the total molecular gas is small compared with those of prototypical starburst galaxies, such as NGC 253. This suggests that the small dense gas fraction is responsible for the low SFE in the center of NGC 4527, though this interpretation could depend on aperture sizes of the observations. The ratio of the dynamical mass to molecular gas mass is 13% within the central region (r < 500 pc). This suggests that molecular gas within the r < 500 pc region could be in a state of gravitational instability. The low SFE, the small dense gas fraction, and the large amount of gravitationally unstable molecular gas can be explained if NGC 4527 is in the very early phase of starburst phenomena or a pre-starburst phase, and the formation of dense molecular gas will begin and the SFE will increase within a short time scale.
C1 Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan.
Natl Astron Observ, Mitaka, Tokyo 1818588, Japan.
RP Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan.
EM shiba@nro.nao.ac.jp
NR 67
TC 7
Z9 7
U1 0
U2 0
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB 25
PY 2003
VL 55
IS 1
BP 87
EP 101
DI 10.1093/pasj/55.1.87
PG 15
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 653MZ
UT WOS:000181441500007
ER
PT J
AU Kohno, K
Vila-Vilaro, B
Sakamoto, S
Kawabe, R
Ishizuki, S
Matsushita, S
AF Kohno, K
Vila-Vilaro, B
Sakamoto, S
Kawabe, R
Ishizuki, S
Matsushita, S
TI Aperture synthesis CO (J=1-0) observations and near-infrared photometry
of the non-barred Seyfert galaxy NGC 5033
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Review
DE galaxies : active; galaxies : individual (NGC 5033); galaxies : ISM;
galaxies : Seyfert; galaxies : structure
ID ACTIVE GALACTIC NUCLEI; MOLECULAR INTERSTELLAR-MEDIUM; NOBEYAMA 45-M
TELESCOPE; SUPERMASSIVE BLACK-HOLE; ON SPIRAL GALAXIES; STAR-FORMATION;
CENTRAL REGIONS; MICRON SPECTROSCOPY; PHYSICAL CONDITIONS; DISK GALAXIES
AB Aperture synthesis observations of CO (J = 1-0) emission and near-infrared broad-band photometry of the non-barred Seyfert galaxy NGC 5033 (D = 18.7 Mpc) were performed. Our 3."9 x 3."6 resolution CO observations reveal a perturbed distribution and the kinematics of molecular gas in the center of NGC 5033; we find the characteristic gaseous features that are widely observed in barred spiral galaxies, such as two bright CO peaks near the center (separated by similar to3" or 270 pc from the nucleus), two offset ridges of CO emission emanating from the CO peaks, and a CO ring (with a radius of similar to14" or 1.3 kpc). Double-peaked velocity profiles are also evident near the two CO peaks, implying that these CO peaks,are orbit crowding zones in a barred/oval potential. Although NIR data only give an upper limit of the possible bar lengths due to a large inclination of the NGC 5033 disk (i = 68degrees), our CO data clearly suggests the presence of a small (the semi-major axis of about 12"-15" or 1.1-1.4 kpc) nuclear bar (or oval structure) in the center of the "non-barred" galaxy NGC 5033. Our results demonstrate that high-resolution CO imaging-spectroscopy is useful to search for nuclear bars, even in highly inclined systems where isophoto fitting techniques are not applicable. We find that the gas mass-to-dynamical mass ratio, M-gas/M-dyn, is small (less than or equal to 1%) within a radius of 2" or 180 pc, in contrast to starburst nuclei. This implies that the starburst does not cohabitate in the type-1.5 Seyfert nucleus of NGC 5033.
C1 Univ Tokyo, Astron Inst, Mitaka, Tokyo 1810015, Japan.
Univ Arizona, Steward Observ, Tucson, AZ 85721 USA.
Natl Astron Observ, Mitaka, Tokyo 1818588, Japan.
Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
RP Univ Tokyo, Astron Inst, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan.
EM kkohno@ioa.s.u-tokyo.ac.jp; bvila@as.arizona.edu; seiichi@nro.nao.ac.jp;
kawabe@nro.nao.ac.jp; ishizksm@cc.nao.ac.jp; smatsushita@cfa.harvard.edu
NR 114
TC 4
Z9 4
U1 0
U2 4
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB 25
PY 2003
VL 55
IS 1
BP 103
EP 119
DI 10.1093/pasj/55.1.103
PG 17
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 653MZ
UT WOS:000181441500008
ER
PT J
AU Matsushita, S
Matsuo, H
AF Matsushita, S
Matsuo, H
TI FTS measurements of submillimeter-wave atmospheric opacity at Pampa la
Bola: III. Water vapor, liquid water, and 183 GHz water vapor line
opacities
SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
LA English
DT Article
DE atmospheric effects; instrumentation : spectrometer; site testing;
submillimeter
ID COMPLEX PERMITTIVITY; PHASE CORRECTION; NORTHERN CHILE; MAUNA-KEA; 1
THZ; MODEL; SITE; TRANSMISSION; MONITORS; ICE
AB Further analysis has been made on the millimeter- and submillimeter-wave (100-1600 GHz or 3mm-188 mum) atmospheric opacity data taken with the Fourier Transform Spectrometer (FTS) at Pampa la Bola, 4800 m above the sea level in northern Chile, which is the site of the Atacama Large Millimeter/submillimeter Array (ALMA). Time-sequence plots of millimeter- and submillimeter-wave opacities show similar variations to each other, except for during the periods with liquid water (fog or clouds) in the atmosphere. Using millimeter- and submillimeter-wave opacity correlations under two conditions, which are affected and not affected by liquid water, we succeeded to separate the measured opacity into water vapor and liquid water opacity components. The water vapor opacity shows a good correlation with the 183 GHz water vapor line opacity, which is also covered in the measured spectra. On the other hand, the liquid water opacity and the 183 GHz line opacity show no correlation. Since only the water vapor component is expected to affect the phase of interferometers significantly, and the submillimeter-wave opacity is less affected by the liquid water component, it may be possible to use the submillimeter-wave opacity for a phase correction of submillimeter interferometers.
C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA.
Natl Astron Observ, Ctr Adv Technol, Mitaka, Tokyo 1818588, Japan.
RP Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA.
EM smatsushita@cfa.harvard.edu; h.matsuo@nao.ac.jp
RI Matsuo, Hiroshi/F-4807-2013
OI Matsuo, Hiroshi/0000-0003-3278-2484
NR 47
TC 11
Z9 11
U1 0
U2 2
PU OXFORD UNIV PRESS
PI OXFORD
PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
SN 0004-6264
EI 2053-051X
J9 PUBL ASTRON SOC JPN
JI Publ. Astron. Soc. Jpn.
PD FEB 25
PY 2003
VL 55
IS 1
BP 325
EP 333
DI 10.1093/pasj/55.1.325
PG 9
WC Astronomy & Astrophysics
SC Astronomy & Astrophysics
GA 653MZ
UT WOS:000181441500028
ER
EF